2021ApJ...908...10N

Query : 2021ApJ...908...10N

2021ApJ...908...10N - Astrophys. J., 908, 10-10 (2021/February-2)

Observations of magnetic fields surrounding LkHα 101 taken by the BISTRO survey with JCMT-POL-2.

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

Abstract (from CDS):

We report the first high spatial resolution measurement of magnetic fields surrounding LkHα 101, part of the Auriga-California molecular cloud. The observations were taken with the POL-2 polarimeter on the James Clerk Maxwell Telescope within the framework of the B-fields In Star-forming Region Observations (BISTRO) survey. Observed polarization of thermal dust emission at 850 µm is found to be mostly associated with the redshifted gas component of the cloud. The magnetic field displays a relatively complex morphology. Two variants of the Davis-Chandrasekhar-Fermi method, unsharp masking and structure function, are used to calculate the strength of magnetic fields in the plane of the sky, yielding a similar result of BPOS ∼ 115 µG. The mass-to-magnetic-flux ratio in critical value units, λ ∼ 0.3, is the smallest among the values obtained for other regions surveyed by POL-2. This implies that the LkHα 101 region is subcritical, and the magnetic field is strong enough to prevent gravitational collapse. The inferred δB/B0 ∼ 0.3 implies that the large-scale component of the magnetic field dominates the turbulent one. The variation of the polarization fraction with total emission intensity can be fitted by a power law with an index of α = 0.82 ± 0.03, which lies in the range previously reported for molecular clouds. We find that the polarization fraction decreases rapidly with proximity to the only early B star (LkHα 101) in the region. Magnetic field tangling and the joint effect of grain alignment and rotational disruption by radiative torques can potentially explain such a decreasing trend.

Abstract Copyright: © 2021. The American Astronomical Society. All rights reserved.

Journal keyword(s): Interstellar magnetic fields - Molecular clouds - Star formation

Simbad objects: 33

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Number of rows : 33
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 NGC 1333 OpC 03 29 11.3 +31 18 36           ~ 1450 1
2 Barnard 1 MoC 03 33 16.3 +31 07 51           ~ 324 0
3 NAME California Molecular Cloud MoC 04 10.0 +39 00           ~ 156 1
4 Barnard 211 DNe 04 17 35 +27 43.1           ~ 127 0
5 LDN 1495 DNe 04 18.1 +27 37           ~ 366 1
6 NAME Auriga reg 04 20 00.0 +38 05 00           ~ 207 0
7 Barnard 213 DNe 04 20 51 +27 16.3           ~ 217 0
8 LDN 1482 DNe 04 28.3 +35 37           ~ 27 0
9 NGC 1579 OpC 04 30 03.4 +35 19 30           ~ 86 1
10 EM* LkHA 101 Em* 04 30 14.4355820328 +35 16 23.983198932   17.91 15.71 13.33   F 356 1
11 NAME Ori A MoC 05 38 -07.1           ~ 3011 0
12 NAME Ori B MoC 05 41 43.0 -01 54 44           ~ 1376 0
13 NAME Orion Molecular Cloud MoC 05 56 -01.8           ~ 1098 1
14 NAME Mon R2 HII 06 07 47.58 -06 22 42.6           ~ 742 2
15 NAME Rosette Molecular Cloud MoC 06 34.7 +04 02           ~ 262 0
16 NGC 2264 OpC 06 40 52.1 +09 52 37           ~ 1793 0
17 NAME rho Oph A Cloud MoC 16 26 26.4 -24 22 33           ~ 289 1
18 NAME VLA 1623-243 Y*O 16 26 26.42 -24 24 30.0           ~ 404 0
19 NAME rho Oph C Cloud MoC 16 26 53.1 -24 32 31           ~ 77 0
20 NAME rho Oph B Cloud MoC 16 27 11 -24 28.5           ~ 84 1
21 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3629 1
22 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 1252 1
23 LDN 1689B DNe 16 34 42.1 -24 36 11           ~ 167 0
24 NGC 6334 HII 17 20 53 -36 07.9           ~ 682 0
25 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 14407 0
26 M 16 OpC 18 18 45.1 -13 47 31           ~ 1028 1
27 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 1100 2
28 GCNM 23 Y*O 18 29 49.63 +01 15 21.9           ~ 273 2
29 NAME Aql Region reg 18 31.1 -02 10           ~ 391 0
30 18P 59 HII 20 32 31.2 +40 16 35           ~ 71 0
31 DR 21 SFR 20 39 01.6 +42 19 38           O4.5 1054 0
32 IC 5146 OpC 21 53 29.3 +47 14 46           ~ 466 2
33 NAME Gould Belt PoG ~ ~           ~ 873 1

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