HH 1050: A Bipolar Flow in the Cloud L 988

Movsessian, T. A.; Magakian, T. Yu.

doi:10.1007/s10511-014-9329-6

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“…The total mass of the Cyg OB 7 cloud complex derived from the 13 CO data is ∼ 1 × 10 5 M⊙. Other than NCS, there are a few known star forming sites in the complex corresponding to opaque regions catalogued by Lynds (1962), e.g., LDN 988 (e.g., Herbig & Dahm 2006;Movsessian & Magakian 2014), LDN 1003 (e.g., Aspin et al 2009), and LDN 1004 (Dobashi et al 2014), which are indicated in figure 1. Compared to the Orion A cloud with a similar molecular mass (e.g., Nagahama et al 1998;Nishimura et al 2015;Shimajiriet al 2014Shimajiriet al , 2015, the Cyg OB 7 cloud is much less active in terms of star formation and is more turbulent (e.g., Dobashi et al 1994).…”

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confidence: 99%

Interaction between the Northern Coalsack in the Cygnus OB 7 cloud complex and multiple supernova remnants including HB 21

Dobashi

Shimoikura

Endo

et al. 2018

Publications of the Astronomical Society of Japan

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We report possible interaction between multiple super nova remnants (SNRs) and Northern Coal Sack (NCS) which is a massive clump (∼ 1 × 10 3 M ⊙ ) in the Cyg OB 7 cloud complex and is forming a massive Class 0 object. We performed molecular observations of the 12 CO(J = 1 − 0), 13 CO(J = 1 − 0), and C 18 O(J = 1 − 0) emission lines using the 45m telescope at the Nobeyama Radio Observatory, and we found that there are mainly four velocity components at V LSR ≃ −20, −6, −4, and 10 km s −1 . The −6 and −4 km s −1 components correspond to the systemic velocities of NCS and the Cygnus OB 7 complex, respectively, and the other velocity components originate from distinct smaller clouds. Interestingly, there are apparent correlations and anti-correlations among the spatial distributions of the four components, suggesting that they are physically interacting with one another. On a larger scale, we find that a group of small clouds belonging to the −20 and 10 km s −1 components are located along two different arcs around some SNRs including HB 21 which has been suggested to be interacting with the Cyg OB 7 cloud complex, and we also find that NCS is located right at the interface of the arcs. The small clouds are likely to be the gas swept up by the stellar wind of the massive stars which created the SNRs. We suggest that the small clouds alined along the two arcs recently encountered NCS and the massive star formation in NCS was triggered by the strong interaction with the small clouds.

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