An Effelsberg - Green Bank galactic H I absorption line survey. II - Results and interpretation

Details An Effelsberg - Green Bank galactic H I absorption line survey. II - Results and interpretation An Effelsberg - Green Bank galactic H I absorption line survey. II - Results and interpretation

Nov 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...115..223m&link_type=abstract

Astronomy and Astrophysics, vol. 115, no. 2, Nov. 1982, p. 223-241.

Astronomy and Astrophysics

Astrophysics

49

Absorption Spectra, Extragalactic Radio Sources, H Lines, Hydrogen Clouds, Interstellar Matter, Brightness Temperature, Emission Spectra, Interferometry, Mean Square Values, Signal To Noise Ratios, Spectrum Analysis, Tables (Data)

Scientific paper

The results of observations of 21 cm line single dish emission and interferometer absoption spectra of galactic H I gas toward 69 extragalactic radio sources are discussed. The decomposition of the spectra into gaussian components is described. Spin temperatures for the gas range from about 10 to 3000 K, while most of the observed H I features have temperatures in the range of 20-140 K with a median of 86 K. The coldest features are probably associated with small scale, moderate or low central optical depth, and low brightness clouds. The hotter gas is probably located in fairly smoothly distributed transition regions between H I clouds and fully ionized hot intercloud medium. The inverse correlation found between the relative amplitude of the RMS spectra and the optical depth of the fluctuating components, as well as the spectral shape of the RMS spectra in the velocity range of large line brightness, suggest that clouds with large optical depth have significant amounts of molecular hydrogen in their centers. The effects of H I emission on the interferometer data is discussed.

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