Astronomy and Astrophysics – Astronomy
Scientific paper
Feb 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apjs..108..489k&link_type=abstract
Astrophysical Journal Supplement v.108, p.489
Astronomy and Astrophysics
Astronomy
17
Ism: H Ii Regions, Ism: Abundances, Ism: Clouds, Ism: Individual Alphanumeric: W51, Radio Lines: Ism
Scientific paper
We have carried out an H I 21 cm absorption line study of the W51 complex, using the VLA and the Arecibo telescope. We present H I 21 cm absorption spectra for the compact sources in G49.5-0.4, G49.4-0.3, and W51B. The spectra show that the absorption features toward the W51 complex divide into two groups, one between vLSR = 0 and vLSR = +35 km s-1 and the other between +35 and +73 km s-1. The former is probably due to the H I gas in the Local arm whereas the latter is probably due to the H I gas in the Sagittarius arm. We have decomposed each absorption spectrum into five to seven Gaussian components. We have found that the absorbing H I column density of the Local arm is similar for all sources, i.e., (3.4--5.0) x 1021 cm-2, whereas for the Sagittarius arm it varies by a factor of 3, i.e., (0.7--2.2) x 1022 cm-2. We discuss individual compact sources based upon the Gaussian parameters of their absorption spectra. For G49.5-0.4, we conclude that it is behind the high-velocity H I stream and that components f + g and components a, b, and e are located on opposite sides of a +62 km s-1 H I cloud. For G49.4-0.3, we conclude that it is likely in front of G49.5-0.4 and that components a and b and components d and f are likely spatially close to each other, respectively.
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