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Chemistry In Disks VII. First detection of HC3N in protoplanetary disks

hal.structure.identifierInstitut de RadioAstronomie Millimétrique [IRAM]
hal.structure.identifierAMOR 2012
dc.contributor.authorCHAPILLON, E.
hal.structure.identifierAMOR 2012
dc.contributor.authorDUTREY, Anne
hal.structure.identifierAMOR 2012
dc.contributor.authorGUILLOTEAU, S.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG ]
dc.contributor.authorPIETU, V.
hal.structure.identifierAMOR 2012
dc.contributor.authorWAKELAM, Valentine
hal.structure.identifierFORMATION STELLAIRE 2012
dc.contributor.authorHERSANT, F.
dc.contributor.authorGUETH, F.
hal.structure.identifierMax-Planck-Institut für Astronomie [MPIA]
dc.contributor.authorHENNING, T.
dc.contributor.authorLAUNHARDT, R.
dc.contributor.authorSCHREYER, K.
hal.structure.identifierMax-Planck-Institut für Astronomie [MPIA]
dc.contributor.authorSEMENOV, D.
dc.date.created2012-07-11
dc.date.issued2012
dc.identifier.issn0004-637X
dc.description.abstractEnMolecular line emission from protoplanetary disks is a powerful tool to constrain their physical and chemical structure. Nevertheless, only a few molecules have been detected in disks so far. We take advantage of the enhanced capabilities of the IRAM 30m telescope by using the new broad band correlator (FTS) to search for so far undetected molecules in the protoplanetary disks surrounding the TTauri stars DM Tau, GO Tau, LkCa 15 and the Herbig Ae star MWC 480. We report the first detection of HC3N at 5 sigma in the GO Tau and MWC 480 disks with the IRAM 30-m, and in the LkCa 15 disk (5 sigma), using the IRAM array, with derived column densities of the order of 10^{12}cm^{-2}. We also obtain stringent upper limits on CCS (N < 1.5 x 10^{12} cm^{-3}). We discuss the observational results by comparing them to column densities derived from existing chemical disk models (computed using the chemical code Nautilus) and based on previous nitrogen and sulfur-bearing molecule observations. The observed column densities of HC3N are typically two orders of magnitude lower than the existing predictions and appear to be lower in the presence of strong UV flux, suggesting that the molecular chemistry is sensitive to the UV penetration through the disk. The CCS upper limits reinforce our model with low elemental abundance of sulfur derived from other sulfur-bearing molecules (CS, H2S and SO).
dc.language.isoen
dc.publisherAmerican Astronomical Society
dc.subject.enSolar and Stellar Astrophysics
dc.subject.enAstrophysics
dc.subject.enGalaxy Astrophysics
dc.title.enChemistry In Disks VII. First detection of HC3N in protoplanetary disks
dc.typeArticle de revue
dc.identifier.doi10.1088/0004-637X/756/1/58
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
dc.identifier.arxiv1207.2682
bordeaux.journalThe Astrophysical Journal
bordeaux.page58
bordeaux.volume756
bordeaux.issue1
bordeaux.peerReviewedoui
hal.identifierhal-00718070
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-00718070v1
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