A search for far-ultraviolet emission from Sirius B

1978 ◽  
Vol 225 ◽  
pp. L67 ◽  
Author(s):  
W. H. Brune ◽  
P. D. Feldman ◽  
G. H. Mount
Keyword(s):  
Ultraviolet Emission ◽  
Far Ultraviolet

High-resolution far ultraviolet emission spectra of electron-excited molecular deuterium

1999 ◽  
Vol 32 (15) ◽  
pp. 3813-3838 ◽  
Author(s):  
H Abgrall ◽  
E Roueff ◽  
Xianming Liu ◽  
D E Shemansky ◽  
G K James
Keyword(s):  
High Resolution ◽  
Emission Spectra ◽  
Ultraviolet Emission ◽  
Far Ultraviolet

High-Resolution Electron-Impact Study of the Far-Ultraviolet Emission Spectrum of Molecular Hydrogen

1995 ◽  
Vol 101 ◽  
pp. 375 ◽  
Author(s):  
Xianming Liu ◽  
Syed M. Ahmed ◽  
Rosalie A. Multari ◽  
Geoffrey K. James ◽  
Joseph M. Ajello
Keyword(s):  
High Resolution ◽  
Emission Spectrum ◽  
Electron Impact ◽  
Molecular Hydrogen ◽  
Impact Study ◽  
Ultraviolet Emission ◽  
Resolution Electron ◽  
Far Ultraviolet

scholarly journals The power spectrum of the Lyman-α Forest at z < 0.5

2019 ◽  
Vol 486 (1) ◽  
pp. 769-782 ◽  
Author(s):  
Vikram Khaire ◽  
Michael Walther ◽  
Joseph F Hennawi ◽  
Jose Oñorbe ◽  
Zarija Lukić ◽  
...  
Keyword(s):  
Power Spectrum ◽  
Intergalactic Medium ◽  
Thermal State ◽  
Hubble Space Telescope ◽  
Companion Paper ◽  
Metal Line ◽  
Ultraviolet Emission ◽  
Line Spread Function ◽  
Quasar Spectra ◽  
Far Ultraviolet

ABSTRACT We present new measurements of the flux power-spectrum P(k) of the z &lt; 0.5 H  i Lyman-α Forest spanning scales $k \sim 0.001\!-\!0.1\, \mathrm{s \, km}^{-1}$. These results were derived from 65 far-ultraviolet quasar spectra (resolution $R \sim 18\, 000$) observed with the Cosmic Origin Spectrograph (COS) on board the Hubble Space Telescope. The analysis required careful masking of all contaminating, coincident absorption from H  i and metal–line transitions of the Galactic interstellar medium and intervening absorbers as well as proper treatment of the complex COS line-spread function. From the P(k) measurements, we estimate the H  i photoionization rate ($\Gamma _{\rm H\,{\small I}}$) in the z &lt; 0.5 intergalactic medium. Our results confirm most of the previous $\Gamma _{\rm H\,{\small I}}$ estimates. We conclude that previous concerns of a photon underproduction crisis are now resolved by demonstrating that the measured $\Gamma _{\rm H\,{\small I}}$ can be accounted for by ultraviolet emission from quasars alone. In a companion paper, we will present constraints on the thermal state of the z &lt; 0.5 intergalactic medium from the P(k) measurements presented here.

scholarly journals Far-ultraviolet Emission from Supernova Remnant Shocks

2000 ◽  
Vol 195 ◽  
pp. 425-426
Author(s):  
R. Sankrit ◽  
W. P. Blair ◽  
Fuse Snr Team
Keyword(s):  
Supernova Remnants ◽  
Supernova Remnant ◽  
Ultraviolet Emission ◽  
Far Ultraviolet ◽  
Rich Spectrum

Supernova remnant shocks produce a rich spectrum of lines in the ultraviolet. Among these are important diagnostic resonance lines of O VI, C III, and N III which lie in the bandpass observable with the recently launched Far Ultraviolet Spectroscopic Explorer. We present an overview of a PI program to observe several supernova remnants using this new telescope.

A Search for Far-Ultraviolet Emission Lines from Diffuse Hot Gas in the Halo of NGC 4631

1995 ◽  
Vol 454 (1) ◽  
Author(s):  
Henry C. Ferguson ◽  
W. Van Dyke Dixon ◽  
Arthur F. Davidsen ◽  
Ralf-Juergen Dettmar
Keyword(s):  
Emission Lines ◽  
Ultraviolet Emission ◽  
Hot Gas ◽  
Far Ultraviolet

Catching Some Sun: Probing the Solar Wind with Cometary X-Ray and Far-Ultraviolet Emission

2004 ◽  
Vol 606 (1) ◽  
pp. L81-L84 ◽  
Author(s):  
D. Bodewits ◽  
Z. Juhsz ◽  
R. Hoekstra ◽  
A. G. G. M. Tielens
Keyword(s):  
Solar Wind ◽  
Ultraviolet Emission ◽  
X Ray ◽  
Far Ultraviolet

PROBING THE SOLAR WIND WITH COMETARY X-RAY AND FAR-ULTRAVIOLET EMISSION

2006 ◽  
Author(s):  
R. HOEKSTRA ◽  
D. BODEWITS ◽  
R. MORGENSTERN ◽  
C. M. LISSE ◽  
A. G. G. M. TIELENS
Keyword(s):  
Solar Wind ◽  
Ultraviolet Emission ◽  
X Ray ◽  
Far Ultraviolet
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