Maser emission toward the very young massive star GH2O 092.67+03.07 (IRAS 21078+5211)

Details Maser emission toward the very young massive star GH2O 092.67+03.07 (IRAS 21078+5211) Maser emission toward the very young massive star GH2O 092.67+03.07 (IRAS 21078+5211)

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008arep...52..211p&link_type=abstract

Astronomy Reports, Volume 52, Issue 3, pp.211-225

Astronomy and Astrophysics

Astronomy

97.10.Fy, 95.85.Bh, Circumstellar Shells, Clouds, And Expanding Envelopes, Circumstellar Masers, Radio, Microwave

Scientific paper

Results of monitoring of the H2O maser observed toward the infrared source IRAS 21078+5211 in the giant molecular cloud Cygnus OB7 are presented. The observations were carried out on the 22-m radio telescope of the Pushchino Radio Astronomy Observatory (Russia) from April 1992 to March 2006. Five cycles of maser activity at various levels were observed. In the periods of highest activity, the spectrum of the H2O maser emission extended from -43 to 12 km/s. During strong flares, the flux densities in some emission features reached nearly 600 Jy. The protostar has a small peculiar velocity with respect to the CO molecular cloud (˜2 km/s). Based on the character of the radial-velocity variations and the tendency for the linewidth to increase with the flux, it is concluded that the medium is strongly fragmented and that there is a small-scale turbulent outflow of ga in the H2O maser region, which may impede the formation of an HII region. The asymmetric distribution of the maser components in V LSR, the difference in the average linewidths of the central and lateral clusters of components, and the fairly high radial velocities relative to the molecular cloud (especially during periods of the highest maser activity) suggest that the maser spots belong to different clusters and different structures of the source: a disk and bipolar outflow.

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