EXTERNALLY HEATED PROTOSTELLAR CORES IN THE OPHIUCHUS STAR-FORMING REGION

被引：14

作者：

Lindberg, Johan E. ^{[1
]}

Charnley, Steven B. ^{[1
]}

Jorgensen, Jes K. ^{[2
,3
]}

Cordiner, Martin A. ^{[1
,4
]}

Bjerkeli, Per ^{[2
,3
,5
]}

机构：

[1] NASA, Goddard Space Flight Ctr, Astrochem Lab, Mail Code 691,8800 Greenbelt Rd, Greenbelt, MD 20771 USA

[2] Univ Copenhagen, Ctr Star & Planet Format, Niels Bohr Inst, Oster Voldgade 5-7, DK-1350 Copenhagen, Denmark

[3] Univ Copenhagen, Nat Hist Museum Denmark, Oster Voldgade 5-7, DK-1350 Copenhagen, Denmark

[4] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA

[5] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden

来源：

ASTROPHYSICAL JOURNAL | 2017年 / 835卷 / 01期

关键词：

astrochemistry; ISM: individual objects (Ophiuchus); ISM: molecules; radiative transfer; stars: formation; LOW-MASS PROTOSTARS; MOLECULAR CLOUDS; DARK CLOUD; COMPARATIVE CHEMISTRY; CORONA AUSTRALIS; SUBMILLIMETER; ENVELOPES; CH3OH; H2CO; DESORPTION;

D O I：

10.3847/1538-4357/835/1/3

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present APEX 218. GHz observations of molecular emission in a complete sample of embedded protostars in the Ophiuchus star-forming region. To study the physical properties of the cores, we calculate H2CO and c-C3H2 rotational temperatures, both of which are good tracers of the kinetic temperature of the molecular gas. We find that the H2CO temperatures range between 16. K and 124. K, with the highest H2CO temperatures toward the hot corino source IRAS. 16293-2422 (69-124 K) and the sources in the.. Oph. A cloud (23-49 K) located close to the luminous Herbig. Be star S1, which externally irradiates the.. Oph. A cores. On the other hand, the c-C3H2 rotational temperature is consistently low (7-17 K) in all sources. Our results indicate that the c-C3H2 emission is primarily tracing more shielded parts of the envelope whereas the H2CO emission (at the angular scale of the APEX beam; 3600 au in Ophiuchus) mainly traces the outer irradiated envelopes, apart from in IRAS. 16293-2422, where the hot corino emission dominates. In some sources, a secondary velocity component is also seen, possibly tracing the molecular outflow.

引用

页数：12

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