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

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Volume 623 (March 2019)

A&A, 623 (2019) A130

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Table 4.

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

(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)
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.
	(°)	(°)	(°)	(°)	(°)		(°)	(°)	(°)
G23.44−0.18 (MM2)	13	+23 ± 40	−67 ± 40	−40 ± 15^d	+30 ± 26^e	+0.69	27 ± 43	13 ± 48	70 ± 30	(1)
					−24 ± 91^f	−0.37		47 ± 81	16 ± 91
G25.83−0.18	11	+23 ± 7	−67 ± 7	+10 ± 15^g	+51 ± 7	+0.69	77 ± 17	28 ± 10	41 ± 17	(2)
G25.71−0.04	23	−51 ± 77	−80 ± 43^h	−90 ± 15^g, i	−71 ± 9	−0.41	10 ± 46	20 ± 78	18 ± 18	(2)
G28.31−0.39	24	+40 ± 44	−50 ± 44	−52 ± 15^g	+85 ± 22	+0.07	2 ± 47	45 ± 49	84 ± 27^j	(2)
G28.83−0.25	10	−45 ± 34	+58 ± 59^h	−40 ± 15^g	−41 ± 10	−0.83	82 ± 61^j	4 ± 35	1 ± 18	(2)
G29.96−0.02	12	+62 ± 17	−29 ± 17	−38 ± 15^g	+80 ± 3	0.51	9 ± 23	18 ± 17	62 ± 16^j	(3)
G43.80−0.13	14	−81 ± 5	+9 ± 5	+38 ± 15^g	−48 ± 5	−0.94	29 ± 16	33 ± 7	86 ± 16	(4)

From Paper III^k

IRAS 20126+4104	4	−70 ± 16	+20 ± 16	−65 ± 5	+87 ± 4	+0.12	85 ± 17	23 ± 17	28 ± 6	(5)
G24.78+0.08-A2	17	−53 ± 2	+37 ± 2	−40 ± 15	−26 ± 19	−0.77	77 ± 15	79 ± 19	66 ± 24	(5)
G25.65+1.05	7	−80 ± 8	−23 ± 51	−15 ± 15	−49 ± 7	−0.87	8 ± 53	31 ± 11	64 ± 17	(5)
G29.86−0.04	17	+46 ± 41	+82 ± 56	+6 ± 15	+8 ± 7	+0.73	76 ± 58	38 ± 42	14 ± 17	(5)
G35.03+0.35	8	−64 ± 5	+26 ± 5	+27 ± 15	−26 ± 19	−0.77	1 ± 16	38 ± 20	53 ± 24	(5)
G37.43+1.51	4	+90 ± 3	+90 ± 3	−4 ± 15	−64 ± 5	−0.87	86 ± 15	26 ± 6	60 ± 16	(5)
G174.20−0.08	4	−	−	−40 ± 15	−63 ± 16	−0.45	−	−	23 ± 22	(5)
G213.70−12.6-IRS3	2	+20 ± 5	−70 ± 5	+53 ± 15	+63 ± 2	+0.95	57 ± 16	43 ± 5	10 ± 15	(5)
Cepheus A	2	−57 ± 28	+30 ± 19	+40 ± 4	−79 ± 9	−0.34	10 ± 19	22 ± 29	61 ± 10	(5)
W75N-group A	3	−13 ± 9	+77 ± 9	+66 ± 15	+43 ± 10	+0.96	11 ± 18	56 ± 14	23 ± 18	(5)
NGC7538-IRS1	6	−30 ± 69	+67 ± 70	−40 ± 10	+84 ± 7	+0.15	73 ± 71	66 ± 69	56 ± 12	(5)
W3(OH)-group II	4	+21 ± 45	−47 ± 44	−	−59 ± 6	−0.84	−	80 ± 45	−	(5)
W51-e2	12	+33 ± 16	−60 ± 21	−50 ± 20	+57 ± 8	+0.70	10 ± 29	24 ± 18	73 ± 22	(5)
IRAS18556+0138	5	−2 ± 11	+88 ± 11	+58 ± 23	−40 ± 2	−0.99	30 ± 26	42 ± 11	82 ± 23	(5)
W48	7	+23 ± 7	−67 ± 7	−	+55 ± 10	+0.70	−	78 ± 12	−	(5)
IRAS06058+2138-NIRS1	4	+49 ± 47	−49 ± 52	−50 ± 15	+78 ± 7	+0.64	1 ± 54	29 ± 48	52 ± 17	(5)
IRAS22272+6358A	2	−80 ± 15	+9 ± 15	−40 ± 15	−35 ± 11	−0.87	49 ± 21	45 ± 19	5 ± 19	(5)
S255-IR	4	+36 ± 12	−54 ± 12	+75 ± 15	−63 ± 49	−0.11	51 ± 19	81 ± 51	42 ± 51	(5)
S231	4	+28 ± 49	−62 ± 49	−47 ± 5	+28 ± 8	+0.97	15 ± 49	0 ± 50	75 ± 9	(5)
G291.27−0.70	7	−32 ± 5	+52 ± 5	−	−77 ± 14	−	−	45 ± 15	−	(5)
G305.21+0.21	9	−51 ± 14	28 ± 14	−	+48 ± 23	−	−	81 ± 27	−	(5)
G309.92+0.47	12	+2 ± 56	−75 ± 56	−	+35 ± 5	−	−	33 ± 56	−	(5)
G316.64−0.08	3	−67 ± 36	+21 ± 36	−	+34 ± 29	−	−	79 ± 46	−	(5)
G335.79+0.17	8	+44 ± 28	−41 ± 28	−	−69 ± 25	−	−	67 ± 38	−	(5)
G339.88−1.26	7	+77 ± 24	−12 ± 24	−	−60 ± 17	−	−	43 ± 29	−	(5)
G345.01+1.79	5	+5 ± 39	−86 ± 39	−	+74 ± 4	−	−	69 ± 39	−	(5)
NGC6334F (central)	5	+77 ± 20	−13 ± 20	+30 ± 15^g	−41 ± 16	−	43 ± 25	62 ± 26	71 ± 41	(5)
NGC6334F (NW)	5	−71 ± 20	+19 ± 20	+30 ± 15^g	−80 ± 38	−	11 ± 25	9 ± 43	70 ± 41^e	(5)

Notes.

^(a)

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

^(b)

Because of the large 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)

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

^(e)

Calculated for the western group of masers.

^(f)

Calculated for the eastern group of masers.

^(g)

We consider an arbitrary conservative error of 15°.

^(h)

Before averaging we use the criterion described in Sect. 3 to estimate the orientation of the magnetic field with respect to the linear polarization vectors.

⁽ⁱ⁾

Since the 6.7 GHz CH₃OH maser is associated with the blue-shifted lobe of the ¹³CO outflow we consider only its PA.

^(j)

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

^(k)

Here we omit all the notes that are already indicated in Table 2 of Paper III.

References. (1) Ren et al. (2011); (2) de Villiers et al. (2014); (3) Cesaroni et al. (2017); (4) López-Sepulcre et al. (2010); (5) Paper III and references therein.

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