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  Widespread SiO and CH3OH emission in filamentary infrared dark clouds

Cosentino, G., Jiménez-Serra, I., Henshaw, J. D., Caselli, P., Viti, S., Barnes, A. T., et al. (2018). Widespread SiO and CH3OH emission in filamentary infrared dark clouds. Monthly Notices of the Royal Astronomical Society, 474, 3760-3781.

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Cosentino, G.1, Author
Jiménez-Serra, I.1, Author
Henshaw, J. D.1, Author
Caselli, P.1, Author
Viti, S.1, Author
Barnes, A. T.1, Author
Fontani, F.1, Author
Tan, J. C.1, Author
Pon, A.1, Author
Affiliations:
1Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners, ou_2421692              

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Free keywords: stars: formation ISM: individual objects: G028.37+00.07 ISM: individual objects: G034.43+00.24 ISM: individual objects: G034.77-00.55 ISM: molecules Astrophysics - Astrophysics of Galaxies Astrophysics - Solar and Stellar Astrophysics
 Abstract: Infrared dark clouds (IRDCs) are cold, dense regions of high (optical and infrared) extinction, believed to be the birthplace of high-mass stars and stellar clusters. The physical mechanisms leading to the formation of these IRDCs are not completely understood and it is thus important to study their molecular gas kinematics and chemical content to search for any signature of the IRDCs formation process. Using the 30-m-diameter antenna at the Instituto de Radioastronomía Milimétrica (IRAM), we have obtained emission maps of dense gas tracers (H13CO+ and HN13C) and typical shock tracers (SiO and CH3OH) towards three IRDCs, G028.37+00.07, G034.43+00.24, and G034.77-00.55 (clouds C, F, and G, respectively). We have studied the molecular gas kinematics in these clouds and, consistent with previous works towards other IRDCs, the clouds show complex gas kinematics with several velocity-coherent substructures separated in velocity space by a few km s-1. Correlated with these complex kinematic structures, widespread (parsec-scale) emission of SiO and CH3OH is present in all the three clouds. For clouds C and F, known to be actively forming stars, widespread SiO and CH3OH is likely associated with on-going star formation activity. However, for cloud G, which lacks either 8 or 24 μm sources and 4.5 μm H2 shock-excited emission, the detected widespread SiO and CH3OH emission may have originated in a large-scale shock interaction, although a scenario involving a population of low- mass stars driving molecular outflows cannot be fully ruled out.

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 Dates: 2018
 Publication Status: Issued
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Title: Monthly Notices of the Royal Astronomical Society
Source Genre: Journal
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Pages: - Volume / Issue: 474 Sequence Number: - Start / End Page: 3760 - 3781 Identifier: -