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  1. OA@INAF
  2. PRODOTTI RICERCA INAF
  3. 1 CONTRIBUTI IN RIVISTE (Journal articles)
  4. 1.01 Articoli in rivista
Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12386/31375
Title: ATLASGAL - Relationship between dense star forming clumps and interstellar masers
Authors: Billington, S. J.
Urquhart, J. S.
König, C.
Beuther, H.
Breen, S. L.
Menten, K. M.
Campbell-White, J.
Ellingsen, S. P.
Thompson, M. A.
Moore, T. J. T.
Eden, D. J.
Kim, W. -J.
Leurini, Silvia 
Issue Date: 2020
Journal: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 
Number: 499
Issue: 2
First Page: 2744
Abstract: We have used catalogues from several Galactic plane surveys and dedicated observations to investigate the relationship between various maser species and Galactic star forming clumps, as identified by the ATLASGAL survey. The maser transitions of interest are the 6.7 & 12.2 GHz methanol masers, 22.2 GHz water masers, and the masers emitting in the four ground-state hyperfine structure transitions of hydroxyl. We find clump association rates for the water, hydroxyl and methanol masers to be 56, 39 and 82 per cent respectively, within the Galactic longitude range of 60{\deg} > $l$ > -60{\deg}. We investigate the differences in physical parameters between maser associated clumps and the full ATLASGAL sample, and find that clumps coincident with maser emission are more compact with increased densities and luminosities. However, we find the physical conditions within the clumps are similar for the different maser species. A volume density threshold of $n$(H$_{2}$) > 10$^{4.1}$ cm$^{-3}$ for the 6.7 GHz methanol maser found in our previous study is shown to be consistent across for all maser species investigated. We find limits that are required for the production of maser emission to be 500 L$_{\odot}$ and 6 M$_{\odot}$ respectively. The evolutionary phase of maser associated clumps is investigated using the L/M ratio of clumps coincident with maser emission, and these have similar L/M ranges (~10$^{0.2}$ - 10$^{2.7}$ L$_{\odot}$/M$_{\odot}$) regardless of the associated transitions. This implies that the conditions required for the production of maser emission only occur during a relatively narrow period during a star's evolution. Lower limits of the statistical lifetimes for each maser species are derived, ranging from ~0.4 - 2 x 10$^{4}$ yrs and are in good agreement with the "straw man" evolutionary model previously presented.
URI: http://hdl.handle.net/20.500.12386/31375
URL: http://arxiv.org/abs/2009.14608v1
https://academic.oup.com/mnras/article/499/2/2744/5912845?login=true
ISSN: 0035-8711
DOI: 10.1093/mnras/staa2936
Bibcode ADS: 2020MNRAS.499.2744B
Fulltext: open
Appears in Collections:1.01 Articoli in rivista

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sta2936_3.pdfparte 31.24 MBAdobe PDFView/Open
sta2936_4.pdfparte 4198.71 kBAdobe PDFView/Open
2009.14608.pdfpreprint8.4 MBAdobe PDFView/Open
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