A study of interstellar absorption at high galactic latitudes. I - Highly ionized gas

Details A study of interstellar absorption at high galactic latitudes. I - Highly ionized gas A study of interstellar absorption at high galactic latitudes. I - Highly ionized gas

Sep 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...260..561p&link_type=abstract

Astrophysical Journal, Part 1, vol. 260, Sept. 15, 1982, p. 561-578.

Other

125

Absorption Spectra, Galactic Structure, Interstellar Extinction, Ionized Gases, Iue, Carbon, Early Stars, Extragalactic Radio Sources, H Beta Line, Iron, Magellanic Clouds, Milky Way Galaxy, Nitrogen, Photometry, Silicon, Ubv Spectra

Scientific paper

IUE interstellar absorption line data for C IV, Si IV, N V and Fe II, in a sample of 24 distant, early-type stars at high galactic latitudes, are analyzed with other published results in order to study the distribution and physical conditions of highly ionized gas in the halo of the Galaxy. The C IV and Si IV lines, which are detected in front of approximately two-thirds of the stars observed, are significantly stronger that those observed in the spectra of disk stars of similar spectral types, and their velocities show no correlation with the velocities of the background stars. The observed variation of the column densities of C (3+) and Si (3+) with distance z from the plane is consistent with the suggested existence of a Galactic transition layer between cool gas in the disk and outer halo regions at temperatures greater than those observable with IUE. Attention is drawn to the fact that the observed C (3+)/Si (3+) ratio may be a characteristic signature of hot gas in galactic halos.

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