2021ApJ...907...33Y

Query : 2021ApJ...907...33Y

2021ApJ...907...33Y - Astrophys. J., 907, 33-33 (2021/January-3)

The JCMT BISTRO survey: alignment between outflows and magnetic fields in dense Cores/Clumps.

YEN H.-W., KOCH P.M., HULL C.L.H., WARD-THOMPSON D., BASTIEN P., HASEGAWA T., KWON W., LAI S.-P., QIU K., CHING T.-C., CHUNG E.J., COUDE S., DI FRANCESCO J., DIEP P.N., DOI Y., ESWARAIAH C., FALLE S., FULLER G., FURUYA R.S., HAN I., HATCHELL J., HOUDE M., INUTSUKA S.-I., JOHNSTONE D., KANG J.-H., KANG M., KIM K.-T., KIRCHSCHLAGER F., KWON J., LEE C.W., LEE C.-F., LIU H.-L., LIU T., LYO A.-R., OHASHI N., ONAKA T., PATTLE K., SADAVOY S., SAITO H., SHINNAGA H., SOAM A., TAHANI M., TAMURA M., TANG Y.-W., TANG X. and ZHANG C.-P.

Abstract (from CDS):

We compare the directions of molecular outflows of 62 low-mass Class 0 and I protostars in nearby (<450 pc) star-forming regions with the mean orientations of the magnetic fields on 0.05-0.5 pc scales in the dense cores/clumps where they are embedded. The magnetic field orientations were measured using the JCMT POL-2 data taken by the BISTRO-1 survey and from the archive. The outflow directions were observed with interferometers in the literature. The observed distribution of the angles between the outflows and the magnetic fields peaks between 15° and 35°. After considering projection effects, our results could suggest that the outflows tend to be misaligned with the magnetic fields by 50° ± 15° in three-dimensional space and are less likely (but not ruled out) randomly oriented with respect to the magnetic fields. There is no correlation between the misalignment and the bolometric temperatures in our sample. In several sources, the small-scale (1000-3000 au) magnetic field is more misaligned with the outflow than the large-scale magnetic field, suggesting that the small-scale magnetic field has been twisted by the dynamics. In comparison with turbulent MHD simulations of core formation, our observational results are more consistent with models in which the energy densities in the magnetic field and the turbulence of the gas are comparable. Our results also suggest that the misalignment alone cannot sufficiently reduce the efficiency of magnetic braking to enable formation of the observed number of large Keplerian disks with sizes larger than 30-50 au.

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

Journal keyword(s): Star formation - Star forming regions - Protostars - Interstellar magnetic fields

Simbad objects: 78

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Number of rows : 78
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 LDN 1448 DNe 03 22.5 +30 35           ~ 515 0
2 IRAS 03222+3034 Y*O 03 25 22.32 +30 45 13.9           ~ 149 0
3 JCMTSE J032525.9+304502 Y*O 03 25 25.9 +30 45 03           ~ 53 0
4 JCMTSE J032536.1+304514 Y*O 03 25 36.22 +30 45 15.7           ~ 126 0
5 IRAS F03226+3033 Y*O 03 25 38.83 +30 44 06.2           ~ 335 0
6 SSTc2d J032539.1+304358 Y*? 03 25 39.12 +30 43 58.2           ~ 48 1
7 NAME LDN 1455 IRS 1 cor 03 27 39.08 +30 13 03.1           ~ 161 0
8 NAME LDN 1455 IRS 4 cor 03 27 43.23 +30 12 28.9           ~ 74 0
9 LDN 1455 DNe 03 28 00.6480 +30 07 58.800           ~ 186 1
10 [TLL2016] Per-emb-35-A Rad 03 28 37.0910 +31 13 30.788           ~ 10 0
11 [TLL2016] Per-emb-35-B Rad 03 28 37.2190 +31 13 31.751           ~ 8 0
12 [JCC87] IRAS 2A Y*O 03 28 55.55 +31 14 36.7           ~ 459 3
13 BD+30 547 Y*O 03 28 57.2114503248 +31 14 19.076151444   10.73 9.98 9.1   G4V 108 1
14 2MASS J03285842+3122175 Y*O 03 28 58.420 +31 22 17.54           ~ 38 0
15 [SK2001] 1 Y*O 03 29 00.55 +31 12 00.8           ~ 58 1
16 NAME HH 7-11 MMS 3 smm 03 29 01.964 +31 15 38.04           ~ 64 0
17 NAME HH 7-11 MMS 2 smm 03 29 03.056 +31 15 51.67           ~ 86 0
18 [HSW2018] NGC 1333-17 smm 03 29 03.73 +31 16 03.8           ~ 99 0
19 [LAL96] 213 Y*O 03 29 07.739 +31 21 57.52           ~ 62 0
20 [JCC87] IRAS 4A Y*O 03 29 10.49 +31 13 30.8           ~ 715 1
21 [JJK2007] 23 Y*O 03 29 10.68 +31 18 20.6           ~ 57 1
22 NGC 1333 OpC 03 29 11.3 +31 18 36           ~ 1450 1
23 [KJD2006] SMM J032917+31184 Y*O 03 29 11.3 +31 18 25           ~ 61 0
24 [JCC87] IRAS 4B Y*O 03 29 12.058 +31 13 02.05           ~ 600 0
25 NAME IRAS 4B1 South Y*O 03 29 12.06 +31 13 01.7           ~ 36 1
26 NAME IRAS 4B1 North Y*O 03 29 12.06 +31 13 05.4           ~ 14 0
27 [JCC87] IRAS 4B2 smm 03 29 12.8 +31 13 02           ~ 19 0
28 2MASS J03291294+3118146 Y*O 03 29 12.945 +31 18 14.61           ~ 39 1
29 SSTc2d J032918.3+312320 Y*O 03 29 18.26 +31 23 19.9           ~ 24 1
30 [SDA2014] West50 Y*O 03 33 14.38 +31 07 10.9           ~ 32 1
31 Barnard 1 MoC 03 33 16.3 +31 07 51           ~ 324 0
32 [EES2009] Per-emb 10 Y*O 03 33 16.45 +31 06 52.5           ~ 19 1
33 2MASS J03331667+3107548 Y*O 03 33 16.68 +31 07 54.9           ~ 125 2
34 JCMTSE J033317.8+310932 cor 03 33 17.85 +31 09 31.9           ~ 113 0
35 [HKM99] B1-b cor 03 33 20.32 +31 07 21.5           ~ 212 0
36 [HRF2005] 3 PoC 03 33 21.3 +31 07 27           ~ 77 0
37 [KJD2006] SMM J033335+31075 PoC 03 33 21.3 +31 07 28           ~ 105 0
38 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1364 0
39 Cl* IC 348 LRL 54362 Y*O 03 43 50.96 +32 03 24.7           ~ 39 1
40 [RZP2014] JVLA 1 Y*O 03 43 51.02 +32 03 08.1           ~ 40 2
41 HH 211 Y*O 03 43 56.52 +32 00 52.8           ~ 368 0
42 NAME HH 211-mm Y*O 03 43 56.816 +32 00 50.06           ~ 63 1
43 [TLL2016] Per-emb-11-A Rad 03 43 57.0650 +32 03 04.788           ~ 7 0
44 [TLL2016] Per-emb-11-C Rad 03 43 57.6880 +32 03 09.975           ~ 7 0
45 IRAS 03410+3152 Y*O 03 44 12.980 +32 01 35.50           ~ 56 0
46 IC 348 OpC 03 44 31.7 +32 09 32           ~ 1392 1
47 Barnard 211 DNe 04 17 35 +27 43.1           ~ 127 0
48 IRAS 04166+2706 Y*O 04 19 42.62736 +27 13 38.4312           ~ 135 0
49 IRAS 04169+2702 Y*O 04 19 58.44936 +27 09 57.0672           K0-M4 117 1
50 NAME Auriga reg 04 20 00.0 +38 05 00           ~ 207 0
51 Barnard 213 DNe 04 20 51 +27 16.3           ~ 217 0
52 LDN 1521F DNe 04 28 39.3 +26 51 43           ~ 210 1
53 LDN 1527 DNe 04 39 53 +25 45.0           ~ 634 0
54 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4415 0
55 HH 212 HH 05 43 51.41 -01 02 53.1           ~ 391 1
56 HH 111 HH 05 51 44.2 +02 48 34           ~ 411 0
57 [CHG85] GSS 30 IRS 3 Y*O 16 26 21.77376 -24 22 51.3948           ~ 66 0
58 GBS-VLA J162626.39-242430.9 Y*O 16 26 26.39 -24 24 30.8           ~ 30 0
59 NAME rho Oph A Cloud MoC 16 26 26.4 -24 22 33           ~ 289 1
60 NAME rho Oph B Cloud MoC 16 27 11 -24 28.5           ~ 84 1
61 Elia 2-32 Y*O 16 27 28.44576 -24 27 21.0348           K6.5 113 1
62 Elia 2-33 Y*O 16 27 30.18024 -24 27 43.3656           M2 117 1
63 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3629 1
64 NAME Serpens Main Cloud MoC 18 29.2 +00 36           ~ 25 0
65 SH 2-68 N Y*O 18 29 48.09 +01 16 45.0           ~ 137 1
66 [WM2000] S68Nc PoC 18 29 48.710 +01 16 57.00           ~ 8 0
67 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 1100 2
68 2MASS J18294960+0117058 Y*O 18 29 49.602 +01 17 05.83           ~ 34 0
69 NAME Serpens SMM 1b mm 18 29 49.69 +01 15 21.2           ~ 10 0
70 NAME Serpens SMM 1a mm 18 29 49.80 +01 15 20.6           ~ 18 0
71 NAME Serpens SMM 1d mm 18 29 49.990 +01 15 22.97           ~ 5 0
72 [AHA2018] Serpens SMM4B Y*O 18 29 56.50 +01 13 11.0           ~ 7 0
73 [AHA2018] Serpens SMM4A Y*O 18 29 56.70 +01 13 15.0           ~ 11 0
74 NAME Serpens SMM 11 smm 18 30 00.3 +01 11 42           ~ 24 0
75 AGAL G030.818-00.056 cor 18 47 47.0 -01 54 28           ~ 164 0
76 LDN 663 DNe 19 36 55 +07 34.4           ~ 645 0
77 LDN 1157 DNe 20 39 06.4 +68 02 13           ~ 572 0
78 NAME Gould Belt PoG ~ ~           ~ 873 1

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