A C 18O Survey of Dense Cloud Cores in Taurus: Core Properties

Details A C 18O Survey of Dense Cloud Cores in Taurus: Core Properties A C 18O Survey of Dense Cloud Cores in Taurus: Core Properties

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...465..815o&link_type=abstract

Astrophysical Journal v.465, p.815

Astronomy and Astrophysics

Astronomy

118

Ism: Clouds, Ism: Individual Name: Taurus Cloud Complex, Ism: Molecules, Ism: Structure, Radio Lines: Ism

Scientific paper

This paper discusses observational results of physical properties of dense cores in the Taurus complex. The observations were carried out in the C18O (J = 1-0) line at a linear resolution of 0.1 pc with the 4 m millimeter radio telescope at Nagoya University. Based on the previous 13CO observations of Mizuno et al. (1995) as a guide map, we obtained 7200 spectra (8 deg2) at a 2' grid spacing, corresponding to more than 90% of the area whose molecular column density is greater than 3.5 x 1021 cm-2. The total molecular mass of the C18O cloud is estimated to be 2900 Msun, which is 43% of the mass of the 13CO cloud. About 97% of the C18O spectra have an optical depth smaller than 0.5, and the C18O emission is optically thin over almost all the region at a size scale down to ˜0.1 pc. The basic structure of the C18O cloud is clumpy. We identified 40 dense cores of n(H2) ˜104 cm-3, whose mass ranges from 1 to 80 Msun. The average physical parameters of the C180 cores are as follows: radius 0.23 pc, line width 0.49 km s-1, column density 6.9 x 1021 cm-2, and mass 23 Msun. The mass spectrum of the cores, dN/dM versus M, is fitted by a power law with an index of -09±02 which is significantly smaller than those of the previous surveys. Most of the cores are spatially elongated; the average aspect ratio is 1.8, and the direction of the major axis of the cores tends to be perpendicular to the typical direction of the optical polarization vectors. An analysis of correlations among the physical quantities of the cores indicates that the line width has a positive correlation with the mass and the column density but not with the size. Most of the cores are roughly gravitationally bound and at least approximately in virial equilibrium.

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