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Article: Low upper limits on the O 2 abundance from the Odin satellite

TitleLow upper limits on the O 2 abundance from the Odin satellite
Authors
KeywordsGalaxy: Abundances
Ism: Molecules
Radio Lines: Ism
Issue Date2003
PublisherE D P Sciences. The Journal's web site is located at http://www.aanda.org
Citation
Astronomy And Astrophysics, 2003, v. 402 n. 3, p. L77-L81 How to Cite?
AbstractFor the first time, a search has been conducted in our Galaxy for the 119 GHz transition connecting to the ground state of O 2, using the Odin satellite. Equipped with a sensitive 3 mm receiver (T sys(SSB) = 600 K), Odin has reached unprecedented upper limits on the abundance of O 2, especially in cold dark clouds where the excited state levels involved in the 487 GHz transition are not expected to be significantly populated. Here we report upper limits for a dozen sources. In cold dark clouds we improve upon the published SWAS upper limits by more than an order of magnitude, reaching N(O 2)/N(H 2) ≤ 10 -7 in half of the sources. While standard chemical models are definitively ruled out by these new limits, our results are compatible with several recent studies that derive lower O 2 abundances. Goldsmith et al. (2002) recently reported a SWAS tentative detection of the 487 GHz transition of O 2 in an outflow wing towards ρ Oph A in a combination of 7 beams covering approximately 10′ × 14′. In a brief (1.3 hour integration time) and partial covering of the SWAS region ≈65% if we exclude their central position), we did not detect the corresponding 119 GHz line. Our 3 sigma upper limit on the O 2 column density is 7.3 × 10 15 cm -2. We presently cannot exclude the possibility that the SWAS signal lies mostly outside of the 9′ Odin beam and has escaped our sensitive detector.
Persistent Identifierhttp://hdl.handle.net/10722/179661
ISSN
2014 Impact Factor: 4.378
2015 SCImago Journal Rankings: 2.446
References

 

DC FieldValueLanguage
dc.contributor.authorPagani, Len_US
dc.contributor.authorOlofsson, AOHen_US
dc.contributor.authorBergman, Pen_US
dc.contributor.authorBernath, Pen_US
dc.contributor.authorBlack, JHen_US
dc.contributor.authorBooth, RSen_US
dc.contributor.authorBuat, Ven_US
dc.contributor.authorCrovisier, Jen_US
dc.contributor.authorCurry, CLen_US
dc.contributor.authorEncrenaz, PJen_US
dc.contributor.authorFalgarone, Een_US
dc.contributor.authorFeldman, PAen_US
dc.contributor.authorFich, Men_US
dc.contributor.authorFloren, HGen_US
dc.contributor.authorFrisk, Uen_US
dc.contributor.authorGerin, Men_US
dc.contributor.authorGregersen, EMen_US
dc.contributor.authorHarju, Jen_US
dc.contributor.authorHasegawa, Ten_US
dc.contributor.authorHjalmarson, Åen_US
dc.contributor.authorJohansson, LEBen_US
dc.contributor.authorKwok, Sen_US
dc.contributor.authorLarsson, Ben_US
dc.contributor.authorLecacheux, Aen_US
dc.contributor.authorLiljeström, Ten_US
dc.contributor.authorLindqvist, Men_US
dc.contributor.authorLiseau, Ren_US
dc.contributor.authorMattila, Ken_US
dc.contributor.authorMitchell, GFen_US
dc.contributor.authorNordh, LHen_US
dc.contributor.authorOlberg, Men_US
dc.contributor.authorOlofsson, Gen_US
dc.contributor.authorRistorcelli, Ien_US
dc.contributor.authorSandqvist, Aaen_US
dc.contributor.authorVon Scheele, Fen_US
dc.contributor.authorSerra, Gen_US
dc.contributor.authorTothill, NFen_US
dc.contributor.authorVolk, Ken_US
dc.contributor.authorWiklind, Ten_US
dc.contributor.authorWilson, CDen_US
dc.date.accessioned2012-12-19T10:02:26Z-
dc.date.available2012-12-19T10:02:26Z-
dc.date.issued2003en_US
dc.identifier.citationAstronomy And Astrophysics, 2003, v. 402 n. 3, p. L77-L81en_US
dc.identifier.issn0004-6361en_US
dc.identifier.urihttp://hdl.handle.net/10722/179661-
dc.description.abstractFor the first time, a search has been conducted in our Galaxy for the 119 GHz transition connecting to the ground state of O 2, using the Odin satellite. Equipped with a sensitive 3 mm receiver (T sys(SSB) = 600 K), Odin has reached unprecedented upper limits on the abundance of O 2, especially in cold dark clouds where the excited state levels involved in the 487 GHz transition are not expected to be significantly populated. Here we report upper limits for a dozen sources. In cold dark clouds we improve upon the published SWAS upper limits by more than an order of magnitude, reaching N(O 2)/N(H 2) ≤ 10 -7 in half of the sources. While standard chemical models are definitively ruled out by these new limits, our results are compatible with several recent studies that derive lower O 2 abundances. Goldsmith et al. (2002) recently reported a SWAS tentative detection of the 487 GHz transition of O 2 in an outflow wing towards ρ Oph A in a combination of 7 beams covering approximately 10′ × 14′. In a brief (1.3 hour integration time) and partial covering of the SWAS region ≈65% if we exclude their central position), we did not detect the corresponding 119 GHz line. Our 3 sigma upper limit on the O 2 column density is 7.3 × 10 15 cm -2. We presently cannot exclude the possibility that the SWAS signal lies mostly outside of the 9′ Odin beam and has escaped our sensitive detector.en_US
dc.languageengen_US
dc.publisherE D P Sciences. The Journal's web site is located at http://www.aanda.orgen_US
dc.relation.ispartofAstronomy and Astrophysicsen_US
dc.subjectGalaxy: Abundancesen_US
dc.subjectIsm: Moleculesen_US
dc.subjectRadio Lines: Ismen_US
dc.titleLow upper limits on the O 2 abundance from the Odin satelliteen_US
dc.typeArticleen_US
dc.identifier.emailKwok, S: deannote@hku.hken_US
dc.identifier.authorityKwok, S=rp00716en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.scopuseid_2-s2.0-0037687320en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-0037687320&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume402en_US
dc.identifier.issue3en_US
dc.identifier.spageL77en_US
dc.identifier.epageL81en_US
dc.publisher.placeFranceen_US
dc.identifier.scopusauthoridPagani, L=7006076032en_US
dc.identifier.scopusauthoridOlofsson, AOH=7006322972en_US
dc.identifier.scopusauthoridBergman, P=7006615192en_US
dc.identifier.scopusauthoridBernath, P=35372923700en_US
dc.identifier.scopusauthoridBlack, JH=25222377400en_US
dc.identifier.scopusauthoridBooth, RS=7202614585en_US
dc.identifier.scopusauthoridBuat, V=7003733332en_US
dc.identifier.scopusauthoridCrovisier, J=35448565400en_US
dc.identifier.scopusauthoridCurry, CL=7101672097en_US
dc.identifier.scopusauthoridEncrenaz, PJ=6603978312en_US
dc.identifier.scopusauthoridFalgarone, E=7003349192en_US
dc.identifier.scopusauthoridFeldman, PA=7103377526en_US
dc.identifier.scopusauthoridFich, M=7003964696en_US
dc.identifier.scopusauthoridFloren, HG=6602447564en_US
dc.identifier.scopusauthoridFrisk, U=8966521600en_US
dc.identifier.scopusauthoridGerin, M=7005195915en_US
dc.identifier.scopusauthoridGregersen, EM=7005825957en_US
dc.identifier.scopusauthoridHarju, J=8908583000en_US
dc.identifier.scopusauthoridHasegawa, T=7404173711en_US
dc.identifier.scopusauthoridHjalmarson, Å=15744175200en_US
dc.identifier.scopusauthoridJohansson, LEB=7401510283en_US
dc.identifier.scopusauthoridKwok, S=22980498300en_US
dc.identifier.scopusauthoridLarsson, B=7202678664en_US
dc.identifier.scopusauthoridLecacheux, A=7003423533en_US
dc.identifier.scopusauthoridLiljeström, T=6602325021en_US
dc.identifier.scopusauthoridLindqvist, M=7006711792en_US
dc.identifier.scopusauthoridLiseau, R=6701345678en_US
dc.identifier.scopusauthoridMattila, K=7102595643en_US
dc.identifier.scopusauthoridMitchell, GF=7403103591en_US
dc.identifier.scopusauthoridNordh, LH=6603608785en_US
dc.identifier.scopusauthoridOlberg, M=16201342800en_US
dc.identifier.scopusauthoridOlofsson, G=7005783479en_US
dc.identifier.scopusauthoridRistorcelli, I=6701750764en_US
dc.identifier.scopusauthoridSandqvist, Aa=35451841800en_US
dc.identifier.scopusauthoridVon Scheele, F=6602800581en_US
dc.identifier.scopusauthoridSerra, G=7202261072en_US
dc.identifier.scopusauthoridTothill, NF=6602148553en_US
dc.identifier.scopusauthoridVolk, K=7006571965en_US
dc.identifier.scopusauthoridWiklind, T=7003555548en_US
dc.identifier.scopusauthoridWilson, CD=7404896077en_US

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