Large scale structure of the R Coronae Australis cloud core

Details Large scale structure of the R Coronae Australis cloud core Large scale structure of the R Coronae Australis cloud core

Nov 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...278..569h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 278, no. 2, p. 569-583

Astronomy and Astrophysics

Astrophysics

47

Astronomical Maps, Background Radiation, Brightness Distribution, Carbon Monoxide, Line Spectra, Molecular Clouds, Star Formation, Atmospheric Density, Line Of Sight, Magnetic Fields, Optical Thickness, Signal To Noise Ratios, Spectral Resolution, Telescopes

Scientific paper

We report the results of C(18)O (J = 1 - 0) mapping with the 15-m Swedish-ESO Submillimeter Telescope (SEST) of the nearby R Coronae Australis dark cloud. A region of size 40' x 10', corresponding to 1.6 x 0.4 pc has been mapped with a spatial resolution of 0.03 pc, and a more extended region has been mapped with a coarser grid in order to outline the general distribution of the dense material. We estimate the total gas mass for the high column density region (with N(H2) greater than 1022/sq cm) to be 120 solar mass. The mapped region can be divided roughly into two parts with contrasting properties of the sub-condensations. The northwestern dense gas region, known as 'the R CrA core', consists of several clumps which appear to be breaking up. The R CrA core, with a diameter of 25' and a mass of 54 solar mass, has a central hole and seems to be rotating differentially around its centre of mass, located in the hole. These features have remarkable similarity with the simulation results of Monaghan & Lattanzio (1991) for the collapse of a cooling, rotating sphere. We therefore suggest that the R CrA core is actually a fragmented disk. In the southeastern 'tail' of the cloud, we have found a quiescent dense core, which to our knowledge is not associated with any young stars. This clump is probably the center of a massive H I to H2 conversion region (Llewellyn et al. 1981), and a likely site of future star formation.

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