The Clump Spectrum of Two High-Latitude Molecular Clouds

Details The Clump Spectrum of Two High-Latitude Molecular Clouds The Clump Spectrum of Two High-Latitude Molecular Clouds

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aas...184.3004b&link_type=abstract

American Astronomical Society, 184th AAS Meeting, #30.04; Bulletin of the American Astronomical Society, Vol. 26, p.905

Astronomy and Astrophysics

Astronomy

Scientific paper

We have applied the clump-finding program of Williams et. al. (1994) to two high galactic latitude molecular clouds. The data consist of large-scale, well-sampled (13) CO(1-0) and CO(1-0) maps of the high-latitude clouds MBM12 (=L1457) and MBM41-44 (Draco Nebula), and have about 500,000 pixels each. This is the first application of the clump-finder to HLCs as well as to large datasets. In each cloud, we find more than 200 clumps ranging from a few hundredths of a solar mass to a few solar masses. We derive the total mass of MBM12 to be 150 M_&sun; and of MBM41-44 to be 140 M_&sun;. In both clouds, the high sensitivity of the maps allow determination of the mass spectrum including substellar mass clumps (M < 0.08 M_&sun;). We find that the clump mass spectrum in MBM41-44 has power-law index alpha =1.40 +/- 0.06, similar to that found for giant molecular clouds. MBM12, however, has a shallower spectrum, alpha =1.07 +/- 0.05. (The quoted errors are statistical uncertainties.) It is surprising that the clump mass spectrum for MBM41-41, a cloud complex far from being gravitationally bound, has the same mass spectrum as the Rosette complex, a well-studied giant molecular cloud. We compare the derived HLC quantities to the results of Williams etal for the Rosette molecular cloud. We find that the HLCS have a significantly steeper size-linewidth relation than the Rosette (Delta V ~ R(0.7) for HLCs; Delta V ~ R(0.4) for the Rosette). We describe a method to determine the internal clump density profile for pressure-bound clumps from the size-linewidth relation. In principle, this method will work even for unresolved clumps. Finally, we report the discovery of a new cloud in the Draco Nebula ``chain.''

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