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\title{arXiv Astrophysics Digest, 2015-07-20}


\author{arXiv Astrophysics Journal Club}
\affil{Affiliation not available}



\date{\today}

\maketitle

\selectlanguage{english}
\begin{abstract}
A Day of Science Preprints%
\end{abstract}%



\sectionhack

\textbf{\huge New submissions} 

\section{Some properties of convection in hybrid stars}
\textit{Yudin, A. V.} ; \textit{Hempel, M.}; \textit{Nadyozhin, D. K.}; \textit{Razinkova, T. L.}\\%
Comment: 11 pages, 3 figures\\%
Subjects: \textbf{Astrophysics - Solar and Stellar Astrophysics}; Astrophysics - High Energy Astrophysical Phenomena; Nuclear Theory\\%
Source: \href{http://arxiv.org/abs/1507.04598}{arXiv:1507.04598} [\href{http://arxiv.org/pdf/1507.04598.pdf}{PDF}]\\%


It is shown that the unusual thermodynamic properties of matter within the
region of two-phase coexistence in hybrid stars result in a change of the
standard condition for beginning of convection. In particular, the thermal flux
transported by convection may be directed towards the stellar center. We
discuss favorable circumstances leading to such an effect of "inverse
convection" and its possible influence on the thermal evolution of hybrid
stars.


\section{Dark Matter Velocity Spectroscopy}
\textit{Speckhard, Eric G.} ; \textit{Ng, Kenny C. Y.}; \textit{Beacom, John F.}; \textit{Laha, Ranjan}\\%
Comment: 5 pages, 3 figures, comments are welcome\\%
Subjects: \textbf{Astrophysics - Cosmology and Nongalactic Astrophysics}; Astrophysics - High Energy Astrophysical Phenomena\\%
Source: \href{http://arxiv.org/abs/1507.04744}{arXiv:1507.04744} [\href{http://arxiv.org/pdf/1507.04744.pdf}{PDF}]\\%


Dark matter decays or annihilations that produce line-like spectra may be
smoking-gun signals. However, even such distinctive signatures can be mimicked
by astrophysical or instrumental causes. We show that velocity spectroscopy-the
measurement of energy shifts induced by relative motion of source and
observer-can separate these three causes with minimal theoretical
uncertainties. The principal obstacle has been energy resolution, but upcoming
and proposed experiments will make significant improvements. As an example, we
show that the imminent Astro-H mission can use Milky Way observations to
separate possible causes of the 3.5-keV line. We discuss other applications.


\section{From Discs to Bulges: effect of mergers on the morphology of galaxies}
\textit{Kannan, Rahul} ; \textit{Maccio', Andrea V.}; \textit{Fontanot, Fabio}; \textit{Moster, Benjamin P.}; \textit{Karman, Wouter}; \textit{Somerville, Rachel S.}\\%
Comment: MNRAS Accepted, 17 pages, 11 figures, 3 Tables\\%
Subjects: \textbf{Astrophysics - Astrophysics of Galaxies}\\%
Source: \href{http://arxiv.org/abs/1507.04746}{arXiv:1507.04746} [\href{http://arxiv.org/pdf/1507.04746.pdf}{PDF}]\\%


We study the effect of mergers on the morphology of galaxies by means of the
simulated merger tree approach first proposed by Moster et al. This method
combines N-body cosmological simulations and semi-analytic techniques to
extract realistic initial conditions for galaxy mergers. These are then evolved
using high resolution hydrodynamical simulations, which include dark matter,
stars, cold gas in the disc and hot gas in the halo. We show that the satellite
mass accretion is not as effective as previously thought, as there is
substantial stellar stripping before the final merger. The fraction of stellar
disc mass transferred to the bulge is quite low, even in the case of a major
merger, mainly due to the dispersion of part of the stellar disc mass into the
halo. We confirm the findings of Hopkins et al., that a gas rich disc is able
to survive major mergers more efficiently. The enhanced star formation
associated with the merger is not localised to the bulge of galaxy, but a
substantial fraction takes place in the disc too. The inclusion of the hot gas
reservoir in the galaxy model contributes to reducing the efficiency of bulge
formation. Overall, our findings suggest that mergers are not as efficient as
previously thought in transforming discs into bulges. This possibly alleviates
some of the tensions between observations of bulgeless galaxies and the
hierarchical scenario for structure formation.


\section{On the dependence of galaxy morphologies on galaxy mergers}
\textit{Fontanot, Fabio} ; \textit{Maccio', Andrea V.}; \textit{Hirschmann, Michaela}; \textit{De Lucia, Gabriella}; \textit{Kannan, Rahul}; \textit{Somerville, Rachel S.}; \textit{Wilman, Dave}\\%
Comment: MNRAS in press, 11 pages, 5 figures\\%
Subjects: \textbf{Astrophysics - Astrophysics of Galaxies}\\%
Source: \href{http://arxiv.org/abs/1507.04748}{arXiv:1507.04748} [\href{http://arxiv.org/pdf/1507.04748.pdf}{PDF}]\\%


The distribution of galaxy morphological types is a key test for models of
galaxy formation and evolution, providing strong constraints on the relative
contribution of different physical processes responsible for the growth of the
spheroidal components. In this paper, we make use of a suite of semi-analytic
models to study the efficiency of galaxy mergers in disrupting galaxy discs and
building galaxy bulges. In particular, we compare standard prescriptions
usually adopted in semi-analytic models, with new prescriptions proposed by
Kannan et al., based on results from high-resolution hydrodynamical
simulations, and we show that these new implementations reduce the efficiency
of bulge formation through mergers. In addition, we compare our model results
with a variety of observational measurements of the fraction of
spheroid-dominated galaxies as a function of stellar and halo mass, showing
that the present uncertainties in the data represent an important limitation to
our understanding of spheroid formation. Our results indicate that the main
tension between theoretical models and observations does not stem from the
survival of purely disc structures (i.e. bulgeless galaxies), rather from the
distribution of galaxies of different morphological types, as a function of
their stellar mass.


\section{The Observed Distribution of Spectroscopic Binaries from the
Anglo-Australian Planet Search}
\textit{Jenkins, James S.} ; \selectlanguage{ngerman}\textit{Díaz, Matias}; \textit{Jones, Hugh R. A.}; \textit{Butler, Paul R.}; \textit{Tinney, Chris G.}; \textit{O'Toole, Simon J.}; \textit{Carter, Brad D.}; \textit{Wittenmyer, Robert A.}; \textit{Pinfield, David J.}\\%
Comment: 42 pages, 11 figures, and 3 tables. Accepted for publication in MNRAS\\%
Subjects: \textbf{Astrophysics - Solar and Stellar Astrophysics}; Astrophysics - Earth and Planetary Astrophysics\\%
Source: \href{http://arxiv.org/abs/1507.04749}{arXiv:1507.04749} [\href{http://arxiv.org/pdf/1507.04749.pdf}{PDF}]\\%


We report the detection of sixteen binary systems from the Anglo-Australian
Planet Search. Solutions to the radial velocity data indicate that the stars
have companions orbiting with a wide range of masses, eccentricities and
periods. Three of the systems potentially contain brown-dwarf companions while
another two have eccentricities that place them in the extreme upper tail of
the eccentricity distribution for binaries with periods less than 1000 d. For
periods up to 12 years, the distribution of our stellar companion masses is
fairly flat, mirroring that seen in other radial velocity surveys, and
contrasts sharply with the current distribution of candidate planetary masses,
which rises strongly below 10MJ. When looking at a larger sample of binaries
that have FGK star primaries as a function of the primary star metallicity, we
find that the distribution maintains a binary fraction of ~43$\pm$4\% between
-1.0 to +0.6 dex in metallicity. This is in stark contrast to the giant
exoplanet distribution. This result is in good agreement with binary formation
models that invoke fragmentation of a collapsing giant molecular cloud,
suggesting this is the dominant formation mechanism for close binaries and not
fragmentation of the primary star's remnant proto-planetary disk.


\section{Accurate PSF-matched photometry and photometric redshifts for the
Extreme Deep Field with the Chebyshev-Fourier functions}
\selectlanguage{ngerman}\textit{Jiménez-Teja, Y.} ; \textit{Benítez, N.}; \textit{Molino, A.}; \textit{Fernandes, C. A. C.}\\%
Comment: 12 pages, 12 figures, submitted to MNRAS 2014 July 10, accepted 2015
July 15\\%
Subjects: \textbf{Astrophysics - Astrophysics of Galaxies}\\%
Source: \href{http://arxiv.org/abs/1507.04750}{arXiv:1507.04750} [\href{http://arxiv.org/pdf/1507.04750.pdf}{PDF}]\\%


Photometric redshifts, which have become the cornerstone of several of the
largest astronomical surveys like PanStarrs, DES, J-PAS or the LSST, require
precise measurements of galaxy photometry in different bands using a consistent
physical aperture. This is not trivial, due to the variation in the shape and
width of the Point Spread Function (PSF) introduced by wavelength differences,
instrument positions and atmospheric conditions. Current methods to correct for
this effect rely on a detailed knowledge of the PSF characteristics as a
function of the survey coordinates, which can be difficult due to the relative
paucity of stars tracking the PSF behaviour. Here we show that it is possible
to measure accurate, consistent multicolour photometry without knowing the
shape of PSF. The Chebyshev-Fourier Functions (CHEFs) can fit the observed
profile of each object and produce high signal-to-noise integrated flux
measurements unaffected by the PSF. These total fluxes, which encompass all the
galaxy populations, are much more useful for Galaxy Evolution studies than
aperture photometry. We compare the total magnitudes and colours obtained using
our software to traditional photometry with SExtractor, using real data from
the COSMOS survey and the Hubble Ultra Deep Field. We also apply the CHEFs
technique to the recently published Extreme Deep Field and compare the results
to those from ColorPro on the HUDF. We produce a photometric catalogue with
35732 sources (10823 with S/N>5), reaching a photometric redshift precision of
2\% due to the extraordinary depth and wavelength coverage of the XDF images.


\section{Mercury-T: A new code to study tidally evolving multi-planet systems.
Applications to Kepler-62}
\textit{Bolmont, Emeline} ; \textit{Raymond, Sean N.}; \textit{Leconte, Jeremy}; \textit{Hersant, Franck}; \textit{Correia, Alexandre C. M.}\\%
Comment: Accepted to A\&A 15 pages, 13 figures\\%
Subjects: \textbf{Astrophysics - Earth and Planetary Astrophysics}\\%
Source: \href{http://arxiv.org/abs/1507.04751}{arXiv:1507.04751} [\href{http://arxiv.org/pdf/1507.04751.pdf}{PDF}]\\%


A large proportion of observed planetary systems contain several planets in a
compact orbital configuration, and often harbor at least one close-in object.
These systems are then most likely tidally evolving. We investigate how the
effects of planet-planet interactions influence the tidal evolution of planets.
We introduce for that purpose a new open-source addition to the Mercury
N-body code, Mercury-T, which takes into account tides, general relativity and
the effect of rotation-induced flattening in order to simulate the dynamical
and tidal evolution of multi-planet systems. It uses a standard equilibrium
tidal model, the constant time lag model. Besides, the evolution of the radius
of several host bodies has been implemented (brown dwarfs, M-dwarfs of mass
$0.1~M_\odot$, Sun-like stars, Jupiter). We validate the new code by comparing
its output for one-planet systems to the secular equations results. We find
that this code does respect the conservation of total angular momentum.
We applied this new tool to the planetary system Kepler-62. We find that
tides influence the stability of the system in some cases. We also show that
while the four inner planets of the systems are likely to have slow rotation
rates and small obliquities, the fifth planet could have a fast rotation rate
and a high obliquity. This means that the two habitable zone planets of this
system, Kepler-62e ad f are likely to have very different climate features, and
this of course would influence their potential at hosting surface liquid water.


\section{The Stripe 82 Massive Galaxy Project II: Stellar Mass Completeness of
Spectroscopic Galaxy Samples from the Baryon Oscillation Spectroscopic Survey}
\textit{Leauthaud, Alexie} ; \textit{Bundy, Kevin}; \textit{Saito, Shun}; \textit{Tinker, Jeremy}; \textit{Maraston, Claudia}; \textit{Tojeiro, Rita}; \textit{Huang, Song}; \textit{Brownstein, Joel R.}; \textit{Schneider, Donald P.}; \textit{Thomas, Daniel}\\%
Comment: 18 pages, 17 figures, 5 tables\\%
Subjects: \textbf{Astrophysics - Astrophysics of Galaxies}; Astrophysics - Cosmology and Nongalactic Astrophysics\\%
Source: \href{http://arxiv.org/abs/1507.04752}{arXiv:1507.04752} [\href{http://arxiv.org/pdf/1507.04752.pdf}{PDF}]\\%


The Baryon Oscillation Spectroscopic Survey (BOSS) has collected spectra for
over one million galaxies at $0.15<z<0.7$ over a volume of 15.3 Gpc$^3$ (9,376
deg$^2$) -- providing us an opportunity to study the most massive galaxy
populations with vanishing sample variance. However, BOSS samples are selected
via complex color cuts that are optimized for cosmology studies, not galaxy
science. In this paper, we supplement BOSS samples with photometric redshifts
from the Stripe 82 Massive Galaxy Catalog and measure the total galaxy stellar
mass function (SMF) at $z\sim0.3$ and $z\sim0.55$. With the total SMF in hand,
we characterize the stellar mass completeness of BOSS samples. The
high-redshift CMASS ("constant mass") sample is significantly impacted by mass
incompleteness and is 80\% complete at $\log_{10}(M_*/M_{\odot}) >11.6$ only in
the narrow redshift range $z=[0.51,0.61]$. The low redshift LOWZ sample is 80\%
complete at $\log_{10}(M_*/M_{\odot}) >11.6$ for $z=[0.15,0.43]$. To construct
mass complete samples at lower masses, spectroscopic samples need to be
significantly supplemented by photometric redshifts. This work will enable
future studies to better utilize the BOSS samples for galaxy-formation science.


\section{Halo Profile Evolution and Velocity Bias}
\textit{Chan, Kwan Chuen} Comment: 20 pages, 15 figures\\%
Subjects: \textbf{Astrophysics - Cosmology and Nongalactic Astrophysics}\\%
Source: \href{http://arxiv.org/abs/1507.04753}{arXiv:1507.04753} [\href{http://arxiv.org/pdf/1507.04753.pdf}{PDF}]\\%


We propose a simple model that elucidates the generation of halo velocity
bias. The fluid equation approximation is often adopted in modelling the
evolution of the halo density field. In this approach, halos are often taken to
be point particles even though in reality they are finite-sized objects. In
this paper, we generalize the fluid equation approximation to halos to include
the finite extent of halos by taking into account the halo profile. We compute
the perturbation of the halo density and velocity field to second order and
find that the profile correction gives rise to $k^2$ correction terms in
Fourier space. These corrections are more important for velocity than for
density. In particular, the profile correction generates $k^2$ correction term
in the velocity bias and the correction terms do not decay away in the long
term limit, but it is not constant. We model the halo profile evolution using
the spherical collapse model. We also measure the evolution of proto-halo
profile at various redshifts numerically. We find that the spherical collapse
model gives a reasonable description of the numerical profile evolution. Static
halo profile is often adopted in modelling halos in theories such as the
excursion set theory. Our work highlights the importance of including the
profile evolution in the calculations.


\section{Tracing the Ingredients for a Habitable Earth from Interstellar Space
through Planet Formation}
\textit{Bergin, Edwin A.} ; \textit{Blake, Geoffrey A.}; \textit{Ciesla, Fred}; \textit{Hirschmann, Marc M.}; \textit{Li, Jie}\\%
Comment: Accepted by PNAS per
http://www.pnas.org/content/early/2015/07/01/1500954112.abstract?sid=9fd8abea-9d33-46d8-b755-217d10b1c24b\\%
Subjects: \textbf{Astrophysics - Earth and Planetary Astrophysics}\\%
Source: \href{http://arxiv.org/abs/1507.04756}{arXiv:1507.04756} [\href{http://arxiv.org/pdf/1507.04756.pdf}{PDF}]\\%


We use the C/N ratio as a monitor of the delivery of key ingredients of life
to nascent terrestrial worlds. Total elemental C and N contents, and their
ratio, are examined for the interstellar medium, comets, chondritic meteorites
and terrestrial planets; we include an updated estimate for the Bulk Silicate
Earth (C/N = 49.0 +/- 9.3). Using a kinetic model of disk chemistry, and the
sublimation/condensation temperatures of primitive molecules, we suggest that
organic ices and macro-molecular (refractory or carbonaceous dust) organic
material are the likely initial C and N carriers. Chemical reactions in the
disk can produce nebular C/N ratios of ~1-12, comparable to those of comets and
the low end estimated for planetesimals. An increase of the C/N ratio is traced
between volatile-rich pristine bodies and larger volatile-depleted objects
subjected to thermal/accretional metamorphism. The C/N ratios of the dominant
materials accreted to terrestrial planets should therefore be higher than those
seen in carbonaceous chondrites or comets. During planetary formation, we
explore scenarios leading to further volatile loss and associated C/N
variations owing to core formation and atmospheric escape. Key processes
include relative enrichment of nitrogen in the atmosphere and preferential
sequestration of carbon by the core. The high C/N BSE ratio therefore is best
satisfied by accretion of thermally processed objects followed by large-scale
atmospheric loss. These two effects must be more profound if volatile
sequestration in the core is effective. The stochastic nature of these
processes hints that the surface/atmospheric abundances of biosphere-essential
materials will likely be variable.


\section{Observations of Solids in Protoplanetary Disks}
\textit{Andrews, Sean M.} Comment: invited pedagogical review for PASP (appearing in October issue); 29
pages, 20 figures\\%
Subjects: \textbf{Astrophysics - Solar and Stellar Astrophysics}; Astrophysics - Earth and Planetary Astrophysics\\%
Source: \href{http://arxiv.org/abs/1507.04758}{arXiv:1507.04758} [\href{http://arxiv.org/pdf/1507.04758.pdf}{PDF}]\\%


This review addresses the state of research that employs astronomical (remote
sensing) observations of solids ("dust") in young circumstellar disks to learn
about planet formation. The intention is for it to serve as an accessible,
introductory, pedagogical resource for junior scientists interested in the
subject. After some historical background and a basic observational primer, the
focus is shifted to the three fundamental topics that broadly define the field:
(1) demographics -- the relationships between disk properties and the
characteristics of their environments and hosts; (2) structure -- the spatial
distribution of disk material and its associated physical conditions and
composition; and (3) evolution -- the signposts of key changes in disk
properties, including the growth and migration of solids and the impact of
dynamical interactions with young planetary systems. Based on the state of the
art results in these areas, suggestions are made for potentially fruitful lines
of work in the near future.


\section{Magnetorotational Instabilities and Pulsar Kick Velocities}
\textit{Heras, Ricardo} Comment: Accepted for publication in New Astronomy\\%
Subjects: \textbf{Astrophysics - High Energy Astrophysical Phenomena}\\%
Source: \href{http://arxiv.org/abs/1507.04763}{arXiv:1507.04763} [\href{http://arxiv.org/pdf/1507.04763.pdf}{PDF}]\\%


At the end of their birth process, neutron stars can be subject to a
magnetorotational instability in which a conversion of kinetic energy of
differential rotation into radiation and kinetic energies is expected to occur
at the Alfv\'en timescale of few ms. This birth energy conversion predicts the
observed large velocity of neutron stars if during the evolving of this
instability the periods are of few ms and the magnetic fields reach values of
$10^{16}$G.


\section{No evidence of mass segregation in the low mass Galactic globular
cluster NGC 6101}
\textit{Dalessandro, E.} ; \textit{Ferraro, F. R.}; \textit{Massari, D.}; \textit{Lanzoni, B.}; \textit{Miocchi, P.}; \textit{Beccari, G.}\\%
Comment: Accepted for publication by ApJ; 33 pages, 13 figures\\%
Subjects: \textbf{Astrophysics - Astrophysics of Galaxies}; Astrophysics - Solar and Stellar Astrophysics\\%
Source: \href{http://arxiv.org/abs/1507.04776}{arXiv:1507.04776} [\href{http://arxiv.org/pdf/1507.04776.pdf}{PDF}]\\%


We used a combination of Hubble Space Telescope and ground based data to
probe the dynamical state of the low mass Galactic globular cluster NGC 6101.
We have re-derived the structural parameters of the cluster by using star
counts and we find that it is about three times more extended than thought
before. By using three different indicators, namely the radial distribution of
Blue Straggler Stars, that of Main Sequence binaries and the luminosity (mass)
function, we demonstrated that NGC 6101 shows no evidence of mass segregation,
even in the innermost regions. Indeed, both the BSS and the binary radial
distributions fully resemble that of any other cluster population. In addition
the slope of the luminosity (mass) functions does not change with the distance,
as expected for non relaxed stellar systems. NGC 6101 is one of the few
globulars where the absence of mass segregation has been observed so far. This
result provides additional support to the use of the "dynamical clock"
calibrated on the radial distribution of the Blue Stragglers as a powerful
indicator of the cluster dynamical age.


\section{From Cosmic Birth to Living Earths: The Future of UVOIR Space Astronomy}
\textit{Dalcanton, Julianne} ; \textit{Seager, Sara}; \textit{Aigrain, Suzanne}; \textit{Battel, Steve}; \textit{Brandt, Niel}; \textit{Conroy, Charlie}; \textit{Feinberg, Lee}; \textit{Gezari, Suvi}; \textit{Guyon, Olivier}; \textit{Harris, Walt}; \textit{Hirata, Chris}; \textit{Mather, John}; \textit{Postman, Marc}; \textit{Redding, Dave}; \textit{Schiminovich, David}; \textit{Stahl, H. Philip}; \textit{Tumlinson, Jason}\\%
Comment: 176 pages, 47 figures. Full resolution report and executive summary
are available at www.hdstvision.org/report\\%
Subjects: \textbf{Astrophysics - Instrumentation and Methods for Astrophysics}; Astrophysics - Cosmology and Nongalactic Astrophysics; Astrophysics - Earth and Planetary Astrophysics; Astrophysics - Astrophysics of Galaxies; Astrophysics - Solar and Stellar Astrophysics\\%
Source: \href{http://arxiv.org/abs/1507.04779}{arXiv:1507.04779} [\href{http://arxiv.org/pdf/1507.04779.pdf}{PDF}]\\%


For the first time in history, humans have reached the point where it is
possible to construct a revolutionary space-based observatory that has the
capability to find dozens of Earth-like worlds, and possibly some with signs of
life. This same telescope, designed as a long-lived facility, would also
produce transformational scientific advances in every area of astronomy and
astrophysics from black hole physics to galaxy formation, from star and planet
formation to the origins of the Solar System. The Association of Universities
for Research in Astronomy (AURA) commissioned a study on a next-generation
UVOIR space observatory with the highest possible scientific impact in the era
following JWST. This community-based study focuses on the future space-based
options for UV and optical astronomy that significantly advance our
understanding of the origin and evolution of the cosmos and the life within it.
The committee concludes that a space telescope equipped with a 12-meter class
primary mirror can find and characterize dozens of Earth-like planets and make
fundamental advances across nearly all fields of astrophysics. The concept is
called the High Definition Space Telescope (HDST). The telescope would be
located at the Sun-Earth L2 point and would cover a spectral range that, at a
minimum, runs from 0.1 to 2 microns. Unlike JWST, HDST will not need to operate
at cryogenic temperatures. HDST can be made to be serviceable on orbit but does
not require servicing to complete its primary scientific objectives. We present
the scientific and technical requirements for HDST and show that it could allow
us to determine whether or not life is common outside the Solar System. We do
not propose a specific design for such a telescope, but show that designing,
building and funding such a facility is feasible beginning in the next decade -
if the necessary strategic investments in technology begin now.


\section{Detection of Fast-Moving Waves Propagating Outward along Sunspots'
Radial Direction in the Photosphere}
\textit{Zhao, Junwei} ; \textit{Chen, Ruizhu}; \textit{Hartlep, Thomas}; \textit{Kosovichev, Alexander G.}\\%
Comment: Accepted for publication in ApJ Letters\\%
Subjects: \textbf{Astrophysics - Solar and Stellar Astrophysics}\\%
Source: \href{http://arxiv.org/abs/1507.04795}{arXiv:1507.04795} [\href{http://arxiv.org/pdf/1507.04795.pdf}{PDF}]\\%


Helioseismic and magnetohydrodynamic waves are abundant in and above
sunspots. Through cross-correlating oscillation signals in the photosphere
observed by the SDO/HMI, we reconstruct how waves propagate away from virtual
wave sources located inside a sunspot. In addition to the usual helioseismic
wave, a fast-moving wave is detected traveling along the sunspot's radial
direction from the umbra to about 15 Mm beyond the sunspot boundary. The wave
has a frequency range of 2.5 - 4.0 mHz with a phase velocity of 45.3 km/s,
substantially faster than the typical speeds of Alfven and magnetoacoustic
waves in the photosphere. The observed phenomenon is consistent with a scenario
of that a magnetoacoustic wave is excited at approximately 5 Mm beneath the
sunspot, and its wavefront travels to and sweeps across the photosphere with a
speed higher than the local magnetoacoustic speed. The fast-moving wave, if
truly excited beneath the sunspot's surface, will help open a new window to
study the internal structure and dynamics of sunspots.


\section{Broadband Spectral Modeling of the Extreme Gigahertz-Peaked Spectrum
Radio Source PKS B0008-421}
\textit{Callingham, J. R.} ; \textit{Gaensler, B. M.}; \textit{Ekers, R. D.}; \textit{Tingay, S. J.}; \textit{Wayth, R. B.}; \textit{Morgan, J.}; \textit{Bernardi, G.}; \textit{Bell, M. E.}; \textit{Bhat, R.}; \textit{Bowman, J. D.}; \textit{Briggs, F.}; \textit{Cappallo, R. J.}; \textit{Deshpande, A. A.}; \textit{Ewall-Wice, A.}; \textit{Feng, L.}; \textit{Greenhill, L. J.}; \textit{Hazelton, B. J.}; \textit{Hindson, L.}; \textit{Hurley-Walker, N.}; \textit{Jacobs, D. C.}; \textit{Johnston-Hollitt, M.}; \textit{Kaplan, D. L.}; \textit{Kudrayavtseva, N.}; \textit{Lenc, E.}; \textit{Lonsdale, C. J.}; \textit{McKinley, B.}; \textit{McWhirter, S. R.}; \textit{Mitchell, D. A.}; \textit{Morales, M. F.}; \textit{Morgan, E.}; \textit{Oberoi, D.}; \textit{Offringa, A. R.}; \textit{Ord, S. M.}; \textit{Pindor, B.}; \textit{Prabu, T.}; \textit{Procopio, P.}; \textit{Riding, J.}; \textit{Srivani, K. S.}; \textit{Subrahmanyan, R.}; \textit{Shankar, N. Udaya}; \textit{Webster, R. L.}; \textit{Williams, A.}; \textit{Williams, C. L.}\\%
Comment: Accepted for publication in ApJ\\%
Subjects: \textbf{Astrophysics - Astrophysics of Galaxies}; Astrophysics - High Energy Astrophysical Phenomena\\%
Source: \href{http://arxiv.org/abs/1507.04819}{arXiv:1507.04819} [\href{http://arxiv.org/pdf/1507.04819.pdf}{PDF}]\\%


We present broadband observations and spectral modeling of PKS B0008-421, and
identify it as an extreme gigahertz-peaked spectrum (GPS) source. PKS B0008-421
is characterized by the steepest known spectral slope below the turnover, close
to the theoretical limit of synchrotron self-absorption, and the smallest known
spectral width of any GPS source. Spectral coverage of the source spans from
0.118 to 22 GHz, which includes data from the Murchison Widefield Array and the
wide bandpass receivers on the Australia Telescope Compact Array. We have
implemented a Bayesian inference model fitting routine to fit the data with
various absorption models. We find that without the inclusion of a
high-frequency exponential break the absorption models can not accurately fit
the data, with significant deviations above and below the peak in the radio
spectrum. The addition of a high-frequency break provides acceptable spectral
fits for the inhomogeneous free-free absorption and double-component
synchrotron self-absorption models, with the inhomogeneous free-free absorption
model statistically favored. The requirement of a high-frequency spectral break
implies that the source has ceased injecting fresh particles. Additional
support for the inhomogeneous free-free absorption model as being responsible
for the turnover in the spectrum is given by the consistency between the
physical parameters derived from the model fit and the implications of the
exponential spectral break, such as the necessity of the source being
surrounded by a dense ambient medium to maintain the peak frequency near the
gigahertz region. The discovery of PKS B0008-421 suggests that the next
generation of low radio frequency surveys could reveal a large population of
GPS sources that have ceased activity, and that a portion of the ultra-steep
spectrum source population could be composed of these GPS sources in a relic
phase.


\section{A Revised Calibration of the Virial Mass Estimator for Black Holes in
Active Galaxies Based on Single-epoch H$\beta$ Spectra}
\textit{Ho, Luis C.} ; \textit{Kim, Minjin}\\%
Comment: To appear in ApJ\\%
Subjects: \textbf{Astrophysics - Astrophysics of Galaxies}\\%
Source: \href{http://arxiv.org/abs/1507.04821}{arXiv:1507.04821} [\href{http://arxiv.org/pdf/1507.04821.pdf}{PDF}]\\%


The masses of supermassive black holes in broad-line active galactic nuclei
(AGNs) can be measured through reverberation mapping, but this method currently
cannot be applied to very large samples or to high-redshift AGNs. As a
practical alternative, one can devise empirical scaling relations, based on the
correlation between broad-line region size and AGN luminosity and the relation
between black hole mass and bulge stellar velocity dispersion, to estimate the
virial masses of black holes from single-epoch spectroscopy. We present a
revised calibration of the black hole mass estimator for the commonly used
H$\beta$ emission line. Our new calibration takes into account the recent
determination of the virial coefficient for pseudo and classical bulges.


\section{Simultaneous Observations of Giant Pulses from the Crab Pulsar, with the
Murchison Widefield Array and Parkes Radio Telescope: Implications for the
Giant Pulse Emission Mechanism}
\textit{Oronsaye, S. I.} ; \textit{Ord, S. M.}; \textit{Bhat, N. D. R.}; \textit{Tremblay, S. E.}; \textit{McSweeney, S. J.}; \textit{Tingay, S. J.}; \textit{van Straten, W.}; \textit{Jameson, A.}; \textit{Bernardi, G.}; \textit{Bowman, J. D.}; \textit{Briggs, F.}; \textit{Cappallo, R. J.}; \textit{Deshpande, A. A.}; \textit{Greenhill, L. J.}; \textit{Hazelton, B. J.}; \textit{Johnston-Hollitt, M.}; \textit{Kaplan, D. L.}; \textit{Lonsdale, C. J.}; \textit{McWhirter, S. R.}; \textit{Mitchell, D. A.}; \textit{Morales, M. F.}; \textit{Morgan, E.}; \textit{Oberoi, D.}; \textit{Prabu, T.}; \textit{Shankar, N. Udaya}; \textit{Srivani, K. S.}; \textit{Subrahmanyan, R.}; \textit{Wayth, R. B.}; \textit{Webster, R. L.}; \textit{Williams, A.}; \textit{Williams, C. L.}\\%
Subjects: \textbf{Astrophysics - High Energy Astrophysical Phenomena}\\%
Source: \href{http://arxiv.org/abs/1507.04830}{arXiv:1507.04830} [\href{http://arxiv.org/pdf/1507.04830.pdf}{PDF}]\\%


We report on observations of giant pulses from the Crab pulsar performed
simultaneously with the Parkes radio telescope and the incoherent combination
of the Murchison Widefield Array (MWA) antenna tiles. The observations were
performed over a duration of approximately one hour at a center frequency of
1382 MHz with 340 MHz bandwidth at Parkes, and at a center frequency of 193 MHz
with 15 MHz bandwidth at the MWA. Our analysis has led to the detection of 55
giant pulses at the MWA and 2075 at Parkes above a threshold of 3.5$\sigma$ and
6.5$\sigma$ respectively. We detected 51$\%$ of the MWA giant pulses at the
Parkes radio telescope, with spectral indices in the range of $-3.6>\alpha>
-4.9$ ($S_{\rm \nu} \propto \nu^\alpha$). We present a Monte Carlo analysis
supporting the conjecture that the giant pulse emission in the Crab is
intrinsically broadband, the less than $100\%$ correlation being due to the
relative sensitivities of the two instruments and the width of the spectral
index distribution. Our observations are consistent with the hypothesis that
the spectral index of giant pulses is drawn from normal distribution of
standard deviation 0.6, but with a mean that displays an evolution with
frequency from -3.00 at 1382 MHz, to -2.85 at 192 MHz.


\section{Adiabatic Mass Loss in Binary Stars. II. From Zero-Age Main Sequence to
the Base of the Giant Branch}
\textit{Ge, Hongwei} ; \textit{Webbink, Ronald F.}; \textit{Chen, Xuefei}; \textit{Han, Zhanwen}\\%
Comment: 56 pages, 11 figures, 4 tables, Accepted to be published in ApJ\\%
Subjects: \textbf{Astrophysics - Solar and Stellar Astrophysics}\\%
Source: \href{http://arxiv.org/abs/1507.04843}{arXiv:1507.04843} [\href{http://arxiv.org/pdf/1507.04843.pdf}{PDF}]\\%


In the limit of extremely rapid mass transfer, the response of a donor star
in an interacting binary becomes asymptotically one of adiabatic expansion. We
survey here adiabatic mass loss from Population I stars of mass 0.10 Msun to
100 Msun from the zero age main sequence to the base of the giant branch, or to
central hydrogen exhaustion for lower main sequence stars. For intermediate-
and high-mass stars, dynamical mass transfer is preceded by an extended phase
of thermal time scale mass transfer as the star is stripped of most of its
envelope mass. The critical mass ratio qad above which this delayed dynamical
instability occurs increases with advancing evolutionary age of the donor star,
by ever-increasing factors for more massive donors. Most intermediate- or
high-mass binaries with nondegenerate accretors probably evolve into contact
before manifesting this instability. As they approach the base of the giant
branch, however, and begin developing a convective envelope, qad plummets
dramatically among intermediate-mass stars, to values of order unity, and a
prompt dynamical instability occurs. Among low-mass stars, the prompt
instability prevails throughout main sequence evolution, with q_ad declining
with decreasing mass. Our calculated qad agree well with the behavior of
timedependent models by Chen \& Han (2003) of intermediate-mass stars initiating
mass transfer in the Hertzsprung gap. Application of our results to cataclysmic
variables, as systems which must be stable against rapid mass transfer, nicely
circumscribes the range in qad as a function of orbital period in which they
are found. These results are intended to advance the verisimilitude of
population synthesis models of close binary evolution.


\section{Enhancing the Cosmic Shear Power Spectrum}
\textit{Simpson, Fergus} ; \selectlanguage{ngerman}\textit{Harnois-Déraps, Joachim}; \textit{Heymans, Catherine}; \textit{Jimenez, Raul}; \textit{Verde, Licia}\\%
Comment: 6 pages, 2 figures\\%
Subjects: \textbf{Astrophysics - Cosmology and Nongalactic Astrophysics}\\%
Source: \href{http://arxiv.org/abs/1507.04862}{arXiv:1507.04862} [\href{http://arxiv.org/pdf/1507.04862.pdf}{PDF}]\\%


Applying a transformation to a non-Gaussian field can enhance the information
content of the resulting power spectrum, by reducing the correlations between
Fourier modes. In the context of weak gravitational lensing, it has been shown
that this gain in information content is significantly compromised by the
presence of shape noise. We apply clipping to mock convergence fields, a
technique which is known to be robust in the presence of noise and has been
successfully applied to galaxy number density fields. When analysed in
isolation the resulting convergence power spectrum returns degraded constraints
on cosmological parameters. However substantial gains can be achieved by
performing a combined analysis of the power spectra derived from both the
original and transformed fields. Even in the presence of realistic levels of
shape noise, we demonstrate that this approach is capable of reducing the area
of likelihood contours within the $\Omega_m - \sigma_8$ plane by more than a
factor of three.


\section{Study of Calibration of Solar Radio Spectrometers and the quiet-Sun
Radio Emission}
\textit{Tan, Chengming} ; \textit{Yan, Yihua}; \textit{Tan, Baolin}; \textit{Fu, Qijun}; \textit{Liu, Yuying}; \textit{Xu, Guirong}\\%
Comment: Accepted by Apj, 24 pages, 10 pages, 3 tables\\%
Subjects: \textbf{Astrophysics - Solar and Stellar Astrophysics}\\%
Source: \href{http://arxiv.org/abs/1507.04866}{arXiv:1507.04866} [\href{http://arxiv.org/pdf/1507.04866.pdf}{PDF}]\\%


This work presents a systematic investigation of the influence of weather
conditions on the calibration errors by using Gaussian fitness, least
chi-square linear fitness and wavelet transform to analyze the calibration
coefficients from observations of the Chinese Solar Broadband Radio
Spectrometers (at frequency bands of 1.0-2.0 GHz, 2.6-3.8 GHz, and 5.2-7.6 GHz)
during 1997-2007. We found that calibration coefficients are influenced by the
local air temperature. Considering the temperature correction, the calibration
error will reduce by about $10\%-20\%$ at 2800 MHz. Based on the above
investigation and the calibration corrections, we further study the radio
emission of the quiet-Sun by using an appropriate hybrid model of the quiet-Sun
atmosphere. The results indicate that the numerical flux of the hybrid model is
much closer to the observation flux than that of other ones.


\section{Detection of TiH$_2$ molecule in the interstellar medium is less
probable}
\textit{Chandra, Suresh} ; \textit{Sharma, Mohit K.}\\%
Comment: 3 pages, 3 figures, 1 table\\%
Subjects: \textbf{Astrophysics - Astrophysics of Galaxies}\\%
Source: \href{http://arxiv.org/abs/1507.04873}{arXiv:1507.04873} [\href{http://arxiv.org/pdf/1507.04873.pdf}{PDF}]\\%


Identification of TiH$^1$ and TiO$^2$ has been historical, as the Titanium
was first time discovered in the interstellar medium (ISM). After finding
TiO$_2$$^3$, there is an obvious question about the search of titanium
dihydride (TiH$_2$). The existence of TiH$_2$ in the ISM is quite probable, as
the atomic abundance of hydrogen is about 1900 times larger than that of
oxygen. We have discussed that the detection of TiH$_2$ in the ISM is less
probable, though it has a large electric dipole moment.


\section{Some observations about the MOLSCAT}
\textit{Sharma, M. K.} ; \textit{Sharma, Monika}; \textit{Chandra, Suresh}\\%
Comment: 9 pages\\%
Subjects: \textbf{Astrophysics - Instrumentation and Methods for Astrophysics}; Astrophysics - Astrophysics of Galaxies; Physics - Chemical Physics\\%
Source: \href{http://arxiv.org/abs/1507.04882}{arXiv:1507.04882} [\href{http://arxiv.org/pdf/1507.04882.pdf}{PDF}]\\%


For calculation of cross sections for collisional transitions between
rotational levels in a molecule, a computer code, MOLSCAT has been developed by
Hutson \& Green (1994). For the transitions between rotational levels in
H$_2$CS due to collisions with He atom, we have calculated cross sections under
the CS approximation. In the MOLSCAT, there is provision to input more than one
values of total energies. Here, for example, we are interested in the cross
sections for total energy 11 cm$^{-1}$. The calculations have been done for the
single energy 11 cm$^{-1}$ and for eight combinations, having energies (11,
12), (12, 11), (10, 11), (11, 10), (11, 12, 13), (9, 10, 11), (10, 11, 12), (9,
10, 11, 12, 13) cm$^{-1}$. We have found that the cross sections for 11
cm$^{-1}$, in general, differ from one another in all the 9 calculations. The
reason for the difference in the results appears that the MOLSCAT uses the
intermediate data of calculations for one energy, in the calculations for other
energies. Under such circumstances, the possible suggestion can be to run the
MOLSCAT for a single energy at a time.


\section{Distinguishing short and long Fermi GRBs}
\textit{Tarnopolski, Mariusz} Comment: 8 pages, 6 figures; resubmitted to MNRAS after adressing referee's
comments\\%
Subjects: \textbf{Astrophysics - High Energy Astrophysical Phenomena}; Astrophysics - Cosmology and Nongalactic Astrophysics; Statistics - Machine Learning\\%
Source: \href{http://arxiv.org/abs/1507.04886}{arXiv:1507.04886} [\href{http://arxiv.org/pdf/1507.04886.pdf}{PDF}]\\%


Two classes of GRBs, short and long, have been determined without any doubts,
and are usually ascribed to different progenitors, yet these classes overlap
for a variety of descriptive parameters. A subsample of 46 long and 22 short
$Fermi$ GRBs with estimated Hurst Exponents (HEs), complemented by minimum
variability time-scales (MVTS) and durations ($T_{90}$) is used to perform a
supervised Machine Learning (ML) and Monte Carlo (MC) simulation using a
Support Vector Machine (SVM) algorithm. It is found that while $T_{90}$ itself
performs very well in distinguishing short and long GRBs, the overall success
ratio is higher when the training set is complemented by MVTS and HE. These
results may allow to introduce a new (non-linear) parameter that might provide
less ambiguous classification of GRBs.


\section{Formation and Search of Large Scale Antimatter Regions}
\textit{Grobov, A. V.} ; \textit{Rubin, S. G.}\\%
Subjects: \textbf{Astrophysics - Cosmology and Nongalactic Astrophysics}\\%
Source: \href{http://arxiv.org/abs/1507.04887}{arXiv:1507.04887} [\href{http://arxiv.org/pdf/1507.04887.pdf}{PDF}]\\%


In the present paper we discuss a generation of large antimatter regions with
sizes exceeding the critical surviving size. In the modern epoch domains with
high antimatter density evolve to single galaxies with a peculiar content of
anti-helium and anti-deuterium.


\section{A Hyper Suprime-Cam View of the Interacting Galaxies of the M81 Group}
\textit{Okamoto, Sakurako} ; \textit{Arimoto, Nobuo}; \textit{Ferguson, Annette M. N.}; \textit{Bernard, Edouard J.}; \textit{Irwin, Mike J.}; \textit{Yamada, Yoshihiko}; \textit{Utsumi, Yousuke}\\%
Comment: 7 pages, 5 figures, accepted for publication in ApJL\\%
Subjects: \textbf{Astrophysics - Astrophysics of Galaxies}\\%
Source: \href{http://arxiv.org/abs/1507.04889}{arXiv:1507.04889} [\href{http://arxiv.org/pdf/1507.04889.pdf}{PDF}]\\%


We present the first results of a wide-field mapping survey of the M81 group
conducted with Hyper Suprime-Cam on the Subaru Telescope. Our deep photometry
reaches $\sim2$ magnitudes below the tip of the red giant branch (RGB) and
reveals the spatial distribution of both old and young stars over an area of
$\sim 100\times115$ kpc at the distance of M81. The young stars ($\sim30-160$
Myr old) closely follow the neutral hydrogen distribution and can be found in a
stellar stream between M81 and NGC\,3077 and in numerous outlying stellar
associations, including the known concentrations of Arp's Loop, Holmberg\,IX,
an arc in the halo of M82, BK3N, and the Garland. Many of these groupings do
not have counterparts in the RGB maps, suggesting they may be genuinely young
systems. Our survey also reveals for the first time the very extended ($\geq
2\times \rm{R_{25}}$) halos of RGB stars around M81, M82 and NGC\,3077, as well
as faint tidal streams that link these systems. The halos of M82 and NGC\,3077
exhibit highly disturbed morphologies, presumably a consequence of the recent
gravitational encounter and their ongoing disruption. While the halos of M81,
NGC\,3077 and the inner halo of M82 have the similar $(g-i)_{0}$ colors, the
outer halo of M82 is significantly bluer indicating it is more metal-poor.
Remarkably, our deep panoramic view of the M81 group demonstrates that the
complexity long-known to be present in HI is equally matched in the low surface
brightness stellar component.


\section{On partition function in Astronomy \& Astrophysics}
\textit{Sharma, M. K.} ; \textit{Sharma, Monika}; \textit{Chandra, Suresh}\\%
Comment: 7 pages, 1 figure, 1 table\\%
Subjects: \textbf{Astrophysics - Astrophysics of Galaxies}; Physics - Chemical Physics\\%
Source: \href{http://arxiv.org/abs/1507.04890}{arXiv:1507.04890} [\href{http://arxiv.org/pdf/1507.04890.pdf}{PDF}]\\%


In order to analyze spectrum from the interstellar medium (ISM), spectrum of
the molecule of interest is recorded in a laboratory, and accurate rotational
and centrifugal distortion constants are derived. By using these constants, one
can calculate accurate partition function. However, in the same paper, where
these constants are derived, the partition function is calculated by using a
semi-empirical expression.
We have looked into the details of this semi-empirical expression and
compared the values, obtained from it, with the accurate ones. As an example,
we have considered the case of Methanimine (CH$_2$NH) which is detected in a
number of cosmic objects. It is found that for the kinetic temperature $T >
120$ K, the semi-empirical expression gives large value as compared to the
accurate one. The deviation becomes about 25\% larger than the accurate one at
the kinetic temperature of 400 K.


\section{A new search for variability-selected active galaxies within the VST
SUDARE-VOICE survey: the Chandra Deep Field South and the SERVS-SWIRE area}
\textit{Falocco, S.} ; \textit{De Cicco, D.}; \textit{Paolillo, M.}; \textit{Covone, G.}; \textit{Longo, G.}; \textit{Grado, A.}; \textit{Limatola, L.}; \textit{Vaccari, M.}; \textit{Botticella, M. T.}; \textit{Pignata, G.}; \textit{Cappellaro, E.}; \textit{Trevese, D.}; \textit{Vagnetti, F.}; \textit{Salvato, M.}; \textit{Radovich, M.}; \textit{Hsu, L.}; \textit{Brandt, W. N.}; \textit{Capaccioli, M.}; \textit{Napolitano, N.}; \textit{Baruffolo, A.}; \textit{Cascone, E.}; \textit{Schipani, P.}\\%
Comment: Refereed Proceeding of the "The Universe of Digital Sky Surveys"
conference held at the INAF - Observatory of Capodimonte, Naples, on
25th-28th november 2014, to be published on Astrophysics and Space Science
Proceedings, edited by Longo, Napolitano, Marconi, Paolillo, Iodice\\%
Subjects: \textbf{Astrophysics - Astrophysics of Galaxies}; Physics - Space Physics\\%
Source: \href{http://arxiv.org/abs/1507.04923}{arXiv:1507.04923} [\href{http://arxiv.org/pdf/1507.04923.pdf}{PDF}]\\%


This work makes use of the VST observations to select variable sources. We
use also the IR photometry, SED fitting and X-ray information where available
to confirm the nature of the AGN candidates. The IR data, available over the
full survey area, allow to confirm the consistency of the variability selection
with the IR color selection method, while the detection of variability may
prove useful to detect the presence of an AGN in IR selected starburst
galaxies.


\section{Performance Analysis of GPU-Accelerated Filter-Based Source Finding for
HI Spectral Line Image Data}
\textit{Westerlund, Stefan} ; \textit{Harris, Christopher}\\%
Comment: 28 pages, 12 figures\\%
Subjects: \textbf{Astrophysics - Instrumentation and Methods for Astrophysics}\\%
Source: \href{http://arxiv.org/abs/1507.04941}{arXiv:1507.04941} [\href{http://arxiv.org/pdf/1507.04941.pdf}{PDF}]\\%


Searching for sources of electromagnetic emission in spectral-line radio
astronomy interferometric data is a computationally intensive process. Parallel
programming techniques and High Performance Computing hardware may be used to
improve the computational performance of a source finding program. However, it
is desirable to further reduce the processing time of source finding in order
to decrease the computational resources required for the task. GPU acceleration
is a method that may achieve significant increases in performance for some
source finding algorithms, particularly for filtering image data. This work
considers the application of GPU acceleration to the task of source finding and
the techniques used to achieve the best performance, such as memory management.
We also examine the changes in performance, where the algorithms that were GPU
accelerated achieved a speedup of around 3.2 times the 12 core per node
CPU-only performance, while the program as a whole experienced a speedup of 2.0
times.


\section{Magnetised cosmological perturbations in the post-recombination era}
\textit{Vasiliou, Hera} ; \textit{Tsagas, Christos G.}\\%
Comment: 16 pages, no figures\\%
Subjects: \textbf{Astrophysics - Cosmology and Nongalactic Astrophysics}\\%
Source: \href{http://arxiv.org/abs/1507.04956}{arXiv:1507.04956} [\href{http://arxiv.org/pdf/1507.04956.pdf}{PDF}]\\%


We study inhomogeneous magnetised cosmologies through the post-recombination
era in the framework of Newtonian gravity and the ideal-magnetohydrodynamic
limit. The nonlinear kinematic and dynamic equations are derived and linearised
around the Newtonian counterpart of the Einstein-de Sitter universe. This
allows for a direct comparison with the earlier relativistic treatments of the
issue. Focusing on the evolution of linear density perturbations, we provide
new analytic solutions which include the effects of the magnetic pressure as
well as those of the field's tension. We find that the extra pressure the
magnetic field introduces into the system inhibits the growth of density
distortions and also induces a purely magnetic Jeans length. On scales larger
than the aforementioned characteristic length the inhomogeneities grow, though
slower than in non-magnetised universes. Wavelengths smaller than the magnetic
Jeans length, on the other hand, typically oscillate with decreasing amplitude.
In all cases, the effect of the field is proportional to its relative strength.


\section{Spectral Line Survey toward Young Massive Protostar NGC 2264 CMM3 in the
4 mm, 3 mm, and 0.8 mm Bands}
\textit{Watanabe, Yoshimasa} ; \textit{Sakai, Nami}; \textit{Lopez-Sepulcre, Ana}; \textit{Furuya, Ryuta}; \textit{Sakai, Takeshi}; \textit{Hirota, Tomoya}; \textit{Liu, Sheng-Yuan}; \textit{Su, Yu-Nung}; \textit{Yamamoto, Satoshi}\\%
Comment: 70 pages, 35 figures, accepted for publication in ApJ\\%
Subjects: \textbf{Astrophysics - Astrophysics of Galaxies}; Astrophysics - Solar and Stellar Astrophysics\\%
Source: \href{http://arxiv.org/abs/1507.04958}{arXiv:1507.04958} [\href{http://arxiv.org/pdf/1507.04958.pdf}{PDF}]\\%


Spectral line survey observations are conducted toward the high-mass
protostar candidate NGC 2264 CMM3 in the 4 mm, 3 mm, and 0.8 mm bands with the
Nobeyama 45 m telescope and the Atacama Submillimeter Telescope Experiment
(ASTE) 10 m telescope. In total, 265 emission lines are detected in the 4 mm
and 3 mm bands, and 74 emission lines in the 0.8 mm band. As a result, 36
molecular species and 30 isotopologues are identified. In addition to the
fundamental molecular species, many emission lines of carbon-chain molecules
such as HC5N, C4H, CCS, and C3S are detected in the 4 mm and 3 mm bands.
Deuterated molecular species are also detected with relatively strong
intensities. On the other hand, emission lines of complex organic molecules
such as HCOOCH3, and CH3OCH3 are found to be weak. For the molecules for which
multiple transitions are detected, rotation temperatures are derived to be 7-33
K except for CH3OH. Emission lines with high upper-state energies (Eu > 150 K)
are detected for CH3OH, indicating existence of a hot core. In comparison with
the chemical composition of the Orion KL, carbon-chain molecules and deuterated
molecules are found to be abundant in NGC 2264 CMM3, while sulfur-bearing
species and complex organic molecules are deficient. These characteristics
indicate chemical youth of NGC 2264 CMM3 in spite of its location at the center
of the cluster forming core, NGC 2264 C.


\section{Modelling the observed properties of carbon-enhanced metal-poor stars
using binary population synthesis}
\textit{Abate, C.} ; \textit{Pols, O. R.}; \textit{Stancliffe, R. J.}; \textit{Izzard, R. G.}; \textit{Karakas, A. I.}; \textit{Beers, T. C.}; \textit{Lee, Y. S.}\\%
Comment: 17 pages, 11 figures, accepted for publication on Astronomy and
Astrophysics\\%
Subjects: \textbf{Astrophysics - Solar and Stellar Astrophysics}; Astrophysics - Astrophysics of Galaxies\\%
Source: \href{http://arxiv.org/abs/1507.04969}{arXiv:1507.04969} [\href{http://arxiv.org/pdf/1507.04969.pdf}{PDF}]\\%


The stellar population in the Galactic halo is characterised by a large
fraction of CEMP stars. Most CEMP stars are enriched in $s$-elements (CEMP-$s$
stars), and some of these are also enriched in $r$-elements (CEMP-$s/r$ stars).
One formation scenario proposed for CEMP stars invokes wind mass transfer in
the past from a TP-AGB primary star to a less massive companion star which is
presently observed. We generate low-metallicity populations of binary stars to
reproduce the observed CEMP-star fraction. In addition, we aim to constrain our
wind mass-transfer model and investigate under which conditions our synthetic
populations reproduce observed abundance distributions. We compare the CEMP
fractions and the abundance distributions determined from our synthetic
populations with observations. Several physical parameters of the binary
stellar population of the halo are uncertain, e.g. the initial mass function,
the mass-ratio and orbital-period distributions, and the binary fraction. We
vary the assumptions in our model about these parameters, as well as the wind
mass-transfer process, and study the consequent variations of our synthetic
CEMP population. The CEMP fractions calculated in our synthetic populations
vary between 7\% and 17\%, a range consistent with the CEMP fractions among very
metal-poor stars recently derived from the SDSS/SEGUE data sample. The results
of our comparison between the modelled and observed abundance distributions are
different for CEMP-$s/r$ stars and for CEMP-$s$ stars. For the latter, our
simulations qualitatively reproduce the observed distributions of C, Na, Sr,
Ba, Eu, and Pb. Contrarily, for CEMP-$s/r$ stars our model cannot reproduce the
large abundances of neutron-rich elements such as Ba, Eu, and Pb. This result
is consistent with previous studies, and suggests that CEMP-$s/r$ stars
experienced a different nucleosynthesis history to CEMP-$s$ stars.


\section{A Coordinated X-ray and Optical Campaign of the Nearby Massive Binary
$\delta$ Orionis Aa: II. X-ray Variability}
\textit{Nichols, J. S.} ; \textit{Huenemoerder, D. P.}; \textit{Corcoran, M. F.}; \textit{Waldron, W.}; \selectlanguage{ngerman}\textit{Nazé, Y.}; \textit{Pollock, A. M. T.}; \textit{Moffat, A. F. J.}; \textit{Lauer, J.}; \textit{Shenar, T.}; \textit{Russell, C. M. P.}; \textit{Richardson, N. D.}; \textit{Pablo, H.}; \textit{Evans, N R.}; \textit{Hamaguchi, K.}; \textit{Gull, T.}; \textit{Hamann, W. R.}; \textit{Oskinova, L.}; \textit{Ignace, R.}; \textit{Hoffman, Jennifer L.}; \textit{Hole, K. T.}; \textit{Lomax, J. R.}\\%
Comment: 36 pages, 14 Tables, 19 Figures, accepted by ApJ, one of 4 related
papers to be published together\\%
Subjects: \textbf{Astrophysics - High Energy Astrophysical Phenomena}; Astrophysics - Solar and Stellar Astrophysics\\%
Source: \href{http://arxiv.org/abs/1507.04972}{arXiv:1507.04972} [\href{http://arxiv.org/pdf/1507.04972.pdf}{PDF}]\\%


We present time-resolved and phase-resolved variability studies of an
extensive X-ray high-resolution spectral dataset of the $\delta$ Orionis Aa
binary system. The four observations, obtained with Chandra ACIS HETGS, have a
total exposure time of ~479 ks and provide nearly complete binary phase
coverage. Variability of the total X-ray flux in the range 5-25 $\AA$ is
confirmed, with maximum amplitude of about +/-15\% within a single ~125 ks
observation. Periods of 4.76d and 2.04d are found in the total X-ray flux, as
well as an apparent overall increase in flux level throughout the 9-day
observational campaign. Using 40 ks contiguous spectra derived from the
original observations, we investigate variability of emission line parameters
and ratios. Several emission lines are shown to be variable, including S XV, Si
XIII, and Ne IX. For the first time, variations of the X-ray emission line
widths as a function of the binary phase are found in a binary system, with the
smallest widths at phase=0.0 when the secondary $\delta$ Orionis Aa2 is at
inferior conjunction. Using 3D hydrodynamic modeling of the interacting winds,
we relate the emission line width variability to the presence of a wind cavity
created by a wind-wind collision, which is effectively void of embedded wind
shocks and is carved out of the X-ray-producing primary wind, thus producing
phase-locked X-ray variability.


\section{Infrared study of transitional disks in Ophiuchus with Herschel}
\textit{Rebollido, Isabel} ; \selectlanguage{ngerman}\textit{Merín, Bruno}; \textit{Ribas, Álvaro}; \textit{Bustamante, Ignacio}; \textit{Bouy, Hervé}; \textit{Riviere-Marichalar, Pablo}; \textit{Prusti, Timo}; \textit{Pilbratt, Göran L.}; \textit{André, Philippe}; \textit{Ábrahám, Péter}\\%
Comment: 21 pages, with 5 figures. Accepted in Astronomy \& Astrophysics\\%
Subjects: \textbf{Astrophysics - Earth and Planetary Astrophysics}\\%
Source: \href{http://arxiv.org/abs/1507.04975}{arXiv:1507.04975} [\href{http://arxiv.org/pdf/1507.04975.pdf}{PDF}]\\%


Context. Observations of nearby star-forming regions with the Herschel Space
Observatory complement our view of the protoplanetary disks in Ophiuchus with
information about the outer disks. Aims. The main goal of this project is to
provide new far-infrared fluxes for the known disks in the core region of
Ophiuchus and to identify potential transitional disks using data from
Herschel. Methods. We obtained PACS and SPIRE photometry of previously
spectroscopically confirmed young stellar objects (YSO) in the region and
analysed their spectral energy distributions. Results. From an initial sample
of 261 objects with spectral types in Ophiuchus, we detect 49 disks in at least
one Herschel band. We provide new far-infrared fluxes for these objects. One of
them is clearly a new transitional disk candidate. Conclusions. The data from
Herschel Space Observatory provides fluxes that complement previous infrared
data and that we use to identify a new transitional disk candidate.


\section{Primordial perturbations from dilaton-induced gauge fields}
\textit{Choi, Kiwoon} ; \textit{Choi, Ki-Young}; \textit{Kim, Hyungjin}; \textit{Shin, Chang Sub}\\%
Comment: 37 pages, 8 figures\\%
Subjects: \textbf{Astrophysics - Cosmology and Nongalactic Astrophysics}; High Energy Physics - Phenomenology\\%
Source: \href{http://arxiv.org/abs/1507.04977}{arXiv:1507.04977} [\href{http://arxiv.org/pdf/1507.04977.pdf}{PDF}]\\%


We study the primordial scalar and tensor perturbations in inflation scenario
involving a spectator dilaton field. In our setup, the rolling spectator
dilaton causes a tachyonic instability of gauge fields, leading to a copious
production of gauge fields in the superhorizon regime, which generates
additional scalar and tensor perturbations through gravitational interactions.
Our prime concern is the possibility to enhance the tensor-to-scalar ratio r
relative to the standard result, while satisfying the observational
constraints. To this end, we allow the dilaton field to be stabilized before
the end of inflation, but after the CMB scales exit the horizon. We show that
for the inflaton slow roll parameter {\epsilon} > 10^-3, the tensor-to-scalar
ratio in our setup can be enhanced only by a factor of O(1) compared to the
standard result. On the other hand, for smaller {\epsilon} corresponding to a
lower inflation energy scale, a much bigger enhancement can be achieved, so
that our setup can give rise to an observably large r > 10^-2 even when
{\epsilon} << 10^-3. The tensor perturbation sourced by the spectator dilaton
can have a strong scale dependence, and is generically red-tilted. We also
discuss a specific model to realize our scenario, and identify the parameter
region giving an observably large r for relatively low inflation energy scales.


\section{Chiral Magnetic Effect in Protoneutron Stars and Magnetic Field Spectral
Evolution}
\selectlanguage{ngerman}\textit{Sigl, Günter} ; \textit{Leite, Natacha}\\%
Comment: 15 pages, 10 figures\\%
Subjects: \textbf{Astrophysics - High Energy Astrophysical Phenomena}; High Energy Physics - Phenomenology\\%
Source: \href{http://arxiv.org/abs/1507.04983}{arXiv:1507.04983} [\href{http://arxiv.org/pdf/1507.04983.pdf}{PDF}]\\%


We investigate the evolution of the chiral magnetic instability in a
protoneutron star and compute the resulting magnetic power and helicity
spectra. The instability may act during the early cooling phase of the hot
protoneutron star after supernova core collapse, where it can contribute to the
buildup of magnetic fields of strength up to the order of $10^{14}$ G. The
maximal field strengths generated by this instability, however, depend
considerably on the temperature of the protoneutron star, on density
fluctuations and turbulence spectrum of the medium. At the end of the hot
cooling phase the magnetic field tends to be concentrated around the
submillimeter to cm scale, where it is subject to slow resistive damping.


\section{Local interstellar cosmic-ray spectra derived from gamma-ray
emissivities}
\textit{Strong, A. W.} Comment: Contribution to the 34th International Cosmic Ray Conference, July 30
to August 6, The Hague, Netherlands\\%
Subjects: \textbf{Astrophysics - High Energy Astrophysical Phenomena}\\%
Source: \href{http://arxiv.org/abs/1507.05006}{arXiv:1507.05006} [\href{http://arxiv.org/pdf/1507.05006.pdf}{PDF}]\\%


Precise gamma-ray emissivities from cosmic-ray interactions with interstellar
gas have been recently derived using Fermi-LAT data, and used to constrain the
local interstellar spectra of protons and leptons. We report on a continuing
effort to exploit these emissivities combined with the latest hadronic
gamma-ray production cross-sections and other constraints such as synchrotron
emission for the leptonic component. The interstellar spectra provide important
information for heliospheric modulation, and cosmic-ray origin and propagation.


\section{Recent extensions to GALPROP}
\textit{Strong, A. W.} Comment: Contribution to the 34th International Cosmic Ray Conference, July 30
to August 6, The Hague, Netherlands\\%
Subjects: \textbf{Astrophysics - High Energy Astrophysical Phenomena}\\%
Source: \href{http://arxiv.org/abs/1507.05020}{arXiv:1507.05020} [\href{http://arxiv.org/pdf/1507.05020.pdf}{PDF}]\\%


Some recent extensions to the GALPROP cosmic-ray propagation package are
described. The enhancements include: an accurate solution option, improved
convection formulation, alternative spatial boundary conditions, polarized
synchrotron emission, new magnetic field models, updated gamma-ray production
cross-sections, free-free radio emission and absorption, primary positrons,
additional injection spectral breaks, deuterium production by pp fusion,
hadronic energy losses, improved HEALPix skymap format, compatibility with
latest HEALPix release, and various bug fixes. The Explanatory Supplement has
been extensively updated, including details of these enhancements. A compatible
plot package GALPLOT for GALPROP output is also provided, as well as other
related software.


\section{The origin of net electric currents in solar active regions}
\textit{Dalmasse, K.} ; \textit{Aulanier, G.}; \selectlanguage{ngerman}\textit{Démoulin, P.}; \textit{Kliem, B.}; \textit{Török, T.}; \textit{Pariat, E.}\\%
Comment: 14 pages and 11 figures (Accepted in The Astrophysical Journal)\\%
Subjects: \textbf{Astrophysics - Solar and Stellar Astrophysics}\\%
Source: \href{http://arxiv.org/abs/1507.05060}{arXiv:1507.05060} [\href{http://arxiv.org/pdf/1507.05060.pdf}{PDF}]\\%


There is a recurring question in solar physics about whether or not electric
currents are neutralized in active regions (ARs). This question was recently
revisited using three-dimensional (3D) magnetohydrodynamic (MHD) numerical
simulations of magnetic flux emergence into the solar atmosphere. Such
simulations showed that flux emergence can generate a substantial net current
in ARs. Another source of AR currents are photospheric horizontal flows. Our
aim is to determine the conditions for the occurrence of net vs. neutralized
currents with this second mechanism. Using 3D MHD simulations, we
systematically impose line-tied, quasi-static, photospheric twisting and
shearing motions to a bipolar potential magnetic field. We find that such
flows: (1) produce both {\it direct} and {\it return} currents, (2) induce very
weak compression currents - not observed in 2.5D - in the ambient field present
in the close vicinity of the current-carrying field, and (3) can generate
force-free magnetic fields with a net current. We demonstrate that neutralized
currents are in general produced only in the absence of magnetic shear at the
photospheric polarity inversion line - a special condition rarely observed. We
conclude that, as magnetic flux emergence, photospheric flows can build up net
currents in the solar atmosphere, in agreement with recent observations. These
results thus provide support for eruption models based on pre-eruption magnetic
fields possessing a net coronal current.


\section{Destruction and Observational Signatures of Sun-Impacting Comets}
\textit{Brown, John C.} ; \textit{Carlson, Robert W.}; \textit{Toner, Mark P.}\\%
Comment: 12 pages, 6 figures, published in Astrophysical Journal\\%
Subjects: \textbf{Astrophysics - Solar and Stellar Astrophysics}; Astrophysics - Earth and Planetary Astrophysics\\%
Source: \href{http://arxiv.org/abs/1507.05062}{arXiv:1507.05062} [\href{http://arxiv.org/pdf/1507.05062.pdf}{PDF}]\\%


Motivated by recent data on comets in the low corona, we discuss destruction
of sun impacting comets in the dense lower solar atmosphere. Perihelion
distances q less than the solar radius and incident masses Mo much greater than
1E12 g are required to reach such depths. Extending earlier work on planetary
atmosphere impacts to solar conditions, we evaluate the mechanisms and spatial
distribution of nucleus mass and energy loss as functions of Mo and q, and of
parameter X = 2Q/CHvovo. Q is the total specific energy for ablative mass loss,
CH the bow shock heat transfer efficiency, and vo the solar escape speed (619
km/s). We discuss factors affecting Q and CH and conclude that, for solar vo, X
is most likely less than 1 so that solar impactors are mostly ablated before
decelerating. Sun impacting comets have kinetic energies 2E30 erg x(Mo/1E15 g),
comparable with the energies of magnetic flares. This is released as a
localised explosive airburst within a few scale heights H around 200 km of the
photosphere, depending weakly on Mo , q and X. For X = 0.01, Mo around 1E15 g,
and a typical Kreutz Group shallow incidence angle, comet the airburst occurs
around atmospheric density n around 3E15 per ml and this would be 1000 times
larger (700 km deeper) for vertical entry. Such airbursts drive flare like
phenomena including prompt radiation, hot rising plumes and photospheric
ripples, the observability and diagnostic value of which we discuss.


\section{Precision age indicators that exploit chemically peculiar stars}
\textit{Worthey, Guy} Comment: 4 pages, 3 figures, accepted for publication in A\&A Letters\\%
Subjects: \textbf{Astrophysics - Astrophysics of Galaxies}; Astrophysics - Solar and Stellar Astrophysics\\%
Source: \href{http://arxiv.org/abs/1507.05076}{arXiv:1507.05076} [\href{http://arxiv.org/pdf/1507.05076.pdf}{PDF}]\\%


We would like to find a way to improve the determination of galaxy star
formation history from integrated light spectroscopy. To this end, several
classes of chemically peculiar (CP) stars arise during the course of normal
evolution in single stars and noninteracting binary stars. An aging stellar
population has periods of time in which CP stars contribute to the integrated
light, and others in which the contributions fade. The HgMn stars, for example,
occupy a narrow temperature range of 10500 to 16000 K, which maps to a narrow
range of ages. Wolf-Rayet stars, He-poor stars, Bp-Ap stars, Am-Fm stars, and C
stars all become very common in a normal stellar population at various ages
between zero and several Gyr, fading in and out in a way that is analogous to
features used in stellar spectral classification. We examine population
fractions and light fractions in order to assess the feasibility of using CP
stars as age tracers. We find that, even though CP stars do not usually
dominate in number, there are enough of them so that the CP spectral features
are detectable in high-quality integrated spectra of young and intermediate age
stellar populations. The new technique should be calibratable and useful.
Furthermore, using CP signatures as age dating tools sidesteps reliance on
photometry that is susceptible to dust and Balmer features that are susceptible
to nebular fill-in.


\section{Detection of magnetic fields in both B-type components of the $\epsilon$
Lupi system: a new constraint on the origin of fossil fields?}
\textit{Shultz, M.} ; \textit{Wade, G. A.}; \textit{Alecian, E.}; \textit{Collaboration, the BinaMIcS}\\%
Comment: 5 pages, 3 figures, accepted for publication in MNRAS\\%
Subjects: \textbf{Astrophysics - Solar and Stellar Astrophysics}\\%
Source: \href{http://arxiv.org/abs/1507.05084}{arXiv:1507.05084} [\href{http://arxiv.org/pdf/1507.05084.pdf}{PDF}]\\%


High-resolution circular spectropolarimetric observations, obtrained with
ESPaDOnS in the context of the BinaMIcS Large Program, have revealed a magnetic
field in the B3V secondary component of the SB2 binary system $\epsilon$ Lupi
(B2/B3). As the B2V primary is already known to be magnetic, this is the first
detection of a magnetic field in both components of an early-type binary
system. The longitudinal magnetic field of the primary is $\sim -200$ G; that
of the secondary $\sim +100$ G. Observations can be approximately reproduced by
a model assuming the magnetic axes of the two stars are anti-aligned, and
roughly parallel to their respective rotation axes. Estimated magnetospheric
radii indicate a high probability that their magnetospheres are interacting. As
many of the arguments for the different proposed formation scenarios of fossil
magnetic fields rely upon evidence drawn from investigations of close binaries,
in particular the rarity of magnetic ABO stars in close binaries and the
previous absence of any known close binary with two magnetic, massive stars,
this discovery may be an important new constraint on the origin of fossil
magnetic fields.


\sectionhack

\textbf{\huge Cross-lists} 

\section{Conflation: a new type of accelerated expansion}
\textit{Fertig, Angelika} ; \textit{Lehners, Jean-Luc}; \textit{Mallwitz, Enno}\\%
Comment: 20 pages, 5 figures\\%
Subjects: \textbf{High Energy Physics - Theory}; Astrophysics - Cosmology and Nongalactic Astrophysics\\%
Source: \href{http://arxiv.org/abs/1507.04742}{arXiv:1507.04742} [\href{http://arxiv.org/pdf/1507.04742.pdf}{PDF}]\\%


In the framework of scaler-tensor theories of gravity, we construct a new
kind of cosmological model that conflates inflation and ekpyrosis. During a
phase of conflation, the universe undergoes accelerated expansion, but with
crucial differences compared to ordinary inflation. In particular, the
potential energy is negative, which is of interest for supergravity and string
theory where both negative potentials and the required scalar-tensor couplings
are rather natural. A distinguishing feature of the model is that it does not
amplify adiabatic scalar and tensor fluctuations, and in particular does not
lead to eternal inflation and the associated infinities. We also show how
density fluctuations in accord with current observations may be generated by
adding a second scalar field to the model. Conflation may be viewed as
complementary to the recently proposed anamorphic universe of Ijjas and
Steinhardt.


\section{Effective Theory of Squeezed Correlation Functions}
\textit{Mirbabayi, Mehrdad} ; \selectlanguage{polish}\textit{Smonović, Marko}\selectlanguage{english}\\%
Comment: 18+6 pages\\%
Subjects: \textbf{High Energy Physics - Theory}; Astrophysics - Cosmology and Nongalactic Astrophysics\\%
Source: \href{http://arxiv.org/abs/1507.04755}{arXiv:1507.04755} [\href{http://arxiv.org/pdf/1507.04755.pdf}{PDF}]\\%


Various inflationary scenarios can often be distinguished from one another by
looking at the squeezed limit behavior of correlation functions. Therefore, it
is useful to have a framework designed to study this limit in a more systematic
and efficient way. We propose using an expansion in terms of weakly coupled
super-horizon degrees of freedom, which is argued to generically exist in a
near de Sitter space-time. The modes have a simple factorized form which leads
to factorization of the squeezed-limit correlation functions with power-law
behavior in $k_{\rm long}/k_{\rm short}$. This approach reproduces the known
results in single-, quasi-single-, and multi-field inflationary models.
However, it is applicable even if, unlike the above examples, the additional
degrees of freedom are not weakly coupled at sub-horizon scales. Stronger
results are derived in two-field (or sufficiently symmetric multi-field)
inflationary models. We discuss the observability of the non-Gaussian 3-point
function in the large-scale structure surveys, and argue that the squeezed
limit behavior has a higher detectability chance than equilateral behavior when
it scales as $(k_{\rm long}/k_{\rm short})^\Delta$ with $\Delta<1$ -- where
local non-Gaussianity corresponds to $\Delta=0$.


\section{Revolving D-branes and Spontaneous Gauge Symmetry Breaking}
\textit{Iso, Satoshi} ; \textit{Kitazawa, Noriaki}\\%
Comment: 22 pages, 3 figures\\%
Subjects: \textbf{High Energy Physics - Phenomenology}; Astrophysics - Cosmology and Nongalactic Astrophysics; High Energy Physics - Theory\\%
Source: \href{http://arxiv.org/abs/1507.04834}{arXiv:1507.04834} [\href{http://arxiv.org/pdf/1507.04834.pdf}{PDF}]\\%


We propose a new mechanism of spontaneous gauge symmetry breaking in the
world-volume theory of revolving D-branes around a fixed point of orbifolds. In
this paper, we consider a simple model of the T6/Z3 orbifold on which we put
D3-branes, D7-branes and their anti-branes. The configuration breaks
supersymmetry, but the R-R tadpole cancellation conditions are satisfied. A set
of three D3-branes at an orbifold fixed point can separate from the point, but
when they move perpendicular to the anti-D7-branes put on the fixed point, they
are forced to be pulled back due to an attractive interaction between the D3
and anti-D7 branes. In order to stabilize the separation of the D3-branes at
nonzero distance, we consider revolution of the D3-branes around the fixed
point. Then the gauge symmetry on D3-branes is spontaneously broken, and the
rank of the gauge group is reduced. The distance can be set at our will by
appropriately choosing the angular momentum of the revolving D3-branes, which
should be determined by the initial condition of the cosmological evolution of
D-brane configurations. The distance corresponds to the vacuum expectation
values of brane moduli fields in the world-volume theory and, if it is written
as M/Ms^2 in terms of the string scale Ms, the scale of gauge symmetry breaking
is given by M. Angular momentum conservation of revolving D3-branes assures the
stability of the scale M against Ms.


\section{First Measurement of the $^{96}$Ru(p,$\gamma$)$^{97}$Rh Cross Section
for the p-Process with a Storage Ring}
\textit{Mei, Bo} ; \textit{Aumann, Thomas}; \textit{Bishop, Shawn}; \textit{Blaum, Klaus}; \textit{Boretzky, Konstanze}; \textit{Bosch, Fritz}; \textit{Brandau, Carsten}; \selectlanguage{ngerman}\textit{Bräuning, Harald}; \textit{Davinson, Thomas}; \textit{Dillmann, Iris}; \textit{Dimopoulou, Christina}; \textit{Ershova, Olga}; \textit{Fülöp, Zsolt}; \textit{Geissel, Hans}; \textit{Glorius, Jan}; \textit{Gyürky, György}; \textit{Heil, Michael}; \textit{Käppeler, Franz}; \textit{Kelic-Heil, Aleksandra}; \textit{Kozhuharov, Christophor}; \textit{Langer, Christoph}; \textit{Bleis, Tudi Le}; \textit{Litvinov, Yuri}; \textit{Lotay, Gavin}; \textit{Marganiec, Justyna}; \textit{Münzenberg, Gottfried}; \textit{Nolden, Fritz}; \textit{Petridis, Nikolaos}; \textit{Plag, Ralf}; \textit{Popp, Ulrich}; \textit{Rastrepina, Ganna}; \textit{Reifarth, René}; \textit{Riese, Björn}; \textit{Rigollet, Catherine}; \textit{Scheidenberger, Christoph}; \textit{Simon, Haik}; \textit{Sonnabend, Kerstin}; \textit{Steck, Markus}; \textit{Stöhlke, Thomas}; \textit{Szücs, Tamás}; \textit{Sümmerer, Klaus}; \textit{Weber, Günter}; \textit{Weick, Helmut}; \textit{Winters, Danyal}; \textit{Winters, Natalya}; \textit{Woods, Philip}; \textit{Zhong, Qiping}\\%
Comment: 10 pages, 7 figs, Accepted for publication at PRC\\%
Subjects: \textbf{Nuclear Experiment}; Astrophysics - Instrumentation and Methods for Astrophysics\\%
Source: \href{http://arxiv.org/abs/1507.04916}{arXiv:1507.04916} [\href{http://arxiv.org/pdf/1507.04916.pdf}{PDF}]\\%


This work presents a direct measurement of the $^{96}$Ru($p,
\gamma$)$^{97}$Rh cross section via a novel technique using a storage ring,
which opens opportunities for reaction measurements on unstable nuclei. A
proof-of-principle experiment was performed at the storage ring ESR at GSI in
Darmstadt, where circulating $^{96}$Ru ions interacted repeatedly with a
hydrogen target. The $^{96}$Ru($p, \gamma$)$^{97}$Rh cross section between 9
and 11 MeV has been determined using two independent normalization methods. As
key ingredients in Hauser-Feshbach calculations, the $\gamma$-ray strength
function as well as the level density model can be pinned down with the
measured ($p, \gamma$) cross section. Furthermore, the proton optical potential
can be optimized after the uncertainties from the $\gamma$-ray strength
function and the level density have been removed. As a result, a constrained
$^{96}$Ru($p, \gamma$)$^{97}$Rh reaction rate over a wide temperature range is
recommended for $p$-process network calculations.


\section{Nonlinear oscillations of compact stars in the vicinity of the maximum
mass configuration}
\textit{Brillante, Alessandro} ; \textit{Mishustin, Igor}\\%
Comment: 15 pages, 8 figures, accepted for publication in EPL\\%
Subjects: \textbf{General Relativity and Quantum Cosmology}; Astrophysics - High Energy Astrophysical Phenomena; Astrophysics - Solar and Stellar Astrophysics\\%
Source: \href{http://arxiv.org/abs/1507.04919}{arXiv:1507.04919} [\href{http://arxiv.org/pdf/1507.04919.pdf}{PDF}]\\%


We solve the dynamical GR equations for the spherically symmetric evolution
of compact stars in the vicinity of the maximum mass, for which instability
sets in according to linear perturbation theory. The calculations are done with
the analytical Zeldovich-like EOS P=a(rho-rho_0) and with the TM1
parametrisation of the RMF model. The initial configurations for the dynamical
calculations are represented by spherical stars with equilibrium density
profile, which are perturbed by either (i) an artificially added inward
velocity field proportional to the radial coordinate, or (ii) a rarefaction
corresponding to a static and expanded star. These configurations are evolved
using a one-dimensional GR hydro code for ideal and barotropic fluids.
Depending on the initial conditions we obtain either stable oscillations or the
collapse to a black hole. The minimal amplitude of the perturbation, needed to
trigger gravitational collapse is evaluated. The approximate independence of
this energy on the type of perturbation is pointed out. At the threshold we
find type I critical behaviour for all stellar models considered and discuss
the dependence of the time scaling exponent on the baryon mass and EOS.


\section{Self-interacting dark matter and cosmology of a light scalar mediator}
\textit{Kainulainen, Kimmo} ; \textit{Tuominen, Kimmo}; \textit{Vaskonen, Ville}\\%
Comment: 17 pages, 4 figures\\%
Subjects: \textbf{High Energy Physics - Phenomenology}; Astrophysics - Cosmology and Nongalactic Astrophysics\\%
Source: \href{http://arxiv.org/abs/1507.04931}{arXiv:1507.04931} [\href{http://arxiv.org/pdf/1507.04931.pdf}{PDF}]\\%


We consider a fermionic dark matter candidate interacting via a scalar
mediator coupled with the Standard Model through a Higgs portal. We consider
general setting including both scalar and pseudoscalar interactions between the
scalar and fermion, and illustrate the relevant features for dark matter
abundance, direct search limits and collider constraints. In addition we
consider the dark matter self-interactions and show how the problems of a light
scalar mediator in the early universe can be resolved.


\section{Shocking Signals of Dark Matter Annihilation}
\textit{Davis, Jonathan H.} ; \textit{Silk, Joseph}; \textit{Boehm, Celine}; \textit{Kotera, Kumiko}; \textit{Norman, Colin}\\%
Comment: 9 pages, 4 figures\\%
Subjects: \textbf{High Energy Physics - Phenomenology}; Astrophysics - High Energy Astrophysical Phenomena\\%
Source: \href{http://arxiv.org/abs/1507.04962}{arXiv:1507.04962} [\href{http://arxiv.org/pdf/1507.04962.pdf}{PDF}]\\%


We examine whether charged particles injected by self-annihilating Dark
Matter into regions undergoing Diffuse Shock Acceleration (DSA) can be
accelerated to high energies. We consider three astrophysical sites where shock
acceleration is supposed to occur, namely the Galactic Centre, galaxy clusters
and Active Galactic Nuclei (AGN). For the Milky Way, we find that the
acceleration of cosmic rays injected by dark matter could lead to a bump in the
cosmic ray spectrum provided that the product of the efficiency of the
acceleration mechanism and the concentration of DM particles is high enough.
Among the various acceleration sources that we consider (namely supernova
remnants (SNRs), Fermi bubbles and AGN jets), we find that the Fermi bubbles
are a potentially more efficient accelerator than SNRs. However both could in
principle accelerate electrons and protons injected by dark matter to very high
energies. At the extragalactic level, the acceleration of dark matter
annihilation products could be responsible for enhanced radio emission from
colliding clusters and prediction of an increase of the anti-deuteron flux
generated near AGNs.


\section{High-pressure, temperature elasticity of Fe- and Al-bearing MgSiO3:
implications for the Earth's lower mantle}
\textit{Zhang, Shuai} ; \textit{Cottaar, Sanne}; \textit{Liu, Tao}; \textit{Stackhouse, Stephen}; \textit{Militzer, Burkhard}\\%
Comment: 26 pages, 6 figures; submitted to journal 8 June 2015\\%
Subjects: \textbf{Physics - Geophysics}; Astrophysics - Earth and Planetary Astrophysics; Condensed Matter - Materials Science\\%
Source: \href{http://arxiv.org/abs/1507.05025}{arXiv:1507.05025} [\href{http://arxiv.org/pdf/1507.05025.pdf}{PDF}]\\%


Fe and Al are two of the most important rock-forming elements other than Mg,
Si, and O. Their presence in the lower mantle's most abundant minerals, MgSiO_3
bridgmanite, MgSiO_3 post-perovskite and MgO periclase, alters their elastic
properties. However, knowledge on the thermoelasticity of Fe- and Al-bearing
MgSiO_3 bridgmanite, and post-perovskite is scarce. In this study, we perform
ab initio molecular dynamics to calculate the elastic and seismic properties of
pure, Fe^{3+}- and Fe^{2+}-, and Al^{3+}-bearing MgSiO_3 perovskite and
post-perovskite, over a wide range of pressures, temperatures, and Fe/Al
compositions. Our results show that a mineral assemblage resembling pyrolite
fits a 1D seismological model well, down to, at least, a few hundred kilometers
above the core-mantle boundary, i.e. the top of the D'' region. In D'', a
similar composition is still an excellent fit to the average velocities and
fairly approximate to the density. We also implement polycrystal plasticity
with a geodynamic model to predict resulting seismic anisotropy, and find
post-perovskite with predominant (001) slip across all compositions agrees best
with seismic observations in the D''.


\section{Testing the Kerr Paradigm with X-ray Observations}
\textit{Bambi, Cosimo} Comment: 6 pages, 3 figures. Talk given at the "14th Marcel Grossmann Meeting"
(12-18 July 2015, Rome, Italy). To appear in the conference proceedings\\%
Subjects: \textbf{General Relativity and Quantum Cosmology}; Astrophysics - High Energy Astrophysical Phenomena\\%
Source: \href{http://arxiv.org/abs/1507.05036}{arXiv:1507.05036} [\href{http://arxiv.org/pdf/1507.05036.pdf}{PDF}]\\%


Astrophysical black hole candidates are thought to be the Kerr black holes of
general relativity, but the actual nature of these objects has still to be
confirmed. The continuum-fitting and the iron line methods are currently the
only available techniques to probe the spacetime geometry around these bodies
and test the Kerr black hole paradigm. The continuum-fitting method is a robust
approach, but the shape of the disk's thermal spectrum is in general too simple
to measure the spin and to constrain possible deviations from the Kerr solution
at the same time. The iron line analysis is potentially a powerful technique,
but at the moment we do not have high quality data and a robust astrophysical
model.


\section{Piercing the Vainshtein screen: Local constraints on modified gravity}
\selectlanguage{ngerman}\textit{Jiménez, Jose Beltrán} ; \textit{Piazza, Federico}; \textit{Velten, Hermano}\\%
Comment: 5 pages, 2 figures\\%
Subjects: \textbf{General Relativity and Quantum Cosmology}; Astrophysics - Cosmology and Nongalactic Astrophysics; High Energy Physics - Theory\\%
Source: \href{http://arxiv.org/abs/1507.05047}{arXiv:1507.05047} [\href{http://arxiv.org/pdf/1507.05047.pdf}{PDF}]\\%


Modifications of gravity of the galileon type rely on the Vainshtein
screening to pass solar system tests. Such a mechanism suppresses the
fluctuations of the scalar field in the vicinity of localized sources, leaving
the gravitons as the only mediators of gravitational interactions. We highlight
that, in galileon 4 and 5 models and their shift-symmetric extensions, the
inevitable presence of the scalar field gradient modifies the dynamics of the
gravitons, leading to unscreened deviations from general relativity. The
observational bounds on the gravitational slip parameter constrain the
Horndeski-extensions of quartic and quintic galileons to the level of
$10^{-5}$. The corresponding beyond-Horndeski models can also be constrained to
the level of $10^{-2}$, by adding to the analysis the limits on the speed of
gravitational waves coming from the observations of the orbital decay of the
Hulse-Taylor pulsar.


\sectionhack

\textbf{\huge Replacements} 

\section{Global fits of the dark matter-nucleon effective interactions}
\textit{Catena, Riccardo} ; \textit{Gondolo, Paolo}\\%
Comment: 32 pages, 11 figures, replaced to match the published version\\%
Subjects: \textbf{High Energy Physics - Phenomenology}; Astrophysics - Cosmology and Nongalactic Astrophysics\\%
Source: \href{http://arxiv.org/abs/1405.2637}{arXiv:1405.2637} [\href{http://arxiv.org/pdf/1405.2637.pdf}{PDF}]\\%


The effective theory of isoscalar dark matter-nucleon interactions mediated
by heavy spin-one or spin-zero particles depends on 10 coupling constants
besides the dark matter particle mass. Here we compare this 11-dimensional
effective theory to current observations in a comprehensive statistical
analysis of several direct detection experiments, including the recent LUX,
SuperCDMS and CDMSlite results. From a multidimensional scan with about 3
million likelihood evaluations, we extract the marginalized posterior
probability density functions (a Bayesian approach) and the profile likelihoods
(a frequentist approach), as well as the associated credible regions and
confidence levels, for each coupling constant vs dark matter mass and for each
pair of coupling constants. We compare the Bayesian and frequentist approach in
the light of the currently limited amount of data. We find that current direct
detection data contain sufficient information to simultaneously constrain not
only the familiar spin-independent and spin-dependent interactions, but also
the remaining velocity and momentum dependent couplings predicted by the dark
matter-nucleon effective theory. For current experiments associated with a null
result, we find strong correlations between some pairs of coupling constants.
For experiments that claim a signal (i.e., CoGeNT and DAMA), we find that pairs
of coupling constants produce degenerate results.


\section{Prospects for direct detection of dark matter in an effective theory
approach}
\textit{Catena, Riccardo} Comment: 23 pages, 7 figures, replaced to match the published version\\%
Subjects: \textbf{High Energy Physics - Phenomenology}; Astrophysics - Cosmology and Nongalactic Astrophysics\\%
Source: \href{http://arxiv.org/abs/1406.0524}{arXiv:1406.0524} [\href{http://arxiv.org/pdf/1406.0524.pdf}{PDF}]\\%


We perform the first comprehensive analysis of the prospects for direct
detection of dark matter with future ton-scale detectors in the general
11-dimensional effective theory of isoscalar dark matter-nucleon interactions
mediated by a heavy spin-1 or spin-0 particle. The theory includes 8 momentum
and velocity dependent dark matter-nucleon interaction operators, besides the
familiar spin-independent and spin-dependent operators. From a variegated
sample of 27 benchmark points selected in the parameter space of the theory, we
simulate independent sets of synthetic data for ton-scale Germanium and Xenon
detectors. From the synthetic data, we then extract the marginal posterior
probability density functions and the profile likelihoods of the model
parameters. The associated Bayesian credible regions and frequentist confidence
intervals allow us to assess the prospects for direct detection of dark matter
at the 27 benchmark points. First, we analyze the data assuming the knowledge
of the correct dark matter nucleon-interaction type, as it is commonly done for
the familiar spin-independent and spin-dependent interactions. Then, we analyze
the simulations extracting the dark matter-nucleon interaction type from the
data directly, in contrast to standard analyses. This second approach requires
an extensive exploration of the full 11-dimensional parameter space of the dark
matter-nucleon effective theory. Interestingly, we identify 5 scenarios where
the dark matter mass and the dark matter-nucleon interaction type can be
reconstructed from the data simultaneously. We stress the importance of
extracting the dark matter nucleon-interaction type from the data directly,
discussing the main challenges found addressing this complex 11-dimensional
problem.


\section{Model independent limits on an ultra-light gravitino from Supernovae}
\textit{Catena, Riccardo} ; \textit{Covi, Laura}; \textit{Emken, Timon}\\%
Comment: 18 pages, 5 figures, replaced to match the published version\\%
Subjects: \textbf{High Energy Physics - Phenomenology}; Astrophysics - Cosmology and Nongalactic Astrophysics\\%
Source: \href{http://arxiv.org/abs/1410.0314}{arXiv:1410.0314} [\href{http://arxiv.org/pdf/1410.0314.pdf}{PDF}]\\%


We revisit astrophysical constraints on models with an ultra-light gravitino,
in particular extending the analysis to more general models and the case of
R-parity breaking. These constraints allow to restrict the value of the
gravitino mass depending on the masses of scalar moduli. We perform both a
frequentist and bayesian analysis and we find comparable results, even if the
bayesian analysis is in part affected by volume effects. Only a small window of
gravitino masses can be excluded by the SN constraints in a model-independent
way, while limits obtained with a definite assumption on the scalar masses
result more stringent.


\section{Form factors for dark matter capture by the Sun in effective theories}
\textit{Catena, Riccardo} ; \textit{Schwabe, Bodo}\\%
Comment: 37 pages, 9 figures, replaced to match the published version\\%
Subjects: \textbf{High Energy Physics - Phenomenology}; Astrophysics - Cosmology and Nongalactic Astrophysics\\%
Source: \href{http://arxiv.org/abs/1501.03729}{arXiv:1501.03729} [\href{http://arxiv.org/pdf/1501.03729.pdf}{PDF}]\\%


In the effective theory of isoscalar and isovector dark matter-nucleon
interactions mediated by a heavy spin-1 or spin-0 particle, 8 isotope-dependent
nuclear response functions can be generated in the dark matter scattering by
nuclei. We compute the 8 nuclear response functions for the 16 most abundant
elements in the Sun, i.e. H, $^{3}$He, $^{4}$He, $^{12}$C, $^{14}$N, $^{16}$O,
$^{20}$Ne, $^{23}$Na, $^{24}$Mg, $^{27}$Al, $^{28}$Si, $^{32}$S, $^{40}$Ar,
$^{40}$Ca, $^{56}$Fe, and $^{59}$Ni, through numerical shell model
calculations. We use our response functions to compute the rate of dark matter
capture by the Sun for all isoscalar and isovector dark matter-nucleon
effective interactions, including several operators previously considered for
dark matter direct detection only. We study in detail the dependence of the
capture rate on specific dark matter-nucleon interaction operators, and on the
different elements in the Sun. We find that a so far neglected momentum
dependent dark matter coupling to the nuclear vector charge gives a larger
contribution to the capture rate than the constant spin-dependent interaction
commonly included in dark matter searches at neutrino telescopes. Our
investigation lays the foundations for model independent analyses of dark
matter induced neutrino signals from the Sun. The nuclear response functions
obtained in this study are listed in analytic form in an appendix, ready to be
used in other projects.


\section{Planck 2015 results. VII. HFI TOI and beam processing}
\textit{Planck Collaboration} ; \textit{Adam, R.}; \textit{Ade, P. A. R.}; \textit{Aghanim, N.}; \textit{Arnaud, M.}; \textit{Ashdown, M.}; \textit{Aumont, J.}; \textit{Baccigalupi, C.}; \textit{Banday, A. J.}; \textit{Barreiro, R. B.}; \textit{Bartolo, N.}; \textit{Battaner, E.}; \textit{Benabed, K.}; \textit{Benoit, A.}; \textit{Benoit-Levy, A.}; \textit{Bernard, J. -P.}; \textit{Bersanelli, M.}; \textit{Bertincourt, B.}; \textit{Bielewicz, P.}; \textit{Bock, J. J.}; \textit{Bonavera, L.}; \textit{Bond, J. R.}; \textit{Borrill, J.}; \textit{Bouchet, F. R.}; \textit{Boulanger, F.}; \textit{Bucher, M.}; \textit{Burigana, C.}; \textit{Calabrese, E.}; \textit{Cardoso, J. -F.}; \textit{Catalano, A.}; \textit{Challinor, A.}; \textit{Chamballu, A.}; \textit{Chary, R. -R.}; \textit{Chiang, H. C.}; \textit{Christensen, P. R.}; \textit{Clements, D. L.}; \textit{Colombi, S.}; \textit{Colombo, L. P. L.}; \textit{Combet, C.}; \textit{Couchot, F.}; \textit{Coulais, A.}; \textit{Crill, B. P.}; \textit{Curto, A.}; \textit{Cuttaia, F.}; \textit{Danese, L.}; \textit{Davies, R. D.}; \textit{Davis, R. J.}; \textit{de Bernardis, P.}; \textit{de Rosa, A.}; \textit{de Zotti, G.}; \textit{Delabrouille, J.}; \textit{Delouis, J. -M.}; \textit{Desert, F. -X.}; \textit{Diego, J. M.}; \textit{Dole, H.}; \textit{Donzelli, S.}; \textit{Dore, O.}; \textit{Douspis, M.}; \textit{Ducout, A.}; \textit{Dupac, X.}; \textit{Efstathiou, G.}; \textit{Elsner, F.}; \textit{Ensslin, T. A.}; \textit{Eriksen, H. K.}; \textit{Falgarone, E.}; \textit{Fergusson, J.}; \textit{Finelli, F.}; \textit{Forni, O.}; \textit{Frailis, M.}; \textit{Fraisse, A. A.}; \textit{Franceschi, E.}; \textit{Frejsel, A.}; \textit{Galeotta, S.}; \textit{Galli, S.}; \textit{Ganga, K.}; \textit{Ghosh, T.}; \textit{Giard, M.}; \textit{Giraud-Heraud, Y.}; \textit{Gjerlow, E.}; \textit{Gonzalez-Nuevo, J.}; \textit{Gorski, K. M.}; \textit{Gratton, S.}; \textit{Gruppuso, A.}; \textit{Gudmundsson, J. E.}; \textit{Hansen, F. K.}; \textit{Hanson, D.}; \textit{Harrison, D. L.}; \textit{Henrot-Versille, S.}; \textit{Herranz, D.}; \textit{Hildebrandt, S. R.}; \textit{Hivon, E.}; \textit{Hobson, M.}; \textit{Holmes, W. A.}; \textit{Hornstrup, A.}; \textit{Hovest, W.}; \textit{Huffenberger, K. M.}; \textit{Hurier, G.}; \textit{Jaffe, A. H.}; \textit{Jaffe, T. R.}; \textit{Jones, W. C.}; \textit{Juvela, M.}; \textit{Keihanen, E.}; \textit{Keskitalo, R.}; \textit{Kisner, T. S.}; \textit{Kneissl, R.}; \textit{Knoche, J.}; \textit{Kunz, M.}; \textit{Kurki-Suonio, H.}; \textit{Lagache, G.}; \textit{Lamarre, J. -M.}; \textit{Lasenby, A.}; \textit{Lattanzi, M.}; \textit{Lawrence, C. R.}; \textit{Jeune, M. Le}; \textit{Leahy, J. P.}; \textit{Lellouch, E.}; \textit{Leonardi, R.}; \textit{Lesgourgues, J.}; \textit{Levrier, F.}; \textit{Liguori, M.}; \textit{Lilje, P. B.}; \textit{Linden-Vornle, M.}; \textit{Lopez-Caniego, M.}; \textit{Lubin, P. M.}; \textit{Macias-Perez, J. F.}; \textit{Maggio, G.}; \textit{Maino, D.}; \textit{Mandolesi, N.}; \textit{Mangilli, A.}; \textit{Maris, M.}; \textit{Martin, P. G.}; \textit{Martinez-Gonzalez, E.}; \textit{Masi, S.}; \textit{Matarrese, S.}; \textit{McGehee, P.}; \textit{Melchiorri, A.}; \textit{Mendes, L.}; \textit{Mennella, A.}; \textit{Migliaccio, M.}; \textit{Mitra, S.}; \textit{Miville-Deschenes, M. -A.}; \textit{Moneti, A.}; \textit{Montier, L.}; \textit{Moreno, R.}; \textit{Morgante, G.}; \textit{Mortlock, D.}; \textit{Moss, A.}; \textit{Mottet, S.}; \textit{Munshi, D.}; \textit{Murphy, J. A.}; \textit{Naselsky, P.}; \textit{Nati, F.}; \textit{Natoli, P.}; \textit{Netterfield, C. B.}; \textit{Norgaard-Nielsen, H. U.}; \textit{Noviello, F.}; \textit{Novikov, D.}; \textit{Novikov, I.}; \textit{Oxborrow, C. A.}; \textit{Paci, F.}; \textit{Pagano, L.}; \textit{Pajot, F.}; \textit{Paoletti, D.}; \textit{Pasian, F.}; \textit{Patanchon, G.}; \textit{Pearson, T. J.}; \textit{Perdereau, O.}; \textit{Perotto, L.}; \textit{Perrotta, F.}; \textit{Pettorino, V.}; \textit{Piacentini, F.}; \textit{Piat, M.}; \textit{Pierpaoli, E.}; \textit{Pietrobon, D.}; \textit{Plaszczynski, S.}; \textit{Pointecouteau, E.}; \textit{Polenta, G.}; \textit{Pratt, G. W.}; \textit{Prezeau, G.}; \textit{Prunet, S.}; \textit{Puget, J. -L.}; \textit{Rachen, J. P.}; \textit{Reinecke, M.}; \textit{Remazeilles, M.}; \textit{Renault, C.}; \textit{Renzi, A.}; \textit{Ristorcelli, I.}; \textit{Rocha, G.}; \textit{Rosset, C.}; \textit{Rossetti, M.}; \textit{Roudier, G.}; \textit{Rowan-Robinson, M.}; \textit{Rusholme, B.}; \textit{Sandri, M.}; \textit{Santos, D.}; \textit{Sauve, A.}; \textit{Savelainen, M.}; \textit{Savini, G.}; \textit{Scott, D.}; \textit{Seiffert, M. D.}; \textit{Shellard, E. P. S.}; \textit{Spencer, L. D.}; \textit{Stolyarov, V.}; \textit{Stompor, R.}; \textit{Sudiwala, R.}; \textit{Sutton, D.}; \textit{Suur-Uski, A. -S.}; \textit{Sygnet, J. -F.}; \textit{Tauber, J. A.}; \textit{Terenzi, L.}; \textit{Toffolatti, L.}; \textit{Tomasi, M.}; \textit{Tristram, M.}; \textit{Tucci, M.}; \textit{Tuovinen, J.}; \textit{Valenziano, L.}; \textit{Valiviita, J.}; \textit{Van Tent, B.}; \textit{Vibert, L.}; \textit{Vielva, P.}; \textit{Villa, F.}; \textit{Wade, L. A.}; \textit{Wandelt, B. D.}; \textit{Watson, R.}; \textit{Wehus, I. K.}; \textit{Yvon, D.}; \textit{Zacchei, A.}; \textit{Zonca, A.}\\%
Subjects: \textbf{Astrophysics - Instrumentation and Methods for Astrophysics}\\%
Source: \href{http://arxiv.org/abs/1502.01586}{arXiv:1502.01586} [\href{http://arxiv.org/pdf/1502.01586.pdf}{PDF}]\\%


The Planck High Frequency Instrument (HFI) has observed the full sky at six
frequencies (100, 143, 217, 353, 545, and 857 GHz) in intensity and at four
frequencies in linear polarization (100, 143, 217, and 353 GHz). In order to
obtain sky maps, the time-ordered information (TOI) containing the detector and
pointing samples must be processed and the angular response must be assessed.
The full mission TOI is included in the Planck 2015 release. This paper
describes the HFI TOI and beam processing for the 2015 release. HFI calibration
and map-making are described in a companion paper. The main pipeline has been
modified since the last release (2013 nominal mission in intensity only), by
including a correction for the non-linearity of the warm readout and by
improving the model of the bolometer time response. The beam processing is an
essential tool that derives the angular response used in all the Planck science
papers and we report an improvement in the effective beam window function
uncertainty of more than a factor 10 relative to the 2013 release. Noise
correlations introduced by pipeline filtering function are assessed using
dedicated simulations. Angular cross-power spectra using datasets that are
decorrelated in time are immune to the main systematic effects.


\section{Planck 2015 results. VIII. High Frequency Instrument data processing:
Calibration and maps}
\textit{Planck Collaboration} ; \textit{Adam, R.}; \textit{Ade, P. A. R.}; \textit{Aghanim, N.}; \textit{Arnaud, M.}; \textit{Ashdown, M.}; \textit{Aumont, J.}; \textit{Baccigalupi, C.}; \textit{Banday, A. J.}; \textit{Barreiro, R. B.}; \textit{Bartolo, N.}; \textit{Battaner, E.}; \textit{Benabed, K.}; \selectlanguage{ngerman}\textit{Benoît, A.}; \textit{Benoit-Lévy, A.}; \textit{Bernard, J. -P.}; \textit{Bersanelli, M.}; \textit{Bertincourt, B.}; \textit{Bielewicz, P.}; \textit{Bock, J. J.}; \textit{Bonavera, L.}; \textit{Bond, J. R.}; \textit{Borrill, J.}; \textit{Bouchet, F. R.}; \textit{Boulanger, F.}; \textit{Bucher, M.}; \textit{Burigana, C.}; \textit{Calabrese, E.}; \textit{Cardoso, J. -F.}; \textit{Catalano, A.}; \textit{Challinor, A.}; \textit{Chamballu, A.}; \textit{Chiang, H. C.}; \textit{Christensen, P. R.}; \textit{Clements, D. L.}; \textit{Colombi, S.}; \textit{Colombo, L. P. L.}; \textit{Combet, C.}; \textit{Couchot, F.}; \textit{Coulais, A.}; \textit{Crill, B. P.}; \textit{Curto, A.}; \textit{Cuttaia, F.}; \textit{Danese, L.}; \textit{Davies, R. D.}; \textit{Davis, R. J.}; \textit{de Bernardis, P.}; \textit{de Rosa, A.}; \textit{de Zotti, G.}; \textit{Delabrouille, J.}; \textit{Delouis, J. -M.}; \textit{Désert, F. -X.}; \textit{Diego, J. M.}; \textit{Dole, H.}; \textit{Donzelli, S.}; \textit{Doré, O.}; \textit{Douspis, M.}; \textit{Ducout, A.}; \textit{Dupac, X.}; \textit{Efstathiou, G.}; \textit{Elsner, F.}; \textit{Enßlin, T. A.}; \textit{Eriksen, H. K.}; \textit{Falgarone, E.}; \textit{Fergusson, J.}; \textit{Finelli, F.}; \textit{Forni, O.}; \textit{Frailis, M.}; \textit{Fraisse, A. A.}; \textit{Franceschi, E.}; \textit{Frejsel, A.}; \textit{Galeotta, S.}; \textit{Galli, S.}; \textit{Ganga, K.}; \textit{Ghosh, T.}; \textit{Giard, M.}; \textit{Giraud-Héraud, Y.}; \textit{Gjerløw, E.}; \textit{González-Nuevo, J.}; \textit{Górski, K. M.}; \textit{Gratton, S.}; \textit{Gruppuso, A.}; \textit{Gudmundsson, J. E.}; \textit{Hansen, F. K.}; \textit{Hanson, D.}; \textit{Harrison, D. L.}; \textit{Henrot-Versillé, S.}; \textit{Herranz, D.}; \textit{Hildebrandt, S. R.}; \textit{Hivon, E.}; \textit{Hobson, M.}; \textit{Holmes, W. A.}; \textit{Hornstrup, A.}; \textit{Hovest, W.}; \textit{Huffenberger, K. M.}; \textit{Hurier, G.}; \textit{Jaffe, A. H.}; \textit{Jaffe, T. R.}; \textit{Jones, W. C.}; \textit{Juvela, M.}; \textit{Keihänen, E.}; \textit{Keskitalo, R.}; \textit{Kisner, T. S.}; \textit{Kneissl, R.}; \textit{Knoche, J.}; \textit{Kunz, M.}; \textit{Kurki-Suonio, H.}; \textit{Lagache, G.}; \textit{Lamarre, J. -M.}; \textit{Lasenby, A.}; \textit{Lattanzi, M.}; \textit{Lawrence, C. R.}; \textit{Jeune, M. Le}; \textit{Leahy, J. P.}; \textit{Lellouch, E.}; \textit{Leonardi, R.}; \textit{Lesgourgues, J.}; \textit{Levrier, F.}; \textit{Liguori, M.}; \textit{Lilje, P. B.}; \textit{Linden-Vørnle, M.}; \textit{López-Caniego, M.}; \textit{Lubin, P. M.}; \textit{Macías-Pérez, J. F.}; \textit{Maggio, G.}; \textit{Maino, D.}; \textit{Mandolesi, N.}; \textit{Mangilli, A.}; \textit{Maris, M.}; \textit{Martin, P. G.}; \textit{Martínez-González, E.}; \textit{Masi, S.}; \textit{Matarrese, S.}; \textit{McGehee, P.}; \textit{Melchiorri, A.}; \textit{Mendes, L.}; \textit{Mennella, A.}; \textit{Migliaccio, M.}; \textit{Mitra, S.}; \textit{Miville-Deschênes, M. -A.}; \textit{Moneti, A.}; \textit{Montier, L.}; \textit{Moreno, R.}; \textit{Morgante, G.}; \textit{Mortlock, D.}; \textit{Moss, A.}; \textit{Mottet, S.}; \textit{Munshi, D.}; \textit{Murphy, J. A.}; \textit{Naselsky, P.}; \textit{Nati, F.}; \textit{Natoli, P.}; \textit{Netterfield, C. B.}; \textit{Nørgaard-Nielsen, H. U.}; \textit{Noviello, F.}; \textit{Novikov, D.}; \textit{Novikov, I.}; \textit{Oxborrow, C. A.}; \textit{Paci, F.}; \textit{Pagano, L.}; \textit{Pajot, F.}; \textit{Paoletti, D.}; \textit{Pasian, F.}; \textit{Patanchon, G.}; \textit{Pearson, T. J.}; \textit{Perdereau, O.}; \textit{Perotto, L.}; \textit{Perrotta, F.}; \textit{Pettorino, V.}; \textit{Piacentini, F.}; \textit{Piat, M.}; \textit{Pierpaoli, E.}; \textit{Pietrobon, D.}; \textit{Plaszczynski, S.}; \textit{Pointecouteau, E.}; \textit{Polenta, G.}; \textit{Pratt, G. W.}; \textit{Prézeau, G.}; \textit{Prunet, S.}; \textit{Puget, J. -L.}; \textit{Rachen, J. P.}; \textit{Reinecke, M.}; \textit{Remazeilles, M.}; \textit{Renault, C.}; \textit{Renzi, A.}; \textit{Ristorcelli, I.}; \textit{Rocha, G.}; \textit{Rosset, C.}; \textit{Rossetti, M.}; \textit{Roudier, G.}; \textit{Rusholme, B.}; \textit{Sandri, M.}; \textit{Santos, D.}; \textit{Sauvé, A.}; \textit{Savelainen, M.}; \textit{Savini, G.}; \textit{Scott, D.}; \textit{Seiffert, M. D.}; \textit{Shellard, E. P. S.}; \textit{Spencer, L. D.}; \textit{Stolyarov, V.}; \textit{Stompor, R.}; \textit{Sudiwala, R.}; \textit{Sutton, D.}; \textit{Suur-Uski, A. -S.}; \textit{Sygnet, J. -F.}; \textit{Tauber, J. A.}; \textit{Terenzi, L.}; \textit{Toffolatti, L.}; \textit{Tomasi, M.}; \textit{Tristram, M.}; \textit{Tucci, M.}; \textit{Tuovinen, J.}; \textit{Valenziano, L.}; \textit{Valiviita, J.}; \textit{Van Tent, B.}; \textit{Vibert, L.}; \textit{Vielva, P.}; \textit{Villa, F.}; \textit{Wade, L. A.}; \textit{Wandelt, B. D.}; \textit{Watson, R.}; \textit{Wehus, I. K.}; \textit{Yvon, D.}; \textit{Zacchei, A.}; \textit{Zonca, A.}\\%
Comment: 28 pages, 19 figures, one of the papers associated with the 2015
Planck data release\\%
Subjects: \textbf{Astrophysics - Cosmology and Nongalactic Astrophysics}; Astrophysics - Instrumentation and Methods for Astrophysics\\%
Source: \href{http://arxiv.org/abs/1502.01587}{arXiv:1502.01587} [\href{http://arxiv.org/pdf/1502.01587.pdf}{PDF}]\\%


This paper describes the processing applied to the Planck High Frequency
Instrument (HFI) cleaned, time-ordered information to produce photometrically
calibrated maps in temperature and (for the first time) in polarization. The
data from the entire 2.5 year HFI mission include almost five independent
full-sky surveys. HFI observes the sky over a broad range of frequencies, from
100 to 857 GHz. To obtain the best accuracy on the calibration over such a
large range, two different photometric calibration schemes have been used. The
545 and 857 GHz data are calibrated using models of planetary atmospheric
emission. The lower frequencies (from 100 to 353 GHz) are calibrated using the
time-variable cosmological microwave background dipole, which we call the
"orbital dipole". This source of calibration only depends on the satellite
velocity with respect to the solar system. Using a CMB temperature of 2.7255
+/- 0.0006 K, it permits an independent measurement of the amplitude of the CMB
solar dipole (3364.3 +/- 1.5 \mu K) which is approximatively 1\sigma\ higher
than the WMAP measurement with a direction that is consistent between both
experiments. We describe the pipeline used to produce the maps of intensity and
linear polarization from the HFI timelines, and the scheme used to set the zero
level of the maps a posteriori. We also summarize the noise characteristics of
the HFI maps in the 2015 Planck data release and present some null tests to
assess their quality. Finally, we discuss the major systematic effects and in
particular the leakage induced by flux mismatch between the detectors that
leads to spurious polarization signal.


\section{Spatial and Spectral Modeling of the Gamma-ray Distribution in the Large
Magellanic Cloud}
\textit{Foreman, Gary} ; \textit{Chu, You-Hua}; \textit{Gruendl, Robert}; \textit{Hughes, Annie}; \textit{Fields, Brian}; \textit{Ricker, Paul}\\%
Comment: 20 pages, 12 figures, published in ApJ\\%
Subjects: \textbf{Astrophysics - High Energy Astrophysical Phenomena}\\%
Source: \href{http://arxiv.org/abs/1502.04337}{arXiv:1502.04337} [\href{http://arxiv.org/pdf/1502.04337.pdf}{PDF}]\\%


We perform spatial and spectral analyses of the Large Magellanic Cloud (LMC)
gamma-ray emission collected over 66 months by the Fermi Gamma-ray Space
Telescope. In our spatial analysis, we model the LMC cosmic-ray distribution
and gamma-ray production using observed maps of the LMC interstellar medium,
star formation history, interstellar radiation field, and synchrotron emission.
We use bootstrapping of the data to quantify the robustness of spatial model
performance. We model the LMC gamma-ray spectrum using fitting functions
derived from the physics of $\pi^0$ decay, bremsstrahlung, and inverse Compton
scattering. We find the integrated gamma-ray flux of the LMC from 200 MeV to 20
GeV to be $1.38 \pm 0.02 \times 10^{-7}$ ph cm$^{-2}$ s$^{-1}$, of which we
attribute about 10\% to inverse Compton scattering and 40\% to bremsstrahlung.
From our work, we conclude that the spectral index of the LMC cosmic-ray proton
population is 2.4$\pm$0.2, and we find that cosmic-ray energy loss through
gamma-ray production is concentrated within a few hundred pc of acceleration
sites. Assuming cosmic-ray energy equipartition with magnetic fields, we
estimate LMC cosmic rays encounter an average magnetic field strength ~3
$\mu$G.


\section{Dark matter signals at neutrino telescopes in effective theories}
\textit{Catena, Riccardo} Comment: 27 pages, 13 figures, replaced to match the published version\\%
Subjects: \textbf{High Energy Physics - Phenomenology}; Astrophysics - Cosmology and Nongalactic Astrophysics\\%
Source: \href{http://arxiv.org/abs/1503.04109}{arXiv:1503.04109} [\href{http://arxiv.org/pdf/1503.04109.pdf}{PDF}]\\%


We constrain the effective theory of one-body dark matter-nucleon
interactions using neutrino telescope observations. We derive exclusion limits
on the 28 coupling constants of the theory, exploring interaction operators
previously considered in dark matter direct detection only, and using new
nuclear response functions recently derived through nuclear structure
calculations. We determine for what interactions neutrino telescopes are
superior to current direct detection experiments, and show that Hydrogen is not
the most important element in the exclusion limit calculation for the majority
of the spin-dependent operators.


\section{Accurate photometric redshift probability density estimation - method
comparison and application}
\textit{Rau, Markus Michael} ; \textit{Seitz, Stella}; \textit{Brimioulle, Fabrice}; \textit{Frank, Eibe}; \textit{Friedrich, Oliver}; \textit{Gruen, Daniel}; \textit{Hoyle, Ben}\\%
Comment: 17 pages, 19 figures, updated to match version accepted in the MNRAS\\%
Subjects: \textbf{Astrophysics - Cosmology and Nongalactic Astrophysics}\\%
Source: \href{http://arxiv.org/abs/1503.08215}{arXiv:1503.08215} [\href{http://arxiv.org/pdf/1503.08215.pdf}{PDF}]\\%


We introduce an ordinal classification algorithm for photometric redshift
estimation, which significantly improves the reconstruction of photometric
redshift probability density functions (PDFs) for individual galaxies and
galaxy samples. As a use case we apply our method to CFHTLS galaxies. The
ordinal classification algorithm treats distinct redshift bins as ordered
values, which improves the quality of photometric redshift PDFs, compared with
non-ordinal classification architectures. We also propose a new single value
point estimate of the galaxy redshift, that can be used to estimate the full
redshift PDF of a galaxy sample. This method is competitive in terms of
accuracy with contemporary algorithms, which stack the full redshift PDFs of
all galaxies in the sample, but requires orders of magnitudes less storage
space.
The methods described in this paper greatly improve the log-likelihood of
individual object redshift PDFs, when compared with a popular Neural Network
code (ANNz). In our use case, this improvement reaches 50\% for high redshift
objects ($z \geq 0.75$).
We show that using these more accurate photometric redshift PDFs will lead to
a reduction in the systematic biases by up to a factor of four, when compared
with less accurate PDFs obtained from commonly used methods. The cosmological
analyses we examine and find improvement upon are the following: gravitational
lensing cluster mass estimates, modelling of angular correlation functions, and
modelling of cosmic shear correlation functions.


\section{Gravitational wave background from Standard Model physics: Qualitative
features}
\textit{Ghiglieri, J.} ; \textit{Laine, M.}\\%
Comment: 19 pages. v2: clarifications and references added, published version\\%
Subjects: \textbf{High Energy Physics - Phenomenology}; Astrophysics - Cosmology and Nongalactic Astrophysics\\%
Source: \href{http://arxiv.org/abs/1504.02569}{arXiv:1504.02569} [\href{http://arxiv.org/pdf/1504.02569.pdf}{PDF}]\\%


Because of physical processes ranging from microscopic particle collisions to
macroscopic hydrodynamic fluctuations, any plasma in thermal equilibrium emits
gravitational waves. For the largest wavelengths the emission rate is
proportional to the shear viscosity of the plasma. In the Standard Model at T >
160 GeV, the shear viscosity is dominated by the most weakly interacting
particles, right-handed leptons, and is relatively large. We estimate the order
of magnitude of the corresponding spectrum of gravitational waves. Even though
at small frequencies (corresponding to the sub-Hz range relevant for planned
observatories such as eLISA) this background is tiny compared with that from
non-equilibrium sources, the total energy carried by the high-frequency part of
the spectrum is non-negligible if the production continues for a long time. We
suggest that this may constrain (weakly) the highest temperature of the
radiation epoch. Observing the high-frequency part directly sets a very
ambitious goal for future generations of GHz-range detectors.


\section{Limits on the fluctuating part of $y$-type distortion monopole from
Planck and SPT results}
\textit{Khatri, Rishi} ; \textit{Sunyaev, Rashid}\\%
Comment: Added comparison with Planck NILC/MILCA maps, and figures of y
probability distribution function. Accepted version\\%
Subjects: \textbf{Astrophysics - Cosmology and Nongalactic Astrophysics}; Astrophysics - Astrophysics of Galaxies; High Energy Physics - Phenomenology\\%
Source: \href{http://arxiv.org/abs/1505.00781}{arXiv:1505.00781} [\href{http://arxiv.org/pdf/1505.00781.pdf}{PDF}]\\%


We use the published Planck and SPT cluster catalogs and recently published
$y$-distortion maps to put strong observational limits on the contribution of
the fluctuating part of the $y$-type distortions to the $y$-distortion
monopole. Our bounds are $5.4\times 10^{-8} < \langle y\rangle < 2.2\times
10^{-6}$. Our upper bound is a factor of 6.8 stronger than the currently best
upper $95\%$ confidence limit from COBE-FIRAS of $\langle y\rangle <15\times
10^{-6}$. In the standard cosmology, large scale structure is the only source
of such distortions and our limits therefore constrain the baryonic physics
involved in the formation of the large scale structure. Our lower limit, from
the detected clusters in the Planck and SPT catalogs, also implies that a
Pixie-like experiment should detect the $y$-distortion monopole at
$>27$-$\sigma$. The biggest sources of uncertainty in our upper limit are the
monopole offsets between different HFI channel maps that we estimate to be
$<10^{-6}$.


\section{Non-Abelian dark matter and dark radiation}
\textit{Buen-Abad, Manuel A.} ; \textit{Marques-Tavares, Gustavo}; \textit{Schmaltz, Martin}\\%
Comment: 25 pages, 8 figures; v2: minor improvements, references added; v3:
added references and an acknowledgement note to J. Lesgourgues; accepted for
publication in PRD\\%
Subjects: \textbf{High Energy Physics - Phenomenology}; Astrophysics - Cosmology and Nongalactic Astrophysics\\%
Source: \href{http://arxiv.org/abs/1505.03542}{arXiv:1505.03542} [\href{http://arxiv.org/pdf/1505.03542.pdf}{PDF}]\\%


We propose a new class of dark matter models with unusual phenomenology. What
is ordinary about our models is that dark matter particles are WIMPs, they are
weakly coupled to the Standard Model and have weak scale masses. What is
unusual is that they come in multiplets of a new "dark" non-Abelian gauge group
with milli-weak coupling. The massless dark gluons of this dark gauge group
contribute to the energy density of the universe as a form of weakly
self-interacting dark radiation. In this paper we explore the consequences of
having i.) dark matter in multiplets ii.) self-interacting dark radiation and
iii.) dark matter which is weakly coupled to dark radiation. We find that i.)
dark matter cross sections are modified by multiplicity factors which have
significant consequences for collider searches and indirect detection, ii.)
dark gluons have thermal abundances which affect the CMB as dark radiation.
Unlike additional massless neutrino species the dark gluons are interacting and
have vanishing viscosity and iii.) the coupling of dark radiation to dark
matter represents a new mechanism for damping the large scale structure power
spectrum. A combination of additional radiation and slightly damped structure
is interesting because it can remove tensions between global $\Lambda$CDM fits
from the CMB and direct measurements of the Hubble expansion rate ($H_0$) and
large scale structure ($\sigma_8$).


\section{Three-dimensional core-collapse supernova simulated using a 15 $M_\odot$
progenitor}
\textit{Lentz, Eric J.} ; \textit{Bruenn, Stephen W.}; \textit{Hix, W. Raphael}; \textit{Mezzacappa, Anthony}; \textit{Messer, O. E. Bronson}; \textit{Endeve, Eirik}; \textit{Blondin, John M.}; \textit{Harris, J. Austin}; \textit{Marronetti, Pedro}; \textit{Yakunin, Konstantin N.}\\%
Comment: 7 pages, accepted for publication in ApJ Letters, animation available
at ChimeraSN.org\\%
Subjects: \textbf{Astrophysics - Solar and Stellar Astrophysics}\\%
Source: \href{http://arxiv.org/abs/1505.05110}{arXiv:1505.05110} [\href{http://arxiv.org/pdf/1505.05110.pdf}{PDF}]\\%


We have performed ab initio neutrino radiation hydrodynamics simulations in
three and two spatial dimensions (3D and 2D) of core-collapse supernovae from
the same 15 $M_\odot$ progenitor through 440 ms after core bounce. Both 3D and
2D models achieve explosions, however, the onset of explosion (shock revival)
is delayed by $\sim$100 ms in 3D relative to the 2D counterpart and the growth
of the diagnostic explosion energy is slower. This is consistent with
previously reported 3D simulations utilizing iron-core progenitors with dense
mantles. In the $\sim$100 ms before the onset of explosion, diagnostics of
neutrino heating and turbulent kinetic energy favor earlier explosion in 2D.
During the delay, the angular scale of convective plumes reaching the shock
surface grows and explosion in 3D is ultimately lead by a single, large-angle
plume, giving the expanding shock a directional orientation not dissimilar from
those imposed by axial symmetry in 2D simulations. We posit that shock revival
and explosion in the 3D simulation may be delayed until sufficiently large
plumes form, whereas such plumes form more rapidly in 2D, permitting earlier
explosions.


\section{Resolving vortices with an isothermal HLLC Riemann solver}
\textit{Jung, Manuel} ; \textit{Illenseer, Tobias F.}; \textit{Duschl, Wolfgang J.}\\%
Comment: Not ready yet\\%
Subjects: \textbf{Physics - Computational Physics}; Astrophysics - Instrumentation and Methods for Astrophysics; Physics - Fluid Dynamics\\%
Source: \href{http://arxiv.org/abs/1505.06974}{arXiv:1505.06974} [\href{http://arxiv.org/pdf/1505.06974.pdf}{PDF}]\\%


The importance of contact discontinuities in 2D isothermal flows has rarely
been discussed, since most Riemann solvers are derived for 1D Euler equations.
We present a new contact resolving approximate Riemann solver for the
isothermal Euler equations and show its performance for several one- and
two-dimensional test problems. The new solver extends the well-known HLL
solver, while retaining its computational simplicity. The significant gain in
resolution of vortices is displayed by a simulation of the K\'arm\'an vortex
street. We discuss the loss of Galilean invariance and its implications for the
resolution of contact discontinuities, which is experienced by all modern
numerical schemes for hydrodynamics in non-moving grids.


\section{Using Double-peaked Supernova Light Curves to Study Extended Material}
\textit{Piro, Anthony L.} Comment: 5 pages, 3 figures, version accepted for publication in The
Astrophysical Journal Letters. Some updates to the models, but the main
results are unchanged\\%
Subjects: \textbf{Astrophysics - High Energy Astrophysical Phenomena}; Astrophysics - Solar and Stellar Astrophysics\\%
Source: \href{http://arxiv.org/abs/1505.07103}{arXiv:1505.07103} [\href{http://arxiv.org/pdf/1505.07103.pdf}{PDF}]\\%


Extended material at large radii surrounding a supernova can result in a
double-peaked light curve. This occurs when the material is sufficiently
massive that the supernova shock continues to propagate into it and
sufficiently extended that it produces a bright first peak. Such material can
be the leftover, low-mass envelope of a star that has been highly stripped, the
mass associated with a wind, or perhaps mass surrounding the progenitor due to
some type of pre-explosion activity. I summarize the conditions necessary for
such a light curve to occur, describe what can be learned about the extended
material from the light curve shape, and provide an analytic model for fitting
the first peak in these double-peaked supernovae. This is applied to the
specific case of a Type Ic super-luminous supernova, LSQ14bdq. The mass in the
extended material around this explosion's progenitor is measured to be small,
~0.3-0.5 Msun. The radius of this material can be ~500-5000 Rsun, but it is
difficult to constrain due to a degeneracy between radius and the supernova's
energy. In the future, spectra taken during the first peak will be important
for measuring the velocity and composition of the extended material so that
this degeneracy can be overcome.


\section{Cosmological Attractors and Initial Conditions for Inflation}
\textit{Carrasco, John Joseph M.} ; \textit{Kallosh, Renata}; \textit{Linde, Andrei}\\%
Comment: 17 pages, 17 figures, minor changes\\%
Subjects: \textbf{High Energy Physics - Theory}; Astrophysics - Cosmology and Nongalactic Astrophysics; General Relativity and Quantum Cosmology; High Energy Physics - Phenomenology\\%
Source: \href{http://arxiv.org/abs/1506.00936}{arXiv:1506.00936} [\href{http://arxiv.org/pdf/1506.00936.pdf}{PDF}]\\%


Inflationary $\alpha$-attractor models in supergravity, which provide
excellent fits to the latest observational data, are based on the Poincare disk
hyperbolic geometry. We refine these models by constructing Kahler potentials
with built-in inflaton shift symmetry and by making a canonical choice of the
goldstino Kahler potential. The refined models are stable with respect to all
scalar fields at all $\alpha$, no additional stabilization terms are required.
The scalar potential V has a nearly Minkowski minimum at small values of the
inflaton field $\varphi$, and an infinitely long dS valley of constant depth
and width at large $\varphi$. Because of the infinite length of this
shift-symmetric valley, the initial value of the inflaton field at the Planck
density is expected to be extremely large. We show that the inflaton field
$\varphi$ does not change much until all fields lose their energy and fall to
the bottom of the dS valley at large $\varphi$. This provides natural initial
conditions for inflation driven by the inflaton field slowly rolling along the
dS valley towards the minimum of the potential at small $\varphi$. A detailed
description of this process is given for $\alpha$-attractors in supergravity,
but we believe that our general conclusions concerning naturalness of initial
conditions for inflation are valid for a broad class of inflationary models
with sufficiently flat potentials.


\section{Nonlinear Galactic Dynamos and the Magnetic Pitch Angle}
\textit{Chamandy, Luke} ; \textit{Taylor, A. Russ}\\%
Comment: 11 pages, 5 figures, 1 table, edited to match ApJ version\\%
Subjects: \textbf{Astrophysics - Astrophysics of Galaxies}\\%
Source: \href{http://arxiv.org/abs/1506.03245}{arXiv:1506.03245} [\href{http://arxiv.org/pdf/1506.03245.pdf}{PDF}]\\%


Pitch angles $p$ of the large-scale magnetic fields $\overline{\bf{\it{B}}}$
of spiral galaxies have previously been inferred from observations to be
systematically larger in magnitude than predicted by standard mean-field dynamo
theory. This discrepancy is more pronounced if dynamo growth has saturated,
which is reasonable to assume given that such fields are generally inferred to
be close to energy equipartition with the interstellar turbulence. This 'pitch
angle problem' is explored using local numerical mean-field dynamo solutions as
well as asymptotic analytical solutions. It is first shown that solutions in
the saturated or kinematic regimes depend on only five dynamo parameters, two
of which are tightly constrained by observations of galaxy rotation curves. The
remaining 3-dimensional (dimensionless) parameter space can be constrained to
some extent using theoretical arguments. Predicted values of $|p|$ can be as
large as $\sim40^\circ$, which is similar to the largest values inferred from
observations, but only for a small and non-standard region of parameter space.
We argue, based on independent evidence, that such non-standard parameter
values are plausible. However, these values are located toward the boundary of
the allowed parameter space, suggesting that additional physical effects may
need to be incorporated. We therefore suggest possible directions for extending
the basic model considered.


\section{Photochemical Heating of Dense Molecular Gas}
\textit{Glassgold, A. E.} ; \textit{Najita, J. R.}\\%
Comment: Accepted for publication in the Astrophysical Journal\\%
Subjects: \textbf{Astrophysics - Solar and Stellar Astrophysics}\\%
Source: \href{http://arxiv.org/abs/1506.04167}{arXiv:1506.04167} [\href{http://arxiv.org/pdf/1506.04167.pdf}{PDF}]\\%


Photochemical heating is analyzed with emphasis on the heating generated by
chemical reactions initiated by the products of photodissociation and
photoionization. The immediate products are slowed down by collisions with the
ambient gas and heat the gas. In addition to this direct process, heating is
also produced by the subsequent chemical reactions initiated by these products.
Some of this chemical heating comes from the kinetic energy of the reaction
products and the rest from collisional de-excitation of the product atoms and
molecules. In considering dense gas dominated by molecular hydrogen, we find
that the chemical heating is sometimes as large if not much larger than the
direct heating. In very dense gas the total photochemical heating approaches 10
eV per photodissociation (or photoionization), competitive with other ways of
heating molecular gas.


\section{Calibration of the optical mass proxy for clusters of galaxies and an
update of the WHL12 cluster catalog}
\textit{Wen, Z. L.} ; \textit{Han, J. L.}\\%
Comment: 11 pages, 8 figures, 4 tables; updated to match the published version\\%
Subjects: \textbf{Astrophysics - Astrophysics of Galaxies}; Astrophysics - Cosmology and Nongalactic Astrophysics\\%
Source: \href{http://arxiv.org/abs/1506.04503}{arXiv:1506.04503} [\href{http://arxiv.org/pdf/1506.04503.pdf}{PDF}]\\%


Accurately determining the mass of galaxy clusters is fundamental for many
studies on cosmology and galaxy evolution. We collect and rescale the cluster
masses of 1191 clusters of 0.05<z<0.75 estimated by X-ray or Sunyaev-Zeldovich
measurements and use them to calibrate the optical mass proxy. The total r-band
luminosity (in units of L^{\ast}) of these clusters are obtained by using
spectroscopic and photometric data of the Sloan Digital Sky Survey (SDSS). We
find that the correlation between the cluster mass M_{500} and total r-band
luminosity L_{500} significantly evolves with redshift. After correcting for
the evolution, we define a new cluster richness
R_{L\ast,500}=L_{500}*E(z)^{1.40} as the optical mass proxy. By using this
newly defined richness and the recently released SDSS DR12 spectroscopic data,
we update the WHL12 cluster catalog and identify 25,419 new rich clusters at
high redshift. In the SDSS spectroscopic survey region, about 89\% of galaxy
clusters have spectroscopic redshifts. The mass can be estimated with a scatter
of 0.17 dex for the clusters in the updated catalog.


\section{Probing the gaseous halo of galaxies through non-thermal emission from
AGN-driven outflows}
\textit{Wang, Xiawei} ; \textit{Loeb, Abraham}\\%
Comment: 12 pages, 7 figures, 1 table, accepted for publication in MNRAS\\%
Subjects: \textbf{Astrophysics - Astrophysics of Galaxies}; Astrophysics - High Energy Astrophysical Phenomena\\%
Source: \href{http://arxiv.org/abs/1506.05470}{arXiv:1506.05470} [\href{http://arxiv.org/pdf/1506.05470.pdf}{PDF}]\\%


Feedback from outflows driven by active galactic nuclei (AGN) can affect the
distribution and properties of the gaseous halos of galaxies. We study the
hydrodynamics and non-thermal emission from the forward outflow shock produced
by an AGN-driven outflow. We consider a few possible profiles for the halo gas
density, self-consistently constrained by the halo mass, redshift and the disk
baryonic concentration of the galaxy. We show that the outflow velocity levels
off at $\sim 10^3\,\rm km\, s^{-1}$ within the scale of the galaxy disk.
Typically, the outflow can reach the virial radius around the time when the AGN
shuts off. We show that the outflows are energy-driven, consistently with
observations and recent theoretical findings. The outflow shock lights up the
halos of massive galaxies across a broad wavelength range. For Milky Way (MW)
mass halos, radio observations by The Jansky Very Large Array (JVLA) and The
Square Kilometer Array (SKA) and infrared/optical observations by The James
Webb Space Telescope (JWST) and Hubble Space Telescope (HST) can detect the
emission signal of angular size $\sim 8"$ from galaxies out to redshift
$z\sim5$. Millimeter observations by The Atacama Large Millimeter/submillimeter
Array (ALMA) are sensitive to non-thermal emission of angular size $\sim 18"$
from galaxies at redshift $z\lesssim1$, while X-ray observations by Chandra,
XMM-Newton and The Advanced Telescope for High Energy Astrophysics (ATHENA) is
limited to local galaxies ($z\lesssim 0.1$) with an emission angular size of
$\sim2'$. Overall, the extended non-thermal emission provides a new way of
probing the gaseous halos of galaxies at high redshifts.


\section{Analysis of Fermi gamma-ray burst duration distribution}
\textit{Tarnopolski, Mariusz} Comment: 6 pages, 3 figures; matches the version to be published\\%
Subjects: \textbf{Astrophysics - High Energy Astrophysical Phenomena}; Astrophysics - Cosmology and Nongalactic Astrophysics; High Energy Physics - Phenomenology; Physics - Space Physics\\%
Source: \href{http://arxiv.org/abs/1506.07324}{arXiv:1506.07324} [\href{http://arxiv.org/pdf/1506.07324.pdf}{PDF}]\\%


Two classes of GRBs, short and long, have been determined without any doubts,
and are usually prescribed to different physical scenarios. A third class,
intermediate in $T_{90}$ durations, has been reported to be present in the
datasets of BATSE, Swift, RHESSI and possibly BeppoSAX. The latest release of
$>1500$ GRBs observed by Fermi gives an opportunity to further investigate the
duration distribution. The aim of this paper is to investigate whether a third
class is present in the $\log T_{90}$ distribution, or is it described by a
bimodal distribution. A standard $\chi^2$ fitting of a mixture of Gaussians is
applied to 25 histograms with different binnings. Different binnings give
various values of the fitting parameters, as well as the shape of the fitted
curve. Among five statistically significant fits none is trimodal. Locations of
the Gaussian components are in agreement with previous works. However, a
trimodal distribution, understood in the sense of having three separated peaks,
is not found for any binning. It is concluded that the duration distribution in
Fermi data is well described by a mixture of three log-normal distributions,
but it is intrinsically bimodal, hence no third class is present in the
$T_{90}$ data of Fermi. It is suggested that the log-normal fit may not be an
adequate model.


\section{Checking Potassium origin of new emission line at 3.5 keV with K XIX
line complex at 3.7 keV}
\textit{Iakubovskyi, Dmytro} Comment: 5 pages, 3 figures. Comments are welcome\\%
Subjects: \textbf{Astrophysics - High Energy Astrophysical Phenomena}; Astrophysics - Cosmology and Nongalactic Astrophysics\\%
Source: \href{http://arxiv.org/abs/1507.02857}{arXiv:1507.02857} [\href{http://arxiv.org/pdf/1507.02857.pdf}{PDF}]\\%


Whether the new line at ~3.5 keV, recently detected in different samples of
galaxy clusters, Andromeda galaxy and central part of our Galaxy, is due to
Potassium emission lines, is now unclear. By using the latest astrophysical
atomic emission line database AtomDB v. 3.0.2, we show that the most
prospective method to directly check its Potassium origin will be the study of
K XIX emission line complex at ~3.7 keV with future X-ray imaging spectrometers
such as Soft X-ray spectometer on-board Astro-H mission or microcalorimeter
on-board Micro-X sounding rocket experiment. To further reduce the remaining
(factor ~3-5) uncertainty of the 3.7/3.5 keV ratio one should perform more
precise modeling including removal of significant spatial inhomogeneities,
detailed treatment of background components, and further extension of the
modeled energy range.


\section{GRB Cosmology and Self-organized Criticality in GRBs}
\textit{Wang, F. Y.} Comment: 7 pages, 5 figures, references added\\%
Subjects: \textbf{Astrophysics - High Energy Astrophysical Phenomena}; Astrophysics - Cosmology and Nongalactic Astrophysics\\%
Source: \href{http://arxiv.org/abs/1507.03802}{arXiv:1507.03802} [\href{http://arxiv.org/pdf/1507.03802.pdf}{PDF}]\\%


Gamma-ray bursts (GRBs), which have isotropic energy up to $10^{54}$ erg,
would be the ideal tool to study the properties of early universe: including
dark energy, star formation rate, and the metal enrichment history of the
Universe. We will briefly review the progress on the field of GRB cosmology.
Meanwhile, X-ray flares, which may have important clues to the central engine,
are common phenomena in the GRB afterglows. We present statistical results of
X-ray flares, i.e., energy, duration time and waiting time distributions, and
compare the results with solar flares. The similarity between the two kinds of
flares are found, which may indicates that the physical mechanism of GRB X-ray
flares is magnetic reconnection.


\section{The deceleration parameter in `tilted' Friedmann universes}
\textit{Tsagas, Christos G.} ; \textit{Kadiltzoglou, Miltiadis I.}\\%
Comment: 16 pages, 1 figure (reference corrected)\\%
Subjects: \textbf{General Relativity and Quantum Cosmology}; Astrophysics - Cosmology and Nongalactic Astrophysics\\%
Source: \href{http://arxiv.org/abs/1507.04266}{arXiv:1507.04266} [\href{http://arxiv.org/pdf/1507.04266.pdf}{PDF}]\\%


Large-scale peculiar motions are believed to reflect the local inhomogeneity
and anisotropy of the universe, triggered by the ongoing process of structure
formation. As a result, realistic observers do not follow the smooth Hubble
flow, but have a peculiar, `tilt', velocity relative to it. Our Local Group of
galaxies, in particular, moves with respect to the universal expansion at a
speed of roughly 600~km/sec. Relative motion effects are known to interfere
with the observations and their interpretation. The strong dipolar anisotropy
seen in the the Cosmic Microwave Background, for example, is not a sign of real
universal anisotropy, but a mere artifact of our peculiar motion relative to
the Hubble flow. With these in mind, we look into the implications of
large-scale bulk motions for the kinematics of their associated observers, by
adopting a `tilted' Friedmann model. Our aim is to examine whether the
deceleration parameter measured in the rest-frame of the bulk flow can differ
from that of the actual universe due to relative-motion effects alone. We find
that there is a difference, which depends on the speed as well as the scale of
the bulk motion. The faster and the smaller the drifting domain, the larger the
difference. In principle, this allows relatively slow peculiar velocities to
have a disproportionately strong effect on the value of the deceleration
parameter measured by observers within bulk flows of, say, few hundred
megaparsecs. In fact, under certain circumstances, it is even possible to
change the sign of the deceleration parameter. It goes without saying that all
these effects vanish identically in the Hubble frame, which makes then an
illusion and mere artifact of the observers' relative motion.


\section{YSOVAR: Mid-infrared Variability Among YSOs in the Star Formation Region
GGD 12-15}
\textit{Wolk, Scott J.} ; \selectlanguage{ngerman}\textit{Günther, H. Moritz}; \textit{Poppenhaeger, Katja}; \textit{Cody, A. M.}; \textit{Rebull, L. M.}; \textit{Forbrich, J.}; \textit{Gutermuth, R. A.}; \textit{Hillenbrand, L. A.}; \textit{Plavchan, P.}; \textit{Stauffer, J. R.}; \textit{Covey, K. R.}; \textit{Song, Inseok}\\%
Comment: Accepted by AJ 47 (large print) pages including 20 figures and 4
tables\\%
Subjects: \textbf{Astrophysics - Solar and Stellar Astrophysics}\\%
Source: \href{http://arxiv.org/abs/1507.04368}{arXiv:1507.04368} [\href{http://arxiv.org/pdf/1507.04368.pdf}{PDF}]\\%


We present an IR-monitoring survey with the $Spitzer$ Space Telescope of the
star forming region GGD 12-15. Over 1000 objects were monitored including about
350 objects within the central 5 arcminutes which is found to be especially
dense in cluster members. The monitoring took place over 38 days and is part of
the Young Stellar Object VARiability (YSOVAR) project. The region was also the
subject of a contemporaneous 67ks $Chandra$ observation. The field includes 119
previously identified pre-main sequence star candidates. X-rays are detected
from 164 objects, 90 of which are identified with cluster members. Overall, we
find that about half the objects in the central 5 arcminutes are young stellar
objects based on a combination of their spectral energy distribution, IR
variability and X-ray emission.
Most of the stars with IR excess relative to a photosphere show large
amplitude (>0.1 mag) mid-IR variability. There are 39 periodic sources, all but
one of these is found to be a cluster member. Almost half of the periodic
sources do not show IR excesses. Overall, more than 85\% of the Class I, flat
spectrum, and Class II sources are found to vary. The amplitude of the
variability is larger in more embedded young stellar objects. Most of the
Class~I/II objects exhibit redder colors in a fainter state, compatible with
time-variable extinction. A few become bluer when fainter, which can be
explained with significant changes in the structure of the inner disk. A search
for changes in the IR due to X-ray events is carried out, but the low number of
flares prevented an analysis of the direct impact of X-ray flares on the IR
lightcurves. However, we find that X-ray detected Class II sources have longer
timescales for change in the mid-IR than a similar set of non-X-ray detected
Class IIs.


\section{Modeling solar coronal bright point oscillations with multiple nanoflare
heated loops}
\textit{Chandrashekhar, K.} ; \textit{Sarkar, Aveek}\\%
Comment: 7 figures, Accepted for publication in APJ\\%
Subjects: \textbf{Astrophysics - Solar and Stellar Astrophysics}\\%
Source: \href{http://arxiv.org/abs/1507.04403}{arXiv:1507.04403} [\href{http://arxiv.org/pdf/1507.04403.pdf}{PDF}]\\%


Intensity oscillations of coronal bright points (BPs) have been studied for
past several years. It has been known for a while that these BPs are closed
magnetic loop like structures. However, initiation of such intensity
oscillations is still an enigma. There have been many suggestions to explain
these oscillations, but modeling of such BPs have not been explored so far.
Using a multithreaded nanoflare heated loop model we study the behavior of such
BPs in this work. We compute typical loop lengths of BPs using potential field
line extrapolation of available data (Chandrashekhar et al. 2013), and set this
as the length of our simulated loops. We produce intensity like observables
through forward modeling and analyze the intensity time series using wavelet
analysis, as was done by previous observers. The result reveals similar
intensity oscillation periods reported in past observations. It is suggested
these oscillations are actually shock wave propagations along the loop. We also
show that if one considers different background subtractions, one can extract
adiabatic standing modes from the intensity time series data as well, both from
the observed and simulated data.


\section{Attenuation of super-soft X-ray sources by circumstellar material}
\textit{Nielsen, Mikkel} ; \textit{Gilfanov, Marat}\\%
Comment: MNRAS, accepted; 11 pages, 10 figures, 1 table\\%
Subjects: \textbf{Astrophysics - High Energy Astrophysical Phenomena}; Astrophysics - Solar and Stellar Astrophysics\\%
Source: \href{http://arxiv.org/abs/1507.04547}{arXiv:1507.04547} [\href{http://arxiv.org/pdf/1507.04547.pdf}{PDF}]\\%


Recent studies have suggested the possibility of significantly obscuring
super-soft X-ray sources in relatively modest amounts of local matter lost from
the binaries themselves. If correct, then this would have explained the paucity
of observed super-soft X-ray sources and would have significance for the search
for single-degenerate type Ia supernova progenitors. We point out that earlier
studies of circumbinary obscuration ignored photo-ionisations of the gas by the
emission from the super-soft X-ray source. We revisit the problem using a full,
self-consistent calculation of the ionisation state of the circumbinary
material photo-ionised by the radiation of the central source. Our results show
that the circumstellar mass-loss rates required for obcuration of super-soft
X-ray sources is about an order of magnitude larger than those reported in
earlier studies, for comparable model parameters. While this does not entrirely
rule out the possibility of circumstellar material obscuring super-soft X-ray
sources, it makes it unlikely that this effect alone can account for the
majority of the missing super-soft X-ray sources. We discuss the observational
appearance of hypothetical obscured nuclear burning white dwarfs and show that
they have signatures making them distinct from photo-ionised nebulae around
super-soft X-ray sources imbedded in the low density ISM.


\section{The internal rotation profile of the B-type star KIC10526294 from
frequency inversion of its dipole gravity modes and statistical model
comparison}
\selectlanguage{ngerman}\textit{Triana, Santiago Andrés} ; \textit{Moravveji, Ehsan}; \textit{Pápics, Péter}; \textit{Aerts, Conny}; \textit{Kawaler, Steven D.}; \textit{Christensen-Dalsgaard, Joergen}\\%
Comment: 52 pages, 32 figures, accepted for publication in The Astrophysical
Journal\\%
Subjects: \textbf{Astrophysics - Solar and Stellar Astrophysics}\\%
Source: \href{http://arxiv.org/abs/1507.04574}{arXiv:1507.04574} [\href{http://arxiv.org/pdf/1507.04574.pdf}{PDF}]\\%


The internal angular momentum distribution of a star is key to determine its
evolution. Fortunately, the stellar internal rotation can be probed through
studies of rotationally-split non-radial oscillation modes. In particular,
detection of non-radial gravity modes (g modes) in massive young stars has
become feasible recently thanks to the Kepler space mission. Our aim is to
derive the internal rotation profile of the Kepler B8V star KIC 10526294
through asteroseismology. We interpret the observed rotational splittings of
its dipole g modes using four different approaches based on the best seismic
models of the star and their rotational kernels. We show that these kernels can
resolve differential rotation the radiative envelope if a smooth rotational
profile is assumed and the observational errors are small. Based on Kepler
data, we find that the rotation rate near the core-envelope boundary is well
constrained to $163\pm89$ nHz. The seismic data are consistent with rigid
rotation but a profile with counter-rotation within the envelope has a
statistical advantage over constant rotation. Our study should be repeated for
other massive stars with a variety of stellar parameters in order to deduce the
physical conditions that determine the internal rotation profile of young
massive stars, with the aim to improve the input physics of their models.

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