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2019ApJ...877...88C - Astrophys. J., 877, 88-88 (2019/June-1)

The JCMT BISTRO Survey: the magnetic field of the Barnard 1 Star-forming Region.

COUDE S., BASTIEN P., HOUDE M., SADAVOY S., FRIESEN R., DI FRANCESCO J., JOHNSTONE D., MAIRS S., HASEGAWA T., KWON W., LAI S.-P., QIU K., WARD-THOMPSON D., BERRY D., CHEN M.C.-Y., FIEGE J., FRANZMANN E., HATCHELL J., LACAILLE K., MATTHEWS B.C., MORIARTY-SCHIEVEN G.H., PON A., ANDRE P., ARZOUMANIAN D., ASO Y., BYUN D.-Y., ESWARAIAH C., CHEN H.-R., CHEN W.P., CHING T.-C., CHO J., CHOI M., CHRYSOSTOMOU A., CHUNG E.J., DOI Y., DRABEK-MAUNDER E., DOWELL C.D., EYRES S.P.S., FALLE S., FRIBERG P., FULLER G., FURUYA R.S., GLEDHILL T., GRAVES S.F., GREAVES J.S., GRIFFIN M.J., GU Q., HAYASHI S.S., HOANG T., HOLLAND W., INOUE T., INUTSUKA S.-I., IWASAKI K., JEONG I.-G., KANAMORI Y., KATAOKA A., KANG J.-H., KANG M., KANG S.-J., KAWABATA K.S., KEMPER F., KIM G., KIM J., KIM K.-T., KIM K.H., KIM M.-R., KIM S., KIRK J.M., KOBAYASHI M.I.N., KOCH P.M., KWON J., LEE J.-E., LEE C.W., LEE S.-S., LI D., LI D., LI H.-B., LIU H.-L., LIU J., LIU S.-Y., LIU T., VAN LOO S., LYO A.-R., MATSUMURA M., NAGATA T., NAKAMURA F., NAKANISHI H., OHASHI N., ONAKA T., PARSONS H., PATTLE K., PERETTO N., PYO T.-S., QIAN L., RAO R., RAWLINGS M.G., RETTER B., RICHER J., RIGBY A., ROBITAILLE J.-F., SAITO H., SAVINI G., SCAIFE A.M.M., SETA M., SHINNAGA H., SOAM A., TAMURA M., TANG Y.-W., TOMISAKA K., TSUKAMOTO Y., WANG H., WANG J.-W., WHITWORTH A.P., YEN H.-W., YOO H., YUAN J., ZENKO T., ZHANG C.-P., ZHANG G., ZHOU J., ZHU L. (The B-fields In STar-forming Regions Observations (BISTRO)

Abstract (from CDS):

We present the POL-2 850 µm linear polarization map of the Barnard 1 clump in the Perseus molecular cloud complex from the B-fields In STar-forming Region Observations survey at the James Clerk Maxwell Telescope. We find a trend of decreasing polarization fraction as a function of total intensity, which we link to depolarization effects toward higher-density regions of the cloud. We then use the polarization data at 850 µm to infer the plane-of-sky orientation of the large-scale magnetic field in Barnard 1. This magnetic field runs north-south across most of the cloud, with the exception of B1-c, where it turns more east-west. From the dispersion of polarization angles, we calculate a turbulence correlation length of 5.0 ± 2.''5 (1500 au) and a turbulent-to-total magnetic energy ratio of 0.5 ± 0.3 inside the cloud. We combine this turbulent-to-total magnetic energy ratio with observations of NH3 molecular lines from the Green Bank Ammonia Survey to estimate the strength of the plane-of-sky component of the magnetic field through the Davis-Chandrasekhar-Fermi method. With a plane-of-sky amplitude of 120 ± 60 µG and a criticality criterion λc = 3.0 ± 1.5, we find that Barnard 1 is a supercritical molecular cloud with a magnetic field nearly dominated by its turbulent component.

Abstract Copyright: © 2019. The American Astronomical Society. All rights reserved.

Journal keyword(s): ISM: clouds - ISM: individual objects: Barnard 1 - ISM: magnetic fields - polarization - stars: formation - submillimeter: ISM

Simbad objects: 28

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2019.09.22-11:25:22

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