SMA OBSERVATIONS OF THE HOT CORES OF DR21(OH)

被引：8

作者：

Minh, Y. C. ^{[1
]}

Chen, H. -R. ^{[2
,3
]}

Su, Y. -N. ^{[4
]}

Liu, S. -Y. ^{[4
]}

机构：

[1] Korea Astron & Space Sci Inst, Taejon 305348, South Korea

[2] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan

[3] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan

[4] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan

来源：

JOURNAL OF THE KOREAN ASTRONOMICAL SOCIETY | 2012年 / 45卷 / 06期

关键词：

ISM: abundances; molecules : individual(DR21(OH)); stars: formation; METHANOL MASERS; INTERFEROMETRIC OBSERVATIONS; MOLECULAR CLOUDS; CONTINUUM; DUST; GAS; ENVELOPES; EMISSION; OUTFLOWS; COMPLEX;

D O I：

10.5303/JKAS.2012.45.6.157

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Using the Submillimeter Array (SMA), we identified two bright hot subcores, MM1a and MM1b (size similar to 1 '' and mass similar to 0.5 M-circle dot) separated by about 1.6 '', in the 230 GHz continuum emission toward the massive star-forming region DR21(OH). Both display typical hot core characteristics but have slightly different chemical properties. For example, highly saturated species show stronger emission toward MM1a and seem to be evaporating directly from the grain mantles. In contrast, simple sulfur-bearing species have brighter emission at MM1b. These features indicate that MM1a is at an earlier stage than MM1b, and the small-scale chemical differences between these two cores may result from the age difference of the order of 10(4) years.

引用

页码：157 / 166

页数：10

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