Physical Properties of Molecular Cloud Cores in L1630 and Implications for Star Formation

Details Physical Properties of Molecular Cloud Cores in L1630 and Implications for Star Formation Physical Properties of Molecular Cloud Cores in L1630 and Implications for Star Formation

Oct 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...488..286l&link_type=abstract

Astrophysical Journal v.488, p.286

Astronomy and Astrophysics

Astronomy

57

Ism: Individual Alphanumeric: L1630, Ism: Molecules, Radio Lines: Ism, Stars: Formation

Scientific paper

We present the results of a multitransition, CS study of massive dense cores in the L1630 molecular cloud with spatial resolutions ranging from 11" to 64". The primary goal of this investigation is to determine whether the physical properties of massive cores are related to their star formation efficiency (SFE) and, in particular, their ability to form rich embedded clusters. The spatial and density structure of four massive cores and two low-mass cores in this cloud were examined. Densities for each core were determined through an large velocity gradient analysis. We find that all the massive cores contain regions with densities of at least 105 cm-3. In general, cores with rich embedded clusters, and consequently with high SFE, tend to be larger (i.e., to have larger areas of detectable CS J = 5 --> 4 emission) than those without clusters and low SFE. In addition, the region emitting CS J = 5 --> 4 emission has a lower volume filling factor of gas denser than 105 cm-3 in high SFE cores than in low SFE cores. These differences suggest that regions forming rich embedded clusters have larger amounts of dense gas and that they are more fragmented.

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