846 research outputs found
Absolute Flux Calibration of the IRAC Instrument on the Spitzer Space Telescope using Hubble Space Telescope Flux Standards
The absolute flux calibration of the James Webb Space Telescope will be based
on a set of stars observed by the Hubble and Spitzer Space Telescopes. In order
to cross-calibrate the two facilities, several A, G, and white dwarf (WD) stars
are observed with both Spitzer and Hubble and are the prototypes for a set of
JWST calibration standards. The flux calibration constants for the four Spitzer
IRAC bands 1-4 are derived from these stars and are 2.3, 1.9, 2.0, and 0.5%
lower than the official cold-mission IRAC calibration of Reach et al. (2005),
i.e. in agreement within their estimated errors of ~2%. The causes of these
differences lie primarily in the IRAC data reduction and secondarily in the
SEDs of our standard stars. The independent IRAC 8 micron band-4 fluxes of
Rieke et al. (2008) are about 1.5 +/- 2% higher than those of Reach et al. and
are also in agreement with our 8 micron result.Comment: 16 pages, 6 figure
Hubble Space Telescope Spectroscopy of the Balmer lines in Sirius B
Sirius B is the nearest and brightest of all white dwarfs, but it is very
difficult to observe at visible wavelengths due to the overwhelming scattered
light contribution from Sirius A. However, from space we can take advantage of
the superb spatial resolution of the Hubble Space Telescope to resolve the A
and B components. Since the closest approach in 1993, the separation between
the two stars has become increasingly favourable and we have recently been able
to obtain a spectrum of the complete Balmer line series for Sirius B using
HST?s Space Telescope Imaging Spectrograph (STIS). The quality of the STIS
spectra greatly exceed that of previous ground-based spectra, and can be used
to provide an important determination of the stellar temperature (Teff =
25193K) and gravity (log g = 8.556). In addition we have obtained a new, more
accurate, gravitational red-shift of 80.42 +/- 4.83 km s-1 for Sirius B.
Combining these results with the photometric data and the Hipparcos parallax we
obtain new determinations of the stellar mass for comparison with the
theoretical mass-radius relation. However, there are some disparities between
the results obtained independently from log g and the gravitational redshift
which may arise from flux losses in the narrow 50x0.2arcsec slit. Combining our
measurements of Teff and log g with the Wood (1995) evolutionary mass-radius
relation we get a best estimate for the white dwarf mass of 0.978 M. Within the
overall uncertainties, this is in agreement with a mass of 1.02 M obtained by
matching our new gravitational red-shift to the theoretical M/R relation.Comment: 11 pages, 6 figures, accepted for publication in the Monthly Notices
of the Royal Astronomical Societ
Faint NUV/FUV Standards from Swift/UVOT, GALEX and SDSS Photometry
At present, the precision of deep ultraviolet photometry is somewhat limited
by the dearth of faint ultraviolet standard stars. In an effort to improve this
situation, we present a uniform catalog of eleven new faint (u sim17)
ultraviolet standard stars. High-precision photometry of these stars has been
taken from the Sloan Digital Sky Survey and Galaxy Evolution Explorer and
combined with new data from the Swift Ultraviolet Optical Telescope to provide
precise photometric measures extending from the Near Infrared to the Far
Ultraviolet. These stars were chosen because they are known to be hot (20,000 <
T_eff < 50,000 K) DA white dwarfs with published Sloan spectra that should be
photometrically stable. This careful selection allows us to compare the
combined photometry and Sloan spectroscopy to models of pure hydrogen
atmospheres to both constrain the underlying properties of the white dwarfs and
test the ability of white dwarf models to predict the photometric measures. We
find that the photometry provides good constraint on white dwarf temperatures,
which demonstrates the ability of Swift/UVOT to investigate the properties of
hot luminous stars. We further find that the models reproduce the photometric
measures in all eleven passbands to within their systematic uncertainties.
Within the limits of our photometry, we find the standard stars to be
photometrically stable. This success indicates that the models can be used to
calibrate additional filters to our standard system, permitting easier
comparison of photometry from heterogeneous sources. The largest source of
uncertainty in the model fitting is the uncertainty in the foreground reddening
curve, a problem that is especially acute in the UV.Comment: Accepted for publication in Astrophysical Journal. 31 pages, 13
figures, electronic tables available from ApJ or on reques
Daytime habitat selection for juvenile parr brown trout (Salmo trutta) in small lowland streams
Physical habitat is important in determining the carrying capacity of juvenile brown
trout, and within freshwater management. Summer daytime physical habitat selection for the
parr lifestage (7â20 cm) juvenile brown trout (Salmo trutta) was assessed
in 6 small lowland streams. Habitat preference was determined for the four variables;
water velocity, water depth, substrate and cover, and the preferences for physical habitat
selection were expressed in terms of habitat suitability indices (HSIâs). The statistical
confidence of HSIâs was evaluated using power analysis. It was found that a minimum of 22
fish observations was needed to have statistical confidence in the HSIs for water depth,
and a minimum of 92 fish observations for water velocity during daytime summer conditions.
Generally parr were utilising the deeper habitats, indicating preference for deeper water.
Cover was also being selected for at all sites, but selection was inconsistent among sites
for the variables substrate and velocity. The results indicate that during daytime summer
conditions water depth is a significant variable for parr habitat selection in these small
lowland streams, with cover also being important. Therefore, daytime refugia may be a
critical limiting factor for parr in small lowland streams, and important for stream
management actions under the Water Framework Directive
Statistical properties of the GALEX spectroscopic stellar sample
The GALEX General Data Release 4/5 includes 174 spectroscopic tiles, obtained
from slitless grism observations, for a total of more than 60,000 ultraviolet
spectra. We have determined statistical properties of the sample of GALEX
stars. We have defined a suitable system of spectroscopic indices, which
measure the main mid-UV features at the GALEX low spectral resolution and we
have employed it to determine the atmospheric parameters of of stars in the
range 4500<Teff<9000 K. Our preliminary results indicate that the sample is
formed by a majority of main sequence F- and G-type stars, with metallicity
[M/H]>-1 dex.Comment: 9 pages, 9 figures, accepted for publication in Astrophysics & Space
Science, UV universe special issu
Convection, Thermal Bifurcation, and the Colors of A stars
Broad-band ultraviolet photometry from the TD-1 satellite and low dispersion
spectra from the short wavelength camera of IUE have been used to investigate a
long-standing proposal of Bohm-Vitense that the normal main sequence A- and
early-F stars may divide into two different temperature sequences: (1) a high
temperature branch (and plateau) comprised of slowly rotating convective stars,
and (2) a low temperature branch populated by rapidly rotating radiative stars.
We find no evidence from either dataset to support such a claim, or to confirm
the existence of an "A-star gap" in the B-V color range 0.22 <= B-V <= 0.28 due
to the sudden onset of convection. We do observe, nonetheless, a large scatter
in the 1800--2000 A colors of the A-F stars, which amounts to ~0.65 mags at a
given B-V color index. The scatter is not caused by interstellar or
circumstellar reddening. A convincing case can also be made against binarity
and intrinsic variability due to pulsations of delta Sct origin. We find no
correlation with established chromospheric and coronal proxies of convection,
and thus no demonstrable link to the possible onset of convection among the A-F
stars. The scatter is not instrumental. Approximately 0.4 mags of the scatter
is shown to arise from individual differences in surface gravity as well as a
moderate spread (factor of ~3) in heavy metal abundance and UV line blanketing.
A dispersion of ~0.25 mags remains, which has no clear and obvious explanation.
The most likely cause, we believe, is a residual imprecision in our correction
for the spread in metal abundances. However, the existing data do not rule out
possible contributions from intrinsic stellar variability or from differential
UV line blanketing effects owing to a dispersion in microturbulent velocity.Comment: 40 pages, 14 figures, 1 table, AAS LaTex, to appear in The
Astrophysical Journa
The HII region G35.673-00.847: another case of triggered star formation?
As part of a systematic study that we are performing with the aim to increase
the observational evidence of triggered star formation in the surroundings of
HII regions, we analyze the ISM around the HII region G35.673-00.847, a poorly
studied source. Using data from large-scale surveys: Two Micron All Sky Survey,
Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSE), MIPSGAL,
Galactic Ring Survey (GRS), VLA Galactic Plane Survey (VGPS), and NRAO VLA Sky
Survey (NVSS) we performed a multiwavelength study of G35.673-00.847 and its
surroundings. The mid IR emission, shows that G35.673-00.847 has an almost
semi-ring like shape with a cut towards the galactic west. The radius of this
semi-ring is about 1.5' (~1.6 pc, at the distance of ~3.7 kpc). The distance
was estimated from an HI absorption study and from the analysis of the
molecular gas. Indeed, we find a molecular shell composed by several clumps
distributed around the HII region, suggesting that its expansion is collecting
the surrounding material. We find several YSO candidates over the molecular
shell. Finally, comparing the HII region dynamical age and the fragmentation
time of the molecular shell, we discard the collect and collapse as the
mechanism responsible for the YSOs formation, suggesting other processes such
as radiative driven implosion and/or small-scale Jeans gravitational
instabilities.Comment: Accepted for publication in A&A, 18 October 2010. Some figures were
degraded to reduce file siz
Induction of viral mimicry upon loss of DHX9 and ADAR1 in breast cancer cells
UNLABELLED: Detection of viral double-stranded RNA (dsRNA) is an important component of innate immunity. However, many endogenous RNAs containing double-stranded regions can be misrecognized and activate innate immunity. The IFN-inducible ADAR1-p150 suppresses dsRNA sensing, an essential function for adenosine deaminase acting on RNA 1 (ADAR1) in many cancers, including breast. Although ADAR1-p150 has been well established in this role, the functions of the constitutively expressed ADAR1-p110 isoform are less understood. We used proximity labeling to identify putative ADAR1-p110-interacting proteins in breast cancer cell lines. Of the proteins identified, the RNA helicase DHX9 was of particular interest. Knockdown of DHX9 in ADAR1-dependent cell lines caused cell death and activation of the dsRNA sensor PKR. In ADAR1-independent cell lines, combined knockdown of DHX9 and ADAR1, but neither alone, caused activation of multiple dsRNA sensing pathways leading to a viral mimicry phenotype. Together, these results reveal an important role for DHX9 in suppressing dsRNA sensing by multiple pathways.
SIGNIFICANCE: These findings implicate DHX9 as a suppressor of dsRNA sensing. In some cell lines, loss of DHX9 alone is sufficient to cause activation of dsRNA sensing pathways, while in other cell lines DHX9 functions redundantly with ADAR1 to suppress pathway activation
Comparing Galaxy Morphology at Ultraviolet and Optical Wavelengths
We have undertaken an imaging survey of 34 nearby galaxies in far-ultraviolet
(FUV, ~1500A) and optical (UBVRI) passbands to characterize galaxy morphology
as a function of wavelength. This sample, which includes a range of classical
Hubble types from elliptical to irregular with emphasis on spirals at low
inclination angle, provides a valuable database for comparison with images of
high-z galaxies whose FUV light is redshifted into the optical and near-
infrared bands. Ultraviolet data are from the UIT Astro-2 mission. We present
images and surface brightness profiles for each galaxy, and we discuss the
wavelength-dependence of morphology for different Hubble types in the context
of understanding high-z objects. In general, the dominance of young stars in
the FUV produces the patchy appearance of a morphological type later than that
inferred from optical images. Prominent rings and circumnuclear star formation
regions are clearly evident in FUV images of spirals, while bulges, bars, and
old, red stellar disks are faint to invisible at these short wavelengths.
However, the magnitude of the change in apparent morphology ranges from
dramatic in early--type spirals with prominent optical bulges to slight in
late-type spirals and irregulars, in which young stars dominate both the UV and
optical emission. Starburst galaxies with centrally concentrated, symmetric
bursts display an apparent ``E/S0'' structure in the FUV, while starbursts
associated with rings or mergers produce a peculiar morphology. We briefly
discuss the inadequacy of the optically-defined Hubble sequence to describe FUV
galaxy images and estimate morphological k-corrections, and we suggest some
directions for future research with this dataset.Comment: Accepted for publication in the ApJS. 15 pages, 17 JPEG figures, 10
GIF figures. Paper and full resolution figures available at
http://nedwww.ipac.caltech.edu/level5/Kuchinski/frames.htm
Synthetic Mid-UV Spectroscopic Indices of Stars
Using the UVBLUE library of synthetic stellar spectra we have computed a set
of mid-UV line and continuum spectroscopic indices. We explore their behavior
in terms of the leading stellar parameters [T_eff,log(g)]. The overall result
is that synthetic indices follow the general trends depicted by those computed
from empirical databases. Separately we also examine the index sensitivity to
changes in chemical composition, an analysis only feasible under a theoretical
approach. In this respect, lines indices FeI3000, BL3096 and MgI2852 and the
continuum index 2828/2921 are the least sensitive features, an important
characteristic to be taken into account for the analyses of integrated spectra
of stellar systems. We also quantify the effects of instrumental resolution on
the indices and find that indices display variations up to 0.1 mag in the
resolution interval between 6-10 angstrom of FWHM. We discuss the extent to
which synthetic indices are compatible with indices measured in spectra
collected by the International Ultraviolet Explorer (IUE). Five line and
continuum indices (FeI3000, 2110/2570, 2828/2921, S2850, and S2850L) display a
remarkable good correlation with observations. The rest of the indices are
either underestimated or overestimated, however, two of them, MgWide and
BL3096, display only marginal discrepancies. For 11 indices we give the
coefficients to convert synthetic indices to the IUE system. This work
represents the first attempt to synthesize mid-UV indices from high resolution
theoretical spectra and foresees important applications for the study of the
ultraviolet morphology of old stellar aggregates.Comment: 20 pages, 6 figures; accepted for publication in The Astrophysical
Journa
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