How to Identify Pre-Protostellar Cores

Details How to Identify Pre-Protostellar Cores How to Identify Pre-Protostellar Cores

2000-03-01

arxiv.org/abs/astro-ph/0003015v1

Astronomy and Astrophysics

Astrophysics

22 pages, 6 figures, to be published in The Astrophysical Journal

Scientific paper

10.1086/309114

We have observed the HCO+ J=3-2 line toward 17 starless cores selected from the list of Ward-Thompson et al. (1994). Six of these cores have line asymmetries indicative of collapse. The excess of blue-skewed profiles over red-skewed profiles is at least as large as that found in samples of Class 0 and early Class I sources. The observed line profiles have the same narrow linewidths and small peak temperatures predicted for young sources in evolutionary models, but the blue/red ratios, like those of older sources, are higher than models predict. The infall signature also occurs over large scales, suggesting that these cores have overall inward motions. We have divided these starless cores into two groups based on the continuum photometry of Ward-Thompson et al. and our HCO+ data. We find stronger HCO+ emission among the cores detected in the submillimeter and all the blue-skewed line profiles are in this group, supporting the suggestion of Ward-Thompson et al. that these are the pre-protostellar cores.

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