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dc.contributor.authorPillai, Thushara G. S.en_US
dc.contributor.authorClemens, Dan P.en_US
dc.contributor.authorReissl, Stefanen_US
dc.contributor.authorMyers, Philip C.en_US
dc.contributor.authorKauffmann, Jensen_US
dc.contributor.authorLopez-Rodriguez, Enriqueen_US
dc.contributor.authorAlves, F. O.en_US
dc.contributor.authorFranco, G. A. P.en_US
dc.contributor.authorHenshaw, Jonathanen_US
dc.contributor.authorMenten, Karl M.en_US
dc.contributor.authorNakamura, Fumitakaen_US
dc.contributor.authorSeifried, Danielen_US
dc.contributor.authorSugitani, Kojien_US
dc.contributor.authorWiesemeyer, Helmuten_US
dc.date.accessioned2021-02-05T19:28:15Z
dc.date.available2021-02-05T19:28:15Z
dc.date.issued2020-12
dc.identifier.citationThushara GS Pillai, Dan P Clemens, Stefan Reissl, Philip C Myers, Jens Kauffmann, Enrique Lopez-Rodriguez, F.O. Alves, G.A.P. Franco, Jonathan Henshaw, Karl M Menten, Fumitaka Nakamura, Daniel Seifried, Koji Sugitani, Helmut Wiesemeyer. 2020. "Magnetized filamentary gas flows feeding the young embedded cluster in Serpens South." Nature Astronomy, Volume 4, Issue 12, pp. 1195 - 1201. https://doi.org/10.1038/s41550-020-1172-6
dc.identifier.issn2397-3366
dc.identifier.urihttps://hdl.handle.net/2144/41996
dc.description.abstractObservations indicate that molecular clouds are strongly magnetized, and that magnetic fields influence the formation of stars. A key observation supporting the conclusion that molecular clouds are significantly magnetized is that the orientation of their internal structure is closely related to that of the magnetic field. At low column densities, the structure aligns parallel with the field, whereas at higher column densities, the gas structure is typically oriented perpendicular to magnetic fields, with a transition at visual extinctions AV ≳ 3 mag. Here we use far-infrared polarimetric observations from the HAWC+ polarimeter on SOFIA to report the discovery of a further transition in relative orientation, that is, a return to parallel alignment at AV ≳ 21 mag in parts of the Serpens South cloud. This transition appears to be caused by gas flow and indicates that magnetic supercriticality sets in near AV ≳ 21 mag, allowing gravitational collapse and star cluster formation to occur even in the presence of relatively strong magnetic fields.en_US
dc.format.extentp. 1195 - 1201en_US
dc.languageen
dc.language.isoen_US
dc.publisherSpringer Science and Business Media LLCen_US
dc.relation.ispartofNature Astronomy
dc.titleMagnetized filamentary gas flows feeding the young embedded cluster in Serpens Southen_US
dc.typeArticleen_US
dc.description.versionAccepted manuscripten_US
dc.identifier.doi10.1038/s41550-020-1172-6
pubs.elements-sourcecrossrefen_US
pubs.notesEmbargo: No embargoen_US
pubs.organisational-groupBoston Universityen_US
pubs.organisational-groupBoston University, College of Arts & Sciencesen_US
pubs.organisational-groupBoston University, College of Arts & Sciences, Department of Astronomyen_US
pubs.publication-statusPublisheden_US
dc.date.online2020-08-17
dc.identifier.orcid0000-0002-9947-4956 (Clemens, Dan P)
dc.identifier.mycv585860


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