Abstract
We present BIMA and SCUBA observations of the young cluster associated with BD +40 4124 in the dense molecular gas tracer CS J = 2 → 1 and the continuum dust emission at λ = 3.1 mm and 850 μm. The dense gas and dust in the system are aligned in a long ridge morphology extending ∼0.4 pc with 16 gas clumps of estimated masses ranging from 0.14 to 1.8 M ⊙. A north-south variation in the CS center line velocity can be explained with a two-cloud model. We posit that the BD +40 4124 stellar cluster formed from a cloud-cloud collision. The largest line widths occur near V1318 Cyg S, a massive star affecting its natal environment. In contrast, the dense gas near the other, more evolved, massive stars displays no evidence for disruption; the material must either be processed into the star, dissipate, or relax fairly quickly. The more evolved low-mass protostars are more likely to be found near the massive stars. If the majority of low-mass stars are coeval, the seemingly evolved low-mass protostars are not older: the massive stars have eroded their structures. Finally, at the highest resolution, the λ = 3.1 mm dust emission is resolved into a flattened structure 3100 × 1500 AU with an estimated mass of 3.4 M⊙. The continuum and CS emission are offset by 1.1 from the southern binary source. A simple estimate of the extinction due to the continuum emission structure is AV ∼ 700 mag. From the offset and because the southern source is detected in the optical, the continuum emission is from a previously unknown very young, intermediate-mass, embedded stellar object.
| Original language | English (US) |
|---|---|
| Pages (from-to) | 330-338 |
| Number of pages | 9 |
| Journal | Astrophysical Journal |
| Volume | 642 |
| Issue number | 1 I |
| DOIs | |
| State | Published - May 1 2006 |
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Keywords
- ISM: clouds
- ISM: jets and outflows
- Radio lines: ISM
- Stars: formation
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science
Cite this
Colliding clouds : The star formation trigger of the stellar cluster around BD +40 4124. / Looney, Leslie W.; Wang, Shiya; Hamidouche, Murad; Safier, Pedro N.; Klein, Randolf.
In: Astrophysical Journal, Vol. 642, No. 1 I, 01.05.2006, p. 330-338.Research output: Contribution to journal › Article
}
TY - JOUR
T1 - Colliding clouds
T2 - The star formation trigger of the stellar cluster around BD +40 4124
AU - Looney, Leslie W.
AU - Wang, Shiya
AU - Hamidouche, Murad
AU - Safier, Pedro N.
AU - Klein, Randolf
PY - 2006/5/1
Y1 - 2006/5/1
N2 - We present BIMA and SCUBA observations of the young cluster associated with BD +40 4124 in the dense molecular gas tracer CS J = 2 → 1 and the continuum dust emission at λ = 3.1 mm and 850 μm. The dense gas and dust in the system are aligned in a long ridge morphology extending ∼0.4 pc with 16 gas clumps of estimated masses ranging from 0.14 to 1.8 M ⊙. A north-south variation in the CS center line velocity can be explained with a two-cloud model. We posit that the BD +40 4124 stellar cluster formed from a cloud-cloud collision. The largest line widths occur near V1318 Cyg S, a massive star affecting its natal environment. In contrast, the dense gas near the other, more evolved, massive stars displays no evidence for disruption; the material must either be processed into the star, dissipate, or relax fairly quickly. The more evolved low-mass protostars are more likely to be found near the massive stars. If the majority of low-mass stars are coeval, the seemingly evolved low-mass protostars are not older: the massive stars have eroded their structures. Finally, at the highest resolution, the λ = 3.1 mm dust emission is resolved into a flattened structure 3100 × 1500 AU with an estimated mass of 3.4 M⊙. The continuum and CS emission are offset by 1.1 from the southern binary source. A simple estimate of the extinction due to the continuum emission structure is AV ∼ 700 mag. From the offset and because the southern source is detected in the optical, the continuum emission is from a previously unknown very young, intermediate-mass, embedded stellar object.
AB - We present BIMA and SCUBA observations of the young cluster associated with BD +40 4124 in the dense molecular gas tracer CS J = 2 → 1 and the continuum dust emission at λ = 3.1 mm and 850 μm. The dense gas and dust in the system are aligned in a long ridge morphology extending ∼0.4 pc with 16 gas clumps of estimated masses ranging from 0.14 to 1.8 M ⊙. A north-south variation in the CS center line velocity can be explained with a two-cloud model. We posit that the BD +40 4124 stellar cluster formed from a cloud-cloud collision. The largest line widths occur near V1318 Cyg S, a massive star affecting its natal environment. In contrast, the dense gas near the other, more evolved, massive stars displays no evidence for disruption; the material must either be processed into the star, dissipate, or relax fairly quickly. The more evolved low-mass protostars are more likely to be found near the massive stars. If the majority of low-mass stars are coeval, the seemingly evolved low-mass protostars are not older: the massive stars have eroded their structures. Finally, at the highest resolution, the λ = 3.1 mm dust emission is resolved into a flattened structure 3100 × 1500 AU with an estimated mass of 3.4 M⊙. The continuum and CS emission are offset by 1.1 from the southern binary source. A simple estimate of the extinction due to the continuum emission structure is AV ∼ 700 mag. From the offset and because the southern source is detected in the optical, the continuum emission is from a previously unknown very young, intermediate-mass, embedded stellar object.
KW - ISM: clouds
KW - ISM: jets and outflows
KW - Radio lines: ISM
KW - Stars: formation
UR - http://www.scopus.com/inward/record.url?scp=33745301523&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=33745301523&partnerID=8YFLogxK
U2 - 10.1086/500925
DO - 10.1086/500925
M3 - Article
AN - SCOPUS:33745301523
VL - 642
SP - 330
EP - 338
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1 I
ER -