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dc.contributor.authorIlee, J. D.
dc.contributor.authorCyganowski, C. J.
dc.contributor.authorNazari, P.
dc.contributor.authorHunter, T. R.
dc.contributor.authorBrogan, C. L.
dc.contributor.authorForgan, D. H.
dc.contributor.authorZhang, Q.
dc.date.accessioned2016-10-11T11:30:22Z
dc.date.available2016-10-11T11:30:22Z
dc.date.issued2016-11-11
dc.identifier.citationIlee , J D , Cyganowski , C J , Nazari , P , Hunter , T R , Brogan , C L , Forgan , D H & Zhang , Q 2016 , ' G11.92-0.61 MM1 : a Keplerian disc around a massive young proto-O star ' Monthly Notices of the Royal Astronomical Society , vol. 462 , no. 4 , pp. 4386-4401 . https://doi.org/10.1093/mnras/stw1912en
dc.identifier.issn1365-2966
dc.identifier.otherPURE: 246547269
dc.identifier.otherPURE UUID: 580b1f60-90bb-4c39-924d-2bc0e7386232
dc.identifier.otherArXiv: http://arxiv.org/abs/1608.05561v1
dc.identifier.otherScopus: 84994519171
dc.identifier.otherWOS: 000385231600066
dc.identifier.urihttp://hdl.handle.net/10023/9643
dc.descriptionJDI gratefully acknowledges support from the DISCSIM project, grant agreement 341137, funded by the European Research Council under ERC-2013-ADG. CJC acknowledges support from STFC grant ST/M001296/1. PN, CJC and JDI gratefully acknowledge support in the form of an Undergraduate Research Bursary from the Royal Astronomical Society. DF acknowledges support from the ECOGAL project, grant agreement 291227, funded by the European Research Council under ERC-2011-ADG.en
dc.description.abstractThe formation process of massive stars is not well understood, and advancement in our understanding benefits from high-resolution observations and modelling of the gas and dust surrounding individual high-mass (proto)stars. Here, we report subarcsecond (≲1550 au) resolution observations of the young massive star G11.92−0.61 MM1 with the Submillimeter Array (SMA) and Very Large Array (VLA). Our 1.3 mm SMA observations reveal consistent velocity gradients in compact molecular line emission from species such as CH3CN, CH3OH, OCS, HNCO, H2CO, DCN and CH3CH2CN, oriented perpendicular to the previously reported bipolar molecular outflow from MM1. Modelling of the compact gas kinematics suggests a structure undergoing rotation around the peak of the dust continuum emission. The rotational profile can be well fitted by a model of a Keplerian disc, including infall, surrounding an enclosed mass of ∼30–60 M⊙, of which 2–3 M⊙ is attributed to the disc. From modelling the CH3CN emission, we determine that two temperature components, of ∼150 K and 230 K, are required to adequately reproduce the spectra. Our 0.9 and 3.0 cm VLA continuum data exhibit an excess above the level expected from dust emission; the full centimetre–submillimetre wavelength spectral energy distribution of MM1 is well reproduced by a model including dust emission, an unresolved hypercompact H II region, and a compact ionized jet. In combination, our results suggest that MM1 is an example of a massive proto-O star forming via disc accretion, in a similar way to that of lower mass stars.
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2016, the Author(s). This work is made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at mnras.oxfordjournals.org / https://doi.org/10.1093/mnras/stw1912en
dc.subjectStars: individual: G11.92-0.61en
dc.subjectStars: massiveen
dc.subjectStars: pre-main sequenceen
dc.subjectStars: protostarsen
dc.subjectRadio continuum: starsen
dc.subjectSubmillimetre: starsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleG11.92-0.61 MM1 : a Keplerian disc around a massive young proto-O staren
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews.St Andrews Centre for Exoplanet Scienceen
dc.identifier.doihttps://doi.org/10.1093/mnras/stw1912
dc.description.statusPeer revieweden


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