Please use this identifier to cite or link to this item: http://hdl.handle.net/10995/103357
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dc.contributor.authorLadeyschikov, D. A.en
dc.contributor.authorUrquhart, J. S.en
dc.contributor.authorSobolev, A. M.en
dc.contributor.authorBreen, S. L.en
dc.contributor.authorBayandina, O. S.en
dc.date.accessioned2021-08-31T15:09:12Z-
dc.date.available2021-08-31T15:09:12Z-
dc.date.issued2020-
dc.identifier.citationThe Physical Parameters of Clumps Associated with Class i Methanol Masers / D. A. Ladeyschikov, J. S. Urquhart, A. M. Sobolev, et al. — DOI 10.3847/1538-3881/abb770 // Astronomical Journal. — 2020. — Vol. 160. — Iss. 5. — 213.en
dc.identifier.issn46256-
dc.identifier.otherFinal2
dc.identifier.otherAll Open Access, Green3
dc.identifier.otherhttps://www.scopus.com/inward/record.uri?eid=2-s2.0-85094966661&doi=10.3847%2f1538-3881%2fabb770&partnerID=40&md5=3edf4a0404fab4d92c6854ca66c86e68
dc.identifier.otherhttp://arxiv.org/pdf/2009.07474m
dc.identifier.urihttp://hdl.handle.net/10995/103357-
dc.description.abstractWe present a study of the association between class I methanol masers and cold dust clumps from the APEX Telescope Large Area Survey of the Galaxy (ATLASGAL) survey. It was found that almost 100% of class I methanol masers are associated with objects listed in the ATLASGAL compact source catalog. We find a statistically significant difference in the flux density, luminosity, number and column density, and temperature distributions of ATLASGAL sources associated with 95/44 GHz methanol masers compared with those ATLASGAL sources devoid of 95 GHz methanol masers. The masers tend to arise in clumps with higher densities, luminosities, and temperatures compared with both the full sample of ATLASGAL clumps, as well as the sample of ATLASGAL sources that were cross-matched with positions previously searched for methanol masers but with no detections. Comparison between the peak position of ATLASGAL clumps and the interferometric positions of the associated class I and II methanol masers reveals that class I masers are generally located at larger physical distances from the peak submillimeter emission than class II masers. We conclude that the tight association between ATLASGAL sources and class I methanol masers may be used as a link toward understanding the conditions of the pumping of these masers and evolutionary stages at which they appear. © 2020. The American Astronomical Society. All rights reserved.en
dc.format.mimetypeapplication/pdfen
dc.language.isoenen
dc.publisherIOP Publishing Ltden
dc.rightsinfo:eu-repo/semantics/openAccessen
dc.sourceAstron. J.2
dc.sourceAstronomical Journalen
dc.titleThe Physical Parameters of Clumps Associated with Class i Methanol Masersen
dc.typeArticleen
dc.typeinfo:eu-repo/semantics/articleen
dc.typeinfo:eu-repo/semantics/publishedVersionen
dc.identifier.doi10.3847/1538-3881/abb770-
dc.identifier.scopus85094966661-
local.contributor.employeeLadeyschikov, D.A., Ural Federal University, 51 Lenin Str., Ekaterinburg, 620051, Russian Federation
local.contributor.employeeUrquhart, J.S., Centre for Astrophysics and Planetary Science, University of Kent, Canterbury, CT2 7NH, United Kingdom
local.contributor.employeeSobolev, A.M., Ural Federal University, 51 Lenin Str., Ekaterinburg, 620051, Russian Federation
local.contributor.employeeBreen, S.L., SKA Organisation, Jodrell Bank ObservatorySK11 9DL, United Kingdom
local.contributor.employeeBayandina, O.S., Joint Institute for VLBI ERIC, Oude Hoogeveensedijk 4, Dwingeloo, 7991 PD, Netherlands
local.issue5-
local.volume160-
local.contributor.departmentUral Federal University, 51 Lenin Str., Ekaterinburg, 620051, Russian Federation
local.contributor.departmentCentre for Astrophysics and Planetary Science, University of Kent, Canterbury, CT2 7NH, United Kingdom
local.contributor.departmentSKA Organisation, Jodrell Bank ObservatorySK11 9DL, United Kingdom
local.contributor.departmentJoint Institute for VLBI ERIC, Oude Hoogeveensedijk 4, Dwingeloo, 7991 PD, Netherlands
local.identifier.pure20134580-
local.identifier.pure940fd7bf-c627-4b2f-afb8-d60574272fffuuid
local.description.order213-
local.identifier.eid2-s2.0-85094966661-
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