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dc.contributor.author van der Wiel, M. H. D.
dc.contributor.author Naylor, David A.
dc.contributor.author Kamp, I.
dc.contributor.author Ménard, F.
dc.contributor.author Thi, W.-F.
dc.contributor.author Woitke, P.
dc.contributor.author Olofsson, G.
dc.contributor.author Pontoppidan, K. M.
dc.contributor.author Di Francesco, J.
dc.contributor.author Glauser, A. M.
dc.contributor.author Greaves, J. S.
dc.contributor.author Ivison, R. J.
dc.date.accessioned 2019-12-13T04:17:31Z
dc.date.available 2019-12-13T04:17:31Z
dc.date.issued 2014
dc.identifier.citation van 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/stu1462 en_US
dc.identifier.uri https://hdl.handle.net/10133/5629
dc.description Sherpa Romeo green journal. Permission to archive final published version en_US
dc.description.abstract Molecular 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.language.iso en_US en_US
dc.publisher Oxford University Press en_US
dc.subject Astrochemistry en_US
dc.subject Protoplanetary discs en_US
dc.subject Circumstellar matter en_US
dc.subject Stars en_US
dc.subject T Tauri en_US
dc.subject Herbig Ae/Be en_US
dc.subject.lcsh Cosmochemistry
dc.subject.lcsh Protoplanetary disks
dc.title Signatures of warm carbon monoxide in protoplanetary discs observed with Herschel SPIRE en_US
dc.type Article en_US
dc.publisher.faculty Arts and Science en_US
dc.publisher.department Department of Physics and Astronomy en_US
dc.description.peer-review Yes en_US
dc.publisher.institution University of Lethbridge en_US
dc.publisher.institution University of Groningen en_US
dc.publisher.institution CNRS en_US
dc.publisher.institution Université Grenoble Alpes en_US
dc.publisher.institution University of St. Andrews en_US
dc.publisher.institution Stockholm University en_US
dc.publisher.institution Space Telescope Science Institute en_US
dc.publisher.institution National Research Council Canada en_US
dc.publisher.institution University of Victoria en_US
dc.publisher.institution ETH Zurich en_US
dc.publisher.institution European Southern Observatory en_US
dc.publisher.institution University of Edinburgh en_US
dc.publisher.url https://doi.org/10.1093/mnras/stu1462 en_US


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