Signatures of warm carbon monoxide in protoplanetary discs observed with Herschel SPIRE

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dc.contributor.authorvan der Wiel, M. H. D.
dc.contributor.authorNaylor, David A.
dc.contributor.authorKamp, I.
dc.contributor.authorMénard, F.
dc.contributor.authorThi, W.-F.
dc.contributor.authorWoitke, P.
dc.contributor.authorOlofsson, G.
dc.contributor.authorPontoppidan, K. M.
dc.contributor.authorDi Francesco, J.
dc.contributor.authorGlauser, A. M.
dc.contributor.authorGreaves, J. S.
dc.contributor.authorIvison, R. J.
dc.date.accessioned2019-12-13T04:17:31Z
dc.date.available2019-12-13T04:17:31Z
dc.date.issued2014
dc.descriptionSherpa Romeo green journal. Permission to archive final published versionen_US
dc.description.abstractMolecular gas constitutes the dominant mass component of protoplanetary discs. To date, these sources have not been studied comprehensively at the longest far-infrared and shortest submillimetre wavelengths. This paper presents Herschel SPIRE FTS spectroscopic observations towards 18 protoplanetary discs, covering the entire 450–1540GHz (666–195 μm) range at ν/ ν ≈ 400–1300. The spectra reveal clear detections of the dust continuum and, in six targets, a significant amount of spectral line emission primarily attributable to 12CO rotational lines. Other targets exhibit little to no detectable spectral lines. Low signal-to-noise detections also include signatures from 13CO, [CI] and HCN. For completeness, we present upper limits of non-detected lines in all targets, including low-energy transitions of H2O and CH+ molecules. The 10 12CO lines that fall within the SPIRE FTS bands trace energy levels of ∼50–500K. Combined with lower and higher energy lines from the literature, we compare the CO rotational line energy distribution with detailed physical–chemical models, for sources where these are available and published. Our 13CO line detections in the disc around Herbig Be star HD 100546 exceed, by factors of ∼10–30, the values predicted by a model that matches a wealth of other observational constraints, including the SPIRE 12COladder. To explain the observed 12CO/13COratio, it may be necessary to consider the combined effects of optical depth and isotope selective (photo)chemical processes. Considering the full sample of 18 objects, we find that the strongest line emission is observed in discs around Herbig Ae/Be stars, although not all show line emission. In addition, two of the six T Tauri objects exhibit detectable 12CO lines in the SPIRE range.en_US
dc.description.peer-reviewYesen_US
dc.identifier.citationvan der Wiel, M. H. D., Naylor, D. A., Kamp, I., Ménard, F., Thi, W. F., Woitke, P., ... Ivison, R. J. (2014). Signatures of warm carbon monoxide in protoplanetary discs observed with Herschel SPIRE. Monthly Notices of the Royal Astronomical Society, 444(4), 3911-3925. doi:10.1093/mnras/stu1462en_US
dc.identifier.urihttps://hdl.handle.net/10133/5629
dc.language.isoen_USen_US
dc.publisherOxford University Pressen_US
dc.publisher.departmentDepartment of Physics and Astronomyen_US
dc.publisher.facultyArts and Scienceen_US
dc.publisher.institutionUniversity of Lethbridgeen_US
dc.publisher.institutionUniversity of Groningenen_US
dc.publisher.institutionCNRSen_US
dc.publisher.institutionUniversité Grenoble Alpesen_US
dc.publisher.institutionUniversity of St. Andrewsen_US
dc.publisher.institutionStockholm Universityen_US
dc.publisher.institutionSpace Telescope Science Instituteen_US
dc.publisher.institutionNational Research Council Canadaen_US
dc.publisher.institutionUniversity of Victoriaen_US
dc.publisher.institutionETH Zurichen_US
dc.publisher.institutionEuropean Southern Observatoryen_US
dc.publisher.institutionUniversity of Edinburghen_US
dc.publisher.urlhttps://doi.org/10.1093/mnras/stu1462en_US
dc.subjectAstrochemistryen_US
dc.subjectProtoplanetary discsen_US
dc.subjectCircumstellar matteren_US
dc.subjectStarsen_US
dc.subjectT Taurien_US
dc.subjectHerbig Ae/Been_US
dc.subject.lcshCosmochemistry
dc.subject.lcshProtoplanetary disks
dc.titleSignatures of warm carbon monoxide in protoplanetary discs observed with Herschel SPIREen_US
dc.typeArticleen_US
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