Astronomy and Astrophysics – Astronomy
Scientific paper
May 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aas...194.7116s&link_type=abstract
American Astronomical Society, 194th AAS Meeting, #71.16; Bulletin of the American Astronomical Society, Vol. 31, p.945
Astronomy and Astrophysics
Astronomy
Scientific paper
We present STIS echelle observations of interstellar D i and H i Lyα and N i (1199.5, 1200.2 and 1200.7 Angstroms), C ii 1334.5 Angstroms, C(*) ii 1335.7 Angstroms, O i 1302 Angstroms, Si ii (1190, 1193, 1260, 1304 and 1526 Angstroms), Si iii 1206.5 Angstroms, Al ii 1670.8 Angstroms, S ii 1259.5 Angstroms and Fe ii 1608.5 Angstroms in the line of sight to the nearby (69 pc) hot, white dwarf (WD) G191-B2B. Compared to the GHRS study of G191-B2B by Vidal-Madjar et al. 1998 (VM98), the STIS E140H spectra have a higher velocity resolution (3 km s(-1) ), better S/N (between 20 to 50) and broader wavelength coverage (1150 to 1700 Angstroms). We use the Barstow & Hubeny stratified non-LTE model atmosphere calculations which include the effects of line-blanketing from more than 9x10(6) atomic transitions (mainly Ni and Fe), both to determine the NLTE shape of the stellar Lyalpha profile and to estimate the contamination of the interstellar lines by WD photospheric lines. The interstellar N i 1200.7 Angstroms, Si ii 1193 & 1304 Angstroms and Fe ii lines show no contamination by WD photospheric lines and are given more weight in our analysis. VM98 reported three components while we detect only two velocity components in all the interstellar species observed: one at ~ 8.5 km s(-1) and one at ~ 19.3 km s(-1) which we identify as the LIC component. Using the NLTE stellar Lyα profile and a total column density of N(H i) ~ 2 x 10(18) cm(-2) for both components (consistent with EUVE observations), we derive confidence contours. We find the D/H ratio with 2sigma confidence limits to lie within 1.77+/-0.2x10(-5) . This value is consistent with the value of (D/H)LIC = 1.6+/-0.1x10(-5) determined towards Capella (Linsky et al. 1995). The STIS data provide no evidence for local or cloud-to-cloud variation in the D/H ratio as suggested by VM98. Re-analysis of the GHRS data and comparison to the STIS data is in progress.
Barstow Martin Adrian
Bowers C. A.
Bruhweiler Fred C.
Feggans Keith
Gull Ted R.
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