@article{d30058e865fc4bc6817bde24686b49e2,
title = "The Twisted Magnetic Field of the Protobinary L483",
abstract = "We present H-band (1.65 μm) and SOFIA HAWC+ 154 μm polarization observations of the low-mass core L483. Our H-band observations reveal a magnetic field that is overwhelmingly in the E-W direction, which is approximately parallel to the bipolar outflow that is observed in scattered IR light and in single-dish 12CO observations. From our 154 μm data, we infer a ∼45° twist in the magnetic field within the inner 5″ (1000 au) of L483. We compare these new observations with published single-dish 350 μm polarimetry and find that the 10,000 au scale H-band data match the smaller-scale 350 μm data, indicating that the collapse of L483 is magnetically regulated on these larger scales. We also present high-resolution 1.3 mm Atacama Large Millimeter/submillimeter Array data of L483 that reveals it is a close binary star with a separation of 34 au. The plane of the binary of L483 is observed to be approximately parallel to the twisted field in the inner 1000 au. Comparing this result to the ∼1000 au protostellar envelope, we find that the envelope is roughly perpendicular to the 1000 au HAWC+ field. Using the data presented, we speculate that L483 initially formed as a wide binary and the companion star migrated to its current position, causing an extreme shift in angular momentum thereby producing the twisted magnetic field morphology observed. More observations are needed to further test this scenario.",
author = "Cox, {Erin G.} and Giles Novak and Sadavoy, {Sarah I.} and Looney, {Leslie W.} and Dennis Lee and Marc Berthoud and Bourke, {Tyler L.} and Simon Coud{\'e} and Frankie Encalada and Fissel, {Laura M.} and Rachel Harrison and Martin Houde and Li, {Zhi Yun} and Myers, {Philip C.} and Kate Pattle and Santos, {Fabio P.} and Stephens, {Ian W.} and Hailin Wang and Sebastian Wolf",
note = "Data cubes containing the CO outflow observations for L483 (Tafalla et al. ; Velusamy et al. ) and the SMA 850 μm continuum observations (Leung et al. ) were kindly provided by Mario Tafalla, Thangasamy Velusamy, and Gigi Leung. This work was based [in part] on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). SOFIA is jointly operated by the Universities Space Research Association, Inc. (USRA), under NASA contract NNA17BF53C, and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 2002 to the University of Stuttgart. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.1.00085.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). This publication makes use of SPIRE data products (NHSC , , ). This research has made use of the NASA/IPAC Infrared Science Archive, which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology. This publication also makes use of data products from the Two Micron All Sky Survey (Skrutskie et al. ), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center (2MASS Team ), funded by the National Aeronautics and Space Administration and the National Science Foundation. This publication has made use of data products based on observations obtained with Planck ( http://www.esa.int/Planck ), an ESA science mission with instruments and contributions directly funded by ESA Member States, NASA, and Canada (Planck Team ). This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. We thank the anonymous referee for their helpful comments in improving this manuscript. L.W.L. acknowledges support from NSF AST-1910364. Z.Y.L. is supported in part by NSF AST-1815784 and NASA 80NSSC20K0533. I.W.S. acknowledges support for this work by NASA through award #08_0186 issued by USRA. Financial support for this work was provided by NASA through award Nos. SOF06-0116 and SOF07-0147 issued by USRA to Northwestern University. K.P. is a Royal Society University Research Fellow, supported by grant number URF\R1\211322. S.I.S. acknowledges support from the Natural Science and Engineering Research Council of Canada (NSERC), RGPIN-2020-0398.",
year = "2022",
month = jun,
day = "1",
doi = "10.3847/1538-4357/ac722a",
language = "English (US)",
volume = "932",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "American Astronomical Society",
number = "1",
}