2015A&A...578A.102S


Query : 2015A&A...578A.102S

2015A&A...578A.102S - Astronomy and Astrophysics, volume 578A, 102-102 (2015/6-1)

EVN observations of 6.7 GHz methanol maser polarization in massive star-forming regions. III. The flux-limited sample.

SURCIS G., VLEMMINGS W.H.T., VAN LANGEVELDE H.J., HUTAWARAKORN KRAMER B., BARTKIEWICZ A. and BLASI M.G.

Abstract (from CDS):

Theoretical simulations and observations at different angular resolutions have shown that magnetic fields have a central role in massive star formation. Like in low-mass star formation, the magnetic field in massive young stellar objects can either be oriented along the outflow axis or randomly. Measuring the magnetic field at milliarcsecond resolution (10-100au) around a substantial number of massive young stellar objects permits determining with a high statistical significance whether the direction of the magnetic field is correlated with the orientation of the outflow axis or not. In late 2012, we started a large VLBI campaign with the European VLBI Network to measure the linearly and circularly polarized emission of 6.7GHz CH3OH masers around a sample of massive star-forming regions. This paper focuses on the first seven observed sources, G24.78+0.08, G25.65+1.05, G29.86-0.04, G35.03+0.35, G37.43+1.51, G174.20-0.08, and G213.70-12.6. For all these sources, molecular outflows have been detected in the past. We detected a total of 176 CH3OH masing cloudlets toward the seven massive star-forming regions, 19% of which show linearly polarized emission. The CH3OH masers around the massive young stellar object MM1 in G174.20-0.08 show neither linearly nor circularly polarized emission. The linear polarization vectors are well ordered in all the other massive young stellar objects. We measured significant Zeeman splitting toward both A1 and A2 in G24.78+0.08, and toward G29.86-0.04 and G213.70-12.6. By considering all the 19 massive young stellar objects reported in the literature for which both the orientation of the magnetic field at milliarcsecond resolution and the orientation of outflow axes are known, we find evidence that the magnetic field (on scales 10-100au) is preferentially oriented along the outflow axes.

Abstract Copyright:

Journal keyword(s): stars: formation - masers - polarization - magnetic fields

VizieR on-line data: <Available at CDS (J/A+A/578/A102): table1.dat tablea1.dat tablea2.dat tablea3.dat tablea4.dat tablea5.dat tablea6.dat tablea7.dat>

Simbad objects: 50

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Number of rows : 50
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 NAME W 3 OH HII 02 27 04.1 +61 52 22           ~ 987 2
2 GAL 174.20-00.08 Cld 05 30 45.9 +33 47 56           ~ 195 2
3 [ZHB2007] MM-5 mm 05 30 47.89 +33 47 51.8           ~ 4 0
4 [PFG2013] A5142-MM3 mm 05 30 47.953 +33 47 52.57           ~ 6 0
5 [PFG2013] A5142-MM2 mm 05 30 48.024 +33 47 53.67           ~ 13 0
6 [PFG2013] A5142-MM1 mm 05 30 48.031 +33 47 54.64           ~ 16 0
7 [ZHB2007] MM-4 mm 05 30 48.193 +33 47 54.62           ~ 4 0
8 SH 2-231 HII 05 39 12.9 +35 45 54           ~ 124 0
9 7C 055201.39+394824.00 QSO 05 55 30.8055972888 +39 48 49.166341920     18.0 17.5   ~ 487 2
10 2MASS J06074564-0623329 Y*O 06 07 45.6405107232 -06 23 32.943013116           ~ 12 0
11 NAME Mon R2 HII 06 07 47.58 -06 22 42.6           ~ 699 2
12 NAME Mon R2 IRS 3 Y*O 06 07 47.8 -06 22 55           ~ 139 0
13 NAME AFGL 5180 IRS 1 IR 06 08 53.4 +21 38 29           ~ 11 0
14 NAME S255-2 IR 06 12 53.8 +17 59 22           ~ 42 0
15 MMB G291.274-00.709 Mas 11 11 53.35 -61 18 23.7           ~ 16 0
16 OH 305.21 +0.21 Mas 13 11 13.7017 -62 34 41.397           ~ 24 1
17 MMB G309.921+00.479 cor 13 50 41.78 -61 35 10.2           ~ 47 1
18 MMB G316.640-00.087 cor 14 44 18.45 -59 55 11.5           ~ 26 0
19 OH 335.79 +0.17 cor 16 29 47.3096249808 -48 15 52.204363524           ~ 56 0
20 OH 339.88 -1.26 Y*O 16 52 04.6776 -46 08 34.404           ~ 72 0
21 OH 345.01 +1.79 Mas 16 56 47.58 -40 14 25.8           ~ 70 0
22 NGC 6334 HII 17 20 51 -36 06.9           ~ 642 0
23 NAME NGC 6334F (NW) HII 17 20 53.18 -35 46 59.3           ~ 7 0
24 NAME NGC 6334F (C) HII 17 20 53.45 -35 47 02.6           ~ 218 1
25 RAFGL 7009S HII 18 34 20.911 -05 59 42.23           ~ 203 0
26 GAL 024.78+00.08 HII 18 36.2 -07 13           ~ 80 0
27 [FCC2002] A2b Y*O 18 36 12.404 -07 12 08.50           ~ 5 0
28 [FCC2002] A2 Y*O 18 36 12.5 -07 12 10           ~ 19 0
29 [FCC2002] A1b Y*O 18 36 12.592 -07 12 11.00           ~ 6 0
30 [FCC2002] A1 HII 18 36 12.6 -07 12 11           ~ 32 0
31 [FCC2002] A1c Y*O 18 36 12.606 -07 12 12.00           ~ 6 0
32 [HBM2005] G29.86-0.04 mm 18 46 00.2 -02 45 09           ~ 9 0
33 [CBH2011c] EGO G35.03+0.35 -CM1 Rad 18 54 00.49098 +02 01 18.2920           ~ 9 0
34 [CBH2011c] EGO G35.03+0.35 -CM4 Rad 18 54 00.523 +02 01 15.60           ~ 6 0
35 [CBH2011c] EGO G35.03+0.35 -CM2 Rad 18 54 00.6498 +02 01 19.320           ~ 10 0
36 [CBH2011c] EGO G35.03+0.35 -CM3 Rad 18 54 00.766 +02 01 22.82           ~ 7 0
37 GAL 035.03+00.35 HII 18 54 01.0 +02 01 32           ~ 43 0
38 IRAS 18517+0437 SFR 18 54 13.8 +04 41 32           ~ 67 0
39 IRAS 18556+0136 mul 18 58 13.1 +01 40 35           ~ 136 0
40 SNR G035.2-01.8 SNR 19 01.6 +01 14           ~ 152 0
41 W 51e2 HII 19 23 43.906 +14 30 34.48           ~ 200 0
42 W 51 SNR 19 23 50 +14 06.0           ~ 1219 1
43 IRAS 20126+4104 Y*O 20 14 25.8816769656 +41 13 36.879427236           B2.5-B0.5 416 0
44 [DSM98] W75N A ? 20 38 26.2 +42 36 32           ~ 3 0
45 NAME Cyg X FIR 33 Y*O 20 38 35.9 +42 37 22           B1.5 379 1
46 NAME BL Lac BLL 22 02 43.2913536816 +42 16 39.979416792   15.66 14.72     ~ 2137 1
47 IRAS 22272+6358A Cld 22 28 52.2 +64 13 43           ~ 51 0
48 NAME Cepheus A SFR 22 56 17.9 +62 01 49           ~ 719 2
49 NGC 7538 OpC 23 13 37 +61 30.0           ~ 852 1
50 [WBN74] NGC 7538 IRS 1 Y*O 23 13 45.318 +61 28 11.69           ~ 395 3

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2022.08.10-19:19:24

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