The JCMT Gould Belt Survey: A First Look at IC 5146
Johnstone, D; Ciccone, S; Kirk, H; et al.Mairs, S; Buckle, J; Berry, DS; Broekhoven-Fiene, H; Currie, MJ; Hatchell, J; Jenness, T; Mottram, JC; Pattle, K; Tisi, S; Francesco, JD; Hogerheijde, MR; Ward-Thompson, D; Bastien, P; Bresnahan, D; Butner, H; Chen, M; Chrysostomou, A; Coudé, S; Davis, CJ; Drabek-Maunder, E; Duarte-Cabral, A; Fich, M; Fiege, J; Friberg, P; Friesen, R; Fuller, GA; Graves, S; Greaves, J; Gregson, J; Holland, W; Joncas, G; Kirk, JM; Knee, LBG; Marsh, K; Matthews, BC; Moriarty-Schieven, G; Mowat, C; Nutter, D; Pineda, JE; Salji, C; Rawlings, J; Richer, J; Robertson, D; Rosolowsky, E; Rumble, D; Sadavoy, S; Thomas, H; Tothill, N; Viti, S; White, GJ; Wouterloot, J; Yates, J; Zhu, M
Date: 14 February 2017
American Astronomical Society / IOP Publishing
We present 450 and 850 μm submillimeter continuum observations of the IC 5146 star-forming region taken as part of the James Clerk Maxwell Telescope Gould Belt Survey. We investigate the location of bright submillimeter (clumped) emission with the larger-scale molecular cloud through comparison with extinction maps, and find that these ...
We present 450 and 850 μm submillimeter continuum observations of the IC 5146 star-forming region taken as part of the James Clerk Maxwell Telescope Gould Belt Survey. We investigate the location of bright submillimeter (clumped) emission with the larger-scale molecular cloud through comparison with extinction maps, and find that these denser structures correlate with higher cloud column density. Ninety-six individual submillimeter clumps are identified using FellWalker, and their physical properties are examined. These clumps are found to be relatively massive, ranging from 0.5 M⊙ to 116 M⊙ with a mean mass of 8 M⊙ and a median mass of 3.7 M⊙ . A stability analysis for the clumps suggests that the majority are (thermally) Jeans stable, with M/Mj < 1. We further compare the locations of known protostars with the observed submillimeter emission, finding that younger protostars, i.e., Class 0 and I sources, are strongly correlated with submillimeter peaks and that the clumps with protostars are among the most Jeans unstable. Finally, we contrast the evolutionary conditions in the two major star-forming regions within IC 5146: the young cluster associated with the Cocoon Nebula and the more distributed star formation associated with the Northern Streamer filaments. The Cocoon Nebula appears to have converted a higher fraction of its mass into dense clumps and protostars, the clumps are more likely to be Jeans unstable, and a larger fraction of these remaining clumps contain embedded protostars. The Northern Streamer, however, has a larger number of clumps in total and a larger fraction of the known protostars are still embedded within these clumps.
Physics and Astronomy
College of Engineering, Mathematics and Physical Sciences
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