Kinematics and Chemistry of the S140/L1204 Molecular Complex

Details Kinematics and Chemistry of the S140/L1204 Molecular Complex Kinematics and Chemistry of the S140/L1204 Molecular Complex

Oct 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995jkas...28..255p&link_type=abstract

Journal of the Korean Astronomical Society, vol. 28, no. 2, p. 255-264

Astronomy and Astrophysics

Astronomy

5

Ism: Clouds, Ism: Hii Regions, Ism: Individual (S140, L1204), Ism: Molecules, Radio Lines: Ism, Stars: Formation

Scientific paper

The HII region S140 and the associated molecular cloud L1204 have been observed with 10 molecular transitions, CO(1-0), 13CO(1-0), C18O(1-0), CS(2-1), HCO+(1-), HCN(1-0), SO(2-1), So2(2-3), OCS(8-7), and HNCO(4-3) with about 50" angular resolutions. More than 7000 spectra were obtained in total. The morphology of this region shows a massive fragment (the S140 core) and the extended envelope to the northeast. Several gas condensations have been identified in the envelope, having masses of about 1e3 Mo and gas number densities of < 1e4/cm3 to 3e5/cm3 in their cores. The column densities of the observed molecular species toward the S140 core appear to be the typical warm clouds' abundances. It seems to be that the S140 core and L1204 have been swept up by an expanding shell called the Cepheus bubble. The large value of Lir(embedded stars)/Mcloud is about 5 Lo/Mo of the S140 core may suggest that the star formation has been stimulated by the HII region, but the shock velocity and the pressure of the region seem to give a hint of the spontaneous star formation by the self gravity.

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