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  The chemical structure of young high-mass star-forming clumps: (II) parsec-scale CO depletion and deuterium fraction of HCO+

Feng, S., Li, D., Caselli, P., Du, F., Lin, Y., Sipilä, O., et al. (2020). The chemical structure of young high-mass star-forming clumps: (II) parsec-scale CO depletion and deuterium fraction of HCO+. The Astrophysical Journal, 901(2): 145. doi:10.3847/1538-4357/abada3.

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Feng, S., Author
Li, D., Author
Caselli, P.1, Author              
Du, F., Author
Lin, Y., Author
Sipilä, O.1, Author              
Beuther, H., Author
Sanhueza, Patricio, Author
Tatematsu, K., Author
Liu, S. Y., Author
Zhang, Q., Author
Wang, Y., Author
Hogge, T., Author
Jimenez-Serra, I., Author
Lu, X., Author
Liu, T., Author
Wang, K., Author
Zhang, Z. Y., Author
Zahorecz, S., Author
Li, G., Author
Liu, H. B., AuthorYuan, J., Author more..
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1Center for Astrochemical Studies at MPE, MPI for Extraterrestrial Physics, Max Planck Society, ou_1950287              

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 Abstract: The physical and chemical properties of cold and dense molecular clouds are key to understanding how stars form. Using the IRAM 30 m and NRO 45 m telescopes, we carried out a Multiwavelength line-Imaging survey of the 70 μm-dArk and bright clOuds (MIAO). At a linear resolution of 0.1–0.5 pc, this work presents a detailed study of parsec-scale CO depletion and HCO+ deuterium (D-) fractionation toward four sources (G11.38+0.81, G15.22–0.43, G14.49–0.13, and G34.74–0.12) included in our full sample. In each source with T < 20 K and n H ~ 104–105 cm−3, we compared pairs of neighboring 70 μm bright and dark clumps and found that (1) the H2 column density and dust temperature of each source show strong spatial anticorrelation; (2) the spatial distribution of CO isotopologue lines and dense gas tracers, such as 1–0 lines of H13CO+ and DCO+, are anticorrelated; (3) the abundance ratio between C18O and DCO+ shows a strong correlation with the source temperature; (4) both the C18O depletion factor and D-fraction of HCO+ show a robust decrease from younger clumps to more evolved clumps by a factor of more than 3; and (5) preliminary chemical modeling indicates that chemical ages of our sources are ~8 × 104 yr, which is comparable to their free-fall timescales and smaller than their contraction timescales, indicating that our sources are likely dynamically and chemically young.

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 Dates: 2020-10-01
 Publication Status: Published online
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 Identifiers: DOI: 10.3847/1538-4357/abada3
Other: LOCALID: 3270384
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Title: The Astrophysical Journal
Source Genre: Journal
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Publ. Info: Bristol; Vienna : IOP Publishing; IAEA
Pages: - Volume / Issue: 901 (2) Sequence Number: 145 Start / End Page: - Identifier: ISSN: 0004-637X
CoNE: https://pure.mpg.de/cone/journals/resource/954922828215_3