High resolution observations of the (9,8) ammonia maser line in W51 - IRS2

Details High resolution observations of the (9,8) ammonia maser line in W51 - IRS2 High resolution observations of the (9,8) ammonia maser line in W51 - IRS2

Nov 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...251l...7w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 251, no. 1, Nov. 1991, p. L7-L10. Research supported by Max-Planck-Gesellschaf

Astronomy and Astrophysics

Astrophysics

3

Ammonia, Interstellar Masers, Line Spectra, Molecular Clouds, Spatial Resolution, Star Formation, Electron Transitions, Emission Spectra, H Ii Regions, Very Large Array (Vla)

Scientific paper

The (J,K)=(9,8) masing transition of para-ammonia has been observed toward the star forming region W51 - IRS2 with a spatial resolution of about 200 milli-arc seconds (mas). The maser is located 3 arcsec southwest of the well studied H II region W51D. The maser center is unresolved; an upper limit to the size is 120 mas. This corresponds to a peak brightness temperature of more than 3 x 10 exp 5 K. A previously undetected continuum source, presumably ultra-compact H II region, is found 65 mass SE of the ammonia maser. This region has a peak flux density of 27 mJy, and a size of less that 100 mas. The (9,8) maser arises from energy levels which are about 1000 K above ground. Thus, the molecular region must be warm. The superposition of the line and continuum regions may be more than just chance; the maser region may represent the remnant of the collapse of a cloud which has formed the H II region.

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