Interstallar gas in the direction of the Large Magellanic Cloud

Details Interstallar gas in the direction of the Large Magellanic Cloud Interstallar gas in the direction of the Large Magellanic Cloud

Jun 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982esasp.176..431m&link_type=abstract

In ESA 3rd European IUE Conf. p 431-433 (SEE N83-11889 02-88)

Computer Science

3

Interstellar Gas, Line Of Sight, Magellanic Clouds, Ultraviolet Spectra, Abundance, Calcium, Interstellar Extinction, Ion Density (Concentration), Lyman Alpha Radiation, Radial Velocity, Resonance Lines

Scientific paper

All the IUE spectra of HD 38282 were co-added and combined with high resolution optical observations of CaII in order to investigate the distribution of material along the line of sight to the star. Abundances relative to neutral hydrogen imply a zinc underabundance, and an overall metal underabundance of 0.5 dex in the Large Magellanic Cloud (LMC). Reddening in the LMC along this line of sight is 0.1. With an estimated error of 0.2 dex in the HI column density, a lower limit on the LMC component of 2 times 10 to the 21st power atoms/sq cm in the line to HD 38282 is estimated. This yields a lower limit for N(HI)/E(B-V) which is larger by a factor of four than the average galactic value, but is comparable with the value towards the central star of 30 Dor.

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