60 research outputs found
Correcting for the Effects of Interstellar Extinction
This paper addresses the issue of how best to correct astronomical data for
the wavelength-dependent effects of Galactic interstellar extinction. The main
general features of extinction from the IR through the UV are reviewed, along
with the nature of observed spatial variations. The enormous range of
extinction properties found in the Galaxy, particularly in the UV spectral
region, is illustrated. Fortunately, there are some tight constraints on the
wavelength dependence of extinction and some general correlations between
extinction curve shape and interstellar environment. These relationships
provide some guidance for correcting data for the effects of extinction.
Several strategies for dereddening are discussed along with estimates of the
uncertainties inherent in each method. In the Appendix, a new derivation of the
wavelength dependence of an average Galactic extinction curve from the IR
through the UV is presented, along with a new estimate of how this extinction
law varies with the parameter R = A(V)/E(B-V). These curves represent the true
monochromatic wavelength dependence of extinction and, as such, are suitable
for dereddening IR--UV spectrophotometric data of any resolution, and can be
used to derive extinction relations for any photometry system.Comment: To appear in PASP (January 1999) 14 pages including 4 pages of
figures Uses emulateapj style. PASP, in press (January 1999
A New Measurement of the Average FUV Extinction Curve
We have measured the extinction curve in the far-ultraviolet wavelength
region of (900 -- 1200 A) using spectra obtained with the Berkeley EUV/FUV
spectrometer during the ORFEUS-I and the ORFEUS-II missions in 1993 and 1996.
From the complete sample of early-type stars observed during these missions,
we have selected pairs of stars with the same spectral type but different
reddenings to measure the differential FUV extinction. We model the effects of
molecular hydrogen absorption and exclude affected regions of the spectrum to
determine the extinction from dust alone. We minimize errors from inaccuracies
in the cataloged spectral types of the stars by making our own determinations
of spectral types based on their IUE spectra. We find substantial scatter in
the curves of individual star pairs and present a detailed examination of the
uncertainties and their effects on each extinction curve. We find that, given
the potentially large uncertainties inherent in using the pair method at FUV
wavelengths, a careful analysis of measurement uncertainties is critical to
assessing the true dust extinction. We present a new measurement of the average
far-ultraviolet extinction curve to the Lyman limit; our new measurement is
consistent with an extrapolation of the standard extinction curve of Savage &
Mathis (1979).Comment: 13 pages text, 7 figures 4 tables. Sent as gzipped tar, with ms.tex
and 7 figure
Ultraviolet Extinction Properties in the Milky Way
We have assembled a homogeneous database of 417 ultraviolet (UV) extinction
curves for reddened sightlines having International Ultraviolet Explorer (IUE)
spectra. We have combined these with optical and 2MASS photometry allowing
estimates of the ratio of total-to-selective extinction, R(V), for the entire
sample. Fitzpatrick-Massa (FM) parameters have also been found for the entire
sample. This is the largest study of parameterized UV extinction curves yet
published and it covers a wide range of environments, from dense molecular
clouds to the diffuse interstellar medium (ISM), with extinctions A(V) ranging
from 0.50 to 4.80. It is the first to extend far beyond the solar neighborhood
and into the Galaxy at large, with 30 sightlines having distances > 5 kpc.
Previously, the longest sightlines with FM parameters and R(V) extended ~ 1
kpc. We find that (1.) the CCM extinction law applies for 93% of the
sightlines, implying that dust processing in the Galaxy is efficient and
systematic; (2.) the central wavelength of the 2175 A bump is constant; (3.)
the 2175 A bump width is dependent on environment. Only four sightlines show
systematic deviations from CCM, HD 29647, 62542, 204827, and 210121. These
sightlines all sample dense, molecule-rich clouds. The new extinction curves
and values of R(V) allow us to revise the CCM law.Comment: 32 pages, 12 figure
The Spectroscopy of Plasma Evolution from Astrophysical Radiation Mission
The Spectroscopy of Plasma Evolution from Astrophysical Radiation (or the
Far-ultraviolet Imaging Spectrograph) instruments, flown aboard the STSAT-1
satellite mission, have provided the first large-area spectral mapping of the
cosmic far ultraviolet (FUV, lambda 900-1750 Ang) background. We observe
diffuse radiation from hot (10^4 to 10^6 K) and ionized plasmas, molecular
hydrogen, and dust scattered starlight. These data provide for the
unprecedented detection and discovery of spectral emission from a variety of
interstellar environments, including the general medium, molecular clouds,
supernova remnants, and super-bubbles. We describe the mission and its data,
present an overview of the diffuse FUV sky's appearance and spectrum, and
introduce the scientific findings detailed later in this volume
Radiative Transfer Analysis of Far-UV Background Observations Obtained with the Far-Ultraviolet Space Telescope (FAUST)
In 1992 the Far-Ultraviolet Space Telescope (FAUST) provided measurements of
the ultraviolet (140-180nm) diffuse sky background at high, medium, and low
Galactic latitudes. A significant fraction of the detected radiation was found
to be of Galactic origin, resulting from scattering by dust in the diffuse
interstellar medium. To simulate the radiative transfer in the Galaxy, we
employed a Monte Carlo model which utilized a realistic, non-isotropic
radiation field based on the measured fluxes (at 156nm) and positions of 58,000
TD-1 stars, and a cloud structure for the interstellar medium. The comparison
of the model predictions with the observations led to a separation of the
Galactic scattered radiation from an approximately constant background,
attributed to airglow and extragalactic radiation, and to a well constrained
determination of the dust scattering properties. The derived dust albedo a =
0.45 +/- 0.05 is substantially lower than albedos derived for dust in dense
reflection nebulae and star-forming regions, while the phase function asymmetry
g = 0.68 +/- 0.10 is indicative of a strongly forward directed phase function.
We show the highly non-isotropic phase function to be responsible, in
conjunction with the non-isotropic UV radiation field, for the wide range of
observed correlations between the diffusely scattered Galactic radiation and
the column densities of neutral atomic hydrogen. The low dust albedo is
attributed to a size distribution of grains in the diffuse medium with average
sizes smaller than those in dense reflection nebulae.Comment: 35 pages, 10 figures included, to be published in the Ap
Ultraviolet Survey of CO and H_2 in Diffuse Molecular Clouds: The Reflection of Two Photochemistry Regimes in Abundance Relationships
(Abridged) We carried out a comprehensive far-ultraviolet (UV) survey of
^12CO and H_2 column densities along diffuse molecular Galactic sight lines in
order to explore in detail the relationship between CO and H_2. We measured new
CO abundances from HST spectra, new H_2 abundances from FUSE data, and new CH,
CH^+, and CN abundances from the McDonald and European Southern Observatories.
A plot of log N(CO) versus log N(H_2) shows that two power-law relationships
are needed for a good fit of the entire sample, with a break located at log
N(CO, cm^-2) = 14.1 and log N(H_2) = 20.4, corresponding to a change in
production route for CO in higher-density gas. Similar logarithmic plots among
all five diatomic molecules allow us to probe their relationships, revealing
additional examples of dual slopes in the cases of CO versus CH (break at log N
= 14.1, 13.0), CH^+ versus H_2 (13.1, 20.3), and CH^+ versus CO (13.2, 14.1).
These breaks are all in excellent agreement with each other, confirming the
break in the CO versus H_2 relationship, as well as the one-to-one
correspondence between CH and H_2 abundances. Our new sight lines were selected
according to detectable amounts of CO in their spectra and they provide
information on both lower-density (< 100 cm^-3) and higher-density diffuse
clouds. The CO versus H_2 correlation and its intrinsic width are shown to be
empirically related to the changing total gas density among the sight lines of
the sample. We employ both analytical and numerical chemical schemes in order
to derive details of the molecular environments. In the low-density gas, where
equilibrium-chemistry studies have failed to reproduce the abundance of CH^+,
our numerical analysis shows that nonequilibrium chemistry must be employed for
correctly predicting the abundances of both CH^+ and CO.Comment: 40 pages in emulateapj style, to appear in the Astrophysical Journa
Spectroscopic survey of Kepler stars. I. HERMES/Mercator observations of A- and F-type stars
The Kepler space mission provided near-continuous and high-precision photometry of about 207 000 stars, which can be used for asteroseismology. However, for successful seismic modeling it is equally important to have accurate stellar physical parameters. Therefore, supplementary ground-based data are needed. We report the results of the analysis of high-resolution spectroscopic data of A- and F-type stars from the Kepler field, which were obtained with the HERMES spectrograph on the Mercator telescope. We determined spectral types, atmospheric parameters and chemical abundances for a sample of 117 stars. Hydrogen Balmer, Feâi, and Feâii lines were used to derive effective temperatures, surface gravities, and microturbulent velocities. We determined chemical abundances and projected rotational velocities using a spectrum synthesis technique. The atmospheric parameters obtained were compared with those from the Kepler Input Catalogue (KIC), confirming that the KIC effective temperatures are underestimated for A stars. Effective temperatures calculated by spectral energy distribution fitting are in good agreement with those determined from the spectral line analysis. The analysed sample comprises stars with approximately solar chemical abundances, as well as chemically peculiar stars of the Am, Ap, and λ Boo types. The distribution of the projected rotational velocity, vsinâi, is typical for A and F stars and ranges from 8 to about 280 km sâ1, with a mean of 134 km sâ1
Effect of manipulation of primary tumour vascularity on metastasis in an adenocarcinoma model
One explanation for the clinical association between tumour vascularity and probability of metastasis is that increased primary tumour vascularity enhances haematogenous dissemination by offering greater opportunity for tumour cell invasion into the circulation (intravasation). We devised an experimental tumour metastasis model that allowed manipulation of primary tumour vascularity with differential exposure of the primary and metastatic tumour site to angiogenic agents. We used this model to assess the effects of local and systemic increases in the level of the angiogenic agent basic fibroblast growth factor on metastasis. BDIX rats with implanted hind limb K12/TR adenocarcinoma tumours received either intratumoural or systemic, basic fibroblast growth factor or saline infusion. Both intratumoural and systemic basic fibroblast growth factor infusion resulted in significant increases in tumour vascularity, blood flow and growth, but not lung metastasis, compared with saline-infused controls. Raised basic fibroblast growth factor levels and increase in primary tumour vascularity did not increase metastasis. The clinical association between tumour vascularity and metastasis is most likely to arise from a metastatic tumour genotype that links increased tumour vascularity with greater metastatic potential
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