Table 2
Comparison between position angle of magnetic field, CH3OH maser distribution, outflows, and linear polarization angles.
| Source | ⟨ χ⟩ | ⟨ ΦB⟩ | PAout | PACH3OH | ρ | | PAout − ⟨ΦB⟩| | | PACH3OH − ⟨χ⟩| | | PACH3OH − PAout| | Ref. |
| (°) | (°) | (°) | (°) | (°) | (°) | (°) | |||
|
|
|||||||||
| Cepheus A | −57 ± 28 | +30 ± 19a | +40 ± 4b | −79 ± 9 | –0.34 | 10 ± 19 | 22 ± 29 | 61 ± 10c | (1), (2) |
| W75N-group A | −13 ± 9 | +77 ± 9a | +66 ± 15d | +43 ± 10 | +0.96 | 11 ± 18 | 56 ± 14 | 23 ± 18 | (3), (4) |
| NGC 7538-IRS1 | −30 ± 69 | +67 ± 70a | −40 ± 10e | +84 ± 7f | +0.15 | 73 ± 71c | 66 ± 69c | 56 ± 12c | (5), (6), (7) |
| W3(OH)-group II | +21 ± 45 | −47 ± 44a | − | −59 ± 6 | –0.84 | − | 80 ± 45 | − | (8) |
| W51-e2 | +33 ± 16 | −60 ± 21a | −50 ± 20g | +57 ± 8 | +0.70 | 10 ± 29 | 24 ± 18 | 73 ± 22c | (8), (9), (10) |
| IRAS 18556+0138 | −2 ± 11 | +88 ± 11a | +58 ± 23h | −40 ± 2 | –0.99 | 30 ± 26 | 42 ± 11 | 82 ± 23c | (8), (11) |
| W48 | +23 ± 7 | −67 ± 7a | − | +55 ± 10 | +0.70 | − | 78 ± 12 | − | (8) |
| IRAS 06058+2138-NIRS1 | +49 ± 47 | −49 ± 52a | −50 ± 15i | +78 ± 7 | +0.64 | 1 ± 54 | 29 ± 48 | 52 ± 17c | (12), (13) |
| IRAS 22272+6358A | −80 ± 15 | +9 ± 15a | −40 ± 15d | −35 ± 11 | –0.87 | 49 ± 21 | 45 ± 19 | 5 ± 19 | (12), (14) |
| S255-IR | +36 ± 12 | −54 ± 12a | +75 ± 15d | −63 ± 49j | –0.11 | 51 ± 19c | 81 ± 51c | 42 ± 51c | (12), (15) |
| S231 | +28 ± 49 | −62 ± 49a | −47 ± 5 | +28 ± 8 | +0.97 | 15 ± 49 | 0 ± 50 | 75 ± 9 | (12), (16) |
| G291.27-0.70 | −32 ± 5 | +52 ± 5 | − | −77 ± 14k | − | − | 45 ± 15 | − | (17) |
| G305.21+0.21 | −51 ± 14 | 28 ± 14 | − | +48 ± 23l | − | − | 81 ± 27c | − | (17), (18) |
| G309.92+0.47 | +2 ± 56 | −75 ± 56 | − | +35 ± 5l | − | − | 33 ± 56 | − | (17), (18) |
| G316.64-0.08 | −67 ± 36 | +21 ± 36 | − | +34 ± 29l | − | − | 79 ± 46c | − | (17) |
| G335.79+0.17 | +44 ± 28 | −41 ± 28 | − | −69 ± 25l | − | − | 67 ± 38c | − | (17), (18) |
| G339.88-1.26 | +77 ± 24 | −12 ± 24 | − | −60 ± 17l | − | − | 43 ± 29c | − | (17), (18) |
| G345.01+1.79 | +5 ± 39 | −86 ± 39 | − | +74 ± 4l | − | − | 69 ± 39 | − | (17), (18) |
| NGC 6334F (central) | +77 ± 20 | −13 ± 20 | − | −41 ± 16k | − | − | 62 ± 26c | − | (17) |
| NGC 6334F (NW) | −71 ± 20 | +19 ± 20 | − | −80 ± 38k | − | − | 9 ± 43 | − | (17) |
Notes.
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.
It has been obtained by flux weighting the angles reported in Table 2 of Curiel et al. (2006).
The differences between the angles are evaluated taking into account that PA ≡ PA ± 180°, ⟨ χ⟩ ≡ ⟨χ⟩ ± 180°, and ⟨ ΦB⟩ ≡ ⟨ΦB⟩ ± 180°.
The errors are evaluated considering the minimum and maximum PA of the CO-outflows reported by Scoville et al. (1986).
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 (PAout) of the rotation axes measured from the CH3CN (PACH3CN = 110°; Zhang et al. 1998) and the H53α flows (PAH53α = 150°; Keto & Klaassen 2008).
The PAout has been estimated from Fig. 4 of Wu et al. (2010).
The errors are overestimated by considering Figs. 1, 5, 9, and 10 of Dodson & Moriarty (2012).
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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