6,188 research outputs found
The star-formation history of the universe - an infrared perspective
A simple and versatile parameterized approach to the star formation history
allows a quantitative investigation of the constraints from far infrared and
submillimetre counts and background intensity measurements.
The models include four spectral components: infrared cirrus (emission from
interstellar dust), an M82-like starburst, an Arp220-like starburst and an AGN
dust torus. The 60 m luminosity function is determined for each chosen
rate of evolution using the PSCz redshift data for 15000 galaxies. The
proportions of each spectral type as a function of 60 m luminosity are
chosen for consistency with IRAS and SCUBA colour-luminosity relations, and
with the fraction of AGN as a function of luminosity found in 12 m
samples. The luminosity function for each component at any wavelength can then
be calculated from the assumed spectral energy distributions. With assumptions
about the optical seds corresponding to each component and, for the AGN
component, the optical and near infrared counts can be accurately modelled.
A good fit to the observed counts at 0.44, 2.2, 15, 60, 90, 175 and 850
m can be found with pure luminosity evolution in all 3 cosmological models
investigated: = 1, = 0.3 ( = 0), and
= 0.3, = 0.7.
All 3 models also give an acceptable fit to the integrated background
spectrum. Selected predictions of the models, for example redshift
distributions for each component at selected wavelengths and fluxes, are shown.
The total mass-density of stars generated is consistent with that observed,
in all 3 cosmological models.Comment: 20 pages, 25 figures. Accepted for publication in ApJ. Full details
of models can be found at http://astro.ic.ac.uk/~mrr/countmodel
Detections and Constraints on White Dwarf Variability from Time-Series GALEX Observations
We search for photometric variability in more than 23,000 known and candidate
white dwarfs, the largest ultraviolet survey compiled for a single study of
white dwarfs. We use gPhoton, a publicly available calibration/reduction
pipeline, to generate time-series photometry of white dwarfs observed by GALEX.
By implementing a system of weighted metrics, we select sources with
variability due to pulsations and eclipses. Although GALEX observations have
short baselines (< 30 min), we identify intrinsic variability in sources as
faint as Gaia G = 20 mag. With our ranking algorithm, we identify 49 new
variable white dwarfs (WDs) in archival GALEX observations. We detect 41 new
pulsators: 37 have hydrogen-dominated atmospheres (DAVs), including one
possible massive DAV, and four are helium-dominated pulsators (DBVs). We also
detect eight new eclipsing systems; five are new discoveries, and three were
previously known spectroscopic binaries. We perform synthetic injections of the
light curve of WD 1145+017, a system with known transiting debris, to test our
ability to recover similar systems. We find that the 3{\sigma} maximum
occurrence rate of WD 1145+017-like transiting objects is < 0.5%.Comment: 17 pages, 13 figure
The Redshift of GRB 970508
GRB 970508 is the second gamma-ray burst (GRB) for which an optical afterglow
has been detected. It is the first GRB for which a distance scale has been
determined: absorption and emission features in spectra of the optical
afterglow place GRB 970508 at a redshift of z >= 0.835 (Metzger et al. 1997a,
1997b). The lack of a Lyman-alpha forest in these spectra further constrains
this redshift to be less than approximately 2.3. I show that the spectrum of
the optical afterglow of GRB 970508, once corrected for Galactic absorption, is
inconsistent with the relativistic blast-wave model unless a second, redshifted
source of extinction is introduced. This second source of extinction may be the
yet unobserved host galaxy. I determine its redshift to be z =
1.09^{+0.14}_{-0.41}, which is consistent with the observed redshift of z =
0.835. Redshifts greater than z = 1.40 are ruled out at the 3 sigma confidence
level.Comment: Accepted to The Astrophysical Journal (Letters), 10 pages, LaTe
The Global Star Formation Rate from the 1.4 GHz Luminosity Function
The decimetric luminosity of many galaxies appears to be dominated by
synchrotron emission excited by supernova explosions. Simple models suggest
that the luminosity is directly proportional to the rate of supernova
explosions of massive stars averaged over the past 30 Myr. The proportionality
may be used together with models of the evolving 1.4 GHz luminosity function to
estimate the global star formation rate density in the era z < 1. The local
value is estimated to be 0.026 solar masses per year per cubic megaparsec, some
50% larger than the value inferred from the Halpha luminosity density. The
value at z ~ 1 is found to be 0.30 solar masses per year per cubic megaparsec.
The 10-fold increase in star formation rate density is consistent with the
increase inferred from mm-wave, far-infrared, ultra-violet and Halpha
observations.Comment: 10 pages, 2 figures, Astrophysical Journal Letters (in press); new PS
version has improved figure placemen
Starburst and AGN activity in ultraluminous infrared galaxies
(Abridged) We examine the power source of 41 local Ultraluminous Infrared
Galaxies using archival infrared and optical photometry. We fit the observed
Spectral Energy Distributions (SEDs) with starburst and AGN components; each
component being drawn from a family of templates. We find all of the sample
require a starburst, whereas only half require an AGN. In 90% of the sample the
starburst provides over half the IR emission, with a mean fractional luminosity
of 82%. When combined with other galaxy samples we find that starburst and AGN
luminosities correlate over 6 decades in IR luminosity suggesting that a common
factor governs both luminosities, plausibly the gas masses in the nuclear
regions. We find that the mid-IR 7.7 micron line-continuum ratio is no
indication of the starburst luminosity, or the fractional AGN luminosity, and
therefore that this ratio is not a reliable diagnostic of the power source in
ULIRGs. We propose that the scatter in the radio-IR correlation in ULIRGs is
due to a skewed starburst IMF and/or relic relativistic electrons from a
previous starburst, rather than contamination from an obscured AGN. We show
that most ULIRGs undergo multiple starbursts during their lifetime, and by
inference that mergers between more than two galaxies may be common amongst
ULIRGs. Our results support the evolutionary model for ULIRGs proposed by
Farrah et al 2001, where they can follow many different evolutionary paths of
starburst and AGN activity in transforming merging spiral galaxies into
elliptical galaxies, but that most do not go through an optical QSO phase. The
lower level of AGN activity in our local sample than in z~1 HLIRGs implies that
the two samples are distinct populations. We postulate that different galaxy
formation processes at high-z are responsible for this difference.Comment: 24 pages, 8 figures. Accepted for publication in MNRA
Modification and Assessment of the Bedside Pediatric Early Warning Score in the Pediatric Allogeneic Hematopoietic Cell Transplant Population
OBJECTIVES:
To determine the validity of the Bedside Pediatric Early Warning Score system in the hematopoietic cell transplant population, and to determine if the addition of weight gain further strengthens the association with need for PICU admission.
DESIGN:
Retrospective cohort study of pediatric allogeneic hematopoietic cell transplant patients from 2009 to 2016. Daily Pediatric Early Warning Score and weights were collected during hospitalization. Logistic regression was used to identify associations between maximum Pediatric Early Warning Score or Pediatric Early Warning Score plus weight gain and the need for PICU intervention. The primary outcome was need for PICU intervention; secondary outcomes included mortality and intubation.
SETTING:
A large quaternary free-standing children's hospital.
PATIENTS:
One-hundred two pediatric allogeneic hematopoietic cell transplant recipients.
INTERVENTIONS:
None.
MEASUREMENTS AND MAIN RESULTS:
Of the 102 hematopoietic cell transplant patients included in the study, 29 were admitted to the PICU. The median peak Pediatric Early Warning Score was 11 (interquartile range, 8-13) in the PICU admission cohort, compared with 4 (interquartile range, 3-5) in the cohort without a PICU admission (p < 0.0001). Pediatric Early Warning Score greater than or equal to 8 had a sensitivity of 76% and a specificity of 90%. The area under the receiver operating characteristics curve was 0.83. There was a high negative predictive value at this Pediatric Early Warning Score of 90%. When Pediatric Early Warning Score greater than or equal to 8 and weight gain greater than or equal to 7% were compared together, the area under the receiver operating characteristic curve increased to 0.88.
CONCLUSIONS:
In this study, a Pediatric Early Warning Score greater than or equal to 8 was associated with PICU admission, having a moderately high sensitivity and high specificity. This study adds to literature supporting Pediatric Early Warning Score monitoring for hematopoietic cell transplant patients. Combining weight gain with Pediatric Early Warning Score improved the discriminative ability of the model to predict the need for critical care, suggesting that incorporation of weight gain into Pediatric Early Warning Score may be beneficial for monitoring of hematopoietic cell transplant patients
Thermal Emission from HII Galaxies: Discovering the Youngest Systems
We studied the radio properties of very young massive regions of star
formation in HII galaxies, with the aim of detecting episodes of recent star
formation in an early phase of evolution where the first supernovae start to
appear. Our sample consists of 31 HII galaxies, characterized by strong
Hydrogen emission lines, for which low resolution VLA 3.5cm and 6cm
observations were obtained. The radio spectral energy distribution has a range
of behaviours; 1) there are galaxies where the SED is characterized by a
synchrotron-type slope, 2) galaxies with a thermal slope, and, 3) galaxies with
possible free-free absorption at long wavelengths. The latter SEDs were found
in a few galaxies and represent a signature of heavily embedded massive star
clusters closely related to the early stages of massive star formation. Based
on the comparison of the star formation rates determined from the recombination
lines and those determined from the radio emission we find that SFR(Ha) is on
average five times higher than SFR(1.4GHz). We confirm this tendency by
comparing the ratio between the observed flux at 20 cm and the expected one,
calculated based on the Ha star formation rates, both for the galaxies in our
sample and for normal ones. This analysis shows that this ratio is a factor of
2 smaller in our galaxies than in normal ones, indicating that they fall below
the FIR/radio correlation. These results suggest that the emission of these
galaxies is dominated by a recent and massive star formation event in which the
first supernovae (SN) just started to explode. We conclude that the systematic
lack of synchrotron emission in those systems with the largest equivalent width
of Hb can only be explained if those are young starbursts of less than 3.5Myr
of age.Comment: Accepted for publication in Ap
Critical behaviour in the nonlinear elastic response of hydrogels
In this paper we study the elastic response of synthetic hydrogels to an
applied shear stress. The hydrogels studied here have previously been shown to
mimic the behaviour of biopolymer networks when they are sufficiently far above
the gel point. We show that near the gel point they exhibit an elastic response
that is consistent with the predicted critical behaviour of networks near or
below the isostatic point of marginal stability. This point separates rigid and
floppy states, distinguished by the presence or absence of finite linear
elastic moduli. Recent theoretical work has also focused on the response of
such networks to finite or large deformations, both near and below the
isostatic point. Despite this interest, experimental evidence for the existence
of criticality in such networks has been lacking. Using computer simulations,
we identify critical signatures in the mechanical response of sub-isostatic
networks as a function of applied shear stress. We also present experimental
evidence consistent with these predictions. Furthermore, our results show the
existence of two distinct critical regimes, one of which arises from the
nonlinear stretch response of semi-flexible polymers.
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