Studies of dense cores in regions of massive star formation. VI. Multitransitional CS and CO observations of G 261.64-2.09, G 268.42-0.85, G 270.26+0.83 and G 301.12-0.20

Details Studies of dense cores in regions of massive star formation. VI. Multitransitional CS and CO observations of G 261.64-2.09, G 268.42-0.85, G 270.26+0.83 and G 301.12-0.20 Studies of dense cores in regions of massive star formation. VI. Multitransitional CS and CO observations of G 261.64-2.09, G 268.42-0.85, G 270.26+0.83 and G 301.12-0.20

Aug 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26a...336.1007l&link_type=abstract

Astronomy and Astrophysics, v.336, p.1007-1023 (1998)

Astronomy and Astrophysics

Astrophysics

16

Stars: Formation, Ism: Clouds, Ism: Molecules, Radio Lines: Ism

Scientific paper

We report the results of a multitransitional study of four southern molecular clouds in the CS J=2-1, J=3-2, J=5-4, J=7-6; CO J=1-0, J=3-2; C(34) S J=2-1 and C(18) O J=1-0 lines observed with SEST and CSO telescopes. To analyze the obtained maps we applied a MEM deconvolution technique which improves the resolution= significantly, if the signal-to-noise ratio is sufficiently high. We compare the molecular line maps with available infrared and molecular maser data and for G 268.42-0.85 also with optical DSS image. Two of four cores (G 268.42-0.85 and G 301.12-0.20) show bipolar structure in CS with blue- and red-shifted peaks symmetrically displaced relative the central IR objects. We found that in all observed regions the deconvolved source size decreases sharply with the quantum number of the rotational transition, and the measured FWHP of the CS lines decreases with radius. From optically thin C(18) O J=1-0 lines we estimate the H_2 column densities to be of the order of 10(23) cm(-2) and from C(34) S J=2-1 the fractional abundance of CS as 5*10(-9) .

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