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dc.contributor.authorPillai, T.
dc.contributor.authorCaselli, P.
dc.contributor.authorKauffmann, J.
dc.contributor.authorZhang, Q.
dc.contributor.authorThompson, M. A.
dc.contributor.authorLis, D. C.
dc.date.accessioned2012-08-08T13:00:16Z
dc.date.available2012-08-08T13:00:16Z
dc.date.issued2012-06-01
dc.identifier.citationPillai , T , Caselli , P , Kauffmann , J , Zhang , Q , Thompson , M A & Lis , D C 2012 , ' H2D+ in the High-Mass Star-Forming Region Cygnus X ' , The Astrophysical Journal , vol. 751 , no. 2 , 135 . https://doi.org/10.1088/0004-637X/751/2/135
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 921611
dc.identifier.otherPURE UUID: 8d069e40-2c27-4614-91f0-86a831672c0f
dc.identifier.otherWOS: 000304204600056
dc.identifier.otherScopus: 84861313366
dc.identifier.urihttp://hdl.handle.net/2299/8812
dc.description.abstractH2D+ is a primary ion that dominates the gas-phase chemistry of cold dense gas. Therefore, it is hailed as a unique tool in probing the earliest, prestellar phase of star formation. Observationally, its abundance and distribution is, however, just beginning to be understood in low-mass prestellar and cluster-forming cores. In high-mass star-forming regions, H2D+ has been detected only in two cores, and its spatial distribution remains unknown. Here, we present the first map of the ortho-H2D+ J(k+, k-) = 1(1,0) -> 1(1,1) and N2H+ 4-3 transition in the DR21 filament of Cygnus X with the James Clerk Maxwell Telescope, and N2D+ 3-2 and dust continuum with the Submillimeter Array. We have discovered five very extended (<= 34,000 AU diameter) weak structures in H2D+ in the vicinity of, but distinctly offset from, embedded protostars. More surprisingly, the H2D+ peak is not associated with either a dust continuum or N2D+ peak. We have therefore uncovered extended massive cold dense gas that was undetected with previous molecular line and dust continuum surveys of the region. This work also shows that our picture of the structure of cores is too simplistic for cluster-forming cores and needs to be refined: neither dust continuum with existing capabilities nor emission in tracers like N2D+ can provide a complete census of the total prestellar gas in such regions. Sensitive H2D+ mapping of the entire DR21 filament is likely to discover more of such cold quiescent gas reservoirs in an otherwise active high-mass star-forming region.en
dc.format.extent9
dc.language.isoeng
dc.relation.ispartofThe Astrophysical Journal
dc.rightsOpen
dc.titleH2D+ in the High-Mass Star-Forming Region Cygnus Xen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Accepted Version
dcterms.dateAccepted2012-06-01
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1088/0004-637X/751/2/135
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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