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arXiv:1706.08970
Date: Tue, 27 Jun 2017 18:00:00 GMT   (3754kb,A)

Title: High resolution spectroscopy of the extended narrow-line region of IC
  5063 and NGC 7212
Authors: E. Congiu (1,2), M. Contini (3), S. Ciroi (1), V. Cracco (1), M.
  Berton (1,2), F. Di Mille (4), M. Frezzato (1), G. La Mura (1), P. Rafanelli
  (1) ((1) Universit\`a di Padova, (2) INAF-Osservatorio Astronomico di Brera,
  (3) School of Physics and Astronomy, Tel Aviv University, (4) Las Campanas
  Observatory - Carnegie Institution of Washington)
Categories: astro-ph.GA
Comments: 29 pages, 32 figures, accepted for publication in MNRAS
\\
  We studied the properties of the gas of the extended narrow line region
(ENLR) of two Seyfert 2 galaxies: IC 5063 and NGC 7212. We analysed high
resolution spectra to investigate how the main properties of this region depend
on the gas velocity. We divided the emission lines in velocity bins and we
calculated several line ratios. Diagnostic diagrams and SUMA composite models
(photo-ionization + shocks), show that in both galaxies there might be evidence
of shocks significantly contributing in the gas ionization at high |V|, even
though photo-ionization from the active nucleus remains the main ionization
mechanism. In IC 5063 the ionization parameter depends on V and its trend might
be explained assuming an hollow bi-conical shape for the ENLR, with one of the
edges aligned with the galaxy disk. On the other hand, NGC 7212 does not show
any kind of dependence. The models show that solar O/H relative abundances
reproduce the observed spectra in all the analysed regions. They also revealed
an high fragmentation of the gas clouds, suggesting that the complex kinematics
observed in these two objects might be caused by interaction between the ISM
and high velocity components, such as jets.
\\ ( https://arxiv.org/abs/1706.08970 ,  3754kb)
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arXiv:1706.08971
Date: Tue, 27 Jun 2017 18:00:00 GMT   (6762kb,D)

Title: Bayesian power-spectrum inference with foreground and target
  contamination treatment
Authors: Jens Jasche and Guilhem Lavaux
Categories: astro-ph.CO
Comments: 15 pages, 11 figures
\\
  This work presents a joint and self-consistent Bayesian treatment of various
foreground and target contaminations when inferring cosmological power-spectra
and three dimensional density fields from galaxy redshift surveys. This is
achieved by introducing additional block sampling procedures for unknown
coefficients of foreground and target contamination templates to the previously
presented ARES framework for Bayesian large scale structure analyses. As a
result the method infers jointly and fully self-consistently three dimensional
density fields, cosmological power-spectra, luminosity dependent galaxy biases,
noise levels of respective galaxy distributions and coefficients for a set of a
priori specified foreground templates. In addition this fully Bayesian approach
permits detailed quantification of correlated uncertainties amongst all
inferred quantities and correctly marginalizes over observational systematic
effects. We demonstrate the validity and efficiency of our approach in
obtaining unbiased estimates of power-spectra via applications to realistic
mock galaxy observations subject to stellar contamination and dust extinction.
While simultaneously accounting for galaxy biases and unknown noise levels our
method reliably and robustly infers three dimensional density fields and
corresponding cosmological power-spectra from deep galaxy surveys. Further our
approach correctly accounts for joint and correlated uncertainties between
unknown coefficients of foreground templates and the amplitudes of the
power-spectrum. An effect amounting up to $10$ percent correlations and
anti-correlations across large ranges in Fourier space.
\\ ( https://arxiv.org/abs/1706.08971 ,  6762kb)
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arXiv:1706.08972
Date: Tue, 27 Jun 2017 18:00:01 GMT   (4080kb,D)

Title: Investigating Cluster Astrophysics and Cosmology with Cross-Correlation
  of the Thermal Sunyaev-Zel'dovich Effect and Weak Lensing
Authors: Ken Osato, Samuel Flender, Daisuke Nagai, Masato Shirasaki, Naoki
  Yoshida
Categories: astro-ph.CO
Comments: 11 pages, 11 figures, submitted to MNRAS
\\
  Recent detections of the cross-correlation of the thermal Sunyaev-Zel'dovich
(tSZ) effect and weak gravitational lensing (WL) enable unique studies of
cluster astrophysics and cosmology. In this work, we present constraints on the
amplitude of the non-thermal pressure fraction in galaxy clusters, $\alpha_0$,
and the amplitude of the matter power spectrum, $\sigma_8$, using measurements
of the tSZ power spectrum from Planck, and the tSZ-WL cross-correlation from
Planck and the Red Cluster Sequence Lensing Survey. We fit the data to a
semi-analytic model with the covariance matrix using $N$-body simulations. We
find that the tSZ power spectrum alone prefers $\sigma_8 \sim 0.8$ and a large
fraction of non-thermal pressure ($\alpha_0 \sim 0.2-0.3$). The tSZ-WL
cross-correlation on the other hand prefers a significantly lower $\sigma_8
\sim 0.6$, and low $\alpha_0 \sim 0.05$. We show that this tension can be
mitigated by allowing for a steep slope in the stellar-mass-halo-mass relation,
which would cause a reduction of the gas in low-mass halos. In such a model,
the combined data prefer $\sigma_8 \sim 0.7$ and $\alpha_0 \sim 0.15$,
consistent with predictions from hydrodynamical simulations.
\\ ( https://arxiv.org/abs/1706.08972 ,  4080kb)
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arXiv:1706.08974
Date: Tue, 27 Jun 2017 18:00:03 GMT   (3540kb)

Title: Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic
  Globular Clusters. V. The rapid rotation of 47 Tuc traced and modeled in
  three dimensions
Authors: A. Bellini (1), P. Bianchini (2,3), A. L. Varri (4), J. Anderson (1),
  G. Piotto (5,6), R. P. van der Marel (1), E. Vesperini (7), L. L. Watkins (1)
  ((1) STScI, (2) Max Plank Heidelberg, (3) McMaster Univ., (4) Univ.
  Edinburgh, (5) UNIPD, (6) INAF-OAPd, (7) Univ. Indiana)
Categories: astro-ph.GA astro-ph.IM astro-ph.SR
Comments: 15 pages, 14 figures, 8 tables, accepted for publication in ApJ
\\
  High-precision proper motions of the globular cluster 47 Tuc have allowed us
to measure for the first time the cluster rotation in the plane of the sky and
the velocity anisotropy profile from the cluster core out to about 13'. These
profiles are coupled with prior measurements along the line of sight and the
surface-brightness profile, and fit all together with self-consistent models
specifically constructed to describe quasi-relaxed stellar systems with
realistic differential rotation, axisymmetry and pressure anisotropy. The
best-fit model provides an inclination angle i between the rotation axis and
the line-of-sight direction of 30 deg, and is able to simultaneously reproduce
the full three-dimensional kinematics and structure of the cluster, while
preserving a good agreement with the projected morphology. Literature models
based solely on line-of-sight measurements imply a significantly different
inclination angle (i=45 deg), demonstrating that proper motions play a key role
in constraining the intrinsic structure of 47 Tuc. Our best-fit global
dynamical model implies an internal rotation higher than previous studies have
shown, and suggests a peak of the intrinsic V/sigma ratio of ~0.9 at around two
half-light radii, with a non-monotonic intrinsic ellipticity profile reaching
values up to 0.45. Our study unveils a new degree of dynamical complexity in 47
Tuc, which may be leveraged to provide new insights into the formation and
evolution of globular clusters.
\\ ( https://arxiv.org/abs/1706.08974 ,  3540kb)
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arXiv:1706.08975
Date: Tue, 27 Jun 2017 18:00:03 GMT   (1993kb)

Title: Effect of dust radial drift on viscous evolution of gaseous disk
Authors: Kazuhiro D. Kanagawa, Takahiro Ueda, Takayuki Muto, and Satoshi
  Okuzumi
Categories: astro-ph.EP
Comments: Accepted for publication in ApJ, 15 pages, 9 figures
\\
  The total amount of dust (or "metallicity") and the dust distribution in
protoplanetary disks are crucial for planet formation. Dust grains radially
drift due to gas--dust friction, and the gas is affected by the feedback from
dust grains. We investigate the effects of the feedback from dust grains on the
viscous evolution of the gas, taking into account the vertical dust settling.
The feedback from the grains pushes the gas outward. When the grains are small
and the dust-to-gas mass ratio is much smaller than unity, the radial drift
velocity is reduced by the feedback effect but the gas still drifts inward.
When the grains are sufficiently large or piled-up, the feedback is so
effective that forces the gas flows outward. Although the dust feedback is
affected by dust settling, we found that the 2D approximation reasonably
reproduces the vertical averaged flux of gas and dust. We also performed the 2D
two-fluid hydrodynamic simulations to examine the effect of the feedback from
the grains on the evolution of the gas disk. We show that when the feedback is
effective, the gas flows outward and the gas density at the region within $\sim
10\ \mbox{AU}$ is significantly depleted. As a result, the dust-to-gas mass
ratio at the inner radii may significantly excess unity, providing the
environment where planetesimals are easily formed via, e.g., streaming
instability. We also show that a simplified 1D model well reproduces the
results of the 2D two-fluid simulations, which would be useful for future
studies.
\\ ( https://arxiv.org/abs/1706.08975 ,  1993kb)
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arXiv:1706.08977
Date: Tue, 27 Jun 2017 18:00:06 GMT   (6404kb,D)

Title: A Millimeter Continuum Size-Luminosity Relationship for Protoplanetary
  Disks
Authors: Anjali Tripathi, Sean M. Andrews, Tilman Birnstiel, David J. Wilner
Categories: astro-ph.EP astro-ph.SR
Comments: Accepted for publication in ApJ
\\
  We present a sub-arcsecond resolution survey of the 340 GHz dust continuum
emission from 50 nearby protoplanetary disks, based on new and archival
observations with the Submillimeter Array. The observed visibility data were
modeled with a simple prescription for the radial surface brightness profile.
The results were used to extract intuitive, empirical estimates of the emission
"size" for each disk, $R_{\rm eff}$, defined as the radius that encircles a
fixed fraction of the total continuum luminosity, $L_{\rm mm}$. We find a
significant correlation between the sizes and luminosities, such that $R_{\rm
eff} \propto L_{\rm mm}^{0.5}$, providing a confirmation and quantitative
characterization of a putative trend that was noted previously. This
correlation suggests that these disks have roughly the same average surface
brightness interior to their given effective radius, ~0.2 Jy arcsec$^{-2}$ (or
8 K in brightness temperature). The same trend remains, but the 0.2dex of
dispersion perpendicular to this relation essentially disappears, when we
account for the irradiation environment of each disk with a crude approximation
of the dust temperatures based on the stellar host luminosities. We consider
two (not mutually exclusive) explanations for the origin of this
size-luminosity relationship. Simple models of the growth and migration of disk
solids can account for the observed trend for a reasonable range of initial
conditions, but only on timescales that are much shorter than the nominal ages
present in the sample. An alternative scenario invokes optically thick emission
concentrated on unresolved scales, with filling factors of a few tens of
percent, that are perhaps manifestations of localized particle traps.
\\ ( https://arxiv.org/abs/1706.08977 ,  6404kb)
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arXiv:1706.08979
Date: Tue, 27 Jun 2017 18:00:07 GMT   (332kb,D)

Title: An Improved Age-Activity Relationship for Cool Stars older than a
  Gigayear
Authors: R. S. Booth, K. Poppenhaeger, C. A. Watson, V. Silva Aguirre and S. J.
  Wolk
Categories: astro-ph.SR astro-ph.EP
Comments: 16 pages, 5 figures, 5 tables, Accepted for publication in MNRAS
\\
  Stars with convective envelopes display magnetic activity, which decreases
over time due to the magnetic braking of the star. This age-dependence of
magnetic activity is well-studied for younger stars, but the nature of this
dependence for older stars is not well understood. This is mainly because
absolute stellar ages for older stars are hard to measure. However, relatively
accurate stellar ages have recently come into reach through asteroseismology.
In this work we present X-ray luminosities, which are a measure for magnetic
activity displayed by the stellar coronae, for 24 stars with well-determined
ages older than a gigayear. We find 14 stars with detectable X-ray luminosities
and use these to calibrate the age-activity relationship. We find a
relationship between stellar X-ray luminosity, normalized by stellar surface
area, and age that is steeper than the relationships found for younger stars,
with an exponent of $-2.80 \pm 0.72$. Previous studies have found values for
the exponent of the age-activity relationship ranging between -1.09 to -1.40,
dependent on spectral type, for younger stars. Given that there are recent
reports of a flattening relationship between age and rotational period for old
cool stars, one possible explanation is that we witness a strong steepening of
the relationship between activity and rotation.
\\ ( https://arxiv.org/abs/1706.08979 ,  332kb)
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arXiv:1706.08980
Date: Tue, 27 Jun 2017 18:00:15 GMT   (656kb)

Title: NuSTAR and XMM-Newton observations of the 2015 outburst decay of GX
  339-4
Authors: H. Stiele, A.K.H. Kong
Categories: astro-ph.HE
Comments: 18 pages, 8 figures, accepted by ApJ
\\
  The extent of the accretion disk in the low/hard state of stellar mass black
hole X-ray binaries remains an open question. There are some evidence
suggesting that the inner accretion disk is truncated and replaced by a hot
flow, while the detection of relativistic broadened iron emission lines seems
to require an accretion disk extending fully to the innermost stable circular
orbit. We present comprehensive spectral and timing analyses of six Nuclear
Spectroscopic Telescope Array (NuSTAR) and XMM-Newton observations of GX 339-4
taken during outburst decay during the autumn of 2015. Using a spectral model
consisting of a thermal accretion disk, Comptonized emission, and a
relativistic reflection component we obtain a decreasing photon index,
consistent with an X-ray binary during outburst decay. Although, we observe a
discrepancy in the inner radius of the accretion disk and that of the
reflector, which can be addressed to the different underlying assumptions in
each model, both model components indicate a truncated accretion disk that
resiles with decreasing luminosity. The evolution of the characteristic
frequency in Fourier power spectra and their missing energy dependence support
the interpretation of a truncated and evolving disk in the hard state. The
XMM-Newton dataset allowed us to study, for the first time, the evolution of
the covariance spectra and ratio during outburst decay. The covariance ratio
increases and steeps during outburst decay, consistent with increased disk
instabilities.
\\ ( https://arxiv.org/abs/1706.08980 ,  656kb)
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arXiv:1706.08982
Date: Tue, 27 Jun 2017 18:01:46 GMT   (42328kb,D)

Title: General Relativistic Radiation Magnetohydrodynamic Simulations of Thin
  Magnetically Arrested Disks
Authors: Danilo Morales Teixeira, Mark J. Avara, Jonathan C. McKinney
Categories: astro-ph.HE
Comments: Submitted do MNRAS, 14 pages and 11 figures
\\
  The classical, relativistic thin-disk theory of Novikov and Thorne (NT)
predicts a maximum accretion efficiency of 40% for an optically thick,
radiatively efficient accretion disk around a maximally spinning black hole
(BH). However, when a strong magnetic field is introduced to numerical
simulations of thin disks, large deviations in efficiency are observed, in part
due to mass and energy carried by jets and winds launched by the disk or BH
spin. The total efficiency of accretion can be significantly enhanced beyond
that predicted by NT but it has remained unclear how the radiative component is
affected. In order to study the effect of a dynamically relevant large-scale
magnetic field on radiatively efficient accretion, we have performed numerical
3D general relativistic - radiative - magnetohydroynamic (GRRMHD) simulations
of a disk with scale height to radius ratio of $H/R~0.1$ around a moderately
spinning BH (a=0.5) using the code HARMRAD. Our simulations are fully global
and allow us to measure the jet, wind, and radiative properties of a
magnetically arrested disk (MAD) that is kept thin via self-consistent
transport of energy by radiation using the M1 closure scheme.
  Our fiducial disk is MAD out to a radius of ~16R_g and the majority of the
total ~13\% efficiency of the accretion flow is carried by a magnetically
driven wind. We find that the radiative efficiency is slightly suppressed
compared to NT, contrary to prior MAD GRMHD simulations with an ad hoc cooling
function, but it is unclear how much of the radiation and thermal energy
trapped in the outflows could ultimately escape.
\\ ( https://arxiv.org/abs/1706.08982 ,  42328kb)
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arXiv:1706.08983
Date: Tue, 27 Jun 2017 18:01:50 GMT   (593kb)

Title: Coronal Heating Topology: the Interplay of Current Sheets and Magnetic
  Field Lines
Authors: A. F. Rappazzo, W. H. Matthaeus, D. Ruffolo, M. Velli, S. Servidio
Categories: astro-ph.SR physics.plasm-ph physics.space-ph
Comments: 11 pages, 4 Figures, ApJ (in press)
\\
  The magnetic topology and field line random walk properties of a
nanoflare-heated and magnetically confined corona are investigated in the
reduced magnetohydrodynamic regime. Field lines originating from current sheets
form coherent structures, called Current Sheet Connected (CSC) regions,
extended around them. CSC field line random walk is strongly anisotropic, with
preferential diffusion along the current sheets' in-plane length. CSC field
line random walk properties remain similar to those of the entire ensemble but
exhibit enhanced mean square displacements and separations due to the stronger
magnetic field intensities in CSC regions. The implications for particle
acceleration and heat transport in the solar corona and wind, and for solar
moss formation are discussed.
\\ ( https://arxiv.org/abs/1706.08983 ,  593kb)
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arXiv:1706.08987
Date: Tue, 27 Jun 2017 18:03:31 GMT   (1448kb,D)

Title: AGN feedback on molecular gas reservoirs in quasars at $z\sim2.4$
Authors: S. Carniani, A. Marconi, R. Maiolino, C. Feruglio, M. Brusa, G.
  Cresci, M. Cano-D\'iaz, C. Cicone, B. Balmaverde, F. Fiore, A. Ferrara, S.
  Gallerani, F. La Franca, V. Mainieri, F. Mannucci, H. Netzer, E. Piconcelli,
  E. Sani, R. Schneider, O. Shemmer, L. Testi
Categories: astro-ph.GA
Comments: 14 pages, 13 figures, 4 tables, accepted for publication in A&A
\\
  We present new ALMA observations aimed at mapping molecular gas reservoirs
through the CO(3-2) transition in three quasars at $z\simeq2.4$, LBQS
0109+0213, 2QZ J002830.4-281706, and [HB89] 0329-385. Previous [OIII]5007
observations of these quasars showed evidence for ionised outflows quenching
star formation in their host galaxies. Systemic CO(3-2) emission has been
detected only in one quasar, LBQS 0109+0213, where the CO(3-2) emission is
spatially anti-correlated with the ionised outflow, suggesting that most of the
molecular gas may have been dispersed or heated in the region swept by the
outflow. In all three sources, including the one detected in CO, our
constraints on the molecular gas mass indicate a significantly reduced
reservoir compared to main-sequence galaxies at the same redshift, supporting a
negative feedback scenario. In the quasar 2QZ J002830.4-281706, we tentatively
detect an emission line blob blue-shifted by $v\sim-2000$ km/s with respect to
the galaxy systemic velocity and spatially offset by 0.2 arcsec (1.7 kpc) with
respect to the ALMA continuum peak. Interestingly, such emission feature is
coincident in both velocity and space with the ionised outflow as seen in
[OIII]5007. This tentative detection must be confirmed with deeper observations
but, if real, it could represent the molecular counterpart of the ionised gas
outflow driven by the AGN. Finally, in all ALMA maps we detect the presence of
serendipitous line emitters within a projected distance $\sim 160$ kpc from the
quasars. By identifying these features with the CO(3-2) transition, the
serendipitous line emitters would be located within |$\Delta v$|$<$500 km/s
from the quasars, hence suggesting an overdensity of galaxies in two out of
three quasars.
\\ ( https://arxiv.org/abs/1706.08987 ,  1448kb)
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arXiv:1706.08990
Date: Tue, 27 Jun 2017 18:09:51 GMT   (557kb,D)

Title: Early Blue Excess from the Type Ia Supernova 2017cbv and Implications
  for its Progenitor
Authors: Griffin Hosseinzadeh, David J. Sand, Stefano Valenti, Peter Brown, D.
  Andrew Howell, Curtis McCully, Daniel Kasen, Iair Arcavi, K. Azalee Bostroem,
  Leonardo Tartaglia, Eric Y. Hsiao, Scott Davis, Melissa Shahbandeh, and
  Maximilian D. Stritzinger
Categories: astro-ph.HE
Comments: submitted to ApJL
\\
  We present very early, high-cadence photometric observations of the nearby
Type Ia supernova 2017cbv. The light curve is unique in that it has a blue bump
lasting ~5 days in the U, B, and g bands, which is clearly resolved given our
photometric cadence of ~5.7 hours during that time span. We model the light
curve as the combination of early shocking of the supernova ejecta against a
nondegenerate companion star plus a standard Type Ia supernova component. Our
best-fit model suggests the presence of a subgiant star ~56 solar radii from
the exploding white dwarf, although this number is highly model-dependent.
While this model matches the optical light curve well, it overpredicts the
expected flux in the ultraviolet bands. This may indicate that the shock is not
a blackbody, perhaps because of line blanketing in the UV. Alternatively, it
could point to another physical explanation for the optical blue bump, such as
interaction with circumstellar material or an unusual nickel distribution.
Early optical spectra of SN 2017cbv show strong carbon (C II $\lambda$6580)
absorption up through day -13 with respect to maximum light, suggesting that
the progenitor system contains a significant amount of unburned material. These
early results on SN 2017cbv illustrate the power of early discovery and intense
follow-up of nearby supernovae to resolve standing questions about the
progenitor systems and explosion mechanisms of Type Ia supernovae.
\\ ( https://arxiv.org/abs/1706.08990 ,  557kb)
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arXiv:1706.08999
Date: Tue, 27 Jun 2017 18:28:09 GMT   (157kb)

Title: Dissipation in a tidally perturbed body librating in longitude
Authors: Michael Efroimsky
Categories: astro-ph.EP
Comments: Submitted
\\
  Dissipation in a tidally perturbed librating body differs from that in a
steadily spinning rotator. First, libration changes the spectral distribution
of tidal damping across the tidal modes, as compared to the steady-spin case.
This adds both to the dissipation rate and the tidal torque. Second, while a
non-librating rotator experiences alternating deformation only due to the
potential force exerted on it by the perturber, a librating body is also
subject to a toroidal force proportional to the angular acceleration. Third,
while the centrifugal force in a steadily spinning body renders only a
permanent deformation, in a librating body this force contains two alternating
components $-$ one purely radial, another a degree-2 potential force. Both
contribute to heating, as well as to the tidal torque and potential (and
thereby to the orbital evolution).
  We build a formalism to describe dissipation of small-amplitude libration in
longitude. This formalism incorporates a linear rheological law defining the
response of the rotator's material to forcing. While the developed formalism
can work with an arbitrary linear rheology, we consider a simple example of a
Maxwell material.
  We find that, independent of the rheology, the forced libration in longitude
can provide a considerable and even leading input in the tidal heating. Based
on the observed parameters, this input amounts to 52% in Phobos, 33% in Mimas,
12% in Enceladus, and 96% in Epimetheus. This supports the hypothesis by
Makarov & Efroimsky (2014) that the additional tidal damping due to the forced
libration may have participated in the early heating of some of the large
moons. E.g., a moon could have been chipped by collisions $-$ so it acquired a
higher triaxiality and a higher forced-libration magnitude and, consequently, a
higher heating rate. After the moon warms up, its triaxiality reduces, and so
does the tidal heating
\\ ( https://arxiv.org/abs/1706.08999 ,  157kb)
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\\
arXiv:1706.09000
Date: Tue, 27 Jun 2017 18:28:13 GMT   (21kb)

Title: Tidal viscosity of Enceladus
Authors: Michael Efroimsky
Categories: astro-ph.EP
Comments: Submitted
\\
  In the preceding paper (Efroimsky 2017), we demonstrated that under weak
libration in longitude most dissipation is due to the gravitational tides
(including the additional tides generated by libration). The other three
sources of dissipation$~-~$which are the alternating parts of the centripetal,
toroidal and purely radial deformations$~-~$are less important when libration
is weak. Whether this is so for large-magnitude libration requires a separate
study. In Ibid. it was also shown that in some situations the forced libration
in longitude can provide a considerable and even leading input into the tidal
heating: 52% in Phobos, 33% in Mimas, 12% in Enceladus, and 96% in Epimetheus.
  Equating our expression for the tidal dissipation rate (with the
libration-generated input included) to the outgoing energy flux due to the
vapour plumes, we estimate the mean tidal viscosity of Enceladus, under the
assumption that the Enceladean mantle behaves as a Maxwell body. This method
yields a value of $\,0.4\times 10^{14}$ Pa s for the mean tidal viscosity,
which is remarkably close to the viscosity of ice near the melting point. We
then demonstrate that, with such a value of the tidal viscosity, the tidal
dissipation in Enceladus is too low to influence its orbital evolution. Thus
the orbital evolution of Enceladus is defined to a much greater extent by the
tidal friction in Saturn.
\\ ( https://arxiv.org/abs/1706.09000 ,  21kb)
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arXiv:1706.09003
Date: Tue, 27 Jun 2017 18:36:08 GMT   (1289kb,D)

Title: Primordial black holes from scalar field evolution in the early universe
Authors: Eric Cotner, Alexander Kusenko
Categories: astro-ph.CO
Comments: 13 pages, 6 figures
\\
  Scalar condensates with large expectation values can form in the early
universe, for example, in theories with supersymmetry. The condensate can
undergo fragmentation into Q-balls before decaying. If the Q-balls dominate the
energy density for some period of time, statistical fluctuations in their
number density can lead to formation of primordial black holes (PBH). In the
case of supersymmetry the mass range is limited from above by $10^{23}$g. For a
general charged scalar field, this robust mechanism can generate black holes
over a much broader mass range, including the black holes with masses of 1-100
solar masses, which is relevant for LIGO observations of gravitational waves.
Topological defects can lead to formation of PBH in a similar fashion.
\\ ( https://arxiv.org/abs/1706.09003 ,  1289kb)
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arXiv:1706.09033
Date: Tue, 27 Jun 2017 20:05:51 GMT   (3276kb)

Title: Validating a novel angular power spectrum estimator using simulated low
  frequency radio-interferometric data
Authors: Samir Choudhuri, Nirupam Roy, Somnath Bharadwaj, Sk. Saiyad Ali, Abhik
  Ghosh and Prasun Dutta
Categories: astro-ph.CO
Comments: 18 pages, 1 table, 9 figures, Accepted for publication in New
  Astronomy
\\
  The "Tapered Gridded Estimator" (TGE) is a novel way to directly estimate the
angular power spectrum from radio-interferometric visibility data that reduces
the computation by efficiently gridding the data, consistently removes the
noise bias, and suppresses the foreground contamination to a large extent by
tapering the primary beam response through an appropriate convolution in the
visibility domain. Here we demonstrate the effectiveness of TGE in recovering
the diffuse emission power spectrum through numerical simulations. We present
details of the simulation used to generate low frequency visibility data for
sky model with extragalactic compact radio sources and diffuse Galactic
synchrotron emission. We then use different imaging strategies to identify the
most effective option of point source subtraction and to study the underlying
diffuse emission. Finally, we apply TGE to the residual data to measure the
angular power spectrum, and assess the impact of incomplete point source
subtraction in recovering the input power spectrum $C_{\ell}$ of the
synchrotron emission. This estimator is found to successfully recovers the
$C_{\ell}$ of input model from the residual visibility data. These results are
relevant for measuring the diffuse emission like the Galactic synchrotron
emission. It is also an important step towards characterizing and removing both
diffuse and compact foreground emission in order to detect the redshifted $21\,
{\rm cm}$ signal from the Epoch of Reionization.
\\ ( https://arxiv.org/abs/1706.09033 ,  3276kb)
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arXiv:1706.09056
Date: Tue, 27 Jun 2017 21:30:25 GMT   (913kb)

Title: The AGN-Star Formation Connection: Future Prospects with JWST
Authors: Allison Kirkpatrick, Stacey Alberts, Alexandra Pope, Guillermo Barro,
  Matteo Bonato, Dale D. Kocevski, Pablo Perez-Gonzalez, George H. Rieke, Lucia
  Rodriguez-Munoz, Anna Sajina, Norman A. Grogin, Kameswara Bharadwaj Mantha,
  Viraj Pandya, Janine Pforr, Paola Santini
Categories: astro-ph.GA
Comments: 14 pages, 10 figures, submitted to ApJ
\\
  The bulk of the stellar growth over cosmic time is dominated by IR luminous
galaxies at cosmic noon (z=1-2), many of which harbor a hidden active galactic
nucleus (AGN). We use state of the art infrared color diagnostics, combining
Spitzer and Herschel observations, to separate dust-obscured AGN from dusty
star forming galaxies (SFGs) in the CANDELS and COSMOS surveys. We calculate 24
micron counts of SFGs, AGN/star forming "Composites", and AGN. AGN and
Composites dominate the counts above 0.8 mJy at 24 micron, and Composites form
at least 25% of an IR sample even to faint detection limits. We develop methods
to use the Mid-Infrared Instrument (MIRI) on JWST to identify dust-obscured AGN
and Composite galaxies from z~1-2. With the sensitivity and spacing of MIRI
filters, we will detect >4 times as many AGN hosts than with Spitzer/IRAC
criteria. Any star formation rates based on the 7.7 micron PAH feature (likely
to be applied to MIRI photometry) must be corrected for the contribution of the
AGN, or the SFR will be overestimated by ~35% for cases where the AGN provides
half the IR luminosity and ~50% when the AGN accounts for 90% of the
luminosity. Finally, we demonstrate that our MIRI color technique can select
AGN with an Eddington ratio of $\lambda_{\rm Edd}\sim0.01$ and will identify
AGN hosts with a higher sSFR than X-ray techniques alone. JWST/MIRI will enable
critical steps forward in identifying and understanding dust-obscured AGN and
the link to their host galaxies.
\\ ( https://arxiv.org/abs/1706.09056 ,  913kb)
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\\
arXiv:1706.09074
Date: Tue, 27 Jun 2017 23:36:01 GMT   (2103kb,D)

Title: The Peculiar Globular Cluster Palomar 1 and Persistence in the
  SDSS-APOGEE Database
Authors: Farbod Jahandar, Kim A. Venn, Matthew D. Shetrone, Mike Irwin, Jo
  Bovy, Charli M. Sakari, Collin L. Kielty, Ruth A. R. Digby and Peter M.
  Frinchaboy
Categories: astro-ph.GA
Comments: 15 pages, 7 tables, 8 figures: Accepted for publication in MNRAS,
  2017 June 23
DOI: 10.1093/mnras/stx1592
\\
  The SDSS-III APOGEE DR12 is a unique resource to search for stars beyond the
tidal radii of star clusters. We have examined the APOGEE DR12 database for new
candidates of the young star cluster Palomar 1, a system with previously
reported tidal tails (Niederste-Ostholt et al. 2010). The APOGEE ASPCAP
database includes spectra and stellar parameters for two known members of Pal 1
(Stars I and II), however these do not agree with the stellar parameters
determined from optical spectra by Sakari et al. (2011). We find that the
APOGEE analysis of these two stars is strongly affected by the known
persistence problem (Majewski et al. 2015; Nidever et al. 2015). By
re-examining the individual visits, and removing the blue (and sometimes green)
APOGEE detector spectra affected by persistence, then we find excellent
agreement in a re-analysis of the combined spectra. These methods are applied
to another five stars in the APOGEE field with similar radial velocities and
metallicities as those of Pal 1. Only one of these new candidates, Star F, may
be a member located in the tidal tail based on its heliocentric radial
velocity, metallicity, and chemistry. The other four candidates are not well
aligned with the tidal tails, and comparison to the Besancon model (Robin et
al. 2003) suggests that they are more likely to be non-members, i.e. part of
the Galactic halo. This APOGEE field could be re-examined for other new
candidates if the persistence problem can be removed from the APOGEE spectral
database.
\\ ( https://arxiv.org/abs/1706.09074 ,  2103kb)
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\\
arXiv:1706.09079
Date: Wed, 28 Jun 2017 00:05:33 GMT   (523kb,D)

Title: Magnetic Flux Cancelation as the Origin of Solar Quiet Region Pre-Jet
  Minifilaments
Authors: Navdeep K. Panesar, Alphonse C. Sterling, Ronald L. Moore
Categories: astro-ph.SR
Comments: 14 pages, 10 figures, 1 table, accepted for publication in ApJ
\\
  We investigate the origin of ten solar quiet region pre-jet minifilaments,
using EUV images from SDO/AIA and magnetograms from SDO/HMI. We recently found
panesar16b that quiet region coronal jets are driven by minifilament eruptions,
where those eruptions result from flux cancelation at the magnetic neutral line
under the minifilament. Here, we study the longer-term origin of the pre-jet
minifilaments themselves. We find that they result from flux cancelation
between minority-polarity and majority-polarity flux patches. In each of ten
pre-jet regions, we find that opposite-polarity patches of magnetic flux
converge and cancel, with a flux reduction of 10--40% from before to after the
minifilament appears. For our ten events, the minifilaments exist for periods
ranging from 1.5 hr to two days before erupting to make a jet. Apparently, the
flux cancelation builds highly sheared field that runs above and traces the
neutral line, and the cool-transition-region-plasma minifilament forms in this
field and is suspended in it. We infer that the convergence of the
opposite-polarity patches results in reconnection in the low corona that builds
a magnetic arcade enveloping the minifilament in its core, and that the
continuing flux cancelation at the neutral line finally destabilizes the
minifilament field so that it erupts and drives the production of a coronal
jet. Thus our observations strongly support that quiet region magnetic flux
cancelation results in both the formation of the pre-jet minifilament and its
jet-driving eruption.
\\ ( https://arxiv.org/abs/1706.09079 ,  523kb)
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\\
arXiv:1706.09082
Date: Wed, 28 Jun 2017 00:13:36 GMT   (1236kb)

Title: Analysis of solar gamma rays and solar neutrons detected on March 7th
  and September 25th of 2011 by Ground Level Neutron Telescopes, SEDA-FIB and
  FERMI-LAT
Authors: Y. Muraki, J. F. Valdes-Galicia, L. X. Gonzalez, K. Kamiya, Y.
  Katayose, K. Koga, H. Matsumoto, S. Masuda, Y. Matsubara, Y. Nagai, M.
  Ohnishi, S. Ozawa, T. Sako, S. Shibata, M. Takita, Y. Tanaka, H. Tsuchiya, K.
  Watanabe, and J. L. Zhang
Categories: astro-ph.HE
Comments: 15 pages
\\
  At the 33rd ICRC, we reported the possible detection of solar gamma rays by a
ground level detector and later re-examined this event. On March 7, 2011, the
solar neutron telescope (SNT) located at Mt. Sierra Negra, Mexico (4,600 m)
observed enhancements of the counting rate from 19:49 to 20:02 UT and from
20:50 to 21:01 UT. The statistical significance was 9.7sigma and 8.5sigma,
respectively. This paper discusses the possibility of using this mountain
detector to detect solar gamma rays. In association with this event, the solar
neutron detector SEDA-FIB onboard the International Space Station has also
detected solar neutrons with a statistical significance of 7.5sigma. The
FERMI-LAT detector also observed high-energy gamma rays from this flare with a
statistical significance of 6.7sigma. We thus attempted to make a unified model
to explain this data. In this paper, we report on another candidate for solar
gamma rays detected on September 25th, 2011 by the SNT located in Tibet (4,300
m) from 04:37 to 04:47 UT with a statistical significance of 8.0sigma (by the
Li-Ma method).
\\ ( https://arxiv.org/abs/1706.09082 ,  1236kb)
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\\
arXiv:1706.09097
Date: Wed, 28 Jun 2017 01:54:46 GMT   (70kb)

Title: Can Turbulence Dominate Depolarization of Optical Blazars?
Authors: Xiaotong Guo, Jirong Mao, Jiancheng Wang (YNAO)
Categories: astro-ph.HE
Comments: ApJ accepted
\\
  We carefully examine the depolarization feature of blazars in the optical and
near-infrared bands using the sample of Mead et al. Magnetohydrodynamics (MHD)
turbulence could be one possible reason for the depolarization of
optical/infrared blazars when we apply the theoretical analysis of Lazarian and
Pogosyan. We further identify in the sample that the depolarization results
shown in most blazars roughly obey the form of the three-dimensional
anisotropic Kolmogorov scaling. The effective Faraday rotation window length
scale is not small enough to resolve the polarization correlation length scale
in the blazar sample. The depolarization and the related turbulent features
show diversities in different blazar sources. We suggest more simultaneous
observations in both the optical/infrared and the high-energy bands for the
study of the blazar polarization.
\\ ( https://arxiv.org/abs/1706.09097 ,  70kb)
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\\
arXiv:1706.09105
Date: Wed, 28 Jun 2017 02:24:13 GMT   (800kb)

Title: Application of Coupled Harmonic Oscillator model to Solar Activity and
  El Ni\~no Phenomena
Authors: Yasushi Muraki
Categories: astro-ph.SR
Comments: submitted to the Proceeding of the 35th ICRC at Busan in July 2017.
  Paper number SH046
\\
  The solar activity provides an important impact not only on the intensity of
cosmic rays but also on the earth environment. In this paper, a coupled
oscillator model is proposed to explain the solar activity. By this model the
89 year Gleissberg cycle can be naturally reduced. Furthermore as an
application of the coupled oscillator model we try to apply it to the El
Nino-La Nina phenomena (ENSO). The 26 year oscillation of the Pacific Ocean is
naturally explained. Finally we search a possible substance of the coupled
oscillators in actual solar activities.
\\ ( https://arxiv.org/abs/1706.09105 ,  800kb)
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\\
arXiv:1706.09116
Date: Wed, 28 Jun 2017 03:35:55 GMT   (2737kb,D)

Title: Heating of an erupting prominence associated with a solar coronal mass
  ejection on 2012 January 27
Authors: Jin-Yi Lee, John C. Raymond, Katharine K. Reeves, Yong-Jae Moon, and
  Kap-Sung Kim
Categories: astro-ph.SR
Comments: Astrophysical Journal in press
\\
  We investigate the heating of an erupting prominence and loops associated
with a coronal mass ejection and X-class flare. The prominence is seen in
absorption in EUV at the beginning of its eruption. Later the prominence
changes to emission, which indicates heating of the erupting plasma. We find
the densities of the erupting prominence using the absorption properties of
hydrogen and helium in different passbands. We estimate the temperatures and
densities of the erupting prominence and loops seen as emission features using
the differential emission measure method, which uses both EUV and X-ray
observations from the Atmospheric Imaging Assembly on board Solar Dynamics
Observatory and the X-ray Telescope on board Hinode. We consider synthetic
spectra using both photospheric and coronal abundances in these calculations.
We verify the methods for the estimation of temperatures and densities for the
erupting plasmas. Then we estimate the thermal, kinetic, radiative loss,
thermal conduction, and heating energies of the erupting prominence and loops.
We find that the heating of the erupting prominence and loop occurs strongly at
early times in the eruption. This event shows a writhing motion of the erupting
prominence, which may indicate a hot flux rope heated by thermal energy release
during magnetic reconnection.
\\ ( https://arxiv.org/abs/1706.09116 ,  2737kb)
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\\
arXiv:1706.09149
Date: Wed, 28 Jun 2017 07:39:24 GMT   (42kb,D)

Title: A measurement of the Hubble constant using galaxy redshift surveys
Authors: Yuting Wang, Lixin Xu, Gong-Bo Zhao
Categories: astro-ph.CO
Comments: 4.5 pages, 3 figures, 1 table
\\
  We perform a measurement of the Hubble constant, $H_0$, using the latest
baryonic acoustic oscillations (BAO) measurements from galaxy surveys of 6dFGS,
SDSS DR7 Main Galaxy Sample, BOSS DR12 sample, and eBOSS DR14 quasar sample, in
the framework of a flat $\Lambda$CDM model. Based on the Kullback-Leibler (KL)
divergence, we examine the consistency of $H_0$ values derived from various
data sets. We find that our measurement is consistent with that derived from
Planck and with the local measurement of $H_0$ using the Cepheids and type Ia
supernovae. We perform forecasts on $H_0$ from future BAO measurements, and
find that the uncertainty of $H_0$ determined by future BAO data alone,
including complete eBOSS, DESI and Euclid-like, is comparable with that from
local measurements.
\\ ( https://arxiv.org/abs/1706.09149 ,  42kb)
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\\
arXiv:1706.09166
Date: Wed, 28 Jun 2017 08:21:47 GMT   (586kb)

Title: Radial pulsations of red giant branch stars
Authors: Yu.A. Fadeyev
Categories: astro-ph.SR
Comments: 13 pages, 6 figures, 1 table, accepted to Astronomy Letters
\\
  We performed hydrodynamic computations of nonlinear stellar pulsations of
population I stars at the evolutionary stages of the ascending red giant branch
and the following luminosity drop due to the core helium flash. Red giants
populating this region of the Hertzsprung--Russel diagram were found to be the
fundamental mode pulsators. The pulsation period is the largest at the tip of
the red giant branch and for stars with initial masses from 1.1M_\odot to
1.9M_\odot ranges from 254 day to 33 day, respectively. The rate of period
change during the core helium flash is comparable with rates of secular period
change in Mira type variables during the thermal pulse in the helium shell
source. The period change rate is largest (\dot\Pi/\Pi\approx -0.01 yr^{-1}) in
stars with initial mass Mzams=1.1M_\odot and decreases to \dot\Pi/\Pi\sim
-0.001\ yr^{-1} for stars of the evolutionary sequence Mzams=1.9M_\odot.
Theoretical light curves of red giants pulsating with periods Pi > 200 day show
the presence of the secondary maximum similar to that observed in many Miras.
\\ ( https://arxiv.org/abs/1706.09166 ,  586kb)
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\\
arXiv:1706.09176
Date: Wed, 28 Jun 2017 09:01:36 GMT   (7343kb)

Title: Onset of a Large Ejective Solar Eruption from a Typical Coronal-Jet-Base
  Field Configuration
Authors: Navin Chandra Joshi, Alphonse C. Sterling, Ronald L. Moore, Tetsuya
  Magara, Young-Jae Moon
Categories: astro-ph.SR
Comments: 36 pages, 14 figures. Accepted for publication in ApJ
\\
  Utilizing multiwavelength observations and magnetic field data from SDO/AIA,
SDO/HMI, GOES and RHESSI, we investigate a large-scale ejective solar eruption
of 2014 December 18 from active region NOAA 12241. This event produced a
distinctive three-ribbon flare, having two parallel ribbons corresponding to
the ribbons of a standard two-ribbon flare, and a larger-scale third
quasi-circular ribbon offset from the other two ribbons. There are two
components to this eruptive event. First, a flux rope forms above a
strong-field polarity-inversion line and erupts and grows as the parallel
ribbons turn on, grow, and spread part from that polarity-inversion line; this
evolution is consistent with the tether-cutting-reconnection mechanism for
eruptions. Second, the eruption of the arcade that has the erupting flux rope
in its core under goes magnetic reconnection at the null point of a fan dome
that envelops the erupting arcade, resulting in formation of the quasi-circular
ribbon; this is consistent with the breakout reconnection mechanism for
eruptions. We find that the parallel ribbons begin well before (12 min)
circular ribbon onset, indicating that tether-cutting reconnection (or a
non-ideal MHD instability) initiated this event, rather than breakout
reconnection. The overall setup for this large-scale (circular-ribbon diameter
100000 km) eruption is analogous to that of coronal jets (base size 10000 km),
many of which, according to recent findings, result from eruptions of
small-scale minifilaments. Thus these findings confirm that eruptions of
sheared-core magnetic arcades seated in fan-spine null-point magnetic topology
happen on a wide range of size scales on the Sun.
\\ ( https://arxiv.org/abs/1706.09176 ,  7343kb)
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\\
arXiv:1706.09195
Date: Wed, 28 Jun 2017 10:03:09 GMT   (460kb,D)

Title: Generating Log-normal Mock Catalog of Galaxies in Redshift Space
Authors: Aniket Agrawal, Ryu Makiya, Chi-Ting Chiang, Donghui Jeong, Shun
  Saito, Eiichiro Komatsu
Categories: astro-ph.CO
Comments: 36 pages, 14 figures, code publicly available as "lognormal_galaxies"
  at http://wwwmpa.mpa-garching.mpg.de/~komatsu/codes.html
Report-no: YITP-SB-17-21
\\
  We present a public code to generate a mock galaxy catalog in redshift space
assuming a log-normal probability density function (PDF) of galaxy and matter
density fields. We draw galaxies by Poisson-sampling the log-normal field, and
calculate the velocity field from the linearised continuity equation of matter
fields, assuming zero vorticity. This procedure yields a PDF of the pairwise
velocity fields that is qualitatively similar to that of N-body simulations. We
check fidelity of the catalog, showing that the measured two-point correlation
function and power spectrum in real space agree with the input precisely. We
find that a linear bias relation in the power spectrum does not guarantee a
linear bias relation in the density contrasts, leading to a cross-correlation
coefficient of matter and galaxies deviating from unity on small scales. We
also find that linearising the Jacobian of the real-to-redshift space mapping
provides a poor model for the two-point statistics in redshift space. That is,
non-linear redshift-space distortion is dominated by non-linearity in the
Jacobian. The power spectrum in redshift space shows a damping on small scales
that is qualitatively similar to that of the well-known Fingers-of-God (FoG)
effect due to random velocities, except that the log-normal mock does not
include random velocities. This damping is a consequence of non-linearity in
the Jacobian, and thus attributing the damping of the power spectrum solely to
FoG, as commonly done in the literature, is misleading.
\\ ( https://arxiv.org/abs/1706.09195 ,  460kb)
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\\
arXiv:1706.09196
Date: Wed, 28 Jun 2017 10:03:35 GMT   (14306kb,D)

Title: The complex magnetic field topology of the cool Ap star 49 Cam
Authors: J. Silvester, O. Kochukhov, N. Rusomarov and G.A. Wade
Categories: astro-ph.SR
Comments: 15 pages, 11 figures, Accepted for publication in MNRAS
\\
  49 Cam is a cool magnetic chemically peculiar star which has been noted for
showing strong, complex Zeeman linear polarisation signatures. This paper
describes magnetic and chemical surface maps obtained for 49 Cam using the
INVERS10 magnetic Doppler imaging code and high-resolution spectropolarimetric
data in all four Stokes parameters collected with the ESPaDOnS and Narval
spectropolarimeters at the Canada-France-Hawaii Telescope and Pic du Midi
Observatory. The reconstructed magnetic field maps of 49 Cam show a relatively
complex structure. Describing the magnetic field topology in terms of spherical
harmonics, we find significant contributions of modes up to l=3, including
toroidal components. Observations cannot be reproduced using a simple low-order
multipolar magnetic field structure. 49 Cam exhibits a level of field
complexity that has not been seen in magnetic maps of other cool Ap stars.
Hence we concluded that relatively complex magnetic fields are observed in Ap
stars at both low and high effective temperatures. In addition to mapping the
magnetic field, we also derive surface abundance distributions of nine chemical
elements, including Ca, Sc, Ti, Cr, Fe, Ce, Pr, Nd, Eu. Comparing these
abundance maps with the reconstructed magnetic field geometry, we find no clear
relationship of the abundance distributions with the magnetic field for some
elements. However, for other elements some distinct patterns are found. We
discuss these results in the context of other recent magnetic mapping studies
and theoretical predictions of radiative diffusion.
\\ ( https://arxiv.org/abs/1706.09196 ,  14306kb)
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\\
arXiv:1706.09202
Date: Wed, 28 Jun 2017 10:18:00 GMT   (631kb,D)

Title: Stability analysis of VBT Echelle spectrograph for precise radial
  velocity measurements
Authors: Sireesha Chamarthi, Ravinder K. Banyal, S. Sriram, Gajendra Pandey
Categories: astro-ph.IM
Comments: 12 pages, 7 figures, Accepted in Journal of Optics (India)
DOI: 10.1007/s12596-017-0422-1
\\
  A fiber-fed Echelle spectrograph at 2.3 m Vainu Bappu Telescope (VBT),
Kavalur, has been in operation since 2005. Owing to various technological
advancements in precision spectroscopy in recent years, several research
avenues have been opened in observational astronomy. These developments have
created a demand to improve the Doppler precision of our spectrograph.
Currently, the stability of the instrument is compromised by the temperature
and pressure fluctuations inside the Echelle room. Further, a better wavelength
calibration approach is needed to carefully track and disentangle the
instrumental effects from stellar spectra. While planning a possible upgrade
with an Iodine absorption gas cell, we measured the raw stability of the
spectrograph using a series of calibration frames taken with the ThAr gas
discharge lamp. The time series data were analysed with cross-correlation
method and the shift in ThAr emission lines was accurately measured across
different Echelle orders. In this paper, we present our stability analysis
methodology and results for the Kavalur spectrograph. We also identify possible
sources of error and discuss our strategy to mitigate them.
\\ ( https://arxiv.org/abs/1706.09202 ,  631kb)
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\\
arXiv:1706.09203
Date: Wed, 28 Jun 2017 10:33:22 GMT   (3900kb)

Title: Shedding new light on the Crab with polarized X-rays
Authors: M. Chauvin, H.-G. Flor\'en, M. Friis, M. Jackson, T. Kamae, J.
  Kataoka, T. Kawano, M. Kiss, V. Mikhalev, T. Mizuno, N. Ohashi, T. Stana, H.
  Tajima, H. Takahashi, N. Uchida, M. Pearce
Categories: astro-ph.HE astro-ph.IM
Comments: Accepted for publication in Scientific Reports, www.nature.com/srep
\\
  Strong magnetic fields, synchrotron emission, and Compton scattering are
omnipresent in compact celestial X-ray sources. Emissions in the X-ray energy
band are consequently expected to be linearly polarized. X-ray polarimetry
provides a unique diagnostic to study the location and fundamental mechanisms
behind emission processes. The polarization of emissions from a bright
celestial X-ray source, the Crab, is reported here for the first time in the
hard X-ray band (~20-160 keV). The Crab is a complex system consisting of a
central pulsar, a diffuse pulsar wind nebula, as well as structures in the
inner nebula including a jet and torus. Measurements are made by a
purpose-built and calibrated polarimeter, PoGO+. The polarization vector is
found to be aligned with the spin axis of the pulsar for a polarization
fraction, PF = (20.9 $\pm$ 5.0)%. This is higher than that of the optical
diffuse nebula, implying a more compact emission site, though not as compact
as, e.g., the synchrotron knot. Contrary to measurements at higher energies, no
significant temporal evolution of phase-integrated polarisation parameters is
observed. The polarization parameters for the pulsar itself are measured for
the first time in the X-ray energy band and are consistent with observations at
optical wavelengths.
\\ ( https://arxiv.org/abs/1706.09203 ,  3900kb)
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\\
arXiv:1706.09208
Date: Wed, 28 Jun 2017 10:44:16 GMT   (8994kb,D)

Title: Asteroid mass estimation using Markov-chain Monte Carlo
Authors: L. Siltala and M. Granvik
Categories: astro-ph.EP
Comments: 14 pages, 20 figures
\\
  Estimates for asteroid masses are based on their gravitational perturbations
on the orbits of other objects such as Mars, spacecraft, or other asteroids
and/or their satellites. In the case of asteroid-asteroid perturbations, this
leads to an inverse problem in at least 13 dimensions where the aim is to
derive the mass of the perturbing asteroid(s) and six orbital elements for both
the perturbing asteroid(s) and the test asteroid(s) based on astrometric
observations. We have developed and implemented three different mass estimation
algorithms utilizing asteroid-asteroid perturbations: the very rough 'marching'
approximation, in which the asteroids' orbital elements are not fitted, thereby
reducing the problem to a one-dimensional estimation of the mass, an
implementation of the Nelder-Mead simplex method, and most significantly, a
Markov-chain Monte Carlo (MCMC) approach. We describe each of these algorithms
with particular focus on the MCMC algorithm, and present example results using
both synthetic and real data. Our results agree with the published mass
estimates, but suggest that the published uncertainties may be misleading as a
consequence of using linearized mass-estimation methods. Finally, we discuss
remaining challenges with the algorithms as well as future plans.
\\ ( https://arxiv.org/abs/1706.09208 ,  8994kb)
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\\
arXiv:1706.09215
Date: Wed, 28 Jun 2017 11:07:30 GMT   (479kb)

Title: Stellar laboratories. IX. New Se V, Sr IV - VII, Te VI, and I VI
  oscillator strengths and the Se, Sr, Te, and I abundances in the hot white
  dwarfs G191-B2B and RE 0503-289
Authors: T. Rauch (1), P. Quinet (2 and 3), M. Knoerzer (1), D. Hoyer (1), K.
  Werner (1), J. W. Kruk (5), M. Demleitner (6) ((1) Institute for Astronomy
  and Astrophysics, Eberhard Karls University, Tuebingen, Germany, (2) Physique
  Atomique et Astrophysique, Universite de Mons - UMONS, Belgium, (3) IPNAS,
  Universite de Liege, Liege, Belgium, (4) Institute of Physics and Astronomy,
  University of Potsdam, Golm, Germany, (5) NASA Goddard Space Flight Center,
  Greenbelt, USA, (6) Astronomisches Rechen-Institut (ARI), Centre for
  Astronomy of Heidelberg University, Heidelberg, Germany)
Categories: astro-ph.SR
Comments: 26 pages, 5 figures
\\
  To analyze spectra of hot stars, advanced non-local thermodynamic equilibrium
(NLTE) model-atmosphere techniques are mandatory. Reliable atomic data is for
the calculation of such model atmospheres.
  We aim to calculate new Sr IV - VII oscillator strengths to identify for the
first time Sr spectral lines in hot white dwarf (WD) stars and to determine the
photospheric Sr abundances. o measure the abundances of Se, Te, and I in hot
WDs, we aim to compute new Se V, Te VI, and I VI oscillator strengths.
  To consider radiative and collisional bound-bound transitions of Se V, Sr IV
- VII, Te VI, and I VI in our NLTE atmosphere models, we calculated oscillator
strengths for these ions.
  We newly identified four Se V, 23 Sr V, 1 Te VI, and three I VI lines in the
ultraviolet (UV) spectrum of RE0503-289. We measured a photospheric Sr
abundance of 6.5 +3.8/-2.4 x 10**-4 (mass fraction, 9500 - 23800 times solar).
We determined the abundances of Se (1.6 +0.9/-0.6 x 10**-3, 8000 - 20000), Te
(2.5 +1.5/-0.9 x 10**-4, 11000 - 28000), and I (1.4 +0.8/-0.5 x 10**-5, 2700 -
6700). No Se, Sr, Te, and I line was found in the UV spectra of G191-B2B and we
could determine only upper abundance limits of approximately 100 times solar.
  All identified Se V, Sr V, Te VI, and I VI lines in the UV spectrum of
RE0503-289 were simultaneously well reproduced with our newly calculated
oscillator strengths.
\\ ( https://arxiv.org/abs/1706.09215 ,  479kb)
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\\
arXiv:1706.09220
Date: Wed, 28 Jun 2017 11:33:14 GMT   (2882kb)

Title: Time-Dependent Cooling in Photoionized Plasma
Authors: Orly Gnat
Categories: astro-ph.GA
Journal-ref: ApJS 228, 11 (2017)
\\
  I explore the thermal evolution and ionization states in gas cooling from an
initially hot state in the presence of external photoionizing radiation. I
compute the equilibrium and nonequilibrium cooling efficiencies, heating rates,
and ion fractions for low-density gas cooling while exposed to the ionizing
metagalactic background radiation at various redshifts (z=0 - 3), for a range
of temperatures (1e8-1e4 K), densities (1e-7 - 1e3 cm^-3) and metallicities
(1e-3 - 2 times solar). The results indicate the existence of a threshold
ionization parameter, above which the cooling efficiencies are very close to
those in photoionization equilibrium (so that departures from equilibrium may
be neglected), and below which the cooling efficiencies resemble those in
collisional time-dependent gas cooling with no external radiation (and are thus
independent of density)
\\ ( https://arxiv.org/abs/1706.09220 ,  2882kb)
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\\
arXiv:1706.09309
Date: Wed, 28 Jun 2017 14:18:36 GMT   (466kb,D)

Title: Safely smoothing spacetime: backreaction in relativistic cosmological
  simulations
Authors: Julian Adamek (LUTH Meudon), Chris Clarkson (Queen Mary, U. of
  London), David Daverio (DAMTP, Cambridge), Ruth Durrer (Geneva U., CAP &
  Geneva U., Dept. Theor. Phys.) and Martin Kunz (Geneva U., CAP & Geneva U.,
  Dept. Theor. Phys.)
Categories: astro-ph.CO gr-qc
Comments: 6 pages, 3 figures
\\
  A persistent theme in the study of dark energy is the question of whether it
really exists or not. It is often claimed hat we are mis-calculating the
cosmological model by neglecting the effects associated with averaging over
large-scale structures. In the Newtonian approximation this is clear: there is
no effect. Within the full relativistic picture this remains an important open
question however, owing to the complex mathematics involved. We study this
issue using particle numerical simulations which account for all relevant
relativistic effects without any problems from shell crossing. In this context
we show for the first time that the backreaction from structure can differ by
many orders of magnitude depending upon the slicing of spacetime one chooses to
average over. In the worst case, where smoothing is carried out in synchronous
spatial surfaces, the corrections can reach ten percent and more. However, when
smoothing on the constant time hypersurface of the Newtonian gauge backreaction
contributions remain 4-5 orders of magnitude smaller.
\\ ( https://arxiv.org/abs/1706.09309 ,  466kb)
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\\
arXiv:1706.09352
Date: Wed, 28 Jun 2017 16:34:50 GMT   (223kb)

Title: Traces of highest energy astrophysical muon and tau neutrinos in the
  Moon shadow
Authors: Daniele Fargion, Pietro Oliva
Categories: astro-ph.HE astro-ph.IM hep-ph
Comments: 9 pages, 2 figures
\\
  The Moon may become soon a novel filtering calorimeter and an amplifier of
energetic muon neutrinos (at TeV up to hundred TeV energy), lepton track
decaying to Earth. Also a more energetic PeV up to EeV tau neutrino events may
be escaping from the Moon to us shining in a surprising way. One or a few gamma
air-shower event inside the Moon shadows may occur each year in near future CTA
or LHAASO TeVs gamma array detector, assuming a non negligible astrophysical
TeV up to hundred TeV neutrino component (respect to our ruling atmospheric
ones); these signals will open a new wonderful passepartout keyhole for
neutrino been seen along the Moon. The lunar solid angle is small and the muon
or tau expected rate is rare, but even future largest tau radio array as the
GIANT one, might reach this new neutrino signals offering a novel and a
spectacular view of the highest energy neutrino sky.
\\ ( https://arxiv.org/abs/1706.09352 ,  223kb)
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\\
arXiv:1706.09359
Date: Wed, 28 Jun 2017 16:52:03 GMT   (6300kb,D)

Title: Dark Energy Survey Year 1 Results: Multi-Probe Methodology and Simulated
  Likelihood Analyses
Authors: E. Krause, T. F. Eifler, J. Zuntz, O. Friedrich, M. A. Troxel, S.
  Dodelson, J. Blazek, L. F. Secco, N. MacCrann, E. Baxter, C. Chang, N. Chen,
  M. Crocce, J. DeRose, A. Ferte, N. Kokron, F. Lacasa, V. Miranda, Y. Omori,
  A. Porredon, R. Rosenfeld, S. Samuroff, M. Wang, R. H. Wechsler, T. M. C.
  Abbott, F. B. Abdalla, S. Allam, J. Annis, K. Bechtol, A. Benoit-Levy, G. M.
  Bernstein, D. Brooks, D. L. Burke, D. Capozzi, M. Carrasco Kind, J.
  Carretero, C. B. D'Andrea, L. N. da Costa, C. Davis, D. L. DePoy, S. Desai,
  H. T. Diehl, J. P. Dietrich, A. E. Evrard, B. Flaugher, P. Fosalba, J.
  Frieman, J. Garcia-Bellido, E. Gaztanaga, T. Giannantonio, D. Gruen, R. A.
  Gruendl, J. Gschwend, G. Gutierrez, K. Honscheid, D. J. James, T. Jeltema, K.
  Kuehn, S. Kuhlmann, O. Lahav, M. Lima, M. A. G. Maia, M. March, et al. (23
  additional authors not shown)
Categories: astro-ph.CO
\\
  We present the methodology for and detail the implementation of the Dark
Energy Survey (DES) 3x2pt DES Year 1 (Y1) analysis, which combines
configuration-space two-point statistics from three different cosmological
probes: cosmic shear, galaxy-galaxy lensing, and galaxy clustering, using data
from the first year of DES observations. We have developed two independent
modeling pipelines and describe the code validation process. We derive
expressions for analytical real-space multi-probe covariances, and describe
their validation with numerical simulations. We stress-test the inference
pipelines in simulated likelihood analyses that vary 6-7 cosmology parameters
plus 20 nuisance parameters and precisely resemble the analysis to be presented
in the DES 3x2pt analysis paper, using a variety of simulated input data
vectors with varying assumptions.
  We find that any disagreement between pipelines leads to changes in assigned
likelihood $\Delta \chi^2 \le 0.045$ with respect to the statistical error of
the DES Y1 data vector. We also find that angular binning and survey mask do
not impact our analytic covariance at a significant level. We determine lower
bounds on scales used for analysis of galaxy clustering (8 Mpc$~h^{-1}$) and
galaxy-galaxy lensing (12 Mpc$~h^{-1}$) such that the impact of modeling
uncertainties in the non-linear regime is well below statistical errors, and
show that our analysis choices are robust against a variety of systematics.
These tests demonstrate that we have a robust analysis pipeline that yields
unbiased cosmological parameter inferences for the flagship 3x2pt DES Y1
analysis. We emphasize that the level of independent code development and
subsequent code comparison as demonstrated in this paper is necessary to
produce credible constraints from increasingly complex multi-probe analyses of
current data.
\\ ( https://arxiv.org/abs/1706.09359 ,  6300kb)
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\\
arXiv:1706.09390
Date: Wed, 28 Jun 2017 17:54:12 GMT   (679kb)

Title: The Factory and the Beehive III: PTFEB132.707+19.810, a Low-Mass
  Eclipsing Binary in Praesepe Observed by PTF and K2
Authors: Adam L. Kraus, Stephanie T. Douglas, Andrew W. Mann, Marcel A.
  Agueros, Nicholas M. Law, Kevin R. Covey, Gregory A. Feiden, Aaron C.
  Rizzuto, Andrew W. Howard, Howard Isaacson, Eric Gaidos, Guillermo Torres,
  Gaspar Bakos
Categories: astro-ph.SR
Comments: Accepted to ApJ; 36 pages, 19 figures, 8 tables in two-column AASTEX6
  format
\\
  Theoretical models of stars constitute a fundamental bedrock upon which much
of astrophysics is built, but large swaths of model parameter space remain
uncalibrated by observations. The best calibrators are eclipsing binaries in
clusters, allowing measurement of masses, radii, luminosities, and
temperatures, for stars of known metallicity and age. We present the discovery
and detailed characterization of PTFEB132.707+19.810, a P=6.0 day eclipsing
binary in the Praesepe cluster ($\tau$~600--800 Myr; [Fe/H]=0.14$\pm$0.04). The
system contains two late-type stars (SpT$_P$=M3.5$\pm$0.2;
SpT$_S$=M4.3$\pm$0.7) with precise masses ($M_p=0.3953\pm0.0020$~$M_{\odot}$;
$M_s=0.2098\pm0.0014$~$M_{\odot}$) and radii ($R_p=0.363\pm0.008$~$R_{\odot}$;
$R_s=0.272\pm0.012$~$R_{\odot}$). Neither star meets the predictions of stellar
evolutionary models. The primary has the expected radius, but is cooler and
less luminous, while the secondary has the expected luminosity, but is cooler
and substantially larger (by 20%). The system is not tidally locked or
circularized. Exploiting a fortuitous 4:5 commensurability between $P_{orb}$
and $P_{rot,prim}$, we demonstrate that fitting errors from the unknown spot
configuration only change the inferred radii by <1--2%. We also analyze subsets
of data to test the robustness of radius measurements; the radius sum is more
robust to systematic errors and preferable for model comparisons. We also test
plausible changes in limb darkening, and find corresponding uncertainties of
~1%. Finally, we validate our pipeline using extant data for GU Boo, finding
that our independent results match previous radii to within the mutual
uncertainties (2--3%). We therefore suggest that the substantial discrepancies
are astrophysical; since they are larger than for old field stars, they may be
tied to the intermediate age of PTFEB132.707+19.810.
\\ ( https://arxiv.org/abs/1706.09390 ,  679kb)
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arXiv:1706.08779 (*cross-listing*)
Date: Tue, 27 Jun 2017 11:07:46 GMT   (80kb)

Title: A solution of the dark energy and its coincidence problem based on local
  antigravity sources without fine-tuning or new scales
Authors: Georgios Kofinas, Vasilios Zarikas
Categories: gr-qc astro-ph.CO hep-th
Comments: 30 pages, 2 figures
\\
  A novel idea is proposed for a natural solution of the dark energy and its
cosmic coincidence problem. The existence of local antigravity sources,
associated with astrophysical matter configurations distributed throughout the
universe, can lead to a recent cosmic acceleration effect. Various physical
theories can be compatible with this idea, but here, in order to test our
proposal, we focus on quantum originated spherically symmetric metrics matched
with the cosmological evolution through a Swiss cheese analysis. In the context
of asymptotically safe gravity, we have explained the observed amount of dark
energy using Newton's constant, the galaxy or cluster length scales, and
dimensionless order one parameters predicted by the theory, without fine-tuning
or extra unproven energy scales. The interior modified Schwarzschild-de Sitter
metric allows us to approximately interpret this result as that the standard
cosmological constant is a composite quantity made of the above parameters,
instead of a fundamental one.
\\ ( https://arxiv.org/abs/1706.08779 ,  80kb)
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\\
arXiv:1706.08907 (*cross-listing*)
Date: Tue, 27 Jun 2017 15:27:11 GMT   (1339kb)

Title: Compton Edge probing basic physics at Jefferson Laboratory: light speed
  isotropy and Lorentz invariance
Authors: Vahe Gurzadyan, David Gaskell, Vanik Kakoyan, Cynthia Keppel, Amur
  Margaryan, Harutyun Khachatryan, Sergey Mirzoyan, Dipangkar Dutta, Branislav
  Vlahovic, Steve Wood
Categories: physics.acc-ph astro-ph.CO
Comments: Submitted to PAC45, Jefferson Laboratory, 38 pages, 14 figures
\\
  We propose to study of the light speed isotropy and Lorentz invariance at
Jefferson Laboratory by means of the measurements of the Compton Edge using of
the Hall A/C existing experimental setup. Methodologically the same experiment
has already been successfully elaborated at GRAAL experiment at the European
Synchrotron Radiation Facility in Grenoble with 6 GeV electron beam. This
Proposal states two goals expected to be reached at Jefferson Laboratory, both
on Lorentz invariance: (a) the one-way light speed isotropy testing accuracy,
following from conservative evaluations at numerical simulations, to about an
order of magnitude better than was GRAAL's; (b) the dependence of the light
speed on the velocity of the apparatus (Kennedy-Thorndike measurement) will be
traced to an accuracy about 3 orders of magnitudes better than the available
limits.
\\ ( https://arxiv.org/abs/1706.08907 ,  1339kb)
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\\
arXiv:1706.09073 (*cross-listing*)
Date: Tue, 27 Jun 2017 23:32:41 GMT   (136kb)

Title: First-principles Equation of State and Shock Compression Predictions of
  Warm Dense Hydrocarbons
Authors: Shuai Zhang, Kevin P. Driver, Fran\c{c}ois Soubiran, Burkhard Militzer
Categories: physics.plasm-ph astro-ph.SR
Comments: 7 pages, 4 figures. Accepted by Physical Review E
\\
  We use path integral Monte Carlo and density functional molecular dynamics to
construct a coherent set of equation of state for a series of hydrocarbon
materials with various C:H ratios (2:1, 1:1, 2:3, 1:2, and 1:4) over the range
of $0.07-22.4$ g/cm$^{3}$ and $6.7\times10^3-1.29\times10^8$ K. The shock
Hugoniot curve derived for each material displays a single compression maximum
corresponding to $K$-shell ionization. For C:H=1:1, the compression maximum
occurs at 4.7-fold of the initial density and we show radiation effects
significantly increase the shock compression ratio above 2 Gbar, surpassing
relativistic effects. The single-peaked structure of the Hugoniot curves
contrasts with previous work on higher-$Z$ plasmas, which exhibit a two-peak
structure corresponding to both $K$- and $L$-shell ionization. Analysis of the
electronic density of states reveals that the change in Hugoniot structure is
due to merging of the $L$-shell eigenstates in carbon, while they remain
distinct for higher-$Z$ elements. Finally, we show that the isobaric-isothermal
linear mixing rule for carbon and hydrogen EOSs is a reasonable approximation
with errors better than 1% for stellar-core conditions.
\\ ( https://arxiv.org/abs/1706.09073 ,  136kb)
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\\
arXiv:1706.09191 (*cross-listing*)
Date: Wed, 28 Jun 2017 09:54:41 GMT   (567kb,D)

Title: The application of the Quark-Hadron Chiral Parity-Doublet Model to
  neutron star matter
Authors: A. Mukherjee, S. Schramm, J. Steinheimer and V. Dexheimer
Categories: nucl-th astro-ph.HE
Comments: 8 pages, 9 figures and 1 table
\\
  The Quark-Hadron Chiral Parity-Doublet Model (Q$\chi$P) is applied to
calculate compact star properties in the presence of a deconfinement phase
transition. Within this model, a consistent description of nuclear matter
properties, chiral symmetry restoration and a transition from hadronic to quark
and gluonic degrees of freedom is possible within one unified approach. We find
that the equation of state obtained is consistent with recent perturbative QCD
results and is able to accommodate observational constraints of massive and
small neutron stars. Furthermore, we show that important features of the
equation of state, like the symmetry energy and its slope, are well within
their observational constraints.
\\ ( https://arxiv.org/abs/1706.09191 ,  567kb)
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\\
arXiv:1706.09371 (*cross-listing*)
Date: Wed, 28 Jun 2017 17:21:15 GMT   (715kb,D)

Title: Phase transition effects on the dynamical stability of hybrid neutron
  stars
Authors: Jonas P. Pereira, C\'esar V. Flores and Germ\'an Lugones
Categories: gr-qc astro-ph.HE
Comments: 14 figures
\\
  We study radial oscillations of hybrid non-rotating neutron stars composed by
a quark matter core and hadronic external layers. At first, we deduce the
junction conditions that should be imposed between two any phases in these
systems when perturbations take place. Then we compute the spectrum exhibited
by the radial oscillations of hybrid neutron stars focusing on the effects of
slow and rapid phase conversions at the quark-hadron interface. For the quark
matter core, we use a generic MIT bag model that allows the inclusion of the
effects of finite quark masses, strong interactions and color
superconductivity. For the hadronic phase, we use a relativistic mean field
theory widely used to describe hadronic matter in neutron stars. In the case of
rapid transitions we report the presence of a new mode, that could be either
the fundamental mode or the first excited one, depending on the equation of
state parametrizations. We show that the speed of the phase conversion at the
hybrid interface plays a key role on the stability of the star as a whole. The
static stability condition $\partial M/\partial \rho_c\geq 0$, where $\rho_c$
is the central density of a star whose total mass is $M$, remains always true
for rapid phase transitions but breaks down in general for slow phase
transitions. In fact, we find that the frequency of the fundamental mode can be
a real number (indicating stability) even for some branches of stellar models
that verify $\partial M/\partial \rho_c \leq 0$. This may lead to the existence
of twin or even triplet stars with the same gravitational mass but different
radii which, if observed, could reveal the nature of reactions in stars and by
consequence their hybrid nature and aspects of their innermost phases.
\\ ( https://arxiv.org/abs/1706.09371 ,  715kb)
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\\
arXiv:1706.09378 (*cross-listing*)
Date: Wed, 28 Jun 2017 17:38:10 GMT   (3257kb,D)

Title: Towards a medium-scale axion helioscope and haloscope
Authors: V. Anastassopoulos, F. Avignone, A. Bykov, G. Cantatore, S.A. Cetin,
  A. Derbin, I. Drachnev, R. Dzhilkibaev, V. Eremin, H. Fischer, A. Gangapshev,
  A. Gardikiotis, S. Gninenko, N. Golubev, D.H.H. Hoffmann, M. Karuza, M.
  Libanov, A. Lutovinov, M. Maroudas V. Matveev, S. Molkov, V. Muratova, V.
  Pantuev, M. Pavlinsky, K. Ptitsyna, G. Rubtsov, D. Semenov, P. Sikivie, A.
  Spiridonov, P. Tinyakov, I. Tkachev, S. Troitsky, E. Unzhakov and K. Zioutas
Categories: hep-ph astro-ph.HE hep-ex
Comments: 38 pages, 15 figures, JINST style
\\
  We discuss the physics case for and the concept of a medium-scale axion
helioscope with sensitivities in the axion-photon coupling a few times better
than CERN Axion Solar Telescope (CAST). Search for an axion-like particle with
these couplings is motivated by several persistent astrophysical anomalies. We
present early conceptual design, existing infrastructure, projected sensitivity
and timeline of such a helioscope (Troitsk Axion Solar Telescope Experiment,
TASTE) to be constructed in the Institute for Nuclear Research, Troitsk,
Russia. The proposed instrument may be also used for the search of dark-matter
halo axions.
\\ ( https://arxiv.org/abs/1706.09378 ,  3257kb)
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\\
arXiv:1706.09383 (*cross-listing*)
Date: Wed, 28 Jun 2017 17:50:32 GMT   (246kb,D)

Title: Weak gravitational lensing of finite beams
Authors: Pierre Fleury, Julien Larena, Jean-Philippe Uzan
Categories: gr-qc astro-ph.CO
Comments: 6 pages, 2 figures
\\
  The standard theory of weak gravitational lensing relies on the infinitesimal
light beam approximation. In this context, images are distorted by convergence
and shear, the respective sources of which unphysically depend on the
resolution of the distribution of matter---the so-called Ricci-Weyl problem. In
this letter, we propose a strong-lensing-inspired formalism to describe the
lensing of finite beams. We address the Ricci-Weyl problem by showing
explicitly that convergence is caused by the matter enclosed by the beam,
regardless of its distribution. Furthermore, shear turns out to be
systematically enhanced by the finiteness of the beam. This implies, in
particular, that the Kaiser-Squires relation between shear and convergence is
violated, which could have profound consequences on the interpretation of weak
lensing surveys.
\\ ( https://arxiv.org/abs/1706.09383 ,  246kb)
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arXiv:1508.06701 (*cross-listing*)
replaced with revised version Wed, 28 Jun 2017 15:27:27 GMT   (543kb)

Title: Deforming regular black holes
Authors: J. C. S. Neves
Categories: gr-qc astro-ph.CO
Comments: 9 pages, 4 figures. Version 3 matches the published version in IJMPA
Journal-ref: Int. J. Mod. Phys. A 32, 1750112 (2017)
DOI: 10.1142/S0217751X17501123
\\ ( https://arxiv.org/abs/1508.06701 ,  543kb)
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\\
arXiv:1607.02151
replaced with revised version Tue, 27 Jun 2017 19:50:59 GMT   (3271kb,D)

Title: The Romulus Cosmological Simulations: A Physical Approach to the
  Formation, Dynamics and Accretion Models of SMBHs
Authors: Michael Tremmel, Michael Karcher, Fabio Governato, Marta Volonteri,
  Tom Quinn, Andrew Pontzen, Lauren Anderson, Jillian Bellovary
Categories: astro-ph.GA
Comments: 21 pages, 17 figures, Accepted to MNRAS, in press. Updated references
\\ ( https://arxiv.org/abs/1607.02151 ,  3271kb)
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\\
arXiv:1610.03509
replaced with revised version Tue, 27 Jun 2017 19:39:58 GMT   (128kb)

Title: Implications of the Occurrence of Glitches in Pulsar Free Precession
  Candidates
Authors: D. I. Jones, G. Ashton and R. Prix
Categories: astro-ph.HE
Comments: 5 pages, updated following comments, published in Phys. Rev. Lett
Journal-ref: Phys. Rev. Lett. 118, 261101 (2017)
DOI: 10.1103/PhysRevLett.118.261101
\\ ( https://arxiv.org/abs/1610.03509 ,  128kb)
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\\
arXiv:1610.07191
replaced with revised version Wed, 28 Jun 2017 16:42:01 GMT   (331kb)

Title: A New Measurement of the Spectral Lag of Gamma-Ray Bursts and its
  Implications for Spectral Evolution Behaviors
Authors: Lang Shao, Bin-Bin Zhang, Fu-Ri Wang, Xue-Feng Wu, Ye-Hao Cheng, Xi
  Zhang, Bang-Yao Yu, Bao-Jia Xi, Xue Wang, Huan-Xue Feng, Meng Zhang, Dong Xu
Categories: astro-ph.HE
Comments: 21 pages, 8 figures, accepted for publication in ApJ
\\ ( https://arxiv.org/abs/1610.07191 ,  331kb)
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\\
arXiv:1611.06977
replaced with revised version Wed, 28 Jun 2017 15:12:20 GMT   (3272kb,D)

Title: Detecting pulsars in the Galactic centre
Authors: Kaustubh Rajwade, Duncan Lorimer, Loren Anderson
Categories: astro-ph.HE
Comments: 9 pages, 6 Figures, 4 tables. Revised calculation of upper limits and
  scattering efficiency based on referee's comments. Accepted for publication
  in MNRAS
\\ ( https://arxiv.org/abs/1611.06977 ,  3272kb)
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\\
arXiv:1611.09362
replaced with revised version Wed, 28 Jun 2017 09:44:22 GMT   (1052kb,D)

Title: Hints against the cold and collisionless nature of dark matter from the
  galaxy velocity function
Authors: Aurel Schneider, Sebastian Trujillo-Gomez, Emmanouil Papastergis,
  Darren S. Reed, George Lake
Categories: astro-ph.CO hep-ph
Comments: Matches published version
\\ ( https://arxiv.org/abs/1611.09362 ,  1052kb)
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\\
arXiv:1612.00457
replaced with revised version Wed, 28 Jun 2017 08:26:36 GMT   (319kb,D)

Title: Searching for Primordial Black Holes in the radio and X-ray sky
Authors: Daniele Gaggero, Gianfranco Bertone, Francesca Calore, Riley M.T.
  Connors, Mark Lovell, Sera Markoff, Emma Storm
Categories: astro-ph.HE
Comments: 5 pages, 2 figures
Journal-ref: Phys. Rev. Lett. 118, 241101 (2017)
DOI: 10.1103/PhysRevLett.118.241101
\\ ( https://arxiv.org/abs/1612.00457 ,  319kb)
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\\
arXiv:1701.02355
replaced with revised version Wed, 28 Jun 2017 06:03:03 GMT   (468kb,D)

Title: Forming short-period Wolf-Rayet X-ray binaries and double black holes
  through stable mass transfer
Authors: Edward P.J. van den Heuvel (UvA), Simon F. Portegies Zwart (Leiden
  Observatory), Selma E. de Mink (UvA)
Categories: astro-ph.SR astro-ph.HE
Comments: MNRAS in press
\\ ( https://arxiv.org/abs/1701.02355 ,  468kb)
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arXiv:1701.07073
replaced with revised version Wed, 28 Jun 2017 17:00:57 GMT   (1312kb,D)

Title: Observational evidence for high neutronization in supernova remnants:
  implications for Type Ia supernova progenitors
Authors: H\'ector Mart\'inez-Rodr\'iguez, Carles Badenes, Hiroya Yamaguchi,
  Eduardo Bravo, F. X. Timmes, Broxton J. Miles, Dean M. Townsley, Anthony L.
  Piro, Hideyuki Mori, Brett Andrews, and Sangwook Park
Categories: astro-ph.HE
Comments: 12 pages, 7 figures, accepted for publication in the ApJ
Journal-ref: The Astrophysical Journal, 843, 35 (2017)
DOI: 10.3847/1538-4357/aa72f8
\\ ( https://arxiv.org/abs/1701.07073 ,  1312kb)
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arXiv:1703.00878
replaced with revised version Wed, 28 Jun 2017 17:41:40 GMT   (18kb)

Title: Enhanced interplanetary panspermia in the TRAPPIST-1 system
Authors: Manasvi Lingam and Abraham Loeb
Categories: astro-ph.EP
Comments: published in Proceedings of the National Academy of Sciences; 7 pages
Journal-ref: PNAS, 114, 6689 (2017)
DOI: 10.1073/pnas.1703517114
\\ ( https://arxiv.org/abs/1703.00878 ,  18kb)
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arXiv:1703.01623 (*cross-listing*)
replaced with revised version Wed, 28 Jun 2017 11:29:51 GMT   (43kb,D)

Title: Higher Derivative Field Theories: Degeneracy Conditions and Classes
Authors: Marco Crisostomi, Remko Klein, Diederik Roest
Categories: hep-th astro-ph.CO gr-qc
Comments: 26 pages, 1 figure. v2: minor changes, references added, matches
  version published in JHEP
Journal-ref: Journal of High Energy Physics, (6), 1-29 (2017)
DOI: 10.1007/JHEP06(2017)124
\\ ( https://arxiv.org/abs/1703.01623 ,  43kb)
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arXiv:1703.02432
replaced with revised version Wed, 28 Jun 2017 09:00:18 GMT   (62kb,D)

Title: An algorithm for the reconstruction of high-energy neutrino-induced
  particle showers and its application to the ANTARES neutrino telescope
Authors: ANTARES Collaboration: A. Albert, M. Andr\'e, M. Anghinolfi, G. Anton,
  M. Ardid, J.-J. Aubert, T. Avgitas, B. Baret, J. Barrios-Mart\'i, S. Basa, V.
  Bertin, S. Biagi, R. Bormuth, S. Bourret, M.C. Bouwhuis, R. Bruijn, J.
  Brunner, J. Busto, A. Capone, L. Caramete, J. Carr, S. Celli, T. Chiarusi, M.
  Circella, J. A. B. Coelho, A. Coleiro, R. Coniglione, H. Costantini, P.
  Coyle, A. Creusot, A. Deschamps, G. De Bonis, C. Distefano, I. Di Palma, A.
  Domi, C. Donzaud, D. Dornic, D. Drouhin, T. Eberl, I. El Bojaddaini, D.
  Els\"asser, A. Enzenh\"ofer, I. Felis, F. Folger, L. A. Fusco, S. Galat\`a,
  P. Gay, V. Giordano, H. Glotin, T. Gr\'egoire, R. Gracia Ruiz, K. Graf, S.
  Hallmann, H. van Haren, A. J. Heijboer, Y. Hello, J. J. Hern\'andez-Rey, J.
  H\"o{\ss}l, J. Hofest\"adt, C. Hugon, G. Illuminati, C. W. James, et al. (59
  additional authors not shown)
Categories: astro-ph.HE
Comments: published version
Journal-ref: Eur. Phys. J. C (2017) 77: 419
DOI: 10.1140/epjc/s10052-017-4979-2
\\ ( https://arxiv.org/abs/1703.02432 ,  62kb)
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arXiv:1703.03083
replaced with revised version Tue, 27 Jun 2017 20:08:27 GMT   (1083kb,D)

Title: The first supermassive black holes
Authors: Aaron Smith, Volker Bromm, Abraham Loeb
Categories: astro-ph.GA
Comments: Invited review, Astronomy & Geophysics, 6 pages, 6 figures, updated
  to reflect the printed version
Journal-ref: Smith, A., Bromm, V., Loeb, A., 2017, Astronomy & Geophysics, 58,
  3.22
DOI: 10.1093/astrogeo/atx099
\\ ( https://arxiv.org/abs/1703.03083 ,  1083kb)
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arXiv:1704.00373
replaced with revised version Wed, 28 Jun 2017 10:50:14 GMT   (300kb,A)

Title: The GAPS Programme with HARPS-N@TNG XIV. Investigating giant planet
  migration history via improved eccentricity and mass determination for 231
  transiting planets
Authors: A. S. Bonomo, S. Desidera, S. Benatti, F. Borsa, S. Crespi, M.
  Damasso, A. F. Lanza, A. Sozzetti, G. Lodato, F. Marzari, C. Boccato, R. U.
  Claudi, R. Cosentino, E. Covino, R. Gratton, A. Maggio, G. Micela, E.
  Molinari, I. Pagano, G. Piotto, E. Poretti, R. Smareglia, L. Affer, K.
  Biazzo, A. Bignamini, M. Esposito, P. Giacobbe, G. H\'ebrard, L. Malavolta,
  J. Maldonado, L. Mancini, A. Martinez Fiorenzano, S. Masiero, V. Nascimbeni,
  M. Pedani, M. Rainer, G. Scandariato
Categories: astro-ph.EP astro-ph.SR
Comments: 44 pages (16 pages of main text and figures), 11 figures, 5
  longtables, published in Astronomy and Astrophysics, Volume 602, A107 (2017).
  Tables with new HARPS-N and TRES radial-velocity data (Tables 1 and 2),
  stellar parameters (Table 7), orbital parameters and RV jitter (Table 8), and
  planet physical parameters (Table 9) are available as ancillary files
  (sidebar on the right)
DOI: 10.1051/0004-6361/201629882
\\ ( https://arxiv.org/abs/1704.00373 ,  300kb)
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arXiv:1704.05059
replaced with revised version Wed, 28 Jun 2017 09:01:38 GMT   (17kb)

Title: Magnetic field line random walk in two-dimensional dynamical turbulence
Authors: J. F. Wang, G. Qin, Q. M. Ma, T. Song, S. B. Yuan
Categories: astro-ph.HE astro-ph.SR
\\ ( https://arxiv.org/abs/1704.05059 ,  17kb)
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arXiv:1704.05094
replaced with revised version Wed, 28 Jun 2017 08:17:48 GMT   (136kb,D)

Title: Plasma Constraints on the Cosmological Abundance of Magnetic Monopoles
  and the Origin of Cosmic Magnetic Fields
Authors: Mikhail V. Medvedev, Abraham Loeb
Categories: astro-ph.CO gr-qc hep-th physics.plasm-ph
Comments: 7 pages, 1 figure, JCAP, in press
\\ ( https://arxiv.org/abs/1704.05094 ,  136kb)
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arXiv:1704.07365
replaced with revised version Tue, 27 Jun 2017 18:11:22 GMT   (1358kb,D)

Title: Observational consequences of optical band milliarcsecond-scale
  structure in active galactic nuclei discovered by Gaia
Authors: Leonid Petrov, Yuri Y. Kovalev
Categories: astro-ph.HE astro-ph.GA
Comments: Revised in accordance with received comments
\\ ( https://arxiv.org/abs/1704.07365 ,  1358kb)
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arXiv:1704.09009
replaced with revised version Wed, 28 Jun 2017 03:28:14 GMT   (111kb)

Title: Evolution of coexisting long and short period stellar activity cycles
Authors: Axel Brandenburg, Savita Mathur, Travis S. Metcalfe
Categories: astro-ph.SR
Comments: 13 pages, 11 figures, 4 tables, resubmitted to ApJ, improved version
  with stellar ages etc
Report-no: NORDITA 2017-041
\\ ( https://arxiv.org/abs/1704.09009 ,  111kb)
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arXiv:1705.01606
replaced with revised version Tue, 27 Jun 2017 18:19:37 GMT   (7694kb,D)

Title: Gemini Observations of Galaxies in Rich Early Environments (GOGREEN) I:
  Survey Description
Authors: Michael L. Balogh, David G. Gilbank, Adam Muzzin, Gregory Rudnick,
  Michael C. Cooper, Chris Lidman, Andrea Biviano, Ricardo Demarco, Sean L.
  McGee, Julie B. Nantais, Allison Noble, Lyndsay Old, Gillian Wilson, Howard
  K.C. Yee, Callum Bellhouse, Pierluigi Cerulo, Jeffrey Chan, Irene
  Pintos-Castro, Rane Simpson, Remco F.J. van der Burg, Dennis Zaritsky,
  Felicia Ziparo, M. Victoria Alonso, Richard G. Bower, Gabriella De Lucia,
  Alexis Finoguenov, Diego Garcia Lambas, Hernan Muriel, Laura C. Parker,
  Alessandro Rettura, Carlos Valotto, Andrew Wetzel
Categories: astro-ph.GA
Comments: Accepted for publication in MNRAS May 26, 2017
\\ ( https://arxiv.org/abs/1705.01606 ,  7694kb)
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arXiv:1705.07799
replaced with revised version Wed, 28 Jun 2017 17:38:52 GMT   (5426kb)

Title: 3D Relativistic MHD numerical simulations of X-shaped radio sources
Authors: P. Rossi, G. Bodo, A. Capetti, S. Massaglia
Categories: astro-ph.GA
Comments: 13 pages, 16 figures, Astronomy and Astrophysics accepted
DOI: 10.1051/0004-6361/201730594
\\ ( https://arxiv.org/abs/1705.07799 ,  5426kb)
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arXiv:1705.08945 (*cross-listing*)
replaced with revised version Wed, 28 Jun 2017 12:46:30 GMT   (28kb)

Title: Does information entropy play a role in the expansion and acceleration
  of the Universe?
Authors: Biswajit Pandey
Categories: gr-qc astro-ph.CO
Comments: 4 pages, no figures, minor revision, Accepted for publication in
  MNRAS Letters
\\ ( https://arxiv.org/abs/1705.08945 ,  28kb)
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arXiv:1706.01916
replaced with revised version Tue, 27 Jun 2017 19:05:19 GMT   (4924kb,D)

Title: Understanding `galaxy groups' as a unique structure in the universe
Authors: S. Paul (1), R. S. John (2), P. Gupta (1) and H. Kumar (2) ((1)
  Department of Physics, SP Pune University, Pune, India, (2) Department. of
  Physics, Pondicherry Engineering College, Pondicherry, India)
Categories: astro-ph.CO astro-ph.GA
Comments: 11 pages, 11 figures, Accepted for publication in MNRAS
DOI: 10.1093/mnras/stx1488
\\ ( https://arxiv.org/abs/1706.01916 ,  4924kb)
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arXiv:1706.03188
replaced with revised version Tue, 27 Jun 2017 21:23:53 GMT   (322kb,D)

Title: Radiative Transfer for Exoplanet Atmospheres
Authors: Kevin Heng, Mark Marley
Categories: astro-ph.EP physics.ao-ph
Comments: 7 pages, no figures, 1 table. Filled in missing information in
  references, main text unchanged
\\ ( https://arxiv.org/abs/1706.03188 ,  322kb)
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arXiv:1706.04790
replaced with revised version Wed, 28 Jun 2017 11:23:10 GMT   (235kb)

Title: The effect of stellar and AGN feedback on the low redshift
  Lyman-$\alpha$ forest in the Sherwood simulation suite
Authors: Fahad Nasir, James S. Bolton, Matteo Viel, Tae-Sun Kim, Martin G.
  Haehnelt, Ewald Puchwein, Debora Sijacki
Categories: astro-ph.CO astro-ph.GA
Comments: 16 pages, 8 figures, Accepted to MNRAS
\\ ( https://arxiv.org/abs/1706.04790 ,  235kb)
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arXiv:1706.05459
replaced with revised version Wed, 28 Jun 2017 01:50:00 GMT   (1634kb,D)

Title: Inferring probabilistic stellar rotation periods using Gaussian
  processes
Authors: Ruth Angus, Timothy Morton, Suzanne Aigrain, Daniel Foreman-Mackey,
  Vinesh Rajpaul
Categories: astro-ph.SR astro-ph.IM
Comments: Submitted to MNRAS. Replaced 27/06/2017: corrections made to
  koi_periods.csv
\\ ( https://arxiv.org/abs/1706.05459 ,  1634kb)
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arXiv:1706.06108
replaced with revised version Wed, 28 Jun 2017 16:07:38 GMT   (1505kb,D)

Title: Microflare Heating of a Solar Active Region Observed with NuSTAR,
  Hinode/XRT, and SDO/AIA
Authors: Paul J. Wright, Iain G. Hannah, Brian W. Grefenstette, Lindsay
  Glesener, S\"am Krucker, Hugh S. Hudson, David M. Smith, Andrew J. Marsh,
  Stephen M. White and Matej Kuhar
Categories: astro-ph.SR
Comments: Accepted for publication in ApJ. 14 pages with 12 figures and 1 table
\\ ( https://arxiv.org/abs/1706.06108 ,  1505kb)
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arXiv:1706.08009 (*cross-listing*)
replaced with revised version Wed, 28 Jun 2017 09:50:54 GMT   (39kb)

Title: Pulsations of a black hole in loop quantum gravity
Authors: Changjun Gao, Youjun Lu, You-Gen Shen and Valerio Faraoni
Categories: gr-qc astro-ph.CO hep-th
Comments: 24 pages, 2 figures
\\ ( https://arxiv.org/abs/1706.08009 ,  39kb)
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arXiv:1706.08539
replaced with revised version Wed, 28 Jun 2017 17:45:07 GMT   (2389kb,D)

Title: The Galaxy in circular polarization: all-sky radio prediction, detection
  strategy, and the charge of the leptonic cosmic rays
Authors: Torsten A. En{\ss}lin, Sebastian Hutschenreuter, Valentina Vacca, and
  Niels Oppermann
Categories: astro-ph.HE
Comments: 10 pages, 4 figures, submitted
\\ ( https://arxiv.org/abs/1706.08539 ,  2389kb)
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