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Article: A spectral line survey of Orion KL in the bands 486-492 and 541-577 GHz with the Odin satellite: I. The observational data

TitleA spectral line survey of Orion KL in the bands 486-492 and 541-577 GHz with the Odin satellite: I. The observational data
Authors
KeywordsISM: individual: objects: Orion KL
ISM: lines and bands
ISM: molecules
Line: identification
Submillimeter
Surveys
Issue Date2007
PublisherEDP Sciences. The Journal's web site is located at http://www.aanda.org
Citation
Astronomy And Astrophysics, 2007, v. 476 n. 2, p. 791-806 How to Cite?
AbstractAims.Spectral line surveys are useful since they allow identification of new molecules and new lines in uniformly calibrated data sets. The subsequent multi-transition analysis will provide improved knowledge of molecular abundances, cloud temperatures and densities, and may also reveal previously unsuspected blends of molecular lines, which otherwise may lead to erroneous conclusions. Nonetheless, large portions of the sub-millimetre spectral regime remain unexplored due to severe absorptions by H 2O and O 2 in the terrestrial atmosphere. The purpose of the measurements presented here is to cover wavelength regions at and around 0.55 mm - regions largely unobservable from the ground.Methods.Using the Odin astronomy/aeronomy satellite, we performed the first spectral survey of the Orion KL molecular cloud core in the bands 486-492 and 541-576 GHz with rather uniform sensitivity (22-25 mK baseline noise). Odin's 1.1 m size telescope, equipped with four cryo-cooled tuneable mixers connected to broad band spectrometers, was used in a satellite position-switching mode. Two mixers simultaneously observed different 1.1 GHz bands using frequency steps of 0.5 GHz (25 h each). An on-source integration time of 20 h was achieved for most bands. The entire campaign consumed ~1100 orbits, each containing one hour of serviceable astro-observation.Results.We identified 280 spectral lines from 38 known interstellar molecules (including isotopologues) having intensities in the range 80 to 0.05 K. An additional 64 weak lines remain unidentified. Apart from the ground state rotational 1-1 transitions of ortho-HO, HO and HO, the high energy 6-7 line of para-HO (K) and the HDO(2-1) line have been observed, as well as the 1 0-0 1 lines from NH and its rare isotopologue NH. We suggest assignments for some unidentified features, notably the new interstellar molecules ND and SH. Severe blends have been detected in the line wings of the HO, HO and CO lines changing the true linewidths of the outflow emission. © 2007 ESO.
Persistent Identifierhttp://hdl.handle.net/10722/80601
ISSN
2014 Impact Factor: 4.378
2015 SCImago Journal Rankings: 2.446
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorOlofsson, AOHen_HK
dc.contributor.authorPersson, CMen_HK
dc.contributor.authorKoning, Nen_HK
dc.contributor.authorBergman, Pen_HK
dc.contributor.authorBernath, PFen_HK
dc.contributor.authorBlack, JHen_HK
dc.contributor.authorFrisk, Uen_HK
dc.contributor.authorGeppert, Wen_HK
dc.contributor.authorHasegawa, TIen_HK
dc.contributor.authorHjalmarson, Åen_HK
dc.contributor.authorKwok, Sen_HK
dc.contributor.authorLarsson, Ben_HK
dc.contributor.authorLecacheux, Aen_HK
dc.contributor.authorNummelin, Aen_HK
dc.contributor.authorOlberg, Men_HK
dc.contributor.authorSandqvist, Aaen_HK
dc.contributor.authorWirström, ESen_HK
dc.date.accessioned2010-09-06T08:08:15Z-
dc.date.available2010-09-06T08:08:15Z-
dc.date.issued2007en_HK
dc.identifier.citationAstronomy And Astrophysics, 2007, v. 476 n. 2, p. 791-806en_HK
dc.identifier.issn0004-6361en_HK
dc.identifier.urihttp://hdl.handle.net/10722/80601-
dc.description.abstractAims.Spectral line surveys are useful since they allow identification of new molecules and new lines in uniformly calibrated data sets. The subsequent multi-transition analysis will provide improved knowledge of molecular abundances, cloud temperatures and densities, and may also reveal previously unsuspected blends of molecular lines, which otherwise may lead to erroneous conclusions. Nonetheless, large portions of the sub-millimetre spectral regime remain unexplored due to severe absorptions by H 2O and O 2 in the terrestrial atmosphere. The purpose of the measurements presented here is to cover wavelength regions at and around 0.55 mm - regions largely unobservable from the ground.Methods.Using the Odin astronomy/aeronomy satellite, we performed the first spectral survey of the Orion KL molecular cloud core in the bands 486-492 and 541-576 GHz with rather uniform sensitivity (22-25 mK baseline noise). Odin's 1.1 m size telescope, equipped with four cryo-cooled tuneable mixers connected to broad band spectrometers, was used in a satellite position-switching mode. Two mixers simultaneously observed different 1.1 GHz bands using frequency steps of 0.5 GHz (25 h each). An on-source integration time of 20 h was achieved for most bands. The entire campaign consumed ~1100 orbits, each containing one hour of serviceable astro-observation.Results.We identified 280 spectral lines from 38 known interstellar molecules (including isotopologues) having intensities in the range 80 to 0.05 K. An additional 64 weak lines remain unidentified. Apart from the ground state rotational 1-1 transitions of ortho-HO, HO and HO, the high energy 6-7 line of para-HO (K) and the HDO(2-1) line have been observed, as well as the 1 0-0 1 lines from NH and its rare isotopologue NH. We suggest assignments for some unidentified features, notably the new interstellar molecules ND and SH. Severe blends have been detected in the line wings of the HO, HO and CO lines changing the true linewidths of the outflow emission. © 2007 ESO.en_HK
dc.languageengen_HK
dc.publisherEDP Sciences. The Journal's web site is located at http://www.aanda.orgen_HK
dc.relation.ispartofAstronomy and Astrophysicsen_HK
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License The original publication is available at [http://www.aanda.org/]-
dc.subjectISM: individual: objects: Orion KLen_HK
dc.subjectISM: lines and bandsen_HK
dc.subjectISM: moleculesen_HK
dc.subjectLine: identificationen_HK
dc.subjectSubmillimeteren_HK
dc.subjectSurveysen_HK
dc.titleA spectral line survey of Orion KL in the bands 486-492 and 541-577 GHz with the Odin satellite: I. The observational dataen_HK
dc.typeArticleen_HK
dc.identifier.openurlhttp://library.hku.hk:4550/resserv?sid=HKU:IR&issn=0004-6361&volume=476&spage=791&epage=806&date=2007&atitle=A+Spectral+Line+Survey+of+Orion+Kl+in+the+Bands+486-492+and+541-577+Ghz+with+the+Odin+Satellite.+I.+The+Observational+Dataen_HK
dc.identifier.emailKwok, S: deannote@hku.hken_HK
dc.identifier.authorityKwok, S=rp00716en_HK
dc.description.naturepublished_or_final_version-
dc.identifier.doi10.1051/0004-6361:20077229en_HK
dc.identifier.scopuseid_2-s2.0-38049170707en_HK
dc.identifier.hkuros146049en_HK
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-38049170707&selection=ref&src=s&origin=recordpageen_HK
dc.identifier.volume476en_HK
dc.identifier.issue2en_HK
dc.identifier.spage791en_HK
dc.identifier.epage806en_HK
dc.identifier.isiWOS:000251285000015-
dc.publisher.placeFranceen_HK
dc.identifier.scopusauthoridOlofsson, AOH=7006322972en_HK
dc.identifier.scopusauthoridPersson, CM=36114949200en_HK
dc.identifier.scopusauthoridKoning, N=15520613500en_HK
dc.identifier.scopusauthoridBergman, P=7006615192en_HK
dc.identifier.scopusauthoridBernath, PF=35372923700en_HK
dc.identifier.scopusauthoridBlack, JH=25222377400en_HK
dc.identifier.scopusauthoridFrisk, U=8966521600en_HK
dc.identifier.scopusauthoridGeppert, W=7004178089en_HK
dc.identifier.scopusauthoridHasegawa, TI=7404173711en_HK
dc.identifier.scopusauthoridHjalmarson, Å=15744175200en_HK
dc.identifier.scopusauthoridKwok, S=22980498300en_HK
dc.identifier.scopusauthoridLarsson, B=7202678664en_HK
dc.identifier.scopusauthoridLecacheux, A=7003423533en_HK
dc.identifier.scopusauthoridNummelin, A=6603768944en_HK
dc.identifier.scopusauthoridOlberg, M=16201342800en_HK
dc.identifier.scopusauthoridSandqvist, Aa=35451841800en_HK
dc.identifier.scopusauthoridWirström, ES=14042809000en_HK

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