Other
Scientific paper
May 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aas...194.3502m&link_type=abstract
American Astronomical Society, 194th AAS Meeting, #35.02; Bulletin of the American Astronomical Society, Vol. 31, p.874
Other
Scientific paper
We carried out an unbiased survey for dense cores toward the Chamaeleon dark cloud complex in the (13) CO and C(18) O (J=1-0) emission with NANTEN 4m millimeter-wave telescope. In this paper, we discuss the star formation activities in the complex in connection with the physical properties of dense cores. Among the three major clouds of the complex, the star formation efficiencies (SFEs) drastically change, i.e., SFEs of Cha I, II, and III are estimated to be 13%, 1%, and 0%, respectively. The SFE of 13% in Cha I is remarkably higher than typical SFE ( ~ a few percent) observed in the other nearby star forming regions (e.g., 2% in Taurus, Mizuno et al. 1995) except for Rho-Oph main cloud whose SFE is estimated to be ~ 20% (e.g., Lada & Wilking, 1984). We identified 23 C(18) O cores, whose typical mass, radius, peak column density, line-width are 22 Msun , 0.22 pc, 9.7 x 10(21) cm(-2) , and 0.82 km s(-1) , respectively. By comparison between the YSO distribution and molecular column density, we revealed that the surface density of CTTSs immediately increases when the column density becomes greater than 10(22) cm(-2) , while that of WTTSs does not show such a trend. It suggests that star formation takes place in the densest parts where the column density is greater than 10(22) cm(-2) and that the link between TTSs and dense gas disappears as the TTSs evolve to the weak-line phase. The average physical properties of the C(18) O cores in Cha I are characterized by (1) high column density, (2) almost virial equilibrium, and (3) high Mcore/Mcloud ratio. The cores in Cha III show the opposite trend, and those in Cha II are in between. Such trends suggest that Cha I is well-evolved or well gravitationally relaxed cloud-core system, which is probably related to the very high star formation activity in the cloud.
Fukui Yasuo
Mizuno Akira
NANTEN Team
Onishi Tatsuo
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