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2019ApJ...876...42W - Astrophys. J., 876, 42-42 (2019/May-1)

JCMT BISTRO survey: magnetic fields within the hub-filament structure in IC 5146.

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

Abstract (from CDS):

We present the 850 µm polarization observations toward the IC 5146 filamentary cloud taken using the Submillimetre Common-User Bolometer Array 2 (SCUBA-2) and its associated polarimeter (POL-2), mounted on the James Clerk Maxwell Telescope, as part of the B-fields In STar forming Regions Observations. This work is aimed at revealing the magnetic field morphology within a core-scale (<=1.0 pc) hub-filament structure (HFS) located at the end of a parsec-scale filament. To investigate whether the observed polarization traces the magnetic field in the HFS, we analyze the dependence between the observed polarization fraction and total intensity using a Bayesian approach with the polarization fraction described by the Rice likelihood function, which can correctly describe the probability density function of the observed polarization fraction for low signal-to-noise ratio data. We find a power-law dependence between the polarization fraction and total intensity with an index of 0.56 in AV ∼ 20-300 mag regions, suggesting that the dust grains in these dense regions can still be aligned with magnetic fields in the IC 5146 regions. Our polarization maps reveal a curved magnetic field, possibly dragged by the contraction along the parsec-scale filament. We further obtain a magnetic field strength of 0.5 ± 0.2 mG toward the central hub using the Davis-Chandrasekhar-Fermi method, corresponding to a mass-to-flux criticality of ∼1.3 ± 0.4 and an Alfvenic Mach number of <0.6. These results suggest that gravity and magnetic field are currently of comparable importance in the HFS and that turbulence is less important.

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

Journal keyword(s): ISM: individual objects: IC 5146 - ISM: magnetic fields - ISM: structure - polarization - radio continuum: ISM - stars: formation

Status in Simbad:  being processed

Simbad objects: 11

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2019.12.16-06:06:33

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