2013A&A...556A..73S


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.21CEST03:13:45

2013A&A...556A..73S - Astronomy and Astrophysics, volume 556A, 73-73 (2013/8-1)

EVN observations of 6.7 GHz methanol maser polarization in massive star-forming regions. II. First statistical results.

SURCIS G., VLEMMINGS W.H.T., VAN LANGEVELDE H.J., HUTAWARAKORN KRAMER B. and QUIROGA-NUNEZ L.H.

Abstract (from CDS):

Magnetic fields have only recently been included in theoretical simulations of high-mass star formation. The simulations show that magnetic fields play an important role in the formation and dynamics of molecular outflows. Masers, in particular 6.7-GHz CH3OH masers, are the best probes of the magnetic field morphologies around massive young stellar objects on the smallest scales of 10-100AU. Providing new observational measurements of the morphology of magnetic fields around massive young stellar objects by using 6.7-GHz CH3OH maser emission is very important for setting constraints on the numerical simulations of massive star formation. This paper focuses on 4 massive young stellar objects, IRAS06058+2138-NIRS 1, IRAS22272+6358A, S255-IR, and S231, which complement our previous 2012 sample (the first EVN group). From all these sources, molecular outflows have been detected in the past. Seven of the European VLBI Network antennas were used to measure the linear polarization and Zeeman-splitting of the 6.7-GHz CH3OH masers in the star-forming regions in this second EVN group. We detected a total of 128 CH3OH masing cloudlets. Fractional linear polarization (0.8%-11.3%) was detected towards 18% of the CH3OH masers in our sample. The linear polarization vectors are well ordered in all the massive young stellar objects. We measured significant Zeeman-splitting in IRAS06058+2138-NIRS 1 (ΔVZ=3.8±0.6m/s) and S255-IR (ΔVZ=3.2±0.7m/s). By considering the 20 massive young stellar objects towards which the morphology of magnetic fields was determined by observing 6.7-GHz CH3OH masers in both hemispheres, we find no evident correlation between the linear distributions of CH3OH masers and the outflows or the linear polarization vectors. On the other hand, we present first statistical evidence that the magnetic field (on scales 10-100AU) is primarily oriented along the large-scale outflow direction. Moreover, we empirically find that the linear polarization fraction of unsaturated CH3OH masers is Pl<4.5%.

Abstract Copyright:

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

Simbad objects: 41

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Number of rows : 41

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 NAME W 3 OH HII 02 27 04.1 +61 52 22           ~ 928 2
2 4C 50.11 QSO 03 59 29.74726473 +50 57 50.1615765           ~ 388 1
3 SH 2-233 HII 05 38 31.5 +35 51 19           ~ 58 1
4 IRAS 05358+3543 mul 05 39 10.4 +35 45 19           ~ 131 1
5 SH 2-231 HII 05 39 12.9 +35 45 54           ~ 115 0
6 SH 2-235 HII 05 41.1 +35 50           ~ 181 0
7 [MBH2005] G188.95+0.89 MM 1 Cld 06 08 52.8 +21 38 37           ~ 7 0
8 [SSM2006] IRAS 06058+2138 MCS B mm 06 08 53.34 +21 38 29.5           ~ 2 0
9 NAME AFGL 5180 IRS 1 IR 06 08 53.4 +21 38 29           ~ 9 0
10 RAFGL 5180 SFR 06 08 54.1 +21 38 25           ~ 108 0
11 NGC 2175 OpC 06 09 39 +20 29.2   7.0 6.8     ~ 245 3
12 SH 2-257 HII 06 12 44 +17 59.3           ~ 119 1
13 [MBH2005] G192.60-0.05 MM 2 Cld 06 12 53.4 +17 59 23           ~ 5 0
14 [WBB2011] S255IR-SMA2 mm 06 12 53.77 +17 59 26.1           ~ 7 0
15 NAME SH 2-255 IRS 1 Y*O 06 12 54.0060 +17 59 22.958           ~ 310 0
16 [MBH2005] G192.60-0.05 MM 3 Cld 06 12 56.8 +17 58 03           ~ 3 0
17 IC 2162 HII 06 13 04.1 +17 58 44           ~ 333 2
18 ICRF J092703.0+390220 Sy1 09 27 03.0139516273 +39 02 20.847968628   17.17 17.00 16.486   ~ 920 1
19 MMB G291.274-00.709 Mas 11 11 53.35 -61 18 23.7           ~ 14 0
20 OH 305.21 +0.21 Mas 13 11 13.7017 -62 34 41.397           ~ 24 1
21 MMB G309.921+00.479 cor 13 50 41.78 -61 35 10.2           ~ 42 1
22 MMB G316.640-00.087 cor 14 44 18.45 -59 55 11.5           ~ 19 0
23 OH 335.79 +0.17 cor 16 29 47.3094168743 -48 15 52.204707131           ~ 49 0
24 OH 339.88 -1.26 Y*O 16 52 04.67 -46 08 34.2           ~ 66 0
25 OH 345.01 +1.79 Mas 16 56 47.58 -40 14 25.8           ~ 69 0
26 NAME NGC 6334F (NW) HII 17 20 53.18 -35 46 59.3           ~ 6 0
27 NAME NGC 6334F (C) HII 17 20 53.45 -35 47 02.6           ~ 200 1
28 GAL 035.2-00.74 MoC 18 58 13 +01 40.6           ~ 151 0
29 IRAS 18556+0136 mul 18 58 13.1 +01 40 35           ~ 132 0
30 SNR G035.2-01.8 SNR 19 01.6 +01 14           ~ 141 0
31 W 51e2 Rad 19 23 43.90 +14 30 34.8           ~ 176 0
32 W 51 SNR 19 23 50 +14 06.0           ~ 1119 1
33 IRAS 20126+4104 Y*O 20 14 25.8816186803 +41 13 36.869078243           B2.5-B0.5 388 0
34 NAME Cyg X FIR 33 Y*O 20 38 35.9 +42 37 22           B1.5 357 1
35 NAME BL Lac BLL 22 02 43.2913773726 +42 16 39.978417860   15.66 14.72     ~ 1975 1
36 LDN 1206 DNe 22 28 52.2 +64 13 43           ~ 61 0
37 IRAS 22272+6358A Cld 22 28 52.2 +64 13 43           ~ 47 0
38 NAME Cepheus A SFR 22 56 17.9 +62 01 49           ~ 690 2
39 NGC 7538 OpC 23 13 37 +61 30.0           ~ 814 0
40 [WBN74] NGC 7538 IRS 1 Y*O 23 13 45.318 +61 28 11.69           ~ 359 3
41 NAME Local Arm reg ~ ~           ~ 344 0

    Equat.    Gal    SGal    Ecl

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2019.10.21-03:13:45

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