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2018ApJ...859....4K - Astrophys. J., 859, 4-4 (2018/May-3)

A first look at BISTRO observations of the ρ Oph-A core.

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

Abstract (from CDS):

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, B-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.

Abstract Copyright: © 2018. The American Astronomical Society. All rights reserved.

Journal keyword(s): circumstellar matter - ISM: individual objects: Ophiuchi - ISM: structure - polarization - radio continuum: ISM - stars: formation

VizieR on-line data: <Available at CDS (J/ApJ/859/4): table1.dat>

Simbad objects: 23

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2020.01.19-12:25:52

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