2020ApJ...899...28D

Query : 2020ApJ...899...28D

2020ApJ...899...28D - Astrophys. J., 899, 28-28 (2020/August-2)

The JCMT BISTRO survey: magnetic fields associated with a network of filaments in NGC 1333.

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

Abstract (from CDS):

We present new observations of the active star formation region NGC 1333 in the Perseus molecular cloud complex from the James Clerk Maxwell Telescope B-Fields In Star-forming Region Observations (BISTRO) survey with the POL-2 instrument. The BISTRO data cover the entire NGC 1333 complex (∼1.5 pc x 2 pc) at 0.02 pc resolution and spatially resolve the polarized emission from individual filamentary structures for the first time. The inferred magnetic field structure is complex as a whole, with each individual filament aligned at different position angles relative to the local field orientation. We combine the BISTRO data with low- and high- resolution data derived from Planck and interferometers to study the multiscale magnetic field structure in this region. The magnetic field morphology drastically changes below a scale of ∼1 pc and remains continuous from the scales of filaments (∼0.1 pc) to that of protostellar envelopes (∼0.005 pc or ∼1000 au). Finally, we construct simple models in which we assume that the magnetic field is always perpendicular to the long axis of the filaments. We demonstrate that the observed variation of the relative orientation between the filament axes and the magnetic field angles are well reproduced by this model, taking into account the projection effects of the magnetic field and filaments relative to the plane of the sky. These projection effects may explain the apparent complexity of the magnetic field structure observed at the resolution of BISTRO data toward the filament network.

Abstract Copyright: © 2020. The American Astronomical Society. All rights reserved.

Journal keyword(s): Interstellar medium - Interstellar magnetic fields - Interstellar filaments - Star formation - Polarimetry - Submillimeter astronomy

Errata: erratum vol. 911, art. 72 (2021)

Simbad objects: 28

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Number of rows : 28
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 SK 1 sg* 00 35 05.4488739024 -74 09 04.137185700 12.82 12.72 12.49   12.38 A0I 27 0
2 BD+30 459 * 02 53 45.1196480472 +31 01 47.380322064   10.80 9.79     F5 4 0
3 [HFR2007] 55 cor 03 28 40.63 +31 17 56.5           ~ 40 1
4 IRAS 03258+3104 Y*O 03 28 55.30 +31 14 27.8           ~ 173 1
5 [JCC87] IRAS 2A Y*O 03 28 55.55 +31 14 36.7           ~ 513 3
6 HH 12 HH 03 28 59.4 +31 20 11           ~ 119 1
7 NAME HH 7-11 MMS 3 smm 03 29 01.964 +31 15 38.04           ~ 69 0
8 NAME HH 7-11 MMS 2 smm 03 29 03.056 +31 15 51.67           ~ 95 0
9 [HSW2018] NGC 1333-17 smm 03 29 03.73 +31 16 03.8           ~ 131 0
10 V* V512 Per Or* 03 29 03.7578170808 +31 16 03.947525688           M3.5 419 0
11 NGC 1333 OpC 03 29 09.2 +31 20 59           ~ 1575 1
12 LZK 12 Or* 03 29 10.393560 +31 21 59.19408   15.814 14.497 14.636   B5:V+F2: 147 0
13 [JCC87] IRAS 4A Y*O 03 29 10.49 +31 13 30.8           ~ 770 1
14 [JCC87] IRAS 4 FIR 03 29 10.9 +31 13 26           ~ 489 0
15 [KJD2006] SMM J032917+31184 Y*O 03 29 11.3 +31 18 25           ~ 64 0
16 [JCC87] IRAS 4B Y*O 03 29 12.058 +31 13 02.05           ~ 625 0
17 [JCC87] IRAS 4C Y*O 03 29 13.54 +31 13 58.2           ~ 122 1
18 Barnard 1 MoC 03 33 16.3 +31 07 51           ~ 350 0
19 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1553 0
20 NAME Per Region reg 03 37 00.0 +31 15 00           ~ 296 0
21 Ass Per OB 2 As* 03 42.2 +33 26           ~ 350 0
22 NAME Ori A MoC 05 38 -07.1           ~ 3187 0
23 NAME rho Oph A Cloud MoC 16 26 26.4 -24 22 33           ~ 312 1
24 NAME rho Oph C Cloud MoC 16 26 53.1 -24 32 31           ~ 80 0
25 NAME rho Oph B Cloud MoC 16 27 11 -24 28.5           ~ 88 1
26 M 16 OpC 18 18 45.1 -13 47 31           ~ 1084 1
27 IC 5146 OpC 21 53 29.3 +47 14 46           ~ 507 2
28 NAME Gould Belt PoG ~ ~           ~ 956 1

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