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dc.contributor.authorBISTRO
dc.date.accessioned2019-08-01T16:11:39Z
dc.date.available2019-08-01T16:11:39Z
dc.date.issued2019-05-22
dc.identifier.citationBISTRO 2019 , ' The JCMT BISTRO Survey : The Magnetic Field In The Starless Core $ρ$ Ophiuchus C ' , The Astrophysical Journal , vol. 877 , no. 1 , 43 . https://doi.org/10.3847/1538-4357/ab0958
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 16402936
dc.identifier.otherPURE UUID: 9f13b177-cf5d-49c0-95bf-13e6fadaaa4b
dc.identifier.otherArXiv: http://arxiv.org/abs/1902.07734v1
dc.identifier.otherORCID: /0000-0002-2859-4600/work/62748440
dc.identifier.otherScopus: 85068692356
dc.identifier.urihttp://hdl.handle.net/2299/21530
dc.description22 pages, 12 figures
dc.description.abstractWe report 850 μm dust polarization observations of a low-mass (∼12 M o) starless core in the ρ Ophiuchus cloud, Ophiuchus C, made with the POL-2 instrument on the James Clerk Maxwell Telescope (JCMT) as part of the JCMT B-fields In STar-forming Region Observations survey. We detect an ordered magnetic field projected on the plane of the sky in the starless core. The magnetic field across the ∼0.1 pc core shows a predominant northeast-southwest orientation centering between ∼40° and ∼100°, indicating that the field in the core is well aligned with the magnetic field in lower-density regions of the cloud probed by near-infrared observations and also the cloud-scale magnetic field traced by Planck observations. The polarization percentage (P) decreases with increasing total intensity (I), with a power-law index of -1.03 ± 0.05. We estimate the plane-of-sky field strength (B pos) using modified Davis-Chandrasekhar-Fermi methods based on structure function (SF), autocorrelation function (ACF), and unsharp masking (UM) analyses. We find that the estimates from the SF, ACF, and UM methods yield strengths of 103 ± 46 μG, 136 ± 69 μG, and 213 ± 115 μG, respectively. Our calculations suggest that the Ophiuchus C core is near magnetically critical or slightly magnetically supercritical (i.e., unstable to collapse). The total magnetic energy calculated from the SF method is comparable to the turbulent energy in Ophiuchus C, while the ACF method and the UM method only set upper limits for the total magnetic energy because of large uncertainties.en
dc.language.isoeng
dc.relation.ispartofThe Astrophysical Journal
dc.subjectISM: individual objects (Ophiuchus)
dc.subjectmagnetic fields
dc.subjectpolarization
dc.subjectstars: formation
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titleThe JCMT BISTRO Survey : The Magnetic Field In The Starless Core $ρ$ Ophiuchus Cen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionRegistry
dc.contributor.institutionSchool of Physics, Engineering & Computer Science
dc.contributor.institutionDepartment of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=85068692356&partnerID=8YFLogxK
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.3847/1538-4357/ab0958
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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