Radio and infrared observations of the H II complex BG 2107 + 49

Details Radio and infrared observations of the H II complex BG 2107 + 49 Radio and infrared observations of the H II complex BG 2107 + 49

Aug 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...235..407v&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 235, no. 1-2, Aug. 1990, p. 407-427. Research supported by ASTRON.

Astronomy and Astrophysics

Astronomy

12

H Ii Regions, Infrared Astronomy Satellite, Infrared Radiation, Interstellar Matter, Radio Sources (Astronomy), Astronomical Spectroscopy, Carbon Monoxide, Emission Spectra, Galactic Structure, Molecular Clouds, Stellar Winds

Scientific paper

The nature of the H II complex BG 107 + 49 is investigated using results of high-resolution radio observations (in the radio continuum at 74 and 21 cm and in the 21-cm H I line) and broad IR maps of BG 2107 + 49, obtained by the IRAS satellite. In addition, H112-alpha spectra were obtained at various positions in the complex. It was found that both the 'head' and the 'tail' components of the complex have a recombination line velocity V(LSR) of -80 km/sec (and are, most likely, physically associated), while the southern continuum feature of the complex is at -64 km/sec. Evidence is presented for a partial shell of H I being associated with the complex, with a systemic velocity of -80 km/sec, an expansion velocity of 24 km/s, and a diameter of 150 pc. It is suggested that this shell, together with the curved ionized tail component of the BG 2107 + 49 complex are part of a swept-up stellar wind shell with a mass of at least 120,000 and an age of 1.9 x 10 to the 6th yrs.

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