Abstract
Hydroxyl (OH) is expected to be abundant in diffuse interstellar molecular gas because it forms along with H2 under similar conditions and forms within a similar extinction range.
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Document Type
Article
Publication Date
2-16-2018
Digital Object Identifier (DOI)
https://doi.org/10.3847/1538-4365/aaa762
Funding Information
This work is supported by the National Key R&D Program of China 2017YFA0402600 and International Partnership Program of Chinese Academy of Sciences No. 114A11KYSB20160008. D.L. acknowledges support from the "CAS Interdisciplinary Innovation Team" program. J.R.D. is the recipient of an Australian Research Council DECRA Fellowship (project number DE170101086). L.B. acknowledges support from CONICYT Project PFB06.
Related Content
Repository Citation
Li, Di; Tang, Ningyu; Nguyen, Hiep; Dawson, J. R.; Heiles, Carl; Xu, Duo; Pan, Zhichen; Goldsmith, Paul F.; Gibson, Steven J.; Murray, Claire E.; Robishaw, Tim; McClure-Griffiths, N. M.; Dickey, John; Pineda, Jorge; Stanimirović, Snežana; Bronfman, L.; and Troland, Thomas, "Where is OH and Does It Trace the Dark Molecular Gas (DMG)?" (2018). Physics and Astronomy Faculty Publications. 585.
https://uknowledge.uky.edu/physastron_facpub/585
Notes/Citation Information
Published in The Astrophysical Journal Supplement Series, v. 235, no.1, 1, p. 1-15.
© 2018. The American Astronomical Society. All rights reserved.
The copyright holder has granted the permission for posting the article here.
This group of authors is collectively known as The PRIMO Collaboration.