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

G. Surcis; W. H. T. Vlemmings; H. J. van Langevelde; B. Hutawarakorn Kramer; L. H. Quiroga-Nuñez

doi:10.1051/0004-6361/201321501

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Volume 556 (August 2013)

A&A, 556 (2013) A73

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Table 2

Comparison between position angle of magnetic field, CH₃OH maser distribution, outflows, and linear polarization angles.

Source	⟨ χ⟩	⟨ Φ_B⟩	PA_out	PA_CH₃OH	ρ	\| PA_out − ⟨Φ_B⟩\|	\| PA_CH₃OH − ⟨χ⟩\|	\| PA_CH₃OH − PA_out\|	Ref.
	(°)	(°)	(°)	(°)		(°)	(°)	(°)

Cepheus A	−57 ± 28	+30 ± 19^a	+40 ± 4^b	−79 ± 9	–0.34	10 ± 19	22 ± 29	61 ± 10^c	(1), (2)
W75N-group A	−13 ± 9	+77 ± 9^a	+66 ± 15^d	+43 ± 10	+0.96	11 ± 18	56 ± 14	23 ± 18	(3), (4)
NGC 7538-IRS1	−30 ± 69	+67 ± 70^a	−40 ± 10^e	+84 ± 7^f	+0.15	73 ± 71^c	66 ± 69^c	56 ± 12^c	(5), (6), (7)
W3(OH)-group II	+21 ± 45	−47 ± 44^a	−	−59 ± 6	–0.84	−	80 ± 45	−	(8)
W51-e2	+33 ± 16	−60 ± 21^a	−50 ± 20^g	+57 ± 8	+0.70	10 ± 29	24 ± 18	73 ± 22^c	(8), (9), (10)
IRAS 18556+0138	−2 ± 11	+88 ± 11^a	+58 ± 23^h	−40 ± 2	–0.99	30 ± 26	42 ± 11	82 ± 23^c	(8), (11)
W48	+23 ± 7	−67 ± 7^a	−	+55 ± 10	+0.70	−	78 ± 12	−	(8)
IRAS 06058+2138-NIRS1	+49 ± 47	−49 ± 52^a	−50 ± 15ⁱ	+78 ± 7	+0.64	1 ± 54	29 ± 48	52 ± 17^c	(12), (13)
IRAS 22272+6358A	−80 ± 15	+9 ± 15^a	−40 ± 15^d	−35 ± 11	–0.87	49 ± 21	45 ± 19	5 ± 19	(12), (14)
S255-IR	+36 ± 12	−54 ± 12^a	+75 ± 15^d	−63 ± 49^j	–0.11	51 ± 19^c	81 ± 51^c	42 ± 51^c	(12), (15)
S231	+28 ± 49	−62 ± 49^a	−47 ± 5	+28 ± 8	+0.97	15 ± 49	0 ± 50	75 ± 9	(12), (16)
G291.27-0.70	−32 ± 5	+52 ± 5	−	−77 ± 14^k	−	−	45 ± 15	−	(17)
G305.21+0.21	−51 ± 14	28 ± 14	−	+48 ± 23^l	−	−	81 ± 27^c	−	(17), (18)
G309.92+0.47	+2 ± 56	−75 ± 56	−	+35 ± 5^l	−	−	33 ± 56	−	(17), (18)
G316.64-0.08	−67 ± 36	+21 ± 36	−	+34 ± 29^l	−	−	79 ± 46^c	−	(17)
G335.79+0.17	+44 ± 28	−41 ± 28	−	−69 ± 25^l	−	−	67 ± 38^c	−	(17), (18)
G339.88-1.26	+77 ± 24	−12 ± 24	−	−60 ± 17^l	−	−	43 ± 29^c	−	(17), (18)
G345.01+1.79	+5 ± 39	−86 ± 39	−	+74 ± 4^l	−	−	69 ± 39	−	(17), (18)
NGC 6334F (central)	+77 ± 20	−13 ± 20	−	−41 ± 16^k	−	−	62 ± 26^c	−	(17)
NGC 6334F (NW)	−71 ± 20	+19 ± 20	−	−80 ± 38^k	−	−	9 ± 43	−	(17)

Notes.

^(a)

Before averaging we use the criterion described in Sect. 4 to estimate the orientation of the magnetic field w.r.t. the linear polarization vectors.

^(b)

It has been obtained by flux weighting the angles reported in Table 2 of Curiel et al. (2006).

^(c)

The differences between the angles are evaluated taking into account that PA ≡ PA ± 180°, ⟨ χ⟩ ≡ ⟨χ⟩ ± 180°, and ⟨ Φ_B⟩ ≡ ⟨Φ_B⟩ ± 180°.

^(d)

We consider an arbitrary conservative error of 15°.

^(e)

The errors are evaluated considering the minimum and maximum PA of the CO-outflows reported by Scoville et al. (1986).

^(f)

We do not consider group E of CH₃OH masers in the fit.

^(g)

Keto & Klaassen (2008) reported that the orientation of the outflow is along the rotation axis of the molecular accretion flows. So we evaluate the arithmetic mean value (PA_out) of the rotation axes measured from the CH₃CN (PA_CH₃CN = 110°; Zhang et al. 1998) and the H53α flows (PA_H53α = 150°; Keto & Klaassen 2008).

^(h)

We overestimate the errors by considering half of the opening angle of the outflow.

⁽ⁱ⁾

The PA_out has been estimated from Fig. 4 of Wu et al. (2010).

^(j)

S255.30 and S255.31 were not included in the fit.

^(k)

The errors are overestimated by considering Figs. 1, 5, 9, and 10 of Dodson & Moriarty (2012).

^(l)

The errors are equal to the difference between the angles determined by Dodson & Moriarty (2012) and by De Buizer (2003).

Reference. (1) Vlemmings et al. (2010); (2) Curiel et al. (2006); (3) Surcis et al. (2009); (4) Hunter et al. (1994); (5) Surcis et al. (2011b); (6) Scoville et al. (1986); (7) Kameya et al. (1989); (8) Surcis et al. (2012); (9) Keto & Klaassen (2008); (10) Zhang et al. (1998); (11) Gibb et al. (2003); (12) This work; (13) Wu et al. (2010); (14) Beltrán et al. (2006); (15) Wang et al. (2011); (16) Ginsburg et al. (2009); (17) Dodson & Moriarty (2012); (18) De Buizer (2003).

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