40 research outputs found
Photometric Calibration of the Swift Ultraviolet/Optical Telescope
We present the photometric calibration of the Swift UltraViolet/Optical
Telescope (UVOT) which includes: optimum photometric and background apertures,
effective area curves, colour transformations, conversion factors for count
rates to flux, and the photometric zero points (which are accurate to better
than 4 per cent) for each of the seven UVOT broadband filters. The calibration
was performed with observations of standard stars and standard star fields that
represent a wide range of spectral star types. The calibration results include
the position dependent uniformity, and instrument response over the 1600-8000A
operational range. Because the UVOT is a photon counting instrument, we also
discuss the effect of coincidence loss on the calibration results. We provide
practical guidelines for using the calibration in UVOT data analysis. The
results presented here supersede previous calibration results.Comment: Minor improvements after referees report. Accepted for publication in
MNRA
Paper II: Calibration of the Swift ultraviolet/optical telescope
The Ultraviolet/Optical Telescope (UVOT) is one of three instruments onboard
the Swift observatory. The photometric calibration has been published, and this
paper follows up with details on other aspects of the calibration including a
measurement of the point spread function with an assessment of the orbital
variation and the effect on photometry. A correction for large scale variations
in sensitivity over the field of view is described, as well as a model of the
coincidence loss which is used to assess the coincidence correction in extended
regions. We have provided a correction for the detector distortion and measured
the resulting internal astrometric accuracy of the UVOT, also giving the
absolute accuracy with respect to the International Celestial Reference System.
We have compiled statistics on the background count rates, and discuss the
sources of the background, including instrumental scattered light. In each case
we describe any impact on UVOT measurements, whether any correction is applied
in the standard pipeline data processing or whether further steps are
recommended.Comment: Accepted for publication in MNRAS. 15 pages, 21 figures, 4 table
Prompt optical observations of GRB050319 with the Swift UVOT
The UVOT telescope on the Swift observatory has detected optical afterglow
emission from GRB 050319. The flux declines with a power law slope of alpha =
-0.57 between the start of observations some 230 seconds after the burst onset
(90s after the burst trigger) until it faded below the sensitivity threshold of
the instrument after ~5 x 10^4s. There is no evidence for the rapidly declining
component in the early light curve that is seen at the same time in the X-ray
band. The afterglow is not detected in UVOT shortward of the B-band, suggesting
a redshift of about 3.5. The optical V-band emission lies on the extension of
the X-ray spectrum, with an optical to X-ray slope of beta = -0.8. The
relatively flat decay rate of the burst suggests that the central engine
continues to inject energy into the fireball for as long as a few x 10^4s after
the burst.Comment: 16 pages, 4 figures, accepted by Ap
Swift-UVOT detection of GRB 050318
We present observations of GRB 050318 by the Ultra-Violet and Optical
Telescope (UVOT) on-board the Swift observatory. The data are the first
detections of a Gamma Ray Burst (GRB) afterglow decay by the UVOT instrument,
launched specifically to open a new window on these transient sources. We
showcase UVOTs ability to provide multi-color photometry and the advantages of
combining UVOT data with simultaneous and contemporaneous observations from the
high-energy detectors on the Swift spacecraft. Multiple filters covering
1,800-6,000 Angstroms reveal a red source with spectral slope steeper than the
simultaneous X-ray continuum. Spectral fits indicate that the UVOT colors are
consistent with dust extinction by systems at z = 1.2037 and z = 1.4436,
redshifts where absorption systems have been pre-identified. However, the data
can be most-easily reproduced with models containing a foreground system of
neutral gas redshifted by z = 2.8 +/- 0.3. For both of the above scenarios,
spectral and decay slopes are, for the most part, consistent with fireball
expansion into a uniform medium, provided a cooling break occurs between the
energy ranges of the UVOT and Swifts X-ray instrumentation.Comment: 15 pages, 4 figures, ApJ Letters, in pres
Ultraviolet, Optical, and X-Ray Observations of the Type Ia Supernova 2005am with Swift
We present ultraviolet and optical light curves in six broadband filters and
grism spectra obtained by Swift's Ultraviolet/Optical Telescope for the Type Ia
supernova SN2005am. The data were collected beginning about four days before
the B-band maximum, with excellent coverage of the rapid decline phase and
later observations extending out to 69 days after the peak. The optical and
near UV light curve match well those of SN1992A. The other UV observations
constitute the first set of light curves shorter than 2500 Angstroms and allow
us to compare the light curve evolution in three UV bands. The UV behavior of
this and other low redshift supernovae can be used to constrain theories of
progenitor evolution or to interpret optical light curves of high redshift
supernovae. Using Swift's X-Ray Telescope, we also report the upper limit to
SN2005am's X-ray luminosity to be 1.77 x 10^40 erg s^-1 in the 0.3--10 keV
range from 58,117 s of exposure time.Comment: 15 pages, including 3 figures and 2 tables, submitted to
Astrophysical Journa
Comparative genome analysis of Pseudogymnoascus spp. reveals primarily clonal evolution with small genome fragments exchanged between lineages
Abstract
Background
Pseudogymnoascus spp. is a wide group of fungi lineages in the family Pseudorotiaceae including an aggressive pathogen of bats P. destructans. Although several lineages of P. spp. were shown to produce ascospores in culture, the vast majority of P. spp. demonstrates no evidence of sexual reproduction. P. spp. can tolerate a wide range of different temperatures and salinities and can survive even in permafrost layer. Adaptability of P. spp. to different environments is accompanied by extremely variable morphology and physiology.
Results
We sequenced genotypes of 14 strains of P. spp., 5 of which were extracted from permafrost, 1 from a cryopeg, a layer of unfrozen ground in permafrost, and 8 from temperate surface environments. All sequenced genotypes are haploid. Nucleotide diversity among these genomes is very high, with a typical evolutionary distance at synonymous sites dS ≈ 0.5, suggesting that the last common ancestor of these strains lived >50Mya. The strains extracted from permafrost do not form a separate clade. Instead, each permafrost strain has close relatives from temperate environments.
We observed a strictly clonal population structure with no conflicting topologies for ~99% of genome sequences. However, there is a number of short (~100–10,000 nt) genomic segments with the total length of 67.6 Kb which possess phylogenetic patterns strikingly different from the rest of the genome. The most remarkable case is a MAT-locus, which has 2 distinct alleles interspersed along the whole-genome phylogenetic tree.
Conclusions
Predominantly clonal structure of genome sequences is consistent with the observations that sexual reproduction is rare in P. spp. Small number of regions with noncanonical phylogenies seem to arise due to some recombination events between derived lineages of P. spp., with MAT-locus being transferred on multiple occasions. All sequenced strains have heterothallic configuration of MAT-locus.http://deepblue.lib.umich.edu/bitstream/2027.42/111733/1/12864_2015_Article_1570.pd
Swift panchromatic observations of the bright gamma-ray burst GRB050525a
The bright gamma-ray burst GRB050525a has been detected with the Swift
observatory, providing unique multiwavelength coverage from the very earliest
phases of the burst. The X-ray and optical/UV afterglow decay light curves both
exhibit a steeper slope ~0.15 days after the burst, indicative of a jet break.
This jet break time combined with the total gamma-ray energy of the burst
constrains the opening angle of the jet to be 3.2 degrees. We derive an
empirical `time-lag' redshift from the BAT data of z_hat = 0.69 +/- 0.02, in
good agreement with the spectroscopic redshift of 0.61.
Prior to the jet break, the X-ray data can be modelled by a simple power law
with index alpha = -1.2. However after 300 s the X-ray flux brightens by about
30% compared to the power-law fit. The optical/UV data have a more complex
decay, with evidence of a rapidly falling reverse shock component that
dominates in the first minute or so, giving way to a flatter forward shock
component at later times.
The multiwavelength X-ray/UV/Optical spectrum of the afterglow shows evidence
for migration of the electron cooling frequency through the optical range
within 25000 s. The measured temporal decay and spectral indices in the X-ray
and optical/UV regimes compare favourably with the standard fireball model for
Gamma-ray bursts assuming expansion into a constant density interstellar
medium.Comment: 31 pages, 7 figures, referee comments implemented, typo corrected in
author list, accepted by Ap
Biodiversity of cryopegs in permafrost
Abstract This study describes the biodiversity of the indigenous microbial community in the sodium-chloride water brines (cryopegs) derived from ancient marine sediments and sandwiched within permafrost 100-120,000 years ago after the Arctic Ocean regression. Cryopegs remain liquid at the in situ temperature of À9 to À11°C and make up the only habitat on the Earth that is characterized by permanently subzero temperatures, high salinity, and the absence of external influence during geological time. From these cryopegs, anaerobic and aerobic, spore-less and spore-forming, halotolerant and halophilic, psychrophilic and psychrotrophic bacteria, mycelial fungi and yeast were isolated and their activity was detected below 0°C
Optical, Infrared, and Ultraviolet Observations of the X-Ray Flash GRB 050416A
We present ultraviolet, optical, and infrared photometry of the afterglow of
the X-ray flash XRF 050416A taken between approximately 100 seconds and 36 days
after the burst. We find an intrinsic spectral slope between 1930 and 22,200
Angstrom of beta = -1.14 +/- 0.20 and a decay rate of alpha = -0.86 +/- 0.15.
There is no evidence for a change in the decay rate between approximately 0.7
and 4.7 days after the burst. Our data implies that there is no spectral break
between the optical and X-ray bands between 0.7 and 4.7 days after the burst,
and is consistent with the cooling break being redward of the K_s band (22,200
Angstrom) at 0.7 days. The combined ultraviolet/optical/infrared spectral
energy distribution shows no evidence for a significant amount of extinction in
the host galaxy along the line of sight to XRF 050416A. Our data suggest that
the extragalactic extinction along the line of sight to the burst is only
approximately A_V = 0.2 mag, which is significantly less than the extinction
expected from the hydrogen column density inferred from -ray observations of
XRF 050416A assuming a dust-to-gas ratio similar to what is found for the Milky
Way. The observed extinction, however, is consistent with the dust-to-gas ratio
seen in the Small Magellanic Cloud. We suggest that XRF 050416A may have a
two-component jet similar to what has been proposed for GRB 030329. If this is
the case the lack of an observed jet break between 0.7 and 42 days is an
illusion due to emission from the wide jet dominating the afterglow after
approximately 1.5 days.Comment: 22 pages, 5 figures, LaTeX, AASTeX 5.2 Minor changes made in response
to the referee's repor
Very Early Optical Afterglows of Gamma-Ray Bursts: Evidence for Relative Paucity of Detection
Very early observations with the Swift satellite of gamma-ray burst (GRB)
afterglows reveal that the optical component is not detected in a large number
of cases. This is in contrast to the bright optical flashes previously
discovered in some GRBs (e.g. GRB 990123 and GRB 021211). Comparisons of the
X-ray afterglow flux to the optical afterglow flux and prompt gamma-ray fluence
is used to quantify the seemingly deficient optical, and in some cases X-ray,
light at these early epochs. This comparison reveals that some of these bursts
appear to have higher than normal gamma-ray efficiencies. We discuss possible
mechanisms and their feasibility for explaining the apparent lack of early
optical emission. The mechanisms considered include: foreground extinction,
circumburst absorption, Ly-alpha blanketing and absorption due to high
redshift, low density environments, rapid temporal decay, and intrinsic
weakness of the reverse shock. Of these, foreground extinction, circumburst
absorption, and high redshift provide the best explanations for most of the
non-detections in our sample. There is tentative evidence of suppression of the
strong reverse shock emission. This could be because of a
Poynting-flux-dominated flow or a pure non-relativistic hydrodynamical reverse
shock.Comment: 22 pages, 5 figures. Accepted for publication in Ap