Highly ionized gas in the GUM nebula and elsewhere - A comparison of IUE and Copernicus satellite results

Details Highly ionized gas in the GUM nebula and elsewhere - A comparison of IUE and Copernicus satellite results Highly ionized gas in the GUM nebula and elsewhere - A comparison of IUE and Copernicus satellite results

Sep 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...396..124e&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 396, no. 1, Sept. 1, 1992, p. 124-134.

Astronomy and Astrophysics

Astrophysics

11

Gum Nebula, Interstellar Gas, Interstellar Matter, Ionized Gases, Iue, Oao 3, Absorption Spectra, Line Of Sight, Line Shape, Spectral Line Width

Scientific paper

The data from six high-dispersion IUE echelle spectra are averaged in order to obtain an interstellar absorption line spectrum with an S/N of about 30 and a resolution of about 25 km/s. The interstellar lines of C IV and Si IV are very strong and broad and N V is detected. The profiles for these species and Al III are compared to the Copernicus satellite profiles for O VI. The high ionization lines toward HD 64760 are much stronger and broader than those recorded toward Zeta Pup and Gamma super 2 Vel, the two exciting stars of the Gum nebula. The profiles for Al III and Si IV are similar and considerably narrower than the O VI profile. An origin in photoionized Gum nebula gas is suggested as the most likely explanation for Al III and Si IV. The C IV profile has a high positive velocity wing extending to approximately +80 km/s, which is similar in appearance to the positive velocity portion of the O VI profile. It is inferred that a substantial part of the observed C IV has an origin in the collisionally ionized gas most likely rsponsible for the O VI.

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