scholarly journals Chlorine in the Galactic Interstellar Medium: Revised f -Values with the Far Ultraviolet Spectroscopic Explorer and the Space Telescope Imaging Spectrograph

2006 ◽  
Vol 650 (2) ◽  
pp. L115-L118 ◽  
Author(s):  
P. Sonnentrucker ◽  
S. D. Friedman ◽  
D. G. York
Keyword(s):  
Interstellar Medium ◽  
Space Telescope ◽  
Far Ultraviolet ◽  
Imaging Spectrograph

scholarly journals The Interstellar Abundance of Lead: Experimental Oscillator Strengths for Pb ii λ1203 and λ1433 and New Detections of Pb ii in the Interstellar Medium

2015 ◽  
Vol 11 (A29A) ◽  
Author(s):  
A. M. Ritchey ◽  
N. Heidarian ◽  
R. E. Irving ◽  
S. R. Federman ◽  
D. G. Ellis ◽  
...  
Keyword(s):  
Interstellar Medium ◽  
Hubble Space Telescope ◽  
Oscillator Strengths ◽  
Interstellar Gas ◽  
Lifetime Measurements ◽  
Space Telescope ◽  
Interstellar Grains ◽  
Imaging Spectrograph ◽  
Theoretical Results ◽  
Beam Foil

AbstractWe present the first experimentally determined oscillator strengths for the Pb ii transitions at 1203.6 Å and 1433.9 Å, obtained from lifetime measurements made using beam-foil techniques. We also present new detections of these lines in the interstellar medium from an analysis of archival spectra acquired by the Space Telescope Imaging Spectrograph onboard the Hubble Space Telescope. Our observations of the Pb ii λ1203 line represent the first detection of this transition in interstellar gas. Our experimental f-values for the Pb ii λ1203 and λ1433 transitions are consistent with recent theoretical results, including our own relativistic calculations, but are significantly smaller than previous values based on older calculations. Our new f-value for Pb ii λ1433 (0.321 ± 0.034) yields an increase in the interstellar abundance of Pb of 0.43 dex over estimates based on the f-value listed by Morton. With our revised f-values, and with our new detections of Pb ii λ1203 and λ1433, we find that the depletion of Pb onto interstellar grains is not nearly as severe as previously thought, and is very similar to the depletions seen for elements such as Zn and Sn, which have similar condensation temperatures.

scholarly journals Development of the Far-ultraviolet Imaging Spectrograph on KAISTSAT-4

2001 ◽  
Vol 183 ◽  
pp. 113-114
Author(s):  
Wonyong Han ◽  
Kyoung Wook Min ◽  
Jerry Edelstein ◽  
Uk-Won Nam ◽  
Jong-Ho Seon ◽  
...  
Keyword(s):  
Interstellar Medium ◽  
Emission Line ◽  
Order Of Magnitude ◽  
Far Ultraviolet ◽  
Imaging Spectrograph

AbstractThe Far-ultraviolet IMaging Spectrograph (FIMS) is a small spectrograph optimized for the observations of diffuse hot interstellar medium in far-ultraviolet wavebands (900–1150Å and 1335–1750Å). The instrument is expected to be sensitive to emission line fluxes an order of magnitude fainter than any previous missions. FIMS is currently under development and is scheduled for launch in 2002.

scholarly journals The far-ultraviolet main auroral emission at Jupiter – Part 2: Vertical emission profile

2015 ◽  
Vol 33 (10) ◽  
pp. 1211-1219 ◽  
Author(s):  
B. Bonfond ◽  
J. Gustin ◽  
J.-C. Gérard ◽  
D. Grodent ◽  
A. Radioti ◽  
...  
Keyword(s):  
Hubble Space Telescope ◽  
Total Power ◽  
Space Telescope ◽  
Auroral Emission ◽  
Ultraviolet Range ◽  
Auroral Emissions ◽  
Generation Mechanisms ◽  
Far Ultraviolet ◽  
Advanced Camera For Surveys ◽  
Imaging Spectrograph

Abstract. The aurorae at Jupiter are made up of many different features associated with a variety of generation mechanisms. The main auroral emission, also known as the main oval, is the most prominent of them as it accounts for approximately half of the total power emitted by the aurorae in the ultraviolet range. The energy of the precipitating electrons is a crucial parameter to characterize the processes at play which give rise to these auroral emissions, and the altitude of the emissions directly depends on this energy. Here we make use of far-UV (FUV) images acquired with the Advanced Camera for Surveys on board the Hubble Space Telescope and spectra acquired with the Space Telescope Imaging Spectrograph to measure the vertical profile of the main emissions. The altitude of the brightness peak as seen above the limb is ~ 400 km, which is significantly higher than the 250 km measured in the post-dusk sector by Galileo in the visible domain. However, a detailed analysis of the effect of hydrocarbon absorption, including both simulations and FUV spectral observations, indicates that FUV apparent vertical profiles should be considered with caution, as these observations are not incompatible with an emission peak located at 250 km. The analysis also calls for spectral observations to be carried out with an optimized geometry in order to remove observational ambiguities.

Space Telescope Imaging Spectrograph Survey of Far‐Ultraviolet Coronal Forbidden Lines in Late‐Type Stars

2003 ◽  
Vol 583 (2) ◽  
pp. 963-984 ◽  
Author(s):  
Thomas R. Ayres ◽  
Alexander Brown ◽  
Graham M. Harper ◽  
Rachel A. Osten ◽  
Jeffrey L. Linsky ◽  
...  
Keyword(s):  
Late Type ◽  
Space Telescope ◽  
Far Ultraviolet ◽  
Imaging Spectrograph

scholarly journals White Dwarf Probes of Interstellar Deuterium

2000 ◽  
Vol 198 ◽  
pp. 485-486
Author(s):  
Wayne Landsman
Keyword(s):  
High Resolution ◽  
Interstellar Medium ◽  
White Dwarf ◽  
White Dwarfs ◽  
Accurate Determination ◽  
The Sun ◽  
Local Interstellar Medium ◽  
Space Telescope ◽  
Imaging Spectrograph

We review the advantages of using hot white dwarfs (WDs) as probes of the deuterium abundance in the local interstellar medium. We then discuss advantages of the Space Telescope Imaging Spectrograph (STIS) for such observations, as compared with earlier observations with the Goddard High Resolution Spectrograph (GHRS). The GHRS Ly α profile of the white dwarf HZ 43 is probably modified by the hot ‘hydrogen wall’ surrounding the Sun; but despite this complication, the sightline remains a promising one for an accurate determination of the deuterium abundance in the local interstellar medium.

Far‐Ultraviolet Space Telescope Imaging Spectrograph Spectra of the White Dwarf REJ 1032+532. II. Stellar Spectrum

1999 ◽  
Vol 517 (2) ◽  
pp. 850-858 ◽  
Author(s):  
J. B. Holberg ◽  
M. A. Barstow ◽  
F. C. Bruhweiler ◽  
I. Hubeny ◽  
E. M. Green
Keyword(s):  
White Dwarf ◽  
Stellar Spectrum ◽  
Space Telescope ◽  
Far Ultraviolet ◽  
Imaging Spectrograph

scholarly journals CO-to-H2 Abundance Ratio of the Foreground Gas of the Carina Nebula

2004 ◽  
Vol 217 ◽  
pp. 192-193
Author(s):  
Shinn Jong-Ho ◽  
Seon Kwang-Il ◽  
Lee Dae-Hee ◽  
Min Kyoung-Wook
Keyword(s):  
Absorption Band ◽  
Molecular Cloud ◽  
Hubble Space Telescope ◽  
Abundance Ratio ◽  
Hot Stars ◽  
Space Telescope ◽  
International Ultraviolet Explorer ◽  
Carina Nebula ◽  
Far Ultraviolet ◽  
Imaging Spectrograph

We analyze CO and H2 absorption lines of the foreground molecular cloud in the Carina nebula. We use HST-STIS (Hubble Space Telescope - Space Telescope Imaging Spectrograph) & IUE (International Ultraviolet Explorer) INES data to analyze the A-X (v=0→2) absorption band of CO for several hot stars toward the Carina nebula, while 9 stars of them have FUSE (Far Ultraviolet Spectroscopic Explorer) spectra to analyze the (v=0→4) vibrational band in the Lyman series of H2. The column densities of CO and H2 varies in the vicinity of N(CO) ~ 1013cm−2 and N(H2) ~ 1019cm−2, respectively. The resultant CO-to-H2 abundance ratio is about 10−6. We investigate the variation of the abundance ratio according to the relative position of the target stars to morphology the molecular cloud in the Carina nebula.

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