Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...450..201c&link_type=abstract
Astrophysical Journal v.450, p.201
Astronomy and Astrophysics
Astronomy
52
Ism: H Ii Regions, Ism: Individual Name: Gemini Ob1, Infrared: Stars, Ism: Molecules, Stars: Formation
Scientific paper
We have conducted a study of the global star formation activity in the Gem OB1 molecular cloud complex using a combination of molecular line, near-infrared, and far-infrared data. A global survey for CS(J = 2-1) emission yielded 11 cores with masses ≳100 Msun. These cores are typically elongated along arcs and filaments previously found in a large-scale 12CO and 13CO survey. Based on the morphology of the cores, the association of some filaments with optical H II regions, and comparison of the observations with models of expanding H II regions, we suggest that these massive cores have formed primarily in swept-up shells of molecular gas. At least eight, and possibly 10, of the 11 cores are associated with star formation as traced by the distribution of IRAS point sources, and the three cores contained in our near-infrared imaging survey each contain a cluster of stars. The high frequency of star formation associated with the cores suggests that star formation in massive dense cores begins soon after the core is formed and that new cores must be continually formed if star formation is to continue in the Gem OB1 complex. A systematic survey in CS of 58 IRAS sources with far-infrared colors characteristic of young stellar objects indicated that the more luminous IRAS sources tend to be associated with more massive cores. This correlation suggests that more massive cores generally form massive stars, although we cannot determine from these data if this is an environmental or statistical effect. Our near-infrared and CS results suggest that dynamical evolution of the clusters and destruction of the cores are important effects to consider when contrasting the properties of different regions. A qualitative model for the Gem OB1 complex is proposed to explain these observations in which the primary mechanism for the formation of the massive dense cores is through the external compression of the molecular gas. The dense cores will generally form clusters of stars that rapidly disperse after the dense core is dissipated. The continual production of dense cores is provided for by the constant interactions of the molecular gas with energetic phenomena in the immediate environment.
Carpenter John Michael
Schloerb Peter F.
Snell Ronald L.
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