2019A&A...623A.130S

Query : 2019A&A...623A.130S

2019A&A...623A.130S - Astronomy and Astrophysics, volume 623A, 130-130 (2019/3-1)

EVN observations of 6.7 GHz methanol maser polarization in massive star-forming regions. IV. Magnetic field strength limits and structure for seven additional sources.

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

Abstract (from CDS):


Context. Magnetohydrodynamical simulations show that the magnetic field can drive molecular outflows during the formation of massive protostars. The best probe to observationally measure both the morphology and the strength of this magnetic field at scales of 10-100 au is maser polarization.
Aims. We measure the direction of magnetic fields at milliarcsecond resolution around a sample of massive star-forming regions to determine whether there is a relation between the orientation of the magnetic field and of the outflows. In addition, by estimating the magnetic field strength via the Zeeman splitting measurements, the role of magnetic field in the dynamics of the massive star-forming region is investigated.
Methods. We selected a flux-limited sample of 31 massive star-forming regions to perform a statistical analysis of the magnetic field properties with respect to the molecular outflows characteristics. We report the linearly and circularly polarized emission of 6.7GHz CH3OH masers towards seven massive star-forming regions of the total sample with the European VLBI Network. The sources are: G23.44-0.18, G25.83-0.18, G25.71-0.04, G28.31-0.39, G28.83-0.25, G29.96-0.02, and G43.80-0.13.
Results. We identified a total of 219 CH3OH maser features, 47 and 2 of which showed linearly and circularly polarized emission, respectively. We measured well-ordered linear polarization vectors around all the massive young stellar objects and Zeeman splitting towards G25.71-0.04 and G28.83-0.25. Thanks to recent theoretical results, we were able to provide lower limits to the magnetic field strength from our Zeeman splitting measurements.
Conclusions. We further confirm (based on ∼80% of the total flux-limited sample) that the magnetic field on scales of 10-100 au is preferentially oriented along the outflow axes. The estimated magnetic field strength of |B|||>61mG and >21mG towards G25.71-0.04 and G28.83-0.25, respectively, indicates that it dominates the dynamics of the gas in both regions.

Abstract Copyright: © ESO 2019

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

VizieR on-line data: <Available at CDS (J/A+A/623/A130): 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 - 2024 		#notes
1 NAME W 3 OH HII 02 27 04.1 +61 52 22           ~ 1028 2
2 GAL 174.20-00.08 Cld 05 30 45.9 +33 47 56           ~ 205 2
3 SH 2-231 Y*O 05 39 13.2 +35 45 48           ~ 132 0
4 NAME Mon R2 HII 06 07 47.58 -06 22 42.6           ~ 742 2
5 NAME Mon R2 IRS 3 Y*O 06 07 47.8 -06 22 55           ~ 142 0
6 [HMW2016] G213.704-12.59 Mas 06 07 47.8584 -06 22 56.586           ~ 6 0
7 NAME AFGL 5180 IRS 1 IR 06 08 53.4 +21 38 29           ~ 11 0
8 RAFGL 5180 SFR 06 08 54.1 +21 38 25           ~ 119 0
9 NAME S255-2 IR 06 12 53.8 +17 59 22           ~ 46 0
10 MMB G291.274-00.709 Mas 11 11 53.35 -61 18 23.7           ~ 16 0
11 [WB2006] G305A Mas 13 11 14.4 -62 34 26           ~ 19 1
12 3C 286 Sy1 13 31 08.2883506368 +30 30 32.960091564   17.51 17.25     ~ 4341 2
13 OH 309.92+00.48 Mas 13 50 41.78 -61 35 10.2           ~ 50 0
14 OH 316.64-00.09 Mas 14 44 18.45 -59 55 11.5           ~ 32 0
15 NAME Nor Arm PoG 16 00 -50.0           ~ 430 0
16 OH 335.79+00.17 Mas 16 29 47.309 -48 15 51.77           ~ 42 0
17 IRAS 16533-4009 HII 16 56 45.58 -40 14 32.4           ~ 47 0
18 NAME NGC 6334F (NW) HII 17 20 53.18 -35 46 59.3           ~ 7 0
19 NAME NGC 6334F (C) HII 17 20 53.45 -35 47 02.6           ~ 230 1
20 RAFGL 7009S HII 18 34 20.911 -05 59 42.23           ~ 214 0
21 [RLW2011] MM1 mm 18 34 39.18 -08 31 46.2           ~ 4 0
22 [RLW2011] MM2 mm 18 34 39.18 -08 31 33.2           ~ 5 0
23 GAL 023.44-00.18 HII 18 34 43.6 -08 32 25           ~ 52 0
24 GAL 024.78+00.08 HII 18 36.2 -07 13           ~ 82 0
25 OH 025.709+00.044 Mas 18 38 03.1450 -06 24 15.190           ~ 17 0
26 GAL 025.83-00.18 ? 18 39 03.6 -06 24 11           ~ 6 0
27 [THW2006] G028.29-00.36 a smm 18 44 22.2 -04 17 39           ~ 8 0
28 [L89b] 28.823-00.226 bub 18 44 44.3 -03 45 34           ~ 78 0
29 Caswell OH 028.83-00.25 Mas 18 44 50.63 -03 46 03.8           ~ 29 0
30 [CBH2011c] EGO G28.83-0.25 -CM1 Rad 18 44 50.737 -03 45 49.26           ~ 3 0
31 [CBH2011c] EGO G28.83-0.25 -CM2 Rad 18 44 51.08 -03 45 48.3           ~ 3 0
32 EGO G028.83-0.25 of? 18 44 51.3 -03 45 48           ~ 18 0
33 [HBM2005] G29.86-0.04 mm 18 46 00.2 -02 45 09           ~ 9 0
34 CORNISH G029.9559-00.0168 Y*O 18 46 04.18 -02 39 21.3           ~ 365 0
35 W 43s Rad 18 47 41.68 -02 00 24.3           ~ 26 0
36 GAL 035.03+00.35 cor 18 54 00.60 +02 01 19.3           ~ 47 0
37 IRAS 18517+0437 SFR 18 54 13.8 +04 41 32           ~ 74 0
38 IRAS 18556+0136 mul 18 58 13.1 +01 40 35           ~ 139 0
39 SNR G035.2-01.8 SNR 19 01.6 +01 14           ~ 154 0
40 IRAS 19095+0930 cor 19 11 54.09216 +09 35 49.6896           ~ 101 0
41 NAME W 51 IRS 1 HII 19 23 41.9 +14 30 36           ~ 113 0
42 W 51e2 PCG 19 23 43.906 +14 30 34.48           ~ 211 0
43 W 51 SNR 19 23 50 +14 06.0           ~ 1278 1
44 IRAS 20126+4104 Y*O 20 14 25.8816769656 +41 13 36.879427236           B2.5-B0.5 441 0
45 NAME W75N(B) cor 20 38 36.44 +42 37 34.1           ~ 47 0
46 NAME BL Lac BLL 22 02 43.2913536816 +42 16 39.979416792   15.66 14.72     ~ 2259 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           ~ 741 2
49 NGC 7538 OpC 23 13 37 +61 30.0           ~ 881 1
50 [WBN74] NGC 7538 IRS 1 Y*O 23 13 45.318 +61 28 11.69           ~ 414 3

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