@article{Behrendt2016,
author = {M. Behrendt and A. Burkert and M. Schartmann},
title = {{Clusters of Small Clumps Can Explain the Peculiar Properties of Giant Clumps in High-redshift Galaxies}},
journal = {The Astrophysical Journal Letters},
volume = {819},
number = {1},
pages = {L2},
url = {http://stacks.iop.org/2041-8205/819/i=1/a=L2},
year = {2016},
abstract = {Giant clumps are a characteristic feature of observed high-redshift disk galaxies. We propose that these kiloparsec-sized clumps have a complex substructure and are the result of many smaller clumps self-organizing themselves into clump clusters (CCs). This bottom-up scenario is in contrast to the common top-down view that these giant clumps form first and then sub-fragment. Using a high-resolution hydrodynamical simulation of an isolated, fragmented massive gas disk and mimicking the observations from Genzel et al. at z ∼ 2, we find remarkable agreement in many details. The CCs appear as single entities of sizes ##IMG## [http://ej.iop.org/images/2041-8205/819/1/L2/apjl522782ieqn1.gif] {${R}_{\mathrm{HWHM}}\;\simeq \;$} 0.9–1.4 kpc and masses ∼(1.5–3) ##IMG## [http://ej.iop.org/images/2041-8205/819/1/L2/apjl522782ieqn2.gif] {$\times \quad {10}^{9}\ {M}_{\odot }$} , representative of high- z observations. They are organized in a ring around the center of the galaxy. The origin of the observed clumps’ high intrinsic velocity dispersion ##IMG## [http://ej.iop.org/images/2041-8205/819/1/L2/apjl522782ieqn3.gif] {${\sigma }_{\mathrm{intrinsic}}\;\simeq \;$} 50–100 ##IMG## [http://ej.iop.org/images/2041-8205/819/1/L2/apjl522782ieqn4.gif] {$\mathrm{km}\;{{\rm{s}}}^{-1}$} is fully explained by the internal irregular motions of their substructure in our simulation. No additional energy input, e.g., via stellar feedback, is necessary. Furthermore, in agreement with observations, we find a small velocity gradient ##IMG## [http://ej.iop.org/images/2041-8205/819/1/L2/apjl522782ieqn5.gif] {${V}_{\mathrm{grad}}\quad \simeq $} 8–27 ##IMG## [http://ej.iop.org/images/2041-8205/819/1/L2/apjl522782ieqn6.gif] {$\mathrm{km}\;{{\rm{s}}}^{-1}\;{\mathrm{kpc}}^{-1}$} along the CCs in the beam-smeared velocity residual maps, which corresponds to net prograde and retrograde rotation with respect to the rotation of the galactic disk. The CC scenario could have strong implications for the internal evolution, lifetimes, and the migration timescales of the observed giant clumps, bulge growth, and active galactic nucleus activity, stellar feedback, and the chemical enrichment history of galactic disks.},
}
@article{Elmegreen2005,
author = {Debra Meloy Elmegreen and Bruce G. Elmegreen and Douglas S. Rubin and Meredith A. Schaffer},
title = {{Galaxy Morphologies in the Hubble Ultra Deep Field: Dominance of Linear Structures at the Detection Limit}},
journal = {The Astrophysical Journal},
volume = {631},
number = {1},
pages = {85},
url = {http://stacks.iop.org/0004-637X/631/i=1/a=85},
year = {2005},
abstract = {Galaxies in the Hubble Ultra Deep Field (UDF) larger than 10 pixels (0 ##IMG## [http://ej.iop.org/icons/Entities/farcs.gif] {farcs} 3) have been classified according to morphology, and their photometric properties are presented. There are 269 spiral, 100 elliptical, 114 chain, 126 double-clump, 97 tadpole, and 178 clump-cluster galaxies. We also cataloged 30 B -band and 13 V -band dropouts and calculated their star formation rates. Chains, doubles, and tadpoles dominate the other types at faint magnitudes. The fraction of obvious bars among spirals is ~10%, a factor of 2-3 lower than in other deep surveys. The distribution function of axial ratios for elliptical galaxies is similar to that seen locally, suggesting that ellipticals relaxed quickly to a standardized shape. The distribution of axial ratios for spiral galaxies is significantly different than locally, having a clear peak at ~0.55 instead of a nearly flat distribution. The falloff at small axial ratio occurs at a higher value than locally, indicating thicker disks by a factor of ~2. The falloff at high axial ratio could be from intrinsic triaxial shapes or selection effects. Inclined disks should be more highly sampled than face-on disks near the surface brightness limit of a survey. Simple models and data distributions demonstrate these effects. The decreased numbers of obvious spiral galaxies at high redshifts could be partly the result of surface brightness selection.},
}
@ARTICLE{Hou2009,
author = {{Hou}, A. and {Parker}, L.~C. and {Harris}, W.~E. and {Wilman}, D.~J.},
title = {{Statistical Tools for Classifying Galaxy Group Dynamics}},
journal = {\apj},
archiveprefix = {arXiv},
eprint = {0908.0938},
primaryclass = {astro-ph.GA},
keywords = {galaxies: interactions, galaxies: statistics},
year = {2009},
month = {sep},
volume = {702},
pages = {1199-1210},
doi = {10.1088/0004-637X/702/2/1199},
adsurl = {http://adsabs.harvard.edu/abs/2009ApJ...702.1199H},
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
}
@article{Masters2010,
author = {Masters, Karen L. and Mosleh, Moein and Romer, A. Kathy and Nichol, Robert C. and Bamford, Steven P. and Schawinski, Kevin and Lintott, Chris J. and Andreescu, Dan and Campbell, Heather C. and Crowcroft, Ben and Doyle, Isabelle and Edmondson, Edward M. and Murray, Phil and Raddick, M. Jordan and Slosar, Anže and Szalay, Alexander S. and Vandenberg, Jan},
title = {{Galaxy Zoo: passive red spirals}},
volume = {405},
number = {2},
pages = {783-799},
year = {2010},
doi = {10.1111/j.1365-2966.2010.16503.x},
abstract = {We study the spectroscopic properties and environments of red (or passive) spiral galaxies found by the Galaxy Zoo project. By carefully selecting face-on disc-dominated spirals, we construct a sample of truly passive discs (i.e. they are not dust reddened spirals, nor are they dominated by old stellar populations in a bulge). As such, our red spirals represent an interesting set of possible transition objects between normal blue spiral galaxies and red early types, making up ∼6 per cent of late-type spirals. We use optical images and spectra from Sloan Digital Sky Survey to investigate the physical processes which could have turned these objects red without disturbing their morphology. We find red spirals preferentially in intermediate density regimes. However, there are no obvious correlations between red spiral properties and environment suggesting that environment alone is not sufficient to determine whether a galaxy will become a red spiral. Red spirals are a very small fraction of all spirals at low masses (M★ < 1010 M⊙), but are a significant fraction of the spiral population at large stellar masses showing that massive galaxies are red independent of morphology. We confirm that as expected, red spirals have older stellar populations and less recent star formation than the main spiral population. While the presence of spiral arms suggests that a major star formation could not have ceased a long ago (not more than a few Gyr), we show that these are also not recent post-starburst objects (having had no significant star formation in the last Gyr), so star formation must have ceased gradually. Intriguingly, red spirals are roughly four times as likely than the normal spiral population to host optically identified Seyfert/low-ionization nuclear emission region (LINER; at a given stellar mass and even accounting for low-luminosity lines hidden by star formation), with most of the difference coming from the objects with LINER-like emission. We also find a curiously large optical bar fraction in the red spirals (70 ± 5 verses 27 ± 5 per cent in blue spirals) suggesting that the cessation of star formation and bar instabilities in spirals are strongly correlated. We conclude by discussing the possible origins of these red spirals. We suggest that they may represent the very oldest spiral galaxies which have already used up their reserves of gas – probably aided by strangulation or starvation, and perhaps also by the effect of bar instabilities moving material around in the disc. We provide an online table listing our full sample of red spirals along with the normal/blue spirals used for comparison.},
url = {http://mnras.oxfordjournals.org/content/405/2/783.abstract},
eprint = {http://mnras.oxfordjournals.org/content/405/2/783.full.pdf+html},
journal = {Monthly Notices of the Royal Astronomical Society},
}
@article{Masters2012,
author = {Masters, Karen L. and Nichol, Robert C. and Haynes, Martha P. and Keel, William C. and Lintott, Chris and Simmons, Brooke and Skibba, Ramin and Bamford, Steven and Giovanelli, Riccardo and Schawinski, Kevin},
title = {{Galaxy Zoo and ALFALFA: atomic gas and the regulation of star formation in barred disc galaxies}},
volume = {424},
number = {3},
pages = {2180-2192},
year = {2012},
doi = {10.1111/j.1365-2966.2012.21377.x},
abstract = {We study the observed correlation between atomic gas content and the likelihood of hosting a large-scale bar in a sample of 2090 disc galaxies. Such a test has never been done before on this scale. We use data on morphologies from the Galaxy Zoo project and information on the galaxies' H I content from the Arecibo Legacy Fast Arecibo L-band Feed Array (ALFALFA) blind H I survey. Our main result is that the bar fraction is significantly lower among gas-rich disc galaxies than gas-poor ones. This is not explained by known trends for more massive (stellar) and redder disc galaxies to host more bars and have lower gas fractions: we still see at fixed stellar mass a residual correlation between gas content and bar fraction. We discuss three possible causal explanations: (1) bars in disc galaxies cause atomic gas to be used up more quickly, (2) increasing the atomic gas content in a disc galaxy inhibits bar formation and (3) bar fraction and gas content are both driven by correlation with environmental effects (e.g. tidal triggering of bars, combined with strangulation removing gas). All three explanations are consistent with the observed correlations. In addition our observations suggest bars may reduce or halt star formation in the outer parts of discs by holding back the infall of external gas beyond bar co-rotation, reddening the global colours of barred disc galaxies. This suggests that secular evolution driven by the exchange of angular momentum between stars in the bar, and gas in the disc, acts as a feedback mechanism to regulate star formation in intermediate-mass disc galaxies.},
url = {http://mnras.oxfordjournals.org/content/424/3/2180.abstract},
eprint = {http://mnras.oxfordjournals.org/content/424/3/2180.full.pdf+html},
journal = {Monthly Notices of the Royal Astronomical Society},
}
@article{Willett2015,
author = {Willett, Kyle W. and Schawinski, Kevin and Simmons, Brooke D. and Masters, Karen L. and Skibba, Ramin A. and Kaviraj, Sugata and Melvin, Thomas and Wong, O. Ivy and Nichol, Robert C. and Cheung, Edmond and Lintott, Chris J. and Fortson, Lucy},
title = {{Galaxy Zoo: the dependence of the star formation–stellar mass relation on spiral disc morphology}},
volume = {449},
number = {1},
pages = {820-827},
year = {2015},
doi = {10.1093/mnras/stv307},
abstract = {We measure the stellar mass–star formation rate (SFR) relation in star-forming disc galaxies at z ≤ 0.085, using Galaxy Zoo morphologies to examine different populations of spirals as classified by their kiloparsec-scale structure. We examine the number of spiral arms, their relative pitch angle, and the presence of a galactic bar in the disc, and show that both the slope and dispersion of the M⋆–SFR relation is constant when varying all the above parameters. We also show that mergers (both major and minor), which represent the strongest conditions for increases in star formation at a constant mass, only boost the SFR above the main relation by ∼0.3 dex; this is significantly smaller than the increase seen in merging systems at z > 1. Of the galaxies lying significantly above the M⋆–SFR relation in the local Universe, more than 50 per cent are mergers. We interpret this as evidence that the spiral arms, which are imperfect reflections of the galaxy's current gravitational potential, are either fully independent of the various quenching mechanisms or are completely overwhelmed by the combination of outflows and feedback. The arrangement of the star formation can be changed, but the system as a whole regulates itself even in the presence of strong dynamical forcing.},
url = {http://mnras.oxfordjournals.org/content/449/1/820.abstract},
eprint = {http://mnras.oxfordjournals.org/content/449/1/820.full.pdf+html},
journal = {Monthly Notices of the Royal Astronomical Society},
}
@INPROCEEDINGS{Hao09,
author = {{Hao}, L. and {Jogee}, S. and {Barazza}, F.~D. and {Marinova}, I. and {Shen}, J.},
title = {{Bars in Starbursts and AGNs - A Quantitative Reexamination}},
booktitle = {Galaxy Evolution: Emerging Insights and Future Challenges},
year = {2009},
series = {Astronomical Society of the Pacific Conference Series},
volume = {419},
archiveprefix = {arXiv},
eprint = {0910.3960},
primaryclass = {astro-ph.CO},
editor = {{Jogee}, S. and {Marinova}, I. and {Hao}, L. and {Blanc}, G.~A.},
month = {dec},
pages = {402},
adsurl = {http://adsabs.harvard.edu/abs/2009ASPC..419..402H},
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
}
@article{Oh2012,
author = {Seulhee Oh and Kyuseok Oh and Sukyoung K. Yi},
title = {{Bar Effects on Central Star Formation and Active Galactic Nucleus Activity}},
journal = {The Astrophysical Journal Supplement Series},
volume = {198},
number = {1},
pages = {4},
url = {http://stacks.iop.org/0067-0049/198/i=1/a=4},
year = {2012},
abstract = {Galactic bars are often suspected to be channels of gas inflow to the galactic center and to trigger central star formation and active galactic nucleus (AGN) activity. However, the current status on this issue based on empirical studies is unsettling, especially regarding AGNs. We investigate this question based on the Sloan Digital Sky Survey Data Release 7. From the nearby (0.01 < z < 0.05) bright ( M r < –19) database, we have constructed a sample of 6658 relatively face-on late-type galaxies through visual inspection. We found 36% of them to have a bar. Bars are found to be more common in galaxies with earlier morphology. This makes sample selection critical. Parameter-based selections would miss a large fraction of barred galaxies of early morphology. Bar effects on star formation or AGNs are difficult to understand properly because multiple factors (bar frequency, stellar mass, black hole mass, gas contents, etc.) seem to contribute to them in intricate manners. In the hope of breaking these degeneracies, we inspect bar effects for fixed galaxy properties. Bar effects on central star formation seem higher in redder galaxies. Bar effects on AGNs on the other hand are higher in bluer and less massive galaxies. These effects seem more pronounced with increasing bar length. We discuss possible implications in terms of gas contents, bar strength, bar evolution, fueling timescale, and the dynamical role of supermassive black hole.},
}
@article{Lintott2008,
author = {Lintott, Chris J. and Schawinski, Kevin and Slosar, Anže and Land, Kate and Bamford, Steven and Thomas, Daniel and Raddick, M. Jordan and Nichol, Robert C. and Szalay, Alex and Andreescu, Dan and Murray, Phil and Vandenberg, Jan},
title = {{Galaxy Zoo: morphologies derived from visual inspection of galaxies from the Sloan Digital Sky Survey}},
volume = {389},
number = {3},
pages = {1179-1189},
year = {2008},
doi = {10.1111/j.1365-2966.2008.13689.x},
abstract = {In order to understand the formation and subsequent evolution of galaxies one must first distinguish between the two main morphological classes of massive systems: spirals and early-type systems. This paper introduces a project, Galaxy Zoo, which provides visual morphological classifications for nearly one million galaxies, extracted from the Sloan Digital Sky Survey (SDSS). This achievement was made possible by inviting the general public to visually inspect and classify these galaxies via the internet. The project has obtained more than 4 × 107 individual classifications made by ∼105 participants. We discuss the motivation and strategy for this project, and detail how the classifications were performed and processed. We find that Galaxy Zoo results are consistent with those for subsets of SDSS galaxies classified by professional astronomers, thus demonstrating that our data provide a robust morphological catalogue. Obtaining morphologies by direct visual inspection avoids introducing biases associated with proxies for morphology such as colour, concentration or structural parameters. In addition, this catalogue can be used to directly compare SDSS morphologies with older data sets. The colour–magnitude diagrams for each morphological class are shown, and we illustrate how these distributions differ from those inferred using colour alone as a proxy for morphology.},
url = {http://mnras.oxfordjournals.org/content/389/3/1179.abstract},
eprint = {http://mnras.oxfordjournals.org/content/389/3/1179.full.pdf+html},
journal = {Monthly Notices of the Royal Astronomical Society},
}
@INPROCEEDINGS{Galloway2016,
author = {{Galloway}, M. and {Willett}, K. and {Fortson}, L. and {Scarlata}, C. and {Beck}, M. and {Masters}, K. and {Melvin}, T.},
title = {{Galaxy Zoo Hubble: First results of the redshift evolution of disk fraction in the red sequence}},
booktitle = {American Astronomical Society Meeting Abstracts},
year = {2016},
series = {American Astronomical Society Meeting Abstracts},
volume = {227},
month = {jan},
eid = {342.40},
pages = {342.40},
adsurl = {http://adsabs.harvard.edu/abs/2016AAS...22734240G},
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
}
@article{Nelson2012,
author = {Erica June Nelson and Pieter G. van Dokkum and Gabriel Brammer and Natascha Förster Schreiber and Marijn Franx and Mattia Fumagalli and Shannon Patel and Hans-Walter Rix and Rosalind E. Skelton and Rachel Bezanson and Elisabete Da Cunha and Mariska Kriek and Ivo Labbe and Britt Lundgren and Ryan Quadri and Kasper B. Schmidt},
title = {{Spatially Resolved Hα Maps and Sizes of 57 Strongly Star-forming Galaxies at z ~ 1 from 3D-HST: Evidence for Rapid Inside-out Assembly of Disk Galaxies}},
journal = {The Astrophysical Journal Letters},
volume = {747},
number = {2},
pages = {L28},
url = {http://stacks.iop.org/2041-8205/747/i=2/a=L28},
year = {2012},
abstract = {We investigate the buildup of galaxies at z ~ 1 using maps of Hα and stellar continuum emission for a sample of 57 galaxies with rest-frame Hα equivalent widths >100 Å in the 3D-HST grism survey. We find that the Hα emission broadly follows the rest-frame R -band light but that it is typically somewhat more extended and clumpy. We quantify the spatial distribution with the half-light radius. The median Hα effective radius r e (Hα) is 4.2 ± 0.1 kpc but the sizes span a large range, from compact objects with r e (Hα) ~ 1.0 kpc to extended disks with r e (Hα) ~ 15 kpc. Comparing Hα sizes to continuum sizes, we find =1.3 ± 0.1 for the full sample. That is, star formation, as traced by Hα, typically occurs out to larger radii than the rest-frame R -band stellar continuum; galaxies are growing their radii and building up from the inside out. This effect appears to be somewhat more pronounced for the largest galaxies. Using the measured Hα sizes, we derive star formation rate surface densities, Σ SFR . We find that Σ SFR ranges from ~0.05 M ☉ yr –1 kpc –2 for the largest galaxies to ~5 M ☉ yr –1 kpc –2 for the smallest galaxies, implying a large range in physical conditions in rapidly star-forming z ~ 1 galaxies. Finally, we infer that all galaxies in the sample have very high gas mass fractions and stellar mass doubling times <500 Myr. Although other explanations are also possible, a straightforward interpretation is that we are simultaneously witnessing the rapid formation of compact bulges and large disks at z ~ 1.},
}
@ARTICLE{Kormendy2016,
author = {{Kormendy}, J.},
title = {{Elliptical Galaxies and Bulges of Disc Galaxies: Summary of Progress and Outstanding Issues}},
journal = {Galactic Bulges},
archiveprefix = {arXiv},
eprint = {1504.03330},
keywords = {Physics},
year = {2016},
volume = {418},
pages = {431},
doi = {10.1007/978-3-319-19378-6_16},
adsurl = {http://adsabs.harvard.edu/abs/2016ASSL..418..431K},
adsnote = {Provided by the SAO/NASA Astrophysics Data System},
}
@article{Maiolino2008,
abstract = {We present initial results of an ESO-VLT large programme (AMAZE) aimed at determining the evolution of the mass-metallicity relation at z>3 by means of deep near-IR spectroscopy. Gas metallicities are measured, for an initial sample of nine star forming galaxies at z{\~{}}3.5, by means of optical nebular lines redshifted into the near-IR. Stellar masses are accurately determined by using Spitzer-IRAC data, which sample the rest-frame near-IR stellar light in these distant galaxies. When compared with previous surveys, the mass-metallicity relation inferred at z{\~{}}3.5 shows an evolution much stronger than observed at lower redshifts. The evolution is prominent even in massive galaxies, indicating that z{\~{}}3 is an epoch of major action in terms of star formation and metal enrichment also for massive systems. There are also indications that the metallicity evolution of low mass galaxies is stronger relative to high mass systems, an effect which can be considered the chemical version of the galaxy downsizing. The mass-metallicity relation observed at z{\~{}}3.5 is difficult to reconcile with the predictions of some hierarchical evolutionary models. Such discrepancies suggest that at z>3 galaxies are assembled mostly with relatively un-evolved sub-units, i.e. small galaxies with low star formation efficiency. The bulk of the star formation and metallicity evolution probably occurs once small galaxies are already assembled into bigger systems.},
archiveprefix = {arXiv},
arxivid = {0806.2410},
author = {Maiolino, R. and Nagao, T. and Grazian, A. and Cocchia, F. and Marconi, A. and Mannucci, F. and Cimatti, A. and Pipino, A. and Ballero, S. and Calura, F. and Chiappini, C. and Fontana, A. and Granato, G. L. and Matteucci, F. and Pastorini, G. and Pentericci, L. and Risaliti, G. and Salvati, M. and Silva, L.},
doi = {10.1051/0004-6361:200809678},
eprint = {0806.2410},
file = {:home/mel/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Maiolino et al. - 2008 - AMAZE.pdf:pdf},
issn = {0004-6361},
journal = {Astronomy and Astrophysics},
month = {sep},
number = {2},
pages = {463--479},
title = {{AMAZE}},
url = {http://arxiv.org/abs/0806.2410},
volume = {488},
year = {2008},
}
@article{Ma2015,
author = {Ma, Zhongyang and Fang, Guanwen and Kong, Xu and Fan, Lulu},
title = {{Physical properties of distant red galaxies in the COSMOS/UltraVISTA field}},
volume = {67},
number = {5},
year = {2015},
doi = {10.1093/pasj/psv059},
abstract = {We present a study on physical properties for a large distant red galaxy (DRG) sample, using the K-selected multi-band photometry catalog of the COSMOS/UltraVISTA field and the CANDELS near-infrared data. Our sample includes 4485 DRGs with (J − K)AB > 1.16 and KAB < 23.4 mag, and 132 DRGs have HST/WFC3 morphological measurements. The results of nonparametric measurements of DRG morphology are consistent with our rest-frame UVJ color classification; quiescent DRGs are generally compact while star-forming DRGs tend to have extended structures. We find the star formation rate (SFR) and the stellar mass of star-forming DRGs present tight “main sequence” relations in all redshift bins. Moreover, the specific SFR (sSFR) of DRGs increases with redshift in all stellar mass bins and DRGs with higher stellar masses generally have lower sSFRs, which indicates that galaxies were much more active on average in the past, and star formation contributes more to the mass growth of low-mass galaxies than to high-mass galaxies. The infrared-derived SFR dominates the total SFR of DRGs which occupy the high-mass range, implying that the J − K color criterion effectively selects massive and dusty galaxies. DRGs with higher M* generally have redder (U − V)rest colors, and the (U − V)rest colors of DRGs become bluer at higher redshifts, suggesting high-mass galaxies have higher internal dust extinctions or older stellar ages and they evolve with time. Finally, we find that DRGs have different overlap among extremely red objects, BzK galaxies, IRAC-selected extremely red objects, and high-z ultraluminous infrared galaxies, indicating that DRGs are not a special population and they can also be selected by other color criteria.},
url = {http://pasj.oxfordjournals.org/content/67/5/91.abstract},
eprint = {http://pasj.oxfordjournals.org/content/67/5/91.full.pdf+html},
journal = {Publications of the Astronomical Society of Japan},
}
@article{Mandelker2015,
abstract = {We study the evolution of giant clumps in high-z disc galaxies using AMR cosmological simulations at redshifts z=6-1. Our sample consists of 34 galaxies, of halo masses 10{\^{}}{\{}11{\}}-10{\^{}}{\{}12{\}}M{\_}s at z=2, run with and without radiation pressure (RP) feedback from young stars. While RP has little effect on the sizes and global stability of discs, it reduces the amount of star-forming gas by a factor of {\~{}}2, leading to a decrease in stellar mass by a similar factor by z{\~{}}2. Both samples undergo violent disc instability (VDI) and form giant clumps of masses 10{\^{}}7-10{\^{}}9M{\_}s at a similar rate, though RP significantly reduces the number of long-lived clumps. When RP is (not) included, clumps with circular velocity <40(20)km/s, baryonic surface density <200(100)M{\_}s/pc{\^{}}2 and baryonic mass <10{\^{}}{\{}8.2{\}}(10{\^{}}{\{}7.3{\}})M{\_}s are short-lived, disrupted in a few free-fall times. The more massive and dense clumps survive and migrate toward the disc centre over a few disc orbital times. In the RP simulations, the distribution of clump masses and star-formation rates (SFRs) normalized to their host disc is very similar at all redshifts. They exhibit a truncated power-law with a slope slightly shallower than -2. Short-lived clumps preferentially have young stellar ages, low masses, high gas fractions and specific SFRs (sSFR), and they tend to populate the outer disc. The sSFR of massive, long-lived clumps declines with age as they migrate towards the disc centre, producing gradients in mass, stellar age, gas fraction, sSFR and metallicity that distinguish them from short-lived clumps. Ex situ mergers make up {\~{}}37{\%} of the mass in clumps and {\~{}}29{\%} of the SFR. They are more massive and with older stellar ages than the in situ clumps, especially near the disc edge. Roughly half the galaxies at redshifts z=4-1 are clumpy over a wide range of stellar mass, with clumps accounting for {\~{}}3-30{\%} of the SFR but {\~{}}0.1-3{\%} of the stellar mass.},
archiveprefix = {arXiv},
arxivid = {1512.08791},
author = {Mandelker, Nir and Dekel, Avishai and Ceverino, Daniel and DeGraf, Colin and Guo, Yicheng and Primack, Joel},
eprint = {1512.08791},
file = {:home/mel/Documents/Papers/1512.08791v1.pdf:pdf},
month = {dec},
pages = {35},
title = {{Giant Clumps in Simulated High-z Galaxies: Properties, Evolution and Dependence on Feedback}},
url = {http://arxiv.org/abs/1512.08791},
year = {2015},
}
@article{Elmegreen2014,
abstract = {The onset of spiral structure in galaxies appears to occur between redshifts 1.4 and 1.8 when disks have developed a cool stellar component, rotation dominates over turbulent motions in the gas, and massive clumps become less frequent. During the transition from clumpy to spiral disks, two unusual types of spirals are found in the Hubble Ultra Deep Field that are massive, clumpy and irregular like their predecessor clumpy disks, yet spiral-like or sheared like their descendants. One type is ``woolly'' with massive clumpy arms all over the disk and is brighter than other disk galaxies at the same redshift, while another type has irregular multiple arms with high pitch angles, star formation knots and no inner symmetry like today's multiple-arm galaxies. The common types of spirals seen locally are also present in a redshift range around z{\~{}}1, namely grand design with two symmetric arms, multiple arm with symmetry in the inner parts and several long, thin arms in the outer parts, and flocculent, with short, irregular and patchy arms that are mostly from star formation. Normal multiple arm galaxies are found only closer than z{\~{}}0.6 in the UDF. Grand design galaxies extend furthest to z{\~{}}1.8, presumably because interactions can drive a two-arm spiral in a disk that would otherwise have a more irregular structure. The difference between these types is understandable in terms of the usual stability parameters for gas and stars, and the ratio of the velocity dispersion to rotation speed.},
archiveprefix = {arXiv},
arxivid = {1312.2215},
author = {Elmegreen, Debra Meloy and Elmegreen, Bruce G.},
doi = {10.1088/0004-637X/781/1/11},
eprint = {1312.2215},
file = {:home/mel/Documents/Papers/pdf.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {jan},
number = {1},
pages = {11},
title = {{THE ONSET OF SPIRAL STRUCTURE IN THE UNIVERSE}},
url = {http://arxiv.org/abs/1312.2215},
volume = {781},
year = {2014},
}
@article{Cisternas2014,
abstract = {We present empirical constraints on the influence of stellar bars on the fueling of active galactic nuclei (AGNs) out to z=0.84 using a sample of X-ray-selected AGNs hosted in luminous non-interacting face-on and moderately inclined disk galaxies from the Chandra COSMOS survey. Using high-resolution Hubble Space Telescope imaging to identify bars, we find that the fraction of barred active galaxies displays a similar behavior as that of inactive spirals, declining with redshift from 71{\%} at z{\~{}}0.3, to 35{\%} at z{\~{}}0.8. With active galaxies being typically massive, we compare them against a mass-matched sample of inactive spirals and show that, while at face value the AGN bar fraction is slightly higher at all redshifts, we cannot rule out that the bar fractions of active and inactive galaxies are the same. The presence of a bar has no influence on the AGN strength, with barred and unbarred active galaxies showing equivalent X-ray luminosity distributions. From our results, we conclude that the occurrence and the efficiency of the fueling process is independent of the large scale structure of a galaxy. The role of bars, if any, may be restricted to providing the suitable conditions for BH fueling to occur, i.e., bring a fresh supply of gas to the central 100 pc. At the high-redshift end, we find that roughly 60{\%} of active disk galaxies are unbarred. We speculate this to be related with the known dynamical state of disks at higher redshifts---more gas-rich and prone to instabilities than local spirals---which could also lead to gas inflows without the need of bars.},
archiveprefix = {arXiv},
arxivid = {1409.2871},
author = {Cisternas, Mauricio and Sheth, Kartik and Salvato, Mara and Knapen, Johan H. and Civano, Francesca and Santini, Paola},
eprint = {1409.2871},
file = {:home/mel/Documents/Papers/1409.2871v3.pdf:pdf},
month = {sep},
pages = {10},
title = {{The role of bars in AGN fueling in disk galaxies over the last seven billion years}},
url = {http://arxiv.org/abs/1409.2871},
year = {2014},
}
@article{Schawinski2015,
abstract = {We present an observational constraint for the typical active galactic nucleus (AGN) phase lifetime. The argument is based on the time lag between an AGN central engine switching on and becoming visible in X-rays, and the time the AGN then requires to photoionize a large fraction of the host galaxy. Based on the typical light travel time across massive galaxies, and the observed fraction of X-ray selected AGN without AGN-photoionized narrow lines, we estimate that the AGN phase typically lasts {\$}\backslashsim10{\^{}}{\{}5{\}}{\$} years. This lifetime is short compared to the total growth time of {\$}10{\^{}}{\{}7{\}}-10{\^{}}{\{}9{\}}{\$} years estimated from e.g. the Soltan argument and implies that black holes grow via many such short bursts and that AGN therefore flicker on and off. We discuss some consequences of this flickering behavior for AGN feedback and the analogy of X-ray binaries and AGN lifecycles.},
archiveprefix = {arXiv},
arxivid = {1505.06733},
author = {Schawinski, Kevin and Koss, Michael and Berney, Simon and Sartori, Lia},
eprint = {1505.06733},
file = {:home/mel/Documents/Papers/1505.06733v1.pdf:pdf},
month = {may},
title = {{Active galactic nuclei flicker: an observational estimate of the duration of black hole growth phases of {\~{}}1e5 years}},
url = {http://arxiv.org/abs/1505.06733},
year = {2015},
}
@article{Buta2010,
abstract = {Spitzer Space Telescope Infrared Array Camera (IRAC) imaging provides an opportunity to study all known morphological types of galaxies in the mid-IR at a depth significantly better than ground-based near-infrared and optical images. The goal of this study is to examine the imprint of the de Vaucouleurs classification volume in the 3.6 micron band, which is the best Spitzer waveband for galactic stellar mass morphology owing to its depth and its reddening-free sensitivity mainly to older stars. For this purpose, we have prepared classification images for 207 galaxies from the Spitzer archive, most of which are formally part of the Spitzer Survey of Stellar Structure in Galaxies (S{\^{}}4G), a Spitzer post-cryogenic (warm) mission Exploration Science Legacy Program survey of 2,331 galaxies closer than 40 Mpc. For the purposes of morphology, the galaxies are interpreted as if the images are {\{}$\backslash$it blue light{\}}, the historical waveband for classical galaxy classification studies. We find that 3.6 micron classifications are well-correlated with blue-light classifications, to the point where the essential features of many galaxies look very similar in the two very different wavelength regimes. Drastic differences are found only for the most dusty galaxies. Consistent with a previous study by Eskridge et al. (2002), the main difference between blue light and mid-IR types is an approximately 1 stage interval difference for S0/a to Sbc or Sc galaxies, which tend to appear earlier in type at 3.6 microns due to the slightly increased prominence of the bulge, the reduced effects of extinction, and the reduced (but not completely eliminated) effect of the extreme population I stellar component. We present an atlas of all of the 207 galaxies analyzed here, and bring attention to special features or galaxy types that are particularly distinctive in the mid-IR.},
archiveprefix = {arXiv},
arxivid = {1008.0805},
author = {Buta, Ronald J. and Sheth, Kartik and Regan, Michael and Hinz, Joannah L. and {Gil de Paz}, Armando and Men{\'{e}}ndez-Delmestre, Karin and Munoz-Mateos, Juan-Carlos and Seibert, Mark and Laurikainen, Eija and Salo, Heikki and Gadotti, Dimitri A. and Athanassoula, E. and Bosma, Albert and Knapen, Johan H. and Ho, Luis C. and Madore, Barry F. and Elmegreen, Debra M. and Masters, Karen L. and Comer{\'{o}}n, Sebastien and Aravena, Manuel and Kim, Taehyun},
doi = {10.1088/0067-0049/190/1/147},
eprint = {1008.0805},
file = {:home/mel/Documents/Papers/0067-0049{\_}190{\_}1{\_}147.pdf:pdf},
issn = {0067-0049},
journal = {The Astrophysical Journal Supplement Series},
month = {sep},
number = {1},
pages = {147--165},
title = {{MID-INFRARED GALAXY MORPHOLOGY FROM THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S 4 G): THE IMPRINT OF THE DE VAUCOULEURS REVISED HUBBLE-SANDAGE CLASSIFICATION SYSTEM AT 3.6 $\mu$m}},
url = {http://arxiv.org/abs/1008.0805 http://cdsarc.u-strasbg.fr/vizier/ftp/cats/J/ApJS/190/147/table1.dat},
volume = {190},
year = {2010},
}
@article{Schawinski2010,
abstract = {{We use data from the Sloan Digital Sky Survey and visual classifications of morphology from the Galaxy Zoo project to study black hole growth in the nearby Universe (z < 0.05) and to break down the AGN host galaxy population by color, stellar mass and morphology. We find that black hole growth at luminosities L{\_}OIII >1E40 erg/s in early- and late-type galaxies is fundamentally different. AGN host galaxies as a population have a broad range of stellar masses (1E10-1E11 Msun), reside in the green valley of the color-mass diagram and their central black holes have median masses around 1E6.5 Msun. However, by comparing early- and late-type AGN host galaxies to their non-active counterparts, we find several key differences: in early-type galaxies, it is preferentially the galaxies with the least massive black holes that are growing, while late-type galaxies, it is preferentially the most massive{\}}black holes that are growing. The duty cycle of AGN in early-type galaxies is strongly peaked in the green valley below the low-mass end (1E10 Msun) of the red sequence at stellar masses where there is a steady supply of blue cloud progenitors. The duty cycle of AGN in late-type galaxies on the other hand peaks in massive (1E11 Msun) green and red late-types which generally do not have a corresponding blue cloud population of similar mass. At high Eddington ratios (L/L{\_}Edd > 0.1), the only population with a substantial fraction of AGN are the low-mass green valley early-type galaxies. Finally, the Milky Way likely resides in the sweet spot on the color-mass diagram where the AGN duty cycle of late-type galaxies is highest. We discuss the implications of these results for our understanding of the role of AGN in the evolution of galaxies},
archiveprefix = {arXiv},
arxivid = {1001.3141},
author = {Schawinski, Kevin and Urry, C. Megan and Virani, Shanil and Coppi, Paolo and Bamford, Steven P. and Treister, Ezequiel and Lintott, Chris J. and Sarzi, Marc and Keel, William C. and Kaviraj, Sugata and Cardamone, Carolin N. and Masters, Karen L. and Ross, Nicholas P. and Andreescu, Dan and Murray, Phil and Nichol, Robert C. and Raddick, M. Jordan and Slosar, Anze and Szalay, Alex S. and Thomas, Daniel and Vandenberg, Jan},
eprint = {1001.3141},
file = {:home/mel/Documents/Papers/1001.3141v1.pdf:pdf},
month = {jan},
pages = {22},
title = {{Galaxy Zoo: The fundamentally different co-evolution of supermassive black holes and their early- and late-type host galaxies}},
url = {http://arxiv.org/abs/1001.3141},
year = {2010},
}
@article{Arnouts2007,
abstract = {(abridged abstract) We present an analysis of the stellar mass growth over the last 10 Gyrs using a large 3.6{\$}\backslashmu{\$} selected sample. We split our sample into active (blue) and quiescent (red) galaxies. Our measurements of the K-LFs and LD evolution support the idea that a large fraction of galaxies is already assembled at {\$}z\backslashsim 1.2{\$}. Based on the analysis of the evolution of the stellar mass-to-light ratio (in K-band) for the spectroscopic sub-sample, we derive the stellar mass density for the entire sample. We find that the global evolution of the stellar mass density is well reproduced by the star formation rate derived from UV dust corrected measurements. Over the last 8Gyrs, we observe that the stellar mass density of the active population remains approximately constant while it gradually increases for the quiescent population over the same timescale. As a consequence, the growth of the stellar mass in the quiescent population must be due to the shutoff of star formation in active galaxies that migrate into the quiescent population. From {\$}z=2{\$} to {\$}z=1.2{\$}, we observe a major build-up of the quiescent population with an increase by a factor of 10 in stellar mass, suggesting that we are observing the epoch when an increasing fraction of galaxies are ending their star formation activity and start to build up the red sequence.},
archiveprefix = {arXiv},
arxivid = {0705.2438},
author = {Arnouts, S. and Walcher, C. J. and {Le F{\`{e}}vre}, O. and Zamorani, G. and Ilbert, O. and {Le Brun}, V. and Pozzetti, L. and Bardelli, S. and Tresse, L. and Zucca, E. and Charlot, S. and Lamareille, F. and McCracken, H. J. and Bolzonella, M. and Iovino, A. and Lonsdale, C. and Polletta, M. and Surace, J. and Bottini, D. and Garilli, B. and Maccagni, D. and Picat, J. P. and Scaramella, R. and Scodeggio, M. and Vettolani, G. and Zanichelli, A. and Adami, C. and Cappi, A. and Ciliegi, P. and Contini, T. and de la Torre, S. and Foucaud, S. and Franzetti, P. and Gavignaud, I. and Guzzo, L. and Marano, B. and Marinoni, C. and Mazure, A. and Meneux, B. and Merighi, R. and Paltani, S. and Pell{\`{o}}, R. and Pollo, A. and Radovich, M. and Temporin, S. and Vergani, D.},
doi = {10.1051/0004-6361:20077632},
eprint = {0705.2438},
file = {:home/mel/Documents/Papers/0705.2438v3.pdf:pdf},
issn = {0004-6361},
journal = {Astronomy and Astrophysics},
month = {dec},
number = {1},
pages = {137--150},
title = {{The SWIRE-VVDS-CFHTLS surveys: stellar mass assembly over the last 10 Gyr. Evidence for a major build up of the red sequence between z = 2 and z = 1}},
url = {http://arxiv.org/abs/0705.2438},
volume = {476},
year = {2007},
}
@article{Marshall2015,
abstract = {We describe Space Warps, a novel gravitational lens discovery service that yields samples of high purity and completeness through crowd-sourced visual inspection. Carefully produced colour composite images are displayed to volunteers via a web- based classification interface, which records their estimates of the positions of candidate lensed features. Images of simulated lenses, as well as real images which lack lenses, are inserted into the image stream at random intervals; this training set is used to give the volunteers instantaneous feedback on their performance, as well as to calibrate a model of the system that provides dynamical updates to the probability that a classified image contains a lens. Low probability systems are retired from the site periodically, concentrating the sample towards a set of lens candidates. Having divided 160 square degrees of Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) imaging into some 430,000 overlapping 82 by 82 arcsecond tiles and displaying them on the site, we were joined by around 37,000 volunteers who contributed 11 million image classifications over the course of 8 months. This Stage 1 search reduced the sample to 3381 images containing candidates; these were then refined in Stage 2 to yield a sample that we expect to be over 90{\%} complete and 30{\%} pure, based on our analysis of the volunteers performance on training images. We comment on the scalability of the SpaceWarps system to the wide field survey era, based on our projection that searches of 10{\$}{\^{}}5{\$} images could be performed by a crowd of 10{\$}{\^{}}5{\$} volunteers in 6 days.},
archiveprefix = {arXiv},
arxivid = {1504.06148},
author = {Marshall, Philip J. and Verma, Aprajita and More, Anupreeta and Davis, Christopher P. and More, Surhud and Kapadia, Amit and Parrish, Michael and Snyder, Chris and Wilcox, Julianne and Baeten, Elisabeth and Macmillan, Christine and Cornen, Claude and Baumer, Michael and Simpson, Edwin and Lintott, Chris J. and Miller, David and Paget, Edward and Simpson, Robert and Smith, Arfon M. and K{\"{u}}ng, Rafael and Saha, Prasenjit and Collett, Thomas E. and Tecza, Matthias},
eprint = {1504.06148},
file = {:home/mel/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Marshall et al. - 2015 - Space Warps I. Crowd-sourcing the Discovery of Gravitational Lenses.pdf:pdf},
month = {apr},
pages = {21},
title = {{Space Warps: I. Crowd-sourcing the Discovery of Gravitational Lenses}},
url = {http://arxiv.org/abs/1504.06148},
year = {2015},
}
@article{Calvi2014,
abstract = {Cosmological surface brightness dimming of the form {\$}(1+z){\^{}}{\{}-4{\}}{\$} affects all sources. The strong dependence of surface brightness dimming on redshift z suggests the presence of a selection bias when searching for high-redshift galaxies, i.e. we tend to detect only those galaxies with a high surface brightness (SB). However, unresolved knots of emission are not affected by SB dimming, thus providing a way to test the clumpiness of high-z galaxies. Our strategy relies on the comparison of the total flux detected for the same source in surveys characterized by different depth. For all galaxies, deeper images permit the better investigation of low-SB features. Cosmological SB dimming makes these low-SB features hard to detect when going to higher and higher redshifts. We used the GOODS and HUDF Hubble Space Telescope legacy datasets to study the effect of SB dimming on low-SB features of high-redshift galaxies and compare it to the prediction for smooth sources. We selected a sample of Lyman-break galaxies at z{\~{}}4 (i.e. B-band dropouts) detected in all of the datasets and found no significant trend when comparing the total magnitudes measured from images with different depth. Through Monte Carlo simulations we derived the expected trend for galaxies with different SB profiles. The comparison to the datahints at a compact distribution for most of the rest-frame ultraviolet light emitted from high-z galaxies.},
archiveprefix = {arXiv},
arxivid = {1410.2281},
author = {Calvi, V. and Stiavelli, M. and Bradley, L. and Pizzella, A. and Kim, S.},
doi = {10.1088/0004-637X/796/2/102},
eprint = {1410.2281},
file = {:home/mel/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Calvi et al. - 2014 - THE EFFECT OF SURFACE BRIGHTNESS DIMMING IN THE SELECTION OF HIGH- z GALAXIES.pdf:pdf},
issn = {1538-4357},
journal = {The Astrophysical Journal},
month = {nov},
number = {2},
pages = {102},
title = {{THE EFFECT OF SURFACE BRIGHTNESS DIMMING IN THE SELECTION OF HIGH- z GALAXIES}},
url = {http://arxiv.org/abs/1410.2281},
volume = {796},
year = {2014},
}
@article{VanderWel2014,
abstract = {Spectroscopic + photometric redshifts, stellar mass estimates, and rest-frame colors from the 3D-HST survey are combined with structural parameter measurements from CANDELS imaging to determine the galaxy size-mass distribution over the redshift range 0<z<3. Separating early- and late-type galaxies on the basis of star-formation activity, we confirm that early-type galaxies are on average smaller than late-type galaxies at all redshifts, and find a significantly different rate of average size evolution at fixed galaxy mass, with fast evolution for the early-type population, R{\_}eff {\~{}} (1+z){\^{}}-1.48, and moderate evolution for the late-type population, R{\_}eff {\~{}} (1+z){\^{}}-0.75. The large sample size and dynamic range in both galaxy mass and redshift, in combination with the high fidelity of our measurements due to the extensive use of spectroscopic data, not only fortify previous results, but also enable us to probe beyond simple average galaxy size measurements. At all redshifts the slope of the size-mass relation is shallow, R{\_}eff {\~{}} M{\_}star{\^{}}0.22, for late-type galaxies with stellar mass >3x10{\^{}}9 M{\_}sol, and steep, R{\_}eff M{\_}star{\^{}}0.75, for early-type galaxies with stellar mass >2x10{\^{}}10 M{\_}sol. The intrinsic scatter is <{\~{}}0.2 dex for all galaxy types and redshifts. For late-type galaxies, the logarithmic size distribution is not symmetric, but skewed toward small sizes: at all redshifts and masses a tail of small late-type galaxies exists that overlaps in size with the early-type galaxy population. The number density of massive ({\~{}}10{\^{}}11 M{\_}sol), compact (R{\_}eff < 2 kpc) early-type galaxies increases from z=3 to z=1.5-2 and then strongly decreases at later cosmic times.},
archiveprefix = {arXiv},
arxivid = {1404.2844},
author = {van der Wel, A. and Franx, M. and van Dokkum, P. G. and Skelton, R. E. and Momcheva, I. G. and Whitaker, K. E. and Brammer, G. B. and Bell, E. F. and Rix, H.-W. and Wuyts, S. and Ferguson, H. C. and Holden, B. P. and Barro, G. and Koekemoer, A. M. and Chang, Yu-Yen and McGrath, E. J. and H{\"{a}}ussler, B. and Dekel, A. and Behroozi, P. and Fumagalli, M. and Leja, J. and Lundgren, B. F. and Maseda, M. V. and Nelson, E. J. and Wake, D. A. and Patel, S. G. and Labb{\'{e}}, I. and Faber, S. M. and Grogin, N. A. and Kocevski, D. D.},
doi = {10.1088/0004-637X/788/1/28},
eprint = {1404.2844},
file = {:home/mel/Documents/Papers/1404.2844v2.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {jun},
number = {1},
pages = {28},
title = {{3D-HST+CANDELS: THE EVOLUTION OF THE GALAXY SIZE-MASS DISTRIBUTION SINCE z = 3}},
url = {http://arxiv.org/abs/1404.2844},
volume = {788},
year = {2014},
}
@article{Hemmati2014,
abstract = {We perform a detailed study of the resolved properties of emission-line galaxies at kpc-scale to investigate how small-scale and global properties of galaxies are related. 119 galaxies with high-resolution Keck/DEIMOS spectra are selected to cover a wide range in morphologies over the redshift range 0.2<z<1.3. Using the HST/ACS and HST/WFC3 imaging data taken as a part of the CANDELS project, for each galaxy we perform SED fitting per resolution element, producing resolved rest-frame U-V color, stellar mass, star formation rate, age and extinction maps. We develop a technique to identify blue and red regions within individual galaxies, using their rest-frame color maps. As expected, for any given galaxy, the red regions are found to have higher stellar mass surface densities and older ages compared to the blue regions. Furthermore, we quantify the spatial distribution of red and blue regions with respect to both redshift and stellar mass, finding that the stronger concentration of red regions toward the centers of galaxies is not a significant function of either redshift or stellar mass. We find that the main sequence of star forming galaxies exists among both red and blue regions inside galaxies, with the median of blue regions forming a tighter relation with a slope of 1.1+/-0.1 and a scatter of {\~{}}0.2 dex compared to red regions with a slope of 1.3+/-0.1 and a scatter of {\~{}}0.6 dex. The blue regions show higher specific Star Formation Rates (sSFR) than their red counterparts with the sSFR decreasing since z{\~{}}1, driver primarily by the stellar mass surface densities rather than the SFRs at a giver resolution element.},
archiveprefix = {arXiv},
arxivid = {1409.4791},
author = {Hemmati, Shoubaneh and Miller, Sarah H. and Mobasher, Bahram and Nayyeri, Hooshang and Ferguson, Henry C. and Guo, Yicheng and Koekemoer, Anton M. and Koo, David C. and Papovich, Casey},
eprint = {1409.4791},
file = {:home/mel/Documents/Papers/1409.4791v1.pdf:pdf},
month = {sep},
pages = {17},
title = {{Kpc-scale Properties of Emission-line Galaxies}},
url = {http://arxiv.org/abs/1409.4791},
year = {2014},
}
@article{Ho2008,
abstract = {A significant fraction of nearby galaxies show evidence of weak nuclear activity unrelated to normal stellar processes. Recent high-resolution, multiwavelength observations indicate that the bulk of this activity derives from black hole accretion with a wide range of accretion rates. The low accretion rates that typify most low-luminosity active galactic nuclei induce significant modifications to their central engine. The broad-line region and obscuring torus disappear in some of the faintest sources, and the optically thick accretion disk transforms into a three-component structure consisting of an inner radiatively inefficient accretion flow, a truncated outer thin disk, and a jet or outflow. The local census of nuclear activity supports the notion that most, perhaps all, bulges host a central supermassive black hole, although the existence of active nuclei in at least some late-type galaxies suggests that a classical bulge is not a prerequisite to seed a nuclear black hole.},
archiveprefix = {arXiv},
arxivid = {0803.2268},
author = {Ho, Luis C.},
doi = {10.1146/annurev.astro.45.051806.110546},
eprint = {0803.2268},
file = {:home/mel/Documents/Papers/apj{\_}747{\_}1{\_}61.pdf:pdf},
issn = {0066-4146},
journal = {Annual Review of Astronomy and Astrophysics},
month = {sep},
number = {1},
pages = {475--539},
title = {{Nuclear Activity in Nearby Galaxies}},
url = {http://arxiv.org/abs/0803.2268},
volume = {46},
year = {2008},
}
@article{Kim2014,
archiveprefix = {arXiv},
arxivid = {1411.4650},
author = {Kim, Taehyun and Sheth, Kartik and Gadotti, Dimitri A. and Lee, Myung Gyoon and Zaritsky, Dennis and Elmegreen, Bruce G. and Athanassoula, E. and Bosma, Albert and Holwerda, Benne and Ho, Luis C. and Comer{\'{o}}n, S{\'{e}}bastien and Knapen, Johan H. and Hinz, Joannah L. and Mu{\~{n}}oz-Mateos, Juan-Carlos and Erroz-Ferrer, Santiago and Buta, Ronald J. and Kim, Minjin and Laurikainen, Eija and Salo, Heikki and Madore, Barry F. and Laine, Jarkko and Men{\'{e}}ndez-Delmestre, Kar{\'{\i}}n and Regan, Michael W. and de Swardt, Bonita and de Paz, Armando Gil and Seibert, Mark and Mizusawa, Trisha},
eprint = {1411.4650},
file = {:home/mel/Documents/Papers/1411.4650v1.pdf:pdf},
month = {nov},
title = {{The Mass Profile and Shape of Bars in the Spitzer Survey of Stellar Structure in Galaxies (S4G): Search for an Age Indicator for Bars}},
url = {http://arxiv.org/abs/1411.4650v1},
year = {2014},
}
@article{Buta2015,
abstract = {The Spitzer Survey of Stellar Structure in Galaxies (S4G) is the largest available database of deep, homogeneous middle-infrared (mid-IR) images of galaxies of all types. The survey, which includes 2352 nearby galaxies, reveals galaxy morphology only minimally affected by interstellar extinction. This paper presents an atlas and classifications of S4G galaxies in the Comprehensive de Vaucouleurs revised Hubble-Sandage (CVRHS) system. The CVRHS system follows the precepts of classical de Vaucouleurs (1959) morphology, modified to include recognition of other features such as inner, outer, and nuclear lenses, nuclear rings, bars, and disks, spheroidal galaxies, X patterns and box/peanut structures, OLR subclass outer rings and pseudorings, bar ansae and barlenses, parallel sequence late-types, thick disks, and embedded disks in 3D early-type systems. We show that our CVRHS classifications are internally consistent, and that nearly half of the S4G sample consists of extreme late-type systems (mostly bulgeless, pure disk galaxies) in the range Scd-Im. The most common family classification for mid-IR types S0/a to Sc is SA while that for types Scd to Sm is SB. The bars in these two type domains are very different in mid-IR structure and morphology. This paper examines the bar, ring, and type classification fractions in the sample, and also includes several montages of images highlighting the various kinds of stellar structures seen in mid-IR galaxy morphology.},
archiveprefix = {arXiv},
arxivid = {1501.00454},
author = {Buta, Ronald J. and Sheth, Kartik and Athanassoula, E. and Bosma, A. and Knapen, Johan H. and Laurikainen, Eija and Salo, Heikki and Elmegreen, Debra and Ho, Luis C. and Zaritsky, Dennis and Courtois, Helene and Hinz, Joannah L. and Mu{\~{n}}oz-Mateos, Juan-Carlos and Kim, Taehyun and Regan, Michael W. and Gadotti, Dimitri A. and de Paz, Armando Gil and Laine, Jarkko and Men{\'{e}}ndez-Delmestre, Kar{\'{\i}}n and Comer{\'{o}}n, S{\'{e}}bastien and Ferrer, Santiago Erroz and Seibert, Mark and Mizusawa, Trisha and Holwerda, Benne and Madore, Barry F.},
doi = {10.1088/0067-0049/217/2/32},
eprint = {1501.00454},
file = {:home/mel/Documents/Papers/1501.00454v2.pdf:pdf},
issn = {1538-4365},
journal = {The Astrophysical Journal Supplement Series},
month = {apr},
number = {2},
pages = {32},
title = {{A CLASSICAL MORPHOLOGICAL ANALYSIS OF GALAXIES IN THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S 4 G)}},
url = {http://arxiv.org/abs/1501.00454},
volume = {217},
year = {2015},
}
@article{Melvin2014,
abstract = {We measure the redshift evolution of the bar fraction in a sample of 2380 visually selected disc galaxies found in Cosmic Evolution Survey (COSMOS) Hubble Space Telescope (HST) images. The visual classifications used to identify both the disc sample and to indicate the presence of stellar bars were provided by citizen scientists via the Galaxy Zoo: Hubble (GZH) project. We find that the overall bar fraction decreases by a factor of two, from 22+/-5{\%} at z=0.4 (tlb = 4.2 Gyr) to 11+/-2{\%} at z=1.0 (tlb = 7.8 Gyr), consistent with previous analysis. We show that this decrease, of the strong bar fraction in a volume limited sample of massive disc galaxies [stellar mass limit of log(Mstar/Msun) > 10.0], cannot be due to redshift dependent biases hiding either bars or disc galaxies at higher redshifts. Splitting our sample into three bins of mass we find that the decrease in bar fraction is most prominent in the highest mass bin, while the lower mass discs in our sample show a more modest evolution. We also include a sample of 98 red disc galaxies. These galaxies have a high bar fraction (45+/-5{\%}), and are missing from other COSMOS samples which used SED fitting or colours to identify high redshift discs. Our results are consistent with a picture in which the evolution of massive disc galaxies begins to be affected by slow (secular) internal process at z{\~{}}1. We discuss possible connections of the decrease in bar fraction to the redshift, including the growth of stable disc galaxies, mass evolution of the gas content in disc galaxies, as well as the mass dependent effects of tidal interactions.},
archiveprefix = {arXiv},
arxivid = {1401.3334},
author = {Melvin, Thomas and Masters, Karen and Lintott, Chris and Nichol, Robert C. and Simmons, Brooke and Bamford, Steven P. and Casteels, Kevin R. V. and Cheung, Edmond and Edmondson, Edward M. and Fortson, Lucy and Schawinski, Kevin and Skibba, Ramin A. and Smith, Arfon M. and Willett, Kyle W.},
eprint = {1401.3334},
file = {:home/mel/Documents/Papers/1401.3334v1.pdf:pdf},
month = {jan},
pages = {18},
title = {{Galaxy Zoo: An independent look at the evolution of the bar fraction over the last eight billion years from HST-COSMOS}},
url = {http://arxiv.org/abs/1401.3334},
year = {2014},
}
@article{Wilkins2015,
author = {Wilkins, D. R. and Gallo, L. C. and Grupe, D. and Bonson, K. and Komossa, S. and Fabian, A. C.},
doi = {10.1093/mnras/stv2130},
file = {:home/mel/Documents/Papers/MNRAS-2015-Wilkins-4440-51.pdf:pdf},
issn = {0035-8711},
journal = {Monthly Notices of the Royal Astronomical Society},
language = {en},
month = {oct},
number = {4},
pages = {4440--4451},
title = {{Flaring from the supermassive black hole in Mrk 335 studied with Swift and NuSTAR}},
url = {http://adslabs.org/adsabs/abs/2015MNRAS.454.4440W/},
volume = {454},
year = {2015},
}
@article{Cameron2013,
abstract = {I present a critical review of techniques for estimating confidence intervals on binomial population proportions inferred from success counts in small-to-intermediate samples. Population proportions arise frequently as quantities of interest in astronomical research; for instance, in studies aiming to constrain the bar fraction, AGN fraction, SMBH fraction, merger fraction, or red sequence fraction from counts of galaxies exhibiting distinct morphological features or stellar populations. However, two of the most widely-used techniques for estimating binomial confidence intervals--the 'normal approximation' and the Clopper {\&} Pearson approach--are liable to misrepresent the degree of statistical uncertainty present under sampling conditions routinely encountered in astronomical surveys, leading to an ineffective use of the experimental data (and, worse, an inefficient use of the resources expended in obtaining that data). Hence, I provide here an overview of the fundamentals of binomial statistics with two principal aims: (i) to reveal the ease with which (Bayesian) binomial confidence intervals with more satisfactory behaviour may be estimated from the quantiles of the beta distribution using modern mathematical software packages (e.g. R, matlab, mathematica, IDL, python); and (ii) to demonstrate convincingly the major flaws of both the 'normal approximation' and the Clopper {\&} Pearson approach for error estimation.},
archiveprefix = {arXiv},
arxivid = {1012.0566},
author = {Cameron, Ewan},
doi = {10.1071/AS10046},
eprint = {1012.0566},
file = {:home/mel/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Cameron - 2013 - On the Estimation of Confidence Intervals for Binomial Population Proportions in Astronomy The Simplicity and Superiori.pdf:pdf},
issn = {1323-3580},
journal = {Publications of the Astronomical Society of Australia},
month = {jan},
number = {02},
pages = {128--139},
title = {{On the Estimation of Confidence Intervals for Binomial Population Proportions in Astronomy: The Simplicity and Superiority of the Bayesian Approach}},
url = {http://arxiv.org/abs/1012.0566},
volume = {28},
year = {2013},
}
@article{Martin2007,
abstract = {We introduce a new quantity, the mass flux density of galaxies evolving from the blue sequence to the red sequence. We propose a simple technique for constraining this mass flux using the volume corrected number density in the extinction-corrected UV-optical color magnitude distribution, the stellar age indexes H-delta-a and D{\_}n(4000), and a simple prescription for spectral evolution using a quenched star formation history. We exploit the excellent separation of red and blue sequences in the NUV-r band color-magnitude diagram. The final value we measure, 0.033 M{\_}sun yr{\^{}}-1 Mpc{\^{}}-3, is strictly speaking an upper limit due to the possible contributions of bursting, composite, and extincted galaxies. However, it compares favorably with estimates of the average mass flux that we make based on the red luminosity function evolution derived from the DEEPII and COMBO-17 surveys (Bell et al 2004; Faber et al. 2005), 0.034 M{\_}sun yr{\^{}}-1 Mpc{\^{}}-3. We find that the blue sequence mass has remained roughly constant since z=1 (mass flux 0.01 M{\_}sun yr{\^{}}-1 Mpc{\^{}}-3) but the average on-going star formation of 0.037{\$} M{\_}sun yr{\^{}}-1 Mpc{\^{}}-3 over 0<z<1 is balanced by mass flux off the blue sequence. We explore the nature of the galaxies in the transition zone with particular attention to the frequency and impact of AGNs. The AGN fraction peaks in the transition zone. We find circumstantial, albeit weak evidence that the quench rates are higher in higher luminosity AGNs.},
archiveprefix = {arXiv},
arxivid = {astro-ph/0703281},
author = {Martin, D. Christopher and Wyder, Ted K. and Schiminovich, David and Barlow, Tom A. and Forster, Karl and Friedman, Peter G. and Morrissey, Patrick and Neff, Susan G. and Seibert, Mark and Small, Todd and Welsh, Barry Y. and Bianchi, Luciana and Donas, Jose and Heckman, Timothy M. and Lee, Young‐Wook and Madore, Barry F. and Milliard, Bruno and Rich, R. Michael and Szalay, Alex S. and Yi, Sukyoung K.},
doi = {10.1086/516639},
eprint = {0703281},
file = {:home/mel/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Martin et al. - 2007 - The UV‐Optical Galaxy Color‐Magnitude Diagram. III. Constraints on Evolution from the Blue to the Red Sequenc.pdf:pdf;:home/mel/Documents/Papers/martin.pdf:pdf},
issn = {0067-0049},
journal = {The Astrophysical Journal Supplement Series},
month = {dec},
number = {2},
pages = {342--356},
primaryclass = {astro-ph},
title = {{The UV‐Optical Galaxy Color‐Magnitude Diagram. III. Constraints on Evolution from the Blue to the Red Sequence}},
url = {http://arxiv.org/abs/astro-ph/0703281},
volume = {173},
year = {2007},
}
@article{Schawinski2009a,
abstract = {The growth of supermassive black holes and their host galaxies are thought to be linked, but the precise nature of this symbiotic relationship is still poorly understood. Both observations and simulations of galaxy formation suggest that the energy input from active galactic nuclei (AGN), as the central supermassive black hole accretes material and grows, heats the interstellar material and suppresses star formation. In this Letter, we show that most host galaxies of moderate-luminosity supermassive black holes in the local universe have intermediate optical colors that imply the host galaxies are transitioning from star formation to quiescence, the first time this has been shown to be true for all AGN independent of obscuration. The intermediate colors suggest that star formation in the host galaxies ceased roughly 100 Myr ago. This result indicates that either the AGN are very long-lived, accreting for more than 1 Gyr beyond the end of star formation, or there is a {\~{}}100 Myr time delay between the shutdown of star formation and detectable black hole growth. The first explanation is unlikely given current estimates for AGN lifetimes, so low-lumiosity AGN must shut down star formation before substantial black hole accretion activity is detected. The scarcity of AGN host galaxies in the blue cloud reported here challenges scenarios where significant star formation and black hole growth are coeval. Lastly, these observations also strongly support the `Unified Model' of AGN as the host galaxy colors are independent of obscuration towards the central engine.},
archiveprefix = {arXiv},
arxivid = {0901.1663},
author = {Schawinski, Kevin and Virani, Shanil and Simmons, Brooke and Urry, C. Megan and Treister, Ezequiel and Kaviraj, Sugata and Kushkuley, Bronika},
doi = {10.1088/0004-637X/692/1/L19},
eprint = {0901.1663},
file = {:home/mel/Documents/Papers/0901.1663v2.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {feb},
number = {1},
pages = {L19--L23},
title = {{DO MODERATE-LUMINOSITY ACTIVE GALACTIC NUCLEI SUPPRESS STAR FORMATION?}},
url = {http://arxiv.org/abs/0901.1663},
volume = {692},
year = {2009},
}
@article{Griffith2012,
abstract = {We present the Advanced Camera for Surveys General Catalog (ACS-GC), a photometric and morphological database using publicly available data obtained with the Advanced Camera for Surveys (ACS) instrument on the Hubble Space Telescope. The goal of the ACS-GC database is to provide a large statistical sample of galaxies with reliable structural and distance measurements to probe the evolution of galaxies over a wide range of look-back times. The ACS-GC includes approximately 470,000 astronomical sources (stars + galaxies) derived from the AEGIS, COSMOS, GEMS, and GOODS surveys. Galapagos was used to construct photometric (SExtractor) and morphological (Galfit) catalogs. The analysis assumes a single S$\backslash$'ersic model for each object to derive quantitative structural parameters. We include publicly available redshifts from the DEEP2, COMBO-17, TKRS, PEARS, ACES, CFHTLS,and zCOSMOS surveys to supply redshifts (spectroscopic and photometric) for a considerable fraction ({\~{}}74{\%}) of the imaging sample. The ACS-GC includes color postage stamps, Galfit residual images, and photometry, structural parameters, and redshifts combined into a single catalog.},
archiveprefix = {arXiv},
arxivid = {1203.1651},
author = {Griffith, Roger L. and Cooper, Michael C. and Newman, Jeffrey A. and Moustakas, Leonidas A. and Stern, Daniel and Comerford, Julia M. and Davis, Marc and Lotz, Jennifer M. and Barden, Marco and Conselice, Christopher J. and Capak, Peter L. and Faber, S. M. and Kirkpatrick, J. Davy and Koekemoer, Anton M. and Koo, David C. and Noeske, Kai G. and Scoville, Nick and Sheth, Kartik and Shopbell, Patrick and Willmer, Christopher N. A. and Weiner, Benjamin},
doi = {10.1088/0067-0049/200/1/9},
eprint = {1203.1651},
file = {:home/mel/Documents/Papers/apjs{\_}200{\_}1{\_}9.pdf:pdf},
issn = {0067-0049},
journal = {The Astrophysical Journal Supplement Series},
month = {may},
number = {1},
pages = {9},
title = {{THE ADVANCED CAMERA FOR SURVEYS GENERAL CATALOG: STRUCTURAL PARAMETERS FOR APPROXIMATELY HALF A MILLION GALAXIES}},
url = {http://arxiv.org/abs/1203.1651},
volume = {200},
year = {2012},
}
@article{Hogg2002,
abstract = {The K correction corrects for the fact that sources observed at different redshifts are, in general, compared with standards or each other at different rest-frame wavelengths. It is part of the relation between the emitted- or rest-frame absolute magnitude of a source in one broad photometric bandpass to the observed-frame apparent magnitude of the same source in another broad bandpass. This short pedagogical paper provides definitions of and equations for the K correction.},
archiveprefix = {arXiv},
arxivid = {astro-ph/0210394},
author = {Hogg, David W. and Baldry, Ivan K. and Blanton, Michael R. and Eisenstein, Daniel J.},
eprint = {0210394},
file = {:home/mel/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Hogg et al. - 2002 - The K correction.pdf:pdf},
month = {oct},
primaryclass = {astro-ph},
title = {{The K correction}},
url = {http://arxiv.org/abs/astro-ph/0210394},
year = {2002},
}
@article{Heckman2014,
archiveprefix = {arXiv},
arxivid = {1403.4620},
author = {Heckman, Timothy and Best, Philip},
eprint = {1403.4620},
file = {:home/mel/Documents/Papers/1403.4620v1.pdf:pdf},
month = {mar},
title = {{The Co-Evolution of Galaxies and Supermassive Black Holes: Insights from Surveys of the Contemporary Universe}},
url = {http://arxiv.org/abs/1403.4620},
year = {2014},
}
@article{Cardamone2010,
annote = {MUSYC photo and speczs},
author = {Cardamone, Carolin N. and van Dokkum, Pieter G. and Urry, C. Megan and Taniguchi, Yoshi and Gawiser, Eric and Brammer, Gabriel and Taylor, Edward and Damen, Maaike and Treister, Ezequiel and Cobb, Bethany E. and Bond, Nicholas and Schawinski, Kevin and Lira, Paulina and Murayama, Takashi and Saito, Tomoki and Sumikawa, Kentaro},
doi = {10.1088/0067-0049/189/2/270},
file = {:home/mel/Documents/Papers/musyc.pdf:pdf},
issn = {0067-0049},
journal = {The Astrophysical Journal Supplement Series},
language = {en},
month = {aug},
number = {2},
pages = {270--285},
title = {{THE MULTIWAVELENGTH SURVEY BY YALE–CHILE (MUSYC): DEEP MEDIUM-BAND OPTICAL IMAGING AND HIGH-QUALITY 32-BAND PHOTOMETRIC REDSHIFTS IN THE ECDF-S}},
url = {http://adslabs.org/adsabs/abs/2010ApJS..189..270C/},
volume = {189},
year = {2010},
}
@article{Jarrett2000,
author = {Jarrett, T. H.},
doi = {10.1086/316603},
file = {:home/mel/Documents/Papers/316603.pdf:pdf},
issn = {0004-6280},
journal = {Publications of the Astronomical Society of the Pacific},
language = {en},
month = {aug},
number = {774},
pages = {1008--1080},
title = {{Near‐Infrared Galaxy Morphology Atlas}},
url = {http://adslabs.org/adsabs/abs/2000PASP..112.1008J/},
volume = {112},
year = {2000},
}
@article{Scarlata2007,
author = {Scarlata, C. and Carollo, C. M. and Lilly, S. and Sargent, M. T. and Feldmann, R. and Kampczyk, P. and Porciani, C. and Koekemoer, A. and Scoville, N. and Kneib, J.‐P. and Leauthaud, A. and Massey, R. and Rhodes, J. and Tasca, L. and Capak, P. and Maier, C. and McCracken, H. J. and Mobasher, B. and Renzini, A. and Taniguchi, Y. and Thompson, D. and Sheth, K. and Ajiki, M. and Aussel, H. and Murayama, T. and Sanders, D. B. and Sasaki, S. and Shioya, Y. and Takahashi, M.},
doi = {10.1086/516582},
file = {:home/mel/Documents/Papers/zest.pdf:pdf},
issn = {0067-0049},
journal = {The Astrophysical Journal Supplement Series},
language = {en},
month = {sep},
number = {1},
pages = {406--433},
title = {{COSMOS Morphological Classification with the Zurich Estimator of Structural Types (ZEST) and the Evolution Since z = 1 of the Luminosity Function of Early, Disk, and Irregular Galaxies}},
url = {http://adslabs.org/adsabs/abs/2007ApJS..172..406S/},
volume = {172},
year = {2007},
}
@article{Cheung2014,
abstract = {We present a new study investigating whether active galactic nuclei (AGN) beyond the local universe are preferentially fed via large-scale bars. Our investigation combines data from Chandra and Galaxy Zoo: Hubble (GZH) in the AEGIS, COSMOS, and GOODS-S surveys to create samples of face-on, disc galaxies at 0.2 < z < 1.0. We use a novel method to robustly compare a sample of 120 AGN host galaxies, defined to have 10{\^{}}42 erg/s < L{\_}X < 10{\^{}}44 erg/s, with inactive control galaxies matched in stellar mass, rest-frame colour, size, Sersic index, and redshift. Using the GZH bar classifications of each sample, we demonstrate that AGN hosts show no statistically significant enhancement in bar fraction or average bar likelihood compared to closely-matched inactive galaxies. In detail, we find that the AGN bar fraction cannot be enhanced above the control bar fraction by more than a factor of two, at 99.7{\%} confidence. We similarly find no significant difference in the AGN fraction among barred and non-barred galaxies. Thus we find no compelling evidence that large-scale bars directly fuel AGN at 0.2<z<1.0. This result, coupled with previous results at z=0, implies that moderate-luminosity AGN have not been preferentially fed by large-scale bars since z=1. Furthermore, given the low bar fractions at z>1, our findings suggest that large-scale bars have likely never directly been a dominant fueling mechanism for supermassive black hole growth.},
archiveprefix = {arXiv},
arxivid = {1409.5434},
author = {Cheung, Edmond and Trump, Jonathan R. and Athanassoula, E. and Bamford, Steven P. and Bell, Eric F. and Bosma, A. and Cardamone, Carolin N. and Casteels, Kevin R. V. and Faber, S. M. and Fang, Jerome J. and Fortson, Lucy F. and Kocevski, Dale D. and Koo, David C. and Laine, Seppo and Lintott, Chris and Masters, Karen L. and Melvin, Thomas and Nichol, Robert C. and Schawinski, Kevin and Simmons, Brooke and Smethurst, Rebecca and Willett, Kyle W.},
eprint = {1409.5434},
file = {:home/mel/Documents/Papers/1409.5434v2.pdf:pdf},
month = {sep},
pages = {13},
title = {{Galaxy Zoo: Are Bars Responsible for the Feeding of Active Galactic Nuclei at 0.2 < z < 1.0?}},
url = {http://arxiv.org/abs/1409.5434},
year = {2014},
}
@article{Coelho2011,
abstract = {We obtained stellar ages and metallicities via spectrum fitting for a sample of 575 bulges with spectra available from the Sloan Digital Sky Survey. The structural properties of the galaxies have been studied in detail in Gadotti (2009b) and the sample contains 251 bulges in galaxies with bars. Using the whole sample, where galaxy stellar mass distributions for barred and unbarred galaxies are similar, we find that bulges in barred and unbarred galaxies occupy similar loci in the age vs. metallicity plane. However, the distribution of bulge ages in barred galaxies shows an excess of populations younger than {\~{}} 4 Gyr, when compared to bulges in unbarred galaxies. Kolmogorov-Smirnov statistics confirm that the age distributions are different with a significance of 99.94{\%}. If we select sub-samples for which the bulge stellar mass distributions are similar for barred and unbarred galaxies, this excess vanishes for galaxies with bulge mass log M < 10.1 M{\_}Sun while for more massive galaxies we find a bimodal bulge age distribution for barred galaxies only, corresponding to two normal distributions with mean ages of 10.4 and 4.7 Gyr. We also find twice as much AGN among barred galaxies, as compared to unbarred galaxies, for low-mass bulges. By combining a large sample of high quality data with sophisticated image and spectral analysis, we are able to find evidence that the presence of bars affect the mean stellar ages of bulges. This lends strong support to models in which bars trigger star formation activity in the centers of galaxies.},
archiveprefix = {arXiv},
arxivid = {1111.1736},
author = {Coelho, Paula and Gadotti, Dimitri A.},
eprint = {1111.1736},
file = {:home/mel/Documents/Papers/1111.1736v1.pdf:pdf},
month = {nov},
pages = {5},
title = {{Bars rejuvenating bulges? Evidence from stellar population analysis}},
url = {http://arxiv.org/abs/1111.1736},
year = {2011},
}
@article{Tojeiro2013,
abstract = {[Abridged] We study the spectral properties of intermediate mass galaxies as a function of colour and morphology. We use Galaxy Zoo to define three morphological classes of galaxies, namely early-types (ellipticals), late-type (disk-dominated) face-on spirals and early-type (bulge-dominated) face-on spirals. We classify these galaxies as blue or red according to their SDSS g-r colour and use the spectral fitting code VESPA to calculate time-resolved star-formation histories, metallicity and total starlight dust extinction from their SDSS fibre spectra. We find that red late-type spirals show less star-formation in the last 500 Myr than blue late-type spirals by up to a factor of three, but share similar star-formation histories at earlier times. This decline in recent star-formation explains their redder colour: their chemical and dust content are the same. We postulate that red late-type spirals are recent descendants of blue late-type spirals, with their star-formation curtailed in the last 500 Myrs. The red late-type spirals are however still forming stars approximately 17 times faster than red ellipticals over the same period. Red early-type spirals lie between red late-type spirals and red ellipticals in terms of recent-to-intermediate star-formation and dust content. Therefore, it is plausible that these galaxies represent an evolutionary link between these two populations. They are more likely to evolve directly into red ellipticals than red late-type spirals. Blue ellipticals show similar star-formation histories as blue spirals (regardless of type), except they have formed less stars in the last 100 Myrs. However, blue ellipticals have different dust content, which peaks at lower extinction values than all spiral galaxies.},
archiveprefix = {arXiv},
arxivid = {1303.3551},
author = {Tojeiro, R. and Masters, K. L. and Richards, J. and Percival, W. J. and Bamford, S. P. and Maraston, C. and Nichol, R. C. and Skibba, R. and Thomas, D.},
doi = {10.1093/mnras/stt484},
eprint = {1303.3551},
file = {:home/mel/Documents/Papers/1303.3551v1.pdf:pdf},
issn = {0035-8711},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {apr},
number = {1},
pages = {359--373},
title = {{The different star formation histories of blue and red spiral and elliptical galaxies}},
url = {http://arxiv.org/abs/1303.3551},
volume = {432},
year = {2013},
}
@article{Galloway2015,
abstract = {We study the influence of the presence of a strong bar in disc galaxies which host an active galactic nucleus (AGN). Using data from the Sloan Digital Sky Survey and morphological classifications from the Galaxy Zoo 2 project, we create a volume-limited sample of 19,756 disc galaxies at {\$}0.01<z<0.05{\$} which have been visually examined for the presence of a bar. Within this sample, AGN host galaxies have a higher overall percentage of bars (51.8{\%}) than inactive galaxies exhibiting central star formation (37.1{\%}). This difference is primarily due to known effects; that the presence of both AGN and galactic bars is strongly correlated with both the stellar mass and integrated colour of the host galaxy. We control for this effect by examining the difference in AGN fraction between barred and unbarred galaxies in fixed bins of mass and colour. Once this effect is accounted for, there remains a small but statistically significant increase that represents 16{\%} of the average barred AGN fraction. Using the {\$}L{\_}{\{}\backslashrm{\{}[O III]{\}}{\}}/M{\_}{\{}BH{\}} {\$}ratio as a measure of AGN strength, we show that barred AGN do not exhibit stronger accretion than unbarred AGN at a fixed mass and colour. The data are consistent with a model in which bar-driven fueling does contribute to the probability of an actively growing black hole, but in which other dynamical mechanisms must contribute to the direct AGN fueling via smaller, non-axisymmetric perturbations.},
archiveprefix = {arXiv},
arxivid = {1502.01033},
author = {Galloway, M. A. and Willett, K. W. and Fortson, L. F. and Cardamone, C. N. and Schawinski, K. and Cheung, E. and Lintott, C. J. and Masters, K. L. and Melvin, T. and Simmons, B. D.},
doi = {10.1093/mnras/stv235},
eprint = {1502.01033},
file = {:home/mel/Documents/GZ2{\_}Bar{\_}AGN{\_}Project/galloway{\_}2015{\_}Source{\_}Files/galloway{\_}BarAGN{\_}2015.pdf:pdf},
issn = {0035-8711},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {mar},
number = {4},
pages = {3442--3454},
title = {{Galaxy Zoo: the effect of bar-driven fuelling on the presence of an active galactic nucleus in disc galaxies}},
url = {http://arxiv.org/abs/1502.01033},
volume = {448},
year = {2015},
}
@article{Monari2015,
abstract = {Evidence for non-zero mean stellar velocities in the direction perpendicular to the Galactic plane has been accumulating from various recent large spectroscopic surveys. Previous analytical and numerical work has shown that a breathing mode of the Galactic disc, similar to what is observed in the Solar vicinity, can be the natural consequence of a non-axisymmetric internal perturbation of the disc. Here we provide a general analytical framework, in the context of perturbation theory, allowing us to compute the vertical bulk motions generated by a single internal perturber (bar or spiral pattern). In the case of the Galactic bar, we show that these analytically predicted bulk motions are well in line with the outcome of a numerical simulation. The mean vertical motions induced by the Milky Way bar are small (mean velocity of less than 1 km/sec) and cannot be responsible alone for the observed breathing mode, but they are existing. Our analytical treatment is valid close to the plane for all the non-axisymmetric perturbations of the disc that can be described by small-amplitude Fourier modes. Further work should study how the coupling of multiple internal perturbers and external perturbers is affecting the present analytical results.},
archiveprefix = {arXiv},
arxivid = {1505.07456},
author = {Monari, Giacomo and Famaey, Benoit and Siebert, Arnaud},
eprint = {1505.07456},
file = {:home/mel/Documents/Papers/1505.07456v1.pdf:pdf},
month = {may},
pages = {9},
title = {{The vertical effects of disc non-axisymmetries from perturbation theory: the case of the Galactic bar}},
url = {http://arxiv.org/abs/1505.07456},
year = {2015},
}
@article{Liu2015,
abstract = {It is commonly believed that the optical/UV and X-ray emissions in luminous AGN are produced in an accretion disk and an embedded hot corona respectively. The inverse Compton scattering of disk photons by hot electrons in the corona can effectively cool the coronal gas if the mass supply is predominantly via a cool disk like flow as in BHXRBs. Thus, the application of such a model to AGNs fails to produce their observed X-ray emission. As a consequence, a fraction of disk accretion energy is usually assumed to be transferred to the corona. To avoid this assumption, we propose that gas in a vertically extended distribution is supplied to a supermassive black hole by the gravitational capture of interstellar medium or stellar wind material. In this picture, the gas partially condenses to an underlying cool disk as it flows toward the black hole, releasing accretion energy as X-ray emission and supplying mass for the disk accretion. Detailed numerical calculations reveal that the X-ray luminosity can reach a few tens of percent of the bolometric luminosity. The value of {\$}\backslashalpha{\_}{\{}\backslashrm ox{\}}{\$} varies from 0.9 to 1.2 for the mass supply rate ranging from 0.03 to 0.1 times the Eddington value. The corresponding photon index in the 2-10 keV energy band varies from 1.9 to 2.3. Such a picture provides a natural extension of the model for low luminosity AGN where condensation is absent at low mass accretion rates and no optically thick disk exists in the inner region.},
archiveprefix = {arXiv},
arxivid = {1505.00551},
author = {Liu, B. F. and Taam, R. E. and Qiao, E. and Yuan, W.},
eprint = {1505.00551},
file = {:home/mel/Documents/Papers/1505.00551v1.pdf:pdf},
month = {may},
pages = {21},
title = {{A Hybrid Two Component Accretion Flow Surrounding Supermassive Black Holes in AGN}},
url = {http://arxiv.org/abs/1505.00551},
year = {2015},
}
@article{Carollo2014,
abstract = {We use ZENS data at low redshift to study the dependence of the quenched satellite fraction and of the morphological mix of these quenched satellites, on three different environmental parameters: group halo mass, halo-centric distance and large-scale structure over-density. The fraction of quenched satellites is independent of halo mass and the surrounding large-scale overdensity, but increases towards the centres of the haloes, as previously found. The morphological mix is, however, constant with radial position, indicating that the well-known morphology-density relation results from the increasing fraction of quenched galaxies towards the centres of haloes. The constancy of the morphological outcome suggests that mass-quenching and satellite quenching have the same effect on the morphologies of the galaxies. The quenched satellites have larger B/T and smaller half-light radii than the star-forming satellites. These are mostly due to differences in the disks. The bulges in quenched satellites have very similar luminosities and surface brightness profiles, and any mass growth of the bulges associated with quenching cannot greatly change these quantities. The quenched disks are fainter and have smaller scale lengths than in star-forming satellites. This can be explained either by a differential fading of the disks or if disks were generally smaller in the past, both of which are expected in an inside-out growth of disks. At least at low redshifts, the structure of massive quenched satellites is produced by processes that operate before quenching takes place. A comparison with semi-analytic models argues for a reduction in the efficiency of group halos in quenching their disk satellites and for mechanisms to increase the B/T of low mass quenched satellites. [abridged]},
archiveprefix = {arXiv},
arxivid = {1402.1172},
author = {Carollo, C. M. and Cibinel, A. and Lilly, S. J. and Pipino, A. and Bonoli, S. and Finoguenov, A. and Miniati, F. and Norberg, P. and Silverman, J. D.},
eprint = {1402.1172},
file = {:home/mel/Documents/Papers/1402.1172v1.pdf:pdf},
month = {feb},
pages = {23},
title = {{ZENS IV. Similar Morphological Changes associated with Mass- and Environment-Quenching, and the Relative importance of Bulge Growth versus the Fading of Disks}},
url = {http://arxiv.org/abs/1402.1172},
year = {2014},
}
@article{Mehta2015,
abstract = {Upcoming space-based surveys such as Euclid and WFIRST-AFTA plan to measure Baryonic Acoustic Oscillations (BAOs) in order to study dark energy. These surveys will use IR slitless grism spectroscopy to measure redshifts of a large number of galaxies over a significant redshift range. In this paper, we use the WFC3 Infrared Spectroscopic Parallel Survey (WISP) to estimate the expected number of Halpha (Ha) emitters observable by these future surveys. WISP is an ongoing HST slitless spectroscopic survey, covering the 0.8-1.65micron wavelength range and allowing the detection of Ha emitters up to z{\~{}}1.5 and [OIII] emitters to z{\~{}}2.3. We derive the Ha-[OIII] bivariate line luminosity function for WISP galaxies at z{\~{}}1 using a maximum likelihood estimator that properly accounts for uncertainties in line luminosity measurement, and demonstrate how it can be used to derive the Ha luminosity function from exclusively fitting [OIII] data. Using the z{\~{}}2 [OIII] line luminosity function, and assuming that the relation between Ha and [OIII] luminosity does not change significantly over the redshift range, we predict the Ha number counts at z{\~{}}2 - the upper end of the redshift range of interest for the future surveys. For the redshift range 0.7<z<2, we expect {\~{}}3000 galaxies/deg{\^{}}2 for a flux limit of 3x10{\^{}}{\{}-16{\}} ergs/s/cm{\^{}}2 (the proposed depth of Euclid galaxy redshift survey) and {\~{}}20,000 galaxies/deg{\^{}}2 for a flux limit of {\~{}}10{\^{}}{\{}-16{\}} ergs/s/cm{\^{}}2 (the baseline depth of WFIRST galaxy redshift survey).},
archiveprefix = {arXiv},
arxivid = {1505.07843},
author = {Mehta, Vihang and Scarlata, Claudia and Colbert, James W. and Dai, Sophia and Dressler, Alan and Henry, Alaina and Malkan, Matt and Rafelski, Marc and Siana, Brian and Teplitz, Harry and Bagley, Micaela and Beck, Melanie and Ross, Nathaniel R. and Rutkowski, Michael and Wang, Yun},
eprint = {1505.07843},
file = {:home/mel/Documents/Papers/1505.07843v1.pdf:pdf},
month = {may},
title = {{Predicting the redshift 2 Halpha luminosity function using [OIII] emission line galaxies}},
url = {http://arxiv.org/abs/1505.07843},
year = {2015},
}
@article{Meert2015,
author = {Meert, Alan and Vikram, Vinu and Bernardi, Mariangela},
doi = {10.1093/mnras/stv2475},
file = {:home/mel/Documents/Papers/MNRAS-2016-Meert-2440-52.pdf:pdf},
issn = {0035-8711},
journal = {Monthly Notices of the Royal Astronomical Society},
language = {en},
month = {nov},
number = {3},
pages = {2440--2452},
title = {{A catalogue of two-dimensional photometric decompositions in the SDSS-DR7 spectroscopic main galaxy sample: extension to g and i bands}},
url = {http://adslabs.org/adsabs/abs/2016MNRAS.455.2440M/},
volume = {455},
year = {2015},
}
@article{Wolf2008,
abstract = {We present an update to the photometric calibration of the COMBO-17 catalogue on the Extended Chandra Deep Field South, which is now consistent with the GaBoDS and MUSYC catalogues. As a result, photometric redshifts become slightly more accurate, with <0.01 rms and little bias in the delta{\_}z/(1+z) of galaxies with R<21 and of QSOs with R<24. With increasing photon noise the rms of galaxies reaches 0.02 for R<23 and 0.035 at R{\~{}}23.5. Consequences for the rest-frame colours of galaxies at z<1 are discussed.},
annote = {GOODS-S and GEMS photozs 2 (also Wolf et al 2004)},
archiveprefix = {arXiv},
arxivid = {0809.2066},
author = {Wolf, C. and Hildebrandt, H. and Taylor, E. N. and Meisenheimer, K.},
doi = {10.1051/0004-6361:200810954},
eprint = {0809.2066},
file = {:home/mel/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Wolf et al. - 2008 - Calibration update of the COMBO-17 CDFS catalogue.pdf:pdf},
issn = {0004-6361},
journal = {Astronomy and Astrophysics},
month = {dec},
number = {3},
pages = {933--936},
title = {{Calibration update of the COMBO-17 CDFS catalogue}},
url = {http://arxiv.org/abs/0809.2066},
volume = {492},
year = {2008},
}
@article{Stern2014,
author = {Stern, D. and Lansbury, G. B. and Assef, R. J. and Brandt, W. N. and Alexander, D. M. and Ballantyne, D. R. and Balokovi{\'{c}}, M. and Bauer, F. E. and Benford, D. and Blain, A. and Boggs, S. E. and Bridge, C. and Brightman, M. and Christensen, F. E. and Comastri, A. and Craig, W. W. and {Del Moro}, A. and Eisenhardt, P. R. M. and Gandhi, P. and Griffith, R. L. and Hailey, C. J. and Harrison, F. A. and Hickox, R. C. and Jarrett, T. H. and Koss, M. and Lake, S. and LaMassa, S. M. and Luo, B. and Tsai, C.-W. and Urry, C. M. and Walton, D. J. and Wright, E. L. and Wu, J. and Yan, L. and Zhang, W. W.},
doi = {10.1088/0004-637X/794/2/102},
file = {:home/mel/Documents/Papers/wise14.pdf:pdf},
issn = {1538-4357},
journal = {The Astrophysical Journal},
language = {en},
month = {sep},
number = {2},
pages = {102},
title = {{NuSTAR AND XMM-NEWTON OBSERVATIONS OF LUMINOUS, HEAVILY OBSCURED, WISE -SELECTED QUASARS AT Z ∼ 2}},
url = {http://adslabs.org/adsabs/abs/2014ApJ...794..102S/},
volume = {794},
year = {2014},
}
@article{Alonso2012,
abstract = {With the aim of assessing the effects of bars on active galactic nuclei (AGN), we present an analysis of host characteristics and nuclear activity of AGN galaxies with and without bars selected from the Sloan Digital Sky Survey Data Release 7 (SDSS-DR7). By visual inspection of SDSS images we classified the hosts of face-on AGN spiral galaxies brighter than g < 16.5 into barred or unbarred. With the purpose of providing an appropriate quantification of the effects of bars, we also constructed a suitable control sample of unbarred AGN galaxies with similar redshift, magnitude, morphology, bulge sizes and local environment distributions. We find that the bar fraction, with respect to the full sample of spiral face-on AGN host galaxies, is 28.5{\%}, in good agreement with previous works. Barred AGN host galaxies show an excess of young stellar populations dominated by red u-r and g-r colors, with respect to the control sample, suggesting that bars produce an important effect on galaxy properties of AGN hosts. Regarding the nuclear activity distribution, we find that barred AGN galaxies show a shift toward higher Lum[OIII] values with respect to AGN without bars. In addition, we also find that this trend is more significant in less massive, younger stellar population and bluer AGN host galaxies. We found that the fraction of powerful AGN increase towards more massive hosts with bluer colors and younger stellar populations residing in denser environments. However, barred host AGN systematically show a higher fraction of powerful active nuclei galaxies with respect to the control sample. We also explored the accretion rate onto the central black holes finding that barred AGN show an excess of objects with high accretion rate values with respect to unbarred AGN galaxies.},
archiveprefix = {arXiv},
arxivid = {1211.5156},
author = {Alonso, Sol and Coldwell, Georgina and Lambas, Diego Garcia},
eprint = {1211.5156},
file = {:home/mel/Documents/Papers/1211.5156v1.pdf:pdf},
month = {nov},
pages = {10},
title = {{Effect of bars in AGN host galaxies and black hole activity}},
url = {http://arxiv.org/abs/1211.5156},
year = {2012},
}
@article{Peng2010,
abstract = {We explore the inter-relationships between mass, star-formation rate and environment in the SDSS, zCOSMOS and other surveys. The differential effects of mass and environment are completely separable to z {\~{}} 1, indicating that two distinct processes are operating, mass-quenching and environment-quenching. Environment-quenching, at fixed over-density, evidently does not change with epoch to z {\~{}} 1, suggesting that it occurs as large-scale structure develops in the Universe. The observed constancy of the mass-function shape for star-forming galaxies, demands that the mass-quenching of galaxies around and above M*, must be proportional to their star-formation rates at all z < 2. We postulate that this simple mass-quenching law also holds over a much broader range of stellar mass and epoch. These two simple quenching processes, plus some additional quenching due to merging, then naturally produce (a) a quasi-static Schechter mass function for star-forming galaxies with a value of M* that is set by the proportionality between the star-formation and mass-quenching rates, (b) a double Schechter function for passive galaxies with two components: the dominant one is produced by mass-quenching and has exactly the same M* as the star-forming galaxies but an alpha shallower by +1, while the other is produced by environment effects and has the same M* and alpha as the star-forming galaxies, and is larger in high density environments. Subsequent merging of quenched galaxies modifies these predictions somewhat in the denser environments, slightly increasing M* and making alpha more negative. All of these detailed quantitative relationships between the Schechter parameters are indeed seen in the SDSS, lending strong support to our simple empirically-based model. The model naturally produces for passive galaxies the anti-hierarchical run of mean ages and alpha-element abundances with mass.},
archiveprefix = {arXiv},
arxivid = {1003.4747},
author = {Peng, Ying-jie and Lilly, Simon J. and Kova{\v{c}}, Katarina and Bolzonella, Micol and Pozzetti, Lucia and Renzini, Alvio and Zamorani, Gianni and Ilbert, Olivier and Knobel, Christian and Iovino, Angela and Maier, Christian and Cucciati, Olga and Tasca, Lidia and Carollo, C. Marcella and Silverman, John and Kampczyk, Pawel and de Ravel, Loic and Sanders, David and Scoville, Nicholas and Contini, Thierry and Mainieri, Vincenzo and Scodeggio, Marco and Kneib, Jean-Paul and {Le F{\`{e}}vre}, Olivier and Bardelli, Sandro and Bongiorno, Angela and Caputi, Karina and Coppa, Graziano and de la Torre, Sylvain and Franzetti, Paolo and Garilli, Bianca and Lamareille, Fabrice and {Le Borgne}, Jean-Francois and {Le Brun}, Vincent and Mignoli, Marco and Montero, Enrique Perez and Pello, Roser and Ricciardelli, Elena and Tanaka, Masayuki and Tresse, Laurence and Vergani, Daniela and Welikala, Niraj and Zucca, Elena and Oesch, Pascal and Abbas, Ummi and Barnes, Luke and Bordoloi, Rongmon and Bottini, Dario and Cappi, Alberto and Cassata, Paolo and Cimatti, Andrea and Fumana, Marco and Hasinger, Gunther and Koekemoer, Anton and Leauthaud, Alexei and Maccagni, Dario and Marinoni, Christian and McCracken, Henry and Memeo, Pierdomenico and Meneux, Baptiste and Nair, Preethi and Porciani, Cristiano and Presotto, Valentina and Scaramella, Roberto},
doi = {10.1088/0004-637X/721/1/193},
eprint = {1003.4747},
file = {:home/mel/Documents/Papers/1003.4747v2.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {sep},
number = {1},
pages = {193--221},
title = {{MASS AND ENVIRONMENT AS DRIVERS OF GALAXY EVOLUTION IN SDSS AND zCOSMOS AND THE ORIGIN OF THE SCHECHTER FUNCTION}},
url = {http://arxiv.org/abs/1003.4747},
volume = {721},
year = {2010},
}
@article{Muzahid2015,
abstract = {We present a detailed analysis of a large-scale galactic outflow in the CGM of a massive (M{\_}h {\~{}} 10{\^{}}12.5 Msun), star-forming (6.9 Msun/yr), sub-L* (0.5 L{\_}B*) galaxy at z=0.39853 that exhibits a wealth of metal-line absorption in the spectra of the background quasar Q 0122-003 at an impact parameter of 163 kpc. The galaxy inclination angle (i=63 degree) and the azimuthal angle (Phi=73 degree) imply that the QSO sightline is passing through the projected minor-axis of the galaxy. The absorption system shows a multiphase, multicomponent structure with ultra-strong, wide velocity spread OVI (logN = 15.16$\backslash$pm0.04, V{\_}{\{}90{\}} = 419 km/s) and NV (logN = 14.69$\backslash$pm0.07, V{\_}{\{}90{\}} = 285 km/s) lines that are extremely rare in the literature. The highly ionized absorption components are well explained as arising in a low density (10{\^{}}{\{}-4.2{\}} cm{\^{}}{\{}-3{\}}), diffuse (10 kpc), cool (10{\^{}}4 K) photoionized gas with a super-solar metallicity ([X/H] > 0.3). From the observed narrowness of the Lyb profile, the non-detection of SIV absorption, and the presence of strong CIV absorption we rule out equilibrium/non-equilibrium collisional ionization models. The low-ionization photoionized gas with a density of 10{\^{}}{\{}-2.5{\}} cm{\^{}}{\{}-3{\}} and a metallicity of [X/H] > -1.4 is possibly tracing recycled halo gas. We estimate an outflow mass of {\~{}}2x10{\^{}}{\{}10{\}} Msun, a mass-flow rate of {\~{}}54 Msun/yr, a kinetic luminosity of {\~{}}9x10{\^{}}{\{}41{\}} erg/s, and a mass loading factor of {\~{}}8 for the outflowing high-ionization gas. These are consistent with the properties of down-the-barrel outflows from infrared-luminous starbursts as studied by Rupke et al. Such powerful, large-scale, metal-rich outflows are the primary means of sufficient mechanical and chemical feedback as invoked in theoretical models of galaxy formation and evolution.},
archiveprefix = {arXiv},
arxivid = {1506.01028},
author = {Muzahid, Sowgat and Kacprzak, Glenn G. and Churchil, Christopher W. and Charlton, Jane C. and Nielsen, Nikole M. and Mathes, Nigel L. and Trujillo-Gomez, Sebastian},
eprint = {1506.01028},
file = {:home/mel/1506.01028v1.pdf:pdf},
month = {jun},
pages = {15},
title = {{An Extreme Metallicity, Large-Scale Outflow from a Star-Forming Galaxy at z {\~{}} 0.4}},
url = {http://arxiv.org/abs/1506.01028},
year = {2015},
}
@article{Williams2015,
abstract = {We present a study of the evolution of the fraction of radio-loud active galactic nuclei (AGN) as a function of their host stellar mass. We make use of two samples of radio galaxies: one in the local universe, {\$}0.01 < z < 0.3{\$}, using a combined SDSS-NVSS sample and one at higher redshifts, {\$}0.5 < z < 2{\$}, constructed from the VLA-COSMOS{\_}DEEP Radio Survey at 1.4 GHz and a K{\$}{\_}s{\$}-selected catalogue of the COSMOS/UltraVISTA field. We observe an increase of more than an order of magnitude in the fraction of lower mass galaxies ({\$}M{\_}* < 10{\^{}}{\{}10.75{\}}{\$} M{\$}{\_}{\{}\backslashodot{\}}{\$}) which host Radio-Loud AGN with radio powers {\$}P{\_}{\{}1.4GHz{\}} > 10{\^{}}{\{}24{\}}{\$} W/Hz at z {\~{}} 1-2 while the radio-loud fraction for higher mass galaxies ({\$}M{\_}* > 10{\^{}}{\{}11.25{\}}{\$} M{\$}{\_}{\{}\backslashodot{\}}{\$}) remains the same. We argue that this increase is driven largely by the increase in cold or radiative mode accretion with increasing cold gas supply at earlier epochs. The increasing population of low mass Radio-Loud AGN can thus explain the upturn in the Radio Luminosity Function (RLF) at high redshift which is important for understanding the impact of AGN feedback in galaxy evolution.},
archiveprefix = {arXiv},
arxivid = {1503.08927},
author = {Williams, W. L. and R{\"{o}}ttgering, H. J. A.},
eprint = {1503.08927},
file = {:home/mel/Documents/Papers/1503.08927v1.pdf:pdf},
month = {mar},
pages = {9},
title = {{Radio-AGN Feedback: When the Little Ones were Monsters}},
url = {http://arxiv.org/abs/1503.08927},
year = {2015},
}
@article{Barden2008,
abstract = {We describe the creation of a set of artificially redshifted galaxies in the range 0.1<z<1.1 using a set of {\~{}}100 SDSS low redshift (v<7000 km/s) images as input. The intention is to generate a training set of realistic images of galaxies of diverse morphologies and a large range of redshifts for the GEMS and COSMOS galaxy evolution projects. This training set allows other studies to investigate and quantify the effects of cosmological redshift on the determination of galaxy morphologies, distortions and other galaxy properties that are potentially sensitive to resolution, surface brightness and bandpass issues. We use galaxy images from the SDSS in the u, g, r, i, z filter bands as input, and computed new galaxy images from these data, resembling the same galaxies as located at redshifts 0.1<z<1.1 and viewed with the Hubble Space Telescope Advanced Camera for Surveys (HST ACS). In this process we take into account angular size change, cosmological surface brightness dimming, and spectral change. The latter is achieved by interpolating a spectral energy distribution that is fit to the input images on a pixel-to-pixel basis. The output images are created for the specific HST ACS point spread function and the filters used for GEMS (F606W and F850LP) and COSMOS (F814W). All images are binned onto the desired pixel grids (0.03 for GEMS and 0.05 for COSMOS) and corrected to an appropriate point spread function. Noise is added corresponding to the data quality of the two projects and the images are added onto empty sky pieces of real data images. We make these datasets available from our website, as well as the code - FERENGI: Full and Efficient Redshifting of Ensembles of Nearby Galaxy Images - to produce datasets for other redshifts and/or instruments.},
archiveprefix = {arXiv},
arxivid = {0812.1022},
author = {Barden, M. and Jahnke, K. and H{\"{a}}u{\ss}ler, B.},
doi = {10.1086/524039},
eprint = {0812.1022},
file = {:home/mel/Documents/Papers/0812.1022v1 (1).pdf:pdf},
issn = {0067-0049},
journal = {The Astrophysical Journal Supplement Series},
month = {mar},
number = {1},
pages = {105--115},
title = {{FERENGI: Redshifting Galaxies from SDSS to GEMS, STAGES, and COSMOS}},
url = {http://arxiv.org/abs/0812.1022},
volume = {175},
year = {2008},
}
@article{Schawinski2007,
abstract = {A major amendment in recent models of hierarchical galaxy formation is the inclusion of so-called AGN feedback. The energy input from an active central massive black hole is invoked to suppress star formation in early-type galaxies at later epochs. A major problem is that this process is poorly understood, and compelling observational evidence for its mere existence is still missing. In search for signatures of AGN feedback, we have compiled a sample of 16,000 early-type galaxies in the redshift range 0.05<z<0.1 from the SDSS database. Key in our approach is the use of a purely morphological selection criterion through visual inspection which produces a sample that is not biased against recent star formation and nuclear activity. The objects with emission ({\~{}}20 per cent) are offset from the red sequence and form a well-defined pattern in the colour-mass diagram. Star forming early-types inhabit the blue cloud, while early-types with AGN are located considerably closer to and almost on the red sequence. Star formation-AGN composites are found right between these two extremes. We further derive galaxy star formation histories using a novel method that combines multiwavelength photometry from near-UV to near-IR and stellar absorption indices. We find that in those objects deviating from the red sequence star formation occurred several 100 Myr in the past involving 1-10 per cent of the total stellar mass. We identify an evolutionary sequence from star formation via nuclear activity to quiescence. This transition process lasts about 1 Gyr, and the peak AGN phase occurs roughly half a Gyr after the starburst. The most likely interpretation is that star formation is suppressed by nuclear activity in these objects before they settle on the red sequence.},
archiveprefix = {arXiv},
arxivid = {0709.3015},
author = {Schawinski, K. and Thomas, D. and Sarzi, M. and Maraston, C. and Kaviraj, S. and Joo, S.-J. and Yi, S. K. and Silk, J.},
doi = {10.1111/j.1365-2966.2007.12487.x},
eprint = {0709.3015},
file = {:home/mel/Documents/Papers/0709.3015v1.pdf:pdf},
issn = {0035-8711},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {dec},
number = {4},
pages = {1415--1431},
title = {{Observational evidence for AGN feedback in early-type galaxies}},
url = {http://arxiv.org/abs/0709.3015},
volume = {382},
year = {2007},
}
@article{Sheth2010,
abstract = {The Spitzer Survey of Stellar Structure in Galaxies S{\^{}}4G is an Exploration Science Legacy Program approved for the Spitzer post-cryogenic mission. It is a volume-, magnitude-, and size-limited (d < 40 Mpc, |b| > 30 degrees, m{\_}(Bcorr) < 15.5, D25>1') survey of 2,331 galaxies using IRAC at 3.6 and 4.5 microns. Each galaxy is observed for 240 s and mapped to > 1.5 x D25. The final mosaicked images have a typical 1 sigma rms noise level of 0.0072 and 0.0093 MJy / sr at 3.6 and 4.5 microns, respectively. Our azimuthally-averaged surface brightness profile typically traces isophotes at mu{\_}3.6 (AB) (1 sigma) {\~{}} 27 mag arcsec{\^{}}-2, equivalent to a stellar mass surface density of {\~{}} 1 Msun pc{\^{}}-2. S{\^{}}4G thus provides an unprecedented data set for the study of the distribution of mass and stellar structures in the local Universe. This paper introduces the survey, the data analysis pipeline and measurements for a first set of galaxies, observed in both the cryogenic and warm mission phase of Spitzer. For every galaxy we tabulate the galaxy diameter, position angle, axial ratio, inclination at mu{\_}3.6 (AB) = 25.5 and 26.5 mag arcsec{\^{}}-2 (equivalent to {\~{}} mu{\_}B (AB) =27.2 and 28.2 mag arcsec{\^{}}-2, respectively). These measurements will form the initial S{\^{}}4G catalog of galaxy properties. We also measure the total magnitude and the azimuthally-averaged radial profiles of ellipticity, position angle, surface brightness and color. Finally, we deconstruct each galaxy using GALFIT into its main constituent stellar components: the bulge/spheroid, disk, bar, and nuclear point source, where necessary. Together these data products will provide a comprehensive and definitive catalog of stellar structures, mass and properties of galaxies in the nearby Universe.},
archiveprefix = {arXiv},
arxivid = {1010.1592},
author = {Sheth, Kartik and Regan, Michael and Hinz, Joannah L. and de Paz, Armando Gil and Men{\'{e}}ndez-Delmestre, Kar{\'{\i}}n and Mu{\~{n}}oz-Mateos, Juan-Carlos and Seibert, Mark and Kim, Taehyun and Laurikainen, Eija and Salo, Heikki and Gadotti, Dimitri A. and Laine, Jarkko and Mizusawa, Trisha and Armus, Lee and Athanassoula, E. and Bosma, Albert and Buta, Ronald J. and Capak, Peter and Jarrett, Thomas H. and Elmegreen, Debra M. and Elmegreen, Bruce G. and Knapen, Johan H. and Koda, Jin and Helou, George and Ho, Luis C. and Madore, Barry F. and Masters, Karen L. and Mobasher, Bahram and Ogle, Patrick and Peng, Chien Y. and Schinnerer, Eva and Surace, Jason A. and Zaritsky, Dennis and Comer{\'{o}}n, S{\'{e}}bastien and de Swardt, Bonita and Meidt, Sharon E. and Kasliwal, Mansi and Aravena, Manuel},
doi = {10.1086/657638},
eprint = {1010.1592},
file = {:home/mel/Documents/Papers/1010.1592v2.pdf:pdf},
issn = {00046280},
journal = {Publications of the Astronomical Society of the Pacific},
month = {dec},
number = {898},
pages = {1397--1414},
title = {{The Spitzer Survey of Stellar Structure in Galaxies}},
url = {http://arxiv.org/abs/1010.1592},
volume = {122},
year = {2010},
}
@article{Leauthaud2012,
abstract = {Using data from the COSMOS survey, we perform the first joint analysis of galaxy-galaxy weak lensing, galaxy spatial clustering, and galaxy number densities. Carefully accounting for sample variance and for scatter between stellar and halo mass, we model all three observables simultaneously using a novel and self-consistent theoretical framework. Our results provide strong constraints on the shape and redshift evolution of the stellar-to-halo mass relation (SHMR) from z=0.2 to z=1. At low stellar mass, we find that halo mass scales as Mh M*{\^{}}0.46 and that this scaling does not evolve significantly with redshift to z=1. We show that the dark-to-stellar ratio, Mh/M*, varies from low to high masses, reaching a minimum of Mh/M*{\~{}}27 at M*=4.5x10{\^{}}10 Msun and Mh=1.2x10{\^{}}12 Msun. This minimum is important for models of galaxy formation because it marks the mass at which the accumulated stellar growth of the central galaxy has been the most efficient. We describe the SHMR at this minimum in terms of the pivot stellar mass, M*piv, the pivot halo mass, Mhpiv, and the pivot ratio, (Mh/M*)piv. Thanks to a homogeneous analysis of a single data set, we report the first detection of mass downsizing trends for both Mhpiv and M*piv. The pivot stellar mass decreases from M*piv=5.75+-0.13x10{\^{}}10 Msun at z=0.88 to M*piv=3.55+-0.17x10{\^{}}10 Msun at z=0.37. Intriguingly, however, the corresponding evolution of Mhpiv leaves the pivot ratio constant with redshift at (Mh/M*)piv{\~{}}27. We use simple arguments to show how this result raises the possibility that star formation quenching may ultimately depend on Mh/M* and not simply Mh, as is commonly assumed. We show that simple models with such a dependence naturally lead to downsizing in the sites of star formation. Finally, we discuss the implications of our results in the context of popular quenching models, including disk instabilities and AGN feedback.},
archiveprefix = {arXiv},
arxivid = {1104.0928},
author = {Leauthaud, Alexie and Tinker, Jeremy and Bundy, Kevin and Behroozi, Peter S. and Massey, Richard and Rhodes, Jason and George, Matthew R. and Kneib, Jean-Paul and Benson, Andrew and Wechsler, Risa H. and Busha, Michael T. and Capak, Peter and Cort{\^{e}}s, Marina and Ilbert, Olivier and Koekemoer, Anton M. and {Le F{\`{e}}vre}, Oliver and Lilly, Simon and McCracken, Henry J. and Salvato, Mara and Schrabback, Tim and Scoville, Nick and Smith, Tristan and Taylor, James E.},
doi = {10.1088/0004-637X/744/2/159},
eprint = {1104.0928},
file = {:home/mel/Documents/Papers/1104.0928v1.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {jan},
number = {2},
pages = {159},
title = {{NEW CONSTRAINTS ON THE EVOLUTION OF THE STELLAR-TO-DARK MATTER CONNECTION: A COMBINED ANALYSIS OF GALAXY-GALAXY LENSING, CLUSTERING, AND STELLAR MASS FUNCTIONS FROM z = 0.2 to z = 1}},
url = {http://arxiv.org/abs/1104.0928},
volume = {744},
year = {2012},
}
@article{Bundy2010,
abstract = {The increasing abundance of passive red-sequence galaxies since z=1-2 is mirrored by a coincident rise in the number of galaxies with spheroidal morphologies. In this paper, however, we show that in detail the correspondence between galaxy morphology and color is not perfect, providing insight into the physical origin of this evolution. Using the COSMOS survey, we study a significant population of red sequence galaxies with disk-like morphologies. These passive disks typically have Sa-Sb morphological types with large bulges, but they are not confined to dense environments. They represent nearly one-half of all red-sequence galaxies and dominate at lower masses (log Mstar < 10) where they are increasingly disk-dominated. As a function of time, the abundance of passive disks with log Mstar < 11 increases, but not as fast as red-sequence spheroidals in the same mass range. At higher mass, the passive disk population has declined since z{\~{}}1, likely because they transform into spheroidals. We estimate that as much as 60{\%} of galaxies transitioning onto the red sequence evolve through a passive disk phase. The origin of passive disks therefore has broad implications for understanding how star formation shuts down. Because passive disks tend to be more bulge-dominated than their star-forming counterparts, a simple fading of blue disks does not fully explain their origin. We explore several more sophisticated explanations, including environmental effects, internal stabilization, and disk regrowth during gas-rich mergers. While previous work has sought to explain color and morphological transformations with a single process, these observations open the way to new insight by highlighting the fact that galaxy evolution may actually proceed through several separate stages.},
archiveprefix = {arXiv},
arxivid = {0912.1077},
author = {Bundy, Kevin and Scarlata, Claudia and Carollo, C. M. and Ellis, Richard S. and Drory, Niv and Hopkins, Philip and Salvato, Mara and Leauthaud, Alexie and Koekemoer, Anton M. and Murray, Norman and Ilbert, Olivier and Oesch, Pascal and Ma, Chung-Pei and Capak, Peter and Pozzetti, Lucia and Scoville, Nick},
doi = {10.1088/0004-637X/719/2/1969},
eprint = {0912.1077},
file = {:home/mel/Documents/Papers/0912.1077v2.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {aug},
number = {2},
pages = {1969--1983},
title = {{THE RISE AND FALL OF PASSIVE DISK GALAXIES: MORPHOLOGICAL EVOLUTION ALONG THE RED SEQUENCE REVEALED BY COSMOS}},
url = {http://arxiv.org/abs/0912.1077},
volume = {719},
year = {2010},
}
@article{Eskridge2002,
abstract = {We announce the initial release of data from the Ohio State University Bright Spiral Galaxy Survey, a BVRJHK imaging survey of a well-defined sample of 205 bright, nearby spiral galaxies. We present H-band morphological classification on the Hubble sequence for the OSU Survey sample. We compare the H-band classification to B-band classification from our own images and from standard galaxy catalogs. Our B-band classifications match well with those of the standard catalogs. On average, galaxies with optical classifications from Sa through Scd appear about one T-type earlier in the H-band than in the B-band, but with large scatter. This result does not support recent claims made in the literature that the optical and near-IR morphologies of spiral galaxies are uncorrelated. We present detailed descriptions of the H-band morphologies of our entire sample, as well as B- and H-band images for a set of 17 galaxies chosen as type examples, and BRH color-composite images of six galaxies chosen to demonstrate the range in morphological variation as a function of wavelength. Data from the survey are accessible at http://www.astronomy.ohio-state.edu/{\~{}}survey/},
archiveprefix = {arXiv},
arxivid = {astro-ph/0206320},
author = {Eskridge, Paul B. and Frogel, Jay A. and Pogge, Richard W. and Quillen, Alice C. and Berlind, Andreas A. and Davies, Roger L. and DePoy, D. L. and Gilbert, Karoline M. and Houdashelt, Mark L. and Kuchinski, Leslie E. and Ramirez, Solange V. and Sellgren, K. and Stutz, Amelia and Terndrup, Donald M. and Tiede, Glenn P.},
doi = {10.1086/342340},
eprint = {0206320},
file = {:home/mel/Documents/Papers/0067-0049{\_}143{\_}1{\_}73.pdf:pdf},
issn = {0067-0049},
journal = {The Astrophysical Journal Supplement Series},
month = {nov},
number = {1},
pages = {73--111},
primaryclass = {astro-ph},
title = {{Near‐Infrared and Optical Morphology of Spiral Galaxies}},
url = {http://arxiv.org/abs/astro-ph/0206320},
volume = {143},
year = {2002},
}
@article{Schawinski2014,
abstract = {We use SDSS+$\backslash$textit{\{}GALEX{\}}+Galaxy Zoo data to study the quenching of star formation in low-redshift galaxies. We show that the green valley between the blue cloud of star-forming galaxies and the red sequence of quiescent galaxies in the colour-mass diagram is not a single transitional state through which most blue galaxies evolve into red galaxies. Rather, an analysis that takes morphology into account makes clear that only a small population of blue early-type galaxies move rapidly across the green valley after the morphologies are transformed from disk to spheroid and star formation is quenched rapidly. In contrast, the majority of blue star-forming galaxies have significant disks, and they retain their late-type morphologies as their star formation rates decline very slowly. We summarize a range of observations that lead to these conclusions, including UV-optical colours and halo masses, which both show a striking dependence on morphological type. We interpret these results in terms of the evolution of cosmic gas supply and gas reservoirs. We conclude that late-type galaxies are consistent with a scenario where the cosmic supply of gas is shut off, perhaps at a critical halo mass, followed by a slow exhaustion of the remaining gas over several Gyr, driven by secular and/or environmental processes. In contrast, early-type galaxies require a scenario where the gas supply and gas reservoir are destroyed virtually instantaneously, with rapid quenching accompanied by a morphological transformation from disk to spheroid. This gas reservoir destruction could be the consequence of a major merger, which in most cases transforms galaxies from disk to elliptical morphology, and mergers could play a role in inducing black hole accretion and possibly AGN feedback.},
archiveprefix = {arXiv},
arxivid = {1402.4814},
author = {Schawinski, Kevin and Urry, C. Megan and Simmons, Brooke D. and Fortson, Lucy and Kaviraj, Sugata and Keel, William C. and Lintott, Chris J. and Masters, Karen L. and Nichol, Robert C. and Sarzi, Marc and Ramin and Skibba and Treister, Ezequiel and Willett, Kyle W. and Wong, O. Ivy and Yi, Sukyoung K.},
eprint = {1402.4814},
file = {:home/mel/Documents/Papers/1402.4814v1.pdf:pdf},
month = {feb},
pages = {21},
title = {{The Green Valley is a Red Herring: Galaxy Zoo reveals two evolutionary pathways towards quenching of star formation in early- and late-type galaxies}},
url = {http://arxiv.org/abs/1402.4814},
year = {2014},
}
@article{DeVaucouleurs1963,
author = {de Vaucouleurs, G.},
doi = {10.1086/190084},
file = {:home/mel/Documents/Papers/1963ApJS....8...31D.pdf:pdf},
issn = {0067-0049},
journal = {The Astrophysical Journal Supplement Series},
language = {en},
month = {apr},
pages = {31},
title = {{Revised Classification of 1500 Bright Galaxies.}},
url = {http://adslabs.org/adsabs/abs/1963ApJS....8...31D/},
volume = {8},
year = {1963},
}
@article{Warren2006,
archiveprefix = {arXiv},
arxivid = {astro-ph/0610191},
author = {Warren, S. J. and Hambly, N. C. and Dye, S. and Almaini, O. and Cross, N. J. G. and Edge, A. C. and Foucaud, S. and Hewett, P. C. and Hodgkin, S. T. and Irwin, M. J. and Jameson, R. F. and Lawrence, A. and Lucas, P. W. and Adamson, A. J. and Bandyopadhyay, R. M. and Bryant, J. and Collins, R. S. and Davis, C. J. and Dunlop, J. S. and Emerson, J. P. and Evans, D. W. and Gonzales-Solares, E. A. and Hirst, P. and Jarvis, M. J. and Kendall, T. R. and Kerr, T. H. and Leggett, S. K. and Lewis, J. R. and Mann, R. G. and McLure, R. J. and McMahon, R. G. and Mortlock, D. J. and Rawlings, M. G. and Read, M. A. and Riello, M. and Simpson, C. and Smith, D. J. B. and Sutorius, E. T. W. and Targett, T. A. and Varricatt, W. P.},
eprint = {0610191},
file = {:home/mel/Documents/Papers/0610191v2.pdf:pdf},
month = {oct},
primaryclass = {astro-ph},
title = {{The UKIRT Infrared Deep Sky Survey First Data Release}},
url = {http://arxiv.org/abs/astro-ph/0610191},
year = {2006},
}
@article{Khiali2015,
abstract = {The detection of astrophysical very high energy (VHE) neutrinos in the range of TeV-PeV energies by the IceCube observatory has opened a new season in high energy astrophysics. Energies {\~{}}PeV imply that the neutrinos are originated from sources where cosmic rays (CRs) can be accelerated up to {\~{}} 10{\^{}}{\{}17{\}}eV. Recently, we have shown that the observed TeV gamma-rays from radio-galaxies may have a hadronic origin in their nuclear region and in such a case this could lead to neutrino production. In this paper we show that relativistic protons accelerated by magnetic reconnection in the core region of these sources may produce VHE neutrinos via the decay of charged pions produced by photo-meson process. We have also calculated the diffuse flux of VHE neutrinos and found that it can be associated to the IceCube data.},
archiveprefix = {arXiv},
arxivid = {1506.01063},
author = {Khiali, Behrouz and Pino, Elisabete M. de Gouveia Dal},
eprint = {1506.01063},
file = {:home/mel/Documents/Papers/1506.01063v1.pdf:pdf},
month = {jun},
pages = {9},
title = {{Very high energy neutrino emission from the core of low luminosity AGNs triggered by magnetic reconnection acceleration}},
url = {http://arxiv.org/abs/1506.01063},
year = {2015},
}
@article{Yoshino2014,
archiveprefix = {arXiv},
arxivid = {1410.8262},
author = {Yoshino, Akira and Yamauchi, Chisato},
eprint = {1410.8262},
file = {:home/mel/Documents/Papers/1410.8262v1.pdf:pdf},
month = {oct},
title = {{Box/Peanut and Bar structures in edge-on and face-on SDSS nearby galaxies I. Catalogue}},
url = {http://arxiv.org/abs/1410.8262},
year = {2014},
}
@article{PlanckCollaboration2015,
abstract = {We present results based on full-mission Planck observations of temperature and polarization anisotropies of the CMB. These data are consistent with the six-parameter inflationary LCDM cosmology. From the Planck temperature and lensing data, for this cosmology we find a Hubble constant, H0= (67.8 +/- 0.9) km/s/Mpc, a matter density parameter Omega{\_}m = 0.308 +/- 0.012 and a scalar spectral index with n{\_}s = 0.968 +/- 0.006. (We quote 68{\%} errors on measured parameters and 95{\%} limits on other parameters.) Combined with Planck temperature and lensing data, Planck LFI polarization measurements lead to a reionization optical depth of tau = 0.066 +/- 0.016. Combining Planck with other astrophysical data we find N{\_} eff = 3.15 +/- 0.23 for the effective number of relativistic degrees of freedom and the sum of neutrino masses is constrained to < 0.23 eV. Spatial curvature is found to be |Omega{\_}K| < 0.005. For LCDM we find a limit on the tensor-to-scalar ratio of r <0.11 consistent with the B-mode constraints from an analysis of BICEP2, Keck Array, and Planck (BKP) data. Adding the BKP data leads to a tighter constraint of r < 0.09. We find no evidence for isocurvature perturbations or cosmic defects. The equation of state of dark energy is constrained to w = -1.006 +/- 0.045. Standard big bang nucleosynthesis predictions for the Planck LCDM cosmology are in excellent agreement with observations. We investigate annihilating dark matter and deviations from standard recombination, finding no evidence for new physics. The Planck results for base LCDM are in agreement with BAO data and with the JLA SNe sample. However the amplitude of the fluctuations is found to be higher than inferred from rich cluster counts and weak gravitational lensing. Apart from these tensions, the base LCDM cosmology provides an excellent description of the Planck CMB observations and many other astrophysical data sets.},
archiveprefix = {arXiv},
arxivid = {1502.01589},
author = {{Planck Collaboration} and Ade, P. A. R. and Aghanim, N. and Arnaud, M. and Ashdown, M. and Aumont, J. and Baccigalupi, C. and Banday, A. J. and Barreiro, R. B. and Bartlett, J. G. and Bartolo, N. and Battaner, E. and Battye, R. and Benabed, K. and Benoit, A. and Benoit-Levy, A. and Bernard, J. -P. and Bersanelli, M. and Bielewicz, P. and Bonaldi, A. and Bonavera, L. and Bond, J. R. and Borrill, J. and Bouchet, F. R. and Boulanger, F. and Bucher, M. and Burigana, C. and Butler, R. C. and Calabrese, E. and Cardoso, J. -F. and Catalano, A. and Challinor, A. and Chamballu, A. and Chary, R. -R. and Chiang, H. C. and Chluba, J. and Christensen, P. R. and Church, S. and Clements, D. L. and Colombi, S. and Colombo, L. P. L. and Combet, C. and Coulais, A. and Crill, B. P. and Curto, A. and Cuttaia, F. and Danese, L. and Davies, R. D. and Davis, R. J. and de Bernardis, P. and de Rosa, A. and de Zotti, G. and Delabrouille, J. and Desert, F. -X. and {Di Valentino}, E. and Dickinson, C. and Diego, J. M. and Dolag, K. and Dole, H. and Donzelli, S. and Dore, O. and Douspis, M. and Ducout, A. and Dunkley, J. and Dupac, X. and Efstathiou, G. and Elsner, F. and Ensslin, T. A. and Eriksen, H. K. and Farhang, M. and Fergusson, J. and Finelli, F. and Forni, O. and Frailis, M. and Fraisse, A. A. and Franceschi, E. and Frejsel, A. and Galeotta, S. and Galli, S. and Ganga, K. and Gauthier, C. and Gerbino, M. and Ghosh, T. and Giard, M. and Giraud-Heraud, Y. and Giusarma, E. and Gjerlow, E. and Gonzalez-Nuevo, J. and Gorski, K. M. and Gratton, S. and Gregorio, A. and Gruppuso, A. and Gudmundsson, J. E. and Hamann, J. and Hansen, F. K. and Hanson, D. and Harrison, D. L. and Helou, G. and Henrot-Versille, S. and Hernandez-Monteagudo, C. and Herranz, D. and Hildebrandt, S. R. and Hivon, E. and Hobson, M. and Holmes, W. A. and Hornstrup, A. and Hovest, W. and Huang, Z. and Huffenberger, K. M. and Hurier, G. and Jaffe, A. H. and Jaffe, T. R. and Jones, W. C. and Juvela, M. and Keihanen, E. and Keskitalo, R. and Kisner, T. S. and Kneissl, R. and Knoche, J. and Knox, L. and Kunz, M. and Kurki-Suonio, H. and Lagache, G. and Lahteenmaki, A. and Lamarre, J. -M. and Lasenby, A. and Lattanzi, M. and Lawrence, C. R. and Leahy, J. P. and Leonardi, R. and Lesgourgues, J. and Levrier, F. and Lewis, A. and Liguori, M. and Lilje, P. B. and Linden-Vornle, M. and Lopez-Caniego, M. and Lubin, P. M. and Macias-Perez, J. F. and Maggio, G. and Maino, D. and Mandolesi, N. and Mangilli, A. and Marchini, A. and Martin, P. G. and Martinelli, M. and Martinez-Gonzalez, E. and Masi, S. and Matarrese, S. and Mazzotta, P. and McGehee, P. and Meinhold, P. R. and Melchiorri, A. and Melin, J. -B. and Mendes, L. and Mennella, A. and Migliaccio, M. and Millea, M. and Mitra, S. and Miville-Deschenes, M. -A. and Moneti, A. and Montier, L. and Morgante, G. and Mortlock, D. and Moss, A. and Munshi, D. and Murphy, J. A. and Naselsky, P. and Nati, F. and Natoli, P. and Netterfield, C. B. and Norgaard-Nielsen, H. U. and Noviello, F. and Novikov, D. and Novikov, I. and Oxborrow, C. A. and Paci, F. and Pagano, L. and Pajot, F. and Paladini, R. and Paoletti, D. and Partridge, B. and Pasian, F. and Patanchon, G. and Pearson, T. J. and Perdereau, O. and Perotto, L. and Perrotta, F. and Pettorino, V. and Piacentini, F. and Piat, M. and Pierpaoli, E. and Pietrobon, D. and Plaszczynski, S. and Pointecouteau, E. and Polenta, G. and Popa, L. and Pratt, G. W. and Prezeau, G. and Prunet, S. and Puget, J. -L. and Rachen, J. P. and Reach, W. T. and Rebolo, R. and Reinecke, M. and Remazeilles, M. and Renault, C. and Renzi, A. and Ristorcelli, I. and Rocha, G. and Rosset, C. and Rossetti, M. and Roudier, G. and D'Orfeuil, B. Rouille and Rowan-Robinson, M. and Rubino-Martin, J. A. and Rusholme, B. and Said, N. and Salvatelli, V. and Salvati, L. and Sandri, M. and Santos, D. and Savelainen, M. and Savini, G. and Scott, D. and Seiffert, M. D. and Serra, P. and Shellard, E. P. S. and Spencer, L. D. and Spinelli, M. and Stolyarov, V. and Stompor, R. and Sudiwala, R. and Sunyaev, R. and Sutton, D. and Suur-Uski, A. -S. and Sygnet, J. -F. and Tauber, J. A. and Terenzi, L. and Toffolatti, L. and Tomasi, M. and Tristram, M. and Trombetti, T. and Tucci, M. and Tuovinen, J. and Turler, M. and Umana, G. and Valenziano, L. and Valiviita, J. and {Van Tent}, B. and Vielva, P. and Villa, F. and Wade, L. A. and Wandelt, B. D. and Wehus, I. K. and White, M. and White, S. D. M. and Wilkinson, A. and Yvon, D. and Zacchei, A. and Zonca, A.},
eprint = {1502.01589},
file = {:home/mel/Documents/Papers/1502.01589v2.pdf:pdf},
month = {feb},
title = {{Planck 2015 results. XIII. Cosmological parameters}},
url = {http://arxiv.org/abs/1502.01589},
year = {2015},
}
@article{Antonini2015,
abstract = {Studying how nuclear star clusters (NSCs) form and how they are related to the growth of the central massive black holes (MBHs) and their host galaxies is fundamental for our understanding of the evolution of galaxies and the processes that have shaped their central structures. We present the results of a semi-analytical galaxy formation model that follows the evolution of dark matter halos along merger trees, as well as that of the baryonic components. This model allows us to study the evolution of NSCs in a cosmological context, by taking into account the growth of NSCs due to both dynamical friction-driven migration of stellar clusters and star formation triggered by infalling gas, while also accounting for dynamical heating from (binary) MBHs. We find that in-situ star formation contributes a significant fraction (up to {\~{}}40{\%}) of the total mass of NSCs in our model. Both NSC growth through in-situ star formation and through star cluster migration are found to generate NSC -- host galaxy scaling correlations that are shallower than the same correlations for MBHs. We explore the role of galaxy mergers on the evolution of NSCs, and show that observational data on NSC -- host galaxy scaling relations provide evidence of partial erosion of NSCs by MBH binaries in luminous galaxies. We show that this observational feature is reproduced by our models, and we make predictions about the NSC and MBH occupation fraction in galaxies. We conclude by discussing several implications for theories of NSC formation.},
archiveprefix = {arXiv},
arxivid = {1506.02050},
author = {Antonini, Fabio and Barausse, Enrico and Silk, Joseph},
eprint = {1506.02050},
file = {:home/mel/Documents/Papers/1506.02050v1.pdf:pdf},
month = {jun},
title = {{Co-evolution of nuclear star clusters, massive black holes and their host galaxies}},
url = {http://arxiv.org/abs/1506.02050},
year = {2015},
}
@article{Belfiore2014a,
abstract = {MaNGA (Mapping Nearby Galaxies at Apache Point Observatory) is a SDSS-IV survey that will obtain spatially resolved spectroscopy from 3600 $\backslash$AA$\backslash$ to 10300 $\backslash$AA$\backslash$ for a representative sample of over 10000 nearby galaxies. In this paper we present the analysis of nebular emission line properties using observations of 14 galaxies obtained with P-MaNGA, a prototype of the MaNGA instrument. By using spatially resolved diagnostic diagrams we find extended star formation in galaxies that are centrally dominated by Seyfert/LINER-like emission, illustrating that galaxy characterisations based on single fibre spectra are necessarily incomplete. We observe extended (up to {\$}\backslashrm 1 R{\_}{\{}e{\}}{\$}) LINER-like emission in the central regions of three galaxies. We make use of the {\$}\backslashrm EW(H \backslashalpha){\$} to argue that the observed emission is consistent with ionisation from hot evolved stars. Using stellar population indices we conclude that galactic regions which are ionised by a Seyfert/LINER-like radiation field are also devoid of recent star formation, presenting older and/or more metal rich stellar populations. We find that low mass galaxies show a positive correlation between metallicity and star formation rate (SFR) surface density, as in less massive systems both metallicity and SFR are highest in galaxy centres. In more massive galaxies we observe a weakening of this correlation, because the central regions are devoid of recent star formation. We further study the relation between N/O vs O/H on resolved scales. We find that regions within individual galaxies, at given N/O, are spread towards lower metallicities, deviating from the sequence defined by galactic central regions, as traced by Sloan 3'' fibre spectra. We suggest that the observed dispersion can be interpreted as tracing gas flows in galaxies: infalls of pristine gas and/or the effect of a galactic fountain.},
archiveprefix = {arXiv},
arxivid = {1410.7781},
author = {Belfiore, F. and Maiolino, R. and Bundy, K. and Thomas, D. and Maraston, C. and Wilkinson, D. and S{\'{a}}nchez, S. F. and Bershady, M. and Blanc, G. A. and Bothwell, M. and Cales, S. L. and Coccato, L. and Drory, N. and Emsellem, E. and Fu, H. and Gelfand, J. and Law, D. and Masters, K. and Parejko, J. and Tremonti, C. and Wake, D. and Weijmans, A. and Yan, R. and Xiao, T. and Zhang, K. and Zheng, T. and Bizyaev, D. and Kinemuchi, K. and Oravetz, D. and Simmons, A.},
eprint = {1410.7781},
file = {:home/mel/Documents/Papers/1410.7781v1.pdf:pdf},
month = {oct},
pages = {37},
title = {{P-MaNGA Galaxies: Emission Lines Properties - Gas Ionisation and Chemical Abundances from Prototype Observations}},
url = {http://arxiv.org/abs/1410.7781},
year = {2014},
}
@article{Bamford2009,
abstract = {We analyse the relationships between galaxy morphology, colour, environment and stellar mass using data for over 100,000 objects from Galaxy Zoo, the largest sample of visually classified morphologies yet compiled. We conclusively show that colour and morphology fractions are very different functions of environment. Both are sensitive to stellar mass; however, at fixed stellar mass, while colour is also highly sensitive to environment, morphology displays much weaker environmental trends. Only a small part of both relations can be attributed to variation in the stellar mass function with environment. Galaxies with high stellar masses are mostly red, in all environments and irrespective of their morphology. Low stellar-mass galaxies are mostly blue in low-density environments, but mostly red in high-density environments, again irrespective of their morphology. The colour-density relation is primarily driven by variations in colour fractions at fixed morphology, in particular the fraction of spiral galaxies that have red colours, and especially at low stellar masses. We demonstrate that our red spirals primarily include galaxies with true spiral morphology. We clearly show there is an environmental dependence for colour beyond that for morphology. Before using the Galaxy Zoo morphologies to produce the above results, we first quantify a luminosity-, size- and redshift-dependent classification bias that affects this dataset, and probably most other studies of galaxy population morphology. A correction for this bias is derived and applied to produce a sample of galaxies with reliable morphological type likelihoods, on which we base our analysis.},
archiveprefix = {arXiv},
arxivid = {0805.2612},
author = {Bamford, Steven P. and Nichol, Robert C. and Baldry, Ivan K. and Land, Kate and Lintott, Chris J. and Schawinski, Kevin and Slosar, An{\v{z}}e and Szalay, Alexander S. and Thomas, Daniel and Torki, Mehri and Andreescu, Dan and Edmondson, Edward M. and Miller, Christopher J. and Murray, Phil and Raddick, M. Jordan and Vandenberg, Jan},
doi = {10.1111/j.1365-2966.2008.14252.x},
eprint = {0805.2612},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {mar},
number = {4},
pages = {1324--1352},
title = {{Galaxy Zoo: the dependence of morphology and colour on environment}},
url = {http://arxiv.org/abs/0805.2612},
volume = {393},
year = {2009},
}
@article{Eser2014,
archiveprefix = {arXiv},
arxivid = {1410.6435},
author = {Eser, E. Kilerci and Goto, T. and Doi, Y.},
eprint = {1410.6435},
file = {:home/mel/Documents/Papers/1410.6479v1.pdf:pdf},
month = {oct},
title = {{Ultraluminous Infrared Galaxies in the AKARI All Sky Survey}},
url = {http://arxiv.org/abs/1410.6435},
year = {2014},
}
@article{Fabian2015,
abstract = {The focussing optics of NuSTAR have enabled high signal-to-noise spectra to be obtained from many X-ray bright Active Galactic Nuclei (AGN) and Galactic Black Hole Binaries (BHB). Spectral modelling then allows robust characterization of the spectral index and upper energy cutoff of the coronal power-law continuum, after accounting for reflection and absorption effects. Spectral-timing studies, such as reverberation and broad iron line fitting, of these sources yield coronal sizes, often showing them to be small and in the range of 3 to 10 gravitational radii in size. Our results indicate that coronae are hot and radiatively compact, lying close to the boundary of the region in the compactness - temperature diagram which is forbidden due to runaway pair production. The coincidence suggests that pair production and annihilation are essential ingredients in the coronae of AGN and BHB and that they control the shape of the observed spectra.},
archiveprefix = {arXiv},
arxivid = {1505.07603},
author = {Fabian, A. C. and Lohfink, A. and Kara, E. and Parker, M. L. and Vasudevan, R. and Reynolds, C. S.},
eprint = {1505.07603},
file = {:home/mel/Documents/Papers/1505.07603v1.pdf:pdf},
month = {may},
pages = {11},
title = {{Properties of AGN coronae in the NuSTAR era}},
url = {http://arxiv.org/abs/1505.07603},
year = {2015},
}
@article{Ho1997,
archiveprefix = {arXiv},
arxivid = {astro-ph/9704100},
author = {Ho, Luis C. and Filippenko, Alexei V. and Sargent, Wallace L. W.},
eprint = {9704100},
file = {:home/mel/Documents/Papers/9704100v1.pdf:pdf},
month = {apr},
primaryclass = {astro-ph},
title = {{The Influence of Bars on Nuclear Activity}},
url = {http://arxiv.org/abs/astro-ph/9704100},
year = {1997},
}
@article{Martinez-Delgado2014,
archiveprefix = {arXiv},
arxivid = {1410.6368},
author = {Martinez-Delgado, David and D'Onghia, Elena and Chonis, Taylor S. and Beaton, Rachael L. and Teuwen, Karel and GaBany, R. Jay and Grebel, Eva K. and Morales, Gustavo},
eprint = {1410.6368},
file = {:home/mel/Documents/Papers/Whale{\_}Galaxy1410.6368.pdf:pdf},
month = {oct},
title = {{Discovery of a stellar tidal stream around the Whale galaxy, NGC 4631}},
url = {http://arxiv.org/abs/1410.6368},
year = {2014},
}
@article{Bouwens2015,
abstract = {The deep, wide-area (900 arcmin**2) near-IR/WFC3/IR + Spitzer/IRAC observations over the CANDELS program represents a significant resource for constraining the bright end of the z{\~{}}9 and z{\~{}}10 luminosity functions (LFs) in the UV. We recently reported the discovery of 6 luminous z{\~{}}9-10 candidates over the GOODS-North+South fields, but extending this search to the full CANDELS program was limited due to the lack of HST-depth 1.05-micron observations in the other 3 CANDELS fields. Here we attempt to significantly realize the potential of CANDELS for z=9-10 science by combining a search over all 5 fields with results from a new HST program (B9-CANDELS) designed to follow up the highest-probability z{\~{}}9-10 galaxy candidates with observations at 1.05 microns. The targeted z{\~{}}9-10 candidates are preselected by taking advantage of the full HST, Spitzer/IRAC S-CANDELS observations, and the deepest-available ground-based optical+near-IR observations. With our follow-up program now 91{\%} complete, we identify 4 new high-probability z{\~{}}9-10 galaxies. This brings our total sample of bright z{\~{}}9-10 galaxies to 14, including several other new sources from the CANDELS GOODS + ERS fields.Through extensive simulations, we replicate the selection process for our sample (both the preselection and follow-up) and obtain an accurate estimate of the volume density of bright galaxies (M{\_}{\{}UV,AB{\}}<-20) at both z{\~{}}9 and z{\~{}}10. The volume density of bright z{\~{}}9 and z{\~{}}10 galaxies that we find is 4.5(-1.3)(+2.5)x and 8(-3)(+7)x lower than found at z{\~{}}8. When compared with the best-fit evolution in the UV luminosities densities from z{\~{}}8 to z{\~{}}4 (>0.4L*), the luminosity densities we find at z{\~{}}9 and z{\~{}}10 are {\~{}}2x lower than the extrapolated trends. We would expect significant additional gains in these results from the on-going 500-orbit BoRG[z910] program and by obtaining additional follow-up observations over the CANDELS-WIDE fields.},
archiveprefix = {arXiv},
arxivid = {1506.01035},
author = {Bouwens, R. J. and Oesch, P. A. and Labbe, I. and Illingworth, G. D. and Fazio, G. and Coe, D. and Holwerda, B. and Smit, R. and Stefanon, M. and van Dokkum, P. G. and Trenti, M. and Ashby, M. and Huang, J. and Spitler, L. and Straatman, C. and Bradley, L. and Magee, D.},
eprint = {1506.01035},
file = {:home/mel/Documents/Papers/1506.01035v1.pdf:pdf},
month = {jun},
pages = {22},
title = {{Most Luminous z=9-10 Galaxies: A First Determination of the Bright End of the z{\~{}}9 and z{\~{}}10 UV Luminosity Functions using all five CANDELS Fields}},
url = {http://arxiv.org/abs/1506.01035},
year = {2015},
}
@article{DOnghia2015,
abstract = {A model based on disk-stability criteria to determine the number of spiral arms of a general disk galaxy with an exponential disk, a bulge and a dark halo described by a Hernquist model is presented. The multifold rotational symmetry of the spiral structure can be evaluated analytically once the structural properties of a galaxy, such as the circular speed curve, and the disk surface brightness, are known. By changing the disk mass, these models are aimed at varying the critical length scale parameter of the disk and lead to a different spiral morphology in agreement with prior models. Previous studies based on the swing amplification and disk stability have been applied to constrain the mass-to-light ratio in disk galaxies. This formalism provides an analytic expression to estimate the number of arms expected by swing amplification making its application straight-forward to large surveys. It can be applied to predict the number of arms in the Milky Way as a function of radius and to constrain the mass-to-light ratio in disk galaxies for which photometric and kinematic measurements are available, like in the DiskMass survey. Hence, the halo contribution to the total mass in the inner parts of disk galaxies can be inferred in light of the ongoing and forthcoming surveys.},
archiveprefix = {arXiv},
arxivid = {1507.00724},
author = {D'Onghia, Elena},
eprint = {1507.00724},
file = {:home/mel/Documents/Papers/1507.00724v1.pdf:pdf},
month = {jul},
pages = {4},
title = {{Disk-stability constraints on the number of arms in spiral galaxies}},
url = {http://arxiv.org/abs/1507.00724},
year = {2015},
}
@article{Kuminski2016,
abstract = {We applied computer analysis to classify the broad morphological type of {\~{}}3,000,000 SDSS galaxies. The catalog provides for each galaxy the DR8 object ID, right ascension, declination, and the certainty of the automatic classification to spiral or elliptical. The certainty of the classification allows controlling the accuracy of a subset of galaxies by sacrificing some of the least certain classifications. The accuracy of the catalog was tested using galaxies that were classified by the manually annotated Galaxy Zoo catalog. The results show that the catalog contains {\~{}}900,000 spiral galaxies and {\~{}}600,000 elliptical galaxies with classification certainty that has a statistical agreement rate of {\~{}}98{\%} with Galaxy Zoo debiased 'superclean' dataset. That also demonstrates the ability of computers to turn large datasets of galaxy images into structured catalogs of galaxy morphology. The catalog can be downloaded at http://vfacstaff.ltu.edu/lshamir/data/morph{\_}catalog. The image analysis software that was used to create the catalog is also publicly available.},
archiveprefix = {arXiv},
arxivid = {1602.06854},
author = {Kuminski, Evan and Shamir, Lior},
eprint = {1602.06854},
file = {:home/mel/Documents/Papers/1602.06854v1.pdf:pdf},
month = {feb},
title = {{Computer-generated visual morphology catalog of {\~{}}3,000,000 SDSS galaxies}},
url = {http://arxiv.org/abs/1602.06854},
year = {2016},
}
@article{Coupon2009,
annote = {AEGIS photozs},
author = {Coupon, J. and Ilbert, O. and Kilbinger, M. and McCracken, H. J. and Mellier, Y. and Arnouts, S. and Bertin, E. and Hudelot, P. and Schultheis, M. and {Le F{\`{e}}vre}, O. and {Le Brun}, V. and Guzzo, L. and Bardelli, S. and Zucca, E. and Bolzonella, M. and Garilli, B. and Zamorani, G. and Zanichelli, A. and Tresse, L. and Aussel, H.},
doi = {10.1051/0004-6361/200811413},
file = {:home/mel/Documents/Papers/aa11413-08.pdf:pdf},
isbn = {doi:10.1051/0004-6361/200811413},
issn = {0004-6361},
journal = {Astronomy and Astrophysics},
language = {en},
month = {jun},
number = {3},
pages = {981--998},
title = {{Photometric redshifts for the CFHTLS T0004 deep and wide fields}},
url = {http://adslabs.org/adsabs/abs/2009A{\%}26A...500..981C/},
volume = {500},
year = {2009},
}
@article{Hubble1929a,
author = {Hubble, E.},
doi = {10.1073/pnas.15.3.168},
file = {:home/mel/Documents/Papers/PNAS-1929-Hubble-168-73.pdf:pdf},
issn = {0027-8424},
journal = {Proceedings of the National Academy of Sciences},
month = {mar},
number = {3},
pages = {168--173},
title = {{A relation between distance and radial velocity among extra-galactic nebulae}},
url = {http://www.pnas.org/cgi/content/long/15/3/168},
volume = {15},
year = {1929},
}
@article{Sellwood2016,
abstract = {We show that the exponential growth rate of a bar in a stellar disk is substantially greater when the disk is embedded in a live halo than in a rigid one having the same mass distribution. We also find that the vigor of the instability in disk-halo systems varies with the shape of the halo velocity ellipsoid. Disks in rigid halos that are massive enough to be stable by the usual criteria, quickly form bars in isotropic halos and much greater halo mass is needed to avoid a strong bar; thus stability criteria derived for disks in rigid halos do not apply when the halo is responsive. The study presented here is of an idealized family of models with near uniform central rotation and that lack an extended halo; we present more realistic models with extended halos in a companion paper. The puzzle presented by the absence of strong bars in some galaxies having gently rising inner rotation curves is compounded by the results presented here.},
archiveprefix = {arXiv},
arxivid = {1601.03406},
author = {Sellwood, J. A.},
eprint = {1601.03406},
file = {:home/mel/Documents/Papers/1601.03406v1.pdf:pdf},
month = {jan},
pages = {8},
title = {{Bar instability in disk-halo systems}},
url = {http://arxiv.org/abs/1601.03406},
year = {2016},
}
@article{Simmons2014,
abstract = {The formation of bars in disc galaxies is a tracer of the dynamical maturity of the population. Previous studies have found that the incidence of bars in discs decreases from the local Universe to z [{\~{}}] 1, and by z > 1 simulations predict that bar features in dynamically mature discs should be extremely rare. Here, we report the discovery of strong barred structures in massive disc galaxies at z [{\~{}}] 1.5 in deep rest-frame optical images from the Cosmic Assembly Near-Infrared Deep Extragalactic Legacy Survey. From within a sample of 876 disc galaxies identified by visual classification in Galaxy Zoo, we identify 123 barred galaxies. Selecting a subsample within the same region of the evolving galaxy luminosity function (brighter than L*), we find that the bar fraction across the redshift range 0.5 [{\&}le;] z [{\&}le;] 2 ( [IMG]f1.gif ALT=Formula BORDER=0> per cent after correcting for incompleteness) does not significantly evolve. We discuss the implications of this discovery in the context of existing simulations and our current understanding of the way disc galaxies have evolved over the last 11 billion years.},
author = {Simmons, B. D. and Melvin, T. and Lintott, C. and Masters, K. L. and Willett, K. W. and Keel, W. C. and Smethurst, R. J. and Cheung, E. and Nichol, R. C. and Schawinski, K. and Rutkowski, M. and Kartaltepe, J. S. and Bell, E. F. and Casteels, K. R. V. and Conselice, C. J. and Almaini, O. and Ferguson, H. C. and Fortson, L. and Hartley, W. and Kocevski, D. and Koekemoer, A. M. and McIntosh, D. H. and Mortlock, A. and Newman, J. A. and Ownsworth, J. and Bamford, S. and Dahlen, T. and Faber, S. M. and Finkelstein, S. L. and Fontana, A. and Galametz, A. and Grogin, N. A. and Grutzbauch, R. and Guo, Y. and Haussler, B. and Jek, K. J. and Kaviraj, S. and Lucas, R. A. and Peth, M. and Salvato, M. and Wiklind, T. and Wuyts, S.},
doi = {10.1093/mnras/stu1817},
file = {:home/mel/Documents/Papers/1409.1214v1.pdf:pdf},
issn = {0035-8711},
journal = {Monthly Notices of the Royal Astronomical Society},
month = {oct},
number = {4},
pages = {3466--3474},
title = {{Galaxy Zoo: CANDELS barred discs and bar fractions}},
url = {http://mnras.oxfordjournals.org/cgi/content/long/445/4/3466},
volume = {445},
year = {2014},
}
@article{Peth2015,
abstract = {To understand the processes driving galaxy morphology and star formation, we need a robust method to classify the structural elements of galaxies. Important but rare and subtle features may be missed by traditional spiral, elliptical, irregular or S$\backslash$'ersic bulge/disc classifications. To overcome this limitation, we use a principal component analysis of non-parametric morphological indicators (concentration, asymmetry, Gini coefficient, {\$}M{\_}{\{}20{\}}{\$}, multi-mode, intensity and deviation) measured at rest-frame {\$}B{\$}-band (corresponding to HST/WFC3 F125W at 1.4 {\$}< z <{\$} 2) to trace the natural distribution of massive ({\$}>10{\^{}}{\{}10{\}} M{\_}{\{}\backslashodot{\}}{\$}) galaxy morphologies. Principal component analysis (PCA) quantifies the correlations between these morphological indicators and determines the relative importance of each. The first three principal components (PCs) capture {\$}\backslashsim{\$}75 per cent of the variance inherent to our sample. We interpret the first principal component (PC) as bulge strength, the second PC as dominated by concentration and the third PC as dominated by asymmetry. Both PC1 and PC2 correlate with the visual appearance of a central bulge and predict galaxy quiescence. We divide the PCA results into 10 groups using an agglomerative hierarchical clustering method. Unlike S$\backslash$'ersic, this classification scheme separates quenched compact galaxies from larger, smooth proto-elliptical systems, and star-forming disc-dominated clumpy galaxies from star-forming bulge-dominated asymmetric galaxies. Distinguishing between these galaxy structural types in a quantitative manner is an important step towards understanding the connections between morphology, galaxy assembly and star-formation.},
archiveprefix = {arXiv},
arxivid = {1504.01751},
author = {Peth, Michael A. and Lotz, Jennifer M. and Freeman, Peter E. and McPartland, Conor and Mortazavi, S. Alireza and Snyder, Gregory F. and Grogin, Norman A. and Guo, Yicheng and Hemati, Shoubaneh and Karteltepe, Jeyhan S. and Kocevski, Dale D. and Koekemoer, Anton M. and McIntosh, Daniel H. and Nayyeri, Hooshang and Papovich, Casey and Primack, Joel R. and Simons, Raymond C. and van der Wel, Arjen},
eprint = {1504.01751},
file = {:home/mel/Documents/Papers/1504.01751v1.pdf:pdf},
month = {apr},
pages = {27},
title = {{Beyond Spheroids and Discs: Classifications of CANDELS Galaxy Structure at 1.4 < z < 2 via Principal Component Analysis}},
url = {http://arxiv.org/abs/1504.01751},
year = {2015},
}
@article{Kauffmann2003,
author = {Kauffmann, Guinevere and Heckman, Timothy M. and {Simon White}, D. M. and Charlot, St{\'{e}}phane and Tremonti, Christy and Brinchmann, Jarle and Bruzual, Gustavo and Peng, Eric W. and Seibert, Mark and Bernardi, Mariangela and Blanton, Michael and Brinkmann, Jon and Castander, Francisco and Cs{\'{a}}bai, Istvan and Fukugita, Masataka and Ivezic, Zeljko and Munn, Jeffrey A. and Nichol, Robert C. and Padmanabhan, Nikhil and Thakar, Aniruddha R. and Weinberg, David H. and York, Donald},
doi = {10.1046/j.1365-8711.2003.06291.x},
file = {:home/mel/Documents/Papers/2003MNRAS.341...33K.pdf:pdf},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
language = {en},
month = {may},
number = {1},
pages = {33--53},
title = {{Stellar masses and star formation histories for 10 5 galaxies from the Sloan Digital Sky Survey}},
url = {http://adslabs.org/adsabs/abs/2003MNRAS.341...33K/},
volume = {341},
year = {2003},
}
@article{MenendezDelmestre2007,
abstract = {We have measured the fraction of bars in nearby spiral galaxies using near-infrared J, H, and Ks images of 151 spiral galaxies from 2MASS. This local sample provides an anchor for the study of the evolution of the bar fraction and bar properties with redshift. We identify bars by analyzing the full two-dimensional light distribution and requiring a combined ellipticity and position angle signature. The combined ``bar signature'' is found in 59{\%} of the galaxies. The bar fraction increases to 67{\%} when we include ``candidate'' bars, where only the ellipticity signature is present. We also measure the change in the bar fraction as a function of bar size; the bar fraction drops to 31{\%} for bars with a semimajor axis larger than 4 kpc. We find that infrared bars typically extend to one-third of the galactic disk, with a deprojected relative size of bar/R25{\&}gt;{\~{}}0.3+/-0.2. Early-type spirals host significantly larger bars, consistent with earlier studies. The bar/R25{\&}gt; is 2 times larger in early types than in late types. The typical bar axial ratio (b/a) is {\~{}}0.5, with a weak trend of higher axial ratios for larger bars.},
author = {Menendez‐Delmestre, Karin and Sheth, Kartik and Schinnerer, Eva and Jarrett, Thomas H. and Scoville, Nick Z.},
doi = {10.1086/511025},
file = {:home/mel/Documents/Papers/65111.web.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
keywords = {Galaxies: Spiral,Galaxies: Structure,Infrared: Galaxies,Methods: Data Analysis,Techniques: Photometric},
month = {mar},
number = {2},
pages = {790--804},
title = {{A Near‐Infrared Study of 2MASS Bars in Local Galaxies: An Anchor for High‐Redshift Studies}},
url = {http://adsabs.harvard.edu/abs/2007ApJ...657..790M},
volume = {657},
year = {2007},
}
@article{Chang2015,
abstract = {We combine SDSS and WISE photometry for the full SDSS spectroscopic galaxy sample, creating SEDs that cover lambda=0.4-22 micron for an unprecedented large and comprehensive sample of 858,365 present-epoch galaxies. Using MAGPHYS we then model simultaneously and consistently both the attenuated stellar SED and the dust emission at 12 micron and 22 micron, producing robust new calibrations for monochromatic mid-IR star formation rate proxies. These modeling results provide the first mid-IR-based view of the bi-modality in star formation activity among galaxies, exhibiting the sequence of star-forming galaxies (main sequence) with a slope of dlogSFR/dlogM*=0.80 and a scatter of 0.39 dex. We find that these new star-formation rates along the SF main sequence are systematically lower by a factor of 1.4 than those derived from optical spectroscopy. We show that for most present-day galaxies the 0.4-22 micron SED fits can exquisitely predict the fluxes measured by Herschel at much longer wavelengths. Our analysis also illustrates that the majorities of stars in the present-day universe is formed in luminous galaxies ({\~{}}L*) in and around the green valley of the color-luminosity plane. We make the matched photometry catalog and SED modeling results publicly available.},
archiveprefix = {arXiv},
arxivid = {1506.00648},
author = {Chang, Yu-Yen and van der Wel, Arjen and da Cunha, Elisabete and Rix, Hans-Walter},
eprint = {1506.00648},
file = {:home/mel/Documents/Papers/1506.00648v1.pdf:pdf},
month = {jun},
title = {{Stellar Masses and SFRs for 1M Galaxies from SDSS and WISE}},
url = {http://arxiv.org/abs/1506.00648},
year = {2015},
}
@article{Buta2003,
abstract = {About one fifth of all spiral disk galaxies include a ring-shaped pattern in the light distribution, and an additional one third appear to have broken or partial rings made up of spiral arms (pseudorings). These rings are a special problem in galaxy morphology with a direct bearing on the internal dynamics and evolution of disk galaxies. Morphological data have shown that rings are most often associated with bars or other common nonaxisymmetric perturbations, such as ovals. Kinematic and metric data have provided considerable evidence for intrinsic oval shapes and preferred alignments between ring major axes and bars. Photometric data have demonstrated that most rings are sites of current active star formation, and in some galaxies a ring is the only place where recent star formation is found. A few rings are sites of the most spectacular ``starbursts'' known in non-violently interacting galaxies. Though a small fraction of observed rings may be due to collisions or mergers of galaxies, or to accretion of intergalactic gas, the vast majority of rings are probably simple resonance phenomena, caused by the actions of a rotating bar or other nonaxisymmetric disturbance on the motions of gas clouds in the disk. The evidence in support of this idea has accumulated steadily during the past 15 years, and our goal in this review is to bring together a large body of theoretical and observational results in one place. We shall see that rings are a natural consequence of barred galaxy dynamics, and that they are more easily understood than the bars and ovals which undoubtedly create them. However, there are interesting problems, such as the lack of any rings in some barred galaxies, the less common but by no means rare cases of rings in nonbarred galaxies, the role of mild tidal interactions, where the gas that fuels star formation in rings actually comes from, the existence of intrinsic bar/ring misalignment, and the simultaneous existence of different ring types of very different time-scales in the same galaxy. We will discuss these problems in some detail here, and indicate where the solutions may lie.},
author = {Buta, R and Combes, F},
file = {:home/mel/Documents/Papers/rings.pdf:pdf},
keywords = {bars,dynamics,evolution,galaxies - structure,rings,simulations},
pages = {1--104},
title = {{Galactic Rings}},
volume = {17},
year = {2003},
}
@article{Willett2013,
abstract = {We present the data release for Galaxy Zoo 2 (GZ2), a citizen science project with more than 16 million morphological classifications of 304,122 galaxies drawn from the Sloan Digital Sky Survey. Morphology is a powerful probe for quantifying a galaxy’s dy- namical history; however, automatic classifications of morphology (either by computer analysis of images or by using other physical parameters as proxies) still have drawbacks when compared to visual inspection. The large number of images available in current surveys makes visual inspection of each galaxy impractical for individual astronomers. GZ2 uses classifications from volunteer citizen scientists to measure morphologies for all galaxies in the DR7 Legacy survey with mr > 17, in addition to deeper images from SDSS Stripe 82. While the original Galaxy Zoo project identified galaxies as early-types, late-types, or mergers, GZ2 measures finer morphological features. These include bars, bulges, and the shapes of edge-on disks, as well as quantifying the relative strengths of galactic bulges and spiral arms. This paper presents the full public data release for the project, including measures of accuracy and bias. The majority (? 90{\%}) of GZ2 classifications agree with those made by professional astronomers, especially for morphological T-types, strong bars, and arm curvature. Both the raw and reduced data products can be obtained in electronic format at http://data.galaxyzoo.org.},
archiveprefix = {arXiv},
arxivid = {arXiv:1308.3496v2},
author = {Willett, Kyle W. and Lintott, Chris J. and Bamford, Steven P. and Masters, Karen L. and Simmons, Brooke D. and Casteels, Kevin R V and Edmondson, Edward M. and Fortson, Lucy F. and Kaviraj, Sugata and Keel, William C. and Melvin, Thomas and Nichol, Robert C. and {Jordan Raddick}, M. and Schawinski, Kevin and Simpson, Robert J. and Skibba, Ramin A. and Smith, Arfon M. and Thomas, Daniel},
doi = {10.1093/mnras/stt1458},
eprint = {arXiv:1308.3496v2},
file = {:home/mel/Documents/Papers/MNRAS-2013-Willett-2835-60.pdf:pdf},
isbn = {doi:10.1093/mnras/stt1458},
issn = {00358711},
journal = {Monthly Notices of the Royal Astronomical Society},
keywords = {Catalogues,Galaxies: elliptical and lenticular,Galaxies: general,Galaxies: spiral,Methods: data analysis},
pages = {2835--2860},
title = {{Galaxy zoo 2: Detailed morphological classifications for 304 122 galaxies from the sloan digital sky survey}},
volume = {435},
year = {2013},
}
@article{Gavazzi2015,
abstract = {A growing body of evidence indicates that the star formation rate per unit stellar mass (sSFR) decreases with increasing mass in normal main-sequence star forming galaxies. Many processes have been advocated as responsible for such a trend (also known as mass quenching), e.g., feedback from active galactic nuclei (AGNs), and the formation of classical bulges. We determine a refined star formation versus stellar mass relation in the local Universe. To this aim we use the Halpha narrow-band imaging follow-up survey (Halpha3) of field galaxies selected from the HI Arecibo Legacy Fast ALFA Survey (ALFALFA) in the Coma and Local superclusters. By complementing this local determination with high-redshift measurements from the literature, we reconstruct the star formation history of main-sequence galaxies as a function of stellar mass from the present epoch up to z=3. In agreement with previous studies, our analysis shows that quenching mechanisms occur above a threshold stellar mass M{\_}knee that evolves with redshift as propto (1+z){\^{}}{\{}2{\}}. Moreover, visual morphological classification of individual objects in our local sample reveals a sharp increase in the fraction of visually-classified strong bars with mass, hinting that strong bars may contribute to the observed downturn in the sSFR above M{\_}knee. We test this hypothesis using a simple but physically-motivated numerical model for bar formation, finding that strong bars can rapidly quench star formation in the central few kpc of field galaxies. We conclude that strong bars contribute significantly to the red colors observed in the inner parts of massive galaxies, although additional mechanisms are likely required to quench the star formation in the outer regions of massive spiral galaxies. Intriguingly, when we extrapolate our model to higher redshifts, we successfully recover the observed redshift evolution for M{\_}knee.},
archiveprefix = {arXiv},
arxivid = {1505.07836},
author = {Gavazzi, G. and Consolandi, G. and Dotti, M. and Fanali, R. and Fossati, M. and Fumagalli, M. and Viscardi, E. and Savorgnan, G. and Boselli, A. and Guti{\'{e}}rrez, L. and Toledo, H. Hern{\'{a}}ndez and Giovanelli, R. and Haynes, M. P.},
eprint = {1505.07836},
file = {:home/mel/Documents/Papers/1505.07836v1.pdf:pdf},
month = {may},
title = {{The role of bars in quenching star formation from z = 3 to the present epoch. Halpha3: an Halpha imaging survey of HI selected galaxies from ALFALFA, VI}},
url = {http://arxiv.org/abs/1505.07836},
year = {2015},
}
@article{Knapen2015,
abstract = {We complement a recent ApJ Letter by Luo et al. by comparing the fraction of starburst galaxies which are interacting with the overall fraction of interacting galaxies in the nearby galaxy population (within 40 Mpc). We confirm that in starburst galaxies the fraction of interacting galaxies is enhanced, by a factor of around 2, but crucially we do so by studying a sample of almost 1500 of the nearest galaxies, including many dwarfs and irregulars. We discuss how adjusting the starburst definition influences the final result and conclude that our result is stable. We find significantly lower fractions of interacting galaxies than Luo et al. did from their larger but more distant sample of galaxies, and argue that the difference is most likely due to various biases in the sample selection, with a representative sample of the nearest galaxies, such as the one used here, being the best possible representation of a general picture. Our overall conclusion is that interactions can and do increase the number of starburst galaxies, and that this result is extremely robust. By far most starburst galaxies, however, show no evidence of a present interaction.},
archiveprefix = {arXiv},
arxivid = {1506.00656},
author = {Knapen, Johan H. and Cisternas, Mauricio},
eprint = {1506.00656},
file = {:home/mel/Documents/Papers/1506.00656v1.pdf:pdf},
month = {jun},
title = {{Starbursts are preferentially interacting: confirmation from the nearest galaxies}},
url = {http://arxiv.org/abs/1506.00656},
year = {2015},
}
@article{Skibba2014,
abstract = {We present measurements of the luminosity and color-dependence of galaxy clustering at 0.2<z<1.0 in the PRIsm MUlti-object Survey (PRIMUS). We quantify the clustering with the redshift-space and projected two-point correlation functions, xi(rp,pi) and wp(rp), using volume-limited samples constructed from a parent sample of over 130,000 galaxies with robust redshifts in seven independent fields covering 9 sq. deg. of sky. We quantify how the scale-dependent clustering amplitude increases with increasing luminosity and redder color, with relatively small errors over large volumes. We find that red galaxies have stronger small-scale (0.1<rp<1 Mpc/h) clustering and steeper correlation functions compared to blue galaxies, as well as a strong color dependent clustering within the red sequence alone. We interpret our measured clustering trends in terms of galaxy bias and obtain values between b{\_}gal=0.9-2.5, quantifying how galaxies are biased tracers of dark matter depending on their luminosity and color. We also interpret the color dependence with mock catalogs, and find that the clustering of blue galaxies is nearly constant with color, while redder galaxies have stronger clustering in the one-halo term due to a higher satellite galaxy fraction. In addition, we measure the evolution of the clustering strength and bias, and we do not detect statistically significant departures from passive evolution. We argue that the luminosity- and color-environment (or halo mass) relations of galaxies have not significantly evolved since z=1. Finally, using jackknife subsampling methods, we find that sampling fluctuations are important and that the COSMOS field is generally an outlier, due to having more overdense structures than other fields; we find that 'cosmic variance' can be a significant source of uncertainty for high-redshift clustering measurements.},
archiveprefix = {arXiv},
arxivid = {1310.1093},
author = {Skibba, Ramin A. and Smith, M. Stephen M. and Coil, Alison L. and Moustakas, John and Aird, James and Blanton, Michael R. and Bray, Aaron D. and Cool, Richard J. and Eisenstein, Daniel J. and Mendez, Alexander J. and Wong, Kenneth C. and Zhu, Guangtun},
doi = {10.1088/0004-637X/784/2/128},
eprint = {1310.1093},
file = {:home/mel/Documents/Papers/1310.1093v3.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {apr},
number = {2},
pages = {128},
title = {{PRIMUS: GALAXY CLUSTERING AS A FUNCTION OF LUMINOSITY AND COLOR AT 0.2 < z < 1}},
url = {http://arxiv.org/abs/1310.1093},
volume = {784},
year = {2014},
}
@article{Knobel2015,
abstract = {We re-examine the fraction of low-redshift Sloan Digital Sky Survey satellites and centrals in which star formation has been quenched, using the environment quenching efficiency formalism that separates out the dependence of stellar mass. We show that the centrals of the groups containing the satellites are responding to the environment in the same way as their satellites (at least for stellar masses above 10{\^{}}10.3 Msun), and that the well-known differences between satellites and the general set of centrals arise because the latter are overwhelmingly dominated by isolated galaxies. The widespread concept of satellite quenching as the cause of environmental effects in the galaxy population can therefore be generalized to group quenching. We then explore the dependence of the quenching efficiency of satellites on overdensity, group-centric distance, halo mass, the stellar mass of the satellite, and the stellar mass and specific star formation rate (sSFR) of its central, trying to isolate the effect of these often interdependent variables. We emphasize the importance of the central sSFR in the quenching efficiency of the associated satellites, and develop the meaning of this galactic conformity effect in a probabilistic description of the quenching of galaxies. We show that conformity is strong, and that it varies strongly across parameter space. Several arguments then suggest that environmental quenching and mass quenching may be different manifestations of the same underlying process. The marked difference in the apparent mass dependencies of environment quenching and mass quenching which produces distinctive signatures in the mass functions of centrals and satellites will arise naturally, since, for satellites at least, the distributions of the environmental variables that we investigate in this work are essentially independent of the stellar mass of the satellite.},
archiveprefix = {arXiv},
arxivid = {1408.2553},
author = {Knobel, Christian and Lilly, Simon J. and Woo, Joanna and Kova{\v{c}}, Katarina},
doi = {10.1088/0004-637X/800/1/24},
eprint = {1408.2553},
file = {:home/mel/Documents/Papers/1408.2553v2.pdf:pdf},
issn = {1538-4357},
journal = {The Astrophysical Journal},
month = {feb},
number = {1},
pages = {24},
title = {{QUENCHING OF STAR FORMATION IN SLOAN DIGITAL SKY SURVEY GROUPS: CENTRALS, SATELLITES, AND GALACTIC CONFORMITY}},
url = {http://arxiv.org/abs/1408.2553},
volume = {800},
year = {2015},
}
@article{Bundy2009,
abstract = {Using deep infrared observations conducted with the MOIRCS on the Subaru Telescope in GOODS-N combined with public surveys in GOODS-S, we investigate the dependence on stellar mass, M{\_}*, and galaxy type of the close pair fraction (5 kpc < r < 20 kpc) and implied merger rate. In common with some recent studies we find that the fraction of paired systems that could result in major mergers is low ({\~{}}4{\%}) and does not increase significantly with redshift to z{\~{}}1.2, with (1+z){\^{}}{\{}1.6 $\backslash$pm 1.6{\}}. Our key finding is that massive galaxies with M{\_}* > 1E11 Msun are more likely to host merging companions than less massive systems (M{\_}* {\~{}} 1E10 Msun). We find evidence for a higher pair fraction for red, spheroidal hosts compared to blue, late-type systems, in line with expectations based on clustering at small scales. So-called dry mergers between early-type galaxies represent nearly 50{\%} of close pairs with M{\_}* > 3E10 Msun at z{\~{}}0.5, but less than 30{\%} at z{\~{}}1. This result can be explained by the increasing abundance of red, early-type galaxies at these masses. We compare the volumetric merger rate of galaxies with different masses to mass-dependent trends in galaxy evolution, finding that major mergers cannot fully account for the formation of spheroidal galaxies since z{\~{}}1. In terms of mass assembly, major mergers contribute little to galaxy growth below M{\_}* {\~{}} 3E10 Msun but are more significant among galaxies with M{\_}* > 1E11 Msun, 30{\%} of which have undergone mostly dry mergers over the observed redshift range. Overall, the relatively more rapid coalescence of high mass galaxies mirrors the expected hierarchical growth of halos and is consistent with recent model predictions, even if the downsizing of star formation and morphological evolution involves additional physical processes.},
annote = {Source of GOODS-N photoz's.},
archiveprefix = {arXiv},
arxivid = {0902.1188},
author = {Bundy, Kevin and Fukugita, Masataka and Ellis, Richard S. and Targett, Thomas A. and Belli, Sirio and Kodama, Tadayuki},
doi = {10.1088/0004-637X/697/2/1369},
eprint = {0902.1188},
file = {:home/mel/Documents/Papers/0902.1188v1.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {jun},
number = {2},
pages = {1369--1383},
title = {{THE GREATER IMPACT OF MERGERS ON THE GROWTH OF MASSIVE GALAXIES: IMPLICATIONS FOR MASS ASSEMBLY AND EVOLUTION SINCE z ≃ 1}},
url = {http://arxiv.org/abs/0902.1188},
volume = {697},
year = {2009},
}
@article{Hogg1999,
abstract = {Formulae for the line-of-sight and transverse comoving distances, proper motion distance, angular diameter distance, luminosity distance, k-correction, distance modulus, comoving volume, lookback time, age, and object intersection probability are all given, some with justifications. Some attempt is made to rationalize disparate terminologies, or at least abuse bad usage.},
archiveprefix = {arXiv},
arxivid = {astro-ph/9905116},
author = {Hogg, David W.},
eprint = {9905116},
file = {:home/mel/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Hogg - 1999 - Distance measures in cosmology.pdf:pdf},
month = {may},
primaryclass = {astro-ph},
title = {{Distance measures in cosmology}},
url = {http://arxiv.org/abs/astro-ph/9905116},
year = {1999},
}
@article{Davies2015,
abstract = {Both theoretical predictions and observations of the very nearby Universe suggest that low-mass galaxies (log{\$}{\_}{\{}10{\}}{\$}[M{\$}{\_}{\{}*{\}}{\$}/M{\$}{\_}{\{}\backslashodot{\}}{\$}]<9.5) are likely to remain star-forming unless they are affected by their local environment. To test this premise, we compare and contrast the local environment of both passive and star-forming galaxies as a function of stellar mass, using the Galaxy and Mass Assembly survey. We find that passive fractions are higher in both interacting pair and group galaxies than the field at all stellar masses, and that this effect is most apparent in the lowest mass galaxies. We also find that essentially all passive log{\$}{\_}{\{}10{\}}{\$}[M{\$}{\_}{\{}*{\}}{\$}/M{\$}{\_}{\{}\backslashodot{\}}{\$}]<8.5 galaxies are found in pair/group environments, suggesting that local interactions with a more massive neighbour cause them to cease forming new stars. We find that the effects of immediate environment (local galaxy-galaxy interactions) in forming passive systems increases with decreasing stellar mass, and highlight that this is potentially due to increasing interaction timescales giving sufficient time for the galaxy to become passive via starvation. We then present a simplistic model to test this premise, and show that given our speculative assumptions, it is consistent with our observed results.},
archiveprefix = {arXiv},
arxivid = {1511.02245},
author = {Davies, L. J. M. and Robotham, A. S. G. and Driver, S. P. and Alpaslan, M. and Baldry, I. K. and Bland-Hawthorn, J. and Brough, S. and Brown, M. J. I. and Cluver, M. E. and Holwerda, B. W. and Hopkins, A. M. and Lara-Lopez, M. A. and Mahajan, S. and Moffett, A. J. and Owers, M. S. and Phillipps, S.},
eprint = {1511.02245},
file = {:home/mel/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Davies et al. - 2015 - Galaxy And Mass Assembly (GAMA) growing up in a bad neighbourhood - how do low-mass galaxies become passive.pdf:pdf},
month = {nov},
pages = {20},
title = {{Galaxy And Mass Assembly (GAMA): growing up in a bad neighbourhood - how do low-mass galaxies become passive?}},
url = {http://arxiv.org/abs/1511.02245},
year = {2015},
}
@article{Wolf2004,
abstract = {We present the COMBO-17 object catalogue of the Chandra Deep Field South for public use, covering a field which is 31.5' x 30' in size. This catalogue lists astrometry, photometry in 17 passbands from 350 to 930 nm, and ground-based morphological data for 63,501 objects. The catalogue also contains multi-colour classification into the categories 'Star', 'Galaxy' and 'Quasar' as well as photometric redshifts. We include restframe luminosities in Johnson, SDSS and Bessell passbands and estimated errors. The redshifts are most reliable at R<24, where the sample contains approximately 100 quasars, 1000 stars and 10000 galaxies. We use nearly 1000 spectroscopically identified objects in conjunction with detailed simulations to characterize the performance of COMBO-17. We show that the selection of quasars, more generally type-1 AGN, is nearly complete and minimally contaminated at z=[0.5,5] for luminosities above M{\_}B=-21.7. Their photometric redshifts are accurate to roughly 5000 km/sec. Galaxy redshifts are accurate to 1{\%} in dz/(1+z) at R<21. They degrade in quality for progressively fainter galaxies, reaching accuracies of 2{\%} for galaxies with R{\~{}}222 and of 10{\%} for galaxies with R>24. The selection of stars is complete to R{\~{}}23, and deeper for M stars. We also present an updated discussion of our classification technique with maps of survey completeness, and discuss possible failures of the statistical classification in the faint regime at R>24.},
annote = {Goods-S and GEMS photo-z's (also wolf et al 2008)},
archiveprefix = {arXiv},
arxivid = {astro-ph/0403666},
author = {Wolf, C. and Meisenheimer, K. and Kleinheinrich, M. and Borch, A. and Dye, S. and Gray, M. and Wisotzki, L. and Bell, E. F. and Rix, H.-W. and Cimatti, A. and Hasinger, G. and Szokoly, G.},
doi = {10.1051/0004-6361:20040525},
eprint = {0403666},
file = {:home/mel/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Wolf et al. - 2004 - A catalogue of the Chandra Deep Field South with multi-colour classification and photometric redshifts from COMBO-1.pdf:pdf},
issn = {0004-6361},
journal = {Astronomy and Astrophysics},
month = {jul},
number = {3},
pages = {913--936},
primaryclass = {astro-ph},
title = {{A catalogue of the Chandra Deep Field South with multi-colour classification and photometric redshifts from COMBO-17}},
url = {http://arxiv.org/abs/astro-ph/0403666},
volume = {421},
year = {2004},
}
@article{Lanzuisi2015,
abstract = {Highly obscured active galactic nuclei (AGN) are common in nearby galaxies, but are difficult to observe beyond the local Universe, where they are expected to significantly contribute to the black hole accretion rate density. Furthermore, Compton-thick (CT) absorbers (NH>10{\^{}}24 cm{\^{}}-2) suppress even the hard X-ray (2-10 keV) AGN nuclear emission, and therefore the column density distribution above 10{\^{}}24 cm{\^{}}-2 is largely unknown. We present the identification and multi-wavelength properties of a heavily obscured (NH>{\~{}}10{\^{}}25 cm{\^{}}-2), intrinsically luminous (L(2-10keV)>10{\^{}}44 erg s{\^{}}-1) AGN at z=0.353 in the COSMOS field. Several independent indicators, such as the shape of the X-ray spectrum, the decomposition of the spectral energy distribution and X-ray/[NeV] and X-ray/6{\{}$\backslash$mu{\}}m luminosity ratios, agree on the fact that the nuclear emission must be suppressed by a 10{\^{}}25 cm{\^{}}-2 column density. The host galaxy properties show that this highly obscured AGN is hosted in a massive star-forming galaxy, showing a barred morphology, which is known to correlate with the presence of CT absorbers. Finally, asymmetric and blueshifted components in several optical high-ionization emission lines indicate the presence of a galactic outflow, possibly driven by the intense AGN activity (L(Bol)/L(Edd) = 0.3-0.5). Such highly obscured, highly accreting AGN are intrinsically very rare at low redshift, whereas they are expected to be much more common at the peak of the star formation and BH accretion history, at z{\~{}}2-3. We demonstrate that a fully multi-wavelength approach can recover a sizable sample of such peculiar sources in large and deep surveys such as COSMOS.},
archiveprefix = {arXiv},
arxivid = {1505.01153},
author = {Lanzuisi, G. and Perna, M. and Delvecchio, I. and Berta, S. and Brusa, M. and Cappelluti, N. and Comastri, A. and Gilli, R. and Gruppioni, C. and Mignoli, M. and Pozzi, F. and Vietri, G. and Vignali, C. and Zamorani, G.},
eprint = {1505.01153},
file = {:home/mel/Documents/Papers/1505.01153v1.pdf:pdf},
month = {may},
pages = {6},
title = {{The most obscured AGN in the COSMOS field}},
url = {http://arxiv.org/abs/1505.01153},
year = {2015},
}
@article{Cen2014,
abstract = {A new physical framework for the emergence of the Hubble sequence is outlined, based on novel analyses performed to quantify the evolution of cold streams of a large sample of galaxies from a state-of-the-art ultra-high resolution, large-scale adaptive mesh-refinement hydrodynamic simulation in a fully cosmological setting. It is found that the following three key physical variables of galactic cold inflows crossing the virial sphere substantially decrease with decreasing redshift: the number of streams N{\_}{\{}90{\}} that make up 90{\%} of concurrent inflow mass flux, average inflow rate per stream dot M{\_}{\{}90{\}} and mean (mass flux weighted) gas density in the streams n{\_}{\{}gas{\}}. Another key variable, the stream dimensionless angular momentum parameter lambda, instead is found to increase with decreasing redshift. Assimilating these trends and others leads naturally to a physically coherent scenario for the emergence of the Hubble sequence, including the following expectations: (1) the predominance of a mixture of disproportionately small irregular and complex disk galaxies at z>2 when most galaxies have multiple concurrent streams, (2) the beginning of the appearance of flocculent spirals at z{\~{}}1-2 when the number of concurrent streams are about 2-3, (3) the grand-design spiral galaxies appear at z<1 when galaxies with only one major cold stream significantly emerge. These expected general trends are in good accord with observations. Early type galaxies are those that have entered a perennial state of zero cold gas stream, with their abundance increasing with decreasing redshift.},
archiveprefix = {arXiv},
arxivid = {1405.0516},
author = {Cen, Renyue},
doi = {10.1088/2041-8205/789/1/L21},
eprint = {1405.0516},
file = {:home/mel/Documents/Papers/1405.0516v1.pdf:pdf},
issn = {2041-8205},
journal = {The Astrophysical Journal},
month = {jul},
number = {1},
pages = {L21},
title = {{EVOLUTION OF COLD STREAMS AND THE EMERGENCE OF THE HUBBLE SEQUENCE}},
url = {http://arxiv.org/abs/1405.0516},
volume = {789},
year = {2014},
}
@article{DeGraf2014,
abstract = {We use the high-resolution simulation MassiveBlackII to examine scaling relations between black hole mass (MBH) and host galaxy properties (sigma, M*, and LV), finding good agreement with observational data, especially at the high-mass end. The simulations have less intrinsic scatter than observations, and the MBH-LV correlation has the largest scatter, suggesting it may the the least fundamental of the three relations. We find Gaussian scatter about all three relations, except among the highest mass galaxies, which host more massive black holes. Below z{\~{}}2 the slopes for the full population remain roughly z-independent, and only steepen by 50{\%} by z{\~{}}4. The normalization of the sigma, LV relations evolve by 0.3, 0.43 dex, while the MBH correlation does not evolve to at least z{\~{}}2. Testing for selection biases, we find samples selected by MBH or M* have steeper slopes than randomly selected samples. If unaccounted for, such a selection function would find faster evolution than inferred from a randomly selected sample, as objects at the highend of the relation tend to evolve more rapidly. We find a potential bias among high-LBH subsamples (tending to reside in higher mass galaxies), but these bright-AGN exhibit no intrinsic bias relative to fainter ones in equivalent-mass hosts, nor is there a significant difference between active- and inactive-samples. Finally we characterize the evolution of individual black holes along the scaling planes. Below the local relation, black holes grow faster than their host (72{\%} of black holes 0.3 dex below the mean relation have a MBH-M* trajectory steeper than the local relation), while those above have shallower trajectories (only 14{\%} are steeper than local). Black holes tend to grow faster than their hosts until surpassing the local relation, at which point their growth is suppressed while their hosts continue to grow, returning them to the mean relation.},
archiveprefix = {arXiv},
arxivid = {1412.4133},
author = {DeGraf, Colin and {Di Matteo}, Tiziana and Treu, Tommaso and Feng, Yu and Woo, Jong-Hak and Park, Daeseong},
eprint = {1412.4133},
file = {:home/mel/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/DeGraf et al. - 2014 - Scaling relations between black holes and their host galaxies comparing theoretical and observational measurement.pdf:pdf},
month = {dec},
pages = {17},
title = {{Scaling relations between black holes and their host galaxies: comparing theoretical and observational measurements, and the impact of selection effects}},
url = {http://arxiv.org/abs/1412.4133},
year = {2014},
}
@article{Emsellem2014b,
abstract = {We study the connection between the large-scale dynamics and the gas fueling toward a central black hole via the analysis of a Milky Way-like simulation at sub-parsec resolution. This allows us to follow a set of processes at various scales (e.g., the triggering of inward gas motion towards inner resonances via the large-scale bar, the connection to the central black hole via mini spirals) in a self-consistent manner. This simulation provides further insights on the role of shear for the inhibition of star formation within the bar in regions with significant amount of gas. We also witness the decoupling of the central gas and nuclear cluster from the large-scale disc, via interactions with the black hole. This break of symmetry in the mass distribution triggers the formation of gas clumps organised in a time-varying 250 pc ring-like structure, the black hole being offset by about 70 pc from its centre. Some clumps form stars, while most get disrupted or merge. Supernovae feedback further creates bubbles and filaments, some of the gas being expelled to 100 pc or higher above the galaxy plane. This helps remove angular momentum from the gas, which gets closer to the central dark mass. Part of the gas raining down is being accreted, forming a 10{\~{}}pc polar disc-like structure around the black hole, leading to an episode of star formation. This gives rise to multiple stellar populations with significantly different angular momentum vectors, and may lead to a natural intermittence in the fueling of the black hole.},
archiveprefix = {arXiv},
arxivid = {1410.6479},
author = {Emsellem, Eric and Renaud, Florent and Bournaud, Fr{\'{e}}d{\'{e}}ric and Elmegreen, Bruce and Combes, Fran{\c{c}}oise and Gabor, Jared},
eprint = {1410.6479},
file = {:home/mel/Documents/Papers/1410.6479v1.pdf:pdf},
month = {oct},
pages = {15},
title = {{The interplay between a galactic bar and a supermassive black hole: nuclear fueling in a sub-parsec resolution galaxy simulation}},
url = {http://arxiv.org/abs/1410.6479},
year = {2014},
}
@article{Warren2007,
archiveprefix = {arXiv},
arxivid = {astro-ph/0703037},
author = {Warren, S. J. and Cross, N. J. G. and Dye, S. and Hambly, N. C. and Almaini, O. and Edge, A. C. and Hewett, P. C. and Hodgkin, S. T. and Irwin, M. J. and Jameson, R. F. and Lawrence, A. and Lucas, P. W. and Mortlock, D. J. and Adamson, A. J. and Bryant, J. and Collins, R. S. and Davis, C. J. and Emerson, J. P. and Evans, D. W. and Gonzales-Solares, E. A. and Hirst, P. and Kerr, T. H. and Lewis, J. R. and Mann, R. G. and Rawlings, M. G. and Read, M. A. and Riello, M. and Sutorius, E. T. W. and Varricatt, W. P.},
eprint = {0703037},
file = {:home/mel/Documents/Papers/0703037v3.pdf:pdf},
month = {mar},
primaryclass = {astro-ph},
title = {{The UKIRT Infrared Deep Sky Survey Second Data Release}},
url = {http://arxiv.org/abs/astro-ph/0703037},
year = {2007},
}
@article{Guo2014a,
abstract = {Although giant clumps of stars are crucial to galaxy formation and evolution, the most basic demographics of clumps are still uncertain, mainly because the definition of clumps has not been thoroughly discussed. In this paper, we study the basic demographics of clumps in star-forming galaxies (SFGs) at 0.5<z<3, using our proposed physical definition that UV-bright clumps are discrete star-forming regions that individually contribute more than 8{\%} of the rest-frame UV light of their galaxies. Clumps defined this way are significantly brighter than the HII regions of nearby large spiral galaxies, either individually or blended, when physical spatial resolution and cosmological dimming are considered. Under this definition, we measure the fraction of SFGs that contain at least one off-center clump (Fclumpy) and the contributions of clumps to the rest-frame UV light and star formation rate of SFGs in the CANDELS/GOODS-S and UDS fields, where our mass-complete sample consists of 3239 galaxies with axial ratio q>0.5. The redshift evolution of Fclumpy changes with the stellar mass (M*) of the galaxies. Low-mass (log(M*/Msun)<9.8) galaxies keep an almost constant Fclumpy of about 60{\%} from z{\~{}}3.0 to z{\~{}}0.5. Intermediate-mass and massive galaxies drop their Fclumpy from 55{\%} at z{\~{}}3.0 to 40{\%} and 15{\%}, respectively, at z{\~{}}0.5. We find that (1) the trend of disk stabilization predicted by violent disk instability matches the Fclumpy trend of massive galaxies; (2) minor mergers are a viable explanation of the Fclumpy trend of intermediate-mass galaxies at z<1.5, given a realistic observability timescale; and (3) major mergers are unlikely responsible for the Fclumpy trend in all masses at z<1.5. The clump contribution to the rest-frame UV light of SFGs shows a broad peak around galaxies with log(M*/Msun){\~{}}10.5 at all redshifts, possibly linked to the molecular gas fraction of the galaxies. (Abridged)},
archiveprefix = {arXiv},
arxivid = {1410.7398},
author = {Guo, Yicheng and Ferguson, Henry C. and Bell, Eric F. and Koo, David C. and Conselice, Christopher J. and Giavalisco, Mauro and Kassin, Susan and Lu, Yu and Lucas, Ray and Mandelker, Nir and McIntosh, Daniel M. and Primack, Joel R. and Ravindranath, Swara and Barro, Guillermo and Ceverino, Daniel and Dekel, Avishai and Faber, Sandra M. and Fang, Jerome J. and Koekemoer, Anton M. and Noeske, Kai and Rafelski, Marc and Straughn, Amber},
eprint = {1410.7398},
file = {:home/mel/Documents/Papers/1410.7398v2 (1).pdf:pdf},
month = {oct},
pages = {22},
title = {{Clumpy Galaxies in CANDELS: I. The Definition of UV Clumps and the Fraction of Clumpy Galaxies at {\$}0.5<z<3{\$}}},
url = {http://arxiv.org/abs/1410.7398},
year = {2014},
}
@article{Kamar2015,
author = {Kamar, Ece and Horvitz, Eric},
file = {:home/mel/Desktop/hierarchical{\_}tasks{\_}AAMAS.pdf:pdf},
isbn = {9781450337700},
issn = {15582914},
journal = {Aamas},
keywords = {complementary computing,consensus tasks,crowdsourcing,mdps,monte carlo planning},
pages = {1191--1199},
title = {{Planning for Crowdsourcing Hierarchical Tasks}},
year = {2015},
}
@article{Schawinski2009,
abstract = {Residual star formation at late times in early-type galaxies and their progenitors must be suppressed in order to explain the population of red, passively evolving systems we see today. Likewise, residual or newly accreted reservoirs of molecular gas that are fuelling star formation must be destroyed. This suppression of star formation in early-type galaxies is now commonly attributed to AGN feedback wherein the reservoir of gas is heated and expelled during a phase of accretion onto the central supermassive black hole. However, direct observational evidence for a link between the destruction of this molecular gas and an AGN phase has been missing so far. We present new mm-wavelength observations from the IRAM 30m telescope of a sample of low redshift SDSS early-type galaxies currently undergoing this process of quenching of late-time star formation. Our observations show that the disappearance of the molecular gas coincides within less than 100 Myr with the onset of accretion onto the black hole and is too rapid to be due to star formation alone. Since our sample galaxies are not associated to powerful quasar activity or radio jets, we conclude that low-luminosity AGN episodes are sufficient to suppress residual star formation in early-type galaxies. This `suppression mode' of AGN feedback is very different from the `truncation mode' linked to powerful quasar activity during early phases of galaxy formation.},
archiveprefix = {arXiv},
arxivid = {0809.1096},
author = {Schawinski, Kevin and Lintott, Chris J. and Thomas, Daniel and Kaviraj, Sugata and Viti, Serena and Silk, Joseph and Maraston, Claudia and Sarzi, Marc and Yi, Sukyoung K. and Joo, Seok-Joo and Daddi, Emanuele and Bayet, Estelle and Bell, Tom and Zuntz, Joe},
doi = {10.1088/0004-637X/690/2/1672},
eprint = {0809.1096},
file = {:home/mel/Documents/Papers/0809.1096v2.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
month = {jan},
number = {2},
pages = {1672--1680},
title = {{DESTRUCTION OF MOLECULAR GAS RESERVOIRS IN EARLY-TYPE GALAXIES BY ACTIVE GALACTIC NUCLEUS FEEDBACK}},
url = {http://arxiv.org/abs/0809.1096},
volume = {690},
year = {2009},
}
@article{Lee2012,
abstract = {We investigate the connection between the presence of bars and AGN activity, using a volume-limited sample of {\$}\backslashsim{\$}9,000 late-type galaxies with axis ratio {\$}b/a>0.6{\$} and {\$}M{\_}{\{}r{\}} < -19.5+5{\{}\backslashrm log{\}}h{\$} at low redshift ({\$}0.02\backslashle z\backslashlesssim 0.055{\$}), selected from Sloan Digital Sky Survey Data Release 7. We find that the bar fraction in AGN-host galaxies (42.6{\%}) is {\$}\backslashsim{\$}2.5 times higher than in non-AGN galaxies (15.6{\%}), and that the AGN fraction is a factor of two higher in strong-barred galaxies (34.5{\%}) than in non-barred galaxies (15.0{\%}). However, these trends are simply caused by the fact that AGN-host galaxies are on average more massive and redder than non-AGN galaxies because the fraction of strong-barred galaxies ({\$}\backslashbfrsbo{\$}) increases with {\$}u-r{\$} color and stellar velocity dispersion. When {\$}u-r{\$} color and velocity dispersion (or stellar mass) are fixed, both the excess of {\$}\backslashbfrsbo{\$} in AGN-host galaxies and the enhanced AGN fraction in strong-barred galaxies disappears. Among AGN-host galaxies we find no strong difference of the Eddington ratio distributions between barred and non-barred systems. These results indicate that AGN activity is not dominated by the presence of bars, and that AGN power is not enhanced by bars. In conclusion we do not find a clear evidence that bars trigger AGN activity.},
archiveprefix = {arXiv},
arxivid = {1203.1693},
author = {Lee, Gwang-Ho and Woo, Jong-Hak and Lee, Myung Gyoon and Hwang, Ho Seong and Lee, Jong Chul and Sohn, Jubee and Lee, Jong Hwan},
eprint = {1203.1693},
file = {:home/mel/Documents/Papers/1203.1693v1.pdf:pdf},
month = {mar},
pages = {13},
title = {{Do Bars Trigger Activity in Galactic Nuclei?}},
url = {http://arxiv.org/abs/1203.1693},
year = {2012},
}
@article{Johnson2015,
abstract = {We show that interferometry can be applied to study irregular, rapidly rotating structures, as are expected in the turbulent accretion flow near a black hole. Specifically, we analyze the lagged covariance between interferometric baselines of similar lengths but slightly different orientations. We demonstrate that the peak in the lagged covariance indicates the direction and angular velocity of the flow. Importantly, measuring the direction of the flow as clockwise or counterclockwise on the sky breaks a degeneracy in accretion disk inclinations when analyzing time-averaged images alone. We explore the potential efficacy using three-dimensional, general relativistic magnetohydrodynamic (GRMHD) simulations, and we highlight several baseline pairs for the Event Horizon Telescope (EHT) that are well-suited to this application. These results indicate that the EHT is capable of determining the direction and angular velocity of the emitting material near Sgr A*, even for highly-inclined flows, and they suggest that a rotating flow may even be utilized to improve imaging capabilities.},
archiveprefix = {arXiv},
arxivid = {1505.07870},
author = {Johnson, Michael D. and Loeb, Abraham and Shiokawa, Hotaka and Chael, Andrew A. and Doeleman, Sheperd S.},
eprint = {1505.07870},
file = {:home/mel/Documents/Papers/1505.07870v1.pdf:pdf},
month = {may},
pages = {8},
title = {{Measuring the Direction and Angular Velocity of a Black Hole Accretion Disk via Lagged Interferometric Covariance}},
url = {http://arxiv.org/abs/1505.07870},
year = {2015},
}
@article{Delvecchio2015,
abstract = {We study the relation of AGN accretion, star formation rate (SFR), and stellar mass (M{\$}{\_}*{\$}) using a sample of {\$}\backslashapprox{\$} 8600 star-forming galaxies up to z=2.5 selected with $\backslash$textit{\{}Herschel{\}} imaging in the GOODS and COSMOS fields. For each of them we derive SFR and M{\$}{\_}*{\$}, both corrected, when necessary, for emission from an active galactic nucleus (AGN), through the decomposition of their spectral energy distributions (SEDs). About 10 per cent of the sample are detected individually in $\backslash$textit{\{}Chandra{\}} observations of the fields. For the rest of the sample we stack the X-ray maps to get average X-ray properties. After subtracting the X-ray luminosity expected from star formation and correcting for nuclear obscuration, we derive the average AGN accretion rate for both detected sources and stacks, as a function of M{\$}{\_}{\{}*{\}}{\$}, SFR and redshift. The average accretion rate correlates with SFR and with M{\$}{\_}*{\$}. The dependence on SFR becomes progressively more significant at z{\$}>{\$}0.8. This may suggest that SFR is the original driver of these correlations. We find that average AGN accretion and star formation increase in a similar fashion with offset from the star-forming main-sequence. Our interpretation is that accretion onto the central black hole and star formation broadly trace each other, irrespective of whether the galaxy is evolving steadily on the main-sequence or bursting.},
archiveprefix = {arXiv},
arxivid = {1501.07602},
author = {Delvecchio, I. and Lutz, D. and Berta, S. and Rosario, D. J. and Zamorani, G. and Pozzi, F. and Gruppioni, C. and Vignali, C. and Brusa, M. and Cimatti, A. and Clements, D. L. and Cooray, A. and Farrah, D. and Lanzuisi, G. and Oliver, S. and Rodighiero, G. and Santini, P. and Symeonidis, M.},
eprint = {1501.07602},
file = {:home/mel/Documents/Papers/1501.07602v2.pdf:pdf},
month = {jan},
pages = {18},
title = {{Mapping the average AGN accretion rate in the SFR-M* plane for Herschel selected galaxies at 0<z<2.5}},
url = {http://arxiv.org/abs/1501.07602},
year = {2015},
}
@article{Athanassoula2015,
abstract = {Bars have a complex three-dimensional shape. In particular their inner part is vertically much thicker than the parts further out. Viewed edge-on, the thick part of the bar is what is commonly known as a boxy-, peanut- or X- bulge and viewed face-on it is referred to as a barlens. These components are due to disc and bar instabilities and are composed of disc material. I review here their formation, evolution and dynamics, using simulations, orbital structure theory and comparisons to observations.},
archiveprefix = {arXiv},
arxivid = {1503.04804},
author = {Athanassoula, E.},
eprint = {1503.04804},
file = {:home/mel/Documents/Papers/1503.04804v1.pdf:pdf},
month = {mar},
pages = {21},
title = {{Boxy/peanut/X bulges, barlenses and the thick part of galactic bars: What are they and how did they form?}},
url = {http://arxiv.org/abs/1503.04804},
year = {2015},
}
@article{Skelton2014,
annote = {3dhst specz and photoz},
author = {Skelton, Rosalind E. and Whitaker, Katherine E. and Momcheva, Ivelina G. and Brammer, Gabriel B. and van Dokkum, Pieter G. and Labb{\'{e}}, Ivo and Franx, Marijn and van der Wel, Arjen and Bezanson, Rachel and {Da Cunha}, Elisabete and Fumagalli, Mattia and {F{\"{o}}rster Schreiber}, Natascha and Kriek, Mariska and Leja, Joel and Lundgren, Britt F. and Magee, Daniel and Marchesini, Danilo and Maseda, Michael V. and Nelson, Erica J. and Oesch, Pascal and Pacifici, Camilla and Patel, Shannon G. and Price, Sedona and Rix, Hans-Walter and Tal, Tomer and Wake, David A. and Wuyts, Stijn},
doi = {10.1088/0067-0049/214/2/24},
file = {:home/mel/Documents/Papers/skelton.pdf:pdf},
issn = {1538-4365},
journal = {The Astrophysical Journal Supplement Series},
language = {en},
month = {oct},
number = {2},
pages = {24},
title = {{3D-HST WFC3-SELECTED PHOTOMETRIC CATALOGS IN THE FIVE CANDELS/3D-HST FIELDS: PHOTOMETRY, PHOTOMETRIC REDSHIFTS, AND STELLAR MASSES}},
url = {http://adslabs.org/adsabs/abs/2014ApJS..214...24S/},
volume = {214},
year = {2014},
}
@article{Zitrin2015,
abstract = {We report the discovery of Lyman-alpha emission (Ly{\$}\backslashalpha{\$}) in the bright galaxy EGSY-2008532660 (hereafter EGSY8p7) using the MOSFIRE spectrograph at the Keck Observatory. First reported by Roberts-Borsani et al. (2015), it was selected for spectroscopic observations because of its photometric redshift ({\$}z{\_}{\{}phot{\}}=8.57{\^{}}{\{}+0.22{\}}{\_}{\{}-0.43{\}}{\$}), apparent brightness (H{\$}{\_}{\{}160{\}}=25.26\backslashpm0.09{\$}) and red Spitzer/IRAC [3.6]-[4.5] color indicative of contamination by strong oxygen emission in the [4.5] band. With a total integration of {\$}\backslashsim{\$}4.3 hours, our data reveal an emission line at {\$}\backslashsimeq{\$}11776 {\{}$\backslash$AA{\}} which we argue is likely Ly{\$}\backslashalpha{\$} at a redshift {\$}z{\_}{\{}spec{\}}=8.683{\^{}}{\{}+0.001{\}}{\_}{\{}-0.004{\}}{\$}, in good agreement with the photometric estimate. The line was detected independently on two nights using different slit orientations and its detection significance is {\$}\backslashsim7.5\backslashsigma{\$}. An overlapping skyline contributes significantly to the uncertainty on the total line flux although the significance of the detected line is robust to a variety of skyline-masking procedures. By direct addition and a Gaussian fit, we estimate a 95$\backslash${\%} confidence range of 1.0--2.5{\$}\backslashtimes10{\^{}}{\{}-17{\}}{\$} erg s{\$}{\^{}}{\{}-1{\}}{\$} cm{\$}{\^{}}{\{}-2{\}}{\$}, corresponding to a rest-frame equivalent width of 17--42 {\{}$\backslash$AA{\}}. EGSY8p7 is the most distant galaxy confirmed spectroscopically to date, and the third luminous source in the EGS field beyond {\$}z{\_}{\{}phot{\}}\backslashgtrsim7.5{\$} with detectable Ly{\$}\backslashalpha{\$} emission viewed at a time when the intergalactic medium is believed to be fairly neutral. Although the reionization process was probably patchy, we discuss whether luminous sources with prominent IRAC color excesses may harbor harder ionizing spectra than the dominant fainter population thereby creating earlier ionized bubbles. Further spectroscopic follow-up of such bright sources promises important insight into the early formation of galaxies.},
archiveprefix = {arXiv},
arxivid = {1507.02679},
author = {Zitrin, Adi and Labbe, Ivo and Belli, Sirio and Bouwens, Rychard and Ellis, Richard S. and Roberts-Borsani, Guido and Stark, Daniel P. and Oesch, Pascal A. and Smit, Renske},
eprint = {1507.02679},
file = {:home/mel/Documents/Papers/1507.02679v3.pdf:pdf},
month = {jul},
pages = {7},
title = {{Lyman-alpha Emission from a Luminous z=8.68 Galaxy: Implications for Galaxies as Tracers of Cosmic Reionization}},
url = {http://arxiv.org/abs/1507.02679},
year = {2015},
}
@article{Momcheva2015,
abstract = {We present reduced data and data products from the 3D-HST survey, a 248-orbit HST Treasury program. The survey obtained WFC3 G141 grism spectroscopy in four of the five CANDELS fields: AEGIS, COSMOS, GOODS-S, and UDS, along with WFC3 {\$}H{\_}{\{}140{\}}{\$} imaging, parallel ACS G800L spectroscopy, and parallel {\$}I{\_}{\{}814{\}}{\$} imaging. In a previous paper (Skelton et al. 2014) we presented photometric catalogs in these four fields and in GOODS-N, the fifth CANDELS field. Here we describe and present the WFC3 G141 spectroscopic data, again augmented with data from GO-1600 in GOODS-N. The data analysis is complicated by the fact that no slits are used: all objects in the WFC3 field are dispersed, and many spectra overlap. We developed software to automatically and optimally extract interlaced 2D and 1D spectra for all objects in the Skelton et al. (2014) photometric catalogs. The 2D spectra and the multi-band photometry were fit simultaneously to determine redshifts and emission line strengths, taking the morphology of the galaxies explicitly into account. The resulting catalog has 98,663 measured redshifts and line strengths down to {\$}JH{\_}{\{}IR{\}}\backslashleq 26{\$} and 22,548 with {\$}JH{\_}{\{}IR{\}}\backslashleq 24{\$}, where we comfortably detect continuum emission. Of this sample 5,459 galaxies are at {\$}z>1.5{\$} and 9,621 are at {\$}0.7<z<1.5{\$}, where H{\$}\backslashalpha{\$} falls in the G141 wavelength coverage. Based on comparisons with ground-based spectroscopic redshifts, and on analyses of paired galaxies and repeat observations, the typical redshift error for {\$}JH{\_}{\{}IR{\}}\backslashleq 24{\$} galaxies in our catalog is {\$}\backslashsigma{\_}z \backslashapprox 0.003 \backslashtimes (1+z){\$}, i.e., one native WFC3 pixel. The {\$}3\backslashsigma{\$} limit for emission line fluxes of point sources is {\$}1.5\backslashtimes10{\^{}}{\{}-17{\}}{\$} ergs s{\$}{\^{}}{\{}-1{\}}{\$} cm{\$}{\^{}}{\{}-2{\}}{\$}. We show various representations of the full dataset, as well as individual examples that highlight the range of spectra that we find in the survey.},
annote = {3dHST spec, grism, and photozs},
archiveprefix = {arXiv},
arxivid = {1510.02106},
author = {Momcheva, Ivelina G. and Brammer, Gabriel B. and van Dokkum, Pieter G. and Skelton, Rosalind E. and Whitaker, Katherine E. and Nelson, Erica J. and Fumagalli, Mattia and Maseda, Michael V. and Leja, Joel and Franx, Marijn and Rix, Hans-Walter and Bezanson, Rachel and {Da Cunha}, Elisabete and Dickey, Claire and Schreiber, Natascha M. F{\"{o}}rster and Illingworth, Garth and Kriek, Mariska and Labb{\'{e}}, Ivo and Lange, Johannes Ulf and Lundgren, Britt F. and Magee, Daniel and Marchesini, Danilo and Oesch, Pascal and Pacifici, Camilla and Patel, Shannon G. and Price, Sedona and Tal, Tomer and Wake, David A. and van der Wel, Arjen and Wuyts, Stijn},
eprint = {1510.02106},
file = {:home/mel/Documents/Papers/1510.02106v1.pdf:pdf},
month = {oct},
title = {{The 3D-HST Survey: Hubble Space Telescope WFC3/G141 grism spectra, redshifts, and emission line measurements for {\$}\backslashsim 100,000{\$} galaxies}},
url = {http://arxiv.org/abs/1510.02106},
year = {2015},
}
@article{Buta2013,
abstract = {Galaxy morphology has many structures that are suggestive of various processes or stages of secular evolution. Internal perturbations such as bars can drive secular evolution through gravity torques that move gas into the central regions and build up a flattened, disk-like central bulge, or which may convert an open spiral pseudoring into a more closed ring. Interaction between individual components of a galaxy, such as between a bar and a dark halo, a bar and a central mass concentration, or between a perturbation and the basic state of a stellar disk, can also drive secular transformations. In this series of lectures, I review many aspects of galaxy morphology with a view to delineating some of the possible evolutionary pathways between different galaxy types.},
archiveprefix = {arXiv},
arxivid = {1304.3529},
author = {Buta, Ronald J.},
eprint = {1304.3529},
file = {:home/mel/Documents/Papers/1304.3529.pdf:pdf},
month = {apr},
pages = {106},
title = {{Galaxy Morphology}},
url = {http://arxiv.org/abs/1304.3529},
year = {2013},
}
@article{Ilbert2009,
annote = {COSMOS photozs},
author = {Ilbert, O. and Capak, P. and Salvato, M. and Aussel, H. and McCracken, H. J. and Sanders, D. B. and Scoville, N. and Kartaltepe, J. and Arnouts, S. and Floc'h, E. Le and Mobasher, B. and Taniguchi, Y. and Lamareille, F. and Leauthaud, A. and Sasaki, S. and Thompson, D. and Zamojski, M. and Zamorani, G. and Bardelli, S. and Bolzonella, M. and Bongiorno, A. and Brusa, M. and Caputi, K. I. and Carollo, C. M. and Contini, T. and Cook, R. and Coppa, G. and Cucciati, O. and de la Torre, S. and de Ravel, L. and Franzetti, P. and Garilli, B. and Hasinger, G. and Iovino, A. and Kampczyk, P. and Kneib, J.-P. and Knobel, C. and Kovac, K. and {Le Borgne}, J. F. and {Le Brun}, V. and F{\`{e}}vre, O. Le and Lilly, S. and Looper, D. and Maier, C. and Mainieri, V. and Mellier, Y. and Mignoli, M. and Murayama, T. and Pell{\`{o}}, R. and Peng, Y. and P{\'{e}}rez-Montero, E. and Renzini, A. and Ricciardelli, E. and Schiminovich, D. and Scodeggio, M. and Shioya, Y. and Silverman, J. and Surace, J. and Tanaka, M. and Tasca, L. and Tresse, L. and Vergani, D. and Zucca, E.},
doi = {10.1088/0004-637X/690/2/1236},
file = {:home/mel/Documents/Papers/cosmosphotoz.pdf:pdf},
issn = {0004-637X},
journal = {The Astrophysical Journal},
language = {en},
month = {jan},
number = {2},
pages = {1236--1249},
title = {{COSMOS PHOTOMETRIC REDSHIFTS WITH 30-BANDS FOR 2-deg 2}},
url = {http://adslabs.org/adsabs/abs/2009ApJ...690.1236I/},
volume = {690},
year = {2009},
}
@article{PlanckCollaboration2013,
abstract = {We present the first results based on Planck measurements of the CMB temperature and lensing-potential power spectra. The Planck spectra at high multipoles are extremely well described by the standard spatially-flat six-parameter LCDM cosmology. In this model Planck data determine the cosmological parameters to high precision. We find a low value of the Hubble constant, H0=67.3+/-1.2 km/s/Mpc and a high value of the matter density parameter, Omega{\_}m=0.315+/-0.017 (+/-1 sigma errors) in excellent agreement with constraints from baryon acoustic oscillation (BAO) surveys. Including curvature, we find that the Universe is consistent with spatial flatness to percent-level precision using Planck CMB data alone. We present results from an analysis of extensions to the standard cosmology, using astrophysical data sets in addition to Planck and high-resolution CMB data. None of these models are favoured significantly over standard LCDM. The deviation of the scalar spectral index from unity is insensitive to the addition of tensor modes and to changes in the matter content of the Universe. We find a 95{\%} upper limit of r<0.11 on the tensor-to-scalar ratio. There is no evidence for additional neutrino-like relativistic particles. Using BAO and CMB data, we find N{\_}eff=3.30+/-0.27 for the effective number of relativistic degrees of freedom, and an upper limit of 0.23 eV for the summed neutrino mass. Our results are in excellent agreement with big bang nucleosynthesis and the standard value of N{\_}eff=3.046. We find no evidence for dynamical dark energy. Despite the success of the standard LCDM model, this cosmology does not provide a good fit to the CMB power spectrum at low multipoles, as noted previously by the WMAP team. While not of decisive significance, this is an anomaly in an otherwise self-consistent analysis of the Planck temperature data.},
archiveprefix = {arXiv},
arxivid = {1303.5076},
author = {{Planck Collaboration} and Ade, P. A. R. and Aghanim, N. and Armitage-Caplan, C. and Arnaud, M. and Ashdown, M. and Atrio-Barandela, F. and Aumont, J. and Baccigalupi, C. and Banday, A. J. and Barreiro, R. B. and Bartlett, J. G. and Battaner, E. and Benabed, K. and Beno{\^{\i}}t, A. and Benoit-L{\'{e}}vy, A. and Bernard, J. -P. and Bersanelli, M. and Bielewicz, P. and Bobin, J. and Bock, J. J. and Bonaldi, A. and Bond, J. R. and Borrill, J. and Bouchet, F. R. and Bridges, M. and Bucher, M. and Burigana, C. and Butler, R. C. and Calabrese, E. and Cappellini, B. and Cardoso, J. -F. and Catalano, A. and Challinor, A. and Chamballu, A. and Chary, R. -R. and Chen, X. and Chiang, H. C. and Chiang, L. -Y and Christensen, P. R. and Church, S. and Clements, D. L. and Colombi, S. and Colombo, L. P. L. and Couchot, F. and Coulais, A. and Crill, B. P. and Curto, A. and Cuttaia, F. and Danese, L. and Davies, R. D. and Davis, R. J. and de Bernardis, P. and de Rosa, A. and de Zotti, G. and Delabrouille, J. and Delouis, J. -M. and D{\'{e}}sert, F. -X. and Dickinson, C. and Diego, J. M. and Dolag, K. and Dole, H. and Donzelli, S. and Dor{\'{e}}, O. and Douspis, M. and Dunkley, J. and Dupac, X. and Efstathiou, G. and Elsner, F. and En{\ss}lin, T. A. and Eriksen, H. K. and Finelli, F. and Forni, O. and Frailis, M. and Fraisse, A. A. and Franceschi, E. and Gaier, T. C. and Galeotta, S. and Galli, S. and Ganga, K. and Giard, M. and Giardino, G. and Giraud-H{\'{e}}raud, Y. and Gjerl{\o}w, E. and Gonz{\'{a}}lez-Nuevo, J. and G{\'{o}}rski, K. M. and Gratton, S. and Gregorio, A. and Gruppuso, A. and Gudmundsson, J. E. and Haissinski, J. and Hamann, J. and Hansen, F. K. and Hanson, D. and Harrison, D. and Henrot-Versill{\'{e}}, S. and Hern{\'{a}}ndez-Monteagudo, C. and Herranz, D. and Hildebrandt, S. R. and Hivon, E. and Hobson, M. and Holmes, W. A. and Hornstrup, A. and Hou, Z. and Hovest, W. and Huffenberger, K. M. and Jaffe, A. H. and Jaffe, T. R. and Jewell, J. and Jones, W. C. and Juvela, M. and Keih{\"{a}}nen, E. and Keskitalo, R. and Kisner, T. S. and Kneissl, R. and Knoche, J. and Knox, L. and Kunz, M. and Kurki-Suonio, H. and Lagache, G. and L{\"{a}}hteenm{\"{a}}ki, A. and Lamarre, J. -M. and Lasenby, A. and Lattanzi, M. and Laureijs, R. J. and Lawrence, C. R. and Leach, S. and Leahy, J. P. and Leonardi, R. and Le{\'{o}}n-Tavares, J. and Lesgourgues, J. and Lewis, A. and Liguori, M. and Lilje, P. B. and Linden-V{\o}rnle, M. and L{\'{o}}pez-Caniego, M. and Lubin, P. M. and Mac{\'{\i}}as-P{\'{e}}rez, J. F. and Maffei, B. and Maino, D. and Mandolesi, N. and Maris, M. and Marshall, D. J. and Martin, P. G. and Mart{\'{\i}}nez-Gonz{\'{a}}lez, E. and Masi, S. and Massardi, M. and Matarrese, S. and Matthai, F. and Mazzotta, P. and Meinhold, P. R. and Melchiorri, A. and Melin, J. -B. and Mendes, L. and Menegoni, E. and Mennella, A. and Migliaccio, M. and Millea, M. and Mitra, S. and Miville-Desch{\^{e}}nes, M. -A. and Moneti, A. and Montier, L. and Morgante, G. and Mortlock, D. and Moss, A. and Munshi, D. and Murphy, J. A. and Naselsky, P. and Nati, F. and Natoli, P. and Netterfield, C. B. and N{\o}rgaard-Nielsen, H. U. and Noviello, F. and Novikov, D. and Novikov, I. and O'Dwyer, I. J. and Osborne, S. and Oxborrow, C. A. and Paci, F. and Pagano, L. and Pajot, F. and Paoletti, D. and Partridge, B. and Pasian, F. and Patanchon, G. and Pearson, D. and Pearson, T. J. and Peiris, H. V. and Perdereau, O. and Perotto, L. and Perrotta, F. and Pettorino, V. and Piacentini, F. and Piat, M. and Pierpaoli, E. and Pietrobon, D. and Plaszczynski, S. and Platania, P. and Pointecouteau, E. and Polenta, G. and Ponthieu, N. and Popa, L. and Poutanen, T. and Pratt, G. W. and Pr{\'{e}}zeau, G. and Prunet, S. and Puget, J. -L. and Rachen, J. P. and Reach, W. T. and Rebolo, R. and Reinecke, M. and Remazeilles, M. and Renault, C. and Ricciardi, S. and Riller, T. and Ristorcelli, I. and Rocha, G. and Rosset, C. and Roudier, G. and Rowan-Robinson, M. and Rubi{\~{n}}o-Mart{\'{\i}}n, J. A. and Rusholme, B. and Sandri, M. and Santos, D. and Savelainen, M. and Savini, G. and Scott, D. and Seiffert, M. D. and Shellard, E. P. S. and Spencer, L. D. and Starck, J. -L. and Stolyarov, V. and Stompor, R. and Sudiwala, R. and Sunyaev, R. and Sureau, F. and Sutton, D. and Suur-Uski, A. -S. and Sygnet, J. -F. and Tauber, J. A. and Tavagnacco, D. and Terenzi, L. and Toffolatti, L. and Tomasi, M. and Tristram, M. and Tucci, M. and Tuovinen, J. and T{\"{u}}rler, M. and Umana, G. and Valenziano, L. and Valiviita, J. and {Van Tent}, B. and Vielva, P. and Villa, F. and Vittorio, N. and Wade, L. A. and Wandelt, B. D. and Wehus, I. K. and White, M. and White, S. D. M. and Wilkinson, A. and Yvon, D. and Zacchei, A. and Zonca, A.},
eprint = {1303.5076},
file = {:home/mel/Documents/Papers/1303.5076v3.pdf:pdf},
month = {mar},
pages = {69},
title = {{Planck 2013 results. XVI. Cosmological parameters}},
url = {http://arxiv.org/abs/1303.5076},
year = {2013},
}
@article{Ilbert2013,
abstract = {We estimate the galaxy stellar mass function and stellar mass density for star-forming and quiescent galaxies with 0.2<z<4. We construct a deep K<24 sample of 220000 galaxies selected using the UltraVISTA DR1 data release. Our analysis is based on precise 30-band photometric redshifts. By comparing these photometric redshifts with 10800 spectroscopic redshifts from the zCOSMOS bright and faint surveys, we find a precision of sigma(dz/(1+z))=0.008 at i<22.5 and sigma(dz/(1+zs))=0.03 at 1.5<z<4. We derive the stellar mass function and correct for the Eddington bias. We find a mass-dependent evolution of the global and star-forming populations. This mass-dependent evolution is a direct consequence of the star formation being quenched in galaxies more massive than M>10{\^{}}10.7Msun. For the mass function of the quiescent galaxies, we do not find any significant evolution of the high-mass end at z<1; however we observe a clear flattening of the faint-end slope. From z{\~{}}3 to z{\~{}}1, the density of quiescent galaxies increases over the entire mass range. Their comoving stellar mass density increases by 1.6 dex between z{\~{}}3 and z{\~{}}1 and by less than 0.2dex at z<1. We infer the star formation history from the mass density evolution and we find an excellent agreement with instantaneous star formation rate measurements at z<1.5, while we find differences of 0.2dex at z>1.5 consistent with the expected uncertainties. We also develop a new method to infer the specific star formation rate from the mass function of star-forming galaxies. We find that the specific star formation rate of 10{\^{}}10Msun galaxies increases continuously in the redshift range 1<z<4. Finally, we compare our results with a semi-analytical model and find that these models overestimate the density of low mass quiescent galaxies by an order of magnitude, while the density of low-mass star-forming galaxies is successfully reproduced.},
annote = {UltraVISTA photozs},
archiveprefix = {arXiv},
arxivid = {1301.3157},
author = {Ilbert, O. and McCracken, H. J. and {Le F{\`{e}}vre}, O. and Capak, P. and Dunlop, J. and Karim, A. and Renzini, M. A. and Caputi, K. and Boissier, S. and Arnouts, S. and Aussel, H. and Comparat, J. and Guo, Q. and Hudelot, P. and Kartaltepe, J. and Kneib, J. P. and Krogager, J. K. and {Le Floc’h}, E. and Lilly, S. and Mellier, Y. and Milvang-Jensen, B. and Moutard, T. and Onodera, M. and Richard, J. and Salvato, M. and Sanders, D. B. and Scoville, N. and Silverman, J. D. and Taniguchi, Y. and Tasca, L. and Thomas, R. and Toft, S. and Tresse, L. and Vergani, D. and Wolk, M. and Zirm, A.},
doi = {10.1051/0004-6361/201321100},
eprint = {1301.3157},
file = {:home/mel/.local/share/data/Mendeley Ltd./Mendeley Desktop/Downloaded/Ilbert et al. - 2013 - Mass assembly in quiescent and star-forming galaxies since z ≃ 4 from UltraVISTA.pdf:pdf},
issn = {0004-6361},
journal = {Astronomy {\&} Astrophysics},
month = {jul},
pages = {A55},
title = {{Mass assembly in quiescent and star-forming galaxies since z ≃ 4 from UltraVISTA}},
url = {http://arxiv.org/abs/1301.3157},
volume = {556},
year = {2013},
}
@article{Peng_2002,
doi = {10.1086/340952},
url = {http://dx.doi.org/10.1086/340952},
year = {2002},
month = {jul},
publisher = {{IOP} Publishing},
volume = {124},
number = {1},
pages = {266--293},
author = {Chien Y. Peng and Luis C. Ho and Chris D. Impey and Hans-Walter Rix},
title = {{Detailed Structural Decomposition of Galaxy Images}},
journal = {The Astronomical Journal},
}
@article{Peng_2010,
doi = {10.1088/0004-6256/139/6/2097},
url = {http://dx.doi.org/10.1088/0004-6256/139/6/2097},
year = {2010},
month = {apr},
publisher = {{IOP} Publishing},
volume = {139},
number = {6},
pages = {2097--2129},
author = {Chien Y. Peng and Luis C. Ho and Chris D. Impey and Hans-Walter Rix},
title = {{{DETAILED} {DECOMPOSITION} {OF} {GALAXY} {IMAGES}. {II}. {BEYOND} {AXISYMMETRIC} {MODELS}}},
journal = {The Astronomical Journal},
}
@article{Holincheck_2016,
doi = {10.1093/mnras/stw649},
url = {http://dx.doi.org/10.1093/mnras/stw649},
year = {2016},
month = {mar},
publisher = {Oxford University Press ({OUP})},
pages = {stw649},
author = {Anthony J. Holincheck and John F. Wallin and Kirk Borne and Lucy Fortson and Chris Lintott and Arfon M. Smith and Steven Bamford and William C. Keel and Michael Parrish},
title = {{Galaxy Zoo: Mergers - Dynamical Models of Interacting Galaxies}},
journal = {Mon. Not. R. Astron. Soc.},
}
@data{Kapadia_2015,
doi = {10.5281/zenodo.16707},
url = {http://dx.doi.org/10.5281/zenodo.16707},
author = {Amit Kapadia},
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