Radio continuum, ammonia, and water maser observations of bright, unassociated IRAS point sources

Details Radio continuum, ammonia, and water maser observations of bright, unassociated IRAS point sources Radio continuum, ammonia, and water maser observations of bright, unassociated IRAS point sources

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apjs...92..173p&link_type=abstract

The Astrophysical Journal Supplement Series, vol. 92, no. 1, p. 173-188

Astronomy and Astrophysics

Astronomy

50

Ammonia, Astronomical Maps, Far Infrared Radiation, H Ii Regions, Interstellar Masers, Mapping, Radio Astronomy, Radio Spectra, Star Formation, Water Masers, Continuous Spectra, Infrared Astronomy Satellite, Point Sources, Radio Telescopes, Very Large Array (Vla)

Scientific paper

We present matching-beam 6 and 2 cm radio continuum observations made with the Very Large Array, and ammonia and water maser observations made at the Haystack Observatory of 12 Infrared Astronomical Satellite (IRAS) point sources selected from the survey of Scalise, Rodriguez, & Mendoza-Torres (1989) of bright, unassociated IRAS point sources. These sources have 60 or 100 micrometer flux densities in excess of 103 Jy and have no previous reference in any of the 37 catalogs considered for association of IRAS sources with known sources. Six of the 12 sources have associated radio continuum, ammonia, and water maser emission, and all of them show at least one of these three emissions. In all sources detected, the ammonia is warm (T approximately 20 K) and suggests the association of dense molecular gas with embedded heating sources. It is argued that all sources in the sample could be associated with time-variable H2O maser emission. The radio and far-infrared data appear to indicate that these sources are star-forming regions, powered by a late O or early B-type star. Several of the sources of lower luminosity (approximately 5 x 103 solar luminosity) appear to have ionizing photon fluxes in excess of those expected for a zero-age main-sequence star. Possible explanations for this discrepancy are discussed.

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