1997/10/24 by E. B. Jenkins, T. M. Tripp, Todd M. Tripp +20 · 2 citations
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Galaxy #Gamma-ray bursts and supernovae #Hubble space telescope #Interstellar medium #Physics #Pulsar #Space Telescope Imaging Spectrograph #Spectral line #Spectrograph #Stars #Stellar, planetary, and galactic studies #Supernova #Telescope #Vela #astro-ph
paper · pdf · doi:10.1086/311114
published as Astrophys.J.492:L147-L150,1998 · 11 pages, 2 figures, Latex. Submitted for the special HST ERO issue of the Astrophysical Journal Letters
arxiv created 1997/10/24 · openalex publication_date 1998/01/10 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06
The star HD 72089 is located behind the Vela supernova remnant and shows a complex array of high- and low-velocity interstellar absorption features arising from shocked clouds. A spectrum of this star was recorded over the wavelength range 1196.4-1397.2 Å at a resolving power of λ/Δλ = 110,000 and a signal-to-noise ratio of 32 by the Space Telescope Imaging Spectrograph on the Hubble Space Telescope . We have identified seven narrow components of C I and have measured their relative populations in excited fine-structure levels. Broader features at heliocentric velocities ranging from -70 to 130 km s -1 are seen in C II, N I, O I, Si II, S II, and Ni II. In the high-velocity components, the unusually low abundances of N I and O I, relative to S II and Si II, suggest that these elements may be preferentially ionized to higher stages by radiation from hot gas immediately behind the shock fronts.