The hot class I methanol maser W33Met

Details The hot class I methanol maser W33Met The hot class I methanol maser W33Met

Mar 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999arep...43..157v&link_type=abstract

Astronomy Reports, Volume 43, Issue 3, March 1999, pp.157-166

Astronomy and Astrophysics

Astronomy

3

Scientific paper

Multifrequency observations of W33Met in various methanol transitions show that four types of methanol-emission source coexist: a class I maser with a high gain and narrow spectral features, a class I quasi-maser with a low gain and little spectral narrowing of the lines, a source of thermal emission in class II lines, and a very weak class II maser. The evolutionary statuses of these objects are different: the narrow and very bright class-I maser lines probably belong to a very young condensation-perhaps the youngest protostar ever observed-whereas the thermal lines, class I quasi-maser, and weak class II maser are probably located around older protostars. Estimates of physical parameters based on observations of the maser-condensation lines show that the class I masers are produced in a unique molecular core that is very hot and dense, with T_k ~ 100 K and n = 6 x 10^7 cm^-3.

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