Large-scale 13CO J=5→4 and [C I] mapping Of Orion A

被引:38
作者
Plume, R
Bensch, F
Howe, JE
Ashby, MLN
Bergin, EA
Chin, G
Erickson, NR
Goldsmith, PF
Harwit, M
Kleiner, S
Koch, DG
Neufeld, DA
Patten, BM
Schieder, R
Snell, RL
Stauffer, JR
Tolls, V
Wang, Z
Winnewisser, G
Zhang, YF
Reynolds, K
Joyce, R
Tavoletti, C
Jack, G
Rodkey, CJ
Melnick, GJ
机构
[1] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
[2] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany
[3] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA
[4] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
[5] Cornell Univ, Dept Astron, Natl Astron & Ionosphere Ctr, Ithaca, NY 14853 USA
[6] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA
[7] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA
[8] Keystone Oaks Planetarium, Pittsburgh, PA 15216 USA
基金
美国国家科学基金会; 美国国家航空航天局;
关键词
ISM : abundances; ISM : clouds; ISM : individual (Orion); ISM : molecules; stars : formation;
D O I
10.1086/312847
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present maps of the (CO)-C-13 J = 5 --> 4 (551 GHz) and [C I] P-3(1) --> P-3(0) (492 GHz) emission in the Orion A molecular cloud, covering a 0 degrees.5 x 2 degrees area. A large velocity gradient (LVG) analysis of (CO)-C-13 J = 5 --> 4 and J = 1 --> 0 suggests that the gas temperatures in the northern part of OMC-1. (north of Delta delta = -20') are similar to 45 K and are, on average, at least 20 K higher than those to the south. The average (CO)-C-13 column density is log (N/cm(-2)) = 16.4 +/- 0.3 and is fairly constant throughout the cloud, even in the low-temperature region south of BN/KL. LVG modeling of the [C I] emission shows a typical C-0 column density of 2 x 10(17) cm(-2), which yields a C/CO abundance ratio in the cloud of similar to 0.1 (rising to levels in excess of 0.5 at the cloud edges). Comparison of the Delta-variance (which measures spatial structure in a manner similar to a power spectrum) of the Submillimeter Wave Astronomy Satellite [C I], Five College Radio Astronomy Observatory (CO)-C-13 J = 1 --> 0, and CS J = 1 --> 0 velocity-integrated maps suggests that the [C I] and (CO)-C-13 emission arise from the same gas. In contrast, the CS emission likely originates in gas that is considerably more clumpy.
引用
收藏
页码:L133 / L136
页数:4
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