NMA CS J=2--1 Line Observations of IRAS 19550+3248

Details NMA CS J=2--1 Line Observations of IRAS 19550+3248 NMA CS J=2--1 Line Observations of IRAS 19550+3248

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997pasj...49..639l&link_type=abstract

Publications of the Astronomical Society of Japan, v.49, p.639-645.

Astronomy and Astrophysics

Astronomy

1

Ism: Individual (Iras 19550+3248), Ism: Molecules, Radio Lines, Star: Formation

Scientific paper

We have carried out CS J=2--1 line observations of IRAS 19550+3248 using the Nobeyama Millimeter Array. IRAS 19550+3248 is a class-I young-stellar object (YSO) deeply embedded in a small molecular cloud. The CS core associated with IRAS 19550+3248 comprises a compact component and extended, weak, diffuse emission. The size of the whole structure is 0.24 pc times 0.1 pc. The total mass is 4.9 MO and most of the mass resides in the compact component. The deconvolved size of the compact component is 0.07 pc times 0.06 pc. The IR source is located at 0.03 pc southeast of the CS peak position. The CS core associated with IRAS 19550+3248 has a large ( ~2.4 kms) velocity dispersion. Our results indicate that the large velocity dispersion results from small (<0.05 pc) clumps moving supersonically in the beam. Individual clumps have a linewidth of ~ 0.7 kms, but the velocity dispersion among the clumps is large. Using a three-dimensional, non-LTE radiative transfer calculation, we have shown that the observed profile can be explained by a clumpy core with a mass of 3.3-3.9 MO . The virial mass is greater than the mass derived from the total flux by an order of magnitude. The large discrepancy may indicate that the clumps are not gravitationally bound to form the CS core, but are dispersing. We discuss the origin of the dispersal. We also detected weak, high-velocity (HV) CS emission, which is considered to be a dense part of the outflow. We compare its properties with those of the CO outflow previously detected in this region.

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