dc.contributor.author | BISTRO | |
dc.contributor.author | Gledhill, Timothy | |
dc.date.accessioned | 2018-06-19T17:37:39Z | |
dc.date.available | 2018-06-19T17:37:39Z | |
dc.date.issued | 2018-05-16 | |
dc.identifier.citation | BISTRO & Gledhill , T 2018 , ' A First Look at BISTRO Observations of the ρ Oph-A core ' , The Astrophysical Journal , vol. 859 , no. 1 , 4 . https://doi.org/10.3847/1538-4357/aabd82 | |
dc.identifier.issn | 0004-637X | |
dc.identifier.other | ArXiv: http://arxiv.org/abs/1804.09313v1 | |
dc.identifier.other | ORCID: /0000-0002-2859-4600/work/54896471 | |
dc.identifier.uri | http://hdl.handle.net/2299/20184 | |
dc.description | This is an author-created, un-copyedited version of an article published in The Astrophysical Journal. The Version of Record is available online at https://doi.org/10.3847/1538-4357/aabd82. | |
dc.description.abstract | We present 850 μm imaging polarimetry data of the ρ Oph-A core taken with the Submillimeter Common-User Bolometer Array-2 (SCUBA-2) and its polarimeter (POL-2) as part of our ongoing survey project, -fields In STar forming RegiOns (BISTRO). The polarization vectors are used to identify the orientation of the magnetic field projected on the plane of the sky at a resolution of 0.01 pc. We identify 10 subregions with distinct polarization fractions and angles in the 0.2 pc ρ Oph-A core; some of them can be part of a coherent magnetic field structure in the ρ Oph region. The results are consistent with previous observations of the brightest regions of ρ Oph-A, where the degrees of polarization are at a level of a few percent, but our data reveal for the first time the magnetic field structures in the fainter regions surrounding the core where the degree of polarization is much higher (>5%). A comparison with previous near-infrared polarimetric data shows that there are several magnetic field components that are consistent at near-infrared and submillimeter wavelengths. Using the Davis-Chandrasekhar-Fermi method, we also derive magnetic field strengths in several subcore regions, which range from approximately 0.2 to 5 mG. We also find a correlation between the magnetic field orientations projected on the sky and the core centroid velocity components. | en |
dc.format.extent | 22 | |
dc.format.extent | 1400956 | |
dc.language.iso | eng | |
dc.relation.ispartof | The Astrophysical Journal | |
dc.subject | circumstellar matter | |
dc.subject | ISM: individual objects (Ophiuchi) | |
dc.subject | ISM: structure | |
dc.subject | polarization | |
dc.subject | radio continuum: ISM | |
dc.subject | stars: formation | |
dc.subject | Astronomy and Astrophysics | |
dc.subject | Space and Planetary Science | |
dc.title | A First Look at BISTRO Observations of the ρ Oph-A core | en |
dc.contributor.institution | School of Physics, Astronomy and Mathematics | |
dc.contributor.institution | Centre for Astrophysics Research (CAR) | |
dc.description.status | Peer reviewed | |
dc.identifier.url | http://www.scopus.com/inward/record.url?scp=85047882276&partnerID=8YFLogxK | |
rioxxterms.versionofrecord | 10.3847/1538-4357/aabd82 | |
rioxxterms.type | Journal Article/Review | |
herts.preservation.rarelyaccessed | true | |