257 research outputs found
The VANDELS survey: Dust attenuation in star-forming galaxies at
We present the results of a new study of dust attenuation at redshifts based on a sample of star-forming galaxies from the VANDELS
spectroscopic survey. Motivated by results from the First Billion Years (FiBY)
simulation project, we argue that the intrinsic spectral energy distributions
(SEDs) of star-forming galaxies at these redshifts have a self-similar shape
across the mass range log probed by
our sample. Using FiBY data, we construct a set of intrinsic SED templates
which incorporate both detailed star formation and chemical abundance
histories, and a variety of stellar population synthesis (SPS) model
assumptions. With this set of intrinsic SEDs, we present a novel approach for
directly recovering the shape and normalization of the dust attenuation curve.
We find, across all of the intrinsic templates considered, that the average
attenuation curve for star-forming galaxies at is similar in shape
to the commonly-adopted Calzetti starburst law, with an average
total-to-selective attenuation ratio of . We show that the
optical attenuation () versus stellar mass () relation
predicted using our method is consistent with recent ALMA observations of
galaxies at in the \emph{Hubble} \emph{Ultra} \emph{Deep} \emph{Field}
(HUDF), as well as empirical relations predicted by a
Calzetti-like law. Our results, combined with other literature data, suggest
that the relation does not evolve over the redshift range
, at least for galaxies with log.
Finally, we present tentative evidence which suggests that the attenuation
curve may become steeper at log.Comment: 16 pages, 12 figures, accepted for publication in MNRA
The VANDELS survey: Dust attenuation in star-forming galaxies at
We present the results of a new study of dust attenuation at redshifts based on a sample of star-forming galaxies from the VANDELS
spectroscopic survey. Motivated by results from the First Billion Years (FiBY)
simulation project, we argue that the intrinsic spectral energy distributions
(SEDs) of star-forming galaxies at these redshifts have a self-similar shape
across the mass range log probed by
our sample. Using FiBY data, we construct a set of intrinsic SED templates
which incorporate both detailed star formation and chemical abundance
histories, and a variety of stellar population synthesis (SPS) model
assumptions. With this set of intrinsic SEDs, we present a novel approach for
directly recovering the shape and normalization of the dust attenuation curve.
We find, across all of the intrinsic templates considered, that the average
attenuation curve for star-forming galaxies at is similar in shape
to the commonly-adopted Calzetti starburst law, with an average
total-to-selective attenuation ratio of . We show that the
optical attenuation () versus stellar mass () relation
predicted using our method is consistent with recent ALMA observations of
galaxies at in the \emph{Hubble} \emph{Ultra} \emph{Deep} \emph{Field}
(HUDF), as well as empirical relations predicted by a
Calzetti-like law. Our results, combined with other literature data, suggest
that the relation does not evolve over the redshift range
, at least for galaxies with log.
Finally, we present tentative evidence which suggests that the attenuation
curve may become steeper at log.Comment: 16 pages, 12 figures, accepted for publication in MNRA
The COBE Diffuse Infrared Background Experiment Search for the Cosmic Infrared Background: IV. Cosmological Implications
In this paper we examine the cosmological constraints of the recent DIRBE and
FIRAS detection of the extragalactic background light between 125-5000 microns
on the metal and star formation histories of the universe.Comment: 38 pages and 9 figures. Accepted for publications in The
Astrophysical Journa
Off-Center Collisions between Clusters of Galaxies
We present numerical simulations of off-center collisions between galaxy
clusters made using a new hydrodynamical code based on the piecewise-parabolic
method (PPM) and an isolated multigrid Poisson solver. We have performed three
gas-only high-resolution simulations of collisions between equal-mass clusters
with different values of the impact parameter (0, 5, and 10 times the core
radius). With these simulations we have studied the observational appearance of
the merging clusters and the variation in equilibration time, luminosity
enhancement during the collision, and structure of the merger remnant with
varying impact parameter. Observational evidence of an ongoing collision is
present for 1-2 sound crossing times after the collision, but only for special
viewing angles. The remnant actually requires at least five crossing times to
reach virial equilibrium. Since the sound crossing time can be as large as 1-2
Gyr, the equilibration time can thus be a large fraction of the age of the
universe. The final merger remnant is very similar for impact parameters of
zero and five core radii. It possesses a roughly isothermal core, with central
density and temperature twice the initial values. Outside the core the
temperature drops as r^-1, and the density roughly as r^-3.8. The core radius
shows a small increase due to shock heating during the merger. For an impact
parameter of ten core radii the core of the remnant possesses a more flattened
density profile, with a steeper dropoff outside the core. In both off-center
cases the merger remnant rotates, but only for the ten-core-radius case does
this appear to have an effect on the structure of the remnant.Comment: 26 pages, 15 figures included, submitted to ApJ; for color figures
and movies see http://www.astro.virginia.edu/~pmr7u/paper_offctr.htm
Tree-formed Verification Data for Trusted Platforms
The establishment of trust relationships to a computing platform relies on
validation processes. Validation allows an external entity to build trust in
the expected behaviour of the platform based on provided evidence of the
platform's configuration. In a process like remote attestation, the 'trusted'
platform submits verification data created during a start up process. These
data consist of hardware-protected values of platform configuration registers,
containing nested measurement values, e.g., hash values, of loaded or started
components. Commonly, the register values are created in linear order by a
hardware-secured operation. Fine-grained diagnosis of components, based on the
linear order of verification data and associated measurement logs, is not
optimal. We propose a method to use tree-formed verification data to validate a
platform. Component measurement values represent leaves, and protected
registers represent roots of a hash tree. We describe the basic mechanism of
validating a platform using tree-formed measurement logs and root registers and
show an logarithmic speed-up for the search of faults. Secure creation of a
tree is possible using a limited number of hardware-protected registers and a
single protected operation. In this way, the security of tree-formed
verification data is maintained.Comment: 15 pages, 11 figures, v3: Reference added, v4: Revised, accepted for
publication in Computers and Securit
The Mass Function of an X-Ray Flux-Limited Sample of Galaxy Clusters
A new X-ray selected and X-ray flux-limited galaxy cluster sample is
presented. Based on the ROSAT All-Sky Survey the 63 brightest clusters with
galactic latitude |bII| >= 20 deg and flux fx(0.1-2.4 keV) >= 2 * 10^{-11}
ergs/s/cm^2 have been compiled. Gravitational masses have been determined
utilizing intracluster gas density profiles, derived mainly from ROSAT PSPC
pointed observations, and gas temperatures, as published mainly from ASCA
observations, assuming hydrostatic equilibrium. This sample and an extended
sample of 106 galaxy clusters is used to establish the X-ray
luminosity--gravitational mass relation. From the complete sample the galaxy
cluster mass function is determined and used to constrain the mean cosmic
matter density and the amplitude of mass fluctuations. Comparison to
Press--Schechter type model mass functions in the framework of Cold Dark Matter
cosmological models and a Harrison--Zeldovich initial density fluctuation
spectrum yields the constraints OmegaM = 0.12^{+0.06}_{-0.04} and sigma8 =
0.96^{+0.15}_{-0.12} (90% c.l.). Various possible systematic uncertainties are
quantified. Adding all identified systematic uncertainties to the statistical
uncertainty in a worst case fashion results in an upper limit OmegaM < 0.31.
For comparison to previous results a relation sigma8 = 0.43 OmegaM^{-0.38} is
derived. The mass function is integrated to show that the contribution of mass
bound within virialized cluster regions to the total matter density is small,
i.e., OmegaCluster = 0.012^{+0.003}_{-0.004} for cluster masses larger than
6.4^{+0.7}_{-0.6} * 10^{13} h_{50}^{-1} Msun.Comment: 35 pages; accepted for publication in The Astrophysical Journal; this
and related papers, supplementary information, as well as electronic files of
the tables given in this paper are available at
http://www.astro.virginia.edu/~thr4f
The Cosmic Infrared Background: Measurements and Implications
The cosmic infrared background records much of the radiant energy released by
processes of structure formation that have occurred since the decoupling of
matter and radiation following the Big Bang. In the past few years, data from
the Cosmic Background Explorer mission provided the first measurements of this
background, with additional constraints coming from studies of the attenuation
of TeV gamma-rays. At the same time there has been rapid progress in resolving
a significant fraction of this background with the deep galaxy counts at
infrared wavelengths from the Infrared Space Observatory instruments and at
submillimeter wavelengths from the Submillimeter Common User Bolometer Array
instrument. This article reviews the measurements of the infrared background
and sources contributing to it, and discusses the implications for past and
present cosmic processes.Comment: 61 pages, incl. 9 figures, to be published in Annual Reviews of
Astronomy and Astrophysics, 2001, Vol. 3
The ISO-IRAS Faint Galaxy Survey: Early results
We present preliminary results for AGNs and starburst galaxies the ISO-IRAS Faint Galaxy Survey (IIFGS). The goal of the survey is to produce a database of infrared-luminous galaxies at redshifts of about 0.1–1 to help explore the AGN-starburst relationship, study the cosmological evolution of luminous infrared galaxies, and identify possible protogalaxy candidates. The candidate list of ∼3700 sources has been extracted from the IRAS Faint Source Survey using criteria selecting for faint, infrared-bright galaxies. The ISO observations will confirm the IRAS detections, yield sensitive 12 & 90 μm fluxes, and provide positions to ∼6" accuracy which will allow unambiguous optical identifications. Confirmed sources are being followed up with ground-based observations to determine optical magnitudes and accurate redshifts. In this preliminary phase we have in hand ∼100 observed fields and are developing techniques to maximize the sensitivity of the observations. Early results for the ISOCAM 12 μm images indicate we can reliably detect sources as faint as ∼0.5 mJy; ∼80% of the fields contain at least one source
Adiabatic and entropy perturbations propagation in a bouncing Universe
By studying some bouncing universe models dominated by a specific class of
hydrodynamical fluids, we show that the primordial cosmological perturbations
may propagate smoothly through a general relativistic bounce. We also find that
the purely adiabatic modes, although almost always fruitfully investigated in
all other contexts in cosmology, are meaningless in the bounce or null energy
condition (NEC) violation cases since the entropy modes can never be neglected
in these situations: the adiabatic modes exhibit a fake divergence that is
compensated in the total Bardeen gravitational potential by inclusion of the
entropy perturbations.Comment: 25 pages, no figure, LaTe
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