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

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Volume 578 (June 2015)

A&A, 578 (2015) A102

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Table 2

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

Source	Φ_f ^a	⟨ χ ⟩ ^b	⟨ Φ_B ⟩ ^b	PA_outflow	PA_CH₃OH	ρ ^c	\| PA_outflow − ⟨ Φ_B ⟩ \|	\| PA_CH₃OH − ⟨ χ ⟩ \|	\| PA_CH₃OH − PA_outflow \|	Ref.^d
	(°)	(°)	(°)	(°)	(°)		(°)	(°)	(°)


IRAS 20126+4104	4	− 70 ± 16	+ 20 ± 16	− 65 ± 5 ^e	+ 87 ± 4	+ 0.12	85 ± 17	23 ± 17 ^f	28 ± 6 ^f	(1), (2)
G24.78+0.08-A2	17	− 53 ± 2	+ 37 ± 2 ^g	− 40 ± 15 ^h	− 26 ± 19	− 0.77	77 ± 15	79 ± 19	66 ± 24	(3), (4)
G25.65+1.05	7	− 80 ± 8	− 23 ± 51 ^g	− 15 ± 15 ^h	− 49 ± 7 ⁱ	− 0.87	8 ± 53	31 ± 11	64 ± 17	(3), (5)
G29.86-0.04	17	+ 46 ± 41	+ 82 ± 56 ^g	+ 6 ± 15 ^h^,^j	+ 8 ± 7 ⁱ	+ 0.73	76 ± 58	38 ± 42	14 ± 17	(3), (6)
G35.03+0.35	8	− 64 ± 5	+ 26 ± 5 ^g	+ 27 ± 15 ^h^,^k	− 26 ± 19	− 0.77	1 ± 16	38 ± 20	53 ± 24	(3), (7), (8)
G37.43+1.51	4	+ 90 ± 3	+ 90 ± 3 ^g	− 4 ± 15 ^h	− 64 ± 5 ⁱ	− 0.87	86 ± 15 ^f	26 ± 6 ^f	60 ± 16	(3), (9)
G174.20-0.08	4	−	−	− 40 ± 15 ^h	− 63 ± 16	− 0.45	−	−	23 ± 22	(3), (10)
G213.70-12.6-IRS3	2	+ 20 ± 5	− 70 ± 5 ^g	+ 53 ± 15 ^h	+ 63 ± 2	+ 0.95	57 ± 16 ^f	43 ± 5	10 ± 15	(3), (11)


From Paper II^l
Cepheus A	2	− 57 ± 28	+ 30 ± 19	+ 40 ± 4	− 79 ± 9	− 0.34	10 ± 19	22 ± 29	61 ± 10	(12)
W75N-group A	3	− 13 ± 9	+ 77 ± 9	+ 66 ± 15	+ 43 ± 10	+ 0.96	11 ± 18	56 ± 14	23 ± 18	(12)
NGC7538-IRS1	6	− 30 ± 69	+ 67 ± 70	− 40 ± 10	+ 84 ± 7	+ 0.15	73 ± 71	66 ± 69	56 ± 12	(12)
W3(OH)-group II	4	+ 21 ± 45	− 47 ± 44	−	− 59 ± 6	− 0.84	−	80 ± 45	−	(12)
W51-e2	12	+ 33 ± 16	− 60 ± 21	− 50 ± 20	+ 57 ± 8	+ 0.70	10 ± 29	24 ± 18	73 ± 22	(12)
IRAS18556+0138	5	− 2 ± 11	+ 88 ± 11	+ 58 ± 23	− 40 ± 2	− 0.99	30 ± 26	42 ± 11	82 ± 23	(12)
W48	7	+ 23 ± 7	− 67 ± 7	−	+ 55 ± 10	+ 0.70	−	78 ± 12	−	(12)
IRAS06058+2138-NIRS1	4	+ 49 ± 47	− 49 ± 52	− 50 ± 15	+ 78 ± 7	+ 0.64	1 ± 54	29 ± 48	52 ± 17	(12)
IRAS22272+6358A	2	− 80 ± 15	+ 9 ± 15	− 40 ± 15	− 35 ± 11	− 0.87	49 ± 21	45 ± 19	5 ± 19	(12)
S255-IR	4	+ 36 ± 12	− 54 ± 12	+ 75 ± 15	− 63 ± 49	− 0.11	51 ± 19	81 ± 51	42 ± 51	(12)
S231	4	+ 28 ± 49	− 62 ± 49	− 47 ± 5	+ 28 ± 8	+ 0.97	15 ± 49	0 ± 50	75 ± 9	(12)
G291.27-0.70	7	− 32 ± 5	+ 52 ± 5	−	− 77 ± 14	−	−	45 ± 15	−	(12)
G305.21+0.21	9	− 51 ± 14	28 ± 14	−	+ 48 ± 23	−	−	81 ± 27	−	(12)
G309.92+0.47	12	+ 2 ± 56	− 75 ± 56	−	+ 35 ± 5	−	−	33 ± 56	−	(12)
G316.64-0.08	3	− 67 ± 36	+ 21 ± 36	−	+ 34 ± 29	−	−	79 ± 46	−	(12)
G335.79+0.17	8	+ 44 ± 28	− 41 ± 28	−	− 69 ± 25	−	−	67 ± 38	−	(12)
G339.88-1.26	7	+ 77 ± 24	− 12 ± 24	−	− 60 ± 17	−	−	43 ± 29	−	(12)
G345.01+1.79	5	+ 5 ± 39	− 86 ± 39	−	+ 74 ± 4	−	−	69 ± 39	−	(12)
NGC 6334F (central)	5	+ 77 ± 20	− 13 ± 20	+ 30 ± 15 ^h	− 41 ± 16	−	43 ± 25	62 ± 26	71 ± 41	(12); (13)
NGC 6334F (NW)	5	− 71 ± 20	+ 19 ± 20	+ 30 ± 15 ^h	− 80 ± 38	−	11 ± 25	9 ± 43	70 ± 41 ^f	(12); (13)

Notes. and references therein; (13) Zhang et al. (2014).

^(a)

Foreground Faraday rotation estimated by using Eq. (3) of Paper I.

^(b)

Because of the high uncertainties of the estimated Φ_f, the angles are not corrected for Φ_f.

^(c)

Pearson product-moment correlation coefficient − 1 ≤ ρ ≤ + 1; ρ = + 1 (ρ = −1) is total positive (negative) correlation, ρ = 0 is no correlation.

^(d)

(1) Surcis et al. (2014); (2) Moscadelli et al. (2011); (3) this work; (4) Beltrán et al. (2011); (5) Sánchez-Monge et al. (2013); (6) de Villiers et al. (2014); (7) Cyganowski et al. (2009); (8) Paron et al. (2012); (9) López-Sepulcre et al. (2010); (10) Goddi et al. (2011); (11) Dierickx et al. (2015); (12) Paper II

^(e)

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

^(f)

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

^(g)

Before averaging, we use the criterion described in Sect. 3 to estimate the orientation of the magnetic field w.r.t the linear polarization vectors.

^(h)

We consider an arbitrary conservative error of 15°.

⁽ⁱ⁾

We consider only group A.

^(j)

We consider the PA of the redshifted lobe of the CO outflow; see Sect. 5.1.

^(k)

We assumed PA_outflow = PA^{4.5 μm}; see Sect. 4.4.

^(l)

Here we omit all the notes that are already included in Table 2 of Paper II.

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