@article{Lang2010,
author = {{Lang}, D. and {Hogg}, D.~W. and {Mierle}, K. and {Blanton}, M. and {Roweis}, S.},
title = {{Astrometry.net: Blind astrometric calibration of arbitrary astronomical images}},
journal = {\AJ},
year = {2010},
volume = {137},
pages = {1782--2800},
note = {arXiv:0910.2233},
adsurl = {http://adsabs.harvard.edu/abs/2009arXiv0910.2233L},
}
@article{Metzger2009,
abstract = {Despite its probable occurrence in Nature, the accretion-induced collapse (AIC) of a white dwarf has not yet been directly observed (or, at least, it has not been unambiguously identified as such). In this contribution we summarize the observational signatures of AIC, emphasizing its possible role as both an optical and high-energy transient.},
archiveprefix = {arXiv},
arxivid = {0908.1127},
author = {Metzger, B. D. and Piro, A. L. and Quataert, E. and Thompson, T. A.},
eprint = {0908.1127},
keywords = {Astrophysics - High Energy Astrophysical Phenomena},
language = {en},
month = {aug},
pages = {6},
title = {{Observable Signatures of the Accretion-Induced Collapse of White Dwarfs}},
url = {http://adsabs.harvard.edu/abs/2009arXiv0908.1127M},
year = {2009},
}
@article{Benetti2005,
author = {Benetti, S and Cappellaro, E and Mazzali, P A and Turatto, M and Altavilla, G and Bufano, F and Elias‐Rosa, N. and Kotak, R and Pignata, G and Salvo, M and Stanishev, V},
doi = {10.1086/428608},
file = {:Users/svalenti/Documents/Mendeley Desktop/2005/The Astrophysical Journal/2005 Benetti.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {apr},
number = {2},
pages = {1011--1016},
title = {{The Diversity of Type Ia Supernovae: Evidence for Systematics?}},
url = {http://stacks.iop.org/0004-637X/623/i=2/a=1011},
volume = {623},
year = {2005},
}
@article{2008ApJ...687.1201K,
author = {Kelly, Patrick L and Kirshner, Robert P and Pahre, Michael},
file = {:Users/svalenti/Documents/Mendeley Desktop/2008/The Astrophysical Journal/2008 Kelly.pdf:pdf},
journal = {The Astrophysical Journal},
month = {nov},
number = {2},
pages = {1201--1207},
title = {{Long $\gamma$-Ray Bursts and Type Ic Core-Collapse Supernovae Have Similar Locations in Hosts}},
volume = {687},
year = {2008},
}
@article{Menzies1987,
author = {Menzies, J. W. and Catchpole, R. M. and van Vuuren, G. and Winkler, H. and Laney, C. D. and Whitelock, P. A. and Cousins, A. W. J. and Carter, B. S. and Marang, F. and {Lloyd Evans}, T. H. H. and Roberts, G. and Kilkenny, D. and {Spencer Jones}, J. and Sekiguchi, K. and Fairall, A. P. and Wolstencroft, R. D.},
file = {:Users/svalenti/Documents/Mendeley Desktop/1987/Monthly Notices of the Royal Astronomical Society/1987MNRAS\_227P\_\_39M.pdf:pdf},
issn = {0035-8711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {ASTRONOMICAL PHOTOMETRY,ASTRONOMICAL SPECTROSCOPY,H ALPHA LINE,LIGHT CURVE,MAGELLANIC CLOUDS,RADII,STELLAR MAGNITUDE,STELLAR TEMPERATURE,SUPERNOVA 1987A,UBV SPECTRA},
language = {en},
month = {aug},
pages = {39P--49P},
title = {{Spectroscopic and photometric observations of SN 1987a - The first 50 days}},
url = {http://adsabs.harvard.edu/abs/1987MNRAS.227P..39M},
volume = {227},
year = {1987},
}
@article{Baron2000,
abstract = {We have calculated fast direct spectral model fits to two early-time spectra of the Type II plateau SN 1999em, using the SYNOW synthetic spectrum code. The first is an extremely early blue optical spectrum and the second a combined Hubble Space Telescope and optical spectrum obtained one week later. Spectroscopically this supernova appears to be a normal Type II, and these fits are in excellent agreement with the observed spectra. Our direct analysis suggests the presence of enhanced nitrogen. We have further studied these spectra with the full non-LTE general model atmosphere code PHOENIX. While we do not find confirmation for enhanced nitrogen (nor do we rule it out), we do require enhanced helium. An even more intriguing possible line identification is complicated Balmer and He I lines, which we show falls naturally out of the detailed calculations with a shallow density gradient. We also show that very early spectra such as those presented here combined with sophisticated spectral modeling allow an independent estimate of the total reddening to the supernova, since when the spectrum is very blue, dereddening leads to changes in the blue flux that cannot be reproduced by altering the ``temperature'' of the emitted radiation. These results are extremely encouraging since they imply that detailed modeling of early spectra can shed light on both the abundances and total extinction of SNe II, the latter improving their utility and reliability as distance indicators.},
author = {Baron, E. and Branch, David and Hauschildt, Peter H. and Filippenko, Alexei V. and Kirshner, R. P. and Challis, P. M. and Jha, S. and Chevalier, R. and Fransson, Claes and Lundqvist, Peter and Garnavich, Peter and Leibundgut, Bruno and McCray, R. and Michael, E. and Panagia, Nino and Phillips, M. M. and Pun, C. S. J. and Schmidt, Brian and Sonneborn, George and Suntzeff, N. B. and Wang, L. and Wheeler, J. C.},
doi = {10.1086/317795},
file = {:Users/svalenti/Documents/Mendeley Desktop/2000/The Astrophysical Journal/51790.web.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {Radiative Transfer,Stars: Atmospheres,Stars: Supernovae: Individual: Alphanumeric: SN 19},
month = {dec},
number = {1},
pages = {444--448},
title = {{Preliminary Spectral Analysis of the Type II Supernova 1999em}},
url = {http://adsabs.harvard.edu/abs/2000ApJ...545..444B},
volume = {545},
year = {2000},
}
@article{Bloom2012,
abstract = {The rate of image acquisition in modern synoptic imaging surveys has already begun to outpace the feasibility of keeping astronomers in the real-time discovery and classification loop. Here we present the inner workings of a framework, based on machine-learning algorithms, that captures expert training and ground-truth knowledge about the variable and transient sky to automate (1) the process of discovery on image differences, and (2) the generation of preliminary science-type classifications of discovered sources. Since follow-up resources for extracting novel science from fast-changing transients are precious, self-calibrating classification probabilities must be couched in terms of efficiencies for discovery and purity of the samples generated. We estimate the purity and efficiency in identifying real sources with a two-epoch image-difference discovery algorithm for the Palomar Transient Factory (PTF) survey. Once given a source discovery, using machine-learned classification trained on PTF data, we distinguish between transients and variable stars with a 3.8\% overall error rate (with 1.7\% errors for imaging within the Sloan Digital Sky Survey footprint). At \>96\% classification efficiency, the samples achieve 90\% purity. Initial classifications are shown to rely primarily on context-based features, determined from the data itself and external archival databases. In the first year of autonomous operations of PTF, this discovery and classification framework led to several significant science results, from outbursting young stars to subluminous Type IIP supernovae to candidate tidal disruption events. We discuss future directions of this approach, including the possible roles of crowdsourcing and the scalability of machine learning to future surveys such as the Large Synoptic Survey Telescope (LSST).},
author = {Bloom, J. S. and Richards, J. W. and Nugent, P. E. and Quimby, R. M. and Kasliwal, M. M. and Starr, D. L. and Poznanski, D. and Ofek, E. O. and Cenko, S. B. and Butler, N. R. and Kulkarni, S. R. and Gal-Yam, A. and Law, N.},
doi = {10.1086/668468},
issn = {00046280},
journal = {Publications of the Astronomical Society of the Pacific},
keywords = {Data Analysis and Techniques},
month = {nov},
number = {921},
pages = {1175--1196},
title = {{Automating Discovery and Classification of Transients and Variable Stars in the Synoptic Survey Era}},
url = {http://adsabs.harvard.edu/abs/2012PASP..124.1175B},
volume = {124},
year = {2012},
}
@article{2012ApJ...749L..28V,
author = {Valenti, Stefano and Taubenberger, Stefan and Pastorello, Andrea and Aramyan, Levon and Botticella, Maria Teresa and Fraser, Morgan and Benetti, Stefano and Smartt, Stephen J and Cappellaro, Enrico and Elias-Rosa, Nancy and Ergon, Mattias and Magill, Lindsay and Magnier, Eugene and Kotak, Rubina and Price, Paul A and Sollerman, Jesper and Tomasella, Lina and Turatto, Massimo and Wright, Darryl E},
doi = {10.1088/2041-8205/749/2/L28},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/The Astrophysical Journal/2012 Valenti.pdf:pdf},
issn = {2041-8205},
journal = {The Astrophysical Journal},
month = {apr},
number = {2},
pages = {L28},
title = {{A Spectroscopically Normal Type Ic Supernova from a Very Massive Progenitor}},
url = {http://stacks.iop.org/2041-8205/749/i=2/a=L28?key=crossref.7a1ecb10314fb28e096730c11f5c9965},
volume = {749},
year = {2012},
}
@article{Gezari2008,
author = {Gezari, Suvi and Dessart, Luc and Basa, St\'{e}phane and Martin, D Chris and Neill, James D and Woosley, S E and Hillier, D John and Bazin, Gurvan and Forster, Karl and Friedman, Peter G and {Le Du}, J\'{e}r\'{e}my and Mazure, Alain and Morrissey, Patrick and Neff, Susan G. and Schiminovich, David and Wyder, Ted K.},
doi = {10.1086/591647},
file = {:Users/svalenti/Documents/Mendeley Desktop/2008/The Astrophysical Journal/2008 Gezari.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {aug},
number = {2},
pages = {L131--L134},
title = {{Probing Shock Breakout with Serendipitous GALEX Detections of Two SNLS Type II-P Supernovae}},
url = {http://stacks.iop.org/1538-4357/683/i=2/a=L131},
volume = {683},
year = {2008},
}
@article{2010MNRAS.406..782S,
author = {Sullivan, M and Conley, A and Howell, D.\~{}A. and Neill, J D and Astier, P and Balland, C and Basa, S and Carlberg, R G and Fouchez, D and Guy, J and Hardin, D and Hook, I M and Pain, R and Palanque-Delabrouille, N and Perrett, K M and Pritchet, C J and Regnault, N and Rich, J and Ruhlmann-Kleider, V and Baumont, S and Hsiao, E and Kronborg, T and Lidman, C and Perlmutter, S and Walker, E S},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2010 Sullivan.pdf:pdf},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {aug},
number = {2},
pages = {782--802},
title = {{The dependence of Type Ia Supernovae luminosities on their host galaxies}},
volume = {406},
year = {2010},
}
@article{Crockett2007,
abstract = {Images of the site of the Type Ic supernova (SN) 2002ap taken before explosion were analysed previously by Smartt et al. We have uncovered new unpublished, archival pre-explosion images from the Canada-France-Hawaii Telescope (CFHT) that are vastly superior in depth and image quality. In this paper we present a further search for the progenitor star of this unusual Type Ic SN. Aligning high-resolution Hubble Space Telescope observations of the SN itself with the archival CFHT images allowed us to pinpoint the location of the progenitor site on the ground-based observations. We find that a source visible in the B- and R-band pre-explosion images close to the position of the SN is (1) not coincident with the SN position within the uncertainties of our relative astrometry and (2) is still visible \~{}4.7-yr post-explosion in late-time observations taken with the William Herschel Telescope. We therefore conclude that it is not the progenitor of SN 2002ap. We derived absolute limiting magnitudes for the progenitor of MB >= -4.2 +/- 0.5 and MR >= -5.1 +/- 0.5. These are the deepest limits yet placed on a Type Ic SN progenitor. We rule out all massive stars with initial masses greater than 7- 8Msolar (the lower mass limit for stars to undergo core collapse) that have not evolved to become Wolf-Rayet stars. This is consistent with the prediction that Type Ic SNe should result from the explosions of Wolf-Rayet stars. Comparing our luminosity limits with stellar models of single stars at appropriate metallicity (Z = 0.008) and with standard mass-loss rates, we find no model that produces a Wolf-Rayet star of low enough mass and luminosity to be classed as a viable progenitor. Models with twice the standard mass-loss rates provide possible single star progenitors but all are initially more massive than 30-40Msolar. We conclude that any single star progenitor must have experienced at least twice the standard mass-loss rates, been initially more massive than 30-40Msolar and exploded as a Wolf-Rayet star of final mass 10-12Msolar. Alternatively a progenitor star of lower initial mass may have evolved in an interacting binary system. Mazzali et al. propose such a binary scenario for the progenitor of SN 2002ap in which a star of initial mass 15-20Msolar is stripped by its binary companion, becoming a 5Msolar Wolf-Rayet star prior to explosion. We constrain any possible binary companion to a main-sequence star of <=20Msolar, a neutron star or a black hole. By combining the pre-explosion limits with the ejecta mass estimates and constraints from X-ray and radio observations we conclude that any binary interaction most likely occurred as Case B mass transfer, either with or without a subsequent common-envelope evolution phase.},
author = {Crockett, R. M. and Smartt, S. J. and Eldridge, J. J. and Mattila, S. and Young, D. R. and Pastorello, A. and Maund, J. R. and Benn, C. R. and Skillen, I.},
doi = {10.1111/j.1365-2966.2007.12283.x},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/Monthly Notices of the Royal Astronomical Society/MNRAS-2007-Crockett-835-50.pdf:pdf},
issn = {0035-8711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {galaxies: individual: M 74,stars: evolution,supernovae: general,supernovae: individual: SN 2002ap},
month = {oct},
number = {2},
pages = {835--850},
title = {{A deeper search for the progenitor of the Type Ic supernova 2002ap}},
url = {http://adsabs.harvard.edu/abs/2007MNRAS.381..835C http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2007.12283.x},
volume = {381},
year = {2007},
}
@article{2007Natur.447..829P,
author = {Pastorello, A and Smartt, S.\~{}J. and Mattila, S and Eldridge, J J and Young, D and Itagaki, K and Yamaoka, H and Navasardyan, H and Valenti, S and Patat, F and Agnoletto, I and Augusteijn, T and Benetti, S and Cappellaro, E and Boles, T and Bonnet-Bidaud, J.-M. and Botticella, M T and Bufano, F and Cao, C and Deng, J and Dennefeld, M and Elias-Rosa, N and Harutyunyan, A and Keenan, F P and Iijima, T and Lorenzi, V and Mazzali, P.\~{}A. and Meng, X and Nakano, S and Nielsen, T B and Smoker, J V and Stanishev, V and Turatto, M and Xu, D and Zampieri, L},
journal = {Nature},
month = {jun},
number = {7},
pages = {829--832},
title = {{A giant outburst two years before the core-collapse of a massive star}},
volume = {447},
year = {2007},
}
@article{Quimby2011,
abstract = {Supernovae are stellar explosions driven by gravitational or thermonuclear energy that is observed as electromagnetic radiation emitted over weeks or more. In all known supernovae, this radiation comes from internal energy deposited in the outflowing ejecta by one or more of the following processes: radioactive decay of freshly synthesized elements (typically (56)Ni), the explosion shock in the envelope of a supergiant star, and interaction between the debris and slowly moving, hydrogen-rich circumstellar material. Here we report observations of a class of luminous supernovae whose properties cannot be explained by any of these processes. The class includes four new supernovae that we have discovered and two previously unexplained events (SN 2005ap and SCP 06F6) that we can now identify as members of the same class. These supernovae are all about ten times brighter than most type Ia supernova, do not show any trace of hydrogen, emit significant ultraviolet flux for extended periods of time and have late-time decay rates that are inconsistent with radioactivity. Our data require that the observed radiation be emitted by hydrogen-free material distributed over a large radius (∼10(15) centimetres) and expanding at high speeds (>10(4) kilometres per second). These long-lived, ultraviolet-luminous events can be observed out to redshifts z > 4.},
archiveprefix = {arXiv},
arxivid = {0910.0059},
author = {Quimby, R M and Kulkarni, S R and Kasliwal, M M and Gal-Yam, A. and Arcavi, I. and Sullivan, M and Nugent, P and Thomas, R and Howell, D. A. and Nakar, E. and Bildsten, L. and Theissen, C. and Law, N M and Dekany, R. and Rahmer, G. and Hale, D. and Smith, R. and Ofek, E. O. and Zolkower, J. and Velur, V. and Walters, R. and Henning, J. and Bui, K. and McKenna, D. and Poznanski, D. and Cenko, S. B. and Levitan, D.},
doi = {10.1038/nature10095},
eprint = {0910.0059},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/Nature/2011 Quimby.pdf:pdf},
issn = {1476-4687},
journal = {Nature},
month = {jun},
number = {7352},
pages = {487--9},
pmid = {21654747},
title = {{Hydrogen-poor superluminous stellar explosions.}},
url = {http://arxiv.org/abs/0910.0059 http://www.ncbi.nlm.nih.gov/pubmed/21654747},
volume = {474},
year = {2011},
}
@article{2008AJ....135.1136M,
annote = {accepted by the Astronomical Journal, 18 pages, emulate-apj, v2 contains more data than v1; conclusions strengthened, SN selection \{\&\},
}
@article{2002AJ....124..417H,
author = {Hamuy, Mario and Maza, Jos\'{e} and Pinto, Philip A and Phillips, M.\~{}M. and Suntzeff, Nicholas B and Blum, R D and Olsen, K A G and Pinfield, David J and Ivanov, Valentin D and Augusteijn, T and Brillant, S and Chadid, M and Cuby, J.-G. and Doublier, V and Hainaut, O R and {Le Floc'h}, E and Lidman, C and Petr-Gotzens, Monika G and Pompei, E and Vanzi, L},
journal = {The Astronomical Journal},
month = {jul},
number = {1},
pages = {417--429},
title = {{Optical and Infrared Spectroscopy of SN 1999ee and SN 1999ex}},
volume = {124},
year = {2002},
}
@article{2010ApJ...721..777A,
author = {Arcavi, Iair and Gal-Yam, Avishay and Kasliwal, Mansi M and Quimby, Robert M and Ofek, Eran O and Kulkarni, Shrinivas R and Nugent, Peter E and Cenko, S Bradley and Bloom, Joshua S and Sullivan, Mark and Howell, D Andrew and Poznanski, Dovi and Filippenko, Alexei V and Law, Nicholas and Hook, Isobel and J\"{o}nsson, Jakob and Blake, Sarah and Cooke, Jeff and Dekany, Richard and Rahmer, Gustavo and Hale, David and Smith, Roger and Zolkower, Jeff and Velur, Viswa and Walters, Richard and Henning, John and Bui, Kahnh and McKenna, Dan and Jacobsen, Janet},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/The Astrophysical Journal/2010 Arcavi.pdf:pdf},
journal = {The Astrophysical Journal},
month = {sep},
number = {1},
pages = {777--784},
title = {{Core-collapse Supernovae from the Palomar Transient Factory: Indications for a Different Population in Dwarf Galaxies}},
volume = {721},
year = {2010},
}
@article{Lyman2013,
abstract = {We present a study of the properties of the host galaxies of unusual transient objects of two types, both being sub-luminous compared with the major classes of supernovae. Those of one type exhibit unusually strong calcium features, and have been termed 'Ca-rich'. Those of the second type, with SN2002cx as the prototype and SN2008ha as the most extreme example to date, have some properties in common with the first, but show typically lower ejecta velocities, and different early spectra. We confirm important differences in the environments of the two types, with the Ca-rich transients preferentially occurring in galaxies dominated by old stellar populations. Quantitatively, the association of the the Ca-rich transients with regions of ongoing star formation is well matched to that of type Ia supernovae. The SN2002cx-like transients are very different, with none of the present sample occurring in an early-type host, and a statistical association with star-formation regions similar to that of type II-P supernovae, and therefore a delay time of 30-50 Myrs.},
archiveprefix = {arXiv},
arxivid = {1306.2474},
author = {Lyman, Joseph and James, Phil and Perets, Hagai B. and Anderson, Joseph P. and Gal-Yam, Avishay and Mazzali, Paolo and Percival, Sue},
doi = {10.1093/mnras/stt1038},
eprint = {1306.2474},
file = {:Users/svalenti/Documents/Mendeley Desktop/2013/Monthly Notices of the Royal Astronomical Society/MNRAS-2013-Lyman-527-41.pdf:pdf},
issn = {0035-8711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {supernovae: general},
language = {en},
month = {jun},
pages = {16},
title = {{Environment-derived constraints on the progenitors of low-luminosity type I supernovae}},
url = {http://adsabs.harvard.edu/abs/2013MNRAS.tmp.1707L http://arxiv.org/abs/1306.2474},
volume = {-1},
year = {2013},
}
@article{Stritzinger2002,
author = {Stritzinger, Maximilian and Hamuy, Mario and Suntzeff, Nicholas B and Smith, R C and Phillips, M. M. and Maza, Jos\'{e} and Strolger, L.-G. and Antezana, Roberto and Gonz\'{a}lez, Luis and Wischnjewsky, Marina and Candia, Pablo and Espinoza, Juan and Gonz\'{a}lez, David and Stubbs, Christopher and Becker, A. C. and Rubenstein, Eric P and Galaz, Gaspar},
doi = {10.1086/342544},
file = {:Users/svalenti/Documents/Mendeley Desktop/2002/The Astronomical Journal/2002 Stritzinger.pdf:pdf},
issn = {00046256},
journal = {The Astronomical Journal},
keywords = {1 visiting astronomer,aura,cerro tololo inter-american observatory,for research in astronomy,inc,individual,photometric,sn 1999ee,sn 1999ex,supernovae,techniques,the association of universities,the national science foundation,under cooperative agreement with,which is operated by},
month = {oct},
number = {4},
pages = {2100--2117},
title = {{Optical Photometry of the Type Ia Supernova 1999ee and the Type Ib/c Supernova 1999ex in IC 5179}},
url = {http://stacks.iop.org/1538-3881/124/i=4/a=2100},
volume = {124},
year = {2002},
}
@article{Botticella2009,
author = {Botticella, M. T. and Pastorello, a. and Smartt, S. J. and Meikle, W. P. S. and Benetti, S. and Kotak, R. and Cappellaro, E. and Crockett, R. M. and Mattila, S. and Sereno, M. and Patat, F. and Tsvetkov, D. and {Van Loon}, J. Th. and Abraham, D. and Agnoletto, I. and Arbour, R. and Benn, C. and {Di Rico}, G. and Elias-Rosa, N. and Gorshanov, D. L. and Harutyunyan, a. and Hunter, D. and Lorenzi, V. and Keenan, F. P. and Maguire, K. and Mendez, J. and Mobberley, M. and Navasardyan, H. and Ries, C. and Stanishev, V. and Taubenberger, S. and Trundle, C. and Turatto, M. and Volkov, I. M.},
doi = {10.1111/j.1365-2966.2009.15082.x},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2009 Botticella.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {agb and post-agb,general,individual,ngc300 ot2008-1,sn 2008s,stars,supernovae},
month = {sep},
number = {3},
pages = {1041--1068},
title = {{SN 2008S: an electron-capture SN from a super-AGB progenitor?}},
url = {http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2009.15082.x},
volume = {398},
year = {2009},
}
@article{1986A&A...154..279M,
abstract = {A chemical evolution model in which nucleosynthesis products coming from type I and II SNe are taken into account is presently used to compute the evolution of C-12, O-16, Mg-24, Si-28, and Fe-56 in the solar neighborhood. A binary model is used for the type I SNe, and a detailed rate of their occurrence is obtained. Attention is given to the implications of the good reproduction obtained for the behavior of the O/Fe abundance ratio in both halo and disk stars. Overabundances of Si and Mg are predicted for metal-poor stars; the finding that C should be overabundant in metal-poor stars, at variance with the observations, is suggested to be due to either a too-high Fe production from type I SNe or to a need for the theoretical yield of C from type II SNe to be smaller.},
author = {{Matteucci, F.} and {Greggio, L.} and Matteucci, F and Greggio, L},
journal = {Astronomy and Astrophysics (ISSN 0004-6361)},
keywords = {CHEMICAL EVOLUTION,COMPUTATIONAL ASTROPHYSICS,GALACTIC EVOLUTION,INTERSTELLAR GAS,NUCLEAR FUSION,SOLAR SYSTEM,STELLAR EVOLUTION,SUPERNOVAE},
month = {jan},
pages = {279--287},
title = {{Relative roles of type I and II supernovae in the chemical enrichment of the interstellar gas}},
url = {http://adsabs.harvard.edu/abs/1986A\&A...154..279M},
volume = {154},
year = {1986},
}
@article{Iwamoto1994,
abstract = {SN 1994I in M51 has provided light curves in various wavelength bands allowing a distinction between models of Type Ic supernovae. We present bolometric and monochromatic light curves of exploding C+O stars that form from approximately 13-15 solar mass stars through the losses of the H-rich and He envelopes in close binary systems. The slopes of the calculated light curves are sensitive to the models and found to be in excellent agreement with the observed light curves for the 0.9 solar mass ejecta model. A high interstellar reddening AV is approximately equal to 1.4 mag) is required. From the light curve fits, a distance modulus of 29.2 +/- 0.3 mag is derived for M51. The ejected Ni-56 mass is found to be 0.07(plus 0.035 or minus 0.025) solar mass. Possibilities to observe gamma rays from SN 1994I with Compton Gamma Ray Observatory (CGRO) are discussed.},
author = {Iwamoto, Kohichi and Nomoto, Ken'ichi and Hoflich, Peter and Yamaoka, Hitoshi and Kumagai, Shiomi and Shigeyama, Toshikazu},
doi = {10.1086/187696},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {BINARY STARS,CARBON STARS,DISTANCE,GAMMA RAY OBSERVATORY,LIGHT CURVE,MONOCHROMATIC RADIATION,NICKEL ISOTOPES,NUMERICAL ANALYSIS,RADIATIVE TRANSFER,STELLAR ENVELOPES,STELLAR MASS,STELLAR MODELS,SUPERNOVAE},
month = {dec},
pages = {L115},
title = {{Theoretical light curves for the type IC supernova SN 1994I}},
url = {http://adsabs.harvard.edu/abs/1994ApJ...437L.115I},
volume = {437},
year = {1994},
}
@article{Capaccioli1989,
author = {Capaccioli, Massimo and della Valle, Massimo and Rosino, Leonida and D'Onofrio, Mauro},
doi = {10.1086/115104},
file = {:Users/svalenti/Documents/Mendeley Desktop/1989/The Astronomical Journal/1989 Capaccioli.pdf:pdf},
issn = {00046256},
journal = {The Astronomical Journal},
month = {jun},
pages = {1622},
title = {{Properties of the nova population in M31}},
url = {http://adsabs.harvard.edu/cgi-bin/bib\_query?1989AJ.....97.1622C},
volume = {97},
year = {1989},
}
@article{2010Msngr.140...20P,
author = {Pasquini, L and Cristiani, S and Garcia-Lopez, R and Haehnelt, M and Mayor, M},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/The Messenger/2010 Pasquini.pdf:pdf},
journal = {The Messenger},
month = {jun},
pages = {20--21},
title = {{CODEX: An Ultra-stable High Resolution Spectrograph for the E-ELT}},
volume = {140},
year = {2010},
}
@article{Smith2011,
author = {Smith, Nathan and Li, Weidong and Filippenko, Alexei V. and Chornock, Ryan},
doi = {10.1111/j.1365-2966.2011.17229.x},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2011 Smith.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {1 i n t,binaries,ccsne,evolution,general,mass-loss,provide key information about,ro d u c,stars,supernovae,t i o n,the evolution and ultimate,the observed fractions of,various types of core-collapse},
month = {apr},
number = {3},
pages = {1522--1538},
title = {{Observed fractions of core-collapse supernova types and initial masses of their single and binary progenitor stars}},
url = {http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2011.17229.x},
volume = {412},
year = {2011},
}
@article{2011ATel.3288....1G,
author = {Gal-Yam, A and Nugent, P and Silverman, J and Badenes, C and Matheson, T and Walker, E and Arcavi, I and Xu, D and Sternberg, A and Bloom, J},
journal = {The Astronomer's Telegram},
month = {apr},
pages = {1},
title = {{PTF weekly SN discovery report, April 15, 2011}},
volume = {3288},
year = {2011},
}
@article{2003MNRAS.338..939E,
author = {Elmhamdi, Abouazza and Danziger, I J and Chugai, N and Pastorello, A and Turatto, M and Cappellaro, E and Altavilla, G and Benetti, S and Patat, F and Salvo, M},
journal = {Monthly Notice of the Royal Astronomical Society},
month = {feb},
number = {4},
pages = {939--956},
title = {{Photometry and spectroscopy of the Type IIP SN 1999em from outburst to dust formation}},
volume = {338},
year = {2003},
}
@article{Eldridge2004,
abstract = {We present maps of the nature of single star progenitors of supernovae and their remnants in mass and metallicity space. We find our results are similar to others but we have gone further in varying the amount of mixing and using various mass-loss schemes to see how the maps change. We find that extra mixing, in the form of convective overshooting, moves boundaries such as the minimum mass for a supernova or Wolf-Rayet (WR) star to lower masses. We also find that the pre-WR mass loss determines the shape of our maps. We find that different mass-loss rates lead to quite different results. We find that the rise in luminosity at second dredge-up places quite tight constraints on the masses of some progenitors and in particular the progenitor of supernova 2003gd.},
author = {Eldridge, J. J. and Tout, C. A.},
doi = {10.1111/j.1365-2966.2004.08041.x},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {stars: Wolf-Rayet,stars: evolution,supernovae: general,supernovae: individual: SN 2003gd},
month = {sep},
number = {1},
pages = {87--97},
title = {{The progenitors of core-collapse supernovae}},
url = {http://adsabs.harvard.edu/abs/2004MNRAS.353...87E},
volume = {353},
year = {2004},
}
@article{2009ApJ...700.1680T,
author = {Tanaka, Masaomi and Yamanaka, Masayuki and Maeda, Keiichi and Kawabata, Koji S and Hattori, Takashi and Minezaki, Takeo and Valenti, Stefano and della Valle, Massimo and Sahu, D.\~{}K. and Anupama, G.\~{}C. and Tominaga, Nozomu and Nomoto, Ken'ichi and Mazzali, Paolo A and Pian, Elena},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/The Astrophysical Journal/2009 Tanaka-2.pdf:pdf},
journal = {The Astrophysical Journal},
month = {aug},
number = {2},
pages = {1680--1685},
title = {{Nebular Phase Observations of the Type Ib Supernova 2008D/X-ray Transient 080109: Side-viewed Bipolar Explosion}},
volume = {700},
year = {2009},
}
@article{Branch2005,
archiveprefix = {arXiv},
arxivid = {arXiv:astro-ph/0503165v1},
author = {Branch, David and Baron, E and Hall, Nicholas and Melakayil, Mercy and Parrent, Jerod},
doi = {10.1086/430135},
eprint = {0503165v1},
file = {:Users/svalenti/Documents/Mendeley Desktop/2005/Publications of the Astronomical Society of the Pacific/2005 Branch.pdf:pdf},
issn = {0004-6280},
journal = {Publications of the Astronomical Society of the Pacific},
month = {jun},
number = {832},
pages = {545--552},
primaryclass = {arXiv:astro-ph},
title = {{Comparative Direct Analysis of Type Ia Supernova Spectra. I. SN 1994D}},
url = {http://www.jstor.org/stable/10.1086/430135},
volume = {117},
year = {2005},
}
@article{Kromer2012b,
abstract = {2002cx-like supernovae are a sub-class of sub-luminous Type Ia supernovae (SNe). Their light curves and spectra are characterized by distinct features that indicate strong mixing of the explosion ejecta. Pure turbulent deflagrations have been shown to produce such mixed ejecta. Here, we present hydrodynamics, nucleosynthesis and radiative-transfer calculations for a 3D full-star deflagration of a Chandrasekhar-mass white dwarf. Our model is able to reproduce the characteristic observational features of SN 2005hk (a prototypical 2002cx-like supernova), not only in the optical, but also in the near-infrared. For that purpose we present, for the first time, five near-infrared spectra of SN 2005hk from -0.2 to 26.6 d with respect to B-band maximum. Since our model burns only small parts of the initial white dwarf, it fails to completely unbind the white dwarf and leaves behind a bound remnant of ˜1.03 M⊙ - consisting mainly of unburned carbon and oxygen, but also enriched by some amount of intermediate-mass and iron-group elements from the explosion products that fall back on the remnant. We discuss possibilities for detecting this bound remnant and how it might influence the late-time observables of 2002cx-like SNe.},
author = {Kromer, M. and Fink, M. and Stanishev, V. and Taubenberger, S. and Ciaraldi-Schoolman, F. and Pakmor, R. and Ropke, F. K. and Ruiter, A. J. and Seitenzahl, I. R. and Sim, S. A. and Blanc, G. and Elias-Rosa, N. and Hillebrandt, W.},
doi = {10.1093/mnras/sts498},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/Monthly Notices of the Royal Astronomical Society/MNRAS-2013-Kromer-2287-97.pdf:pdf},
issn = {0035-8711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {hydrodynamics,methods: numerical,radiative transfer,supernovae: individual: SN 2005hk,techniques: spectroscopic},
month = {dec},
number = {3},
pages = {2287--2297},
title = {{3D deflagration simulations leaving bound remnants: a model for 2002cx-like Type Ia supernovae}},
url = {http://adsabs.harvard.edu/abs/2013MNRAS.429.2287K},
volume = {429},
year = {2012},
}
@article{2012MNRAS.425.1917S,
author = {Silverman, Jeffrey M and Filippenko, Alexei V},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {sep},
number = {3},
pages = {1917--1933},
title = {{Berkeley Supernova Ia Program - IV. Carbon detection in early-time optical spectra of Type Ia supernovae}},
volume = {425},
year = {2012},
}
@article{2010ApJ...717L..83M,
author = {Moriya, Takashi and Tominaga, Nozomu and Tanaka, Masaomi and Maeda, Keiichi and Nomoto, Ken'ichi},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/The Astrophysical Journal Letters/2010 Moriya-1.pdf:pdf},
journal = {The Astrophysical Journal Letters},
month = {jul},
number = {2},
pages = {L83--------L86},
title = {{A Core-collapse Supernova Model for the Extremely Luminous Type Ic Supernova 2007bi: An Alternative to the Pair-instability Supernova Model}},
volume = {717},
year = {2010},
}
@article{Kromer2012,
abstract = {2002cx-like supernovae are a sub-class of sub-luminous Type Ia supernovae. Their light curves and spectra are characterized by distinct features that indicate strong mixing of the explosion ejecta. Pure turbulent deflagrations have been shown to produce such mixed ejecta. Here, we present hydrodynamics, nucleosynthesis and radiative transfer calculations for a 3D full-star deflagration of a Chandrasekhar-mass white dwarf. Our model is able to reproduce the characteristic observational features of SN 2005hk (a proto-typical 2002cx-like supernova), not only in the optical, but also in the near-infrared. For that purpose we present, for the first time, five near-infrared spectra of SN 2005hk from -0.2 to 26.6 days with respect to B-band maximum. Since our model burns only small parts of the initial white dwarf, it fails to completely unbind the white dwarf and leaves behind a bound remnant of \~{}1.03 solar masses -- consisting mainly of unburned carbon and oxygen, but also enriched by some amount of intermediate-mass and iron-group elements from the explosion products that fall back on the remnant. We discuss possibilities for detecting this bound remnant and how it might influence the late-time observables of 2002cx-like SNe.},
archiveprefix = {arXiv},
arxivid = {1210.5243},
author = {Kromer, M and Fink, M and Stanishev, V and Taubenberger, S and Ciaraldi-Schoolman, F. and Pakmor, R and Ropke, F. K. and Ruiter, A J and Seitenzahl, I. R. and Sim, S A and Blanc, G and Elias-Rosa, N. and Hillebrandt, W},
doi = {10.1093/mnras/sts498},
eprint = {1210.5243},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/Monthly Notices of the Royal Astronomical Society/arXiv 2012 Kromer.pdf:pdf},
issn = {0035-8711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {hydrodynamics,individual,meth-,numerical,ods,radiative transfer,sn 2005hk,spectroscopic,supernovae,techniques},
month = {dec},
number = {3},
pages = {2287--2297},
title = {{3D deflagration simulations leaving bound remnants: a model for 2002cx-like Type Ia supernovae}},
url = {http://arxiv.org/abs/1210.5243 http://mnras.oxfordjournals.org/cgi/doi/10.1093/mnras/sts498},
volume = {429},
year = {2012},
}
@article{Otsuka2012,
abstract = {We present BVRIJHK-band photometry of six core-collapse supernovae, SNe 1999bw, 2002hh, 2003gd, 2004et, 2005cs, and 2006bc, measured at late epochs (\>2 yr) based on the Hubble Space Telescope (HST), and the Gemini North, and WIYN telescopes. We also show the JHK light curves of supernova impostor SN 2008S up to day 575 because it was serendipitously in our SN 2002hh field of view. Of our 43 HST observations in total, 36 observations are successful in detecting the light from the SNe alone and measuring magnitudes of all the targets. HST observations show a resolved scattered light echo around SN 2003gd at day 1520 and around SN 2002hh at day 1717. Our Gemini and WIYN observations detected SNe 2002hh and 2004et as well. Combining our data with previously published data, we show VRIJHK-band light curves and estimate decline magnitude rates at each band in four different phases. Our prior work on these light curves and other data indicate that dust is forming in our targets from days \~{}300 to 400, supporting SN dust formation theory. In this paper we focus on other physical properties derived from late-time light curves. We estimate 56Ni masses for our targets (0.5-14 × 10-2 M ⊙) from the bolometric light curve of each of days \~{}150-300 using SN 1987A as a standard (7.5 × 10-2 M ⊙). The flattening or sometimes increasing fluxes in the late-time light curves of SNe 2002hh, 2003gd, 2004et, and 2006bc indicate the presence of light echoes. We estimate the circumstellar hydrogen density of the material causing the light echo and find that SN 2002hh is surrounded by relatively dense materials (n(H) \>400 cm-3) and SNe 2003gd and 2004et have densities more typical of the interstellar medium (\~{}1 cm-3). We analyze the sample as a whole in the context of physical properties derived in prior work. The 56Ni mass appears well correlated with progenitor mass with a slope of 0.31 × 10-2, supporting the previous work by Maeda et al., who focus on more massive Type II SNe. The dust mass does not appear to be correlated with progenitor mass.},
author = {Otsuka, Masaaki and Meixner, Margaret and Panagia, Nino and Fabbri, Joanna and Barlow, Michael J. and Clayton, Geoffrey C. and Gallagher, Joseph S. and Sugerman, Ben E. K. and Wesson, Roger and Andrews, Jennifer E. and Ercolano, Barbara and Welch, Douglas},
doi = {10.1088/0004-637X/744/1/26},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {dust,extinction,supernovae: individual: SN1999bw SN2002hh SN 2003g},
month = {jan},
number = {1},
pages = {26},
title = {{LATE-TIME LIGHT CURVES OF TYPE II SUPERNOVAE: PHYSICAL PROPERTIES OF SUPERNOVAE AND THEIR ENVIRONMENT}},
url = {http://adsabs.harvard.edu/abs/2012ApJ...744...26O},
volume = {744},
year = {2012},
}
@article{Taubenberger2011,
abstract = {Extensive optical and near-infrared (NIR) observations of the Type IIb supernova (SN IIb) 2008ax are presented, covering the first year after the explosion. The light curve is mostly similar in shape to that of the prototypical SN IIb 1993J, but shows a slightly faster decline rate at late phases and lacks the prominent narrow early-time peak of SN 1993J. From the bolometric light curve and ejecta expansion velocities, we estimate that about 0.07-0.15 M⊙ of 56Ni was produced during the explosion and that the total ejecta mass was between 2 and 5 M⊙, with a kinetic energy of at least 1051 erg. The spectral evolution of SN 2008ax is similar to that of SN Ib/IIb 2007Y, exhibiting high-velocity Ca II features at early phases and signs of ejecta-wind interaction from H$\alpha$ observations at late times. NIR spectra show strong He I lines similar to SN Ib 1999ex and a large number of emission features at late times. Particularly interesting are the strong, double-peaked He I lines in late NIR spectra, which - together with the double-peaked [O I] emission in late optical spectra - provide clues for the asymmetry and large-scale Ni mixing in the ejecta. a Phase in days with respect to the explosion date (JD =245 4528.80 ± 0.15). B-band maximum light occurred on day 18.3. b Average seeing in arcsec over all filter bands. c CAFOS = Calar Alto 2.2m Telescope + CAFOS; DOLORES = 3.58m Telescopio Nazionale Galileo + DOLORES; AFOSC = Asiago 1.82m Copernico Telescope + AFOSC.},
author = {Taubenberger, S. and Navasardyan, H. and Maurer, J. I. and Zampieri, L. and Chugai, N. N. and Benetti, S. and Agnoletto, I. and Bufano, F. and Elias-Rosa, N. and Turatto, M. and Patat, F. and Cappellaro, E. and Mazzali, P. A. and Iijima, T. and Valenti, S. and Harutyunyan, A. and Claudi, R. and Dolci, M.},
doi = {10.1111/j.1365-2966.2011.18287.x},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {galaxies: individual: NGC 4490,supernovae: general,supernovae: individual: SN 1993J,supernovae: individual: SN 1999ex,supernovae: individual: SN 2007Y,supernovae: individual: SN 2008ax},
month = {may},
number = {3},
pages = {2140--2156},
title = {{The He-rich stripped-envelope core-collapse supernova 2008ax★}},
url = {http://adsabs.harvard.edu/abs/2011arXiv1101.1824T},
volume = {413},
year = {2011},
}
@article{Folatelli2006,
author = {Folatelli, Gaston and Contreras, Carlos and Phillips, M. M. and Woosley, S. E. and Blinnikov, Sergei and Morrell, Nidia and Suntzeff, Nicholas B. and Lee, Brian L. and Hamuy, Mario and Gonzalez, Sergio and Krzeminski, Wojtek and Roth, Miguel and Li, Weidong and Filippenko, Alexei V. and Foley, Ryan J. and Freedman, W. L. and Madore, Barry F. and Persson, S. E. and Murphy, David and Boissier, Samuel and Galaz, Gaspar and Gonzalez, Luis and McCarthy, P. J. and McWilliam, Andrew and Pych, Wojtek},
doi = {10.1086/500531},
file = {:Users/svalenti/Documents/Mendeley Desktop/2006/The Astrophysical Journal/2006 Folatelli.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {apr},
number = {2},
pages = {1039--1050},
title = {{SN 2005bf: A Possible Transition Event between Type Ib/c Supernovae and Gamma‐Ray Bursts}},
url = {http://iopscience.iop.org/0004-637X/641/2/1039 http://stacks.iop.org/0004-637X/641/i=2/a=1039},
volume = {641},
year = {2006},
}
@article{2011MNRAS.413.2140T,
author = {Taubenberger, S and Navasardyan, H and Maurer, J I and Zampieri, L and Chugai, N N and Benetti, S and Agnoletto, I and Bufano, F and Elias-Rosa, N and Turatto, M and Patat, F and Cappellaro, E and Mazzali, P.\~{}A. and Iijima, T and Valenti, S and Harutyunyan, A and Claudi, R and Dolci, M},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2011 Taubenberger.pdf:pdf},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {may},
number = {3},
pages = {2140--2156},
title = {{The He-rich stripped-envelope core-collapse supernova 2008ax}},
volume = {413},
year = {2011},
}
@article{2004MNRAS.347...74P,
author = {Pastorello, A and Zampieri, L and Turatto, M and Cappellaro, E and Meikle, W.\~{}P.\~{}S. and Benetti, S and Branch, D and Baron, E and Patat, F and Armstrong, M and Altavilla, G and Salvo, M and Riello, M},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {jan},
number = {1},
pages = {74--94},
title = {{Low-luminosity Type II supernovae: spectroscopic and photometric evolution}},
volume = {347},
year = {2004},
}
@article{2009svlt.conf..225H,
author = {Hook, Isobel},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/Science with the VLT in the ELT Era/2009 Hook.pdf:pdf},
journal = {Science with the VLT in the ELT Era},
pages = {225},
title = {{The Science Case for the European ELT}},
year = {2009},
}
@article{2010ApJ...715..767S,
author = {Shen, Ken J and Kasen, Dan and Weinberg, Nevin N and Bildsten, Lars and Scannapieco, Evan},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/The Astrophysical Journal/2010 Shen.pdf:pdf},
journal = {The Astrophysical Journal},
month = {jun},
number = {2},
pages = {767--774},
title = {{Thermonuclear .Ia Supernovae from Helium Shell Detonations: Explosion Models and Observables}},
volume = {715},
year = {2010},
}
@article{Dessart:2012tv,
annote = {22 pages, 14 figures, accepted to MNRAS},
author = {Dessart, Luc and Hillier, D John and Li, Chengdong and Woosley, Stan},
doi = {10.1111/j.1365-2966.2012.21374.x},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/Monthly Notices of the Royal Astronomical Society/arXiv 2012 Dessart.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {aug},
number = {3},
pages = {2139--2159},
title = {{On the nature of supernovae Ib and Ic}},
url = {http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2012.21374.x},
volume = {424},
year = {2012},
}
@article{2007MNRAS.377.1531P,
author = {Pastorello, A and Mazzali, P.\~{}A. and Pignata, G and Benetti, S and Cappellaro, E and Filippenko, A V and Li, W and Meikle, W.\~{}P.\~{}S. and Arkharov, A.\~{}A. and Blanc, G and Bufano, F and Derekas, A and Dolci, M and Elias-Rosa, N and Foley, R J and Ganeshalingam, M and Harutyunyan, A and Kiss, L L and Kotak, R and Larionov, V.\~{}M. and Lucey, J R and Napoleone, N and Navasardyan, H and Patat, F and Rich, J and Ryder, S D and Salvo, M and Schmidt, B P and Stanishev, V and Sz\'{e}kely, P and Taubenberger, S and Temporin, S and Turatto, M and Hillebrandt, W},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {jun},
number = {4},
pages = {1531--1552},
title = {{ESC and KAIT observations of the transitional Type Ia SN 2004eo}},
volume = {377},
year = {2007},
}
@article{2010CBET.2339....1D,
author = {Drake, A J and Djorgovski, S G and Mahabal, A and Grahamm, M J and Williams, R and Prieto, J.\~{}L. and Catelan, M and Beshore, E C and Larson, S M and Christensen, E},
journal = {Central Bureau Electronic Telegrams},
month = {jun},
pages = {1},
title = {{Supernovae 2010en, 2010eo, 2010ep, 2010eq, 2010er, 2010es, and 2010et}},
volume = {2339},
year = {2010},
}
@article{1996AJ....111..327R,
author = {Richmond, M.\~{}W. and van Dyk, S D and Ho, W and Peng, C Y and Paik, Y and Treffers, R R and Filippenko, A V and Bustamante-Donas, J and Moeller, M and Pawellek, C and Tartara, H and Spence, M},
journal = {Astronomical Journal v.111},
month = {jan},
pages = {327},
title = {{UBVRI Photometry of the Type IC SN 1994I in M51}},
volume = {111},
year = {1996},
}
@article{2010MNRAS.408..947M,
author = {Maurer, I and Mazzali, P.\~{}A.},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2010 Maurer.pdf:pdf},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {oct},
number = {2},
pages = {947--960},
title = {{Oxygen recombination in the nebular phase of supernovae 1998bw and 2002ap}},
volume = {408},
year = {2010},
}
@article{2008MNRAS.384.1109E,
author = {Eldridge, John J and Izzard, Robert G and Tout, Christopher A},
file = {:Users/svalenti/Documents/Mendeley Desktop/2008/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2008 Eldridge.pdf:pdf},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {mar},
number = {3},
pages = {1109--1118},
title = {{The effect of massive binaries on stellar populations and supernova progenitors}},
volume = {384},
year = {2008},
}
@article{2009A&A...508..371H,
abstract = {We present photometric and spectroscopic observations at optical and near-infrared wavelengths of the nearby type Ic SN 2007gr. These represent the most extensive data-set to date of any supernova of this sub-type, with frequent coverage from shortly after discovery to more than one year post-explosion. We deduce a rise time to B-band maximum of 11.5 $\backslash$pm 2.7 days. We find a peak B-band magnitude of M\_B=-16.8, and light curves which are remarkably similar to the so-called 'hypernova' SN 2002ap. In contrast, the spectra of SNe 2007gr and 2002ap show marked differences, not least in their respective expansion velocities. We attribute these differences primarily to the density profiles of their progenitor stars at the time of explosion i.e. a more compact star for SN 2007gr compared to SN 2002ap. From the quasi-bolometric light curve of SN 2007gr, we estimate that 0.076 \$\backslash pm\$ 0.010 Msun of 56Ni was produced in the explosion. Our near-infrared (IR) spectra clearly show the onset and disappearance of the first overtone of carbon monoxide (CO) between \~{}70 to 175 days relative to B-band maximum. The detection of the CO molecule implies that ionised He was not microscopically mixed within the carbon/oxygen layers. From the optical spectra, near-IR light curves, and colour evolution, we find no evidence for dust condensation in the ejecta out to about 400 days. Given the combination of unprecedented temporal coverage, and high signal-to-noise data, we suggest that SN 2007gr could be used as a template object for supernovae of this sub-class.},
archiveprefix = {arXiv},
arxivid = {0909.3780},
author = {Hunter, Deborah J and Valenti, Stefano and Kotak, Rubina and Meikle, W. P. S. and Taubenberger, Stefan and Pastorello, Andrea and Benetti, Stefano and Stanishev, Vallery and Smartt, Steven J. and Trundle, Carrie and Arkharov, Arkady A. and Bufano, F. and Cappellaro, Enrico and {Di Carlo}, Elisa and Dolci, Mauro and Elias-Rosa, Nancy and Frandsen, Soeren and Fynbo, Johan U. and Hopp, Ulrich and Larionov, Valeri M. and Laursen, Peter and Mazzali, Paolo and Navasardyan, Hripsime and Ries, Christoph and Riffeser, Arno and Rizzi, Luca and Tsvetkov, Dmitrii Y. and Turatto, Massimo and Wilke, Silona},
doi = {10.1051/0004-6361/200912896},
eprint = {0909.3780},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/Astronomy and Astrophysics/2009 Hunter.pdf:pdf},
issn = {0004-6361},
journal = {Astronomy and Astrophysics},
keywords = {general,individual,sn 2002ap,sn 2007gr,supernovae},
month = {dec},
number = {1},
pages = {371--389},
title = {{Extensive optical and near-infrared observations of the nearby, narrow-lined type Ic SN 2007gr: days 5 to 415}},
url = {http://arxiv.org/abs/0909.3780 http://www.aanda.org/10.1051/0004-6361/200912896},
volume = {508},
year = {2009},
}
@article{2012MNRAS.422.1178I,
abstract = {We compare and analyse a time series of spectral observations obtained during the first 30 d of evolution of SN 2007od with the non-local thermodynamic equilibrium code PHOENIX. Despite some spectroscopic particularities in the Balmer features, this supernova appears to be a normal Type II, and the fits proposed are generally in good agreement with the observations. As a starting point, we have carried out an analysis with the parametrized synthetic spectrum code SYNOW to confirm line identifications and to highlight differences between the results of the two codes. The analysis computed using PHOENIX suggests the presence of a high-velocity feature in H$\beta$ and an H$\alpha$ profile reproduced with a density profile steeper than that of the other elements. We also show a detailed analysis of the ions velocities of the six synthetic spectra. The distance is estimated for each epoch with the spectral-fitting expanding atmosphere method. Consistent results are found using all the spectra which give the explosion date of JD 245 4403 (2007 October 29) and a distance modulus $\mu$= 32.2 ± 0.3.},
annote = {From Duplicate 1 ( Quantitative photospheric spectral analysis of the Type IIP supernova 2007od - Inserra, C; Baron, E; Turatto, M )},
author = {Inserra, C. and Baron, E. and Turatto, M.},
doi = {10.1111/j.1365-2966.2012.20691.x},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {galaxies: distances and redshifts,line: identification,supernovae: general,supernovae: individual: SN 2007od},
month = {may},
number = {2},
pages = {1178--1185},
title = {{Quantitative photospheric spectral analysis of the Type IIP supernova 2007od}},
url = {http://adsabs.harvard.edu/abs/2012MNRAS.422.1178I},
volume = {422},
year = {2012},
}
@article{2011MNRAS.413.2583S,
author = {Sahu, D.\~{}K. and Gurugubelli, U.\~{}K. and Anupama, G.\~{}C. and Nomoto, K},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {jun},
number = {4},
pages = {2583--2594},
title = {{Optical studies of SN 2009jf: a Type Ib supernova with an extremely slow decline and aspherical signature}},
volume = {413},
year = {2011},
}
@article{2009MNRAS.397..677T,
author = {Taubenberger, S. and Valenti, S. and Benetti, S. and Cappellaro, E. and {Della Valle}, M. and Elias-Rosa, N. and Hachinger, S. and Hillebrandt, W. and Maeda, K. and Mazzali, P.\~{}A. a. and Pastorello, a. and Patat, F. and Sim, S.\~{}A. a. and Turatto, M.},
doi = {10.1111/j.1365-2966.2009.15003.x},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2009 Taubenberger.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {1 i n t,cc-sn,core-collapse supernova,ejecta has been scrutinized,for about 10 yr,general,line,profiles,ro d u c,since the as-,spectroscopic,supernovae,t i o n,techniques,the geometry of stripped-envelope},
month = {aug},
number = {2},
pages = {677--694},
title = {{Nebular emission-line profiles of Type Ib/c supernovae - probing the ejecta asphericity}},
url = {http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2009.15003.x},
volume = {397},
year = {2009},
}
@article{Patat2011a,
abstract = {Aims: The present study was conducted to determine the optical extinction curve for Cerro Paranal under typical clear-sky observing conditions, with the purpose of providing the community with a function to be used to correct the observed spectra, with an accuracy of 0.01 mag airmass-1. Additionally, this work was meant to analyze the variability of the various components, to derive the main atmospheric parameters, and to set a term of reference for future studies, especially in view of the construction of the Extremely Large Telescope on the nearby Cerro Armazones. Methods: The extinction curve of Paranal was obtained through low-resolution spectroscopy of 8 spectrophotometric standard stars observed with FORS1 mounted at the 8.2 m Very Large Telescope, covering a spectral range 3300-8000 \AA. A total of 600 spectra were collected on more than 40 nights distributed over six months, from October 2008 to March 2009. The average extinction curve was derived using a global fit algorithm, which allowed us to simultaneously combine all the available data. The main atmospheric parameters were retrieved using the LBLRTM radiative transfer code, which was also utilised to study the impact of variability of the main molecular bands of O2, O3, and H2O, and to estimate their column densities. Results: In general, the extinction curve of Paranal appears to conform to those derived for other astronomical sites in the Atacama desert, like La Silla and Cerro Tololo. However, a systematic deficit with respect to the extinction curve derived for Cerro Tololo before the El Chich\'{o}n eruption is detected below 4000 \AA. We attribute this downturn to a non standard aerosol composition, probably revealing the presence of volcanic pollutants above the Atacama desert. An analysis of all spectroscopic extinction curves obtained since 1974 shows that the aerosol composition has been evolving during the last 35 years. The persistence of traces of non meteorologic haze suggests the effect of volcanic eruptions, like those of El Chich\'{o}n and Pinatubo, lasts several decades. The usage of the standard CTIO and La Silla extinction curves implemented in IRAF and MIDAS produce systematic over/under-estimates of the absolute flux. Based on observations made with ESO Telescopes at Paranal Observatory.},
author = {Patat, F. and Moehler, S. and O’Brien, K. and Pompei, E. and Bensby, T. and Carraro, G. and {de Ugarte Postigo}, A. and Fox, A. and Gavignaud, I. and James, G. and Korhonen, H. and Ledoux, C. and Randall, S. and Sana, H. and Smoker, J. and Stefl, S. and Szeifert, T.},
doi = {10.1051/0004-6361/201015537},
issn = {0004-6361},
journal = {Astronomy \& Astrophysics},
keywords = {Earth,atmospheric effects,site testing,techniques: spectroscopic},
month = {jan},
pages = {A91},
title = {{Optical atmospheric extinction over Cerro Paranal}},
url = {http://adsabs.harvard.edu/abs/2011A\&A...527A..91P},
volume = {527},
year = {2011},
}
@article{atel5237,
author = {Shappee, B. J. and Kochanek, C. S. and Stanek and Basu and Holoien, T. W-S. and Jencson, J. and Beacom, J. F. and Prieto, J. L. and Szczygiel, D. and Pojmanski, G. and Dubberley, M. and Elphick, M. and Foale, S. and Hawkins, E. and Mullens, D. and Rosing, W. and Ross, R. and Walker, Z. and Brimacombe, J.},
journal = {The Astronomer's Telegram},
title = {{Pre-explosion ASAS-SN V-Band Upper-Limits on SN 2013ej (PSN J01364816+1545310)}},
year = {2013},
}
@article{2012PASP..124..668Y,
abstract = {We have entered an era of massive data sets in astronomy. In particular, the number of supernova (SN) discoveries and classifications has substantially increased over the years from few tens to thousands per year. It is no longer the case that observations of a few prototypical events encapsulate most spectroscopic information about SNe, motivating the development of modern tools to collect, archive, organize and distribute spectra in general, and SN spectra in particular. For this reason we have developed the Weizmann Interactive Supernova data REPository - WISeREP - an SQL-based database (DB) with an interactive web-based graphical interface. The system serves as an archive of high quality SN spectra, including both historical (legacy) data as well as data that is accumulated by ongoing modern programs. The archive provides information about objects, their spectra, and related meta-data. Utilizing interactive plots, we provide a graphical interface to visualize data, perform line identification of the major relevant species, determine object redshifts, classify SNe and measure expansion velocities. Guest users may view and download spectra or other data that have been placed in the public domain. Registered users may also view and download data that are proprietary to specific programs with which they are associated. The DB currently holds >8000 spectra, of which >5000 are public; the latter include published spectra from the Palomar Transient Factory, all of the SUSPECT archive, the Caltech-Core-Collapse Program, the CfA SN spectra archive and published spectra from the UC Berkeley SNDB repository. It offers an efficient and convenient way to archive data and share it with colleagues, and we expect that data stored in this way will be easy to access, increasing its visibility, usefulness and scientific impact.},
archiveprefix = {arXiv},
arxivid = {1204.1891},
author = {Yaron, Ofer and Gal-Yam, Avishay},
doi = {10.1086/666656},
eprint = {1204.1891},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/Publications of the Astronomical Society of the Pacific/2012 Yaron.pdf:pdf},
issn = {00046280},
journal = {Publications of the Astronomical Society of the Pacific},
month = {jul},
number = {917},
pages = {668--681},
title = {{WISeREP—An Interactive Supernova Data Repository}},
url = {http://arxiv.org/abs/1204.1891 http://www.jstor.org/stable/info/10.1086/666656},
volume = {124},
year = {2012},
}
@article{2012arXiv1208.5949G,
annote = {11 pages, 6 figures, accepted for publication in MNRAS},
author = {Gall, E E E and Taubenberger, S and Kromer, M and Sim, S.\~{}A. and Benetti, S and Blanc, G and Elias-Rosa, N and Hillebrandt, W},
journal = {arXiv.org},
month = {aug},
pages = {5949},
title = {{Interpreting the near-infrared spectra of the 'golden standard' Type Ia supernova 2005cf}},
volume = {1208},
year = {2012},
}
@article{Andrews2011,
abstract = {SN 2007it is a bright, Type IIP supernova which shows indications of both pre-existing and newly formed dust. The visible photometry shows a bright late-time luminosity, powered by the 0.09 M sun of 56Ni present in the ejecta. There is also a sudden drop in optical brightness after day 339, and a corresponding brightening in the IR due to new dust forming in the ejecta. CO and SiO emission, generally thought to be precursors to dust formation, may have been detected in the mid-IR photometry of SN 2007it. The optical spectra show stronger than average [O I] emission lines and weaker than average [Ca II] lines, which may indicate a 16-27 M sun progenitor, on the higher end of expected Type IIP masses. Multi-component [O I] lines are also seen in the optical spectra, most likely caused by an asymmetric blob or a torus of oxygen core material being ejected during the SN explosion. Interaction with circumstellar material prior to day 540 may have created a cool dense shell between the forward and reverse shocks where new dust is condensing. At late times there is also a flattening of the visible light curve as the ejecta luminosity fades and a surrounding light echo becomes visible. Radiative transfer models of SN 2007it spectral energy distributions indicate that up to 10-4 M sun of new dust has formed in the ejecta, which is consistent with the amount of dust formed in other core-collapse supernovae.},
author = {Andrews, J. E. and Sugerman, B. E. K. and Clayton, Geoffrey C. and Gallagher, J. S. and Barlow, M. J. and Clem, J. and Ercolano, B. and Fabbri, J. and Meixner, M. and Otsuka, M. and Welch, D. L. and Wesson, R.},
doi = {10.1088/0004-637X/731/1/47},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {circumstellar matter,dust,extinction,supernovae: general,supernovae: individual: SN 2007it},
month = {apr},
number = {1},
pages = {47},
title = {{PHOTOMETRIC AND SPECTROSCOPIC EVOLUTION OF THE IIP SN 2007it TO DAY 944}},
url = {http://adsabs.harvard.edu/abs/2011ApJ...731...47A},
volume = {731},
year = {2011},
}
@article{Rabinak2011,
abstract = {We derive a simple approximate model describing the early, hours to days, UV/optical (UV/O) supernova emission, which is produced by the expansion of the outer lsim10-2 M sun part of the shock-heated envelope, and precedes optical emission driven by radioactive decay. Our model includes an approximate description of the time dependence of the opacity (mainly due to recombination), and of the deviation of the emitted spectrum from a blackbody spectrum. We show that the characteristics of the early UV/O emission constrain the radius of the progenitor star, R *, its envelope composition, and the ratio of the ejecta energy to its mass, E/M. For He envelopes, neglecting the effect of recombination may lead to an overestimate of R * by more than an order of magnitude. We also show that the relative extinction at different wavelengths (A $\lambda$ - AV ) may be inferred from the light curves at these wavelengths, removing the uncertainty in the estimate of R * due to reddening (but not the uncertainty in E/M due to uncertainty in absolute extinction). The early UV/O observations of the types Ib SN 2008D and IIp SNLS-04D2dc are consistent with our model predictions. For SN 2008D, we find R * ≈ 1011 cm, and an indication that the He envelope contains a significant C/O fraction.},
author = {Rabinak, Itay and Waxman, Eli},
doi = {10.1088/0004-637X/728/1/63},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/The Astrophysical Journal/apj\_728\_1\_63.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {radiative transfer,shock waves,stars: evolution,supernovae: general,supernovae: individual: SN 2008D},
month = {feb},
number = {1},
pages = {63},
title = {{THE EARLY UV/OPTICAL EMISSION FROM CORE-COLLAPSE SUPERNOVAE}},
url = {http://adsabs.harvard.edu.proxy.library.ucsb.edu:2048/abs/2011ApJ...728...63R},
volume = {728},
year = {2011},
}
@article{EldridgeJohnJ.2013,
abstract = {[ABRIDGED] We present an extensive search for the progenitors of type Ibc supernovae in all available pre-discovery imaging since 1998. To date there have been 12 type Ibc supernovae with either deep ground-based imaging or Hubble Space Telescope archival imaging of their explosion sites. Our analysis shows there is no detection of any progenitor in these images, with the deepest limits probing absolute magnitudes of between -4 and -5 in broad-band B, V and R. We compare the magnitude limits with the observed Wolf-Rayet population in the Large Magellanic Cloud. There is only a 15 per cent probability that this is actually the progenitor population and that we have failed to detect a Wolf-Rayet progenitor by chance selection. If SN Ibc progenitors are drawn from such populations then either Wolf-Rayet stars evolve significantly in the last stages of their lives, or we have underestimated circumstellar dust and extinction towards the progenitors. We review the relative rates of Ibc SNe, finding agreement with previous work that they occur too frequently to originate only from progenitors with initial masses \>25$\backslash$msun. Hence we propose that a Wolf-Rayet origin for the bulk of the normal Ibc population is unlikely. We present results from binary stellar evolution calculations that show that stars less than approximately 20$\backslash$msun, in interacting binaries can fit all of these observational constraints. These stars lose their hydrogen envelopes through either Roche-lobe overflow or common envelope evolution and end their lives as low mass helium stars. We show that such helium stars in model binaries retain a low mass hydrogen envelope until after the end of core helium burning and lose the last of the hydrogen approximately 10\^{}4 years before core-collapse. Hence it is not surprising that they have been difficult to identify, but some viable Ibc progenitor systems exist.},
author = {{Eldridge, John J.} and {Fraser, Morgan} and {Smartt, Stephen J.} and {Maund, Justyn R.} and {Crockett, R. Mark}},
journal = {eprint arXiv:1301.1975},
keywords = {Astrophysics - Cosmology and Extragalactic Astroph,Astrophysics - Solar and Stellar Astrophysics},
title = {{The death of massive stars - II. Observational constraints on the progenitors of type Ibc supernovae}},
url = {http://adsabs.harvard.edu/abs/2013arXiv1301.1975E},
year = {2013},
}
@article{1998ApJ...500..525S,
author = {Schlegel, David J and Finkbeiner, Douglas P and Davis, Marc},
doi = {10.1086/305772},
file = {:Users/svalenti/Documents/Mendeley Desktop/1998/The Astrophysical Journal/1998 Schlegel.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {jun},
number = {2},
pages = {525--553},
title = {{Maps of Dust Infrared Emission for Use in Estimation of Reddening and Cosmic Microwave Background Radiation Foregrounds}},
url = {http://stacks.iop.org/0004-637X/500/i=2/a=525},
volume = {500},
year = {1998},
}
@article{2005ASPC..342..268S,
author = {Stanishev, V and Collaboration, European Supernova},
journal = {1604-2004: Supernovae as Cosmological Lighthouses},
month = {dec},
pages = {268},
title = {{Spectroscopy and Photometry of Type Ia Supernova 2003du: Results of the ESC/RTN Campaign}},
volume = {342},
year = {2005},
}
@article{2008A&A...488..383H,
author = {Harutyunyan, A H and Pfahler, P and Pastorello, A and Taubenberger, S and Turatto, M and Cappellaro, E and Benetti, S and Elias-Rosa, N. and Navasardyan, H and Valenti, S and Stanishev, V and Patat, F and Riello, M and Pignata, G and Hillebrandt, W},
doi = {10.1051/0004-6361:20078859},
file = {:Users/svalenti/Documents/Mendeley Desktop/2008/Astronomy and Astrophysics/2008 Harutyunyan.pdf:pdf},
issn = {0004-6361},
journal = {Astronomy and Astrophysics},
keywords = {data analysis,general,methods,supernovae},
month = {sep},
number = {1},
pages = {383--399},
title = {{ESC supernova spectroscopy of non-ESC targets}},
url = {http://www.aanda.org/10.1051/0004-6361:20078859},
volume = {488},
year = {2008},
}
@article{2010MNRAS.408.2115M,
author = {Mannucci, F and Cresci, G and Maiolino, R and Marconi, A and Gnerucci, A},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2010 Mannucci.pdf:pdf},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {nov},
number = {4},
pages = {2115--2127},
title = {{A fundamental relation between mass, star formation rate and metallicity in local and high-redshift galaxies}},
volume = {408},
year = {2010},
}
@article{Baron2003,
author = {Baron, E and Nugent, Peter E and Branch, David and Hauschildt, Peter H and Turatto, M and Cappellaro, E.},
doi = {10.1086/367888},
file = {:Users/svalenti/Documents/Mendeley Desktop/2003/The Astrophysical Journal/2003 Baron.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {apr},
number = {2},
pages = {1199--1210},
title = {{Determination of Primordial Metallicity and Mixing in the Type II‐P Supernova 1993W}},
url = {http://stacks.iop.org/0004-637X/586/i=2/a=1199},
volume = {586},
year = {2003},
}
@article{Yoon2012,
abstract = {The progenitors of many Type II supernovae have been observationally identified but the search for Type Ibc supernova (SN Ibc) progenitors has thus far been unsuccessful, despite the expectation that they are luminous Wolf-Rayet (WR) stars. We investigate how the evolution of massive helium stars affects their visual appearances, and discuss the implications for the detectability of SN Ibc progenitors. Massive WR stars that rapidly lose their helium envelopes through stellar-wind mass-loss end their lives when their effective temperatures -- related to their hydrostatic surfaces -- exceed about 150kK.At their pre-supernova stage, their surface properties resemble those of hot Galactic WR stars of WO sub-type. These are visually faint with narrow-band visual magnitudes Mv = -1.5 \~{} -2.5, despite their high bolometric luminosities (log L/Lsun = 5.6 \~{} 5.7), compared to the bulk of Galactic WR stars (Mv < -4). In contrast, relatively low-mass helium stars that retain a thick helium envelope appear fairly bright in optical bands, depending on the final masses and the history of the envelope expansion during the late evolutionary stages. We conclude that SNe Ibc observations have so far not provided strong constraints on progenitor bolometric luminosities and masses, even with the deepest searches. We also argue that Ic progenitors are more challenging to identify than Ib progenitors in any optical images.},
archiveprefix = {arXiv},
arxivid = {1207.3683},
author = {Yoon, S.-C. and Gr\"{a}fener, G. and Vink, J. S. and Kozyreva, A. and Izzard, R. G.},
doi = {10.1051/0004-6361/201219790},
eprint = {1207.3683},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/Astronomy \& Astrophysics/2012-1.pdf:pdf},
issn = {0004-6361},
journal = {Astronomy \& Astrophysics},
keywords = {binary,evolution,general,stars,supernovae,wolf-rayet},
month = {aug},
number = {1994},
pages = {L11},
title = {{On the nature and detectability of Type Ib/c supernova progenitors}},
url = {http://arxiv.org/abs/1207.3683 http://www.aanda.org/10.1051/0004-6361/201219790},
volume = {544},
year = {2012},
}
@article{1997A&A...328..203C,
author = {Cappellaro, E and Mazzali, P.\~{}A. and Benetti, S and Danziger, I J and Turatto, M and {Della Valle}, M and Patat, F},
journal = {Astronomy and Astrophysics},
month = {dec},
pages = {203--210},
title = {{SN IA light curves and radioactive decay}},
volume = {328},
year = {1997},
}
@article{Roming2005,
abstract = {The Ultra-Violet/Optical Telescope (UVOT) is one of three instruments flying aboard the Swift Gamma-ray Observatory. It is designed to capture the early (˜1 min) UV and optical photons from the afterglow of gamma-ray bursts in the 170 600 nm band as well as long term observations of these afterglows. This is accomplished through the use of UV and optical broadband filters and grisms. The UVOT has a modified Ritchey Chr\'{e}tien design with micro-channel plate intensified charged-coupled device detectors that record the arrival time of individual photons and provide sub-arcsecond positioning of sources. We discuss some of the science to be pursued by the UVOT and the overall design of the instrument.},
author = {Roming, Peter W. A. and Kennedy, Thomas E. and Mason, Keith O. and Nousek, John A. and Ahr, Lindy and Bingham, Richard E. and Broos, Patrick S. and Carter, Mary J. and Hancock, Barry K. and Huckle, Howard E. and Hunsberger, S D. and Kawakami, Hajime and Killough, Ronnie and Koch, T Scott and Mclelland, Michael K. and Smith, Kelly and Smith, Philip J. and Soto, Juan Carlos and Boyd, Patricia T. and Breeveld, Alice A. and Holland, Stephen T. and Ivanushkina, Mariya and Pryzby, Michael S. and Still, Martin D. and Stock, Joseph},
doi = {10.1007/s11214-005-5095-4},
issn = {0038-6308},
journal = {Space Science Reviews},
month = {oct},
number = {3-4},
pages = {95--142},
title = {{The Swift Ultra-Violet/Optical Telescope}},
url = {http://adsabs.harvard.edu/abs/2005SSRv..120...95R},
volume = {120},
year = {2005},
}
@article{Dessart2006,
abstract = {Multi-epoch multi-wavelength spectroscopic observations of photospheric-phase type II supernovae (SN) provide information on massive-star progenitor properties, the core-collapse mechanism, and distances in the Universe. Following successes of recent endeavors (Dessart \& Hillier 2005a, A\&A, 437, 667; 2005b, A\&A, 439, 671) with the non-LTE model atmosphere code CMFGEN (Hillier \& Miller 1998, ApJ, 496, 407), we present a detailed quantitative spectroscopic analysis of the type II SN1999em and, using the Expanding Photosphere Method (EPM) or synthetic fits to observed spectra, \`{a} la Baron et al. (2004, ApJ, 616, 91), we estimate its distance. Selecting eight epochs, which cover the first 38 days after discovery, we obtain satisfactory fits to optical spectroscopic observations of SN1999em (including the UV and near-IR ranges when available). We use the same iron-group metal content for the ejecta, the same power-law density distribution (with exponent n = 10\{-\}12), and a Hubble-velocity law at all times. We adopt a H/He/C/N/O abundance pattern compatible with CNO-cycle equilibrium values for a RSG/BSG progenitor, with C/O enhanced and N depleted at later times. The overall evolution of the spectral energy distribution, whose peak shifts to longer wavelengths as time progresses, reflects the steady temperature/ionization-level decrease of the ejecta, associated non-linearly with a dramatic shift to ions with stronger line-blocking powers in the UV and optical (Fe ii, Tiii). In the parameter space investigated, CMFGEN is very sensitive and provides photospheric temperatures and velocities, reddenings, and the H/He abundance ratio with an accuracy of ±500 K, ±10\%, 0.05 and 50\%, respectively. Following Leonard et al. (2002, PASP, 114, 35), and their use of correction factors from Hamuy et al. (2001, ApJ, 558, 615), we estimate an EPM distance to SN1999em that also falls 30\% short of the Cepheid distance of 11.7 Mpc to its host galaxy NGC 1637 (Leonard et al. 2003, ApJ, 594, 247). However, using the systematically higher correction factors of Dessart \& Hillier (2005b) removes the discrepancy. A significant scatter, arising primarily from errors in the correction factors and derived temperatures, is seen in distances derived using different band passes. However, adopting both correction factors and corresponding color-temperatures from tailored models to each observation leads to a good agreement between distance estimates obtained from different band passes. The need for detailed model computations thus defeats the appeal and simplicity of the original EPM method, which uses tabulated correction factors and broadband fluxes, for distance determinations. However, detailed fits to SN optical spectra, based on tailored models for individual SN observations, offers a promising approach to obtaining accurate distances, either through the EPM or via the technique of Baron et al. (2004). Our best distance-estimate to SN1999em is 11.5 ± 1.0 Mpc. We note that to achieve 10-20\% accuracy in such distance estimates requires multiple observations, covering preferentially a range of early epochs preceding the hydrogen-recombination phase.},
author = {Dessart, L. and Hillier, D. J.},
doi = {10.1051/0004-6361:20054044},
file = {:Users/svalenti/Documents/Mendeley Desktop/2006/Astronomy and Astrophysics/aa4044-05.pdf:pdf},
issn = {0004-6361},
journal = {Astronomy and Astrophysics},
keywords = {methods: numerical,radiative transfer,stars: atmospheres,stars: distances,stars: evolution,stars: supernovae: individual: SN1999em},
month = {feb},
number = {2},
pages = {691--707},
title = {{Quantitative spectroscopic analysis of and distance to SN1999em}},
url = {http://adsabs.harvard.edu/abs/2006A\&A...447..691D},
volume = {447},
year = {2006},
}
@article{Waagen2013,
abstract = {CBET 3609 available at Central Bureau for Astronomical Telegrams.},
author = {Waagen, E. O. and Cook, M. and Harris, B. and Sonka, A. and Stritof, N. and Smith, H. and Amorim, A. and Novichonok, A. and Wenzel, K. and Kida, K.},
journal = {Central Bureau Electronic Telegrams},
title = {{Supernova 2013ej in M74 = Psn J01364816+1545310}},
url = {http://adsabs.harvard.edu/abs/2013CBET.3609....3W},
year = {2013},
}
@article{Pastorello2007,
abstract = {An anomalous transient in the early Hubble-type (S0) galaxy Messier 85 (M85) in the Virgo cluster was discovered by Kulkarni et al. on 7 January 2006 that had very low luminosity (peak absolute R-band magnitude M(R) of about -12) that was constant over more than 80 days, red colour and narrow spectral lines, which seem inconsistent with those observed in any known class of transient events. Kulkarni et al. suggest an exotic stellar merger as the possible origin. An alternative explanation is that the transient in M85 was a type II-plateau supernova of extremely low luminosity, exploding in a lenticular galaxy with residual star-forming activity. This intriguing transient might be the faintest supernova that has ever been discovered.},
author = {Pastorello, A and {Della Valle}, M and Smartt, S J and Zampieri, L and Benetti, S and Cappellaro, E and Mazzali, P A and Patat, F and Spiro, S and Turatto, M and Valenti, S},
doi = {10.1038/nature06282},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/Nature/2007 Pastorello.pdf:pdf},
issn = {1476-4687},
journal = {Nature},
month = {oct},
number = {7164},
pages = {E1--2},
pmid = {17943088},
title = {{A very faint core-collapse supernova in M85.}},
url = {http://www.nature.com/nature/journal/vaop/ncurrent/full/nature06282.html http://www.ncbi.nlm.nih.gov/pubmed/17943088},
volume = {449},
year = {2007},
}
@article{Foley2013a,
abstract = {Two twin Type Ia supernovae (SNe Ia), SNe 2011by and 2011fe, have extremely similar optical light-curve shapes, colors, and spectra, yet have different ultraviolet (UV) continua as measured in Hubble Space Telescope spectra and measurably different peak luminosities. We attribute the difference in the UV continua to significantly different progenitor metallicities. This is the first robust detection of different metallicities for SN Ia progenitors. Theoretical reasoning suggests that differences in metallicity also lead to differences in luminosity. SNe Ia with higher progenitor metallicities have lower 56Ni yields and lower luminosities for the same light-curve shape. SNe 2011by and 2011fe have different peak luminosities ($\Delta$MV ≈ 0.6 mag), which correspond to different 56Ni yields: M\_11fe(\^{}\{56\}Ni) / M\_11by(\^{}\{56\}Ni) = 1.7\^{}\{+0.7\}\_\{-0.5\}. From theoretical models that account for different neutron-to-proton ratios in progenitors, the differences in 56Ni yields for SNe 2011by and 2011fe imply that their progenitor stars were above and below solar metallicity, respectively. Although we can distinguish progenitor metallicities in a qualitative way from UV data, the quantitative interpretation in terms of abundances is limited by the present state of theoretical models.},
author = {Foley, Ryan J. and Kirshner, Robert P.},
doi = {10.1088/2041-8205/769/1/L1},
file = {:Users/svalenti/Documents/Mendeley Desktop/2013/The Astrophysical Journal/apjl\_769\_1\_1.pdf:pdf},
issn = {2041-8205},
journal = {The Astrophysical Journal},
keywords = {supernovae: general,supernovae: individual: SN 2011by SN 2011fe},
month = {may},
number = {1},
pages = {L1},
title = {{METALLICITY DIFFERENCES IN TYPE Ia SUPERNOVA PROGENITORS INFERRED FROM ULTRAVIOLET SPECTRA}},
url = {http://adsabs.harvard.edu/abs/2013ApJ...769L...1F},
volume = {769},
year = {2013},
}
@article{Richardson2002,
author = {Richardson, Dean and Branch, David and Casebeer, Darrin and Millard, Jennifer and Thomas, R C and Baron, E},
doi = {10.1086/338318},
file = {:Users/svalenti/Documents/Mendeley Desktop/2002/The Astronomical Journal/2002 Richardson.pdf:pdf},
issn = {00046256},
journal = {The Astronomical Journal},
keywords = {catalogs,general,supernovae},
month = {feb},
number = {2},
pages = {745--752},
title = {{A Comparative Study of the Absolute Magnitude Distributions of Supernovae}},
url = {http://stacks.iop.org/1538-3881/123/i=2/a=745},
volume = {123},
year = {2002},
}
@article{2011ApJS..192....3P,
author = {Paxton, Bill and Bildsten, Lars and Dotter, Aaron and Herwig, Falk and Lesaffre, Pierre and Timmes, Frank},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/The Astrophysical Journal Supplement/2011 Paxton.pdf:pdf},
journal = {The Astrophysical Journal Supplement},
month = {jan},
number = {1},
pages = {3},
title = {{Modules for Experiments in Stellar Astrophysics (MESA)}},
volume = {192},
year = {2011},
}
@article{Hachinger2012,
author = {Hachinger, S. and Mazzali, P. a. and Taubenberger, S. and Hillebrandt, W. and Nomoto, K. and Sauer, D. N.},
doi = {10.1111/j.1365-2966.2012.20464.x},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2012 Hachinger.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {1 i n t,general,ib and ic,individual,radiative transfer,ro d u c,sn 1994i,sn 2008ax,sne iib,spectroscopic,stripped core-collapse supernovae of,supernovae,t i o n,techniques,types iib},
month = {may},
number = {1},
pages = {70--88},
title = {{How much H and He is ‘hidden’ in SNe Ib/c? - I. Low-mass objects}},
url = {http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2012.20464.x},
volume = {422},
year = {2012},
}
@article{2009ApJ...707..193F,
annote = {Detonation involves a supersonic exothermic front accelerating through a medium that eventually drives a shock front propagating directly in front of it Deflagration is a term describing subsonic combustion that usually propagates through thermal conductivity; hot burning material heats the next layer of cold material and ignites it. Deflagration is different from detonation, which is supersonic and propagates through shock compression. white dwarfs accreting hydrogen at a low rate undergo nova eruptions and lose more mass in the outburst than they have accreted prior to it At moderate accretion rates, a degenerate layer of helium is thought to form which might flash and could give rise to sub-Chandrasekhar explosions type of explosion AIC : accretion induced collapse: WD accrete C/O burn in O/Mg/Ne and collapse ? Nickel \{\&\}lt; 0.05 .Ia: helium flash on a WD, WD accrete Helium from a companion EC: Ia standard: WD accrete, mass exceed MCh, pressure and density grow, carbon fusion start a deflagration flame front is born, powered by carbon fusion. fail deflagration: deflagration off axis for which the WD expand, break the degeneracy and leave material unburned QUESTIONS: more IME in DENOTATION or DEFLAGRATION ?},
author = {Fryer, Chris L and Brown, Peter J and Bufano, Filomena and Dahl, Jon A and Fontes, Christopher J and Frey, Lucille H and Holland, Stephen T and Hungerford, Aimee L and Immler, Stefan and Mazzali, Paolo and Milne, Peter A and Scannapieco, Evan and Weinberg, Nevin and Young, Patrick A},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/The Astrophysical Journal/2009 Fryer.pdf:pdf},
journal = {The Astrophysical Journal},
month = {dec},
number = {1},
pages = {193--207},
title = {{Spectra and Light Curves of Failed Supernovae}},
volume = {707},
year = {2009},
}
@article{2009ApJ...705L.138P,
author = {Pumo, M L and Turatto, M and Botticella, M T and Pastorello, A and Valenti, S and Zampieri, L and Benetti, S and Cappellaro, E and Patat, F},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/The Astrophysical Journal Letters/2009 Pumo.pdf:pdf},
journal = {The Astrophysical Journal Letters},
month = {nov},
number = {2},
pages = {L138--------L142},
title = {{EC-SNe from Super-Asymptotic Giant Branch Progenitors: Theoretical Models Versus Observations}},
volume = {705},
year = {2009},
}
@article{Mazzali2007,
abstract = {Type Ia supernovae, the thermonuclear explosions of white dwarf stars composed of carbon and oxygen, were instrumental as distance indicators in establishing the acceleration of the universe's expansion. However, the physics of the explosion are debated. Here we report a systematic spectral analysis of a large sample of well-observed type Ia supernovae. Mapping the velocity distribution of the main products of nuclear burning, we constrain theoretical scenarios. We find that all supernovae have low-velocity cores of stable iron-group elements. Outside this core, nickel-56 dominates the supernova ejecta. The outer extent of the iron-group material depends on the amount of nickel-56 and coincides with the inner extent of silicon, the principal product of incomplete burning. The outer extent of the bulk of silicon is similar in all supernovae, having an expansion velocity of approximately 11,000 kilometers per second and corresponding to a mass of slightly over one solar mass. This indicates that all the supernovae considered here burned similar masses and suggests that their progenitors had the same mass. Synthetic light-curve parameters and three-dimensional explosion simulations support this interpretation. A single explosion scenario, possibly a delayed detonation, may thus explain most type Ia supernovae.},
author = {Mazzali, Paolo a and R\"{o}pke, Friedrich K and Benetti, Stefano and Hillebrandt, Wolfgang},
doi = {10.1126/science.1136259},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/Science (New York, N.Y.)/2007 Mazzali.pdf:pdf},
issn = {1095-9203},
journal = {Science (New York, N.Y.)},
month = {feb},
number = {5813},
pages = {825--8},
pmid = {17289993},
title = {{A common explosion mechanism for type Ia supernovae.}},
url = {http://www.ncbi.nlm.nih.gov/pubmed/17289993},
volume = {315},
year = {2007},
}
@article{1992AJ....104..340L,
author = {Landolt, Arlo U},
doi = {10.1086/116242},
issn = {00046256},
journal = {The Astronomical Journal},
month = {jul},
pages = {340},
title = {{UBVRI photometric standard stars in the magnitude range 11.5-16.0 around the celestial equator}},
url = {http://adsabs.harvard.edu/cgi-bin/bib\_query?1992AJ....104..340L},
volume = {104},
year = {1992},
}
@article{2011AN....332..262B,
author = {Bufano, F and Benetti, S and Sollerman, J and Pian, E and Cupani, G},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/Astronomische Nachrichten/2011 Bufano.pdf:pdf},
journal = {Astronomische Nachrichten},
month = {mar},
number = {3},
pages = {262},
title = {{Studying the SN-GRB connection with X-shooter: The GRB 100316D / SN 2010bh case}},
volume = {332},
year = {2011},
}
@article{2011MNRAS.418.1517M,
author = {Maurer, I and Jerkstrand, A and Mazzali, P. A. and Taubenberger, S and Hachinger, S and Kromer, M and Sim, S and Hillebrandt, W},
doi = {10.1111/j.1365-2966.2011.19376.x},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2011 Maurer.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {dec},
number = {3},
pages = {1517--1525},
title = {{nero- a post-maximum supernova radiation transport code}},
url = {http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2011.19376.x},
volume = {418},
year = {2011},
}
@article{Evans:2007tj,
annote = {To appear in the proceedings of Massive Stars: Fundamental Parameters and Circumstellar Interactions},
author = {Evans, C J},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/arXiv.org/arXiv 2007 Evans.pdf:pdf},
journal = {arXiv.org},
month = {apr},
title = {{Massive Stars: From the VLT to the ELT}},
volume = {astro-ph},
year = {2007},
}
@article{Zampieri2003,
abstract = {A number of supernovae, classified as Type II, show remarkably peculiar properties such as an extremely low expansion velocity and an extraordinarily small amount of 56Ni in the ejecta. We present a joint analysis of the available observations for two of these peculiar Type II supernovae, SN 1997D and SN 1999br, using a comprehensive semi-analytic method that can reproduce the light curve and the evolution of the line velocity and continuum temperature. We find that these events are underenergetic with respect to a typical Type II supernova and that the inferred mass of the ejecta is relatively large. We discuss the possibility that these supernovae originate from the explosion of a massive progenitor in which the rate of early infall of stellar material on the collapsed core is large. Events of this type could form a black hole remnant, giving rise to significant fallback and late-time accretion.},
author = {Zampieri, L. and Pastorello, A. and Turatto, M. and Cappellaro, E. and Benetti, S. and Altavilla, G. and Mazzali, P. and Hamuy, M.},
doi = {10.1046/j.1365-8711.2003.06082.x},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {methods: analytical,supernovae: general,supernovae: individual: SN 1997D,supernovae: individual: SN 1999br},
month = {jan},
number = {3},
pages = {711--716},
title = {{Peculiar, low-luminosity Type II supernovae: low-energy explosions in massive progenitors?}},
url = {http://adsabs.harvard.edu/abs/2003MNRAS.338..711Z},
volume = {338},
year = {2003},
}
@article{2011MNRAS.416..881M,
abstract = {The optical and near-infrared late-time spectrum of the under-luminous Type Ia supernova 2003hv is analysed with a code that computes nebular emission from a supernova nebula. Synthetic spectra based on the classical explosion model W7 are unable to reproduce the large $\backslash$FeIII/$\backslash$FeII$\backslash$ ratio and the low infrared flux at \$\backslash sim 1\$ year after explosion, although the optical spectrum of SN$\backslash$,2003hv is reproduced reasonably well for a supernova of luminosity intermediate between normal and subluminous (SN$\backslash$,1991bg-like) ones. A possible solution is that the inner layers of the supernova ejecta (\$v \backslash lsim 8000\$$\backslash$,$\backslash$kms) contain less mass than predicted by classical explosion models like W7. If this inner region contains \$\backslash sim 0.5 \backslash Msun\$ of material, as opposed to \$\backslash sim 0.9 \backslash Msun\$ in Chandrasekhar-mass models developed within the Single Degenerate scenario, the low density inhibits recombination, favouring the large $\backslash$FeIII/$\backslash$FeII$\backslash$ ratio observed in the optical, and decreases the flux in the $\backslash$FeII$\backslash$ lines which dominate the IR spectrum. The most likely scenario may be an explosion of a sub-Chandrasekhar mass white dwarf. Alternatively, the violent/dynamical merger of two white dwarfs with combined mass exceeding the Chandrasekhar limit also shows a reduced inner density.},
archiveprefix = {arXiv},
arxivid = {1105.1298},
author = {Mazzali, Paolo A. and Maurer, I and Stritzinger, M. and Taubenberger, S. and Benetti, S. and Hachinger, S.},
doi = {10.1111/j.1365-2966.2011.19000.x},
eprint = {1105.1298},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2011 Mazzali.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {general,individual,radiation,sn 2003hv,supernovae},
month = {sep},
number = {2},
pages = {881--892},
title = {{The nebular spectrum of the Type Ia supernova 2003hv: evidence for a non-standard event}},
url = {http://arxiv.org/abs/1105.1298 http://onlinelibrary.wiley.com/doi/10.1111/j.1365-2966.2011.19000.x/full http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2011.19000.x},
volume = {416},
year = {2011},
}
@article{2010arXiv1004.2262C,
archiveprefix = {arXiv},
arxivid = {1004.2262},
author = {Chornock, Ryan and Berger, Edo and Levesque, Emily M and Soderberg, Alicia M and Foley, Ryan J and Fox, Derek B and Frebel, Anna and Simon, Joshua D and Bochanski, John J and Challis, Peter J and Kirshner, Robert P and Podsiadlowski, Philipp and Roth, Katherine and Rutledge, Robert E and Schmidt, Brian P and Sheppard, Scott S and Simcoe, Robert A},
eprint = {1004.2262},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/arXiv.org/arXiv 2010 Chornock.pdf:pdf},
journal = {arXiv.org},
month = {apr},
pages = {2262},
title = {{Spectroscopic Discovery of the Broad-Lined Type Ic Supernova 2010bh Associated with the Low-Redshift GRB 100316D}},
volume = {1004},
year = {2010},
}
@article{2012ATel.4037....1V,
author = {Valenti, S and Pastorello, A and Benitez-Herrera, S and Taubenberger, S and Smartt, S.\~{}J. and Sullivan, M and Benetti, S and Cappellaro, E and Greggio, L and Hachinger, S and Turatto, M and Zampieri, L and Baltay, C and Ellman, N and Hadjiyska, E and McKinnon, R and Rabinowitz, D and Nugent, P and Mazzali, P.\~{}A. and Maguire, K and Pan, Yen-Chen and Hook, I and Fraser, M and Inserra, C and Magill, L and Maund, J and McCrum, M and Kotak, R and Smith, K W and Young, D.\~{}R. and Chen, T.-W. and Wright, D and Scalzo, R and Schmidt, B P and Sim, S.\~{}A. and Yuan, F and Stanishev, V and Patat, N and Botticella, M T and Dall'Ora, M and Limongi, M and Pumo, M L and Dennefeld, M and Blagorodnova, N Elias-Rosa N and Walton, N A and Cellier-Holzem, F and Bongard, S and Regnault, N and Pain, R and Guillou, L Le and Hillebrandt, W and Kromer, M and Sternberg, A and Bufano, F and Pignata, G and Anderson, J.\~{}P. and Hamuy, M and Clocchiatti, A and Eldridge, J J and Feindt, U and Kowalski, M and Kankare, E and Mattila, S and Walker, E S and Amanullah, R and Fransson, C and Goobar, A and Sollerman, J and Ergon, M and Gal-Yam, A and Yaron, O},
journal = {The Astronomer's Telegram},
month = {apr},
pages = {1},
title = {{PESSTO spectroscopic classification of La Silla-Quest Transients}},
volume = {4037},
year = {2012},
}
@article{2006ApJ...647..483L,
author = {Limongi, Marco and Chieffi, Alessandro},
file = {:Users/svalenti/Documents/Mendeley Desktop/2006/The Astrophysical Journal/2006 Limongi.pdf:pdf},
journal = {The Astrophysical Journal},
month = {aug},
number = {1},
pages = {483--500},
title = {{The Nucleosynthesis of 26Al and 60Fe in Solar Metallicity Stars Extending in Mass from 11 to 120 Msolar: The Hydrostatic and Explosive Contributions}},
volume = {647},
year = {2006},
}
@article{Roy2011,
author = {Roy, Rupak and Kumar, Brijesh and Benetti, Stefano and Pastorello, Andrea and Yuan, Fang and Brown, Peter J. and Immler, Stefan and Fatkhullin, Timur a. and Moskvitin, Alexander S. and Maund, Justyn and Akerlof, Carl W. and Wheeler, J. Craig and Sokolov, Vladimir V. and Quimby, Rorbert M. and Bufano, Filomena and Kumar, Brajesh and Misra, Kuntal and Pandey, S. B. and Elias-Rosa, Nancy and Roming, Peter W. a. and Sagar, Ram},
doi = {10.1088/0004-637X/736/2/76},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/The Astrophysical Journal/2011 Roy.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {2008in,color figures,general,individual,online-only material,supernovae},
month = {aug},
number = {2},
pages = {76},
title = {{SN 2008in---Bridging the Gap between Normal and Faint Supernovae of Type IIP}},
url = {http://stacks.iop.org/0004-637X/736/i=2/a=76?key=crossref.89c5d66cf3c2387dc25cf7eb1e51c9f3},
volume = {736},
year = {2011},
}
@article{2008ApJ...673..999P,
author = {Prieto, Jos\'{e} L and Stanek, Krzysztof Z and Beacom, John F},
file = {:Users/svalenti/Documents/Mendeley Desktop/2008/The Astrophysical Journal/2008 Prieto.pdf:pdf},
journal = {The Astrophysical Journal},
month = {feb},
number = {2},
pages = {999--1008},
title = {{Characterizing Supernova Progenitors via the Metallicities of their Host Galaxies, from Poor Dwarfs to Rich Spirals}},
volume = {673},
year = {2008},
}
@article{2009A&A...504..945T,
author = {Trundle, C and Pastorello, A and Benetti, S and Kotak, R and Valenti, S and Agnoletto, I and Bufano, F and Dolci, M and Elias-Rosa, N and Greiner, T and Hunter, D and Keenan, F P and Lorenzi, V and Maguire, K and Taubenberger, S},
journal = {Astronomy and Astrophysics},
month = {sep},
number = {3},
pages = {945--958},
title = {{Possible evidence of asymmetry in SN 2007rt, a type IIn supernova}},
volume = {504},
year = {2009},
}
@article{Patat2011,
abstract = {Aims: Recurrent nova systems like RS Oph have been proposed as a possible channel to Type Ia Supernova explosions, based on the high mass of the accreting white dwarf. Additional support to this hypothesis has been recently provided by the detection of circumstellar material around SN2006X and SN2007le, showing a structure compatible with that expected for recurrent nova outbursts.In this paper we investigate the circumstellar environment of RS Oph and its structure, with the aim of establishing a firmer and independent link between this class of objects and Type Ia SN progenitors. Methods: We study the time evolution of CaII, NaI and KI absorption features in RS Oph, before, during, and after the last outburst, using multi-epoch, high-resolution spectroscopy, and applying the same method adopted for SN2006X and SN2007le. Results: A number of components, blue-shifted with respect to the systemic velocity of RS Oph, are detected. In particular, one feature strongly weakens in the first two weeks after the outburst, simultaneously with the disappearance of very narrow P-Cyg profiles overimposed on the much wider nova emission lines of H, He, FeII and other elements. Conclusions: We interpret these facts as the signature of density enhancements in the circumstellar material, suggesting that the recurrent eruptions might indeed create complex structures within the material lost by the donor star. This establishes a strong link between RS Oph and the progenitor system of the Type Ia SN2006X, for which similar features have been detected.},
archiveprefix = {arXiv},
arxivid = {1104.0506},
author = {Patat, F and Chugai, N N and Podsiadlowski, Ph and Mason, E and Melo, C and Pasquini, L},
doi = {10.1051/0004-6361/201116865},
eprint = {1104.0506},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/Astronomy \& Astrophysics/2011 Patat.pdf:pdf},
issn = {0004-6361},
journal = {Astronomy \& Astrophysics},
keywords = {- supernovae,binaries,cataclysmic variables - stars,general - supernovae,individual,rs ophiuchi,sn 2006x,sn 2007le,symbiotic - novae},
month = {may},
pages = {A63},
title = {{Connecting RS Ophiuchi to [some] type Ia supernovae}},
url = {http://arxiv.org/abs/1104.0506 http://www.aanda.org/10.1051/0004-6361/201116865},
volume = {530},
year = {2011},
}
@article{Piro2013,
abstract = {The light curve of the explosion of a star with a radius \<\~{} 10-100 R ☉ is powered mostly by radioactive decay. Observationally, such events are dominated by hydrogen-deficient progenitors and classified as Type I supernovae (SNe I), i.e., white dwarf thermonuclear explosions (Type Ia), and core collapses of hydrogen-stripped massive stars (Type Ib/c). Current transient surveys are finding SNe I in increasing numbers and at earlier times, allowing their early emission to be studied in unprecedented detail. Motivated by these developments, we summarize the physics that produces their rising light curves and discuss ways in which observations can be utilized to study these exploding stars. The early radioactive-powered light curves probe the shallowest deposits of 56Ni. If the amount of 56Ni mixing in the outermost layers of the star can be deduced, then it places important constraints on the progenitor and properties of the explosive burning. In practice, we find that it is difficult to determine the level of mixing because it is hard to disentangle whether the explosion occurred recently and one is seeing radioactive heating near the surface or whether the explosion began in the past and the radioactive heating is deeper in the ejecta. In the latter case, there is a dark phase between the moment of explosion and the first observed light emitted once the shallowest layers of 56Ni are exposed. Because of this, simply extrapolating a light curve from radioactive heating back in time is not a reliable method for estimating the explosion time. The best solution is to directly identify the moment of explosion, either through observing shock breakout (in X-ray/UV) or the cooling of the shock-heated surface (in UV/optical), so that the depth being probed by the rising light curve is known. However, since this is typically not available, we identify and discuss a number of other diagnostics that are helpful for deciphering how recently an explosion occurred. As an example, we apply these arguments to the recent SN Ic PTF 10vgv. We demonstrate that just a single measurement of the photospheric velocity and temperature during the rise places interesting constraints on its explosion time, radius, and level of 56Ni mixing.},
author = {Piro, Anthony L. and Nakar, Ehud},
doi = {10.1088/0004-637X/769/1/67},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {hydrodynamics,shock waves,supernovae: general},
month = {may},
number = {1},
pages = {67},
title = {{WHAT CAN WE LEARN FROM THE RISING LIGHT CURVES OF RADIOACTIVELY POWERED SUPERNOVAE?}},
url = {http://adsabs.harvard.edu/abs/2013ApJ...769...67P},
volume = {769},
year = {2013},
}
@article{2006MNRAS.370.1752P,
author = {Pastorello, A and Sauer, D and Taubenberger, S and Mazzali, P. A. and Nomoto, K and Kawabata, K. S. and Benetti, S and Elias-Rosa, N and Harutyunyan, A and Navasardyan, H and Zampieri, L and Iijima, T and Botticella, M T and {Di Rico}, G. and {Del Principe}, M and Dolci, M and Gagliardi, S and Ragni, M and Valentini, G},
doi = {10.1111/j.1365-2966.2006.10587.x},
file = {:Users/svalenti/Documents/Mendeley Desktop/2006/Monthly Notices of the Royal Astronomical Society/2006MNRAS\_370\_1752P.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {jun},
number = {4},
pages = {1752--1762},
title = {{SN 2005cs in M51 - I. The first month of evolution of a subluminous SN II plateau}},
url = {http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2006.10587.x},
volume = {370},
year = {2006},
}
@article{1994AJ....107.1022R,
author = {Richmond, Michael W and Treffers, Richard R and Filippenko, Alexei V and Paik, Young and Leibundgut, Bruno and Schulman, Eric and Cox, Caroline V},
journal = {Astronomical Journal (ISSN 0004-6256)},
month = {mar},
pages = {1022--1040},
title = {{UBVRI photometry of SN 1993J in M81: The first 120 days}},
volume = {107},
year = {1994},
}
@article{2012ApJ...748...35S,
author = {Shen, Ken J. and Bildsten, Lars and Kasen, Daniel and Quataert, Eliot},
doi = {10.1088/0004-637X/748/1/35},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/The Astrophysical Journal/2012 Shen.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {abundances,binaries,close,color figures,general,nuclear reactions,nucleosynthesis,online-only material,supernovae,white dwarfs},
month = {mar},
number = {1},
pages = {35},
title = {{The Long-term Evolution of Double White Dwarf Mergers}},
url = {http://stacks.iop.org/0004-637X/748/i=1/a=35?key=crossref.2894de2790dfc375ad6ab09013d258f4},
volume = {748},
year = {2012},
}
@article{2007ApJ...662L..95B,
author = {Bildsten, Lars and Shen, Ken J and Weinberg, Nevin N and Nelemans, Gijs},
doi = {10.1086/519489},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/The Astrophysical Journal/2007 Bildsten.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {jun},
number = {2},
pages = {L95--L98},
title = {{Faint Thermonuclear Supernovae from AM Canum Venaticorum Binaries}},
url = {http://stacks.iop.org/1538-4357/662/i=2/a=L95},
volume = {662},
year = {2007},
}
@article{2012MNRAS.426.1465P,
author = {Poznanski, Dovi and Prochaska, J Xavier and Bloom, Joshua S},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {oct},
number = {2},
pages = {1465--1474},
title = {{An empirical relation between sodium absorption and dust extinction}},
volume = {426},
year = {2012},
}
@article{Grieco2012,
abstract = {Supernovae Ib/c are likely to be associated to long GRBs, therefore it is important to compare the SN rate in galaxies with the GRB rate. To do that we computed Type Ib/c SN rates in galaxies of different morphological type by assuming different histories of star formation and different supernova Ib/c progenitors. We included some recent suggestions about the dependence of the minimum mass of single Wolf-Rayet (WR) stars upon the stellar metallicity and therefore upon galactic chemical evolution. We adopted several cosmic star formation rates as functions of cosmic time, either observationally or theoretically derived, including the one computed with our galaxy models. Then we computed the cosmic Type Ib/c SN rates. We derived the following conclusions: i) the ratio cosmic GRB - Type Ib/c rate varies in the range 10\^{}\{-2\}-10\^{}\{-4\} in the whole redshift range, thus suggesting that only a small fraction of all the Type Ib/c SNe gives rise to GRBs. ii) The metallicity dependence of Type Ib/c SN progenitors produces lower cosmic SN Ib/c rates at early times, for any chosen cosmic star formation rate. iii) Different theoretical cosmic star formation rates, computed under different scenarios of galaxy formation, produce SN Ib/c cosmic rates which differ mainly at very high redshift. However, it is difficult to draw firm conclusions on the high redshift trend because of the large uncertainties in the data. iv) GRBs can be important tracers of star formation at high redshift if their luminosity function does not vary with redshift and they can help in discriminating among different galaxy formation models.},
archiveprefix = {arXiv},
arxivid = {1204.2417},
author = {Grieco, V. and Matteucci, F. and Meynet, G. and Longo, F. and {Della Valle}, M. and Salvaterra, R.},
eprint = {1204.2417},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/arXiv preprint arXiv \ldots/arXiv 2012 Grieco.pdf:pdf},
journal = {arXiv preprint arXiv: \ldots},
keywords = {galaxy evolution,gamma-ray bursts,supernovae},
month = {apr},
number = {April},
pages = {10},
title = {{Metallicity effects on the cosmic SNIb/c and GRB rates}},
url = {http://arxiv.org/abs/1204.2417},
year = {2012},
}
@inproceedings{2007AIPC..924..291V,
author = {Valenti, Stefano},
booktitle = {THE MULTICOLORED LANDSCAPE OF COMPACT OBJECTS AND THEIR EXPLOSIVE ORIGINS. AIP Conference Proceedings},
month = {aug},
organization = {Physics Department, University of Ferrara, I-44100 Ferrara, ItalyEuropean Southern Observatory, Garching bei Munich, Germany},
pages = {291--296},
title = {{Supernova 2003jd: Optical observations}},
year = {2007},
}
@article{2007A&A...469..645S,
author = {Stanishev, V and Goobar, A and Benetti, S and Kotak, R and Pignata, G and Navasardyan, H and Mazzali, P and Amanullah, R and Garavini, G and Nobili, S and Qiu, Y and Elias-Rosa, N and Ruiz-Lapuente, P and Mendez, J and Meikle, P and Patat, F and Pastorello, A and Altavilla, G and Gustafsson, M and Harutyunyan, A and Iijima, T and Jakobsson, P and Kichizhieva, M V and Lundqvist, P and Mattila, S and Melinder, J and Pavlenko, E P and Pavlyuk, N N and Sollerman, J and Tsvetkov, D Yu. and Turatto, M and Hillebrandt, W},
journal = {Astronomy and Astrophysics},
month = {jul},
number = {2},
pages = {645--661},
title = {{SN 2003du: 480 days in the life of a normal type Ia supernova}},
volume = {469},
year = {2007},
}
@article{Nomoto1984,
abstract = {The carbon deflagration models in accreting C + O white dwarfs are presented as a plausible model for Type I supernovae. The evolution of the white dwarf is calculated from the beginning of accretion. The relatively rapid accretion studied here (Mdot \> 4 x 10-8 Msun yr-1) leads to the initiation of the carbon deflagration at the center. Subsequent propagation of the convective carbon deflagration wave and associated explosive nucleosynthesis are calculated for several cases of mixing length in the convection theory. The deflagration wave synthesizes 0.5-0.6 Msun 56Ni in the inner layer of the star; this amount is sufficient to power the light curve of Type I supernovae by the radioactive decays of 56Ni and 56Co. In the outer layers, substantial amount of intermediate mass elements, Ca, Ar, S, Si, Mg, and O are synthesized in the decaying deflagration wave; this is consistent with the spectra of Type I supernovae near maximum light. As a result of large nuclear energy release, the star is disrupted completely, leaving no compact star remnant behind. Thus the carbon deflagration model can account for many of the observed features of Type I supernovae. Nucleosynthesis in the deflagration models is discussed based on the reaction network calculation including 205 species: The abundance ratios of these species with respect to 56Fe normalized to the solar values are shown. These ratios are ˜1 for 40Ca and ˜0.5 for 36Ar, 32S, and 28Si. This suggests that Type I supernovae produce a significant fraction of these elements in the Galaxy besides iron peak elements, which may be complementary to the nucleosynthesis in massive star models for Type II supernovae. The production of neutronrich isotopes, $\gamma$-radioactivities, and 5- and r-process elements are discussed. Finally, the light curves and early time spectra based on the present models are compared with Type I supernova observations.},
author = {Nomoto, K. and Thielemann, F.-K. and Yokoi, K.},
doi = {10.1086/162639},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {CARBON STARS,DEFLAGRATION,HYDRODYNAMICS,LIGHT CURVE,NEUTRINOS,NUCLEAR FUSION,STELLAR COMPOSITION,STELLAR MASS ACCRETION,STELLAR MODELS,SUPERNOVAE,WAVE PROPAGATION,WHITE DWARF STARS},
month = {nov},
pages = {644},
title = {{Accreting white dwarf models of Type I supernovae. III - Carbon deflagration supernovae}},
url = {http://adsabs.harvard.edu/abs/1984ApJ...286..644N},
volume = {286},
year = {1984},
}
@article{Howell2009,
abstract = {In the next decade Type Ia supernovae (SNe Ia) will be used to test theories predicting changes in the Dark Energy equation of state with time. Ultimately this requires a dedicated space mission like JDEM. SNe Ia are mature cosmological probes --- their limitations are well characterized, and a path to improvement is clear. Dominant systematic errors include photometric calibration, selection effects, reddening, and population-dependent differences. Building on past lessons, well-controlled new surveys are poised to make strides in these areas: the Palomar Transient Factory, Skymapper, La Silla QUEST, Pan-STARRS, the Dark Energy Survey, LSST, and JDEM. They will obviate historical calibrations and selection biases, and allow comparisons via large subsamples. Some systematics follow from our ignorance of SN Ia progenitors, which there is hope of determining with SN Ia rate studies from 0<z<4. Aside from cosmology, SNe Ia regulate galactic and cluster chemical evolution, inform stellar evolution, and are laboratories for extreme physics. Essential probes of SNe Ia in these contexts include spectroscopy from the UV to the IR, X-ray cluster and SN remnant observations, spectropolarimetry, and advanced theoretical studies. While there are an abundance of discovery facilities planned, there is a deficit of follow-up resources. Living in the systematics era demands deep understanding rather than larger statistics. NOAO ReSTAR initiative to build 2-4m telescopes would provide necessary follow-up capability. Finally, to fully exploit LSST, well-matched wide-field spectroscopic capabilities are desirable.},
archiveprefix = {arXiv},
arxivid = {0903.1086},
author = {Howell, D. A. and Conley, A. and {Della Valle}, M. and Nugent, P. E. and Perlmutter, S. and Marion, G. H. and Krisciunas, K. and Badenes, C. and Mazzali, P. and Aldering, G. and Antilogus, P. and Baron, E. and Becker, A. and Baltay, C. and Benetti, S. and Blondin, S. and Branch, D. and Brown, E. F. and Deustua, S. and Ealet, A. and Ellis, R. S. and Fouchez, D. and Freedman, W. and Gal-Yam, A. and Jha, S. and Kasen, D. and Kessler, R. and Kim, A. G. and Leonard, D. C. and Li, W. and Livio, M. and Maoz, D. and Mannucci, F. and Matheson, T. and Neill, J. D. and Nomoto, K. and Panagia, N. and Perrett, K. and Phillips, M. and Poznanski, D. and Quimby, R. and Rest, A. and Riess, A. and Sako, M. and Soderberg, A. M. and Strolger, L. and Thomas, R. and Turatto, M. and van Dyk, S. and Wood-Vasey, W. M.},
eprint = {0903.1086},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/Unknown/arXiv 2009 Howell.pdf:pdf},
month = {mar},
title = {{Type Ia supernova science 2010-2020}},
url = {http://arxiv.org/abs/0903.1086},
year = {2009},
}
@article{Seitenzahl2009,
author = {Seitenzahl, I. R. and Taubenberger, S. and Sim, S. a.},
doi = {10.1111/j.1365-2966.2009.15478.x},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2009 Seitenzahl.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {1 i n t,abundances,general,individual,novae,nuclear reactions,nucleosynthesis,one of the great,ro d u c,sn 1998bw,successes of nuclear astrophysics,super-,supernovae,t i o n,was demonstrat-,white dwarfs},
month = {nov},
number = {1},
pages = {531--535},
title = {{Late-time supernova light curves: the effect of internal conversion and Auger electrons}},
url = {http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2009.15478.x},
volume = {400},
year = {2009},
}
@article{Hamuy2001,
abstract = {I report photometry and spectroscopy for 16 Type II supernovae (SNe) observed during the Calan/Tololo, SOIRS, and CTIO SN programs, a valuable resource for astrophysical studies. I perform a detailed assessment of the performance of the expanding photosphere method (EPM) in the determination of extragalactic distances. EPM proves very sensitive to the many steps involved in the analysis which can make it an art instead of an objective measurement tool. To minimize biases I implement objective procedures to compute synthetic magnitudes, measure true photospheric velocities, interpolate velocities, estimate dust extinction and realistic errors. While EPM performs well during the initial phases of SN evolution, I find distance residuals as large as 50\% as the photosphere approaches the H recombination temperature. Despite the effort to lend credence to EPM, it proves necessary to exercise great care to avoid biasing the results. The main sources of uncertainties are observational errors (8\%), dilution factors (11\%), velocity interpolations (12\%), and dust extinction (14\%). The EPM Hubble diagram suggests the true error in an individual EPM distance is 20\%. I find values of 63 +/- 8 and 67 +/- 7 km s-1 Mpc-1 for the Hubble constant, depending on the redshift sample chosen for the analysis. This result is independent of the extragalactic distance scale which yields 65 +/- 5 from Cepheid/SNe la distances. From four objects the comparison of EPM and Tully-Fisher yields D(EPM)/D(TF) = 0.82 +/- 0.12. I derive bolometric corrections for plateau SNe (SNe II-P) that permit me to obtain reliable bolometric luminosities from BVI photometry. Despite the great diversity displayed by SNe II-P, the duration of the plateau is approximately the same and the luminosities and expansion velocities measured in the middle of the plateau prove highly correlated. From the luminosity of the exponential tail I obtain 56Co masses ranging between 0.02 and 0.28 M⊙ , and some evidence that SNe with brighter plateaus produce more Ni (and its daughter Co). The correlation between expansion velocity and luminosity permits me the use of SNe II-P as standard candles with a magnitude dispersion between 0.39--0.20 mag. Using SN 1987A to calibrate the Hubble diagram I get H0 = 55 +/- 12 and H 0 = 56 +/- 9 from the V and I filters, respectively.},
author = {Hamuy, Mario Andres},
journal = {ProQuest Dissertations And Theses; Thesis (Ph.D.)--The University of Arizona},
title = {{Type II supernovae as distance indicators}},
url = {http://adsabs.harvard.edu/abs/2001PhDT.......173H},
year = {2001},
}
@article{2008ATel.1354....1S,
author = {Soderberg, Alicia},
journal = {The Astronomer's Telegram},
month = {jan},
pages = {1},
title = {{Radio observations of the transient in NGC 2770}},
volume = {1354},
year = {2008},
}
@article{Anonymous:v22vTf7_,
month = {jul},
pages = {1--8},
title = {{v1.3}},
year = {2012},
}
@article{2010ApJ...717L..52B,
author = {Botticella, M T and Trundle, C and Pastorello, A and Rodney, S and Rest, A and Gezari, S and Smartt, S.\~{}J. and Narayan, G and Huber, M E and Tonry, J L and Young, D and Smith, K and Bresolin, F and Valenti, S and Kotak, R and Mattila, S and Kankare, E and Wood-Vasey, W M and Riess, A and Neill, J D and Forster, K and Martin, D C and Stubbs, C W and Burgett, W S and Chambers, K C and Dombeck, T and Flewelling, H and Grav, T and Heasley, J N and Hodapp, K W and Kaiser, N and Kudritzki, R and Luppino, G and Lupton, R H and Magnier, E A and Monet, D G and Morgan, J S and Onaka, P M and Price, P A and Rhoads, P H and Siegmund, W A and Sweeney, W E and Wainscoat, R J and Waters, C and Waterson, M F and Wynn-Williams, C G},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/The Astrophysical Journal Letters/2010 Botticella.pdf:pdf},
journal = {The Astrophysical Journal Letters},
month = {jul},
number = {1},
pages = {L52--------L56},
title = {{Supernova 2009kf: An Ultraviolet Bright Type IIP Supernova Discovered with Pan-STARRS 1 and GALEX}},
volume = {717},
year = {2010},
}
@article{ValentiS.2013,
abstract = {We report a spectroscopic observation of PSN J19243815+5941471, located at RA= 19:24:38.15 DEC= +59:41:47.1 (J2000). The coordinates are consistent with the Galactic dwarf nova SN 1998di (IAUC6983).},
author = {{Valenti, S.} and {Graham, M. L.} and {Howell, D. A.} and {Sand, D.} and {Parrent, J. T.} and {Ciabattari, F.} and {Mazzoni, E.} and {Rossi, M.} and {Donati, S.}},
journal = {The Astronomer's Telegram},
keywords = {Nova,Optical},
title = {{Spectroscopy for PSN J19243815+5941471 with FLOYDS at Faulkes Telescope North: another dwarf nova outburst of SN1998di ?}},
url = {http://adsabs.harvard.edu/abs/2013ATel.5188....1V},
year = {2013},
}
@article{Juric2011,
abstract = {The advent of deep, wide, accurate, digital photometric surveys exemplified by the Sloan Digital Sky Survey (SDSS) has had a profound impact on studies of the Milky Way. In the past decade, we have transitioned from a scarcity to an (over)abundance of precise, well calibrated, observations of stars over a large fraction of the Galaxy. The avalanche of data will continue throughout this decade, culminating with Gaia and LSST. This new reality will necessitate changes in methodology, habits, and expectations both on the side of the large survey projects as well as the astrophysics community at large. We argue, based on the experience with SDSS, that surveys should release data as early and often as possible incorporating incremental improvements in each subsequent release, as opposed to holding off for a single, big, final release. The scientific community will need to reciprocate by performing analyses and (re-analyses) appropriate to the current fidelity of the released data, understanding that these are continually evolving and improving products.},
archiveprefix = {arXiv},
arxivid = {1102.1116},
author = {Juri\'{c}, M. and Ivezi\'{c}, \v{Z}.},
doi = {10.1051/eas/1045047},
eprint = {1102.1116},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/EAS Publications Series/arXiv 2011 Juri\'{c}.pdf:pdf},
issn = {1633-4760},
journal = {EAS Publications Series},
month = {feb},
pages = {281--286},
title = {{SDSS, LSST and Gaia: Lessons and Synergies}},
url = {http://arxiv.org/abs/1102.1116 http://www.eas-journal.org/10.1051/eas/1045047},
volume = {45},
year = {2011},
}
@article{1990IAUC.5111....1F,
author = {Filippenko, A V and Shields, J C and Petschek, A G},
journal = {IAU Circ.},
month = {oct},
pages = {1},
title = {{Supernova 1990aa in UGC 540}},
volume = {5111},
year = {1990},
}
@phdthesis{2000PhDT.........6F,
annote = {From Duplicate 2 ( Direct analysis of type Ia supernovae spectra - Fisher, Adam Keith ) Publication Number: 9962949; Advisor: Branch, David},
author = {Fisher, Adam Keith},
booktitle = {Thesis (PhD). THE UNIVERSITY OF OKLAHOMA},
month = {aug},
pages = {6},
school = {THE UNIVERSITY OF OKLAHOMA},
title = {{Direct analysis of type Ia supernovae spectra}},
year = {2000},
}
@article{Chugai2007,
abstract = {We propose new diagnostics for circumstellar interaction in Type IIP supernovae (SNe IIP) by the detection of high-velocity (HV) absorption features in H$\alpha$ and He I 10830 \AA lines during the photospheric stage. To demonstrate the method, we compute the ionization and excitation of H and He in supernova ejecta taking into account time-dependent effects and X-ray irradiation. We find that the interaction with a typical red supergiant wind should result in the enhanced excitation of the outer layers of unshocked ejecta and the emergence of corresponding HV absorption, i.e., a depression in the blue absorption wing of H$\alpha$ and a pronounced absorption of He I 10830 \AA at a radial velocity of about -104 km s-1. We identify HV absorption in H$\alpha$ and He I 10830 \AA lines of SN 1999em and in H$\alpha$ of SN 2004dj as being due to this effect. The derived mass-loss rate is close to 10-6 Msolar yr-1 for both supernovae, assuming a wind velocity 10 km s-1. We argue that in addition to the HV absorption formed in the unshocked ejecta, spectra of SN 2004dj and SN 1999em show a HV notch feature that is formed in the cool dense shell (CDS) modified by the Rayleigh-Taylor instability. The CDS results from both shock breakout and radiative cooling of gas that has passed through the reverse shock wave. The notch becomes dominant in the HV absorption during the late photospheric phase, \>\~{}60 days. The wind density deduced from the velocity of the CDS is consistent with the wind density found from the HV absorption produced by unshocked ejecta.},
author = {Chugai, Nikolai N. and Chevalier, Roger A. and Utrobin, Victor P.},
doi = {10.1086/518160},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/The Astrophysical Journal/71336.web.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {Stars: Mass Loss,Stars: Supernovae: General,Stars: Supernovae: Individual: Alphanumeric: SN 19,Stars: Supernovae: Individual: Alphanumeric: SN 20},
month = {jun},
number = {2},
pages = {1136--1147},
title = {{Optical Signatures of Circumstellar Interaction in Type IIP Supernovae}},
url = {http://adsabs.harvard.edu/abs/2007ApJ...662.1136C},
volume = {662},
year = {2007},
}
@article{2011ApJ...730..134K,
author = {Kasliwal, Mansi M and Kulkarni, Shri R and Arcavi, Iair and Quimby, Robert M and Ofek, Eran O and Nugent, Peter and Jacobsen, Janet and Gal-Yam, Avishay and Green, Yoav and Yaron, Ofer and Fox, Derek B and Howell, Jacob L and Cenko, S Bradley and Kleiser, Io and Bloom, Joshua S and Miller, Adam and Li, Weidong and Filippenko, Alexei V and Starr, Dan and Poznanski, Dovi and Law, Nicholas M and Helou, George and Frail, Dale A and Neill, James D and Forster, Karl and Martin, D Christopher and Tendulkar, Shriharsh P and Gehrels, Neil and Kennea, Jamie and Sullivan, Mark and Bildsten, Lars and Dekany, Richard and Rahmer, Gustavo and Hale, David and Smith, Roger and Zolkower, Jeff and Velur, Viswa and Walters, Richard and Henning, John and Bui, Kahnh and McKenna, Dan and Blake, Cullen},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/The Astrophysical Journal/2011 Kasliwal.pdf:pdf},
journal = {The Astrophysical Journal},
month = {apr},
number = {2},
pages = {134},
title = {{PTF 10fqs: A Luminous Red Nova in the Spiral Galaxy Messier 99}},
volume = {730},
year = {2011},
}
@article{Prieto2012,
abstract = {We present the discovery and follow-up observations of SN 2008jb, a core-collapse supernova in the southern dwarf irregular galaxy ESO 302-14 (MB = -15.3 mag) at 9.6 Mpc. This nearby transient was missed by galaxy-targeted surveys and was only found in archival optical images obtained by the Catalina Real-time Transient Survey and the All-Sky Automated Survey. The well-sampled archival photometry shows that SN 2008jb was detected shortly after explosion and reached a bright optical maximum, V max \~{}= 13.6 mag (M V, max \~{}= -16.5). The shape of the light curve shows a plateau of \~{}100 days, followed by a drop of \~{}1.4 mag in the V band to a slow decline with an approximate 56Co decay slope. The late-time light curve is consistent with 0.04 ± 0.01 M ⊙ of 56Ni synthesized in the explosion. A spectrum of the supernova obtained two years after explosion shows a broad, boxy H$\alpha$ emission line, which is unusual for normal Type II-Plateau supernovae at late times. We detect the supernova in archival Spitzer and WISE images obtained 8-14 months after explosion, which show clear signs of warm (600-700 K) dust emission. The dwarf irregular host galaxy, ESO 302-14, has a low gas-phase oxygen abundance, 12 + log(O/H) = 8.2 (\~{}1/5 Z ⊙), similar to those of the Small Magellanic Cloud and the hosts of long gamma-ray bursts and luminous core-collapse supernovae. This metallicity is one of the lowest among local (lsim 10 Mpc) supernova hosts. We study the host environment using GALEX far-UV, R-band, and H$\alpha$ images and find that the supernova occurred in a large star formation complex. The morphology of the H$\alpha$ emission appears as a large shell (R \~{}= 350 pc) surrounding the FUV and optical emission. Using the H$\alpha$-to-FUV ratio and FUV and R-band luminosities, we estimate an age of \~{}9 Myr and a total mass of \~{}2 × 105 M ⊙ for the star formation complex, assuming a single-age starburst. These properties are consistent with the expanding H$\alpha$ supershells observed in many well-studied nearby dwarf galaxies, which are tell-tale signs of feedback from the cumulative effect of massive star winds and supernovae. The age estimated for the star-forming region where SN 2008jb exploded suggests a relatively high-mass progenitor star with an initial mass M \~{} 20 M ⊙ and warrants further study. We discuss the implications of these findings in the study of core-collapse supernova progenitors. This paper includes data gathered with the 6.5 m Magellan telescope at Las Campanas Observatory, Chile.},
author = {Prieto, J. L. and Lee, J. C. and Drake, A. J. and McNaught, R. and Garradd, G. and Beacom, J. F. and Beshore, E. and Catelan, M. and Djorgovski, S. G. and Pojmanski, G. and Stanek, K. Z. and Szczygieł, D. M.},
doi = {10.1088/0004-637X/745/1/70},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {galaxies: dwarf,supernovae: general,supernovae: individual: SN 2008jb},
month = {jan},
number = {1},
pages = {70},
title = {{SN 2008jb: A “LOST” CORE-COLLAPSE SUPERNOVA IN A STAR-FORMING DWARF GALAXY AT ∼10 Mpc}},
url = {http://adsabs.harvard.edu/abs/2012ApJ...745...70P},
volume = {745},
year = {2012},
}
@article{2010MNRAS.402..161M,
author = {Maurer, J I and Mazzali, P.\~{}A. and Deng, J and Filippenko, A V and Hamuy, M and Kirshner, R P and Matheson, T and Modjaz, M and Pian, E and Stritzinger, M and Taubenberger, S and Valenti, S},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2010 Maurer-2.pdf:pdf},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {feb},
number = {1},
pages = {161--172},
title = {{Characteristic velocities of stripped-envelope core-collapse supernova cores}},
volume = {402},
year = {2010},
}
@article{2011ApJ...738...21W,
author = {Waldman, Roni and Sauer, Daniel and Livne, Eli and Perets, Hagai and Glasner, Ami and Mazzali, Paolo and Truran, James W and Gal-Yam, Avishay},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/The Astrophysical Journal/2011 Waldman.pdf:pdf},
journal = {The Astrophysical Journal},
month = {sep},
number = {1},
pages = {21},
title = {{Helium Shell Detonations on Low-mass White Dwarfs as a Possible Explanation for SN 2005E}},
volume = {738},
year = {2011},
}
@article{Kim2013,
abstract = {CBET 3606 available at Central Bureau for Astronomical Telegrams.},
author = {Kim, M. and Zheng, W. and Li, W. and Filippenko, A. V. and Cenko, S. B. and Richmond, M. W. and Amorim, A. and Balam, D. D. and Graham, M. L. and Hsiao, E. Y.},
journal = {Central Bureau Electronic Telegrams},
title = {{Supernova 2013ej in M74 = Psn J01364816+1545310}},
url = {http://adsabs.harvard.edu/abs/2013CBET.3606....1K},
year = {2013},
}
@article{Silverman2012,
abstract = {In this third paper in a series we compare spectral feature measurements to photometric properties of 108 low-redshift (z \< 0.1, \<z\> ≈ 0.023) Type Ia supernovae (SNe Ia) for which we have optical spectra within 5 d of maximum brightness. The spectral data were obtained from 1989 to the end of 2008 as part of the Berkeley Supernova Ia Program (BSNIP) and are presented in BSNIP I by Silverman et al., and the photometric data come mainly from the Lick Observatory Supernova Search and are published by Ganeshalingam et al. The spectral measurements are presented and discussed in BSNIP II by Silverman, Kong \& Filippenko, and the light-curve fits and photometric parameters can be found in Ganeshalingam et al. (in preparation). A variety of previously proposed correlations between spectral and photometric parameters are investigated using the large and self-consistent BSNIP data set. We find the pseudo-equivalent width (pEW) of the Si II $\lambda$4000 line to be a good indicator of light-curve width, and the pEWs of the Mg II and Fe II complexes are relatively good proxies for SN colour. We also employ a combination of light-curve parameters (specifically the Spectral Adaptive Light-curve Template 2 stretch and colour parameters x1 and c, respectively) and spectral measurements to calculate distance moduli. The residuals from these models are then compared to the standard model which uses only light-curve stretch and colour. Our investigations show that a distance model that uses x1, c and the velocity of the Si II $\lambda$6355 feature does not lead to a decrease in the Hubble residuals. We also find that distance models with flux ratios alone or in conjunction with light-curve information rarely perform better than the standard (x1, c) model. However, when adopting a distance model which combines the ratio of fluxes near ˜3750 and 4550 \AA with both x1 and c, the Hubble residuals are decreased by ˜10 per cent, which is found to be significant at about the 2$\sigma$ level. The weighted root mean square of the residuals using this model is 0.130 ± 0.017 mag (as compared with 0.144 ± 0.019 mag when using the same sample with the standard model). This Hubble diagram fit has one of the smallest scatters ever published and at the highest significance ever seen in such a study. Finally, these results are discussed with regard to how they can improve the cosmological accuracy of future, large-scale SN Ia surveys.},
author = {Silverman, Jeffrey M. and Ganeshalingam, Mohan and Li, Weidong and Filippenko, Alexei V.},
doi = {10.1111/j.1365-2966.2012.21526.x},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {cosmology: observations,distance scale,methods: data analysis,supernovae: general},
month = {sep},
number = {3},
pages = {1889--1916},
title = {{Berkeley Supernova Ia Program - III. Spectra near maximum brightness improve the accuracy of derived distances to Type Ia supernovae}},
url = {http://adsabs.harvard.edu/abs/2012MNRAS.425.1889S},
volume = {425},
year = {2012},
}
@article{2011ApJ...728...14P,
author = {Pignata, Giuliano and Stritzinger, Maximilian and Soderberg, Alicia and Mazzali, Paolo and Phillips, M.\~{}M. and Morrell, Nidia and Anderson, J.\~{}P. and Boldt, Luis and Campillay, Abdo and Contreras, Carlos and Folatelli, Gast\'{o}n and F\"{o}rster, Francisco and Gonz\'{a}lez, Sergio and Hamuy, Mario and Krzeminski, Wojtek and Maza, Jos\'{e} and Roth, Miguel and Salgado, Francisco and Levesque, Emily M and Rest, Armin and Crain, J Adam and Foster, Andrew C and Haislip, Joshua B and Ivarsen, Kevin M and LaCluyze, Aaron P and Nysewander, Melissa C and Reichart, Daniel E},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/The Astrophysical Journal/2011 Pignata.pdf:pdf},
journal = {The Astrophysical Journal},
month = {feb},
number = {1},
pages = {14},
title = {{SN 2009bb: A Peculiar Broad-lined Type Ic Supernova}},
volume = {728},
year = {2011},
}
@article{Taddia2012,
author = {Taddia, F and Stritzinger, M D and Phillips, M M and Burns, C. R. and Heinrich-Josties, E. and Morrell, N. and Sollerman, J. and Valenti, S. and Anderson, J P and Boldt, L and Campillay, A and Castellon, S and Contreras, C and Folatelli, G. and Freedman, W. L. and Hamuy, M. and Krzeminski, W. and Leloudas, G. and Maeda, K. and Persson, S. E. and Roth, M. and Suntzeff, N. B.},
doi = {10.1051/0004-6361/201220105},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/Astronomy \& Astrophysics/2012-2.pdf:pdf},
issn = {0004-6361},
journal = {Astronomy \& Astrophysics},
keywords = {general,individual,sn 2008j,supernovae},
month = {sep},
number = {2010},
pages = {L7},
title = {{Supernova 2008J: early time observations of a heavily reddened SN 2002ic-like transient}},
url = {http://www.aanda.org/10.1051/0004-6361/201220105},
volume = {545},
year = {2012},
}
@article{1997A&A...318..269M,
abstract = {The profile, radial velocity and equivalent width of the interstellar lines of Na I (5890.0, 5895.9\AA) and K I (7699.0\AA) have been obtained from Echelle+CCD observations at resolving power $\lambda$/\{DELTA\}$\lambda$\~{}16,500 for 32 O and early B stars suffering from a reddening between E\_B-V\_=0.06 and 1.57. The data have been used to search for and calibrate a relation between equivalent width and reddening. When the interstellar lines show a single and sharp component, useful relations to estimate reddening from equivalent widths have been derived. The relation for Na I is most sensitive in the range 0.0<=E\_B-V\_<=0.4, and the one for K I takes over at higher reddening. Good quality equivalent width measurements allow E\_B-V\_ to be estimated with an accuracy of about 0.05 mag. For multi-component profiles of Na I and K I lines the estimate of reddening is more ambiguous with a general scatter of 0.15mag. Close blends of multiple components allow only an estimate of an upper limit to E\_B-V\_.},
author = {Munari, U. and Zwitter, T.},
journal = {Astronomy and Astrophysics},
keywords = {EXTINCTION,INTERSTELLAR MEDIUM: ATOMS,INTERSTELLAR MEDIUM: DUST},
title = {{Equivalent width of NA I and K I lines and reddening.}},
url = {http://adsabs.harvard.edu/abs/1997A\&A...318..269M},
year = {1997},
}
@article{Smith2010,
abstract = {We present progenitor-star detections, light curves, and optical spectra of supernova (SN) 2009ip and the 2009 optical transient in UGC 2773 (U2773-OT), which were not genuine SNe. Precursor variability in the decade before outburst indicates that both of the progenitor stars were luminous blue variables (LBVs). Their pre-outburst light curves resemble the S Doradus phases that preceded giant eruptions of the prototypical LBVs $\eta$ Carinae and SN 1954J (V12 in NGC 2403), with intermediate progenitor luminosities. Hubble Space Telescope detections a decade before discovery indicate that the SN 2009ip and U2773-OT progenitors were supergiants with likely initial masses of 50-80 M sun and gsim20 M sun, respectively. Both outbursts had spectra befitting known LBVs, although in different physical states. SN 2009ip exhibited a hot LBV spectrum with characteristic speeds of 550 km s-1, plus evidence for faster material up to 5000 km s-1, resembling the slow Homunculus and fast blast wave of $\eta$ Carinae. In contrast, U2773-OT shows a forest of narrow absorption and emission lines comparable to that of S Dor in its cool state, plus [Ca II] emission and an infrared excess indicative of dust, similar to SN 2008S and the 2008 optical transient in NGC 300 (N300-OT). The [Ca II] emission is probably tied to a dusty pre-outburst environment, and is not a distinguishing property of the outburst mechanism. The LBV nature of SN 2009ip and U2773-OT may provide a critical link between historical LBV eruptions, while U2773-OT may provide a link between LBVs and the unusual dust-obscured transients SN 2008S and N300-OT. Future searches will uncover more examples of precursor LBV variability of this kind, providing key clues that may help unravel the instability driving LBV eruptions in massive stars.},
author = {Smith, Nathan and Miller, Adam and Li, Weidong and Filippenko, Alexei V. and Silverman, Jeffrey M. and Howard, Andrew W. and Nugent, Peter and Marcy, Geoffrey W. and Bloom, Joshua S. and Ghez, Andrea M. and Lu, Jessica and Yelda, Sylvana and Bernstein, Rebecca A. and Colucci, Janet E.},
doi = {10.1088/0004-6256/139/4/1451},
issn = {0004-6256},
journal = {The Astronomical Journal},
keywords = {circumstellar matter,outflows,stars: evolution,stars: mass-loss,stars: variables: general,stars: winds,supernovae: general},
month = {apr},
number = {4},
pages = {1451--1467},
title = {{DISCOVERY OF PRECURSOR LUMINOUS BLUE VARIABLE OUTBURSTS IN TWO RECENT OPTICAL TRANSIENTS: THE FITFULLY VARIABLE MISSING LINKS UGC 2773-OT AND SN 2009ip}},
url = {http://adsabs.harvard.edu/abs/2010AJ....139.1451S},
volume = {139},
year = {2010},
}
@article{2005NCimC..28..633V,
author = {Valenti, S and Cappellaro, E and {Della Valle}, M and Frontera, F and Guidorzi, C and Montanari, E},
journal = {Il Nuovo Cimento C},
month = {jul},
number = {4},
pages = {633},
title = {{SN/GRB connection: A statistical approach with BATSE and Asiago Catalogues}},
volume = {28},
year = {2005},
}
@article{Kennicutt1998,
abstract = {Measurements of H-alpha, HI, and CO distributions in 61 normal spiral galaxies are combined with published far-infrared and CO observations of 36 infrared-selected starburst galaxies, in order to study the form of the global star formation law, over the full range of gas densities and star formation rates (SFRs) observed in galaxies. The disk-averaged SFRs and gas densities for the combined sample are well represented by a Schmidt law with index N = 1.4+-0.15. The Schmidt law provides a surprisingly tight parametrization of the global star formation law, extending over several orders of magnitude in SFR and gas density. An alternative formulation of the star formation law, in which the SFR is presumed to scale with the ratio of the gas density to the average orbital timescale, also fits the data very well. Both descriptions provide potentially useful recipes for modelling the SFR in numerical simulations of galaxy formation and evolution.},
archiveprefix = {arXiv},
arxivid = {astro-ph/9712213},
author = {Kennicutt, Robert C},
doi = {10.1086/305588},
eprint = {9712213},
file = {:Users/svalenti/Documents/Mendeley Desktop/1998/The Astrophysical Journal/annurev\%2Eastro\%2E36\%2E1\%2E189.pdf:pdf},
issn = {0004637X},
journal = {The Astrophysical Journal},
number = {2},
pages = {541--552},
primaryclass = {astro-ph},
publisher = {IOP Publishing},
title = {{The Global Schmidt Law in Star‐forming Galaxies}},
url = {http://stacks.iop.org/0004-637X/498/i=2/a=541},
volume = {498},
year = {1998},
}
@article{2008MNRAS.384..107E,
author = {Elias-Rosa, N. and Benetti, S. and Turatto, M. and Cappellaro, E. and Valenti, S. and Arkharov, A.\~{}A. a. and Beckman, J. E. and {Di Paola}, a. and Dolci, M. and Filippenko, a. V. and Foley, R. J. and Krisciunas, K. and Larionov, V.\~{}M. M. and Li, W. and Meikle, W.\~{}P.\~{}S. P. S. and Pastorello, a. and Valentini, G. and Hillebrandt, W.},
doi = {10.1111/j.1365-2966.2007.12638.x},
file = {:Users/svalenti/Documents/Mendeley Desktop/2008/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2008 Elias-Rosa.pdf:pdf},
issn = {0035-8711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {1 i n t,are believed to result,dust,extinction,from the explosion,general,individual,limit after ac-,of white dwarfs when,ro d u c,sn 2002cv,sne ia,supernovae,t i o n,they reach the chandrasekhar,type ia supernovae},
month = {feb},
number = {1},
pages = {107--122},
title = {{SN 2002cv: a heavily obscured Type Ia supernova}},
url = {http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2007.12638.x},
volume = {384},
year = {2008},
}
@article{Limongi2003,
author = {Limongi, Marco and Chieffi, Alessandro},
doi = {10.1086/375703},
file = {:Users/svalenti/Documents/Mendeley Desktop/2003/The Astrophysical Journal/2003 Limongi.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {jul},
number = {1},
pages = {404--433},
title = {{Evolution, Explosion, and Nucleosynthesis of Core‐Collapse Supernovae}},
url = {http://stacks.iop.org/0004-637X/592/i=1/a=404},
volume = {592},
year = {2003},
}
@article{2007AN....328..948S,
author = {Stanishev, V},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/Astronomische Nachrichten/2007 Stanishev.pdf:pdf},
journal = {Astronomische Nachrichten},
month = {nov},
number = {9},
pages = {948},
title = {{Correcting second-order contamination in low-resolution spectra}},
volume = {328},
year = {2007},
}
@article{Quimby2007,
author = {Quimby, Robert M and Wheeler, J Craig and Hoflich, Peter and Akerlof, Carl W and Brown, Peter J and Rykoff, Eli S},
doi = {10.1086/520532},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/The Astrophysical Journal/2007 Quimby.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {sep},
number = {2},
pages = {1093--1107},
title = {{SN 2006bp: Probing the Shock Breakout of a Type II‐P Supernova}},
url = {http://stacks.iop.org/0004-637X/666/i=2/a=1093},
volume = {666},
year = {2007},
}
@article{2011MNRAS.417..261I,
author = {Inserra, C and Turatto, M and Pastorello, A and Benetti, S and Cappellaro, E and Pumo, M L and Zampieri, L and Agnoletto, I and Bufano, F and Botticella, M T and {Della Valle}, M and Elias-Rosa, N and Iijima, T and Spiro, S and Valenti, S},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/Monthly Notices of the Royal Astronomical Society/MNRAS-2011-Inserra-261-79.pdf:pdf},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {oct},
number = {1},
pages = {261--279},
title = {{The Type IIP SN 2007od in UGC 12846: from a bright maximum to dust formation in the nebular phase}},
volume = {417},
year = {2011},
}
@article{1996MNRAS.283....1T,
author = {Turatto, M and Benetti, S and Cappellaro, E and Danziger, I J and {Della Valle}, M and Gouiffes, C and Mazzali, P.\~{}A. and Patat, F},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {nov},
pages = {1--17},
title = {{The properties of the peculiar type Ia supernova 1991bg. I. Analysis and discussion of two years of observations.}},
volume = {283},
year = {1996},
}
@article{2010ApJ...719.1445M,
author = {Moriya, Takashi and Tominaga, Nozomu and Tanaka, Masaomi and Nomoto, Ken'ichi and Sauer, Daniel N and Mazzali, Paolo A and Maeda, Keiichi and Suzuki, Tomoharu},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/The Astrophysical Journal/2010 Moriya.pdf:pdf},
journal = {The Astrophysical Journal},
month = {aug},
number = {2},
pages = {1445--1453},
title = {{Fallback Supernovae: A Possible Origin of Peculiar Supernovae with Extremely Low Explosion Energies}},
volume = {719},
year = {2010},
}
@article{Pan2012,
archiveprefix = {arXiv},
arxivid = {1111.3648v1},
author = {Pan, Tony and Loeb, Abraham and Kasen, Daniel},
doi = {10.1111/j.1365-2966.2012.21030.x},
eprint = {1111.3648v1},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2012 Pan.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {galaxies,star clusters,supernovae},
month = {jul},
number = {3},
pages = {2203--2208},
title = {{Pair-instability supernovae via collision runaway in young dense star clusters}},
url = {http://onlinelibrary.wiley.com/doi/10.1111/j.1365-2966.2012.21030.x/full http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2012.21030.x},
volume = {423},
year = {2012},
}
@article{Inserra2013,
abstract = {Context. Core-collapse Supernovae (CC-SNe) descend from progenitors more massive than about 8 M⊙. Because of the young age of the progenitors, the ejecta may eventually interact with the circumstellar medium (CSM) via highly energetic processes detectable in the radio, X-ray, ultraviolet (UV) and, sometimes, in the optical domains. Aims: In this paper we present ultraviolet, optical and near infrared observations of five Type II SNe, namely SNe 2009dd, 2007pk, 2010aj, 1995ad, and 1996W. Together with few other SNe they form a group of moderately luminous Type II events. We investigate the photometric similarities and differences among these bright objects. We also attempt to characterise them by analysing the spectral evolutions, in order to find some traces of CSM-ejecta interaction. Methods: We collected photometry and spectroscopy with several telescopes in order to construct well-sampled light curves and spectral evolutions from the photospheric to the nebular phases. Both photometry and spectroscopy indicate a degree of heterogeneity in this sample. Modelling the data of SNe 2009dd, 2010aj and 1995ad allows us to constrain the explosion parameters and the properties of the progenitor stars. Results: The light curves have luminous peak magnitudes (-16.95 < MB < -18.70). The ejected masses of 56Ni for three SNe span a wide range of values (2.8 × 10-2 M⊙ < M(56Ni)< 1.4 × 10-1 M⊙), while for a fourth (SN 2010aj) we could determine a stringent upper limit (7 × 10-3 M⊙). Clues of interaction, such as the presence of high velocity (HV) features of the Balmer lines, are visible in the photospheric spectra of SNe 2009dd and 1996W. For SN 2007pk we observe a spectral transition from a Type IIn to a standard Type II SN. Modelling the observations of SNe 2009dd, 2010aj and 1995ad with radiation hydrodynamics codes, we infer kinetic plus thermal energies of about 0.2-0.5 foe, initial radii of 2-5 × 1013 cm and ejected masses of \~{}5.0-9.5 M⊙. Conclusions: These values suggest moderate-mass, super-asymptotic giant branch (SAGB) or red super-giants (RSG) stars as SN precursors, in analogy with other luminous Type IIP SNe 2007od and 2009bw. This paper is based on observations made with the following facilities: the Italian Telescopio Nazionale Galileo, the Liverpool Telescope, the North Optical Telescope, the William Herschel (La Palma, Spain), the Copernico telescope (Asiago, Italy), the Calar Alto Observatory (Sierra de los Filabres, Spain), the orbital telescope Swift (NASA), the Hale Telescope at the Palomar Observatory, and the ESO Telescopes at the La Silla and Paranal Observatories.The spectra (FITS files) are available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/555/A142},
author = {Inserra, C. and Pastorello, A. and Turatto, M. and Pumo, M. L. and Benetti, S. and Cappellaro, E. and Botticella, M. T. and Bufano, F. and Elias-Rosa, N. and Harutyunyan, A. and Taubenberger, S. and Valenti, S. and Zampieri, L.},
doi = {10.1051/0004-6361/201220496},
file = {:Users/svalenti/Documents/Mendeley Desktop/2013/Astronomy \& Astrophysics/aa20496-12.pdf:pdf},
issn = {0004-6361},
journal = {Astronomy \& Astrophysics},
keywords = {supernovae: general,supernovae: individual: SN 1995ad,supernovae: individual: SN 1996W,supernovae: individual: SN 2007pk,supernovae: individual: SN 2009dd,supernovae: individual: SN 2010aj},
month = {may},
title = {{Moderately luminous Type II supernovae}},
url = {http://adsabs.harvard.edu/abs/2013A\&A...555A.142I},
volume = {555},
year = {2013},
}
@article{ValentiSATel4958,
abstract = {We report a spectroscopic classification of LSQ13vy located at ra= 16:06:55.85 dec=+03:00:15.1. A spectrum (range 350-1000 nm) obtained robotically on Apr. 06.70 UT with the FLOYDS spectrograph at Faulkes Telescope South at Siding Spring, shows it to be a SN type Ia several days before maxium at a redshift of 0.032. Comparisons with a library of supernova spectra using the Superfit SN spectral identification code (Howell et al.},
author = {Valenti, S. and Graham, M. L. and Howell, D. A. and Sand, D. and Parrent, J. T. and Hadjiyska, E. and Walker, E. S. and Rabinowitz, D. and Baltay, C. and Ellman, N. and McKinnon, R. and Feindt, U. and Nugent, P.},
journal = {The Astronomer's Telegram},
keywords = {Optical,Supernovae},
title = {{Classification of LSQ Supernova LSQ13vy with FLOYDS at Faulkes Telescope South}},
url = {http://adsabs.harvard.edu/abs/2013ATel.4958....1V},
year = {2013},
}
@article{Thielemann1996,
author = {Thielemann, Friedrich-Karl and Nomoto, Ken'ichi and Hashimoto, Masa-Aki},
doi = {10.1086/176980},
file = {:Users/svalenti/Documents/Mendeley Desktop/1996/The Astrophysical Journal/1996 Thielemann.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {mar},
pages = {408},
title = {{Core-Collapse Supernovae and Their Ejecta}},
url = {http://adsabs.harvard.edu/doi/10.1086/176980},
volume = {460},
year = {1996},
}
@article{Liu2012,
abstract = {The explosion of a Type Ia supernova, SN 2011ef, in the nearby Pinwheel galaxy (M101 at 6.4 Mpc) provides an opportunity to study pre-explosion images and search for the progenitor, which should consist of a white dwarf (WD), possibly surrounded by an accretion disk, in orbit with another star. We report on our use of deep Chandra observations to limit the luminosity and temperature of the pre-explosion white dwarf (WD). It is found that if the spectrum was a blackbody, then WDs of highest possible temperatures and luminosities are excluded but, even if the WD was emitting at the Eddington luminosity, values of kT less than roughly 60 eV are permitted. This allows the progenitor to be an accreting nuclear-burning WD with an expanded photosphere. Pre-SN HST observations were used to derive a lower limit of about 10 eV for the expanded photosphere. Li et al.$\backslash$, (2011) have already ruled out the possibility of a giant donor. We consider the combined emission from the WD, disk, and donor, and find that even the combined emission from a bright subgiant, WD and disk would not likely have been observed prior to explosion, and neither would some local candidates for the nuclear-burning WD model.},
archiveprefix = {arXiv},
arxivid = {1110.2506},
author = {Liu, Jifeng and {Di Stefano}, Rosanne and Wang, Tao and Moe, Maxwell},
doi = {10.1088/0004-637X/749/2/141},
eprint = {1110.2506},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/The Astrophysical Journal/2012 Liu.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {apr},
number = {2},
pages = {141},
title = {{On the Nature of the Progenitor of the Type Ia SN2011fe in M101}},
url = {http://arxiv.org/abs/1110.2506 http://stacks.iop.org/0004-637X/749/i=2/a=141?key=crossref.0157076c5a1bc66231c54fd558449a08},
volume = {749},
year = {2012},
}
@article{Gamezo2005,
author = {Gamezo, Vadim N. and Khokhlov, Alexei M. and Oran, Elaine S.},
doi = {10.1086/428767},
file = {:Users/svalenti/Documents/Mendeley Desktop/2005/The Astrophysical Journal/2005 Gamezo.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {apr},
number = {1},
pages = {337--346},
title = {{Three‐dimensional Delayed‐Detonation Model of Type Ia Supernovae}},
url = {http://stacks.iop.org/0004-637X/623/i=1/a=337},
volume = {623},
year = {2005},
}
@article{2009ApJ...699.1365S,
author = {Shen, Ken J. and Bildsten, Lars},
doi = {10.1088/0004-637X/699/2/1365},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/The Astrophysical Journal/2009 Shen.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {binaries,cataclysmic variables,close,general,novae,supernovae,white dwarfs},
month = {jul},
number = {2},
pages = {1365--1373},
title = {{Unstable Helium Shell Burning on Accreting White Dwarfs}},
url = {http://stacks.iop.org/0004-637X/699/i=2/a=1365?key=crossref.15a1a2e9880bdcadd2b8d41e13da7945},
volume = {699},
year = {2009},
}
@article{2008ATel.1368....1P,
author = {Pooley, David and Soderberg, Alicia},
journal = {The Astronomer's Telegram},
month = {jan},
pages = {1},
title = {{Chandra Detection of the Type Ibc SNe 2007uy and 2008D in NGC 2770}},
volume = {1368},
year = {2008},
}
@article{Mazzali2005,
abstract = {Type Ic supernovae, the explosions after the core collapse of massive stars that have previously lost their hydrogen and helium envelopes, are particularly interesting because of their link with long-duration gamma ray bursts. Although indications exist that these explosions are aspherical, direct evidence has been missing. Late-time observations of supernova SN 2003jd, a luminous type Ic supernova, provide such evidence. Recent Subaru and Keck spectra reveal double-peaked profiles in the nebular lines of neutral oxygen and magnesium. These profiles are different from those of known type Ic supernovae, with or without a gamma ray burst, and they can be understood if SN 2003jd was an aspherical axisymmetric explosion viewed from near the equatorial plane. If SN 2003jd was associated with a gamma ray burst, we missed the burst because it was pointing away from us.},
author = {Mazzali, Paolo a and Kawabata, Koji S and Maeda, Keiichi and Nomoto, Ken'ichi and Filippenko, Alexei V and Ramirez-Ruiz, Enrico and Benetti, Stefano and Pian, Elena and Deng, Jinsong and Tominaga, Nozomu and Ohyama, Youichi and Iye, Masanori and Foley, Ryan J and Matheson, Thomas and Wang, Lifan and Gal-Yam, Avishay},
doi = {10.1126/science.1111384},
file = {:Users/svalenti/Documents/Mendeley Desktop/2005/Science (New York, N.Y.)/2005 Mazzali.pdf:pdf},
issn = {1095-9203},
journal = {Science (New York, N.Y.)},
month = {may},
number = {5726},
pages = {1284--7},
pmid = {15919986},
title = {{An asymmetric energetic type Ic supernova viewed off-axis, and a link to gamma ray bursts.}},
url = {http://www.ncbi.nlm.nih.gov/pubmed/15919986},
volume = {308},
year = {2005},
}
@article{2004AJ....128.3034K,
author = {Krisciunas, Kevin and Suntzeff, Nicholas B and Phillips, Mark M and Candia, Pablo and Prieto, Jos\'{e} Luis and Antezana, Roberto and Chassagne, Robin and Chen, Hsiao-Wen and Dickinson, Mark and Eisenhardt, Peter R and Espinoza, Juan and Garnavich, Peter M and Gonz\'{a}lez, David and Harrison, Thomas E and Hamuy, Mario and Ivanov, Vladimir D and Krzeminski, Wojtek and Kulesa, Craig and McCarthy, Patrick and Moro-Mart\'{\i}n, Amaya and Muena, C\'{e}sar and Noriega-Crespo, Alberto and Persson, S.\~{}E. and Pinto, Philip A and Roth, Miguel and Rubenstein, Eric P and Stanford, S Adam and Stringfellow, Guy S and Zapata, Abner and Porter, Alain and Wischnjewsky, Marina},
journal = {The Astronomical Journal},
month = {dec},
number = {6},
pages = {3034--3052},
title = {{Optical and Infrared Photometry of the Type Ia Supernovae 1991T, 1991bg, 1999ek, 2001bt, 2001cn, 2001cz, and 2002bo}},
volume = {128},
year = {2004},
}
@article{Cushing2004,
abstract = {We describe an IDL-based package for the reduction of spectral data obtained with SpeX, a medium-resolution, 0.8-5.5 $\mu$m cross-dispersed spectrograph and imager for the NASA Infrared Telescope Facility. The package, called Spextool, carries out all the procedures necessary to produce fully reduced spectra including preparation of calibration frames, processing and extraction of spectra from science frames, wavelength calibration of spectra, and flux calibration of spectra. The package incorporates an ``optimal extraction'' algorithm for point-source data and also generates realistic error arrays associated with the extracted spectra. Because it is fairly quick and easy to use, requiring minimal user interaction, Spextool can be run by observers at the telescope to estimate the signal-to-noise ratio of their data. We describe the procedures incorporated into Spextool and show examples of extracted spectra.},
author = {Cushing, Michael C. and Vacca, William D. and Rayner, John T.},
doi = {10.1086/382907},
issn = {0004-6280},
journal = {Publications of the Astronomical Society of the Pacific},
keywords = {Instrumentation: Spectrographs,Methods: Data Analysis,Techniques: Spectroscopic},
month = {apr},
number = {818},
pages = {362--376},
title = {{Spextool: A Spectral Extraction Package for SpeX, a 0.8–5.5 Micron Cross‐Dispersed Spectrograph}},
url = {http://adsabs.harvard.edu/abs/2004PASP..116..362C},
volume = {116},
year = {2004},
}
@article{2007ApJ...666.1116S,
annote = {14 pages, 4 color figs. accepted by ApJ. expanded from original version, but original conclusions unchanged},
author = {Smith, Nathan and Li, Weidong and Foley, Ryan J and Wheeler, J Craig and Pooley, David and Chornock, Ryan and Filippenko, Alexei V and Silverman, Jeffrey M and Quimby, Robert and Bloom, Joshua S and Hansen, Charles},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/The Astrophysical Journal/2007 Smith.pdf:pdf},
journal = {The Astrophysical Journal},
month = {sep},
number = {2},
pages = {1116--1128},
title = {{SN 2006gy: Discovery of the Most Luminous Supernova Ever Recorded, Powered by the Death of an Extremely Massive Star like $\eta$ Carinae}},
volume = {666},
year = {2007},
}
@article{Mazzali2001,
author = {Mazzali, Paolo A. and Nomoto, Ken’ichi Ken'ichi and Patat, Ferdinando and Maeda, Keiichi},
doi = {10.1086/322420},
file = {:Users/svalenti/Documents/Mendeley Desktop/2001/The Astrophysical Journal/2001 Mazzali.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {oct},
number = {2},
pages = {1047--1053},
title = {{The Nebular Spectra of the Hypernova SN 1998bw and Evidence for Asymmetry}},
url = {http://stacks.iop.org/0004-637X/559/i=2/a=1047},
volume = {559},
year = {2001},
}
@article{2010MNRAS.404..981M,
author = {Maguire, K and di Carlo, E and Smartt, S.\~{}J. and Pastorello, A and Tsvetkov, D Yu. and Benetti, S and Spiro, S and Arkharov, A.\~{}A. and Beccari, G and Botticella, M T and Cappellaro, E and Cristallo, S and Dolci, M and Elias-Rosa, N and Fiaschi, M and Gorshanov, D and Harutyunyan, A and Larionov, V.\~{}M. and Navasardyan, H and Pietrinferni, A and Raimondo, G and di Rico, G and Valenti, S and Valentini, G and Zampieri, L},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2010 Maguire.pdf:pdf},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {may},
number = {2},
pages = {981--1004},
title = {{Optical and near-infrared coverage of SN 2004et: physical parameters and comparison with other Type IIP supernovae}},
volume = {404},
year = {2010},
}
@article{Herrmann2008,
abstract = {As the first step to determine disk mass-to-light ratios for normal spiral galaxies, we present the results of an imaging survey for planetary nebulae (PNe) in six nearby, face-on systems: IC 342, M74 (NGC 628), M83 (NGC 5236), M94 (NGC 4736), NGC 5068, and NGC 6946. Using Blanco/Mosaic II and WIYN/OPTIC, we identify 165, 153, 241, 150, 19, and 71 PN candidates, respectively, and use the planetary nebula luminosity function (PNLF) to obtain distances. For M74 and NGC 5068, our distances of 8.6+/-0.3 and 5.4+0.2-0.4 Mpc are the first reliable estimates to these objects; for IC 342 (3.5+/-0.3 Mpc), M83 (4.8+/-0.1 Mpc), M94 (4.4+0.1-0.2 Mpc), and NGC 6946 (6.1+/-0.6 Mpc) our values agree well with those in the literature. In the larger systems, we find no evidence for any systematic change in the PNLF with galactic position, although we do see minor field-to-field variations in the luminosity function. In most cases, these changes do not affect the measurement of distance, but in one case the fluctuations result in a \~{}0.2 mag shift in the location of the PNLF cutoff. We discuss the possible causes of these small-scale changes, including internal extinction in the host galaxies and age/metallicity changes in the underlying stellar population.},
author = {Herrmann, Kimberly A. and Ciardullo, Robin and Feldmeier, John J. and Vinciguerra, Matt},
doi = {10.1086/589920},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {Cosmology: Distance Scale,Galaxies: Distances and Redshifts,ISM: Planetary Nebulae: General},
month = {aug},
number = {2},
pages = {630--643},
title = {{Planetary Nebulae in Face‐On Spiral Galaxies. I. Planetary Nebula Photometry and Distances}},
url = {http://adsabs.harvard.edu/abs/2008ApJ...683..630H},
volume = {683},
year = {2008},
}
@article{Patat2001,
author = {Patat, Ferdinando and Cappellaro, Enrico and Danziger, John and Mazzali, Paolo A and Sollerman, Jesper and Augusteijn, Thomas and Brewer, James and Doublier, Vanessa and Gonzalez, Jean Francois and Hainaut, Olivier and Lidman, Chris and Leibundgut, Bruno and Nomoto, Ken’ichi and Nakamura, Takayoshi and Spyromilio, Jason and Rizzi, Luca and Turatto, Massimo and Walsh, Jeremy and Galama, Titus J and van Paradijs, Jan and Kouveliotou, Chryssa and Vreeswijk, Paul M and Frontera, Filippo and Masetti, Nicola and Palazzi, Eliana and Pian, Elena},
doi = {10.1086/321526},
file = {:Users/svalenti/Documents/Mendeley Desktop/2001/The Astrophysical Journal/2001 Patat.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {jul},
number = {2},
pages = {900--917},
title = {{The Metamorphosis of SN 1998bw}},
url = {http://stacks.iop.org/0004-637X/555/i=2/a=900},
volume = {555},
year = {2001},
}
@article{2006PASP..118..791B,
author = {Branch, David and Jeffery, David J and Young, Timothy R and Baron, E},
journal = {The Publications of the Astronomical Society of the Pacific},
month = {jun},
number = {8},
pages = {791--796},
title = {{Hydrogen in Type Ic Supernovae?}},
volume = {118},
year = {2006},
}
@article{Elmhamdi2004,
author = {Elmhamdi, A and Danziger, I J and Cappellaro, E and {Della Valle}, M. and Gouiffes, C and Phillips, M M and Turatto, M},
doi = {10.1051/0004-6361:20041318},
file = {:Users/svalenti/Documents/Mendeley Desktop/2004/Astronomy and Astrophysics/2004 Elmhamdi.pdf:pdf},
issn = {0004-6361},
journal = {Astronomy and Astrophysics},
keywords = {general,individual,photometric,sn ib 1990i,spectroscopic,stars,supernovae,techniques},
month = {nov},
number = {3},
pages = {963--977},
title = {{SN Ib 1990I: Clumping and dust in the ejecta?}},
url = {http://www.edpsciences.org/10.1051/0004-6361:20041318},
volume = {426},
year = {2004},
}
@article{2012A&A...546A..28J,
author = {Jerkstrand, A and Fransson, C and Maguire, K and Smartt, S and Ergon, M and Spyromilio, J},
journal = {Astronomy and Astrophysics},
month = {oct},
pages = {28},
title = {{The progenitor mass of the Type IIP supernova SN 2004et from late-time spectral modeling}},
volume = {546},
year = {2012},
}
@article{2009ApJ...692.1131T,
annote = {13 pages, 10 figures, Accepted for publication in ApJ, typos corrected},
author = {Tanaka, Masaomi and Tominaga, Nozomu and Nomoto, Ken'ichi and Valenti, S and Sahu, D.\~{}K. and Minezaki, T and Yoshii, Y and Yoshida, M and Anupama, G.\~{}C. and Benetti, S and Chincarini, G and {Della Valle}, M and Mazzali, P.\~{}A. and Pian, E},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/The Astrophysical Journal/2009 Tanaka.pdf:pdf},
journal = {The Astrophysical Journal},
month = {feb},
number = {2},
pages = {1131--1142},
title = {{Type Ib Supernova 2008D Associated With the Luminous X-Ray Transient 080109: An Energetic Explosion of a Massive Helium Star}},
volume = {692},
year = {2009},
}
@article{2009ApJ...706.1078N,
author = {Newman, Andrew B and Treu, Tommaso and Ellis, Richard S and Sand, David J and Richard, Johan and Marshall, Philip J and Capak, Peter and Miyazaki, Satoshi},
journal = {The Astrophysical Journal},
month = {dec},
number = {2},
pages = {1078--1094},
title = {{The Distribution of Dark Matter Over Three Decades in Radius in the Lensing Cluster Abell 611}},
volume = {706},
year = {2009},
}
@article{2008MNRAS.383.1485V,
annote = {From Duplicate 1 ( The broad-lined Type Ic supernova 2003jd - Valenti, S; Benetti, S; Cappellaro, E; Patat, F; Mazzali, P; Turatto, M; Hurley, K; Maeda, K; Gal-Yam, A; Foley, R J; Filippenko, A V; Pastorello, A; Challis, P; Frontera, F; Harutyunyan, A; Iye, M; Kawabata, K; Kirshner, R P; Li, W; Lipkin, Y M; Matheson, T; Nomoto, K; Ofek, E O; Ohyama, Y; Pian, E; Poznanski, D; Salvo, M; Sauer, D N; Schmidt, B P; Soderberg, A; Zampieri, L ) 19 pages, 19 figures, Accepted for publication in MNRAS},
author = {Valenti, S. and Benetti, S. and Cappellaro, E. and Patat, F. and Mazzali, P. and Turatto, M. and Hurley, K. and Maeda, K. and Gal-Yam, a. and Foley, R. J. and Filippenko, a. V. and Pastorello, a. and Challis, P. and Frontera, F. and Harutyunyan, a. and Iye, M. and Kawabata, K. and Kirshner, R. P. and Li, W. and Lipkin, Y. M. and Matheson, T. and Nomoto, K. and Ofek, E. O. and Ohyama, Y. and Pian, E. and Poznanski, D. and Salvo, M. and Sauer, D. N. and Schmidt, B. P. and Soderberg, a. and Zampieri, L.},
doi = {10.1111/j.1365-2966.2007.12647.x},
file = {:Users/svalenti/Documents/Mendeley Desktop/2008/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2008 Valenti.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {2003jd,general,individual,supernovae},
month = {feb},
number = {4},
pages = {1485--1500},
title = {{The broad-lined Type Ic supernova 2003jd}},
url = {http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2007.12647.x},
volume = {383},
year = {2008},
}
@article{Gal-Yam2011,
author = {Gal-Yam, Avishay and Kasliwal, Mansi M. and Arcavi, Iair and Green, Yoav and Yaron, Ofer and Ben-Ami, Sagi and Xu, Dong and Sternberg, Assaf and Quimby, Robert M. and Kulkarni, Shrinivas R. and Ofek, Eran O. and Walters, Richard and Nugent, Peter E. and Poznanski, Dovi and Bloom, Joshua S. and Cenko, S. Bradley and Filippenko, Alexei V. and Li, Weidong and Silverman, Jeffrey M. and Walker, Emma S. and Sullivan, Mark and Maguire, K. and {Andrew Howell}, D. and Mazzali, Paolo a. and Frail, Dale a. and Bersier, David and James, Phil a. and Akerlof, C. W. and Yuan, Fang and Law, Nicholas and Fox, Derek B. and Gehrels, Neil},
doi = {10.1088/0004-637X/736/2/159},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/The Astrophysical Journal/2011 Gal-Yam.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {challenging for existing systems,color figures,general,individual,initial progress in securing,machine-readable table,online-only material,optical transients was made,ptf10vdl,supernovae,very early-time observations of},
month = {aug},
number = {2},
pages = {159},
title = {{Real-Time Detection and Rapid Multiwavelength Follow-Up Observations of a Highly Subluminous Type Ii-P Supernova From the Palomar Transient Factory Survey}},
url = {http://stacks.iop.org/0004-637X/736/i=2/a=159?key=crossref.a132816a7f17a749baf3f5f45d932fff},
volume = {736},
year = {2011},
}
@article{Valenti2013,
abstract = {CBET 3609 available at Central Bureau for Astronomical Telegrams.},
author = {Valenti, S. and Sand, D. and Howell, D. A. and Graham, M. L. and Parrent, J. T. and Zheng, W. and Cenko, B. and Dhungana, G. and Vinko, J. and Wheeler, J. C. and Silverman, J. M. and Kehoe, R. and Ferrante, F. V. and Marion, G. H. and Quimby, R. and Yuan, F. and Akerlof, C.},
journal = {Central Bureau Electronic Telegrams},
title = {{Supernova 2013ej in M74 = Psn J01364816+1545310}},
url = {http://adsabs.harvard.edu/abs/2013CBET.3609....1V},
year = {2013},
}
@article{2010ARA&A..48..673F,
author = {Freedman, Wendy L and Madore, Barry F},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/Annual Review of Astronomy \{\&\} Astrophysics/2010 Freedman.pdf:pdf},
journal = {Annual Review of Astronomy \{\&\} Astrophysics},
month = {sep},
pages = {673--710},
title = {{The Hubble Constant}},
volume = {48},
year = {2010},
}
@article{Blinnikov2002,
abstract = {Numerical modeling of shock breakout in compact presupernovae of type Ib/c is done by two independent methods. Peak color temperatures reach 4 to 8 million K for explosion energies 1 to 9 foe with a typical local time-scale of 0.03 seconds. In the obverver's frame the burst is smeared over few seconds due to light travel time correction R/c.},
archiveprefix = {arXiv},
arxivid = {astro-ph/0212564},
author = {Blinnikov, S I and Nadyozhin, D K and Woosley, S E and Sorokina, E I},
eprint = {0212564},
file = {:Users/svalenti/Documents/Mendeley Desktop/2002/Unknown/2002 Blinnikov.pdf:pdf},
month = {dec},
pages = {4},
primaryclass = {astro-ph},
title = {{Shock breakouts in SNe Ib/c}},
url = {http://arxiv.org/abs/astro-ph/0212564},
year = {2002},
}
@article{Arcavi2012,
abstract = {We present R-band light curves of Type II supernovae (SNe) from the Caltech Core-Collapse Project (CCCP). With the exception of interacting (Type IIn) SNe and rare events with long rise times, we find that most light curve shapes belong to one of three apparently distinct classes: plateau, slowly declining, and rapidly declining events. The last class is composed solely of Type IIb SNe which present similar light curve shapes to those of SNe Ib, suggesting, perhaps, similar progenitor channels. We do not find any intermediate light curves, implying that these subclasses are unlikely to reflect variance of continuous parameters, but rather might result from physically distinct progenitor systems, strengthening the suggestion of a binary origin for at least some stripped SNe. We find a large plateau luminosity range for SNe IIP, while the plateau lengths seem rather uniform at approximately 100 days. As analysis of additional CCCP data goes on and larger samples are collected, demographic studies of core-collapse SNe will likely continue to provide new constraints on progenitor scenarios.},
author = {Arcavi, Iair and Gal-Yam, Avishay and Cenko, S. Bradley and Fox, Derek B. and Leonard, Douglas C. and Moon, Dae-Sik and Sand, David J. and Soderberg, Alicia M. and Kiewe, Michael and Yaron, Ofer and Becker, Adam B. and Scheps, Raphael and Birenbaum, Gali and Chamudot, Daniel and Zhou, Jonathan},
doi = {10.1088/2041-8205/756/2/L30},
issn = {2041-8205},
journal = {The Astrophysical Journal},
keywords = {supernovae: general},
month = {sep},
number = {2},
pages = {L30},
title = {{CALTECH CORE-COLLAPSE PROJECT (CCCP) OBSERVATIONS OF TYPE II SUPERNOVAE: EVIDENCE FOR THREE DISTINCT PHOTOMETRIC SUBTYPES}},
url = {http://adsabs.harvard.edu/abs/2012ApJ...756L..30A},
volume = {756},
year = {2012},
}
@article{2007ApJ...657L.105F,
author = {Foley, Ryan J and Smith, Nathan and Ganeshalingam, Mohan and Li, Weidong and Chornock, Ryan and Filippenko, Alexei V},
journal = {The Astrophysical Journal},
month = {mar},
number = {2},
pages = {L105--------L108},
title = {{SN 2006jc: A Wolf-Rayet Star Exploding in a Dense He-rich Circumstellar Medium}},
volume = {657},
year = {2007},
}
@article{Bufano2009,
abstract = {We present the entire sample of ultraviolet (UV) spectra of supernovae (SNe) obtained with the Ultraviolet/Optical Telescope (UVOT) on board the Swift satellite during the first two years of observations (2005/2006). A total of 29 UV-grism and 22 V-grism spectra of nine SNe have been collected, of which six are thermonuclear (Type Ia) and three core-collapse (Type Ibc/II) SNe. All the spectra have been obtained during the photospheric phase. After a comparison of the spectra of our sample with those in the literature (SNe 1992A, 1990N, and 1999em), we confirm some degree of diversity in the UV emission of Type Ia SNe and a greater homogeneity in the Type II Plateau SN sample. Signatures of interaction between the ejecta and the circumstellar environment have been found in the UV spectrum of SN 2006jc, the only SN Type Ib/c for which UVOT grism data are available. Currently, Swift UVOT is the best suited instrument for early SN studies in the UV due to its fast response and flexible scheduling capabilities. However, in order to increase the quality of the data and significantly improve our understanding of the UV properties of SNe and to fully maximize the scientific potential of UVOT grism observations, a larger investment in observing time and longer exposures are needed.},
author = {Bufano, F. and Immler, S. and Turatto, M. and Landsman, W. and Brown, P. and Benetti, S. and Cappellaro, E. and Holland, S. T. and Mazzali, P. and Milne, P. and Panagia, N. and Pian, E. and Roming, P. and Zampieri, L. and Breeveld, A. A. and Gehrels, N.},
doi = {10.1088/0004-637X/700/2/1456},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/The Astrophysical Journal/apj\_700\_2\_1456.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {supernovae: general,supernovae: individual: SNe 2005am 2005cf 2005cs 2,ultraviolet: general},
month = {aug},
number = {2},
pages = {1456--1472},
title = {{ULTRAVIOLET SPECTROSCOPY OF SUPERNOVAE: THE FIRST TWO YEARS OF SWIFT OBSERVATIONS}},
url = {http://adsabs.harvard.edu/abs/2009ApJ...700.1456B},
volume = {700},
year = {2009},
}
@article{Pignata2004,
author = {Pignata, G. and Patat, F. and Benetti, S. and Blinnikov, S. and Hillebrandt, W. and Kotak, R. and Leibundgut, B. and Mazzali, P. a. and Meikle, P. and Qiu, Y. and Ruiz-Lapuente, P. and Smartt, S. J. and Sorokina, E. and Stritzinger, M. and Stehle, M. and Turatto, M. and Marsh, T. and Martin-Luis, F. and McBride, N. and Mendez, J. and Morales-Rueda, L. and Narbutis, D. and Street, R.},
doi = {10.1111/j.1365-2966.2004.08308.x},
file = {:Users/svalenti/Documents/Mendeley Desktop/2004/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2004 Pignata.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {general,individual,photometric,supernovae,techniques},
month = {nov},
number = {1},
pages = {178--190},
title = {{Photometric observations of the Type Ia SN 2002er in UGC 10743}},
url = {http://doi.wiley.com/10.1111/j.1365-2966.2004.08308.x},
volume = {355},
year = {2004},
}
@article{2011arXiv1102.3511S,
author = {Suh, Hyewon and Yoon, Sung-chul and Jeong, Hyunjin and Yi, Sukyoung K.},
doi = {10.1088/0004-637X/730/2/110},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/The Astrophysical Journal/arXiv 2011 Suh.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {apr},
number = {2},
pages = {110},
title = {{EARLY-TYPE HOST GALAXIES OF TYPE II AND Ib SUPERNOVAE}},
url = {http://stacks.iop.org/0004-637X/730/i=2/a=110?key=crossref.0f48de4dc909d8920fa23c29da10d38a},
volume = {730},
year = {2011},
}
@article{2011MNRAS.412.2735T,
abstract = {SN 2009dc shares similarities with normal Type Ia supernovae, but is clearly overluminous, with a (pseudo-bolometric) peak luminosity of log(L) = 43.47 [erg/s]. Its light curves decline slowly over half a year after maximum light, and the early-time near-IR light curves show secondary maxima, although the minima between the first and second peaks are not very pronounced. Bluer bands exhibit an enhanced fading after \~{}200 d, which might be caused by dust formation or an unexpectedly early IR catastrophe. The spectra of SN 2009dc are dominated by intermediate-mass elements and unburned material at early times, and by iron-group elements at late phases. Strong C II lines are present until \~{}2 weeks past maximum, which is unprecedented in thermonuclear SNe. The ejecta velocities are significantly lower than in normal and even subluminous SNe Ia. No signatures of CSM interaction are found in the spectra. Assuming that the light curves are powered by radioactive decay, analytic modelling suggests that SN 2009dc produced \~{}1.8 solar masses of 56Ni assuming the smallest possible rise time of 22 d. Together with a derived total ejecta mass of \~{}2.8 solar masses, this confirms that SN 2009dc is a member of the class of possible super-Chandrasekhar-mass SNe Ia similar to SNe 2003fg, 2006gz and 2007if. A study of the hosts of SN 2009dc and other superluminous SNe Ia reveals a tendency of these SNe to explode in low-mass galaxies. A low metallicity of the progenitor may therefore be an important pre-requisite for producing superluminous SNe Ia. We discuss a number of explosion scenarios, ranging from super-Chandrasekhar-mass white-dwarf progenitors over dynamical white-dwarf mergers and Type I 1/2 SNe to a core-collapse origin of the explosion. None of the models seem capable of explaining all properties of SN 2009dc, so that the true nature of this SN and its peers remains nebulous.},
archiveprefix = {arXiv},
arxivid = {1011.5665},
author = {Taubenberger, S. and Benetti, S. and Childress, M. and Pakmor, R. and Hachinger, S. and Mazzali, P.\~{}A. A. and Stanishev, V. and Elias-Rosa, N. and Agnoletto, I. and Bufano, F. and Ergon, M. and Harutyunyan, A. and Inserra, C. and Kankare, E. and Kromer, M. and Navasardyan, H. and Nicolas, J. and Pastorello, A. and Prosperi, E. and Salgado, F. and Sollerman, J. and Stritzinger, M. and Turatto, M. and Valenti, S. and Hillebrandt, W.},
doi = {10.1111/j.1365-2966.2010.18107.x},
eprint = {1011.5665},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2011 Taubenberger-1.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {general,individual,sn 2009dc,supernovae},
month = {apr},
number = {4},
pages = {2735--2762},
title = {{High luminosity, slow ejecta and persistent carbon lines: SN 2009dc challenges thermonuclear explosion scenarios}},
url = {http://arxiv.org/abs/1011.5665 http://onlinelibrary.wiley.com/doi/10.1111/j.1365-2966.2010.18107.x/full http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2010.18107.x},
volume = {412},
year = {2011},
}
@article{Parrent2011,
abstract = {One of the major differences between various explosion scenarios of Type Ia supernovae (SNe Ia) is the remaining amount of unburned (C+O) material and its velocity distribution within the expanding ejecta. While oxygen absorption features are not uncommon in the spectra of SNe Ia before maximum light, the presence of strong carbon absorption has been reported only in a minority of objects, typically during the pre-maximum phase. The reported low frequency of carbon detections may be due to low signal-to-noise data, low abundance of unburned material, line blending between C II $\lambda$6580 and Si II $\lambda$6355, ejecta temperature differences, asymmetrical distribution effects, or a combination of these. However, a survey of published pre-maximum spectra reveals that more SNe Ia than previously thought may exhibit C II $\lambda$6580 absorption features and relics of line blending near \~{}6300 \AA. Here we present new SN Ia observations where spectroscopic signatures of C II $\lambda$6580 are detected and investigate the presence of C II $\lambda$6580 in the optical spectra of 19 SNe Ia using the parameterized spectrum synthesis code, SYNOW. Most of the objects in our sample that exhibit C II $\lambda$6580 absorption features are of the low-velocity gradient subtype. Our study indicates that the morphology of carbon-rich regions is consistent with either a spherical distribution or a hemispheric asymmetry, supporting the recent idea that SN Ia diversity may be a result of off-center ignition coupled with observer line-of-sight effects.},
author = {Parrent, Jerod T. and Thomas, R. C. and Fesen, Robert A. and Marion, G. H. and Challis, Peter and Garnavich, Peter M. and Milisavljevic, Dan and Vink\`{o}, J\`{o}zsef and Wheeler, J. Craig},
doi = {10.1088/0004-637X/732/1/30},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {supernovae: general,supernovae: individual: SN 2010Y 2010ai PTF10icb},
month = {may},
number = {1},
pages = {30},
title = {{A STUDY OF CARBON FEATURES IN TYPE Ia SUPERNOVA SPECTRA}},
url = {http://adsabs.harvard.edu.proxy.library.ucsb.edu:2048/abs/2011ApJ...732...30P},
volume = {732},
year = {2011},
}
@article{2009A&A...500.1013P,
author = {Pastorello, A and Crockett, R M and Martin, R and Smartt, S.\~{}J. and Altavilla, G and Benetti, S and Botticella, M T and Cappellaro, E and Mattila, S and Maund, J R and Ryder, S D and Salvo, M and Taubenberger, S and Turatto, M},
journal = {Astronomy and Astrophysics},
month = {jun},
number = {3},
pages = {1013--1023},
title = {{SN 1999ga: a low-luminosity linear type II supernova?}},
volume = {500},
year = {2009},
}
@article{Fraser2013,
abstract = {We present ultraviolet, optical and near-infrared observations of the interacting transient SN 2009ip, covering the period from the start of the outburst in 2012 October until the end of the 2012 observing season. The transient reached a peak magnitude of MV = -17.7 mag, with a total integrated luminosity of 1.9 × 1049 erg over the period of 2012 August-December. The light curve fades rapidly, dropping by 4.5 mag from the V-band peak in 100 d. The optical and near-infrared spectra are dominated by narrow emission lines with broad electron scattering wings, signalling a dense circumstellar environment, together with multiple components of broad emission and absorption in H and He at velocities in the range 0.5-1.2 × 104 km s-1. We see no evidence for nucleosynthesized material in SN 2009ip, even in late-time pseudo-nebular spectra. We set a limit of <0.02 M⊙ on the mass of any possible synthesized 56Ni from the late-time light curve. A simple model for the narrow Balmer lines is presented and used to derive number densities for the circumstellar medium in the range ˜109-1010 cm-3. Our near-infrared data do not show any excess at longer wavelengths, and we see no other signs of dust formation. Our last data, taken in 2012 December, show that SN 2009ip has spectroscopically evolved to something quite similar to its appearance in late 2009, albeit with higher velocities. It is possible that neither of the eruptive and high-luminosity events of SN 2009ip were induced by a core collapse. We show that the peak and total integrated luminosity can be due to the efficient conversion of kinetic energy from colliding ejecta, and that around 0.05-0.1 M⊙ of material moving at 0.5-1 × 104 km s-1 could comfortably produce the observed luminosity. We discuss the possibility that these shells were ejected by the pulsational pair instability mechanism, in which case the progenitor star may still exist, and will be observed after the current outburst fades. The long-term monitoring of SN 2009ip, due to its proximity, has given the most extensive data set yet gathered of a high-luminosity interacting transient and its progenitor. It is possible that some purported Type IIn supernovae are in fact analogues of the 2012b event and that pre-explosion outbursts have gone undetected.},
author = {Fraser, M. and Inserra, C. and Jerkstrand, A. and Kotak, R. and Pignata, G. and Benetti, S. and Botticella, M.-T. and Bufano, F. and Childress, M. and Mattila, S. and Pastorello, A. and Smartt, S. J. and Turatto, M. and Yuan, F. and Anderson, J. P. and Bayliss, D. D. R. and Bauer, F. E. and Chen, T.-W. and {Forster Buron}, F. and Gal-Yam, A. and Haislip, J. B. and Knapic, C. and {Le Guillou}, L. and Marchi, S. and Mazzali, P. and Molinaro, M. and Moore, J. P. and Reichart, D. and Smareglia, R. and Smith, K. W. and Sternberg, A. and Sullivan, M. and Takats, K. and Tucker, B. E. and Valenti, S. and Yaron, O. and Young, D. R. and Zhou, G.},
doi = {10.1093/mnras/stt813},
file = {:Users/svalenti/Documents/Mendeley Desktop/2013/Monthly Notices of the Royal Astronomical Society/MNRAS-2013-Fraser-1312-37.pdf:pdf},
issn = {0035-8711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {stars: mass-loss,stars: massive,supernovae: general,supernovae: individual: SN 2009ip},
month = {jun},
number = {2},
pages = {1312--1337},
title = {{SN 2009ip a la PESSTO: no evidence for core collapse yet}},
url = {http://adsabs.harvard.edu/abs/2013MNRAS.433.1312F},
volume = {433},
year = {2013},
}
@article{2009Natur.460..869K,
author = {Kasen, D and R\"{o}pke, F.\~{}K. and Woosley, S E},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/Nature/2009 Kasen.pdf:pdf},
journal = {Nature},
month = {aug},
number = {7},
pages = {869--872},
title = {{The diversity of type Ia supernovae from broken symmetries}},
volume = {460},
year = {2009},
}
@article{2009Natur.459..674V,
abstract = {The final fate of massive stars depends on many factors. Theory suggests that some with initial masses greater than 25 to 30 solar masses end up as Wolf-Rayet stars, which are deficient in hydrogen in their outer layers because of mass loss through strong stellar winds. The most massive of these stars have cores which may form a black hole and theory predicts that the resulting explosion of some of them produces ejecta of low kinetic energy, a faint optical luminosity and a small mass fraction of radioactive nickel. An alternative origin for low-energy supernovae is the collapse of the oxygen-neon core of a star of 7-9 solar masses. No weak, hydrogen-deficient, core-collapse supernovae have hitherto been seen. Here we report that SN 2008ha is a faint hydrogen-poor supernova. We propose that other similar events have been observed but have been misclassified as peculiar thermonuclear supernovae (sometimes labelled SN 2002cx-like events). This discovery could link these faint supernovae to some long-duration gamma-ray bursts, because extremely faint, hydrogen-stripped core-collapse supernovae have been proposed to produce such long gamma-ray bursts, the afterglows of which do not show evidence of associated supernovae.},
author = {Valenti, S and Pastorello, A and Cappellaro, E and Benetti, S and Mazzali, P a and Manteca, J and Taubenberger, S and Elias-Rosa, N and Ferrando, R and Harutyunyan, A and Hentunen, V P and Nissinen, M and Pian, E and Turatto, M and Zampieri, L and Smartt, S J},
doi = {10.1038/nature08023},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/Nature/2009 Valenti.pdf:pdf},
issn = {1476-4687},
journal = {Nature},
month = {jun},
number = {7247},
pages = {674--7},
pmid = {19494909},
publisher = {Nature Publishing Group},
title = {{A low-energy core-collapse supernova without a hydrogen envelope.}},
url = {http://www.ncbi.nlm.nih.gov/pubmed/19494909},
volume = {459},
year = {2009},
}
@article{2011ApJ...734...38W,
author = {Woosley, S E and Kasen, Daniel},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/The Astrophysical Journal/2011 Woosley.pdf:pdf},
journal = {The Astrophysical Journal},
month = {jun},
number = {1},
pages = {38},
title = {{Sub-Chandrasekhar Mass Models for Supernovae}},
volume = {734},
year = {2011},
}
@article{Foley2003,
archiveprefix = {arXiv},
arxivid = {astro-ph/0307136},
author = {Foley, Ryan J. and Papenkova, Marina S. and Swift, Brandon J. and Filippenko, Alexei V. and Li, Weidong and Mazzali, Paolo A. and Chornock, Ryan and Leonard, Douglas C. and {Van Dyk}, Schuyler D.},
doi = {10.1086/378242},
eprint = {0307136},
file = {:Users/svalenti/Documents/Mendeley Desktop/2003/Publications of the Astronomical Society of the Pacific/378242.pdf:pdf},
issn = {0004-6280},
journal = {Publications of the Astronomical Society of the Pacific},
keywords = {Stars: Supernovae: General,Stars: Supernovae: Individual: Alphanumeric: SN 19,gamma-rays: bursts,line: identification,supernovae: individual (SN 2002ap)},
language = {en},
month = {oct},
number = {812},
pages = {1220--1235},
primaryclass = {astro-ph},
title = {{Optical Photometry and Spectroscopy of the SN 1998bw–like Type Ic Supernova 2002ap}},
url = {http://adsabs.harvard.edu/abs/2003PASP..115.1220F},
volume = {115},
year = {2003},
}
@article{2009AJ....138..727M,
author = {Marion, G. H. and H\"{o}flich, P. and Gerardy, C. L. and Vacca, W. D. and Wheeler, J. C. and Robinson, E. L.},
doi = {10.1088/0004-6256/138/3/727},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/The Astronomical Journal/2009 Marion.pdf:pdf},
issn = {0004-6256},
journal = {The Astronomical Journal},
keywords = {be reduced by an,color figures,cosmology,general,identification,infrared,level of high-precision cosmology,line,measurements the dispersion must,observations,online-only material,order of,required for dark energy,supernovae},
month = {sep},
number = {3},
pages = {727--757},
title = {{A CATALOG OF NEAR-INFRARED SPECTRA FROM TYPE Ia SUPERNOVAE}},
url = {http://stacks.iop.org/1538-3881/138/i=3/a=727?key=crossref.c0a15d1bc80b3277664e34cfdc8685e3},
volume = {138},
year = {2009},
}
@article{Graham2013,
abstract = {We report a spectroscopic classification of PSN J20540830-7820035 located at ra=20:54:08.30 dec=-78:20:03.5. A spectrum (range 330-1000 nm) obtained robotically on May 17.70 UT with the FLOYDS spectrograph at Faulkes Telescope South at Siding Springs shows it to be a SN Ia near maximum at a redshift of 0.03. Classification was performed via supernova spectrum cross correlation using SNID (Blondin \& Tonry, 2007, ApJ, 666, 1024), which yields the best match with SN 2003du (Stanishev et al.},
author = {Graham, M. L. and Howell, D. A. and Valenti, S. and Sand, D. and Parrent, J. T.},
journal = {The Astronomer's Telegram},
keywords = {Optical,Supernovae},
title = {{Classification of PSN J20540830-7820035 with FLOYDS at Faulkes Telescope South}},
url = {http://adsabs.harvard.edu/abs/2013ATel.5071....1G},
year = {2013},
}
@article{2005ApJ...631..231P,
author = {Pilyugin, Leonid S and Thuan, Trinh X},
file = {:Users/svalenti/Documents/Mendeley Desktop/2005/The Astrophysical Journal/2005 Pilyugin.pdf:pdf},
journal = {The Astrophysical Journal},
month = {sep},
number = {1},
pages = {231--243},
title = {{Oxygen Abundance Determination in H II Regions: The Strong Line Intensities-Abundance Calibration Revisited}},
volume = {631},
year = {2005},
}
@article{2007A&A...476.1133F,
author = {Fink, M and Hillebrandt, W and R\"{o}pke, F K},
doi = {10.1051/0004-6361:20078438},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/Astronomy and Astrophysics/2007 Fink.pdf:pdf},
issn = {0004-6361},
journal = {Astronomy and Astrophysics},
keywords = {abundances,general,hydrodynamics,methods,nuclear reactions,nucleosynthesis,numerical,supernovae},
month = {dec},
number = {3},
pages = {1133--1143},
title = {{Double-detonation supernovae of sub-Chandrasekhar mass white dwarfs}},
url = {http://www.aanda.org/10.1051/0004-6361:20078438},
volume = {476},
year = {2007},
}
@article{Arnett1980,
author = {Arnett, W. D.},
doi = {10.1086/157898},
file = {:Users/svalenti/Documents/Mendeley Desktop/1980/The Astrophysical Journal/1980 Arnett.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {apr},
pages = {541},
title = {{Analytic solutions for light curves of supernovae of Type II}},
url = {http://adsabs.harvard.edu/doi/10.1086/157898},
volume = {237},
year = {1980},
}
@article{Bersten2012,
abstract = {A set of hydrodynamical models based on stellar evolutionary progenitors is used to study the nature of SN 2011dh. Our modeling suggests that a large progenitor star—with R \~{} 200 R ⊙—is needed to reproduce the early light curve (LC) of SN 2011dh. This is consistent with the suggestion that the yellow super-giant star detected at the location of the supernova (SN) in deep pre-explosion images is the progenitor star. From the main peak of the bolometric LC and expansion velocities, we constrain the mass of the ejecta to be ≈2 M ⊙, the explosion energy to be E = (6-10) × 1050 erg, and the 56Ni mass to be approximately 0.06 M ⊙. The progenitor star was composed of a helium core of 3-4 M ⊙ and a thin hydrogen-rich envelope of ≈0.1M ⊙ with a main-sequence mass estimated to be in the range of 12-15 M ⊙. Our models rule out progenitors with helium-core masses larger than 8 M ⊙, which correspond to M ZAMS \>\~{} 25M ⊙. This suggests that a single star evolutionary scenario for SN 2011dh is unlikely.},
author = {Bersten, Melina C. and Benvenuto, Omar G. and Nomoto, Ken'ichi and Ergon, Mattias and Folatelli, Gast\'{o}n and Sollerman, Jesper and Benetti, Stefano and Botticella, Maria Teresa and Fraser, Morgan and Kotak, Rubina and Maeda, Keiichi and Ochner, Paolo and Tomasella, Lina},
doi = {10.1088/0004-637X/757/1/31},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/The Astrophysical Journal/apj\_757\_1\_31.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {hydrodynamics,supernovae: general,supernovae: individual: SN 2011dh},
month = {sep},
number = {1},
pages = {31},
title = {{THE TYPE IIb SUPERNOVA 2011dh FROM A SUPERGIANT PROGENITOR}},
url = {http://adsabs.harvard.edu/abs/2012ApJ...757...31B},
volume = {757},
year = {2012},
}
@article{Sim2013,
abstract = {In a companion paper, Seitenzahl et al. (2013) presented a set of three-dimensional delayed detonation models for thermonuclear explosions of near-Chandrasekhar mass white dwarfs (WDs). Here, we present multi-dimensional radiative transfer simulations that provide synthetic light curves and spectra for those models. The model sequence explores both changes in the strength of the deflagration phase (controlled by the ignition configuration) and the WD central density. In agreement with previous studies, we find that the strength of the deflagration significantly affects the explosion and the observables. Variations in the central density also have an influence on both brightness and colour, but overall it is a secondary parameter in our set of models. In many respects, the models yield a good match to normal Type Ia supernovae (SNe Ia): peak brightness, rise/decline time scales and synthetic spectra are all in reasonable agreement. There are, however, several differences. In particular, the models are too red around maximum light, manifest spectral line velocities that are a little too high and yield I-band light curves that do not match observations. Although some of these discrepancies may simply relate to approximations made in the modelling, some pose real challenges to the models. If viewed as a complete sequence, our models do not reproduce the observed light-curve width-luminosity relation (WLR) of SNe Ia: all our models show similar B-band decline rates, irrespective of peak brightness. This suggests that simple variations in the strength of the deflagration phase in Chandrasekhar-mass deflagration-to-detonation models do not readily explain the observed diversity of normal SNe Ia. This may imply that some other parameter within the Chandrasekhar-mass paradigm is key to the WLR, or that a substantial fraction of normal SNe Ia arise from an alternative explosion scenario.},
archiveprefix = {arXiv},
arxivid = {1308.4833},
author = {Sim, S. A. and Seitenzahl, I. R. and Kromer, M. and Ciaraldi-Schoolmann, F. and Ropke, F. K. and Fink, M. and Hillebrandt, W. and Pakmor, R. and Ruiter, A. J. and Taubenberger, S.},
doi = {10.1093/mnras/stt1574},
eprint = {1308.4833},
issn = {0035-8711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {binaries: close,hydrodynamics,methods: numerical,radiative transfer,supernovae: general,white dwarfs},
language = {en},
month = {sep},
pages = {16},
title = {{Synthetic light curves and spectra for three-dimensional delayed-detonation models of Type Ia supernovae}},
url = {http://adsabs.harvard.edu/abs/2013MNRAS.tmp.2228S},
volume = {-1},
year = {2013},
}
@article{2010ApJ...723L..98K,
author = {Kasliwal, Mansi M and Kulkarni, S.\~{}R. and Gal-Yam, Avishay and Yaron, Ofer and Quimby, Robert M and Ofek, Eran O and Nugent, Peter and Poznanski, Dovi and Jacobsen, Janet and Sternberg, Assaf and Arcavi, Iair and Howell, D Andrew and Sullivan, Mark and Rich, Douglas J and Burke, Paul F and Brimacombe, Joseph and Milisavljevic, Dan and Fesen, Robert and Bildsten, Lars and Shen, Ken and Cenko, S Bradley and Bloom, Joshua S and Hsiao, Eric and Law, Nicholas M and Gehrels, Neil and Immler, Stefan and Dekany, Richard and Rahmer, Gustavo and Hale, David and Smith, Roger and Zolkower, Jeff and Velur, Viswa and Walters, Richard and Henning, John and Bui, Kahnh and McKenna, Dan},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/The Astrophysical Journal Letters/2010 Kasliwal.pdf:pdf},
journal = {The Astrophysical Journal Letters},
month = {nov},
number = {1},
pages = {L98--------L102},
title = {{Rapidly Decaying Supernova 2010X: A Candidate .Ia Explosion}},
volume = {723},
year = {2010},
}
@article{2006MNRAS.371.1459T,
author = {Taubenberger, S. and Pastorello, a. and Mazzali, P.\~{}A. a. and Valenti, S. and Pignata, G. and Sauer, D. N. and Arbey, a. and B\"{a}rnbantner, O and Benetti, S. and {Della Valle}, a. and Deng, J. and Elias-Rosa, N. and Filippenko, a. V. and Foley, R. J. and Goobar, a. and Kotak, R. and Li, W. and Meikle, P. and Mendez, J. and Patat, F. and Pian, E. and Ries, C. and Ruiz-Lapuente, P. and Salvo, M. and Stanishev, V. and Turatto, M. and Hillebrandt, W. and B��rnbantner, O.},
doi = {10.1111/j.1365-2966.2006.10776.x},
file = {:Users/svalenti/Documents/Mendeley Desktop/2006/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2006 Taubenberger.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {galaxies,general,indi-,individual,ngc 3997,sn 1994i,sn 2002ap,sn 2003jd,sn 2004aw,supernovae,vidual},
month = {sep},
number = {3},
pages = {1459--1477},
title = {{SN 2004aw: confirming diversity of Type Ic supernovae}},
url = {http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2006.10776.x},
volume = {371},
year = {2006},
}
@article{1997A&A...322..431C,
author = {Cappellaro, E and Turatto, M and Tsvetkov, D Yu. and Bartunov, O S and Pollas, C and Evans, R and Hamuy, M},
file = {:Users/svalenti/Documents/Mendeley Desktop/1997/Astronomy and Astrophysics/1997 Cappellaro.pdf:pdf},
journal = {Astronomy and Astrophysics},
month = {jun},
pages = {431--441},
title = {{The rate of supernovae from the combined sample of five searches.}},
volume = {322},
year = {1997},
}
@article{Sharina1996,
abstract = {Based on photometry of the brightest blue stars we derived distance moduli for NGC 628 and its dwarf irregular companions: DDO 13, UGC 1171, UGC 1104, and K 10. The mean modulus of the group is estimated to be 29.46 mag with a formal (internal) error of 0.11. The total mass to luminosity ratio of 40Msun\_/Lsun\_ seems sufficient for NGC 628 to keep its companions in bound orbits.},
author = {Sharina, M. E. and Karachentsev, I. D. and Tikhonov, N. A.},
journal = {Astronomy and Astrophysics Supplement},
keywords = {DISTANCES AND REDSHIFTS,GALAXIES: INDIVIDUAL: NGC 628,IRREGULAR},
title = {{Photometric distances to NGC 628 and its four companions.}},
url = {http://adsabs.harvard.edu/abs/1996A\&AS..119..499S},
year = {1996},
}
@article{1992ApJ...384L..37F,
author = {Filippenko, Alexei V.},
doi = {10.1086/186257},
file = {:Users/svalenti/Documents/Mendeley Desktop/1992/The Astrophysical Journal/1992 Filippenko.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {jan},
pages = {L37},
title = {{Early-time spectra of type IC supernovae - Further evidence for the presence of hydrogen}},
url = {http://adsabs.harvard.edu/doi/10.1086/186257},
volume = {384},
year = {1992},
}
@article{2002MNRAS.333...27P,
author = {Pastorello, A and Turatto, M and Benetti, S and Cappellaro, E and Danziger, I J and Mazzali, P.\~{}A. and Patat, F and Filippenko, A V and Schlegel, D.\~{}J. and Matheson, T},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {jun},
number = {1},
pages = {27--38},
title = {{The type IIn supernova 1995G: interaction with the circumstellar medium}},
volume = {333},
year = {2002},
}
@article{Organisation2012,
author = {Organisation, European and Hemisphere, Southern and Retzlaff, J},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/Unknown/2012.pdf:pdf},
title = {{Data Management and Operations Division}},
year = {2012},
}
@article{Modjaz2008,
author = {Modjaz, M. and Kirshner, R. P. and Blondin, S. and Challis, P. and Matheson, T.},
doi = {10.1086/593135},
file = {:Users/svalenti/Documents/Mendeley Desktop/2008/The Astrophysical Journal/2008 Modjaz-1.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {nov},
number = {1},
pages = {L9--L12},
title = {{Double-Peaked Oxygen Lines Are Not Rare in Nebular Spectra of Core-Collapse Supernovae}},
url = {http://stacks.iop.org/1538-4357/687/i=1/a=L9},
volume = {687},
year = {2008},
}
@article{1995AJ....109.2121R,
author = {Richmond, Michael W and Treffers, Richard R and Filippenko, Alexei V and van Dyk, Schuyler D and Paik, Young and Peng, Chien and Marschall, Laurence A and Laaksonen, Bentley D and Macintosh, Bruce and McLean, Ian S},
journal = {Astronomical Journal v.109},
month = {may},
pages = {2121},
title = {{UBVRI Photometry of the Type IA SN 1994D in NGC 4526}},
volume = {109},
year = {1995},
}
@article{2010MNRAS.408..181P,
author = {Pastorello, A and Botticella, M T and Trundle, C and Taubenberger, S and Mattila, S and Kankare, E and Elias-Rosa, N and Benetti, S and Duszanowicz, G and Hermansson, L and Beckman, J E and Bufano, F and Fraser, M and Harutyunyan, A and Navasardyan, H and Smartt, S.\~{}J. and van Dyk, S D and Vink, J S and Wagner, R M},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {oct},
number = {1},
pages = {181--198},
title = {{Multiple major outbursts from a restless luminous blue variable in NGC 3432}},
volume = {408},
year = {2010},
}
@article{Stiavelli:2007vd,
annote = {5 pages, 2 figures, proceedings of the conference Science with the VLT in the ELT era},
author = {Stiavelli, Massimo},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/arXiv.org/arXiv 2007 Stiavelli.pdf:pdf},
journal = {arXiv.org},
month = {dec},
title = {{Observational Cosmology with the ELT and JWST}},
volume = {astro-ph},
year = {2007},
}
@article{Cumbres2010,
author = {Cumbres, Las and Global, Observatory and Network, Telescope},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/Unknown/2010.pdf:pdf},
number = {May},
title = {{EMPLOYEE}},
year = {2010},
}
@article{2007CBET.1101....1F,
author = {Filippenko, A V and Silverman, J.\~{}M. and Foley, R J and Modjaz, M and Papovich, C and Willmer, C N A and Blondin, S and Brown, W},
journal = {Central Bureau Electronic Telegrams},
month = {oct},
pages = {1},
title = {{Supernovae 2007iq, 2007ir, 2007ke, and 2007le}},
volume = {1101},
year = {2007},
}
@article{2010A&A...512A..70Y,
author = {Young, D.\~{}R. and Smartt, S.\~{}J. and Valenti, S and Pastorello, A and Benetti, S and Benn, C.\~{}R. and Bersier, D and Botticella, M T and Corradi, R.\~{}L.\~{}M. and Harutyunyan, A.\~{}H. and Hrudkova, M and Hunter, I and Mattila, S and de Mooij, E.\~{}J.\~{}W. and Navasardyan, H and Snellen, I.\~{}A.\~{}G. and Tanvir, N.\~{}R. and Zampieri, L},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/Astronomy and Astrophysics/2010 Young.pdf:pdf},
journal = {Astronomy and Astrophysics},
month = {mar},
pages = {70},
title = {{Two type Ic supernovae in low-metallicity, dwarf galaxies: diversity of explosions}},
volume = {512},
year = {2010},
}
@article{Gal-Yam2011a,
abstract = {The Palomar Transient Factory (PTF) is an optical wide-field variability survey carried out using a camera with a 7.8 deg2 field of view mounted on the 48 inch Oschin Schmidt telescope at Palomar Observatory. One of the key goals of this survey is to conduct high-cadence monitoring of the sky in order to detect optical transient sources shortly after they occur. Here, we describe the real-time capabilities of the PTF and our related rapid multiwavelength follow-up programs, extending from the radio to the $\gamma$-ray bands. We present as a case study observations of the optical transient PTF10vdl (SN 2010id), revealed to be a very young core-collapse (Type II-P) supernova having a remarkably low luminosity. Our results demonstrate that the PTF now provides for optical transients the real-time discovery and rapid-response follow-up capabilities previously reserved only for high-energy transients like gamma-ray bursts.},
author = {Gal-Yam, Avishay and Kasliwal, Mansi M. and Arcavi, Iair and Green, Yoav and Yaron, Ofer and Ben-Ami, Sagi and Xu, Dong and Sternberg, Assaf and Quimby, Robert M. and Kulkarni, Shrinivas R. and Ofek, Eran O. and Walters, Richard and Nugent, Peter E. and Poznanski, Dovi and Bloom, Joshua S. and Cenko, S. Bradley and Filippenko, Alexei V. and Li, Weidong and Silverman, Jeffrey M. and Walker, Emma S. and Sullivan, Mark and Maguire, K. and {Andrew Howell}, D. and Mazzali, Paolo A. and Frail, Dale A. and Bersier, David and James, Phil A. and Akerlof, C. W. and Yuan, Fang and Law, Nicholas and Fox, Derek B. and Gehrels, Neil},
doi = {10.1088/0004-637X/736/2/159},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/The Astrophysical Journal/apj\_736\_2\_159.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {supernovae: general,supernovae: individual: PTF10vdl},
month = {aug},
number = {2},
pages = {159},
title = {{REAL-TIME DETECTION AND RAPID MULTIWAVELENGTH FOLLOW-UP OBSERVATIONS OF A HIGHLY SUBLUMINOUS TYPE II-P SUPERNOVA FROM THE PALOMAR TRANSIENT FACTORY SURVEY}},
url = {http://adsabs.harvard.edu/abs/2011ApJ...736..159G},
volume = {736},
year = {2011},
}
@article{2010ApJ...712..350H,
author = {Hayden, Brian T. and Garnavich, Peter M. and Kessler, Richard and Frieman, Joshua a. and Jha, Saurabh W. and Bassett, Bruce and Cinabro, David and Dilday, Benjamin and Kasen, Daniel and Marriner, John and Nichol, Robert C. and Riess, Adam G. and Sako, Masao and Schneider, Donald P. and Smith, Mathew and Sollerman, Jesper},
doi = {10.1088/0004-637X/712/1/350},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/The Astrophysical Journal/2010 Hayden.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {color figure,data analysis,general,methods,online-only material,supernovae,white dwarfs},
month = {mar},
number = {1},
pages = {350--366},
title = {{THE RISE AND FALL OF TYPE Ia SUPERNOVA LIGHT CURVES IN THE SDSS-II SUPERNOVA SURVEY}},
url = {http://stacks.iop.org/0004-637X/712/i=1/a=350?key=crossref.4a87ac4ac49dd9e37b56329dc8e6bc16},
volume = {712},
year = {2010},
}
@article{2010A&A...514A..53F,
author = {Kromer, M. and Sim, S. a. and Fink, M. and R\"{o}pke, F. K. and Seitenzahl, I. R. and Hillebrandt, W.},
doi = {10.1051/0004-6361/200913892},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/Astronomy and Astrophysics/2010 Kromer.pdf:pdf;:Users/svalenti/Documents/Mendeley Desktop/2010/Astronomy and Astrophysics/2010 Fink.pdf:pdf},
issn = {0004-6361},
journal = {Astronomy and Astrophysics},
keywords = {abundances,general,hydrodynamics,methods,nuclear reactions,nucleosynthesis,numerical,radiative transfer,supernovae},
month = {may},
number = {2},
pages = {A53},
title = {{Double-Detonation Sub-Chandrasekhar Supernovae: Synthetic Observables for Minimum Helium Shell Mass Models}},
url = {http://www.aanda.org/10.1051/0004-6361/200913892 http://stacks.iop.org/0004-637X/719/i=2/a=1067?key=crossref.205775f140c7bb0394ab6128e2b88867},
volume = {514},
year = {2010},
}
@article{2012MNRAS.420.3451M,
author = {Maguire, K and Jerkstrand, A and Smartt, S.\~{}J. and Fransson, C and Pastorello, A and Benetti, S and Valenti, S and Bufano, F and Leloudas, G},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2012 Maguire.pdf:pdf},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {mar},
number = {4},
pages = {3451--3468},
title = {{Constraining the physical properties of Type II-Plateau supernovae using nebular phase spectra}},
volume = {420},
year = {2012},
}
@article{Rayner2003,
abstract = {We present the design, construction, and performance of SpeX, a medium-resolution 0.8-5.5 $\mu$m cryogenic spectrograph and imager, now in operation at the 3.0 m NASA Infrared Telescope Facility (IRTF) on Mauna Kea. The design uses prism cross-dispersers and gratings to provide resolving powers up to R\~{}2000 simultaneously across 0.8-2.4, 1.9-4.2, or 2.4-5.5 $\mu$m, with a 15 long slit. A high-throughput low-resolution R\~{}200 prism mode is also provided for faint-object and occultation spectroscopy. Single-order 60 long-slit modes with resolving powers up to R\~{}2000 are available for extended objects. The spectrograph employs an Aladdin 3 1024×1024 InSb array and uses narrow slits and a spatial scale of 0.15 pixel-1 for optimum sensitivity on point sources. An autonomous infrared slit viewer is used for object acquisition, infrared guiding, and scientific imaging in the wavelength range 0.8-5.5 $\mu$m. The imager employs an Aladdin 2 512×512 InSb array that covers a 60''×60'' field of view at 0.12 pixel-1. SpeX was successfully commissioned on IRTF during 2000 May, June, and July. Astronomical observations are presented to illustrate performance.},
author = {Rayner, J. T. and Toomey, D. W. and Onaka, P. M. and Denault, A. J. and Stahlberger, W. E. and Vacca, W. D. and Cushing, M. C. and Wang, S.},
doi = {10.1086/367745},
issn = {0004-6280},
journal = {Publications of the Astronomical Society of the Pacific},
keywords = {Brown Dwarfs,Instrumentation: Detectors,Instrumentation: Spectrographs,Stars: Hertzsprung-Russell Diagram,Stars: Low-Mass,Stars: Wolf-Rayet},
month = {mar},
number = {805},
pages = {362--382},
title = {{SpeX: A Medium‐Resolution 0.8–5.5 Micron Spectrograph and Imager for the NASA Infrared Telescope Facility}},
url = {http://adsabs.harvard.edu/abs/2003PASP..115..362R},
volume = {115},
year = {2003},
}
@article{Iwamoto2000,
author = {Iwamoto, Koichi and Nakamura, Takayoshi and Nomoto, Ken’ichi and Mazzali, Paolo A and Danziger, I John and Garnavich, Peter and Kirshner, Robert and Jha, Saurabh and Balam, David and Thorstensen, John},
doi = {10.1086/308761},
file = {:Users/svalenti/Documents/Mendeley Desktop/2000/The Astrophysical Journal/2000 Iwamoto.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {may},
number = {2},
pages = {660--669},
title = {{The Peculiar Type Ic Supernova 1997ef: Another Hypernova}},
url = {http://stacks.iop.org/0004-637X/534/i=2/a=660},
volume = {534},
year = {2000},
}
@article{Howell2011,
abstract = {Empirically, Type Ia supernovae are the most useful, precise, and mature tools for determining astronomical distances. Acting as calibrated candles they revealed the presence of dark energy and are being used to measure its properties. However, the nature of the Type Ia explosion, and the progenitors involved, have remained elusive, even after seven decades of research. But now, new large surveys are bringing about a paradigm shift--we can finally compare samples of hundreds of supernovae to isolate critical variables. As a result of this, and advances in modelling, breakthroughs in understanding all aspects of these supernovae are finally starting to happen.},
archiveprefix = {arXiv},
arxivid = {1011.0441},
author = {Howell, D Andrew},
doi = {10.1038/ncomms1344},
eprint = {1011.0441},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/Nature communications/2011 Howell.pdf:pdf},
issn = {2041-1723},
journal = {Nature communications},
keywords = {Astronomy,Astronomy: methods,Celestial,Cosmic Radiation,Light,Models,Spectrum Analysis,Stars,Theoretical},
month = {jan},
pages = {350},
pmid = {21673671},
title = {{Type Ia supernovae as stellar endpoints and cosmological tools.}},
url = {http://arxiv.org/abs/1011.0441 http://www.ncbi.nlm.nih.gov/pubmed/21673671},
volume = {2},
year = {2011},
}
@article{2006MNRAS.369.1939S,
author = {Sauer, D N and Mazzali, P. A. and Deng, J and Valenti, S and Nomoto, K and Filippenko, A V},
doi = {10.1111/j.1365-2966.2006.10438.x},
file = {:Users/svalenti/Documents/Mendeley Desktop/2006/Monthly Notices of the Royal Astronomical Society/2006MNRAS\_369\_1939S.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {jun},
number = {4},
pages = {1939--1948},
title = {{The properties of the ‘standard’ Type Ic supernova 1994I from spectral models}},
url = {http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2006.10438.x},
volume = {369},
year = {2006},
}
@article{2012ARA&A..50..107L,
annote = {57 pages, 10 figures; see http://www.annualreviews.org/toc/astro/forthcoming for complete preliminary paper},
author = {Langer, N},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/Annual Review of Astronomy \{\&\} Astrophysics/2012 Langer.pdf:pdf},
journal = {Annual Review of Astronomy \{\&\} Astrophysics},
month = {sep},
pages = {107--164},
title = {{Presupernova Evolution of Massive Single and Binary Stars}},
volume = {50},
year = {2012},
}
@article{Kulkarni2007,
abstract = {Historically, variable and transient sources have both surprised astronomers and provided new views of the heavens. Here we report the discovery of an optical transient in the outskirts of the lenticular galaxy Messier 85 in the Virgo cluster. With a peak absolute R magnitude of -12, this event is distinctly brighter than novae, but fainter than type Ia supernovae (which are expected in a population of old stars in lenticular galaxies). Archival images of the field do not show a luminous star at that position with an upper limit in the g filter of about -4.1 mag, so it is unlikely to be a giant eruption from a luminous blue variable star. Over a two-month period, the transient source emitted radiation energy of almost 10(47) erg and subsequently faded in the optical sky. It is similar to, but six times more luminous at peak than, an enigmatic transient in the galaxy M31 (ref. 1). A possible origin of M85 OT2006-1 is a stellar merger. If so, searches for similar events in nearby galaxies will not only allow study of the physics of hyper-Eddington sources, but also probe an important phase in the evolution of stellar binary systems.},
archiveprefix = {arXiv},
arxivid = {arXiv:0705.3668v1},
author = {Kulkarni, S R and Ofek, E O and Rau, A and Cenko, S B and Soderberg, A M and Fox, D B and Gal-Yam, A and Capak, P L and Moon, D S and Li, W and Filippenko, A V and Egami, E and Kartaltepe, J and Sanders, D B},
doi = {10.1038/nature05822},
eprint = {arXiv:0705.3668v1},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/Nature/2007 Rau.pdf:pdf},
issn = {1476-4687},
journal = {Nature},
month = {may},
number = {7143},
pages = {458--60},
pmid = {17522679},
title = {{An unusually brilliant transient in the galaxy M85.}},
url = {http://www.nature.com/nature/journal/vaop/ncurrent/full/nature05822.html http://www.ncbi.nlm.nih.gov/pubmed/17522679},
volume = {447},
year = {2007},
}
@article{2005A&A...430...83C,
author = {Cappellaro, E and Riello, M and Altavilla, G and Botticella, M T and Benetti, S and Clocchiatti, A and Danziger, J I and Mazzali, P and Pastorello, A and Patat, F and Salvo, M and Turatto, M and Valenti, S},
file = {:Users/svalenti/Documents/Mendeley Desktop/2005/Astronomy and Astrophysics/2005 Cappellaro.pdf:pdf},
journal = {Astronomy and Astrophysics},
month = {jan},
pages = {83--93},
title = {{Death rate of massive stars at redshift ˜0.3}},
volume = {430},
year = {2005},
}
@article{2009arXiv0908.1127M,
abstract = {Despite its probable occurrence in Nature, the accretion-induced collapse (AIC) of a white dwarf has not yet been directly observed (or, at least, it has not been unambiguously identified as such). In this contribution we summarize the observational signatures of AIC, emphasizing its possible role as both an optical and high-energy transient.},
annote = {6 pages; 3 figures; proceedings of Neutron Stars \{\&\} Gamma-Ray Bursts - Cairo \{\&\} Alexandria, Egypt},
archiveprefix = {arXiv},
arxivid = {0908.1127},
author = {Metzger, B. D. and Piro, A. L. and Quataert, E and Thompson, T A},
eprint = {0908.1127},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/arXiv.org/arXiv 2009 Metzger.pdf:pdf},
journal = {arXiv.org},
month = {aug},
pages = {6},
title = {{Observable Signatures of the Accretion-Induced Collapse of White Dwarfs}},
url = {http://arxiv.org/abs/0908.1127},
volume = {0908},
year = {2009},
}
@article{2008MNRAS.389..955P,
author = {Pastorello, A and Kasliwal, M.\~{}M. and Crockett, R M and Valenti, S and Arbour, R and Itagaki, K and Kaspi, S and Gal-Yam, A and Smartt, S.\~{}J. and Griffith, R and Maguire, K and Ofek, E O and Seymour, N and Stern, D and Wiethoff, W},
file = {:Users/svalenti/Documents/Mendeley Desktop/2008/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2008 Pastorello.pdf:pdf},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {sep},
number = {2},
pages = {955--966},
title = {{The Type IIb SN 2008ax: spectral and light curve evolution}},
volume = {389},
year = {2008},
}
@article{Kennicutt1998a,
abstract = {Observations of star formation rates (SFRs) in galaxies provide vital clues to the physical nature of the Hubble sequence and are key probes of the evolutionary histories of galaxies. The focus of this review is on the broad patterns in the star formation properties of galaxies along the Hubble sequence and their implications for understanding galaxy evolution and the physical processes that drive the evolution. Star formation in the disks and nuclear regions of galaxies are reviewed separately, then discussed within a common interpretive framework. The diagnostic methods used to measure SFRs are also reviewed, and a self-consistent set of SFR calibrations is presented as an aid to workers in the field.},
author = {Kennicutt, Robert C.},
doi = {10.1146/annurev.astro.36.1.189},
issn = {0066-4146},
journal = {Annual Review of Astronomy and Astrophysics},
month = {sep},
number = {1},
pages = {189--231},
title = {{STAR FORMATION IN GALAXIES ALONG THE HUBBLE SEQUENCE}},
url = {http://adsabs.harvard.edu/abs/1998ARA\&A..36..189K},
volume = {36},
year = {1998},
}
@article{Chevalier2008,
abstract = {The X-ray transient 080109, associated with SN 2008D, can be attributed to the shock breakout emission from a normal Type Ib/c supernova. If the observed emission is interpreted as thermal emission, the temperature and radiated energy are close to expectations, considering that scattering dominates absorption processes so that spectrum formation occurs deep within the photosphere. The X-ray emission observed at \~{}10 days is attributed to inverse Compton scattering of photospheric photons with relativistic electrons produced in the interaction of the supernova with the progenitor wind. A simple model for the optical/ultraviolet emission from shock breakout is developed and applied to SN 1987A, SN 1999ex, SN 2008D, and SN 2006aj, all of which have optical emission observed at t\~{}1 day. The emission from the first three can plausibly be attributed to shock breakout emission. The photospheric temperature is most sensitive to the radius of the progenitor star core and the radii in these cases are in line with expectations from stellar evolution. The early optical/ultraviolet observations of SN 2006aj cannot be accommodated by a nonrelativistic shock breakout model in a straightforward way.},
author = {Chevalier, Roger A. and Fransson, Claes},
doi = {10.1086/591522},
file = {:Users/svalenti/Documents/Mendeley Desktop/2008/The Astrophysical Journal/591522.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {Shock Waves,Stars: Supernovae: General,supernovae: individual (SN 2008D)},
month = {aug},
number = {2},
pages = {L135--L138},
title = {{Shock Breakout Emission from a Type Ib/c Supernova: XRT 080109/SN 2008D}},
url = {http://adsabs.harvard.edu.proxy.library.ucsb.edu:2048/abs/2008ApJ...683L.135C},
volume = {683},
year = {2008},
}
@article{2010Natur.465..322P,
author = {Perets, H.\~{}B. and Gal-Yam, A and Mazzali, P.\~{}A. and Arnett, D and Kagan, D and Filippenko, A V and Li, W and Arcavi, I and Cenko, S.\~{}B. and Fox, D.\~{}B. and Leonard, D.\~{}C. and Moon, D.\~{}S. and Sand, D.\~{}J. and Soderberg, A.\~{}M. and Anderson, J.\~{}P. and James, P.\~{}A. and Foley, R J and Ganeshalingam, M and Ofek, E O and Bildsten, L and Nelemans, G and Shen, K.\~{}J. and Weinberg, N.\~{}N. and Metzger, B.\~{}D. and Piro, A.\~{}L. and Quataert, E and Kiewe, M and Poznanski, D},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/Nature/2010 Perets.pdf:pdf},
journal = {Nature},
month = {may},
number = {7},
pages = {322--325},
title = {{A faint type of supernova from a white dwarf with a helium-rich companion}},
volume = {465},
year = {2010},
}
@article{Patat1994,
abstract = {All photometric observations of Type II Supernovae published to date, and collected in Paper 1, have been reanalyzed along with data from SN spectroscopy. The light curves are very different both as saturation and slopes of the different portions. For sake of simplicity, the average decline rates have been used to describe the gross characteristics of the light curves. It is shown that this sample, numeric parameter well discriminates among the Plateau and Linear shapes. Aslo the color curves are very different, with the Linears on average bluer than Plateaus. By comparing the light curves in absolute magnitude we confirm that at maximum there is a large dispersion in the absolute magnitude. On the hypothesis that the late light curve is powered by the radioactive decay of Co-56, from the observed dispersion of Mv at 300 days we conclude that the amount of Ni-56 synthesized in the explosion of SNII must be in the range 0.04-0.10 solar mass. With the aim to determine how many parameters are needed to characterize the properties of SNII, we performed a Multivariate Factor Analysis on a number of observables, including also some spectroscopic parameters.},
author = {Patat, F. and Barbon, R. and Cappellaro, E. and Turatto, M.},
journal = {Astronomy and Astrophysics (ISSN 0004-6361)},
keywords = {ASTRONOMICAL PHOTOMETRY,ASTRONOMICAL SPECTROSCOPY,COBALT ISOTOPES,LIGHT CURVE,MULTIVARIATE STATISTICAL ANALYSIS,NICKEL ISOTOPES,RADIOACTIVE DECAY,SPECTROSCOPIC ANALYSIS,STELLAR COLOR,STELLAR SPECTRA,SUPERNOVAE},
pages = {731--741},
title = {{Light curves of type II supernovae. 2: The analysis}},
url = {http://adsabs.harvard.edu/abs/1994A\&A...282..731P},
volume = {282},
year = {1994},
}
@article{2007ApJ...661..892M,
author = {Mazzali, Paolo A and Foley, Ryan J and Deng, Jinsong and Patat, Ferdinando and Pian, Elena and Baade, Dietrich and Bloom, Joshua S and Filippenko, Alexei V and Perley, Daniel A and Valenti, Stefano and Wang, Lifan and Kawabata, Koji and Maeda, Keiichi and Nomoto, Ken-ichi},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/The Astrophysical Journal/2007 Mazzali-3.pdf:pdf},
journal = {The Astrophysical Journal},
month = {jun},
number = {2},
pages = {892--898},
title = {{Keck and European Southern Observatory Very Large Telescope View of the Symmetry of the Ejecta of the XRF/SN 2006aj}},
volume = {661},
year = {2007},
}
@article{Parrent2011a,
abstract = {One of the major differences between various explosion scenarios of Type Ia supernovae (SNe Ia) is the remaining amount of unburned (C+O) material and its velocity distribution within the expanding ejecta. While oxygen absorption features are not uncommon in the spectra of SNe Ia before maximum light, the presence of strong carbon absorption has been reported only in a minority of objects, typically during the pre-maximum phase. The reported low frequency of carbon detections may be due to low signal-to-noise data, low abundance of unburned material, line blending between C II $\lambda$6580 and Si II $\lambda$6355, ejecta temperature differences, asymmetrical distribution effects, or a combination of these. However, a survey of published pre-maximum spectra reveals that more SNe Ia than previously thought may exhibit C II $\lambda$6580 absorption features and relics of line blending near \~{}6300 \AA. Here we present new SN Ia observations where spectroscopic signatures of C II $\lambda$6580 are detected and investigate the presence of C II $\lambda$6580 in the optical spectra of 19 SNe Ia using the parameterized spectrum synthesis code, SYNOW. Most of the objects in our sample that exhibit C II $\lambda$6580 absorption features are of the low-velocity gradient subtype. Our study indicates that the morphology of carbon-rich regions is consistent with either a spherical distribution or a hemispheric asymmetry, supporting the recent idea that SN Ia diversity may be a result of off-center ignition coupled with observer line-of-sight effects.},
author = {Parrent, Jerod T. and Thomas, R. C. and Fesen, Robert A. and Marion, G. H. and Challis, Peter and Garnavich, Peter M. and Milisavljevic, Dan and Vink\`{o}, J\`{o}zsef and Wheeler, J. Craig},
doi = {10.1088/0004-637X/732/1/30},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {supernovae: general,supernovae: individual: SN 2010Y 2010ai PTF10icb},
month = {may},
number = {1},
pages = {30},
title = {{A STUDY OF CARBON FEATURES IN TYPE Ia SUPERNOVA SPECTRA}},
url = {http://adsabs.harvard.edu/abs/2011ApJ...732...30P},
volume = {732},
year = {2011},
}
@article{Drout2013,
abstract = {We present extensive multi-wavelength observations of the extremely rapidly declining Type Ic supernova (SN Ic), SN 2005ek. Reaching a peak magnitude of MR = –17.3 and decaying by \~{}3 mag in the first 15 days post-maximum, SN 2005ek is among the fastest Type I supernovae observed to date. The spectra of SN 2005ek closely resemble those of normal SN Ic, but with an accelerated evolution. There is evidence for the onset of nebular features at only nine days post-maximum. Spectroscopic modeling reveals an ejecta mass of \~{}0.3 M ⊙ that is dominated by oxygen (\~{}80\%), while the pseudo-bolometric light curve is consistent with an explosion powered by \~{}0.03 M ⊙ of radioactive 56Ni. Although previous rapidly evolving events (e.g., SN 1885A, SN 1939B, SN 2002bj, SN 2010X) were hypothesized to be produced by the detonation of a helium shell on a white dwarf, oxygen-dominated ejecta are difficult to reconcile with this proposed mechanism. We find that the properties of SN 2005ek are consistent with either the edge-lit double detonation of a low-mass white dwarf or the iron-core collapse of a massive star, stripped by binary interaction. However, if we assume that the strong spectroscopic similarity of SN 2005ek to other SNe Ic is an indication of a similar progenitor channel, then a white-dwarf progenitor becomes very improbable. SN 2005ek may be one of the lowest mass stripped-envelope core-collapse explosions ever observed. We find that the rate of such rapidly declining Type I events is at least 1\%-3\% of the normal SN Ia rate.},
author = {Drout, M. R. and Soderberg, A. M. and Mazzali, P. A. and Parrent, J. T. and Margutti, R. and Milisavljevic, D. and Sanders, N. E. and Chornock, R. and Foley, R. J. and Kirshner, R. P. and Filippenko, A. V. and Li, W. and Brown, P. J. and Cenko, S. B. and Chakraborti, S. and Challis, P. and Friedman, A. and Ganeshalingam, M. and Hicken, M. and Jensen, C. and Modjaz, M. and Perets, H. B. and Silverman, J. M. and Wong, D. S.},
doi = {10.1088/0004-637X/774/1/58},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {supernovae: general,supernovae: individual: SN2005ek},
month = {sep},
number = {1},
pages = {58},
title = {{THE FAST AND FURIOUS DECAY OF THE PECULIAR TYPE Ic SUPERNOVA 2005ek}},
url = {http://adsabs.harvard.edu/abs/2013ApJ...774...58D},
volume = {774},
year = {2013},
}
@article{2008A&A...479...49B,
author = {Botticella, M T and Riello, M and Cappellaro, E and Benetti, S and Altavilla, G and Pastorello, A and Turatto, M and Greggio, L and Patat, F and Valenti, S and Zampieri, L and Harutyunyan, A and Pignata, G and Taubenberger, S},
journal = {Astronomy and Astrophysics},
month = {feb},
number = {1},
pages = {49--66},
title = {{Supernova rates from the Southern inTermediate Redshift ESO Supernova Search (STRESS)}},
volume = {479},
year = {2008},
}
@article{2010ApJ...714L..52S,
author = {Sim, S.\~{}A. and R\"{o}pke, F.\~{}K. and Hillebrandt, W and Kromer, M and Pakmor, R and Fink, M and Ruiter, A.\~{}J. and Seitenzahl, I.\~{}R.},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/The Astrophysical Journal Letters/2010 Sim.pdf:pdf},
journal = {The Astrophysical Journal Letters},
month = {may},
number = {1},
pages = {L52--------L57},
title = {{Detonations in Sub-Chandrasekhar-mass C+O White Dwarfs}},
volume = {714},
year = {2010},
}
@article{2005NCimC..28..767R,
author = {Reichart, D and Nysewander, M and Moran, J and Bartelme, J and Bayliss, M and Foster, A and Clemens, J C and Price, P and Evans, C and Salmonson, J and Trammell, S and Carney, B and Keohane, J and Gotwals, R},
journal = {Il Nuovo Cimento C},
month = {jul},
number = {4},
pages = {767},
title = {{PROMPT: Panchromatic Robotic Optical Monitoring and Polarimetry Telescopes}},
volume = {28},
year = {2005},
}
@article{Clough2005,
abstract = {The radiative transfer models developed at AER are being used extensively for a wide range of applications in the atmospheric sciences. This communication is intended to provide a coherent summary of the various radiative transfer models and associated databases publicly available from AER (http://www.rtweb.aer.com). Among the communities using the models are the remote sensing community (e.g. TES, IASI), the numerical weather prediction community (e.g. ECMWF, NCEP GFS, WRF, MM5), and the climate community (e.g. ECHAM5). Included in this communication is a description of the central features and recent updates for the following models: the line-by-line radiative transfer model (LBLRTM); the line file creation program (LNFL); the longwave and shortwave rapid radiative transfer models, RRTM\_LW and RRTM\_SW; the Monochromatic Radiative Transfer Model (MonoRTM); the MT\_CKD Continuum; and the Kurucz Solar Source Function. LBLRTM and the associated line parameter database (e.g. HITRAN 2000 with 2001 updates) play a central role in the suite of models. The physics adopted for LBLRTM has been extensively analyzed in the context of closure experiments involving the evaluation of the model inputs (e.g. atmospheric state), spectral radiative measurements and the spectral model output. The rapid radiative transfer models are then developed and evaluated using the validated LBLRTM model.},
author = {Clough, S.A. and Shephard, M.W. and Mlawer, E.J. and Delamere, J.S. and Iacono, M.J. and Cady-Pereira, K. and Boukabara, S. and Brown, P.D.},
doi = {10.1016/j.jqsrt.2004.05.058},
issn = {00224073},
journal = {Journal of Quantitative Spectroscopy and Radiative Transfer},
month = {mar},
number = {2},
pages = {233--244},
title = {{Atmospheric radiative transfer modeling: a summary of the AER codes}},
url = {http://adsabs.harvard.edu/abs/2005JQSRT..91..233C},
volume = {91},
year = {2005},
}
@article{Hendry2005,
abstract = {We present photometric and spectroscopic data of the Type II-P supernova (SN II-P) 2003gd, which was discovered in M74 close to the end of its plateau phase. SN 2003gd is the first Type II supernova (SN) to have a directly confirmed red supergiant (RSG) progenitor. We compare SN 2003gd to SN 1999em, a similar SN II-P, and estimate an explosion date of 2003 March 18. We determine a reddening towards the SN of E(B-V) = 0.14 +/- 0.06, using three different methods. We also calculate three new distances to M74 of 9.6 +/- 2.8, 7.7 +/- 1.7 and 9.6 +/- 2.2Mpc. The former was estimated using the standard candle method (SCM), for Type II supernovae (SNe II), and the latter two using the brightest supergiants method (BSM). When combined with existing kinematic and BSM distance estimates, we derive a mean value of 9.3 +/- 1.8Mpc. SN 2003gd was found to have a lower tail luminosity compared with other normal Type II-P supernovae (SNe II-P) bringing into question the nature of this SN. We present a discussion concluding that this is a normal SN II-P, which is consistent with the observed progenitor mass of 8+4-2 Msolar.},
author = {Hendry, M. A. and Smartt, S. J. and Maund, J. R. and Pastorello, A. and Zampieri, L. and Benetti, S. and Turatto, M. and Cappellaro, E. and Meikle, W. P. S. and Kotak, R. and Irwin, M. J. and Jonker, P. G. and Vermaas, L. and Peletier, R. F. and van Woerden, H. and Exter, K. M. and Pollacco, D. L. and Leon, S. and Verley, S. and Benn, C. R. and Pignata, G.},
doi = {10.1111/j.1365-2966.2005.08928.x},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {galaxies: distances and redshifts,galaxies: individual: M74,stars: evolution,supernovae: general,supernovae: individual: SN 2003gd},
month = {may},
number = {3},
pages = {906--926},
title = {{A study of the Type II-P supernova 2003gd in M74}},
url = {http://adsabs.harvard.edu/abs/2005MNRAS.359..906H},
volume = {359},
year = {2005},
}
@article{2001AJ....121.1648M,
author = {Matheson, Thomas and Filippenko, Alexei V and Li, Weidong and Leonard, Douglas C and Shields, Joseph C},
doi = {10.1086/319390},
file = {:Users/svalenti/Documents/Mendeley Desktop/2001/The Astronomical Journal/2001 Matheson.pdf:pdf},
issn = {00046256},
journal = {The Astronomical Journal},
keywords = {gamma rays \`{e} stars,general,mass loss \`{e} supernovae},
month = {mar},
number = {3},
pages = {1648--1675},
title = {{Optical Spectroscopy of Type IB/C Supernovae}},
url = {http://stacks.iop.org/1538-3881/121/i=3/a=1648},
volume = {121},
year = {2001},
}
@article{Maeda2007,
author = {Maeda, K. and Tanaka, M. and Nomoto, K. and Tominaga, N. and Kawabata, K. and Mazzali, P. a. and Umeda, H. and Suzuki, T. and Hattori, T.},
doi = {10.1086/520054},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/The Astrophysical Journal/2007 Maeda.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {sep},
number = {2},
pages = {1069--1082},
title = {{The Unique Type Ib Supernova 2005bf at Nebular Phases: A Possible Birth Event of a Strongly Magnetized Neutron Star}},
url = {http://stacks.iop.org/0004-637X/666/i=2/a=1069},
volume = {666},
year = {2007},
}
@article{2013CBET.3422....2B,
abstract = {CBET 3421 available at Central Bureau for Astronomical Telegrams.},
author = {Blanchard, P. and Zheng, W. and Cenko, S. B. and Li, W. and Filippenko, A. V. and Brimacombe, J. and Martignoni, M. and Cucchiara, A. and Valenti, S. and Sand, D. and Parrent, J. T. and Graham, M. L. and Howell, D. A.},
journal = {Central Bureau Electronic Telegrams},
title = {{Supernova 2013ab in NGC 5669 = Psn J14324449+0953123}},
url = {http://adsabs.harvard.edu/abs/2013CBET.3421....1B},
year = {2013},
}
@article{Houck1996,
author = {Houck, John C. and Fransson, Claes},
doi = {10.1086/176699},
file = {:Users/svalenti/Documents/Mendeley Desktop/1996/The Astrophysical Journal/1996 Houck.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {jan},
pages = {811},
title = {{Analysis of the Late Optical Spectra of SN 1993J}},
url = {http://adsabs.harvard.edu/doi/10.1086/176699},
volume = {456},
year = {1996},
}
@article{2013ATel.4824....1A,
abstract = {We report spectroscopic observation of PSN J14324449+0953123 (listed on the IAU Central Bureau's TOCP page). A spectrum (range 350-1000 nm) obtained robotically on Feb. 18.70 UT with the FLOYDS (FTS) spectrograph shows it to be a young type-II supernova. The spectrum shows a blue continuum with a broad feature at \~{} 4600A. The Balmer lines are not visible. Comparisons with a library of supernova spectra using the GELATO code (Harutyunyan et al.},
author = {Valenti, S. and Sand, D. and Parrent, J. T. and Graham, M. L. and Howell, D. A.},
journal = {The Astronomer's Telegram},
keywords = {Optical,Supernovae},
title = {{Spectroscopic Classification of PSN J14324449+0953123}},
url = {http://adsabs.harvard.edu/abs/2013ATel.4822....1V},
year = {2013},
}
@article{Chevalier2011,
abstract = {We examine the case where a circumstellar medium around a supernova is sufficiently opaque that a radiation dominated shock propagates in the circumstellar region. The initial propagation of the shock front into the circumstellar region can be approximated by a self-similar solution that determines the radiative energy in a shocked shell; the eventual escape of this energy gives the maximum luminosity of the supernova. If the circumstellar density is described by $\backslash$rho=Dr\^{}\{-2\} out to a radius R\_w, where D is a constant, the properties of the shock breakout radiation depend on R\_w and R\_d$\backslash$equiv$\backslash$kappa Dv\_\{sh\}/c, where $\backslash$kappa is the opacity and v\_\{sh\} is the shock velocity. If R\_w>R\_d, the rise to maximum light begins at \~{} R\_d/v\_\{sh\}; the duration of the rise is also \~{} R\_d/v\_\{sh\}; the outer parts of the opaque medium are extended and at low velocity at the time of peak luminosity; and a dense shell forms whose continued interaction with the dense mass loss gives a characteristic flatter portion of the declining light curve. If R\_w<R\_d, the rise to maximum light begins at R\_w/v\_\{sh\}; the duration of the rise is R\_w\^{}2/v\_\{sh\}R\_d; the outer parts of the opaque medium are not extended and are accelerated to high velocity by radiation pressure at the time of maximum luminosity; and a dense shell forms but does not affect the light curve near maximum. We argue that SN 2006gy is an example of the first kind of event, while SN 2010gx and related supernovae are examples of the second.},
archiveprefix = {arXiv},
arxivid = {1101.1111},
author = {Chevalier, Roger A and Irwin, Christopher M},
doi = {10.1088/2041-8205/729/1/L6},
eprint = {1101.1111},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/The Astrophysical Journal/2011 Chevalier.pdf:pdf},
issn = {2041-8205},
journal = {The Astrophysical Journal},
month = {mar},
number = {1},
pages = {L6},
title = {{Shock Breakout in Dense Mass Loss: Luminous Supernovae}},
url = {http://arxiv.org/abs/1101.1111 http://stacks.iop.org/2041-8205/729/i=1/a=L6?key=crossref.8756ced077e9151037772d5dc3b83f11},
volume = {729},
year = {2011},
}
@article{Stubbs2007,
abstract = {Motivated by the recognition that variation in the optical transmission of the atmosphere is probably the main limitation to the precision of ground-based CCD measurements of celestial fluxes, we review the physical processes that attenuate the passage of light through the Earth's atmosphere. The next generation of astronomical surveys, such as PanSTARRS and LSST, will greatly benefit from dedicated apparatus to obtain atmospheric transmission data that can be associated with each survey image. We review and compare various approaches to this measurement problem, including photometry, spectroscopy, and LIDAR. In conjunction with careful measurements of instrumental throughput, atmospheric transmission measurements should allow next-generation imaging surveys to produce photometry of unprecedented precision. Our primary concerns are the real-time determination of aerosol scattering and absorption by water along the line of sight, both of which can vary over the course of a night's observations.},
archiveprefix = {arXiv},
arxivid = {0708.1364},
author = {Stubbs, Christopher W. and High, F. William and George, Matthew R. and DeRose, Kimberly L. and Blondin, St\'{e}phane and Tonry, John L. and Chambers, Kenneth C. and Granett, Benjamin R. and Burke, David L. and Smith, R. Chris},
doi = {10.1086/522208},
eprint = {0708.1364},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/Publications of the Astronomical Society of the Pacific/2007 Stubbs.pdf:pdf},
issn = {0004-6280},
journal = {Publications of the Astronomical Society of the Pacific},
month = {oct},
number = {860},
pages = {1163--1178},
title = {{Toward More Precise Survey Photometry for PanSTARRS and LSST: Measuring Directly the Optical Transmission Spectrum of the Atmosphere}},
url = {http://arxiv.org/abs/0708.1364 http://www.jstor.org/stable/10.1086/522208},
volume = {119},
year = {2007},
}
@article{Uomoto1986,
author = {Uomoto, Alan},
doi = {10.1086/184777},
file = {:Users/svalenti/Documents/Mendeley Desktop/1986/The Astrophysical Journal/1986 Uomoto.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {nov},
pages = {L35},
title = {{What stars become peculiar type I supernovae?}},
url = {http://adsabs.harvard.edu/doi/10.1086/184777},
volume = {310},
year = {1986},
}
@article{2009ApJ...696..713S,
author = {Stritzinger, Maximilian and Mazzali, Paolo and Phillips, Mark M. and Immler, Stefan and Soderberg, Alicia and Sollerman, Jesper and Boldt, Luis and Braithwaite, Jonathan and Brown, Peter and Burns, Christopher R. and Contreras, Carlos and Covarrubias, Ricardo and Folatelli, Gast\'{o}n and Freedman, Wendy L. and Gonz\'{a}lez, Sergio and Hamuy, Mario and Krzeminski, Wojtek and Madore, Barry F. and Milne, Peter and Morrell, Nidia and Persson, S. E. and Roth, Miguel and Smith, Mathew and Suntzeff, Nicholas B.},
doi = {10.1088/0004-637X/696/1/713},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/The Astrophysical Journal/2009 Stritzinger.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {may},
number = {1},
pages = {713--728},
title = {{the He-Rich Core-Collapse Supernova 2007Y: Observations From X-Ray To Radio Wavelengths}},
url = {http://stacks.iop.org/0004-637X/696/i=1/a=713?key=crossref.e4554b279d69c4296deb61a031ed9915},
volume = {696},
year = {2009},
}
@article{MarguttiR.2013,
abstract = {SN2013ab has been recently classified as a young type II supernova in NGC 5669 (CBET 3422, Atel \#4823, Atel \#4824). A Swift-ToO was executed starting from 2013-02-21T02:31:55 UT. Using 1.2 ks of Swift/XRT observation we find no evidence for X-ray emission arising from PSN J14324449+0953123 down to a 3-sigma limit of 1.2E-02 cts/s in the 0.3-10 keV energy band. The Galactic neutral hydrogen column density in the direction of the transient is 1.87d20 1/cm2 (Kalberla 2005).},
author = {{Margutti, R.} and {Soderberg, A. M.} and {Milisavljevic, D.}},
journal = {The Astronomer's Telegram},
keywords = {Optical,Supernovae,Transient,Ultra-Violet},
title = {{Swift observations of the young SN II in NGC 5669 (SN2013ab)}},
url = {http://adsabs.harvard.edu/abs/2013ATel.4832....1M},
year = {2013},
}
@article{2009Natur.462..624G,
author = {Gal-Yam, A and Mazzali, P and Ofek, E O and Nugent, P.\~{}E. and Kulkarni, S.\~{}R. and Kasliwal, M.\~{}M. and Quimby, R.\~{}M. and Filippenko, A V and Cenko, S.\~{}B. and Chornock, R and Waldman, R and Kasen, D and Sullivan, M and Beshore, E C and Drake, A J and Thomas, R C and Bloom, J.\~{}S. and Poznanski, D and Miller, A A and Foley, R J and Silverman, J.\~{}M. and Arcavi, I and Ellis, R S and Deng, J},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/Nature/2009 Gal-Yam.pdf:pdf},
journal = {Nature},
month = {dec},
number = {7},
pages = {624--627},
title = {{Supernova 2007bi as a pair-instability explosion}},
volume = {462},
year = {2009},
}
@article{1982ApJ...253..785A,
author = {Arnett, W. D.},
doi = {10.1086/159681},
file = {:Users/svalenti/Documents/Mendeley Desktop/1982/The Astrophysical Journal/1982 Arnett.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {feb},
pages = {785},
title = {{Type I supernovae. I - Analytic solutions for the early part of the light curve}},
url = {http://adsabs.harvard.edu/doi/10.1086/159681},
volume = {253},
year = {1982},
}
@article{Nomoto1991,
author = {Nomoto, Ken'ichi and Kondo, Yoji},
doi = {10.1086/185922},
file = {:Users/svalenti/Documents/Mendeley Desktop/1991/The Astrophysical Journal/1991 Nomoto.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {jan},
pages = {L19},
title = {{Conditions for accretion-induced collapse of white dwarfs}},
url = {http://adsabs.harvard.edu/doi/10.1086/185922},
volume = {367},
year = {1991},
}
@article{2012ApJ...753...67B,
author = {Bufano, Filomena and Pian, Elena and Sollerman, Jesper and Benetti, Stefano and Pignata, Giuliano and Valenti, Stefano and Covino, Stefano and D'Avanzo, Paolo and Malesani, Daniele and Cappellaro, Enrico and della Valle, Massimo and Fynbo, Johan and Hjorth, Jens and Mazzali, Paolo A and Reichart, Daniel E and Starling, Rhaana L C and Turatto, Massimo and Vergani, Susanna D and Wiersema, Klass and Amati, Lorenzo and Bersier, David and Campana, Sergio and Cano, Zach and Castro-Tirado, Alberto J and Chincarini, Guido and D'Elia, Valerio and {de Ugarte Postigo}, Antonio and Deng, Jinsong and Ferrero, Patrizia and Filippenko, Alexei V and Goldoni, Paolo and Gorosabel, Javier and Greiner, Jochen and Hammer, Francois and Jakobsson, Pall and Kaper, Lex and Kawabata, Koji S and Klose, Sylvio and Levan, Andrew J and Maeda, Keiichi and Masetti, Nicola and Milvang-Jensen, Bo and Mirabel, Felix I and M\o ller, Palle and Nomoto, Ken'ichi and Palazzi, Eliana and Piranomonte, Silvia and Salvaterra, Ruben and Stratta, Giulia and Tagliaferri, Gianpiero and Tanaka, Masaomi and Tanvir, Nial R and Wijers, Ralph A M J},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/The Astrophysical Journal/2012 Bufano.pdf:pdf},
journal = {The Astrophysical Journal},
month = {jul},
number = {1},
pages = {67},
title = {{The Highly Energetic Expansion of SN 2010bh Associated with GRB 100316D}},
volume = {753},
year = {2012},
}
@article{Inserra2013a,
abstract = {We report extensive observational data for five of the lowest redshift Super-Luminous Type Ic Supernovae (SL-SNe Ic) discovered to date, namely, PTF10hgi, SN2011ke, PTF11rks, SN2011kf, and SN2012il. Photometric imaging of the transients at +50 to +230 days after peak combined with host galaxy subtraction reveals a luminous tail phase for four of these SL-SNe. A high-resolution, optical, and near-infrared spectrum from xshooter provides detection of a broad He I $\lambda$10830 emission line in the spectrum (+50 days) of SN2012il, revealing that at least some SL-SNe Ic are not completely helium-free. At first sight, the tail luminosity decline rates that we measure are consistent with the radioactive decay of 56Co, and would require 1-4 M ⊙ of 56Ni to produce the luminosity. These 56Ni masses cannot be made consistent with the short diffusion times at peak, and indeed are insufficient to power the peak luminosity. We instead favor energy deposition by newborn magnetars as the power source for these objects. A semi-analytical diffusion model with energy input from the spin-down of a magnetar reproduces the extensive light curve data well. The model predictions of ejecta velocities and temperatures which are required are in reasonable agreement with those determined from our observations. We derive magnetar energies of 0.4 <\~{} E(1051 erg) lsim 6.9 and ejecta masses of 2.3 <\~{} M ej(M ⊙) lsim 8.6. The sample of five SL-SNe Ic presented here, combined with SN 2010gx—the best sampled SL-SNe Ic so far—points toward an explosion driven by a magnetar as a viable explanation for all SL-SNe Ic.},
author = {Inserra, C. and Smartt, S. J. and Jerkstrand, A. and Valenti, S. and Fraser, M. and Wright, D. and Smith, K. and Chen, T.-W. and Kotak, R. and Pastorello, A. and Nicholl, M. and Bresolin, F. and Kudritzki, R. P. and Benetti, S. and Botticella, M. T. and Burgett, W. S. and Chambers, K. C. and Ergon, M. and Flewelling, H. and Fynbo, J. P. U. and Geier, S. and Hodapp, K. W. and Howell, D. A. and Huber, M. and Kaiser, N. and Leloudas, G. and Magill, L. and Magnier, E. A. and McCrum, M. G. and Metcalfe, N. and Price, P. A. and Rest, A. and Sollerman, J. and Sweeney, W. and Taddia, F. and Taubenberger, S. and Tonry, J. L. and Wainscoat, R. J. and Waters, C. and Young, D.},
doi = {10.1088/0004-637X/770/2/128},
file = {:Users/svalenti/Documents/Mendeley Desktop/2013/The Astrophysical Journal/apj\_770\_2\_128.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {stars: magnetars,supernovae: general,supernovae: individual: PTF10hgi PTF11rks SN 2011k},
month = {jun},
number = {2},
pages = {128},
title = {{SUPER-LUMINOUS TYPE Ic SUPERNOVAE: CATCHING A MAGNETAR BY THE TAIL}},
url = {http://adsabs.harvard.edu/abs/2013ApJ...770..128I},
volume = {770},
year = {2013},
}
@inproceedings{Kaiser2002,
abstract = {The IFA and collaborators are embarking on a project to develop a 4-telescope synoptic survey instrument. While somewhat smaller than the 6.5m class telescope envisaged by the decadal review in their proposal for a LSST, this facility will nonetheless be able to accomplish many of the LSST science goals. In this paper we will describe the motivation for a ‘distributed aperture approach for the LSST, the current concept for Pan-STARRS -- a pilot project for the LSST proper -- and its performance goals and science reach. We will also discuss how the facility may be expanded.},
author = {Kaiser, Nicholas and Aussel, Herve and Burke, Barry E. and Boesgaard, Hans and Chambers, Ken and Chun, Mark R. and Heasley, James N. and Hodapp, Klaus-Werner and Hunt, Bobby and Jedicke, Robert and Jewitt, D. and Kudritzki, Rolf and Luppino, Gerard A. and Maberry, Michael and Magnier, Eugene and Monet, David G. and Onaka, Peter M. and Pickles, Andrew J. and Rhoads, Pui Hin H. and Simon, Theodore and Szalay, Alexander and Szapudi, Istvan and Tholen, David J. and Tonry, John L. and Waterson, Mark and Wick, John},
booktitle = {Survey and Other Telescope Technologies and Discoveries. Edited by Tyson},
doi = {10.1117/12.457365},
editor = {Tyson, J. Anthony and Wolff, Sidney},
month = {dec},
pages = {154--164},
title = {{<title>Pan-STARRS: A Large Synoptic Survey Telescope Array</title>}},
url = {http://adsabs.harvard.edu/abs/2002SPIE.4836..154K},
volume = {4836},
year = {2002},
}
@article{2010Natur.465..326K,
abstract = {The unusual helium-rich (type Ib) supernova SN 2005E is distinguished from all supernovae hitherto observed by its faint and rapidly fading light curve, prominent calcium lines in late-phase spectra and lack of any mark of recent star formation near the supernova location. These properties are claimed to be explained by a helium detonation in a thin surface layer of an accreting white dwarf. Here we report that the observed properties of SN 2005cz, which appeared in an elliptical galaxy, resemble those of SN 2005E. We argue that these properties are best explained by a core-collapse supernova at the low-mass end (8-12 solar masses) of the range of massive stars that explode. Such a low-mass progenitor lost its hydrogen-rich envelope through binary interaction, had very thin oxygen-rich and silicon-rich layers above the collapsing core, and accordingly ejected a very small amount of radioactive (56)Ni and oxygen. Although the host galaxy NGC 4589 is an elliptical, some studies have revealed evidence of recent star-formation activity, consistent with the core-collapse model.},
author = {Kawabata, K S and Maeda, K and Nomoto, K and Taubenberger, S and Tanaka, M and Deng, J and Pian, E and Hattori, T and Itagaki, K},
doi = {10.1038/nature09055},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/Nature/2010 Kawabata.pdf:pdf},
issn = {1476-4687},
journal = {Nature},
month = {may},
number = {7296},
pages = {326--8},
pmid = {20485430},
publisher = {Nature Publishing Group},
title = {{A massive star origin for an unusual helium-rich supernova in an elliptical galaxy.}},
url = {http://dx.doi.org/10.1038/nature09055 http://www.ncbi.nlm.nih.gov/pubmed/20485430},
volume = {465},
year = {2010},
}
@article{Agnoletto2009,
abstract = {We present an optical photometric and spectroscopic study of the very luminous type IIn SN 2006gy for a time period spanning more than one year. In photometry, a broad, bright (M\_R\~{}-21.7) peak characterizes all BVRI light curves. Afterwards, a rapid luminosity fading is followed by a phase of slow luminosity decline between day \~{}170 and \~{}237. At late phases (>237 days), because of the large luminosity drop (>3 mag), only upper visibility limits are obtained in the B, R and I bands. In the near-infrared, two K-band detections on days 411 and 510 open new issues about dust formation or IR echoes scenarios. At all epochs the spectra are characterized by the absence of broad P-Cygni profiles and a multicomponent Halpha profile, which are the typical signatures of type IIn SNe. After maximum, spectroscopic and photometric similarities are found between SN 2006gy and bright, interaction-dominated SNe (e.g. SN 1997cy, SN 1999E and SN 2002ic). This suggests that ejecta-CSM interaction plays a key role in SN 2006gy about 6 to 8 months after maximum, sustaining the late-time-light curve. Alternatively, the late luminosity may be related to the radioactive decay of \~{}3M\_sun of 56Ni. Models of the light curve in the first 170 days suggest that the progenitor was a compact star (R\~{}6-8 10\^{}(12)cm, M\_ej\~{}5-14M\_sun), and that the SN ejecta collided with massive (6-10M\_sun), opaque clumps of previously ejected material. These clumps do not completely obscure the SN photosphere, so that at its peak the luminosity is due both to the decay of 56Ni and to interaction with CSM. A supermassive star is not required to explain the observational data, nor is an extra-ordinarily large explosion energy.},
archiveprefix = {arXiv},
arxivid = {0810.0635},
author = {Agnoletto, I and Benetti, S and Cappellaro, E and Zampieri, L and Turatto, M and Mazzali, P and Pastorello, A and Valle, M. Della and Bufano, F and Harutyunyan, A and Navasardyan, H and Elias-Rosa, N. and Taubenberger, S and Spiro, S and Valenti, S.},
doi = {10.1088/0004-637X/691/2/1348},
eprint = {0810.0635},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/The Astrophysical Journal/2009 Agnoletto.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {feb},
number = {2},
pages = {1348--1359},
title = {{SN 2006gy: Was it Really Extraordinary?}},
url = {http://arxiv.org/abs/0810.0635 http://stacks.iop.org/0004-637X/691/i=2/a=1348?key=crossref.834b1884cecc01e027711b992e27f01f},
volume = {691},
year = {2009},
}
@article{Hirschi2005,
abstract = {We present a new set of stellar yields obtained from rotating stellar models at solar metallicity covering the massive star range (12-60 solar masses). The stellar models were calculated with the latest version of the Geneva stellar evolution code described in Hirschi et al (2004). Evolution and nucleosynthesis are in general followed up to silicon burning. The yields of our non-rotating models are consistent with other calculations and differences can be understood in the light of the treatment of convection and the rate used for C12(a,g)O16. This verifies the accuracy of our calculations and gives a safe basis for studying the effects of rotation on the yields. The contributions from stellar winds and supernova explosions to the stellar yields are presented separately. We then add the two contributions to compute the total stellar yields. Below about 30 solar masses, rotation increases the total metal yields, Z, and in particular the yields of carbon and oxygen by a factor of 1.5-2.5. As a rule of thumb, the yields of a rotating 20 solar masses star are similar to the yields of a non-rotating 30 solar masses star, at least for the light elements considered in this work. For very massive stars (around 60 solar masses), rotation increases the yield of helium but does not significantly affect the yields of heavy elements.},
archiveprefix = {arXiv},
arxivid = {astro-ph/0412454},
author = {Hirschi, R and Meynet, G and Maeder, A},
doi = {10.1051/0004-6361:20041554},
eprint = {0412454},
file = {:Users/svalenti/Documents/Mendeley Desktop/2005/Astronomy and Astrophysics/2005 Hirschi.pdf:pdf},
issn = {0004-6361},
journal = {Astronomy and Astrophysics},
keywords = {abundances,evolution,rayet,rotation,stars,supernova,wolf},
month = {apr},
number = {3},
pages = {1013--1022},
primaryclass = {astro-ph},
title = {{Yields of rotating stars at solar metallicity}},
url = {http://scholar.google.com/scholar?hl=en\&btnG=Search\&q=intitle:Yields+of+rotating+stars+at+solar+metallicity\#0 http://arxiv.org/abs/astro-ph/0412454 http://www.edpsciences.org/10.1051/0004-6361:20041554},
volume = {433},
year = {2005},
}
@article{1989A&AS...81..421B,
author = {Barbon, R and Cappellaro, E and Turatto, M},
journal = {Astronomy and Astrophysics Supplement},
month = {dec},
pages = {421},
title = {{The Asiago Supernova Catalogue}},
volume = {81},
year = {1989},
}
@article{VanDyk2013,
author = {{Van Dyk}, S. D. and Petigura, E. A. and Cenko, S. B. and Zheng, W. and Marcy, G. W. and Howard, A. W. and Foley, R. J. and Tucker, B. E. and Kelly, P. L. and Filippenko, A. V.},
journal = {The Astronomer's Telegram},
title = {{The Probable Progenitor of PSN J01364816+1545310 in M74}},
year = {2013},
}
@article{Anonymous:qMDWmRGv,
month = {may},
pages = {1--38},
title = {{Employee\{\_\}manual}},
year = {2010},
}
@article{2008ApJ...673L.155V,
author = {Valenti, S and Elias-Rosa, N. and Taubenberger, S and Stanishev, V and Agnoletto, I and Sauer, D and Cappellaro, E and Pastorello, A and Benetti, S and Riffeser, A and Hopp, U and Navasardyan, H and Tsvetkov, D and Lorenzi, V and Patat, F and Turatto, M and Barbon, R and Ciroi, S and {Di Mille}, F. and Frandsen, S and Fynbo, J P U and Laursen, P and Mazzali, P A},
doi = {10.1086/527672},
file = {:Users/svalenti/Documents/Mendeley Desktop/2008/The Astrophysical Journal/2008 Valenti.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {feb},
number = {2},
pages = {L155--L158},
title = {{The Carbon-rich Type Ic SN 2007gr: The Photospheric Phase}},
url = {http://stacks.iop.org/1538-4357/673/i=2/a=L155},
volume = {673},
year = {2008},
}
@article{Branch2002,
author = {Branch, David and Benetti, S and Kasen, Daniel and Baron, E and Jeffery, David J and Hatano, Kazuhito and Stathakis, R A and Filippenko, Alexei V and Matheson, Thomas and Pastorello, A and Altavilla, G and Cappellaro, E and Rizzi, L and Turatto, M and Li, Weidong and Leonard, Douglas C and Shields, Joseph C},
doi = {10.1086/338127},
file = {:Users/svalenti/Documents/Mendeley Desktop/2002/The Astrophysical Journal/2002 Branch.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {feb},
number = {2},
pages = {1005--1017},
title = {{Direct Analysis of Spectra of Type Ib Supernovae}},
url = {http://stacks.iop.org/0004-637X/566/i=2/a=1005},
volume = {566},
year = {2002},
}
@article{2006A&A...447...31A,
author = {Astier, P and Guy, J and Regnault, N and Pain, R and Aubourg, E and Balam, D and Basa, S and Carlberg, R G and Fabbro, S and Fouchez, D and Hook, I M and Howell, D.\~{}A. and Lafoux, H and Neill, J D and Palanque-Delabrouille, N and Perrett, K and Pritchet, C J and Rich, J and Sullivan, M and Taillet, R and Aldering, G and Antilogus, P and Arsenijevic, V and Balland, C and Baumont, S and Bronder, J and Courtois, H and Ellis, R S and Filiol, M and Gon\c{c}alves, A C and Goobar, A and Guide, D and Hardin, D and Lusset, V and Lidman, C and McMahon, R and Mouchet, M and Mourao, A and Perlmutter, S and Ripoche, P and Tao, C and Walton, N},
journal = {Astronomy and Astrophysics},
month = {feb},
number = {1},
pages = {31--48},
title = {{The Supernova Legacy Survey: measurement of $\Omega$M, $\Omega$$\Lambda$ and w from the first year data set}},
volume = {447},
year = {2006},
}
@article{2012ATel.4047....1B,
author = {Benitez-Herrera, S and Taubenberger, S and Valenti, S and Benetti, S and Pastorello, A},
journal = {The Astronomer's Telegram},
month = {apr},
pages = {1},
title = {{ESO-NTT Large Program spectroscopic classification of SNhunt 121}},
volume = {4047},
year = {2012},
}
@article{2009ApJ...698.1307T,
author = {Th\"{o}ne, Christina C and Micha$\backslash$lowski, Micha$\backslash$l J and Leloudas, Giorgos and Cox, Nick L J and Fynbo, Johan P U and Sollerman, Jesper and Hjorth, Jens and Vreeswijk, Paul M},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/The Astrophysical Journal/2009 Th\"{o}ne.pdf:pdf},
journal = {The Astrophysical Journal},
month = {jun},
number = {2},
pages = {1307--1320},
title = {{NGC 2770: A Supernova Ib Factory?}},
volume = {698},
year = {2009},
}
@article{Kewley2002,
author = {Kewley, L. J. and Dopita, M. A.},
doi = {10.1086/341326},
file = {:Users/svalenti/Documents/Mendeley Desktop/2002/The Astrophysical Journal Supplement Series/2002 Kewley.pdf:pdf},
issn = {0067-0049},
journal = {The Astrophysical Journal Supplement Series},
month = {sep},
number = {1},
pages = {35--52},
title = {{Using Strong Lines to Estimate Abundances in Extragalactic H ii Regions and Starburst Galaxies}},
url = {http://stacks.iop.org/0067-0049/142/i=1/a=35},
volume = {142},
year = {2002},
}
@article{Foley2013,
abstract = {We describe observed properties of the Type Iax class of supernovae (SNe Iax), consisting of SNe observationally similar to its prototypical member, SN 2002cx. The class currently has 25 members, and we present optical photometry and/or optical spectroscopy for most of them. SNe Iax are spectroscopically similar to SNe Ia, but have lower maximum-light velocities (2000 < |v| < 8000 km/s), typically lower peak magnitudes (-14.2 > M\_V,peak > -18.9 mag), and most have hot photospheres. Relative to SNe Ia, SNe Iax have low luminosities for their light-curve shape. There is a correlation between luminosity and light-curve shape, similar to that of SNe Ia, but offset from that of SNe Ia and with larger scatter. Despite a host-galaxy morphology distribution that is highly skewed to late-type galaxies without any SNe Iax discovered in elliptical galaxies, there are several indications that the progenitor stars are white dwarfs (WDs): evidence of C/O burning in their maximum-light spectra, low ejecta masses, strong Fe lines in their late-time spectra, a lack of X-ray detections, and deep limits on massive stars and star formation at the SN sites. However, two SNe Iax show strong He lines in their spectra. The progenitor system and explosion model that best fits all of the data is a binary system of a C/O WD that accretes matter from a He star and has a significant deflagration. At least some of the time, this explosion will not disrupt the WD. We estimate that in a given volume there are 31\^{}+17\_-13 SNe Iax for every 100 SNe Ia, and for every 1 M\_sun of iron generated by SNe Ia at z = 0, SNe Iax generate 0.052\^{}+0.017\_-0.014 M\_sun. Being the largest class of peculiar SNe, thousands of SNe Iax will be discovered by LSST. Future detailed observations of SNe Iax should further our understanding of both their progenitor systems and explosions as well as those of SNe Ia.},
archiveprefix = {arXiv},
arxivid = {1212.2209},
author = {Foley, Ryan J and Challis, P J and Chornock, R and Ganeshalingam, M and Li, W and Marion, G H and Morrell, N I and Pignata, G and Stritzinger, M D and Silverman, J M and Wang, X and Anderson, J P and Filippenko, A V and Freedman, W L and Hamuy, M and Jha, S W and Kirshner, R P and McCully, C. and Persson, S E and Phillips, M M and Reichart, D E and Soderberg, A M},
doi = {10.1088/0004-637X/767/1/57},
eprint = {1212.2209},
file = {:Users/svalenti/Documents/Mendeley Desktop/2013/The Astrophysical Journal/arXiv 2012 Foley.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {apr},
number = {1},
pages = {57},
title = {{Type Iax Supernovae: A New Class of Stellar Explosion}},
url = {http://arxiv.org/abs/1212.2209 http://stacks.iop.org/0004-637X/767/i=1/a=57?key=crossref.be847ca54941021d2dbe7cb5b7ddacc5},
volume = {767},
year = {2013},
}
@article{2006ApJ...640..854M,
author = {Maeda, K and Nomoto, K and Mazzali, P.\~{}A. and Deng, J},
file = {:Users/svalenti/Documents/Mendeley Desktop/2006/The Astrophysical Journal/2006 Maeda.pdf:pdf},
journal = {The Astrophysical Journal},
month = {apr},
number = {2},
pages = {854--877},
title = {{Nebular Spectra of SN 1998bw Revisited: Detailed Study by One- and Two-dimensional Models}},
volume = {640},
year = {2006},
}
@article{2006AJ....131.2233R,
author = {Richardson, Dean and Branch, David and Baron, E},
file = {:Users/svalenti/Documents/Mendeley Desktop/2006/The Astronomical Journal/2006 Richardson.pdf:pdf},
journal = {The Astronomical Journal},
month = {apr},
number = {4},
pages = {2233--2244},
title = {{Absolute Magnitude Distributions and Light Curves of Stripped-Envelope Supernovae}},
volume = {131},
year = {2006},
}
@article{Riess2011,
author = {Riess, Adam G. and Macri, Lucas and Casertano, Stefano and Lampeitl, Hubert and Ferguson, Henry C. and Filippenko, Alexei V. and Jha, Saurabh W. and Li, Weidong and Chornock, Ryan},
doi = {10.1088/0004-637X/730/2/119},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/The Astrophysical Journal/2011 Riess.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {cepheids,cosmological parameters,dark energy,distance scale,distances and redshifts,galaxies,general,machine-readable table,online-only material,stars,supernovae,variables},
month = {apr},
number = {2},
pages = {119},
title = {{a 3\% Solution: Determination of the Hubble Constant With the Hubble Space Telescope and Wide Field Camera 3}},
url = {http://stacks.iop.org/0004-637X/730/i=2/a=119?key=crossref.0346fbe7b96549057efaa663496febef},
volume = {730},
year = {2011},
}
@article{1995A&AS..110..513B,
author = {Barbon, R and Benetti, S and Cappellaro, E and Patat, F and Turatto, M and Iijima, T},
journal = {Astronomy and Astrophysics Supplement},
month = {may},
pages = {513},
title = {{SN 1993J in M 81: One year of observations at Asiago.}},
volume = {110},
year = {1995},
}
@article{Benetti2011,
author = {Benetti, S. and Turatto, M. and Valenti, S. and Pastorello, a. and Cappellaro, E. and Botticella, M. T. and Bufano, F. and Ghinassi, F. and Harutyunyan, a. and Inserra, C. and Magazz\`{u}, a. and Patat, F. and Pumo, M. L. and Taubenberger, S.},
doi = {10.1111/j.1365-2966.2010.17873.x},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2011 Benetti.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {1 i n t,1999dn,are defined,as the subclass of,cc-sne,core-collapse explosions,general,in the supernova,individual,ro d u c,sn,snib,supernovae,t i o n,taxonomy,type ib sne,whose early-},
month = {mar},
number = {4},
pages = {2726--2738},
title = {{The Type Ib SN 1999dn: one year of photometric and spectroscopic monitoring★}},
url = {http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2010.17873.x},
volume = {411},
year = {2011},
}
@article{Heger2002,
author = {Heger, A and Woosley, S E},
doi = {10.1086/338487},
file = {:Users/svalenti/Documents/Mendeley Desktop/2002/The Astrophysical Journal/2002 Heger.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {mar},
number = {1},
pages = {532--543},
title = {{The Nucleosynthetic Signature of Population III}},
url = {http://stacks.iop.org/0004-637X/567/i=1/a=532},
volume = {567},
year = {2002},
}
@article{Yuan2013,
abstract = {We put constraints on the properties of the progenitors of peculiar calcium-rich transients using the distribution of locations within their host galaxies. We confirm that this class of transients do not follow the galaxy stellar mass profile and are more likely to be found in remote locations of their apparent hosts. We test the hypothesis that these transients are from low metallicity progenitors by comparing their spatial distributions with the predictions of self-consistent cosmological simulations that include star formation and chemical enrichment. We find that while metal-poor stars and our transient sample show a consistent preference for large offsets, metallicity alone cannot explain the extreme cases. Invoking a lower age limit on the progenitor helps to improve the match, indicating these events may result from a very old metal-poor population. We also investigate the radial distribution of globular cluster systems, and show that they too are consistent with the class of calcium-rich transients. Because photometric upper limits exist for globular clusters for some members of the class, a production mechanism related to the dense environment of globular clusters is not favoured for the calcium-rich events. However the methods developed in this paper may be used in the future to constrain the effects of low metallicity on radially distant core-collapse events or help establish a correlation with globular clusters for other classes of peculiar explosions.},
archiveprefix = {arXiv},
arxivid = {1304.2400},
author = {Yuan, F. and Kobayashi, C. and Schmidt, B. P. and Podsiadlowski, P. and Sim, S. A. and Scalzo, R. A.},
doi = {10.1093/mnras/stt591},
eprint = {1304.2400},
file = {:Users/svalenti/Documents/Mendeley Desktop/2013/Monthly Notices of the Royal Astronomical Society/Yuan et al. - 2013 - Locations of peculiar supernovae as a diagnostic of their origins.pdf:pdf},
issn = {0035-8711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {galaxies: abundances,methods: statistical,supernovae: general},
language = {en},
month = {may},
number = {2},
pages = {1680--1686},
title = {{Locations of peculiar supernovae as a diagnostic of their origins}},
url = {http://adsabs.harvard.edu/abs/2013MNRAS.tmp.1244Y},
volume = {432},
year = {2013},
}
@inproceedings{Taubenberger:un,
annote = {Source: Scopus},
author = {Taubenberger, S and Valenti, S},
booktitle = {AIP Conference Proceedings},
pages = {402--405},
title = {{Emission-line profiles in SNe Ib/c - Probing the ejecta geometry}},
}
@article{2003IAUC.8159....2F,
author = {Filippenko, A V and Chornock, R and Swift, B and Modjaz, M and Simcoe, R and Rauch, M},
journal = {IAU Circ.},
month = {jun},
pages = {2},
title = {{Supernovae 2001co, 2003H, 2003dg, and 2003dr}},
volume = {8159},
year = {2003},
}
@article{Sutherland1984,
author = {Sutherland, P. G. and Wheeler, J. C.},
doi = {10.1086/161995},
file = {:Users/svalenti/Documents/Mendeley Desktop/1984/The Astrophysical Journal/1984 Sutherland.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {may},
pages = {282},
title = {{Models for Type I supernovae - Partially incinerated white dwarfs}},
url = {http://adsabs.harvard.edu/doi/10.1086/161995},
volume = {280},
year = {1984},
}
@article{2009PASP..121.1334R,
annote = {15 pages, 6 figures, submitted to PASP},
author = {Rau, Arne and Kulkarni, Shrinivas R and Law, Nicholas M and Bloom, Joshua S and Ciardi, David and Djorgovski, George S and Fox, Derek B and Gal-Yam, Avishay and Grillmair, Carl C and Kasliwal, Mansi M and Nugent, Peter E and Ofek, Eran O and Quimby, Robert M and Reach, William T and Shara, Michael and Bildsten, Lars and Cenko, S Bradley and Drake, Andrew J and Filippenko, Alexei V and Helfand, David J and Helou, George and Howell, D Andrew and Poznanski, Dovi and Sullivan, Mark},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/Publications of the Astronomical Society of the Pacific/2009 Rau.pdf:pdf},
journal = {Publications of the Astronomical Society of the Pacific},
month = {dec},
pages = {1334--1351},
title = {{Exploring the Optical Transient Sky with the Palomar Transient Factory}},
volume = {121},
year = {2009},
}
@article{2011ApJ...731L..11N,
author = {Narayan, G and Foley, R J and Berger, E and Botticella, M T and Chornock, R and Huber, M E and Rest, A and Scolnic, D and Smartt, S and Valenti, S and Soderberg, A.\~{}M. and Burgett, W S and Chambers, K C and Flewelling, H A and Gates, G and Grav, T and Kaiser, N and Kirshner, R P and Magnier, E A and Morgan, J S and Price, P A and Riess, A.\~{}G. and Stubbs, C W and Sweeney, W E and Tonry, J L and Wainscoat, R J and Waters, C and Wood-Vasey, W M},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/The Astrophysical Journal Letters/2011 Narayan.pdf:pdf},
journal = {The Astrophysical Journal Letters},
month = {apr},
number = {1},
pages = {L11},
title = {{Displaying the Heterogeneity of the SN 2002cx-like Subclass of Type Ia Supernovae with Observations of the Pan-STARRS-1 Discovered SN 2009ku}},
volume = {731},
year = {2011},
}
@article{Tomasella2013,
archiveprefix = {arXiv},
arxivid = {1305.5789},
author = {Tomasella, L. and Cappellaro, E. and Fraser, M. and Pumo, M. L. and Pastorello, A. and Pignata, G. and Benetti, S. and Bufano, F. and Dennefeld, M. and Harutyunyan, A. and Iijima, T. and Jerkstrand, A. and Kankare, E. and Kotak, R. and Magill, L. and Nascimbeni, V. and Ochner, P. and Siviero, A. and Smartt, S. and Sollerman, J. and Stanishev, V. and Taddia, F. and Taubenberger, S. and Turatto, M. and Valenti, S. and Wright, D. E. and Zampieri, L.},
doi = {10.1093/mnras/stt1130},
eprint = {1305.5789},
file = {:Users/svalenti/Documents/Mendeley Desktop/2013/Monthly Notices of the Royal Astronomical Society/MNRAS-2013-Tomasella-mnras\_stt1130.pdf:pdf},
issn = {0035-8711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {galaxies: individual: NGC 3239,supernovae: general,supernovae: individual: SN 2012A},
language = {en},
month = {jul},
pages = {1813},
title = {{Comparison of progenitor mass estimates for the Type IIP SN 2012A}},
url = {http://adsabs.harvard.edu/abs/2013MNRAS.tmp.1813T},
volume = {-1},
year = {2013},
}
@article{2006A&A...450..305E,
author = {Elmhamdi, A and Danziger, I J and Branch, D and Leibundgut, B and Baron, E and Kirshner, R P},
file = {:Users/svalenti/Documents/Mendeley Desktop/2006/Astronomy and Astrophysics/2006 Elmhamdi.pdf:pdf},
journal = {Astronomy and Astrophysics},
month = {apr},
number = {1},
pages = {305--330},
title = {{Hydrogen and helium traces in type Ib-c supernovae}},
volume = {450},
year = {2006},
}
@article{Brown2013,
abstract = {Las Cumbres Observatory Global Telescope (LCOGT) is a young organization dedicated to time-domain observations at optical and (potentially) near-IR wavelengths. To this end, LCOGT is constructing a world-wide network of telescopes, including the two 2m Faulkes telescopes, as many as 17 x 1m telescopes, and as many as 23 x 40cm telescopes. These telescopes initially will be outfitted for imaging and (excepting the 40cm telescopes) spectroscopy at wavelengths between the atmospheric UV cutoff and the roughly 1-micron limit of silicon detectors. Since the first of LCOGT's 1m telescopes are now being deployed, we lay out here LCOGT's scientific goals and the requirements that these goals place on network architecture and performance, we summarize the network's present and projected level of development, and we describe our expected schedule for completing it. In the bulk of the paper, we describe in detail the technical approaches that we have adopted to attain the desired performance. In particular, we discuss our choices for the number and location of network sites, for the number and sizes of telescopes, for the specifications of the first generation of instruments, for the software that will schedule and control the network's telescopes and reduce and archive its data, and for the structure of the scientific and educational programs for which the network will provide observations.},
author = {Brown, T. M. and Baliber, N. and Bianco, F. B. and Bowman, M. and Burleson, B. and Conway, P. and Crellin, M. and Depagne, \'{E}. and {De Vera}, J. and Dilday, B. and Dragomir, D. and Dubberley, M. and Eastman, J. D. and Elphick, M. and Falarski, M. and Foale, S. and Ford, M. and Fulton, B. J. and Garza, J. and Gomez, E. L. and Graham, M. and Greene, R. and Haldeman, B. and Hawkins, E. and Haworth, B. and Haynes, R. and Hidas, M. and Hjelstrom, A. E. and Howell, D. A. and Hygelund, J. and Lister, T. A. and Lobdill, R. and Martinez, J. and Mullins, D. S. and Norbury, M. and Parrent, J. and Paulson, R. and Petry, D. L. and Pickles, A. and Posner, V. and Rosing, W. E. and Ross, R. and Sand, D. J. and Saunders, E. S. and Shobbrook, J. and Shporer, A. and Street, R. A. and Thomas, D. and Tsapras, Y. and Tufts, J. R. and Valenti, S. and {Vander Horst}, K. and Walker, Z. and White, G. and Willis, M.},
journal = {eprint arXiv:1305.2437},
keywords = {Astrophysics - Instrumentation and Methods for Ast},
title = {{Las Cumbres Observatory Global Telescope Network}},
url = {http://adsabs.harvard.edu/abs/2013arXiv1305.2437B},
year = {2013},
}
@article{Tominaga2007,
author = {Tominaga, Nozomu and Umeda, Hideyuki and Nomoto, Ken’ichi},
doi = {10.1086/513063},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/The Astrophysical Journal/2007 Tominaga.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {may},
number = {1},
pages = {516--540},
title = {{Supernova Nucleosynthesis in Population III 13–50 M ⊙ Stars and Abundance Patterns of Extremely Metal‐poor Stars}},
url = {http://iopscience.iop.org/0004-637X/660/1/516 http://stacks.iop.org/0004-637X/660/i=1/a=516},
volume = {660},
year = {2007},
}
@article{Burke2010,
abstract = {The science goals for future ground-based all-sky surveys, such as the Dark Energy Survey, PanSTARRS, and the Large Synoptic Survey Telescope, require calibration of broadband photometry that is stable in time and uniform over the sky to precisions of 1\% or better, and absolute calibration of color measurements that are similarly accurate. This performance will need to be achieved with measurements made from multiple images taken over the course of many years, and these surveys will observe in less than ideal conditions. This paper describes a technique to implement a new strategy to directly measure variations of atmospheric transmittance at optical wavelengths and application of these measurements to calibration of ground-based observations. This strategy makes use of measurements of the spectra of a small catalog of bright probe stars as they progress across the sky and back-light the atmosphere. The signatures of optical absorption by different atmospheric constituents are recognized in these spectra by their characteristic dependences on wavelength and airmass. State-of-the-art models of atmospheric radiation transport and modern codes are used to accurately compute atmospheric extinction over a wide range of observing conditions. We present results of an observing campaign that demonstrate that correction for extinction due to molecular constituents and aerosols can be done with precisions of a few millimagnitudes with this technique.},
author = {Burke, David L. and Axelrod, T. and Blondin, St\'{e}phane and Claver, Chuck and Ivezi\'{c}, \v{Z}eljko and Jones, Lynne and Saha, Abhijit and Smith, Allyn and Smith, R. Chris and Stubbs, Christopher W.},
doi = {10.1088/0004-637X/720/1/811},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {atmospheric effects,methods: observational,surveys,techniques: photometric},
month = {sep},
number = {1},
pages = {811--823},
title = {{PRECISION DETERMINATION OF ATMOSPHERIC EXTINCTION AT OPTICAL AND NEAR-INFRARED WAVELENGTHS}},
url = {http://adsabs.harvard.edu/abs/2010ApJ...720..811B},
volume = {720},
year = {2010},
}
@article{2009ApJ...703.2205K,
author = {Kasen, Daniel and Woosley, S E},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/The Astrophysical Journal/2009 Kasen-1.pdf:pdf},
journal = {The Astrophysical Journal},
month = {oct},
number = {2},
pages = {2205--2216},
title = {{Type II Supernovae: Model Light Curves and Standard Candle Relationships}},
volume = {703},
year = {2009},
}
@article{2004MNRAS.348L..59P,
author = {Pettini, Max and Pagel, Bernard E J},
file = {:Users/svalenti/Documents/Mendeley Desktop/2004/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2004 Pettini.pdf:pdf},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {mar},
number = {3},
pages = {L59--------L63},
title = {{[OIII]/[NII] as an abundance indicator at high redshift}},
volume = {348},
year = {2004},
}
@article{Chevalier1992,
abstract = {The initial planar expansion of a supernova can be described by a self-similar solution if the progenitor star is sufficiently compact that radiative transfer effects do not play an important role during this phase. The later free expansion of the gas leads to radial power laws for the density and pressure profiles, although the effects of spherical geometry give some inaccuracy in this result. If the initial expansion does set up power laws for the density and pressure, effects of radiative diffusion can be described by a self-similar diffusion wave that moves back into the gas. The self-similar solution shows that there is a sharp transition between adiabatic flow and flow with constant comoving luminosity. The model is applied to SN 1987A and shown to aproximately reproduce the declining luminosity observed during the first few days after the explosion.},
author = {Chevalier, Roger A.},
doi = {10.1086/171612},
file = {:Users/svalenti/Documents/Mendeley Desktop/1992/The Astrophysical Journal/1992ApJ\_\_\_394\_\_599C.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {COMPUTATIONAL ASTROPHYSICS,DIFFUSION WAVES,EXPANSION,RADIATIVE TRANSFER,STELLAR ENVELOPES,STELLAR EVOLUTION,STELLAR LUMINOSITY,STELLAR MODELS,SUPERNOVA 1987A},
month = {aug},
pages = {599},
title = {{Early expansion and luminosity evolution of supernovae}},
url = {http://adsabs.harvard.edu.proxy.library.ucsb.edu:2048/abs/1992ApJ...394..599C},
volume = {394},
year = {1992},
}
@article{Kozma2005,
abstract = {Late time synthetic spectra of type Ia supernovae, based on three-dimensional deflagration models, are presented. We mainly focus on one model, “c3\_3d\_256\_10s”, for which the hydrodynamics (R\"{o}pke 2005, A\&A, 432, 969) and nucleosynthesis (Travaglio et al. 2004, A\&A, 425, 1029) was calculated up to the homologous phase of the explosion. Other models with different ignition conditions and different resolution are also briefly discussed. The synthetic spectra are compared to observed late time spectra. We find that while the model spectra after 300 to 500 days show a good agreement with the observed Fe II-III features, they also show too strong O I and C I lines compared to the observed late time spectra. The oxygen and carbon emission originates from the low-velocity unburned material in the central regions of these models. To get agreement between the models and observations we find that only a small mass of unburned material may be left in the center after the explosion. This may be a problem for pure deflagration models, although improved initial conditions, as well as higher resolution decrease the discrepancy. The relative intensity from the different ionization stages of iron is sensitive to the density of the emitting iron-rich material. We find that clumping, with the presence of low density regions, is needed to reproduce the observed iron emission, especially in the range between 4000 and 6000 \AA. Both temperature and ionization depend sensitively on density, abundances and radioactive content. This work therefore illustrates the importance of including the inhomogeneous nature of realistic three-dimensional explosion models. We briefly discuss the implications of the spectral modeling for the nature of the explosion.},
author = {Kozma, C. and Fransson, C. and Hillebrandt, W. and Travaglio, C. and Sollerman, J. and Reinecke, M. and R\"{o}pke, F. K. and Spyromilio, J.},
doi = {10.1051/0004-6361:20053044},
file = {:Users/svalenti/Documents/Mendeley Desktop/2005/Astronomy and Astrophysics/aa3044-05.pdf:pdf},
issn = {0004-6361},
journal = {Astronomy and Astrophysics},
keywords = {abundances,hydrodynamics,line: formation,line: identification,nuclear reactions,nucleosynthesis,stars: supernovae: general},
month = {jul},
number = {3},
pages = {983--995},
title = {{Three-dimensional modeling of type Ia supernovae – The power of late time spectra}},
url = {http://adsabs.harvard.edu/abs/2005A\%26A...437..983K http://www.edpsciences.org/10.1051/0004-6361:20053044},
volume = {437},
year = {2005},
}
@article{2007ApJ...670..592M,
author = {Mazzali, P.\~{}A. and Kawabata, K.\~{}S. and Maeda, K and Foley, R J and Nomoto, K and Deng, J and Suzuki, T and Iye, M and Kashikawa, N and Ohyama, Y and Filippenko, A V and Qiu, Y and Wei, J},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/The Astrophysical Journal/2007 Mazzali-1.pdf:pdf},
journal = {The Astrophysical Journal},
month = {nov},
number = {1},
pages = {592--599},
title = {{The Aspherical Properties of the Energetic Type Ic SN 2002ap as Inferred from Its Nebular Spectra}},
volume = {670},
year = {2007},
}
@article{Fryer2007,
author = {Fryer, Chris L. and Mazzali, Paolo A. and Prochaska, Jason and Cappellaro, Enrico and Panaitescu, Alin and Berger, Edo and van Putten, Maurice and van den Heuvel, Ed P. J. and Young, Patrick and Hungerford, Aimee and Rockefeller, Gabriel and Yoon, Sung‐Chul and Podsiadlowski, Philipp and Nomoto, Ken’ichi and Chevalier, Roger and Schmidt, Brian and Kulkarni, Shri},
doi = {10.1086/523768},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/Publications of the Astronomical Society of the Pacific/2007 Fryer.pdf:pdf},
issn = {0004-6280},
journal = {Publications of the Astronomical Society of the Pacific},
month = {nov},
number = {861},
pages = {1211--1232},
title = {{Constraints on Type Ib/c Supernovae and Gamma‐Ray Burst Progenitors}},
url = {http://www.journals.uchicago.edu/doi/abs/10.1086/523768},
volume = {119},
year = {2007},
}
@article{2012ApJ...755..161K,
abstract = {From the first two seasons of the Palomar Transient Factory, we identify three peculiar transients (PTF09dav, PTF10iuv, PTF11bij) with five distinguishing characteristics: peak luminosity in the gap between novae and supernovae (M\_R = 15.5 to -16.5), rapid photometric evolution (rise-time \~{}12--15 days), large photospheric velocities (\~{}6000 to 11000 km/s), early spectroscopic evolution into nebular phase (\~{}1 to 3 months) and peculiar nebular spectra dominated by Calcium. We also culled the extensive decade-long Lick Observatory Supernova Search database and identified an additional member of this group, SN 2007ke. Our choice of photometric and spectroscopic properties was motivated by SN 2005E (Perets et al. 2010). To our surprise, as in the case of SN 2005E, all four members of this group are also clearly offset from the bulk of their host galaxy. Given the well-sampled early and late-time light curves, we derive ejecta masses in the range of 0.4--0.7 Msun. Spectroscopically, we find that there may be a diversity in the photospheric phase, but the commonality is in the unusual nebular spectra. Our extensive follow-up observations rule out standard thermonuclear and standard core-collapse explosions for this class of Calcium-rich gap transients. If the progenitor is a white dwarf, we are likely seeing a detonation of the white dwarf core and perhaps, even shockfront interaction with a previously ejected nova shell. In the less likely scenario of a massive star progenitor, a very non-standard channel specific to a low-metallicity environment needs to be invoked (e.g., ejecta fallback leading to black hole formation). Detection (or lack thereof) of a faint underlying host (dwarf galaxy, cluster) will provide a crucial and decisive diagnostic to choose between these alternatives.},
annote = {From Duplicate 2 ( Calcium-rich Gap Transients in the Remote Outskirts of Galaxies - Kasliwal, Mansi M; Kulkarni, S.\~{}R.; Gal-Yam, Avishay; Nugent, Peter E; Sullivan, Mark; Bildsten, Lars; Yaron, Ofer; Perets, Hagai B; Arcavi, Iair; Ben-Ami, Sagi; Bhalerao, Varun B; Bloom, Joshua S; Cenko, S Bradley; Filippenko, Alexei V; Frail, Dale A; Ganeshalingam, Mohan; Horesh, Assaf; Howell, D Andrew; Law, Nicholas M; Leonard, Douglas C; Li, Weidong; Ofek, Eran O; Polishook, David; Poznanski, Dovi; Quimby, Robert M; Silverman, Jeffrey M; Sternberg, Assaf; Xu, Dong ) 12 figures, 3 tables},
archiveprefix = {arXiv},
arxivid = {1111.6109},
author = {Kasliwal, Mansi M. and Kulkarni, S.\~{}R. R. and Gal-Yam, Avishay and Nugent, Peter E. and Sullivan, Mark and Bildsten, Lars and Yaron, Ofer and Perets, Hagai B and Arcavi, Iair and Ben-Ami, Sagi and Bhalerao, Varun B and Bloom, Joshua S. and Cenko, S. Bradley and Filippenko, Alexei V. and Frail, Dale A. and Ganeshalingam, Mohan and Horesh, Assaf and Howell, D. Andrew and Law, Nicholas M. and Leonard, Douglas C. and Li, Weidong and Ofek, Eran O. and Polishook, David and Poznanski, Dovi and Quimby, Robert M. and Silverman, Jeffrey M. and Sternberg, Assaf and Xu, Dong},
doi = {10.1088/0004-637X/755/2/161},
eprint = {1111.6109},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/The Astrophysical Journal/2012 Kasliwal.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {aug},
number = {2},
pages = {161},
title = {{CALCIUM-RICH GAP TRANSIENTS IN THE REMOTE OUTSKIRTS OF GALAXIES}},
url = {http://arxiv.org/abs/1111.6109 http://stacks.iop.org/0004-637X/755/i=2/a=161?key=crossref.31ab5c99407bb6ddae35e0fed4ca6a56},
volume = {755},
year = {2012},
}
@article{VanDokkum2001,
abstract = {Conventional algorithms for rejecting cosmic rays in single CCD exposures rely on the contrast between cosmic rays and their surroundings and may produce erroneous results if the point-spread function is smaller than the largest cosmic rays. This paper describes a robust algorithm for cosmic-ray rejection, based on a variation of Laplacian edge detection. The algorithm identifies cosmic rays of arbitrary shapes and sizes by the sharpness of their edges and reliably discriminates between poorly sampled point sources and cosmic rays. Examples of its performance are given for spectroscopic and imaging data, including Hubble Space Telescope Wide Field Planetary Camera 2 images.},
author = {van Dokkum, Pieter G.},
doi = {10.1086/323894},
issn = {0004-6280},
journal = {Publications of the Astronomical Society of the Pacific},
keywords = {Instrumentation: Detectors,Methods: Data Analysis-techniques: image processin},
month = {nov},
number = {789},
pages = {1420--1427},
title = {{Cosmic‐Ray Rejection by Laplacian Edge Detection}},
url = {http://adsabs.harvard.edu/abs/2001PASP..113.1420V},
volume = {113},
year = {2001},
}
@article{Mazzali2006,
abstract = {Supernovae connected with long-duration gamma-ray bursts (GRBs) are hyper-energetic explosions resulting from the collapse of very massive stars ( approximately 40 M$\backslash$circ, where M$\backslash$circ is the mass of the Sun) stripped of their outer hydrogen and helium envelopes. A very massive progenitor, collapsing to a black hole, was thought to be a requirement for the launch of a GRB. Here we report the results of modelling the spectra and light curve of SN 2006aj (ref. 9), which demonstrate that the supernova had a much smaller explosion energy and ejected much less mass than the other GRB-supernovae, suggesting that it was produced by a star whose initial mass was only approximately 20 M$\backslash$circ. A star of this mass is expected to form a neutron star rather than a black hole when its core collapses. The smaller explosion energy of SN 2006aj is matched by the weakness and softness of GRB 060218 (an X-ray flash), and the weakness of the radio flux of the supernova. Our results indicate that the supernova-GRB connection extends to a much broader range of stellar masses than previously thought, possibly involving different physical mechanisms: a 'collapsar' (ref. 8) for the more massive stars collapsing to a black hole, and magnetic activity of the nascent neutron star for the less massive stars.},
archiveprefix = {arXiv},
arxivid = {astro-ph/0603567},
author = {Mazzali, Paolo A and Deng, Jinsong and Nomoto, Ken'ichi and Sauer, Daniel N and Pian, Elena and Tominaga, Nozomu and Tanaka, Masaomi and Maeda, Keiichi and Filippenko, Alexei V},
doi = {10.1038/nature05081},
eprint = {0603567},
issn = {1476-4687},
journal = {Nature},
language = {en},
month = {aug},
number = {7106},
pages = {1018--20},
pmid = {16943833},
primaryclass = {astro-ph},
title = {{A neutron-star-driven X-ray flash associated with supernova SN 2006aj.}},
url = {http://adsabs.harvard.edu/abs/2006Natur.442.1018M},
volume = {442},
year = {2006},
}
@article{2011arXiv1110.2363S,
annote = {18 pages, 10 figures, V2 has minor revisions; more information at https://www.cfa.harvard.edu/\~{}nsanders/papers/2010ay/summary.html},
author = {Sanders, Nathan E and Soderberg, A.\~{}M. M. and Valenti, S and Foley, R J and Chornock, R and Chomiuk, L and Berger, E and Smartt, S and Hurley, K and Barthelmy, S D and Levesque, E.\~{}M. M. and Narayan, G and Botticella, M T and Briggs, M S and Connaughton, V and Terada, Y and Gehrels, N and Golenetskii, S and Mazets, E and Cline, T and von Kienlin, A and Boynton, W and Chambers, K C and Grav, T and Heasley, J N and Hodapp, K W and Jedicke, R and Kaiser, N and Kirshner, R P and Kudritzki, R.-P. -P. and Luppino, G.\~{}A. A. and Lupton, R H and Magnier, E A and Monet, D G and Morgan, J S and Onaka, P M and Price, P A and Stubbs, C W and Tonry, J L and Wainscoat, R J and Waterson, M F},
doi = {10.1088/0004-637X/756/2/184},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/The Astrophysical Journal/arXiv 2011 Sanders.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {sep},
number = {2},
pages = {184},
title = {{SN 2010ay IS A LUMINOUS AND BROAD-LINED TYPE Ic SUPERNOVA WITHIN A LOW-METALLICITY HOST GALAXY}},
url = {http://stacks.iop.org/0004-637X/756/i=2/a=184?key=crossref.9dae07ab85d6e127c578ad2323fd1cba},
volume = {756},
year = {2011},
}
@article{2011MNRAS.416.2607G,
author = {Ganeshalingam, Mohan and Li, Weidong and Filippenko, Alexei V.},
doi = {10.1111/j.1365-2966.2011.19213.x},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2011 Ganeshalingam.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {oct},
number = {4},
pages = {2607--2622},
title = {{The rise-time distribution of nearby Type Ia supernovae}},
url = {http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2011.19213.x},
volume = {416},
year = {2011},
}
@article{2012arXiv1205.0571L,
annote = {8 pages, 2 Figures. To appear in the Proceedings of IAU Symposium 279 Death of Massive Stars: Supernovae and Gamma-ray Bursts (eds. P. Roming, N. Kawai, E. Pian). Contains updates with respect to Leloudas et al. (2010)},
author = {Leloudas, Giorgos},
doi = {10.1017/S1743921312012914},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/Proceedings of the International Astronomical Union/arXiv 2012 Leloudas.pdf:pdf},
issn = {1743-9213},
journal = {Proceedings of the International Astronomical Union},
month = {sep},
number = {S279},
pages = {191--198},
title = {{The locations of SNe Ib/c and their comparison to those of WR stars and GRBs}},
url = {http://www.journals.cambridge.org/abstract\_S1743921312012914},
volume = {7},
year = {2012},
}
@inproceedings{2003fthp.conf..200T,
author = {Turatto, Massimo and Benetti, Stefano and Cappellaro, Enrico},
booktitle = {From Twilight to Highlight: The Physics of Supernovae: Proceedings of the ESO/MPA/MPE Workshop Held at Garching},
organization = {INAF, Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 35122 Padova, Italia},
pages = {200},
title = {{Variety in Supernovae}},
year = {2003},
}
@article{2011MNRAS.417.1417F,
author = {Fraser, M and Ergon, M and Eldridge, J J and Valenti, S and Pastorello, A and Sollerman, J and Smartt, S.\~{}J. and Agnoletto, I and Arcavi, I and Benetti, S and Botticella, M T and Bufano, F and Campillay, A and Crockett, R M and Gal-Yam, A and Kankare, E and Leloudas, G and Maguire, K and Mattila, S and Maund, J R and Salgado, F and Stephens, A and Taubenberger, S and Turatto, M},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2011 Fraser.pdf:pdf},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {oct},
number = {2},
pages = {1417--1433},
title = {{SN 2009md: another faint supernova from a low-mass progenitor}},
volume = {417},
year = {2011},
}
@inproceedings{2007AIPC..924..358Z,
author = {Zampieri, Luca},
booktitle = {THE MULTICOLORED LANDSCAPE OF COMPACT OBJECTS AND THEIR EXPLOSIVE ORIGINS. AIP Conference Proceedings},
month = {aug},
organization = {INAF-Astronomical Observatory of Padua, Vicolo dell'Osservatorio 5, I-35122 Padova, Italy},
pages = {358--365},
title = {{Exploring the Physics of Type II Supernovae}},
year = {2007},
}
@article{Vink2004,
archiveprefix = {arXiv},
arxivid = {astro-ph/0408571},
author = {Vink�, J. and Blake, R. M. and S�rneczky, K. and Cs�k, B. and F?r�sz, G. and Csizmadia, Sz. and Kiss, L. L. and Szab�, Gy. M. and Szab�, R. and DeBond, H. and de Robertis, M. M. and Thomson, J. R. and Mochnacki, S. W.},
doi = {10.1051/0004-6361:20040272},
eprint = {0408571},
issn = {0004-6361},
journal = {Astronomy and Astrophysics},
keywords = {galaxies: individual: M 74,stars: supernovae: individual: SN 2002ap},
language = {en},
month = {nov},
number = {2},
pages = {453--464},
primaryclass = {astro-ph},
title = {{Distance of the hypernova SN�2002ap via the expanding photosphere method}},
url = {http://adsabs.harvard.edu/abs/2004A\&A...427..453V},
volume = {427},
year = {2004},
}
@article{2011A&A...530A..95L,
author = {Leloudas, G and Gallazzi, A and Sollerman, J and Stritzinger, M.\~{}D. and Fynbo, J.\~{}P.\~{}U. and Hjorth, J and Malesani, D and Micha$\backslash$lowski, M.\~{}J. and Milvang-Jensen, B and Smith, M},
journal = {Astronomy and Astrophysics},
month = {jun},
pages = {95},
title = {{The properties of SN Ib/c locations}},
volume = {530},
year = {2011},
}
@article{1992ApJ...391..246P,
author = {Podsiadlowski, Ph. and {Joss, P. C.} and Hsu, J J L},
journal = {Astrophysical Journal},
month = {may},
pages = {246--264},
title = {{Presupernova evolution in massive interacting binaries}},
volume = {391},
year = {1992},
}
@article{2011ApJ...739L..37M,
author = {Maund, J R and Fraser, M and Ergon, M and Pastorello, A and Smartt, S.\~{}J. and Sollerman, J and Benetti, S and Botticella, M T and Bufano, F and Danziger, I J and Kotak, R and Magill, L and Stephens, A W and Valenti, S},
journal = {The Astrophysical Journal Letters},
month = {oct},
number = {2},
pages = {L37},
title = {{The Yellow Supergiant Progenitor of the Type II Supernova 2011dh in M51}},
volume = {739},
year = {2011},
}
@article{2012MNRAS.420.3003S,
author = {Sim, S. a. and Fink, M. and Kromer, M. and R\"{o}pke, F. K. and Ruiter, a. J. and Hillebrandt, W.},
doi = {10.1111/j.1365-2966.2011.20162.x},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2012 Sim.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {an explosion can occur,anism for igniting such,binaries,close,e,g,general,hillebrandt,hydrodynamics,in binary systems,methods,niemeyer 2000,numerical,one possible mech-,radiative transfer,star,supernovae,wd,white dwarfs},
month = {mar},
number = {4},
pages = {3003--3016},
title = {{2D simulations of the double-detonation model for thermonuclear transients from low-mass carbon-oxygen white dwarfs}},
url = {http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2011.20162.x},
volume = {420},
year = {2012},
}
@article{Leonard2002,
abstract = {We present 30 optical spectra and 49 photometric epochs sampling the first 517 days after discovery of supernova (SN) 1999em and derive its distance through the expanding photosphere method (EPM). SN 1999em is shown to be a Type II-plateau (II-P) event, with a photometric plateau lasting until about 100 days after explosion. We identify the dominant ions responsible for most of the absorption features seen in the optical portion of the spectrum during the plateau phase. Using the weakest unblended absorption features to estimate photospheric velocity, we find the distance to SN 1999em to be D=8.2+/-0.6 Mpc, with an explosion date of HJD 2,451,475.6+/-1.4, or 5.3+/-1.4 days before discovery. We show that this distance estimate is about 10\% closer than the distance that results if the strong Fe II $\lambda$$\lambda$4924, 5018, 5169 absorption features, which have often been used in previous EPM studies, are used to estimate photospheric velocity. We examine potential sources of systematic error in EPM-derived distances and find the most significant to result from uncertainty in the theoretical modeling of the flux distribution emitted by the SN photosphere (i.e., the ``flux dilution factor''). We compare previously derived EPM distances to eight SNe II in galaxies (or members of the same group) for which a recently revised Cepheid distance exists from the Hubble Space Telescope Key Project and find DCepheids/DEPM=0.87+/-0.06 (statistical); eliminating the three SNe II distances for which a Cepheid distance exists only to a group member, and not the host galaxy itself, yields DCepheids/DEPM=0.96+/-0.09. Additional direct comparisons, especially to spectroscopically and photometrically normal SNe II-P, will certainly help to produce a more robust comparison. Finally, we investigate the possible use of SNe II-P as standard candles and find that for eight photometrically confirmed SNe II-P with previously derived EPM distances and SN 1999em, the mean plateau absolute brightness is MV(plateau)=-16.4+/-0.6 mag, implying that distances good to \~{}30\% (1 $\sigma$) may be possible without the need for a complete EPM analysis. At MV(plateau)=-15.9+/-0.2 mag, SN 1999em is somewhat fainter than the average SN II-P. The general consistency of absolute SNe II-P brightness during the plateau suggests that the standard candle assumption may allow SNe II-P to be viable cosmological beacons at z\>2.},
author = {Leonard, Douglas C. and Filippenko, Alexei V. and Gates, Elinor L. and Li, Weidong and Eastman, Ronald G. and Barth, Aaron J. and Bus, Schelte J. and Chornock, Ryan and Coil, Alison L. and Frink, Sabine and Grady, Carol A. and Harris, Alan W. and Malkan, Matthew A. and Matheson, Thomas and Quirrenbach, Andreas and Treffers, Richard R.},
doi = {10.1086/324785},
file = {:Users/svalenti/Documents/Mendeley Desktop/2002/Publications of the Astronomical Society of the Pacific/0109535v1.pdf:pdf},
issn = {0004-6280},
journal = {Publications of the Astronomical Society of the Pacific},
keywords = {Cosmology: Distance Scale,Cosmology: Observations,Galaxies: Individual: NGC Number: NGC 1637,supernovae: individual (SN 1999em)},
month = {jan},
number = {791},
pages = {35--64},
title = {{The Distance to SN 1999em in NGC 1637 from the Expanding Photosphere Method}},
url = {http://adsabs.harvard.edu/abs/2002PASP..114...35L},
volume = {114},
year = {2002},
}
@article{Kankare2012,
abstract = {Optical \$UBVRI\$ photometry and medium resolution spectroscopy of the type Ib supernova SN 2009jf, during the period \$\backslash sim -15\$ to +250days with respect to the \$B\$ maximum are reported. The light curves are broad, with an extremely slow decline. The early post-maximum decline rate in the \$V\$ band is similar to SN 2008D, however, the late phase decline rate is slower than other studied type Ib supernovae. With an absolute magnitude of \$M\_\{V\} = -17.96\backslash pm0.19\$ magnitude at peak, SN 2009jf is a normally bright supernova. The peak bolometric luminosity and the energy deposition rate via \$\^{}\{56\}\$Ni \$\backslash rightarrow\$ \$\^{}\{56\}\$Co chain indicate that \$\backslash sim \{0.17\}\^{}\{+0.03\}\_\{-0.03\}\$ M\$\_\{\backslash odot\}\$ of \$\^{}\{56\}\$Ni was ejected during the explosion. He$\backslash$,I 5876 $\backslash$AA$\backslash$ line is clearly identified in the first spectrum of day \$\backslash sim -15\$, at a velocity of \$\backslash sim 16000\$ km sec\$\^{}\{-1\}\$. The [O$\backslash$,I] 6300-6364 $\backslash$AA$\backslash$ line seen in the nebular spectrum has a multi-peaked and asymmetric emission profile, with the blue peak being stronger. The estimated flux in this line implies \$\backslash ga 1.34\$ M\$\_\backslash odot\$ oxygen was ejected. The slow evolution of the light curves of SN 2009jf indicates the presence of a massive ejecta. The high expansion velocity in the early phase and broader emission lines during the nebular phase suggest it to be an explosion with a large kinetic energy. A simple qualitative estimate leads to the ejecta mass of M\$\_\{\backslash rm ej\} = 4-9\$ M\$\_\backslash odot\$, and kinetic energy E\$\_\{\backslash rm K\} = 3-8 \backslash times 10\^{}\{51\}\$ erg. The ejected mass estimate is indicative of an initial main-sequence mass of \$\backslash ga 20- 25\$ M\$\_\backslash odot\$.},
archiveprefix = {arXiv},
arxivid = {1101.2068},
author = {Kankare, E and Ergon, M and Bufano, F. and Spyromilio, J. and Mattila, S. and Chugai, N. N. and Lundqvist, P. and Pastorello, A. and Kotak, R. and Benetti, S. and Botticella, M.-T. and Cumming, R. J. and Fransson, C. and Fraser, M. and Leloudas, G. and Miluzio, M. and Sollerman, J. and Stritzinger, M. and Turatto, M. and Valenti, S.},
doi = {10.1111/j.1365-2966.2012.21224.x},
eprint = {1101.2068},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2011 Sahu.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {general - supernovae,in-,individual,sn 2009jf - galaxies,supernovae},
month = {aug},
number = {2},
pages = {855--873},
title = {{SN 2009kn - the twin of the Type IIn supernova 1994W}},
url = {http://onlinelibrary.wiley.com/doi/10.1111/j.1365-2966.2012.21224.x/full http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2012.21224.x},
volume = {424},
year = {2012},
}
@article{2009MNRAS.394.2266P,
author = {Pastorello, A and Valenti, S and Zampieri, L and Navasardyan, H and Taubenberger, S and Smartt, S. J. and Arkharov, A. A. and B\"{a}rnbantner, O and Barwig, H and Benetti, S and Birtwhistle, P and Botticella, M T and Cappellaro, E and {Del Principe}, M and {Di Mille}, F. and {Di Rico}, G. and Dolci, M and Elias-Rosa, N and Efimova, N. V. and Fiedler, M and Harutyunyan, A and H\"{o}flich, P. A. and Kloehr, W and Larionov, V. M. and Lorenzi, V and Maund, J R and Napoleone, N and Ragni, M and Richmond, M and Ries, C and Spiro, S and Temporin, S and Turatto, M and Wheeler, J. C.},
doi = {10.1111/j.1365-2966.2009.14505.x},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2009 Pastorello.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {apr},
number = {4},
pages = {2266--2282},
title = {{SN 2005cs in M51 - II. Complete evolution in the optical and the near-infrared}},
url = {http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2009.14505.x},
volume = {394},
year = {2009},
}
@article{Sand2013a,
abstract = {We report a spectroscopic classification of PSN J00513484+2943149 located at RA=00:51:34.84 DEC=+29:43:14.9 (J2000). A spectrum (range 500-1000 nm) obtained robotically on June 28.55 UT with the FLOYDS spectrograph at Faulkes Telescope North at Haleakala shows it to be a SN Ia roughly 40 to 50 days after maximum light, and is consistent with the host galaxy (UGC 525) redshift of z=0.0164.},
author = {Sand, D. and Valenti, S. and Graham, M. L. and Howell, D. A. and Parrent, J. T.},
journal = {The Astronomer's Telegram},
keywords = {Optical,Supernovae},
title = {{Classification of PSN J00513484+2943149 with FLOYDS at Faulkes Telescope North}},
url = {http://adsabs.harvard.edu/abs/2013ATel.5175....1S},
year = {2013},
}
@article{2006AJ....131.1163S,
author = {Skrutskie, M.\~{}F. and Cutri, R.\~{}M. and Stiening, R and Weinberg, M.\~{}D. and Schneider, S and Carpenter, J.\~{}M. and Beichman, C and Capps, R and Chester, T and Elias, J and Huchra, J and Liebert, J and Lonsdale, C and Monet, D G and Price, S and Seitzer, P and Jarrett, T and Kirkpatrick, J.\~{}D. and Gizis, J.\~{}E. and Howard, E and Evans, T and Fowler, J and Fullmer, L and Hurt, R and Light, R and Kopan, E.\~{}L. and Marsh, K.\~{}A. and McCallon, H.\~{}L. and Tam, R and {Van Dyk}, S and Wheelock, S},
file = {:Users/svalenti/Documents/Mendeley Desktop/2006/The Astronomical Journal/2006 Skrutskie.pdf:pdf},
journal = {The Astronomical Journal},
month = {feb},
number = {2},
pages = {1163--1183},
title = {{The Two Micron All Sky Survey (2MASS)}},
volume = {131},
year = {2006},
}
@article{2008MNRAS.389..131P,
author = {Pastorello, A and Quimby, R.\~{}M. and Smartt, S.\~{}J. and Mattila, S and Navasardyan, H and Crockett, R M and Elias-Rosa, N and Mondol, P and Wheeler, J.\~{}C. and Young, D.\~{}R.},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {sep},
number = {1},
pages = {131--140},
title = {{Massive stars exploding in a He-rich circumstellar medium - II. The transitional case of SN 2005la}},
volume = {389},
year = {2008},
}
@article{Swartz1991,
author = {Swartz, Douglas A. and Wheeler, J. C.},
doi = {10.1086/186142},
file = {:Users/svalenti/Documents/Mendeley Desktop/1991/The Astrophysical Journal/1991 Swartz.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {sep},
pages = {L13},
title = {{The late-time light curve of SN 1984L}},
url = {http://adsabs.harvard.edu/doi/10.1086/186142},
volume = {379},
year = {1991},
}
@article{Waxman2007,
abstract = {We show that the prompt and afterglow X-ray emission of GRB 060218, as well as its early (t<\~{}1 day) optical-UV emission, can be explained by a model in which a radiation-mediated shock propagates outward from a compact progenitor star into a dense wind. The prompt thermal X-ray emission is produced in this model when the mildly relativistic shock, $\beta$\~{}0.85, carrying a few times 1049 erg, reaches the wind (Thomson) photosphere, where the postshock thermal radiation is released and the shock becomes collisionless. Adopting this interpretation of the thermal X-ray emission, we predict a subsequent X-ray afterglow, due to synchrotron emission and inverse Compton scattering of supernova UV photons by electrons accelerated in the collisionless shock. Early optical-UV emission is also predicted, due to the cooling of the outer $\delta$M\~{}10-3 Msolar envelope of the star, which was heated to high temperature during the shock passage. The observed X-ray afterglow and the early optical-UV emission are both consistent with those expected in this model. Detailed analysis of the early optical-UV emission may provide detailed constraints on the density distribution near the stellar surface.},
author = {Waxman, E. and Meszaros, P. and Campana, S.},
doi = {10.1086/520715},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/The Astrophysical Journal/71463.web.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {Gamma Rays: Bursts,Shock Waves,Stars: Supernovae: General},
month = {sep},
number = {1},
pages = {351--357},
title = {{GRB 060218: A Relativistic Supernova Shock Breakout}},
url = {http://adsabs.harvard.edu/abs/2007ApJ...667..351W},
volume = {667},
year = {2007},
}
@article{1989ApJ...343..323F,
author = {Fransson, Claes and Chevalier, Roger A.},
doi = {10.1086/167707},
file = {:Users/svalenti/Documents/Mendeley Desktop/1989/The Astrophysical Journal/1989 Fransson.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {aug},
pages = {323},
title = {{Late emission from supernovae - A window on stellar nucleosynthesis}},
url = {http://adsabs.harvard.edu/doi/10.1086/167707},
volume = {343},
year = {1989},
}
@article{Osterbrock1992,
author = {Osterbrock, Donald E. and Martel, Andre},
doi = {10.1086/132961},
file = {:Users/svalenti/Documents/Mendeley Desktop/1992/Publications of the Astronomical Society of the Pacific/1992 Osterbrock.pdf:pdf},
issn = {0004-6280},
journal = {Publications of the Astronomical Society of the Pacific},
month = {jan},
pages = {76},
title = {{Sky spectra at a light-polluted site and the use of atomic and OH sky emission lines for wavelength calibration}},
url = {http://ucp.uchicago.edu/cgi-bin/resolve?id=doi:10.1086/132961},
volume = {104},
year = {1992},
}
@article{Drout2011,
abstract = {We present detailed optical photometry for 25 Type Ibc supernovae within d$\backslash$approx150 Mpc obtained with the robotic Palomar 60-inch telescope in 2004-2007. This study represents the first uniform, systematic, and statistical sample of multi-band SNe Ibc light curves available to date. We correct the light curves for host galaxy extinction using a new technique based on the photometric color evolution, namely, we show that the (V-R) color of extinction-corrected SNe Ibc at t$\backslash$approx10 days after V-band maximum is tightly distributed, (V-R)=0.26+-0.06 mag. Using this technique, we find that SNe Ibc typically suffer from significant host galaxy extinction, E(B-V)$\backslash$approx0.4 mag. A comparison of the extinction-corrected light curves for SNe Ib and Ic reveals that they are statistically indistinguishable, both in luminosity and decline rate. We report peak absolute magnitudes of M\_R=-17.9+-0.9 mag and M\_R=-18.3+-0.6 mag for SNe Ib and Ic, respectively. Focusing on the broad-lined SNe Ic, we find that they are more luminous than the normal SNe Ibc sample, M\_R=-19.0+-1.1 mag, with a probability of only 1.6\% that they are drawn from the same population of explosions. By comparing the peak absolute magnitudes of SNe Ic-BL with those inferred for local engine-driven explosions (GRB-SN 1998bw, XRF-SN 2006aj, and SN2009bb) we find a 25\% probability that they are drawn from the SNe Ic-BL population. Finally, we fit analytic models to the light-curves to derive typical Ni-56 masses of M\_Ni $\backslash$approx0.2 and 0.5 M\_sun for SNe Ibc and SNe Ic-BL, respectively. With reasonable assumptions for the photospheric velocities, we extract kinetic energy and ejecta mass values of M\_ej $\backslash$approx 2 M\_sun and E\_K$\backslash$approx1e+51 erg for SNe Ibc, while for SNe Ic-BL we find higher values, M\_ej$\backslash$approx5 M\_sun and E\_K$\backslash$approx1e+52 erg. We discuss the implications for the progenitors of SNe Ibc and their relation to engine-driven explosions [ABRIDGED].},
archiveprefix = {arXiv},
arxivid = {1011.4959},
author = {Drout, Maria R. and Soderberg, Alicia M. and Gal-Yam, Avishay and Cenko, S. Bradley and Fox, Derek B. and Leonard, Douglas C. and Sand, David J. and Moon, Dae-Sik and Arcavi, Iair and Green, Yoav},
doi = {10.1088/0004-637X/741/2/97},
eprint = {1011.4959},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/The Astrophysical Journal/2011 Drout.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {nov},
number = {2},
pages = {97},
title = {{The First Systematic Study of Type Ibc Supernova Multi-band Light Curves}},
url = {http://arxiv.org/abs/1011.4959 http://stacks.iop.org/0004-637X/741/i=2/a=97?key=crossref.e1b83392a98538b29c76eaa9389b7731},
volume = {741},
year = {2011},
}
@article{2010ApJ...717..245K,
author = {Kasen, Daniel and Bildsten, Lars},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/The Astrophysical Journal/2010 Kasen.pdf:pdf},
journal = {The Astrophysical Journal},
month = {jul},
number = {1},
pages = {245--249},
title = {{Supernova Light Curves Powered by Young Magnetars}},
volume = {717},
year = {2010},
}
@article{2009ApJ...702..226M,
author = {Modjaz, M and Li, W and Butler, N and Chornock, R and Perley, D and Blondin, S and Bloom, J.\~{}S. and Filippenko, A V and Kirshner, R P and Kocevski, D and Poznanski, D and Hicken, M and Foley, R J and Stringfellow, G.\~{}S. and Berlind, P and y Navascues, D and Blake, C.\~{}H. and Bouy, H and Brown, W.\~{}R. and Challis, P and Chen, H and de Vries, W.\~{}H. and Dufour, P and Falco, E and Friedman, A and Ganeshalingam, M and Garnavich, P and Holden, B and Illingworth, G and Lee, N and Liebert, J and Marion, G.\~{}H. and Olivier, S.\~{}S. and Prochaska, J.\~{}X. and Silverman, J.\~{}M. and Smith, N and Starr, D and Steele, T.\~{}N. and Stockton, A and Williams, G.\~{}G. and Wood-Vasey, W M},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/The Astrophysical Journal/2009 Modjaz.pdf:pdf},
journal = {The Astrophysical Journal},
month = {sep},
number = {1},
pages = {226--248},
title = {{From Shock Breakout to Peak and Beyond: Extensive Panchromatic Observations of the Type Ib Supernova 2008D Associated with Swift X-ray Transient 080109}},
volume = {702},
year = {2009},
}
@article{Mazzali2008,
abstract = {The only supernovae (SNe) to show gamma-ray bursts (GRBs) or early x-ray emission thus far are overenergetic, broad-lined type Ic SNe (hypernovae, HNe). Recently, SN 2008D has shown several unusual features: (i) weak x-ray flash (XRF), (ii) an early, narrow optical peak, (iii) disappearance of the broad lines typical of SN Ic HNe, and (iv) development of helium lines as in SNe Ib. Detailed analysis shows that SN 2008D was not a normal supernova: Its explosion energy (E approximately 6x10(51) erg) and ejected mass [ approximately 7 times the mass of the Sun (M(middle dot in circle))] are intermediate between normal SNe Ibc and HNe. We conclude that SN 2008D was originally a approximately 30 M(middle dot in circle) star. When it collapsed, a black hole formed and a weak, mildly relativistic jet was produced, which caused the XRF. SN 2008D is probably among the weakest explosions that produce relativistic jets. Inner engine activity appears to be present whenever massive stars collapse to black holes.},
author = {Mazzali, Paolo a and Valenti, Stefano and {Della Valle}, Massimo and Chincarini, Guido and Sauer, Daniel N and Benetti, Stefano and Pian, Elena and Piran, Tsvi and D'Elia, Valerio and Elias-Rosa, Nancy and Margutti, Raffaella and Pasotti, Francesco and Antonelli, L Angelo and Bufano, Filomena and Campana, Sergio and Cappellaro, Enrico and Covino, Stefano and D'Avanzo, Paolo and Fiore, Fabrizio and Fugazza, Dino and Gilmozzi, Roberto and Hunter, Deborah and Maguire, Kate and Maiorano, Elisabetta and Marziani, Paola and Masetti, Nicola and Mirabel, Felix and Navasardyan, Hripsime and Nomoto, Ken'ichi and Palazzi, Eliana and Pastorello, Andrea and Panagia, Nino and Pellizza, L J and Sari, Re'em and Smartt, Stephen and Tagliaferri, Gianpiero and Tanaka, Masaomi and Taubenberger, Stefan and Tominaga, Nozomu and Trundle, Carrie and Turatto, Massimo},
doi = {10.1126/science.1158088},
file = {:Users/svalenti/Documents/Mendeley Desktop/2008/Science (New York, N.Y.)/2008 Mazzali.pdf:pdf},
issn = {1095-9203},
journal = {Science (New York, N.Y.)},
month = {aug},
number = {5893},
pages = {1185--8},
pmid = {18653846},
title = {{The metamorphosis of supernova SN 2008D/XRF 080109: a link between supernovae and GRBs/hypernovae.}},
url = {http://www.ncbi.nlm.nih.gov/pubmed/18653846},
volume = {321},
year = {2008},
}
@article{Vacca2003,
abstract = {We present a method for correcting near-infrared medium-resolution spectra for telluric absorption. The method makes use of a spectrum of an A0 V star, observed near in time and close in air mass to the target object, and a high-resolution model of Vega, to construct a telluric correction spectrum that is free of stellar absorption features. The technique was designed specifically to perform telluric corrections on spectra obtained with SpeX, a 0.8-5.5 $\mu$m medium-resolution cross-dispersed spectrograph at the NASA Infrared Telescope Facility, and uses the fact that for medium resolutions there exist spectral regions uncontaminated by atmospheric absorption lines. However, it is also applicable (in a somewhat modified form) to spectra obtained with other near-infrared spectrographs. An IDL-based code that carries out the procedures is available for downloading via the World Wide Web. Based on observations obtained with the Infrared Telescope Facility, which is operated by the University of Hawaii under contract to the National Aeronautics and Space Administration.},
author = {Vacca, William D. and Cushing, Michael C. and Rayner, John T.},
doi = {10.1086/346193},
issn = {0004-6280},
journal = {Publications of the Astronomical Society of the Pacific},
keywords = {Atmospheric Effects,Methods: Data Analysis,Techniques: Spectroscopic},
month = {mar},
number = {805},
pages = {389--409},
title = {{A Method of Correcting Near‐Infrared Spectra for Telluric Absorption1}},
url = {http://adsabs.harvard.edu/abs/2003PASP..115..389V},
volume = {115},
year = {2003},
}
@article{2011CBET.2695....1R,
author = {Rich, D and Brimacombe, J and Gall, E and Taubenberger, S and Maurer, I and Pakmor, R and Valenti, S and Benetti, S},
journal = {Central Bureau Electronic Telegrams},
month = {apr},
pages = {1},
title = {{Supernova 2011bm in IC 3917 = Psn J12565389+2222282}},
volume = {2695},
year = {2011},
}
@article{Fink2013,
abstract = {We investigate whether pure deflagration models of Chandrasekhar-mass carbon-oxygen white dwarf stars can account for one or more sub-class of the observed population of Type Ia supernova (SN Ia) explosions. We compute a set of three-dimensional full-star hydrodynamic explosion models, in which the deflagration strength is parametrized using the multi-spot ignition approach. For each model, we calculate detailed nucleosynthesis yields in a post-processing step with a 384 nuclide nuclear network. We also compute synthetic observables with our three-dimensional Monte-Carlo radiative transfer code for comparison with observations. For weak and intermediate deflagration strengths (energy release E\_nuc \<\~{} 1.1 x 10\^{}51 erg), we find that the explosion leaves behind a bound remnant enriched with 3 to 10 per cent (by mass) of deflagration ashes. However, we do not obtain the large kick velocities recently reported in the literature. We find that weak deflagrations with E\_nuc \~{} 0.5 x 10\^{}51 erg fit well both the light curves and spectra of 2002cx-like SNe Ia, and models with even lower explosion energies could explain some of the fainter members of this sub-class. By comparing our synthetic observables with the properties of SNe Ia, we can exclude the brightest, most vigorously ignited models as candidates for any observed class of SN Ia: their B - V colours deviate significantly from both normal and 2002cx-like SNe Ia and they are too bright to be candidates for other sub-classes.},
author = {Fink, M. and Kromer, M. and Seitenzahl, I. R. and Ciaraldi-Schoolmann, F. and Roepke, F. K. and Sim, S. A. and Pakmor, R. and Ruiter, A. J. and Hillebrandt, W.},
journal = {eprint arXiv:1308.3257},
keywords = {Astrophysics - Solar and Stellar Astrophysics},
title = {{Three-dimensional pure deflagration models with nucleosynthesis and synthetic observables for Type Ia supernovae}},
url = {http://adsabs.harvard.edu/abs/2013arXiv1308.3257F},
year = {2013},
}
@article{2009MNRAS.399..559A,
author = {Anderson, J.\~{}P. and James, P.\~{}A.},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2009 Anderson.pdf:pdf},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {oct},
number = {2},
pages = {559--573},
title = {{Comparisons of the radial distributions of core-collapse supernovae with those of young and old stellar populations}},
volume = {399},
year = {2009},
}
@article{2004ApJ...617..240K,
author = {Kobulnicky, Henry A and Kewley, Lisa J},
file = {:Users/svalenti/Documents/Mendeley Desktop/2004/The Astrophysical Journal/2004 Kobulnicky.pdf:pdf},
journal = {The Astrophysical Journal},
month = {dec},
number = {1},
pages = {240--261},
title = {{Metallicities of 0.3<z<1.0 Galaxies in the GOODS-North Field}},
volume = {617},
year = {2004},
}
@article{2012ApJ...744...38F,
author = {Foley, Ryan J and Challis, P.\~{}J. and Filippenko, A V and Ganeshalingam, M and Landsman, W and Li, W and Marion, G.\~{}H. and Silverman, J.\~{}M. and Beaton, R L and Bennert, V N and Cenko, S.\~{}B. and Childress, M and Guhathakurta, P and Jiang, L and Kalirai, J S and Kirshner, R P and Stockton, A and Tollerud, E J and Vink\'{o}, J and Wheeler, J.\~{}C. and Woo, J.-H.},
journal = {The Astrophysical Journal},
month = {jan},
number = {1},
pages = {38},
title = {{Very Early Ultraviolet and Optical Observations of the Type Ia Supernova 2009ig}},
volume = {744},
year = {2012},
}
@article{Seaton2005,
abstract = {All monochromatic opacity data from the Opacity Project (OP), together with all codes required for the calculation of mean opacities and radiative accelerations for any required chemical mixture, temperature and mass density, are being put on a 700-MB CD which will be made generally available. The present letter gives a concise summary of the contents of the CD. More complete documentation will be provided on the CD itself.},
author = {Seaton, M. J.},
doi = {10.1111/j.1365-2966.2005.00019.x},
issn = {1745-3925},
journal = {Monthly Notices of the Royal Astronomical Society: Letters},
keywords = {atomic processes,radiative transfer,stars: interiors},
month = {sep},
number = {1},
pages = {L1--L3},
title = {{Opacity Project data on CD for mean opacities and radiative accelerations}},
url = {http://adsabs.harvard.edu/abs/2005MNRAS.362L...1S},
volume = {362},
year = {2005},
}
@article{2007Natur.450..390W,
author = {Woosley, S E and Blinnikov, S and Heger, Alexander},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/Nature/2007 Woosley.pdf:pdf},
journal = {Nature},
month = {nov},
number = {7},
pages = {390--392},
title = {{Pulsational pair instability as an explanation for the most luminous supernovae}},
volume = {450},
year = {2007},
}
@article{2012arXiv1206.2643S,
abstract = {We present the largest spectroscopic study of the host environments of Type Ibc supernovae (SN Ibc) discovered exclusively by untargeted SN searches. Past studies of SN Ibc host environments have been biased towards high-mass, high-metallicity galaxies by focusing on SNe discovered in galaxy-targeted SN searches. Our new observations more than double the total number of spectroscopic stellar population age and metallicity measurements published for untargeted SN Ibc host environments, and extend to a median redshift about twice as large as previous statistical studies (z = 0.04). For the 12 SNe Ib and 21 SNe Ic in our metallicity sample, we find median metallicities of log(O/H)+12 = 8.48 and 8.61, respectively, but determine that the discrepancy in the full distribution of metallicities is not statistically significant. This median difference would correspond to only a small difference in the mass loss via metal-line driven winds (<30\%), suggesting this does not play the dominant role in distinguishing SN Ib and Ic progenitors. However, the median metallicity of the 7 broad-lined SN Ic (SN Ic-BL) in our sample is significantly lower, log(O/H)+12 = 8.34. The age of the young stellar population of SN Ic-BL host environments also seems to be lower than for SN Ib and Ic, but our age sample is small. A synthesis of SN Ibc host environment spectroscopy to date does not reveal a significant difference in SN Ib and Ic metallicities, but reinforces the significance of the lower metallicities for SN Ic-BL. This combined sample demonstrates that galaxy-targeted SN searches introduce a significant bias for studies seeking to infer the metallicity distribution of SN progenitors, and we identify and discuss other systematic effects that play smaller roles. We discuss the path forward for making progress on SN Ibc progenitor studies in the LSST era.},
annote = {From Duplicate 2 ( A Spectroscopic Study of Type Ibc Supernova Host Galaxies from Untargeted Surveys - Sanders, Nathan E; Soderberg, Alicia M; Levesque, Emily M; Foley, Ryan J; Chornock, Ryan; Milisavljevic, Dan; Margutti, Raffaella; Berger, Edo; Drout, Maria R; Czekala, Ian; Dittmann, Jason A ) 28 pages, 13 Figures, ApJ Submitted, more information at http://www.cfa.harvard.edu/\~{}nsanders/papers/Ibchosts/summary.html},
archiveprefix = {arXiv},
arxivid = {1206.2643},
author = {Sanders, Nathan E and Soderberg, Alicia M and Levesque, Emily M and Foley, Ryan J and Chornock, Ryan and Milisavljevic, Dan and Margutti, Raffaella and Berger, Edo and Drout, Maria R and Czekala, Ian and Dittmann, Jason A},
doi = {10.1088/0004-637X/758/2/132},
eprint = {1206.2643},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/arXiv.org/arXiv 2012 Sanders.pdf:pdf},
issn = {0004-637X},
journal = {arXiv.org},
month = {jun},
number = {2},
pages = {2643},
title = {{A Spectroscopic Study of Type Ibc Supernova Host Galaxies from Untargeted Surveys}},
url = {http://arxiv.org/abs/1206.2643 http://stacks.iop.org/0004-637X/758/i=2/a=132?key=crossref.b4f249ea7f9f50a6027c3e8818979bf2},
volume = {1206},
year = {2012},
}
@article{2006NuPhA.777..424N,
abstract = {We present new nucleosynthesis yields as functions of the stellar mass, metallicity, and explosion energy (corresponding to normal supernovae and Hypernovae). We apply the results to the chemical evolution of the solar neighborhood. Our new yields are based on the new developments in the observational/theoretical studies of supernovae (SNe) and extremely metal-poor (EMP) stars in the halo, which have provided excellent opportunities to test the explosion models and their nucleosynthesis. We use the light curve and spectra fitting of individual SN to estimate the mass of the progenitor, explosion energy, and produced 56Ni mass. Comparison with the abundance patterns of EMP stars has made it possible to determine the model parameters of core-collapse SNe, such as mixing-fallback parameters. More specifically, we take into account the two distinct new classes of massive SNe: 1) very energetic Hypernovae, whose kinetic energy (KE) is more than 10 times the KE of normal core-collapse SNe, and 2) very faint and low energy SNe (Faint SNe). These two new classes of SNe are likely to be ``black-hole-forming'' SNe with rotating or non-rotating black holes. Nucleosynthesis in Hypernovae is characterized by larger abundance ratios (Zn,Co,V,Ti)/Fe and smaller (Mn,Cr)/Fe than normal SNe, which can explain the observed trends of these ratios in EMP stars. Nucleosynthesis in Faint SNe is characterized by a large amount of fall-back, which explains the abundance pattern of the most Fe-poor stars. These comparisons suggest that black-hole-forming SNe made important contributions to the early Galactic (and cosmic) chemical evolution.},
archiveprefix = {arXiv},
arxivid = {astro-ph/0605725},
author = {Nomoto, Ken'ichi and Tominaga, Nozomu and Umeda, Hideyuki and Kobayashi, Chiaki and Maeda, Keiichi},
doi = {10.1016/j.nuclphysa.2006.05.008},
eprint = {0605725},
file = {:Users/svalenti/Documents/Mendeley Desktop/2006/Nuclear Physics A/Nuclear Physics A 2006 Nomoto.pdf:pdf},
issn = {03759474},
journal = {Nuclear Physics A},
month = {oct},
number = {February 2008},
pages = {424--458},
primaryclass = {astro-ph},
title = {{Nucleosynthesis yields of core-collapse supernovae and hypernovae, and galactic chemical evolution}},
url = {http://arxiv.org/abs/astro-ph/0605725 http://linkinghub.elsevier.com/retrieve/pii/S0375947406001953},
volume = {777},
year = {2006},
}
@article{2007Msngr.127...11G,
author = {Gilmozzi, R and Spyromilio, J},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/The Messenger/2007 Gilmozzi.pdf:pdf},
journal = {The Messenger},
month = {mar},
pages = {11},
title = {{The European Extremely Large Telescope (E-ELT)}},
volume = {127},
year = {2007},
}
@article{2005MNRAS.360..950P,
author = {Pastorello, A and Baron, E and Branch, D and Zampieri, L and Turatto, M and Ramina, M and Benetti, S and Cappellaro, E and Salvo, M and Patat, F and Piemonte, A and Sollerman, J and Leibundgut, B and Altavilla, G},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {jul},
number = {3},
pages = {950--962},
title = {{SN 1998A: explosion of a blue supergiant}},
volume = {360},
year = {2005},
}
@article{2011arXiv1110.1377K,
annote = {Comments welcome, submitted to ApJ, v2 has minor revisions},
author = {Kelly, Patrick L and Kirshner, Robert P},
doi = {10.1088/0004-637X/759/2/107},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/The Astrophysical Journal/arXiv 2011 Kelly.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {nov},
number = {2},
pages = {1377},
title = {{Core-Collapse Supernovae and Host Galaxy Stellar Populations}},
url = {http://stacks.iop.org/0004-637X/759/i=2/a=107?key=crossref.7fd16a43e4d068bf1c58c287cbcd5a5e},
volume = {759},
year = {2011},
}
@article{1990A&A...237...79B,
author = {Barbon, R and Benetti, S and Rosino, L and Cappellaro, E and Turatto, M},
journal = {Astronomy and Astrophysics (ISSN 0004-6361)},
month = {oct},
pages = {79--90},
title = {{Type IA supernova 1989B in NGC 3627}},
volume = {237},
year = {1990},
}
@article{Hillebrandt2000,
author = {Hillebrandt, Wolfgang and Niemeyer, Jens C},
doi = {10.1146/annurev.astro.38.1.191},
file = {:Users/svalenti/Documents/Mendeley Desktop/2000/Annual Review of Astronomy and Astrophysics/2000 Hillebrandt.pdf:pdf},
issn = {0066-4146},
journal = {Annual Review of Astronomy and Astrophysics},
keywords = {abstract because calibrated light,also its geomet-,considerable attention has been,curves of type ia,given to models of,hydrodynamics,major tool to determine,of the universe and,rical structure,stellar evolution,supernovae have become a,the local expansion rate,these events over},
month = {sep},
number = {1},
pages = {191--230},
title = {{Type IA Supernova Explosion Models}},
url = {http://www.annualreviews.org/doi/abs/10.1146/annurev.astro.38.1.191},
volume = {38},
year = {2000},
}
@article{Ofek2007,
author = {Ofek, E O and Cameron, P B and Kasliwal, M M and Gal-Yam, A. and Rau, A and Kulkarni, S R and Frail, D A and Chandra, P and Cenko, S B and Soderberg, A M and Immler, S},
doi = {10.1086/516749},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/The Astrophysical Journal/2007 Ofek-1.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {apr},
number = {1},
pages = {L13--L16},
title = {{SN 2006gy: An Extremely Luminous Supernova in the Galaxy NGC 1260}},
url = {http://stacks.iop.org/1538-4357/659/i=1/a=L13},
volume = {659},
year = {2007},
}
@article{2012A&A...537A.141P,
author = {Pastorello, A and Pumo, M L and Navasardyan, H and Zampieri, L and Turatto, M and Sollerman, J and Taddia, F and Kankare, E and Mattila, S and Nicolas, J and Prosperi, E and {San Segundo Delgado}, A and Taubenberger, S and Boles, T and Bachini, M and Benetti, S and Bufano, F and Cappellaro, E and Cason, A D and Cetrulo, G and Ergon, M and Germany, L and Harutyunyan, A and Howerton, S and Hurst, G M and Patat, F and Stritzinger, M and Strolger, L.-G. and Wells, W},
journal = {Astronomy and Astrophysics},
month = {jan},
pages = {141},
title = {{SN 2009E: a faint clone of SN 1987A}},
volume = {537},
year = {2012},
}
@article{2009ARA&A..47...63S,
author = {Smartt, Stephen J},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/Annual Review of Astronomy \{\&\} Astrophysics/2009 Smartt.pdf:pdf},
journal = {Annual Review of Astronomy \{\&\} Astrophysics},
month = {sep},
number = {1},
pages = {63--106},
title = {{Progenitors of Core-Collapse Supernovae}},
volume = {47},
year = {2009},
}
@article{2007MNRAS.376.1301P,
author = {Pastorello, A and Taubenberger, S and Elias-Rosa, N and Mazzali, P.\~{}A. and Pignata, G and Cappellaro, E and Garavini, G and Nobili, S and Anupama, G.\~{}C. and Bayliss, D D R and Benetti, S and Bufano, F and Chakradhari, N K and Kotak, R and Goobar, A and Navasardyan, H and Patat, F and Sahu, D.\~{}K. and Salvo, M and Schmidt, B P and Stanishev, V and Turatto, M and Hillebrandt, W},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {apr},
number = {3},
pages = {1301--1316},
title = {{ESC observations of SN 2005cf - I. Photometric evolution of a normal Type Ia supernova}},
volume = {376},
year = {2007},
}
@article{2012MNRAS.422.1122I,
author = {Inserra, C and Turatto, M and Pastorello, A and Pumo, M L and Baron, E and Benetti, S and Cappellaro, E and Taubenberger, S and Bufano, F and Elias-Rosa, N and Zampieri, L and Harutyunyan, A and Moskvitin, A S and Nissinen, M and Stanishev, V and Tsvetkov, D.\~{}Y. and Hentunen, V.\~{}P. and Komarova, V N and Pavlyuk, N N and Sokolov, V V and Sokolova, T N},
file = {:Users/svalenti/Documents/Mendeley Desktop/2012/Monthly Notices of the Royal Astronomical Society/MNRAS-2012-Inserra-1122-39.pdf:pdf},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {may},
number = {2},
pages = {1122--1139},
title = {{The bright Type IIP SN 2009bw, showing signs of interaction}},
volume = {422},
year = {2012},
}
@article{Wyse:2006gy,
annote = {IAU Symposium No. 232, eds P. Whitelock, B. Leidundgeit \{\&\} M. Dennefeld},
author = {Wyse, Rosemary F G and Gilmore, Gerard},
file = {:Users/svalenti/Documents/Mendeley Desktop/2006/arXiv.org/arXiv 2006 Wyse.pdf:pdf},
journal = {arXiv.org},
month = {apr},
title = {{Stellar Populations with ELTs}},
volume = {astro-ph},
year = {2006},
}
@article{Maurer2010,
author = {Maurer, I. and Mazzali, P. a. and Taubenberger, S. and Hachinger, S.},
doi = {10.1111/j.1365-2966.2010.17186.x},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2010 Maurer-1.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {1 i n t,8 m,central regions is consumed,collapse when the nuclear,formation,fuel in their,general,individual,line,massive stars,producing a core-collapse supernova,ro d u c,sn 2008ax,supernovae,t i o n},
month = {dec},
number = {4},
pages = {1441--1454},
title = {{Hydrogen and helium in the late phase of supernovae of Type IIb}},
url = {http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2010.17186.x},
volume = {409},
year = {2010},
}
@article{Clocchiatti1997,
author = {Clocchiatti, A and Wheeler, J.\~{}C. C.},
doi = {10.1086/304961},
file = {:Users/svalenti/Documents/Mendeley Desktop/1997/The Astrophysical Journal/1997 Clocchiatti.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {dec},
number = {1},
pages = {375--380},
title = {{On the Light Curves of Stripped‐Envelope Supernovae}},
url = {http://stacks.iop.org/0004-637X/491/i=1/a=375},
volume = {491},
year = {1997},
}
@article{QuimbyRobertMichael2006,
abstract = {Supernovae (SNe) are popular tools to explore the cosmological expansion of the Universe owing to their bright peak magnitudes and reasonably high rates; however, even the relatively homogeneous Type Ia supernovae are not intrinsically perfect standard candles. Their absolute peak brightness must be established by corrections that have been largely empirical. Hundreds of SNe are now found every year, shrinking the statistical errors in the cosmological parameters, but most of these distant discoveries do little to further the physical understanding of SNe, which could illuminate unknown systematics. The Texas Supernova Search was not designed to discover the most SNe nor the most distant SNe, but it was instead created to amass a small collection of well-observed nearby SNe with detailed, multi-epoch spectral observations beginning at the earliest possible phases. For the past two years, I have pointed ROTSE-IIIb's 1.85 X 1.85 degree field of view at nearby galaxy clusters and searched thousands of galaxies, covering hundreds of square degrees on the sky, for supernovae. With ToO time on the neighboring 9.2m Hobby-Eberly Telescope, the search has captured SNe spectra at some of the earliest phases ever. In this dissertation I describe the Texas Supernova Search and present the 30 supernovae, 11 novae, and 6 dwarf novae discovered in the first two years of the program.},
author = {{Quimby, Robert Michael}},
journal = {ProQuest Dissertations And Theses; Thesis (Ph.D.)--The University of Texas at Austin},
title = {{The Texas Supernova Search}},
url = {http://adsabs.harvard.edu/abs/2006PhDT........13Q},
year = {2006},
}
@article{Taubenberger2013,
abstract = {In this Letter, a late-phase spectrum of SN 2010lp, a subluminous Type Ia supernova (SN Ia), is presented and analyzed. As in 1991bg-like SNe Ia at comparable epochs, the spectrum is characterized by relatively broad [Fe II] and [Ca II] emission lines. However, instead of narrow [Fe III] and [Co III] lines that dominate the emission from the innermost regions of 1991bg-like supernovae (SNe), SN 2010lp shows [O I] $\lambda$$\lambda$6300, 6364 emission, usually associated with core-collapse SNe and never previously observed in a subluminous thermonuclear explosion. The [O I] feature has a complex profile with two strong, narrow emission peaks. This suggests that oxygen is distributed in a non-spherical region close to the center of the ejecta, severely challenging most thermonuclear explosion models discussed in the literature. We conclude that, given these constraints, violent mergers are presently the most promising scenario to explain SN 2010lp. Based on observations at ESO Paranal under program ID 088.D-0184.},
author = {Taubenberger, S. and Kromer, M. and Pakmor, R. and Pignata, G. and Maeda, K. and Hachinger, S. and Leibundgut, B. and Hillebrandt, W.},
doi = {10.1088/2041-8205/775/2/L43},
issn = {2041-8205},
journal = {The Astrophysical Journal},
keywords = {supernovae: general,supernovae: individual: SN 2010lp SN 1991bg SN 199},
month = {oct},
number = {2},
pages = {L43},
title = {{[O I] $\lambda$$\lambda$6300, 6364 IN THE NEBULAR SPECTRUM OF A SUBLUMINOUS TYPE Ia SUPERNOVA}},
url = {http://adsabs.harvard.edu/abs/2013ApJ...775L..43T},
volume = {775},
year = {2013},
}
@article{2008Sci...319.1220M,
annote = {Science 319, 1220 (2008) (29 February 2008 issue). Submitted on 20 August 2007, accepted on 17 January 2008. The resolution of SOM Figure 1 is lower than the original. Includes Supporting Online Material (SOM), 21 pages 3 figures, 1 table, and 2 SOM figures and 1 SOM table},
author = {Maeda, Keiichi and Kawabata, Koji and Mazzali, Paolo A and Tanaka, Masaomi and Valenti, Stefano and Nomoto, Ken'ichi and Hattori, Takashi and Deng, Jinsong and Pian, Elena and Taubenberger, Stefan and Iye, Masanori and Matheson, Thomas and Filippenko, Alexei V and Aoki, Kentaro and Kosugi, George and Ohyama, Youichi and Sasaki, Toshiyuki and Takata, Tadafumi},
file = {:Users/svalenti/Documents/Mendeley Desktop/2008/Science/2008 Maeda.pdf:pdf},
journal = {Science},
month = {feb},
number = {5},
pages = {1220--------},
title = {{Asphericity in Supernova Explosions from Late-Time Spectroscopy}},
volume = {319},
year = {2008},
}
@article{Brown2009a,
abstract = {We present ultraviolet (UV) observations of supernovae (SNe) obtained with the UltraViolet/Optical Telescope (UVOT) on board the Swift spacecraft. This is the largest sample of UV light curves from any single instrument and covers all major SN types and most subtypes. The UV light curves of SNe Ia are fairly homogenous, while SNe Ib/c and IIP show more variety in their light-curve shapes. The UV-optical colors clearly differentiate SNe Ia and IIP, particularly at early times. The color evolution of SNe IIP, however, makes their colors similar to SNe Ia at about 20 days after explosion. SNe Ib/c are shown to have varied UV-optical colors. The use of UV colors to help type SNe will be important for high-redshift SNe discovered in optical observations. These data can be added to ground-based optical and near infrared data to create bolometric light curves of individual objects and as checks on generic bolometric corrections used in the absence of UV data. This sample can also be compared with rest-frame UV observations of high-redshift SNe observed at optical wavelengths.},
author = {Brown, Peter J. and Holland, Stephen T. and Immler, Stefan and Milne, Peter and Roming, Peter W. A. and Gehrels, Neil and Nousek, John and Panagia, Nino and Still, Martin and {Vanden Berk}, Daniel},
doi = {10.1088/0004-6256/137/5/4517},
issn = {0004-6256},
journal = {The Astronomical Journal},
keywords = {distance scale,dust,extinction,galaxies: distances and redshifts,supernovae: general,ultraviolet: general},
month = {may},
number = {5},
pages = {4517--4525},
title = {{ULTRAVIOLET LIGHT CURVES OF SUPERNOVAE WITH THE SWIFT ULTRAVIOLET/OPTICAL TELESCOPE}},
url = {http://adsabs.harvard.edu/abs/2009AJ....137.4517B},
volume = {137},
year = {2009},
}
@article{Drake2009,
abstract = {We report on the results from the first six months of the Catalina Real-Time Transient Survey (CRTS). In order to search for optical transients (OTs) with timescales of minutes to years, the CRTS analyses data from the Catalina Sky Survey which repeatedly covers 26,000 of square degrees on the sky. The CRTS provides a public stream of transients that are bright enough to be followed up using small telescopes. Since the beginning of the survey, all CRTS transients have been made available to astronomers around the world in real time using HTML tables,RSS feeds, and VOEvents. As part of our public outreach program, the detections are now also available in Keyhole Markup Language through Google Sky. The initial discoveries include over 350 unique OTs rising more than 2 mag from past measurements. Sixty two of these are classified as supernovae (SNe), based on light curves, prior deep imaging and spectroscopic data. Seventy seven are due to cataclysmic variables (CVs; only 13 previously known), while an additional 100 transients were too infrequently sampled to distinguish between faint CVs and SNe. The remaining OTs include active galactic nucleus, blazars, high-proper-motions stars, highly variable stars (such as UV Ceti stars), and transients of an unknown nature. Our results suggest that there is a large population of SNe missed by many current SN surveys because of selection biases. These objects appear to be associated with faint host galaxies. We also discuss the unexpected discovery of white dwarf binary systems through dramatic eclipses.},
author = {Drake, A. J. and Djorgovski, S. G. and Mahabal, A. and Beshore, E. and Larson, S. and Graham, M. J. and Williams, R. and Christensen, E. and Catelan, M. and Boattini, A. and Gibbs, A. and Hill, R. and Kowalski, R.},
doi = {10.1088/0004-637X/696/1/870},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {BL Lacertae objects: general,cataclysmic variables,galaxies: general,novae,stars: flare,supernovae: general},
month = {may},
number = {1},
pages = {870--884},
title = {{FIRST RESULTS FROM THE CATALINA REAL-TIME TRANSIENT SURVEY}},
url = {http://adsabs.harvard.edu/abs/2009ApJ...696..870D},
volume = {696},
year = {2009},
}
@article{2011MNRAS.415L..81P,
author = {Poznanski, Dovi and Ganeshalingam, Mohan and Silverman, Jeffrey M and Filippenko, Alexei V},
journal = {Monthly Notices of the Royal Astronomical Society: Letters},
month = {jul},
number = {1},
pages = {L81----L84},
title = {{Low-resolution sodium D absorption is a bad proxy for extinction}},
volume = {415},
year = {2011},
}
@article{2010ApJ...711L..40C,
author = {Chevalier, Roger A and Soderberg, Alicia M},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/The Astrophysical Journal Letters/2010 Chevalier.pdf:pdf},
journal = {The Astrophysical Journal Letters},
month = {mar},
number = {1},
pages = {L40--------L43},
title = {{Type IIb Supernovae with Compact and Extended Progenitors}},
volume = {711},
year = {2010},
}
@article{2011ApJ...731L...4M,
author = {Modjaz, M and Kewley, L and Bloom, J.\~{}S. and Filippenko, A V and Perley, D and Silverman, J.\~{}M.},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/The Astrophysical Journal Letters/2011 Modjaz.pdf:pdf},
journal = {The Astrophysical Journal Letters},
month = {apr},
number = {1},
pages = {L4},
title = {{Progenitor Diagnostics for Stripped Core-collapse Supernovae: Measured Metallicities at Explosion Sites}},
volume = {731},
year = {2011},
}
@article{2011MNRAS.416.3138V,
author = {Valenti, S and Fraser, M and Benetti, S and Pignata, G. and Sollerman, J. and Inserra, C. and Cappellaro, E. and Pastorello, A. and Smartt, S. J. and Ergon, M. and Botticella, M. T. and Brimacombe, J. and Bufano, F. and Crockett, M. and Eder, I. and Fugazza, D. and Haislip, J. B and Hamuy, M. and Harutyunyan, A. and Ivarsen, K. M. and Kankare, E. and Kotak, R. and LaCluyze, A. P. and Magill, L. and Mattila, S. and Maza, J. and Mazzali, P. A. and Reichart, D. E. and Taubenberger, S. and Turatto, M. and Zampieri, L.},
doi = {10.1111/j.1365-2966.2011.19262.x},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2011 Valenti.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {galaxies,general,in-,ngc 7479,on observations with several,sn 2009jf,supernovae,telescopes,this paper is based},
month = {oct},
number = {4},
pages = {3138--3159},
title = {{SN 2009jf: a slow-evolving stripped-envelope core-collapse supernova★}},
url = {http://onlinelibrary.wiley.com/doi/10.1111/j.1365-2966.2011.19262.x/full http://mnras.oxfordjournals.org/cgi/doi/10.1111/j.1365-2966.2011.19262.x},
volume = {416},
year = {2011},
}
@article{2009A&A...502..611G,
author = {Georgy, C and Meynet, G and Walder, R and Folini, D and Maeder, A},
doi = {10.1051/0004-6361/200811339},
issn = {0004-6361},
journal = {Astronomy and Astrophysics},
month = {aug},
number = {2},
pages = {611--622},
title = {{The different progenitors of type Ib, Ic SNe, and of GRB}},
url = {http://www.aanda.org/10.1051/0004-6361/200811339},
volume = {502},
year = {2009},
}
@article{2012arXiv1204.1523F,
annote = {Submitted to ApJ Letters},
author = {Fraser, M and Maund, J R and Smartt, S. J. and Botticella, M.-T. and Dall'Ora, M and Inserra, C and Tomasella, L and Benetti, S and Ciroi, S and Eldridge, J J and Ergon, M and Kotak, R and Mattila, S and Ochner, P and Pastorello, A and Reilly, E and Sollerman, J and Stephens, A and Taddia, F and Valenti, S},
doi = {10.1088/2041-8205/759/1/L13},
issn = {2041-8205},
journal = {The Astrophysical Journal},
month = {nov},
number = {1},
pages = {L13},
title = {{RED AND DEAD: THE PROGENITOR OF SN 2012aw IN M95}},
url = {http://stacks.iop.org/2041-8205/759/i=1/a=L13?key=crossref.6a548bca95683e8a4254975101b020b0},
volume = {759},
year = {2012},
}
@article{Pumo2011,
abstract = {We have developed a relativistic, radiation-hydrodynamics Lagrangian code, specifically tailored to simulate the evolution of the main observables (light curve and the evolution of photospheric velocity and temperature) in core-collapse supernova (CC-SN) events. The distinctive features of the code are an accurate treatment of radiative transfer coupled to relativistic hydrodynamics, a self-consistent treatment of the evolution of the innermost ejecta taking into account the gravitational effects of the central compact remnant, and a fully implicit Lagrangian approach to the solution of the coupled nonlinear finite difference system of equations. Our aim is to use it as a numerical tool to perform calculations of a grid of models to be compared with observations of CC-SNe. In this paper, we present some testcase simulations and a comparison with observations of SN 1987A, as well as with the results obtained with other numerical codes. We also briefly discuss the influence of the main physical parameters (ejected mass, progenitor radius, explosion energy, amount of 56Ni) on the evolution of the ejecta, and the implications of our results in connection with the possibility to standardize hydrogen-rich CC-SNe for using them as candles to measure cosmological distances.},
author = {Pumo, M. L. and Zampieri, L.},
doi = {10.1088/0004-637X/741/1/41},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {distance scale,hydrodynamics,methods: numerical,radiative transfer,supernovae: general,supernovae: individual: SN 1987A},
month = {nov},
number = {1},
pages = {41},
title = {{RADIATION-HYDRODYNAMICAL MODELING OF CORE-COLLAPSE SUPERNOVAE: LIGHT CURVES AND THE EVOLUTION OF PHOTOSPHERIC VELOCITY AND TEMPERATURE}},
url = {http://adsabs.harvard.edu/abs/2011ApJ...741...41P},
volume = {741},
year = {2011},
}
@article{2013ATel.4825....1A,
abstract = {We report the discovery, with the 0.76-m Katzman Automatic Imaging Telescope (KAIT) at Lick Observatory, of a possible new supernova in the nearby galaxy NGC 5669. The new object, dubbed PSN J14324449+0953123 (by the IAU), is located at (J2000.0) coordinates RA = 14:32:44.49, Dec = +09:53:12.3. Following discovery in an unfiltered image obtained at 12:59 UT on 2013 Feb. 17, KAIT autonomously began a sequence of triggered follow-up observations in the U, B, V, and clear (roughly R) filters beginning only 4 minutes later.},
author = {Zheng, W. and Blanchard, P. and Cenko, S. B. and Filippenko, A. V. and Cucchiara, A.},
journal = {The Astronomer's Telegram},
keywords = {Optical,Supernovae,Transient},
title = {{KAIT Discovery and Robotic Follow-up of a young SN Ia in NGC5669}},
url = {http://adsabs.harvard.edu/abs/2013ATel.4823....1Z},
year = {2013},
}
@article{2007ApJ...659.1536R,
author = {Rau, A and Kulkarni, S.\~{}R. and Ofek, E O and Yan, L},
journal = {The Astrophysical Journal},
month = {apr},
number = {2},
pages = {1536--1540},
title = {{Spitzer Observations of the New Luminous Red Nova M85 OT2006-1}},
volume = {659},
year = {2007},
}
@article{2006MNRAS.372..265M,
author = {Matteucci, F and Panagia, N and Pipino, A and Mannucci, F and Recchi, S and {Della Valle}, M},
file = {:Users/svalenti/Documents/Mendeley Desktop/2006/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2006 Matteucci.pdf:pdf},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {oct},
number = {1},
pages = {265--275},
title = {{A new formulation of the Type Ia supernova rate and its consequences on galactic chemical evolution}},
volume = {372},
year = {2006},
}
@article{2010arXiv1008.2144T,
abstract = {Massive stars and their supernovae are prominent sources of radioactive isotopes, the observations of which thus can help to improve our astrophysical models of those. Our understanding of stellar evolution and the final explosive endpoints such as supernovae or hypernovae or gamma-ray bursts relies on the combination of magneto-hydrodynamics, energy generation due to nuclear reactions accompanying composition changes, radiation transport, and thermodynamic properties (such as the equation of state of stellar matter). Nuclear energy production includes all nuclear reactions triggered during stellar evolution and explosive end stages, also among unstable isotopes produced on the way. Radiation transport covers atomic physics (e.g. opacities) for photon transport, but also nuclear physics and neutrino nucleon/nucleus interactions in late phases and core collapse. Here we want to focus on the astrophysical aspects, i.e. a description of the evolution of massive stars and their endpoints, with a special emphasis on the composition of their ejecta (in form of stellar winds during the evolution or of explosive ejecta). Low and intermediate mass stars end their evolution as a white dwarf with an unburned C and O composition. Massive stars evolve beyond this point and experience all stellar burning stages from H over He, C, Ne, O and Si-burning up to core collapse and explosive endstages. In this chapter we discuss the nucleosynthesis processes involved and the production of radioactive nuclei in more detail.},
archiveprefix = {arXiv},
arxivid = {1008.2144},
author = {Thielemann, Friedrich-Karl and Hirschi, Raphael and Liebend\"{o}rfer, Matthias and Diehl, Roland},
doi = {10.1007/978-3-642-12698-7\_4},
eprint = {1008.2144},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/Unknown/arXiv 2010 Thielemann.pdf:pdf},
month = {aug},
pages = {79},
title = {{Massive Stars and their Supernovae}},
url = {http://arxiv.org/abs/1008.2144},
volume = {astro-ph.H},
year = {2010},
}
@article{2010Sci...327...58P,
abstract = {Analyses of supernovae (SNe) have revealed two main types of progenitors: exploding white dwarfs and collapsing massive stars. Here we describe SN 2002bj, which stands out as different from any SN reported to date. Its light curve rose and declined very rapidly, yet reached a peak intrinsic brightness greater than -18 magnitude. A spectrum obtained 7 days after discovery shows the presence of helium and intermediate-mass elements, yet no clear hydrogen or iron-peak elements. The spectrum only barely resembles that of a type Ia SN, with added carbon and helium. Its properties suggest that SN 2002bj may be representative of a class of progenitors that previously has been only hypothesized: a helium detonation on a white dwarf, ejecting a small envelope of material. New surveys should find many such objects, despite their scarcity.},
author = {Poznanski, Dovi and Chornock, Ryan and Nugent, Peter E and Bloom, Joshua S and Filippenko, Alexei V and Ganeshalingam, Mohan and Leonard, Douglas C and Li, Weidong and Thomas, Rollin C},
doi = {10.1126/science.1181709},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/Science (New York, N.Y.)/2010 Poznanski.pdf:pdf},
issn = {1095-9203},
journal = {Science (New York, N.Y.)},
month = {jan},
number = {5961},
pages = {58--60},
pmid = {19892941},
title = {{An unusually fast-evolving supernova.}},
url = {http://www.ncbi.nlm.nih.gov/pubmed/19892941},
volume = {327},
year = {2010},
}
@article{1998ApJ...503..325A,
author = {Alard, C and Lupton, Robert H},
journal = {Astrophysical Journal v.503},
month = {aug},
pages = {325},
title = {{A Method for Optimal Image Subtraction}},
volume = {503},
year = {1998},
}
@article{2000A&AS..144..363A,
author = {Alard, C},
journal = {Astronomy and Astrophysics Supplement},
month = {jun},
pages = {363--370},
title = {{Image subtraction using a space-varying kernel}},
volume = {144},
year = {2000},
}
@article{Gezari:2010bh,
author = {Gezari, S and Rest, A and Huber, M E and Narayan, G and Forster, K and Neill, J D and Martin, D C and Valenti, S and Smartt, S.\~{}J. and Chornock, R and Berger, E and Soderberg, A.\~{}M. and Mattila, S and Kankare, E and Burgett, W S and Chambers, K C and Dombeck, T and Grav, T and Heasley, J N and Hodapp, K W and Jedicke, R and Kaiser, N and Kudritzki, R and Luppino, G and Lupton, R H and Magnier, E A and Monet, D G and Morgan, J S and Onaka, P M and Price, P A and Rhoads, P H and Siegmund, W A and Stubbs, C W and Tonry, J L and Wainscoat, R J and Waterson, M F and Wynn-Williams, C G},
journal = {Astrophys.J.},
pages = {L77--------L81},
title = {{GALEX and Pan-STARRS1 Discovery of SN IIP 2010aq: The First Few Days After Shock Breakout in a Red Supergiant Star}},
volume = {720},
year = {2010},
}
@article{2008MNRAS.388L..74F,
author = {F\"{o}rster, Francisco and Schawinski, Kevin},
file = {:Users/svalenti/Documents/Mendeley Desktop/2008/Monthly Notices of the Royal Astronomical Society Letters/2008 F\"{o}rster.pdf:pdf},
journal = {Monthly Notices of the Royal Astronomical Society: Letters},
month = {jul},
number = {1},
pages = {L74--------L78},
title = {{The radial distribution of Type Ia supernovae in early-type galaxies: implications for progenitor scenarios}},
volume = {388},
year = {2008},
}
@article{2011ApJ...734..102K,
annote = {submitted to ApJ},
author = {Kasen, Daniel and Woosley, S E and Heger, Alexander},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/The Astrophysical Journal/2011 Kasen.pdf:pdf},
journal = {The Astrophysical Journal},
month = {jun},
number = {2},
pages = {102},
title = {{Pair Instability Supernovae: Light Curves, Spectra, and Shock Breakout}},
volume = {734},
year = {2011},
}
@article{2008MNRAS.385...75T,
abstract = {Optical observations of the Type Ia supernova (SN Ia) 2005bl in NGC 4070, obtained from -6 to +66d with respect to the B-band maximum, are presented. The photometric evolution is characterized by rapidly declining light curves [$\Delta$m15(B)true = 1.93] and red colours at peak and soon thereafter. With MB,max = -17.24 the SN is an underluminous SN Ia, similar to the peculiar SNe 1991bg and 1999by. This similarity also holds for the spectroscopic appearance, the only remarkable difference being the likely presence of carbon in pre-maximum spectra of SN 2005bl. A comparison study among underluminous SNe Ia is performed, based on a number of spectrophotometric parameters. Previously reported correlations of the light-curve decline rate with peak luminosity and (Si) are confirmed, and a large range of post-maximum SiII $\lambda$6355 velocity gradients is encountered. 1D synthetic spectra for SN 2005bl are presented, which confirm the presence of carbon and suggest an overall low burning efficiency with a significant amount of leftover unburned material. Also, the Fe content in pre-maximum spectra is very low, which may point to a low metallicity of the precursor. Implications for possible progenitor scenarios of underluminous SNe Ia are briefly discussed. Based on observations at ESO-Paranal, Programme 075.D-0662(B). E-mail: [email protected]},
author = {Taubenberger, S. and Hachinger, S. and Pignata, G. and Mazzali, P. A. and Contreras, C. and Valenti, S. and Pastorello, A. and Elias-Rosa, N. and B\"{a}rnbantner, O. and Barwig, H. and Benetti, S. and Dolci, M. and Fliri, J. and Folatelli, G. and Freedman, W. L. and Gonzalez, S. and Hamuy, M. and Krzeminski, W. and Morrell, N. and Navasardyan, H. and Persson, S. E. and Phillips, M. M. and Ries, C. and Roth, M. and Suntzeff, N. B. and Turatto, M. and Hillebrandt, W.},
doi = {10.1111/j.1365-2966.2008.12843.x},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {galaxies: individual: NGC 4070,supernovae: general,supernovae: individual: SN 1991bg,supernovae: individual: SN 1998de,supernovae: individual: SN 1999by,supernovae: individual: SN 2005bl},
month = {feb},
number = {1},
pages = {75--96},
title = {{The underluminous Type Ia supernova 2005bl and the class of objects similar to SN 1991bg★}},
url = {http://adsabs.harvard.edu/abs/2008MNRAS.385...75T},
volume = {385},
year = {2008},
}
@article{Benetti2006,
author = {Benetti, S. and Cappellaro, E. and Turatto, M. and Taubenberger, S. and Harutyunyan, A. and Valenti, S.},
doi = {10.1086/510667},
file = {:Users/svalenti/Documents/Mendeley Desktop/2006/The Astrophysical Journal/2006 Benetti.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {dec},
number = {2},
pages = {L129--L132},
title = {{Supernova 2002ic: The Collapse of a Stripped-Envelope, Massive Star in a Dense Medium?}},
url = {http://stacks.iop.org/1538-4357/653/i=2/a=L129},
volume = {653},
year = {2006},
}
@article{2009ApJS..182..543A,
author = {Abazajian, Kevork N and Adelman-McCarthy, Jennifer K and Ag\"{u}eros, Marcel A and Allam, Sahar S and {Allende Prieto}, Carlos and An, Deokkeun and Anderson, Kurt S J and Anderson, Scott F and Annis, James and Bahcall, Neta A and Bailer-Jones, C.\~{}A.\~{}L. and Barentine, J.\~{}C. and Bassett, Bruce A and Becker, Andrew C and Beers, Timothy C and Bell, Eric F and Belokurov, Vasily and Berlind, Andreas A and Berman, Eileen F and Bernardi, Mariangela and Bickerton, Steven J and Bizyaev, Dmitry and Blakeslee, John P and Blanton, Michael R and Bochanski, John J and Boroski, William N and Brewington, Howard J and Brinchmann, Jarle and Brinkmann, J and Brunner, Robert J and Budav\'{a}ri, Tam\'{a}s and Carey, Larry N and Carliles, Samuel and Carr, Michael A and Castander, Francisco J and Cinabro, David and Connolly, A J and Csabai, Istv\'{a}n and Cunha, Carlos E and Czarapata, Paul C and Davenport, James R A and de Haas, Ernst and Dilday, Ben and Doi, Mamoru and Eisenstein, Daniel J and Evans, Michael L and Evans, N W and Fan, Xiaohui and Friedman, Scott D and Frieman, Joshua A and Fukugita, Masataka and G\"{a}nsicke, Boris T and Gates, Evalyn and Gillespie, Bruce and Gilmore, G and Gonzalez, Belinda and Gonzalez, Carlos F and Grebel, Eva K and Gunn, James E and Gy\"{o}ry, Zsuzsanna and Hall, Patrick B and Harding, Paul and Harris, Frederick H and Harvanek, Michael and Hawley, Suzanne L and Hayes, Jeffrey J E and Heckman, Timothy M and Hendry, John S and Hennessy, Gregory S and Hindsley, Robert B and Hoblitt, J and Hogan, Craig J and Hogg, David W and Holtzman, Jon A and Hyde, Joseph B and Ichikawa, Shin-ichi and Ichikawa, Takashi and Im, Myungshin and Ivezi\'{c}, \v{Z}eljko and Jester, Sebastian and Jiang, Linhua and Johnson, Jennifer A and Jorgensen, Anders M and Juri\'{c}, Mario and Kent, Stephen M and Kessler, R and Kleinman, S.\~{}J. and Knapp, G.\~{}R. and Konishi, Kohki and Kron, Richard G and Krzesinski, Jurek and Kuropatkin, Nikolay and Lampeitl, Hubert and Lebedeva, Svetlana and Lee, Myung Gyoon and Lee, Young Sun and {French Leger}, R and L\'{e}pine, S\'{e}bastien and Li, Nolan and Lima, Marcos and Lin, Huan and Long, Daniel C and Loomis, Craig P and Loveday, Jon and Lupton, Robert H and Magnier, Eugene and Malanushenko, Olena and Malanushenko, Viktor and Mandelbaum, Rachel and Margon, Bruce and Marriner, John P and Mart\'{\i}nez-Delgado, David and Matsubara, Takahiko and McGehee, Peregrine M and McKay, Timothy A and Meiksin, Avery and Morrison, Heather L and Mullally, Fergal and Munn, Jeffrey A and Murphy, Tara and Nash, Thomas and Nebot, Ada and Neilsen, Eric H Jr and Newberg, Heidi Jo and Newman, Peter R and Nichol, Robert C and Nicinski, Tom and Nieto-Santisteban, Maria and Nitta, Atsuko and Okamura, Sadanori and Oravetz, Daniel J and Ostriker, Jeremiah P and Owen, Russell and Padmanabhan, Nikhil and Pan, Kaike and Park, Changbom and Pauls, George and Peoples, John Jr and Percival, Will J and Pier, Jeffrey R and Pope, Adrian C and Pourbaix, Dimitri and Price, Paul A and Purger, Norbert and Quinn, Thomas and Raddick, M Jordan and {Re Fiorentin}, Paola and Richards, Gordon T and Richmond, Michael W and Riess, Adam G and Rix, Hans-Walter and Rockosi, Constance M and Sako, Masao and Schlegel, David J and Schneider, Donald P and Scholz, Ralf-Dieter and Schreiber, Matthias R and Schwope, Axel D and Seljak, Uro\v{s} and Sesar, Branimir and Sheldon, Erin and Shimasaku, Kazu and Sibley, Valena C and Simmons, A E and Sivarani, Thirupathi and {Allyn Smith}, J and Smith, Martin C and Smol\v{c}i\'{c}, Vernesa and Snedden, Stephanie A and Stebbins, Albert and Steinmetz, Matthias and Stoughton, Chris and Strauss, Michael A and SubbaRao, Mark and Suto, Yasushi and Szalay, Alexander S and Szapudi, Istv\'{a}n and Szkody, Paula and Tanaka, Masayuki and Tegmark, Max and Teodoro, Luis F A and Thakar, Aniruddha R and Tremonti, Christy A and Tucker, Douglas L and Uomoto, Alan and {Vanden Berk}, Daniel E and Vandenberg, Jan and Vidrih, S and Vogeley, Michael S and Voges, Wolfgang and Vogt, Nicole P and Wadadekar, Yogesh and Watters, Shannon and Weinberg, David H and West, Andrew A and White, Simon D M and Wilhite, Brian C and Wonders, Alainna C and Yanny, Brian and Yocum, D.\~{}R. and York, Donald G and Zehavi, Idit and Zibetti, Stefano and Zucker, Daniel B},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/The Astrophysical Journal Supplement/2009 Abazajian.pdf:pdf},
journal = {The Astrophysical Journal Supplement},
month = {jun},
number = {2},
pages = {543--558},
title = {{The Seventh Data Release of the Sloan Digital Sky Survey}},
volume = {182},
year = {2009},
}
@article{Patat2007,
abstract = {Type Ia supernovae are important cosmological distance indicators. Each of these bright supernovae supposedly results from the thermonuclear explosion of a white dwarf star that, after accreting material from a companion star, exceeds some mass limit, but the true nature of the progenitor star system remains controversial. Here we report the spectroscopic detection of circumstellar material in a normal type Ia supernova explosion. The expansion velocities, densities, and dimensions of the circumstellar envelope indicate that this material was ejected from the progenitor system. In particular, the relatively low expansion velocities suggest that the white dwarf was accreting material from a companion star that was in the red-giant phase at the time of the explosion.},
author = {Patat, F and Chandra, P and Chevalier, R and Justham, S and Podsiadlowski, Ph and Wolf, C and Gal-Yam, a and Pasquini, L and Crawford, I a and Mazzali, P a and Pauldrach, a W a and Nomoto, K and Benetti, S and Cappellaro, E and Elias-Rosa, N and Hillebrandt, W and Leonard, D C and Pastorello, a and Renzini, a and Sabbadin, F and Simon, J D and Turatto, M},
doi = {10.1126/science.1143005},
file = {:Users/svalenti/Documents/Mendeley Desktop/2007/Science (New York, N.Y.)/2007 Patat.pdf:pdf},
issn = {1095-9203},
journal = {Science (New York, N.Y.)},
month = {aug},
number = {5840},
pages = {924--6},
pmid = {17626848},
title = {{Detection of circumstellar material in a normal type Ia supernova.}},
url = {http://www.ncbi.nlm.nih.gov/pubmed/17626848},
volume = {317},
year = {2007},
}
@article{2010ApJ...714L.280F,
author = {Fraser, M and Takats, K and Pastorello, A and Smartt, S.\~{}J. and Mattila, S and Botticella, M T and Valenti, S and Ergon, M and Sollerman, J and Arcavi, I and Benetti, S and Bufano, F and Crockett, R M and Danziger, I J and Gal-Yam, A and Maund, J R and Taubenberger, S and Turatto, M},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/The Astrophysical Journal Letters/2010 Fraser-1.pdf:pdf},
journal = {The Astrophysical Journal Letters},
month = {may},
number = {2},
pages = {L280--------L284},
title = {{On the Progenitor and Early Evolution of the Type II Supernova 2009kr}},
volume = {714},
year = {2010},
}
@inproceedings{2008AIPC..990..263K,
author = {Kasen, Daniel and Heger, Alex and Woosley, Stan},
booktitle = {FIRST STARS III: First Stars II Conference. AIP Conference Proceedings},
file = {:Users/svalenti/Documents/Mendeley Desktop/2008/FIRST STARS III First Stars II Conference. AIP Conference Proceedings/2008 Kasen.pdf:pdf},
month = {mar},
organization = {The Johns Hopkins University and Space Telescope Science Institute, Baltimore, MD; Department of Physics and Astronomy, UC Santa Cruz, CA},
pages = {263--267},
title = {{The First Stellar Explosions: Theoretical Light Curves and Spectra of Pair-Instability Supernovae}},
year = {2008},
}
@article{2008CBET.1191....2B,
abstract = {CBET 1191 available at Central Bureau for Astronomical Telegrams.},
author = {Blondin, S and Calkins, M and {Nakano, S.} and {Kadota, K.} and {Itagaki, K.} and {Corelli, P.}},
journal = {Central Bureau Electronic Telegrams},
month = {jan},
pages = {2},
title = {{Supernova 2007uy in NGC 2770}},
url = {http://adsabs.harvard.edu/abs/2008CBET.1191....1N},
volume = {1191},
year = {2008},
}
@article{Arcavi2011,
abstract = {On 2011 May 31 UT a supernova (SN) exploded in the nearby galaxy M51 (the Whirlpool Galaxy). We discovered this event using small telescopes equipped with CCD cameras and also detected it with the Palomar Transient Factory survey, rapidly confirming it to be a Type II SN. Here, we present multi-color ultraviolet through infrared photometry which is used to calculate the bolometric luminosity and a series of spectra. Our early-time observations indicate that SN 2011dh resulted from the explosion of a relatively compact progenitor star. Rapid shock-breakout cooling leads to relatively low temperatures in early-time spectra, compared to explosions of red supergiant stars, as well as a rapid early light curve decline. Optical spectra of SN 2011dh are dominated by H lines out to day 10 after explosion, after which He I lines develop. This SN is likely a member of the cIIb (compact IIb) class, with progenitor radius larger than that of SN 2008ax and smaller than the eIIb (extended IIb) SN 1993J progenitor. Our data imply that the object identified in pre-explosion Hubble Space Telescope images at the SN location is possibly a companion to the progenitor or a blended source, and not the progenitor star itself, as its radius (\~{}1013 cm) would be highly inconsistent with constraints from our post-explosion spectra.},
author = {Arcavi, Iair and Gal-Yam, Avishay and Yaron, Ofer and Sternberg, Assaf and Rabinak, Itay and Waxman, Eli and Kasliwal, Mansi M. and Quimby, Robert M. and Ofek, Eran O. and Horesh, Assaf and Kulkarni, Shrinivas R. and Filippenko, Alexei V. and Silverman, Jeffrey M. and Cenko, S. Bradley and Li, Weidong and Bloom, Joshua S. and Sullivan, Mark and Nugent, Peter E. and Poznanski, Dovi and Gorbikov, Evgeny and Fulton, Benjamin J. and Howell, D. Andrew and Bersier, David and Riou, Amedee and Lamotte-Bailey, Stephane and Griga, Thomas and Cohen, Judith G. and Hachinger, Stephan and Polishook, David and Xu, Dong and Ben-Ami, Sagi and Manulis, Ilan and Walker, Emma S. and Maguire, Kate and Pan, Yen-Chen and Matheson, Thomas and Mazzali, Paolo A. and Pian, Elena and Fox, Derek B. and Gehrels, Neil and Law, Nicholas and James, Philip and Marchant, Jonathan M. and Smith, Robert J. and Mottram, Chris J. and Barnsley, Robert M. and Kandrashoff, Michael T. and Clubb, Kelsey I.},
doi = {10.1088/2041-8205/742/2/L18},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/The Astrophysical Journal/apjl\_742\_2\_18.pdf:pdf},
issn = {2041-8205},
journal = {The Astrophysical Journal},
keywords = {solSN2011dh,supernovae: individual: PTF11eon\&},
month = {dec},
number = {2},
pages = {L18},
title = {{SN 2011dh: DISCOVERY OF A TYPE IIb SUPERNOVA FROM A COMPACT PROGENITOR IN THE NEARBY GALAXY M51}},
url = {http://adsabs.harvard.edu.proxy.library.ucsb.edu:2048/abs/2011ApJ...742L..18A},
volume = {742},
year = {2011},
}
@article{1996AJ....112..732R,
author = {Richmond, Michael W and Treffers, Richard R and Filippenko, Alexei V and Paik, Young},
journal = {Astronomical Journal v.112},
month = {aug},
pages = {732},
title = {{UBVRI Photometry of SN 1993J in M81: Days 3 to 365}},
volume = {112},
year = {1996},
}
@article{Shigeyama1994,
author = {Shigeyama, Toshikazu and Suzuki, Tomoharu and Kumagai, Shiomi and Nomoto, Ken'ichi and Saio, Hideyuki and Yamaoka, Hitoshi},
doi = {10.1086/173564},
file = {:Users/svalenti/Documents/Mendeley Desktop/1994/The Astrophysical Journal/1994 Shigeyama.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {jan},
pages = {341},
title = {{Theoretical light curves of Type IIb supernova 1993J}},
url = {http://adsabs.harvard.edu/doi/10.1086/173564},
volume = {420},
year = {1994},
}
@article{1994ApJ...427..628F,
author = {Freedman, Wendy L and Hughes, Shaun M and Madore, Barry F and Mould, Jeremy R and Lee, Myung Gyoon and Stetson, Peter and Kennicutt, Robert C and Turner, Anne and Ferrarese, Laura and Ford, Holland and Graham, John A and Hill, Robert and Hoessel, John G and Huchra, John and Illingworth, Garth D},
journal = {Astrophysical Journal},
month = {jun},
pages = {628--655},
title = {{The Hubble Space Telescope Extragalactic Distance Scale Key Project. 1: The discovery of Cepheids and a new distance to M81}},
volume = {427},
year = {1994},
}
@article{2010ApJ...724L..16P,
author = {Pastorello, A and Smartt, S.\~{}J. and Botticella, M T and Maguire, K and Fraser, M and Smith, K and Kotak, R and Magill, L and Valenti, S and Young, D.\~{}R. and Gezari, S and Bresolin, F and Kudritzki, R and Howell, D.\~{}A. and Rest, A and Metcalfe, N and Mattila, S and Kankare, E and Huang, K.\~{}Y. and Urata, Y and Burgett, W S and Chambers, K C and Dombeck, T and Flewelling, H and Grav, T and Heasley, J N and Hodapp, K W and Kaiser, N and Luppino, G.\~{}A. and Lupton, R H and Magnier, E A and Monet, D G and Morgan, J S and Onaka, P M and Price, P A and Rhoads, P H and Siegmund, W A and Stubbs, C W and Sweeney, W E and Tonry, J L and Wainscoat, R J and Waterson, M F and Waters, C and Wynn-Williams, C G},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/The Astrophysical Journal Letters/2010 Pastorello.pdf:pdf},
journal = {The Astrophysical Journal Letters},
month = {nov},
number = {1},
pages = {L16--------L21},
title = {{Ultra-bright Optical Transients are Linked with Type Ic Supernovae}},
volume = {724},
year = {2010},
}
@article{Chevalier1994,
author = {Chevalier, Roger A. and Fransson, Claes},
doi = {10.1086/173557},
file = {:Users/svalenti/Documents/Mendeley Desktop/1994/The Astrophysical Journal/1994 Chevalier.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {jan},
pages = {268},
title = {{Emission from circumstellar interaction in normal Type II supernovae}},
url = {http://adsabs.harvard.edu/doi/10.1086/173557},
volume = {420},
year = {1994},
}
@article{1998ApJ...498L.129T,
author = {Turatto, M and Mazzali, P.\~{}A. and Young, T R and Nomoto, K and Iwamoto, K and Benetti, S and Cappellaro, E and Danziger, I J and de Mello, D F and Phillips, M.\~{}M. and Suntzeff, N.\~{}B. and Clocchiatti, A and Piemonte, A and Leibundgut, B and Covarrubias, R and Maza, J and Sollerman, J},
journal = {Astrophysical Journal Letters v.498},
month = {may},
pages = {L129},
title = {{The Peculiar Type II Supernova 1997D: A Case for a Very Low 56Ni Mass}},
volume = {498},
year = {1998},
}
@article{Vinko2006,
abstract = {New BV RI photometry and optical spectroscopy of the Type IIp supernova 2004dj in NGC 2403, obtained during the first year since discovery, are presented. The progenitor cluster, Sandage 96, is also detected on pre-explosion frames. The light curve indicates that the explosion occurred about 30d before discovery, and the plateau phase lasted about +110 +/- 20 d after that. The plateau-phase spectra have been modelled with the SYNOW spectral synthesis code using H, NaI, TiII, ScII, FeII and BaI lines. The SN distance is inferred from the expanding photosphere method and the standard candle method applicable for SNeIIp. They resulted in distances that are consistent with each other as well as earlier Cepheid and Tully-Fisher distances. The average distance, D = 3.47 +/- 0.29 Mpc is proposed for SN 2004dj and NGC 2403. The nickel mass produced by the explosion is estimated as \~{}0.02 +/- 0.01 Msolar. The spectral energy distribution of the progenitor cluster is reanalysed by fitting population synthesis models to our observed BV RI data supplemented by U and JHK magnitudes from the literature. The $\chi$2 minimization revealed a possible `young' solution with cluster age Tcl = 8 Myr, and an `old' solution with Tcl = 20-30 Myr. The `young' solution would imply a progenitor mass M \> 20 Msolar, which is higher than the previously detected progenitor masses for Type II SNe. Based on observations obtained at David Dunlap Observatory (Canada), F. L. Whipple Observatory (USA), Konkoly Observatory and Szeged Observatory (Hungary). E-mail: [email protected]},
author = {Vink\'{o}, J. and Tak\'{a}ts, K. and S\'{a}rneczky, K. and Szab\'{o}, Gy. M. and M\'{e}sz\'{a}ros, Sz. and Csorv\'{a}si, R. and Szalai, T. and G\'{a}sp\'{a}r, A. and P\'{a}l, A. and Csizmadia, Sz. and K\'{o}sp\'{a}l, A. and R\'{a}cz, M. and Kun, M. and Cs\'{a}k, B. and F\"{u}r\'{e}sz, G. and DeBond, H. and Grunhut, J. and Thomson, J. and Mochnacki, S. and Koktay, T.},
doi = {10.1111/j.1365-2966.2006.10416.x},
file = {:Users/svalenti/Documents/Mendeley Desktop/2006/Monthly Notices of the Royal Astronomical Society/2006MNRAS\_369\_1780V.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {galaxies: individual: NGC 2403,stars: evolution,stars: evolution: supernovae: individual: SN 2004d,supernovae: individual: SN 2004dj},
month = {jun},
number = {4},
pages = {1780--1796},
title = {{The first year of SN 2004dj in NGC 2403★}},
url = {http://adsabs.harvard.edu/abs/2006MNRAS.369.1780V},
volume = {369},
year = {2006},
}
@article{2010MNRAS.408...87M,
author = {Mazzali, Paolo A and Maurer, I and Valenti, S and Kotak, R and Hunter, D},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/Monthly Notices of the Royal Astronomical Society/Monthly Notices of the Royal Astronomical Society 2010 Mazzali.pdf:pdf},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {oct},
number = {1},
pages = {87--96},
title = {{The Type Ic SN 2007gr: a census of the ejecta from late-time optical-infrared spectra}},
volume = {408},
year = {2010},
}
@article{Lundqvist2013,
abstract = {We present predictions for hydrogen and helium emission line luminosities from circumstellar matter around Type Ia supernovae (SNe Ia) using time dependent photoionization modelling. Early high-resolution ESO/Very Large Telescope (VLT) optical echelle spectra of the SN Ia 2000cx were taken before and up to ˜70 d after maximum to probe the existence of such narrow emission lines from the supernova. We detect no such lines, and from our modelling place an upper limit on the mass-loss rate for the putative wind from the progenitor system, dot\{M\}≲ 1.3× 10\^{}\{-5\} M\_\{⊙\} yr\^{}\{-1\}, assuming a speed of 10 km s-1 and solar abundances for the wind. If the wind would be helium-enriched and/or faster, the upper limit on dot\{M\} could be significantly higher. In the helium-enriched case, we show that the best line to constrain the mass-loss would be He I $\lambda$10 830. In addition to confirming the details of interstellar Na I and Ca II absorption towards SN 2000cx as discussed by Patat et al., we also find evidence for 6613.56 \AA diffuse interstellar band absorption in the Milky Way. We also discuss measurements of the X-ray emission from the interaction between the supernova ejecta and the wind and we re-evaluate observations of SN 1992A obtained ˜16 d after maximum by Schlegel \& Petre. We find an upper limit of dot\{M\}˜ 1.3× 10\^{}\{-5\} M\_\{⊙\} yr\^{}\{-1\} which is significantly higher than that estimated by Schlegel \& Petre. These results, together with the previous observational work on the normal SNe Ia 1994D and 2001el, disfavour a symbiotic star in the upper mass-loss rate regime (so-called Mira-type systems) from being the likely progenitor scenario for these SNe. Our model calculations are general, and can also be used for the subclass of SNe Ia that do show circumstellar interaction, e.g. the recent PTF 11kx. To constrain hydrogen in late-time spectra, we present ESO/VLT and ESO/New Technology Telescope optical and infrared observations of SNe Ia 1998bu and 2000cx in the nebular phase, 251-388 d after maximum. We see no signs of hydrogen line emission in SNe 1998bu and 2000cx at these epochs, and from the absence of H$\alpha$ with a width of the order of ˜103 km s-1, we argue from modelling that the mass of such hydrogen-rich gas must be ≲0.03 M⊙ for both supernovae. Comparing similar upper limits with recent models of Pan et al., it seems that hydrogen-rich donors with a separation of ≲5 times the radius of the donor may be ruled out for the five SNe Ia 1998bu, 2000cx, 2001el, 2005am and 2005cf. Larger separation, helium-rich donors, or a double-degenerate origin for these supernovae seems more likely. Our models have also been used to put the limit on hydrogen-rich gas in the recent SN 2011fe, and for this supernova, a double-degenerate origin seems likely.},
author = {Lundqvist, P. and Mattila, S. and Sollerman, J. and Kozma, C. and Baron, E. and Cox, N. L. J. and Fransson, C. and Leibundgut, B. and Spyromilio, J.},
doi = {10.1093/mnras/stt1303},
issn = {0035-8711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {circumstellar matter,supernovae: general,supernovae: individual: SN 1992A,supernovae: individual: SN 1998bu,supernovae: individual: SN 2000cx},
month = {aug},
number = {1},
pages = {329--345},
title = {{Hydrogen and helium in the spectra of Type Ia supernovae}},
url = {http://adsabs.harvard.edu/abs/2013MNRAS.435..329L},
volume = {435},
year = {2013},
}
@article{Sand2013,
abstract = {We report a spectroscopic classification of ASASSN-13ar (Atel \#5138) located at RA=01:18:41.76 dec=-07:26:39.70 (J2000). A spectrum (range 330-1000 nm) obtained robotically on June 21.80 UT with the FLOYDS spectrograph at Faulkes Telescope South at Siding Springs shows it to be a SN Ia within a couple days of maximum light, and is consistent with the host galaxy redshift of z=0.0178.},
author = {Sand, D. and Valenti, S. and Graham, M. L. and Parrent, J. T.},
journal = {The Astronomer's Telegram},
keywords = {Optical,Supernovae},
title = {{Classification of ASASSN-13ar with FLOYDS at Faulkes Telescope South}},
url = {http://adsabs.harvard.edu/abs/2013ATel.5155....1S},
year = {2013},
}
@misc{TheMendeleySupportTeam2011a,
abstract = {A quick introduction to Mendeley. Learn how Mendeley creates your personal digital library, how to organize and annotate documents, how to collaborate and share with colleagues, and how to generate citations and bibliographies.},
address = {London},
author = {{The Mendeley Support Team}},
booktitle = {Mendeley Desktop},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/Mendeley Desktop/FAQ.pdf:pdf},
keywords = {Mendeley,how-to,user manual},
pages = {1--16},
publisher = {Mendeley Ltd.},
title = {{Getting Started with Mendeley}},
url = {http://www.mendeley.com},
year = {2011},
}
@article{ValentiS.2013a,
abstract = {We report a spectroscopic observation of PSN J03175245-0718021, located at RA= 03:17:52.45, DEC = -07:18:02.1 (J2000). A spectrum (range 320-1000 nm) obtained robotically on July 13.72 UT with the FLOYDS spectrograph at Faulkes Telescope South at Siding Spring shows a blue continuum with He I features with a P-cygni profile. No Hydrogen lines are visible.},
author = {{Valenti, S.} and {Graham, M. L.} and {Howell, D. A.} and {Sand, D.} and {Parrent, J. T.}},
journal = {The Astronomer's Telegram},
keywords = {Optical,Supernovae},
title = {{Spectroscopic classification for PSN J03175245-0718021 with FLOYDS at Faulkes Telescope South}},
url = {http://adsabs.harvard.edu/abs/2013ATel.5206....1V},
year = {2013},
}
@article{2004ApJ...614..858M,
annote = {19 pages, 6 figures. To appear in the Astrophysical Journal (October 20, 2004)},
author = {Mazzali, P.\~{}A. and Deng, J and Maeda, K and Nomoto, K and Filippenko, A V and Matheson, T},
file = {:Users/svalenti/Documents/Mendeley Desktop/2004/The Astrophysical Journal/2004 Mazzali.pdf:pdf},
journal = {The Astrophysical Journal},
month = {oct},
number = {2},
pages = {858--863},
title = {{Properties of Two Hypernovae Entering the Nebular Phase: SN 1997ef and SN 1997dq}},
volume = {614},
year = {2004},
}
@article{2009AIPC.1111..406V,
author = {Valenti, Stefano},
journal = {PROBING STELLAR POPULATIONS OUT TO THE DISTANT UNIVERSE: CEFALU 2008},
month = {may},
pages = {406--410},
title = {{New Insights on Stripped Envelope CC Supernovae}},
volume = {1111},
year = {2009},
}
@article{2011ApJ...730...89P,
author = {Perets, Hagai B and Badenes, Carles and Arcavi, Iair and Simon, Joshua D and Gal-Yam, Avishay},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/The Astrophysical Journal/2011 Perets.pdf:pdf},
journal = {The Astrophysical Journal},
month = {apr},
number = {2},
pages = {89},
title = {{An Emerging Class of Bright, Fast-evolving Supernovae with Low-mass Ejecta}},
volume = {730},
year = {2011},
}
@article{2011ApJ...732..118S,
author = {Sullivan, M and Kasliwal, M.\~{}M. and Nugent, P.\~{}E. and Howell, D.\~{}A. and Thomas, R C and Ofek, E O and Arcavi, I and Blake, S and Cooke, J and Gal-Yam, A and Hook, I M and Mazzali, P and Podsiadlowski, P and Quimby, R and Bildsten, L and Bloom, J.\~{}S. and Cenko, S.\~{}B. and Kulkarni, S.\~{}R. and Law, N and Poznanski, D},
file = {:Users/svalenti/Documents/Mendeley Desktop/2011/The Astrophysical Journal/2011 Sullivan.pdf:pdf},
journal = {The Astrophysical Journal},
month = {may},
number = {2},
pages = {118},
title = {{The Subluminous and Peculiar Type Ia Supernova PTF 09dav}},
volume = {732},
year = {2011},
}
@article{2009AJ....138..376F,
annote = {22 pages, 15 figures, submitted to AJ},
author = {Foley, Ryan J and Chornock, Ryan and Filippenko, Alexei V and Ganeshalingam, Mohan and Kirshner, Robert P and Li, Weidong and Cenko, S Bradley and Challis, Peter J and Friedman, Andrew S and Modjaz, Maryam and Silverman, Jeffrey M and Wood-Vasey, W Michael},
file = {:Users/svalenti/Documents/Mendeley Desktop/2009/The Astronomical Journal/2009 Foley.pdf:pdf},
journal = {The Astronomical Journal},
month = {aug},
number = {2},
pages = {376--391},
title = {{SN 2008ha: An Extremely Low Luminosity and Exceptionally Low Energy Supernova}},
volume = {138},
year = {2009},
}
@article{2003LNP...598...47B,
author = {Branch, D and Baron, E A and Jeffery, D J},
journal = {Supernovae and Gamma-Ray Bursters. Edited by K. Weiler.},
pages = {47--75},
title = {{Optical Spectra of Supernovae}},
volume = {598},
year = {2003},
}
@article{Pastorello2013,
abstract = {We report the results of a three-year-long dedicated monitoring campaign of a restless luminous blue variable (LBV) in NGC 7259. The object, named SN 2009ip, was observed photometrically and spectroscopically in the optical and near-infrared domains. We monitored a number of erupting episodes in the past few years, and increased the density of our observations during eruptive episodes. In this paper, we present the full historical data set from 2009 to 2012 with multi-wavelength dense coverage of the two high-luminosity events between 2012 August and September. We construct bolometric light curves and measure the total luminosities of these eruptive or explosive events. We label them the 2012a event (lasting \~{}50 days) with a peak of 3 × 1041 erg s-1, and the 2012b event (14 day rise time, still ongoing) with a peak of 8 × 1042 erg s-1. The latter event reached an absolute R-band magnitude of about -18, comparable to that of a core-collapse supernova (SN). Our historical monitoring has detected high-velocity spectral features (\~{}13,000 km s-1) in 2011 September, one year before the current SN-like event. This implies that the detection of such high-velocity outflows cannot, conclusively, point to a core-collapse SN origin. We suggest that the initial peak in the 2012a event was unlikely to be due to a faint core-collapse SN. We propose that the high intrinsic luminosity of the latest peak, the variability history of SN 2009ip, and the detection of broad spectral lines indicative of high-velocity ejecta are consistent with a pulsational pair-instability event, and that the star may have survived the last outburst. The question of the survival of the LBV progenitor star and its future fate remain open issues, only to be answered with future monitoring of this historically unique explosion.},
author = {Pastorello, A. and Cappellaro, E. and Inserra, C. and Smartt, S. J. and Pignata, G. and Benetti, S. and Valenti, S. and Fraser, M. and Tak\'{a}ts, K. and Benitez, S. and Botticella, M. T. and Brimacombe, J. and Bufano, F. and Cellier-Holzem, F. and Costado, M. T. and Cupani, G. and Curtis, I. and Elias-Rosa, N. and Ergon, M. and Fynbo, J. P. U. and Hambsch, F.-J. and Hamuy, M. and Harutyunyan, A. and Ivarson, K. M. and Kankare, E. and Martin, J. C. and Kotak, R. and LaCluyze, A. P. and Maguire, K. and Mattila, S. and Maza, J. and McCrum, M. and Miluzio, M. and Norgaard-Nielsen, H. U. and Nysewander, M. C. and Ochner, P. and Pan, Y.-C. and Pumo, M. L. and Reichart, D. E. and Tan, T. G. and Taubenberger, S. and Tomasella, L. and Turatto, M. and Wright, D.},
doi = {10.1088/0004-637X/767/1/1},
file = {:Users/svalenti/Documents/Mendeley Desktop/2013/The Astrophysical Journal/apj\_767\_1\_1.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {galaxies: individual: NGC 7259,supernovae: general,supernovae: individual: SN 2009ip SN 2000ch},
month = {apr},
number = {1},
pages = {1},
title = {{INTERACTING SUPERNOVAE AND SUPERNOVA IMPOSTORS: SN 2009ip, IS THIS THE END?}},
url = {http://adsabs.harvard.edu/abs/2013ApJ...767....1P},
volume = {767},
year = {2013},
}
@article{McGaugh1991,
author = {McGaugh, Stacy S.},
doi = {10.1086/170569},
file = {:Users/svalenti/Documents/Mendeley Desktop/1991/The Astrophysical Journal/1991 McGaugh.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {oct},
pages = {140},
title = {{H II region abundances - Model oxygen line ratios}},
url = {http://adsabs.harvard.edu/doi/10.1086/170569},
volume = {380},
year = {1991},
}
@article{2010ApJ...719L.204W,
annote = {submitted to Astrophysical Journal Letters},
author = {Woosley, S E},
file = {:Users/svalenti/Documents/Mendeley Desktop/2010/The Astrophysical Journal Letters/2010 Woosley.pdf:pdf},
journal = {The Astrophysical Journal Letters},
month = {aug},
number = {2},
pages = {L204--------L207},
title = {{Bright Supernovae from Magnetar Birth}},
volume = {719},
year = {2010},
}
@techreport{Anonymous:OX0dHMDd,
month = {may},
title = {{Microsoft Word - p3edpstd3\{\_\}2012-05-22.docx}},
year = {2012},
}
@article{Bose2013,
abstract = {We present densely-sampled UBVRI/griz photometric and low-resolution (6-10A) optical spectroscopic observations from 4 to 270 days after explosion of a newly discovered type II SN 2012aw in a nearby (\~{}9.9 Mpc) galaxy M95. The light-curve characteristics of apparent magnitudes, colors, bolometric luminosity and the presence and evolution of prominent spectral features are found to have striking similarity with the archetypal IIP SNe 1999em, 1999gi and 2004et. The early time observations of SN 2012aw clearly detect minima in the light-curve of V, R and I bands near 37 days after explosion and this we suggest to be an observational evidence for emergence of recombination phase. The mid-plateau MV magnitude (-16.67 \$\backslash pm\$ 0.04) lies in between the bright (\~{} -18) and subluminous (\~{} -15) IIP SNe. The mass of nickel is 0.06\$\backslash pm\$0.01 M\_sun. The SYNOW modelling of spectra indicate that the value and evolution of photospheric velocity is similar to SN 2004et, but about \~{}600 km/s higher than that of SNe 1999em and 1999gi at comparable epochs. This trend is more apparent in the line velocities of H alpha and H beta. A comparison of ejecta velocity properties with that of existing radiation-hydrodynamical simulations indicate that the energy of explosion lies in the range 1-2x10\^{}51 ergs; a further comparison of nebular phase [Oi] doublet luminosity with SNe 2004et and 1987A indicate that the mass of progenitor star is about 14-15 M\_sun. The presence of high-velocity absorption features in the mid-to-late plateau and possibly in early phase spectra show signs of interaction between ejecta and the circumstellar matter; being consistent with its early-time detection at X-ray and radio wavebands.},
archiveprefix = {arXiv},
arxivid = {1305.3152},
author = {Bose, S. and Kumar, B. and Sutaria, F. and Roy, R. and Bhatt, V. K. and Pandey, S. B. and Chandola, H. C. and Sagar, R. and Misra, K. and Chakraborti, S.},
doi = {10.1093/mnras/stt864},
eprint = {1305.3152},
issn = {0035-8711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {galaxies: individual: NGC 3551,supernovae: general,supernovae: individual: SN 1999em,supernovae: individual: SN 1999gi,supernovae: individual: SN 2004et,supernovae: individual: SN 2012aw},
language = {en},
month = {jun},
pages = {22},
title = {{Supernova 2012aw - a high-energy clone of archetypal Type IIP SN 1999em}},
url = {http://adsabs.harvard.edu/abs/2013MNRAS.tmp.1583B},
volume = {-1},
year = {2013},
}
@article{Elias-Rosa2013,
abstract = {We report the identification of potential candidates for the progenitor star of the Type Ic PSN J12015272-1852183 discovered by the CHASE survey (CBAT TOCP) from archival Hubble Space Telescope (HST) WFPC2 images in F555W (\~{}V), and F814W (\~{}I). These images were obtained from 2008-12-02 to 2009-02-09 UT for the HST proposal 11962, PI: A. Riess. We used a good-quality, acquisition image of the SN obtained at TNG Telescope (+Dolores) on June 23.88 UT to geometrically match the HST mosaics.},
author = {Elias-Rosa, N. and Pastorello, A. and Benetti, S. and Cappellaro, E. and Pignata, G. and Takats, K. and Valenti, S. and Harutyunyan, A.},
journal = {The Astronomer's Telegram},
keywords = {Optical,Supernovae},
title = {{A Preliminary Search for the Progenitor Candidate of PSN J12015272-1852183 in the Antennae Galaxies (NGC 4038)}},
url = {http://adsabs.harvard.edu/abs/2013ATel.5162....1E},
year = {2013},
}
@article{Fraser_2011,
title = {{SN 2009md: another faint supernova from a low-mass progenitor}},
volume = {417},
issn = {0035-8711},
url = {http://dx.doi.org/10.1111/j.1365-2966.2011.19370.x},
doi = {10.1111/j.1365-2966.2011.19370.x},
number = {2},
journal = {Monthly Notices of the Royal Astronomical Society},
publisher = {Oxford University Press (OUP)},
author = {Fraser, M. and Ergon, M. and Eldridge, J. J. and Valenti, S. and Pastorello, A. and Sollerman, J. and Smartt, S. J. and Agnoletto, I. and Arcavi, I. and Benetti, S. and et al.},
year = {2011},
month = {Oct},
pages = {1417–1433},
}
