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dc.contributor.authorCyganowski, C. J.
dc.contributor.authorIlee, J. D.
dc.contributor.authorBrogan, C. L.
dc.contributor.authorHunter, T. R.
dc.contributor.authorZhang, S.
dc.contributor.authorHarries, T. J.
dc.contributor.authorHaworth, T. J.
dc.date.accessioned2022-06-07T12:30:03Z
dc.date.available2022-06-07T12:30:03Z
dc.date.issued2022-06-01
dc.identifier279354383
dc.identifier106c3bd8-4420-4b1c-a305-7ef1c69e7853
dc.identifier85132011611
dc.identifier000804405600001
dc.identifier.citationCyganowski , C J , Ilee , J D , Brogan , C L , Hunter , T R , Zhang , S , Harries , T J & Haworth , T J 2022 , ' Discovery of a 500 au protobinary in the massive prestellar core G11.92-0.61 MM2 ' , Astrophysical Journal Letters , vol. 931 , no. 2 , L31 . https://doi.org/10.3847/2041-8213/ac69caen
dc.identifier.issn2041-8205
dc.identifier.otherArXiv: http://arxiv.org/abs/2204.09163v2
dc.identifier.urihttps://hdl.handle.net/10023/25497
dc.descriptionFunding: C.J.C. acknowledges support from the University of St Andrews Restarting Research Funding Scheme (SARRF), which is funded through the SFC grant reference SFC/AN/08/020. J.D.I. acknowledges support from the UK’s STFC under ST/T000287/1. S.Z. is funded by the China Scholarship Council–University of St Andrews Scholarship (PhD programmes, No. 201806190010). T.J.H. is funded by a Royal Society Dorothy Hodgkin Fellowship.en
dc.description.abstractWe present high-resolution (< ~160 au) Atacama Large Millimeter/submillimeter Array (ALMA) 1.3 mm observations of the high-mass prestellar core candidate G11.92-0.61 MM2, which reveal that this source is in fact a protobinary system with a projected separation of 505 au. The binary components, MM2E and MM2W, are compact (radii < 140 au) sources within the partially optically thick dust emission with α0.9 cm-1.3 mm =2.47-2.94. The 1.3 mm brightness temperatures, Tb=68.4/64.6 K for MM2E/MM2W, imply internal heating and minimum luminosities L* > 24.7 L⊙ for MM2E and L* > 12.6 L⊙ for MM2W. The compact sources are connected by a "bridge" of lower-surface-brightness dust emission and lie within more extended emission that may correspond to a circumbinary disk. The circumprotostellar gas mass, estimated from ~0.2" resolution VLA 0.9 cm observations assuming optically thin emission, is 6.8 ± 0.9 M⊙. No line emission is detected towards MM2E and MM2W in our high-resolution 1.3 mm ALMA observations. The only line detected is 13CO J=2-1, in absorption against the 1.3 mm continuum, which likely traces a layer of cooler molecular material surrounding the protostars. We also report the discovery of a highly asymmetric bipolar molecular outflow that appears to be driven by MM2E and/or MM2W in new deep, ~0.5" resolution (1680 au) ALMA 0.82 mm observations. This outflow, traced by low-excitation CH3OH emission, indicates ongoing accretion onto the protobinary system. Overall, the super-Alfvenic models of Mignon-Risse et al. (2021) agree well with the observed properties of the MM2E/MM2W protobinary, suggesting that this system may be forming in an environment with a weak magnetic field.
dc.format.extent9
dc.format.extent1279103
dc.language.isoeng
dc.relation.ispartofAstrophysical Journal Lettersen
dc.subjectStars: formationen
dc.subjectStars: protostarsen
dc.subjectISM: individual objects (G11.92.-0.61 MM2)en
dc.subjectISM: jets and outflowsen
dc.subjectAccretion, accretion discsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleDiscovery of a 500 au protobinary in the massive prestellar core G11.92-0.61 MM2en
dc.typeJournal articleen
dc.contributor.sponsorScottish Funding Councilen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doi10.3847/2041-8213/ac69ca
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/2204.09163en
dc.identifier.grantnumberN/Aen


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