Publication:
A molecular line survey of W3(OH) and W3 IRS 5 from 84.7 to 115.6 GHz: Observational data and analyses

dc.contributor.author Kim, Sang-Joon en_US
dc.contributor.author Lee, Youngung en_US
dc.contributor.author Minh, Y en_US
dc.contributor.author Burton, Michael en_US
dc.contributor.author Millar, Tom en_US
dc.contributor.author Lee, Dong-Wook en_US
dc.contributor.author Kim, Hun-Dae en_US
dc.contributor.author Balasubramanyam, Ramesh en_US
dc.date.accessioned 2021-11-25T12:56:15Z
dc.date.available 2021-11-25T12:56:15Z
dc.date.issued 2006 en_US
dc.description.abstract We have carried out observations toward the W3 complex and G34.3+0.15 using the TRAO14 m radio telescope to examine in detail the chemical variations occurring while molecular clouds evolve from the prestellar to the H II region phase. Observations include spectral surveys of these objects between 84.7 and 115.6 GHz; mapping observations toward W3(OH) with the emissions of CS (2-1), HCN (1-0), HNC (1-0), and HCO+ (1-0); and mapping of CS (2-1) emission toward W3 IRS 5. Chemical model calculations are used to estimate the age of W3(OH) by comparing with the fractional abundances of detected molecules. We found that G34.3+0.15 and W3(OH) are at a similar evolutionary stage, although large differences in the fractional abundances are found in CH3CN and HC3N. Overall, the properties of the detected species and abundances in three regions support the view that chemistry varies as molecular clouds evolve from a cold, collapsing phase to a high-temperature phase, such as the hot core and H II phase. Chemical model calculations for W3(OH) indicate that the evolutionary age of the cloud is 10(4)-10(5) yr with temperature in the range 10-60 K. en_US
dc.identifier.issn 0067-0049 en_US
dc.identifier.uri http://hdl.handle.net/1959.4/38598
dc.language English
dc.language.iso EN en_US
dc.rights CC BY-NC-ND 3.0 en_US
dc.rights.uri https://creativecommons.org/licenses/by-nc-nd/3.0/au/ en_US
dc.source Legacy MARC en_US
dc.subject.other HII regions. en_US
dc.subject.other ISM : abundances. en_US
dc.subject.other ISM : individual (W3(OH. en_US
dc.subject.other W3IRS 5. en_US
dc.subject.other G34.3+0.15. en_US
dc.title A molecular line survey of W3(OH) and W3 IRS 5 from 84.7 to 115.6 GHz: Observational data and analyses en_US
dc.type Journal Article en
dcterms.accessRights open access
dspace.entity.type Publication en_US
unsw.accessRights.uri https://purl.org/coar/access_right/c_abf2
unsw.description.notePublic The Astrophysical Journal Supplement Series is published by the University of Chicago Press. en_US
unsw.identifier.doiPublisher http://dx.doi.org/10.1086/491473 en_US
unsw.relation.faculty Science
unsw.relation.ispartofissue 1 en_US
unsw.relation.ispartofjournal Astrophysical Journal Supplement Series en_US
unsw.relation.ispartofpagefrompageto 161-206 en_US
unsw.relation.ispartofvolume 162 en_US
unsw.relation.originalPublicationAffiliation Kim, Sang-Joon en_US
unsw.relation.originalPublicationAffiliation Lee, Youngung en_US
unsw.relation.originalPublicationAffiliation Minh, Y en_US
unsw.relation.originalPublicationAffiliation Burton, Michael, Physics, Faculty of Science, UNSW en_US
unsw.relation.originalPublicationAffiliation Millar, Tom en_US
unsw.relation.originalPublicationAffiliation Lee, Dong-Wook en_US
unsw.relation.originalPublicationAffiliation Kim, Hun-Dae en_US
unsw.relation.originalPublicationAffiliation Balasubramanyam, Ramesh, Physics, Faculty of Science, UNSW en_US
unsw.relation.school School of Physics *
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