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C. M. Oliveira, J. C. Howk, J. W. Kruk, P. Chayer, H. W. Moos (Johns Hopkins University)
We present new high-resolution spectra of the hot DA white dwarf GD 246 obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE) in the wavelength range 905-1187Å. The sightline to this star, located at a distance of ~79pc in the direction l=87.25 and b=-45.11, probes the Local Interstellar Cloud and at least one other nearby HI cloud.
The effective temperature and gravity of this star (Teff ~ 53000K and log(g) ~ 7.85) provide a smooth stellar continuum against which the interstellar lines are cleanly seen. Only a few stellar lines are present (PIV-V, SiIV), and neither molecular hydrogen nor OVI are seen along this line of sight.
Using the new FUSE data in conjunction with archival HST/STIS high-resolution echelle data we determine the column densities of HI, CII*, NI, OI, SiII, PII, SII, ArI, and FeII using both profile fitting and curve of growth methods.
We have determined the neutral hydrogen column density along this sightline by fitting the strong damping wings of interstellar luman alpha, using a newly computed model atmosphere to account for the stellar continuum in the vicinity of this line.
We discuss metal abundances and depletions along this line of sight and compare the OI/HI and NI/HI ratios with those derived by Meyer et al.
This work is based on data obtained for the FUSE Guaranteed Time Team by the NASA-CNES-CSA FUSE mission operated by the Johns Hopkins University. Financial support to U. S. participants has been provided in part by NASA contract NAS5-32985. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS5-26555.
The author(s) of this abstract have provided an email address for comments about the abstract: oliveira@pha.jhu.edu