Table 3.
Magnetic fields measurements around massive YSOs determined by observing, with the EVN, the circularly polarized emission of 6.7 GHz CH3OH masers.
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | |
|---|---|---|---|---|---|---|---|---|---|---|---|
| Source name | Maser ID | Peak flux | Vlsr | ΔVia | TbΔΩa | θ | PV | ΔVZ | |B|||b | |B|c | Ref. |
| Density (I) | |||||||||||
| (Jy beam−1) | (km s−1) | (km s−1) | (log K sr) | (°) | (%) | (m s−1) | (mG) | (mG) | |||
| W75N(B) | A4 | 47.58 | +5.82 | − | − | − | 0.5 | +0.80 ± 0.03d | > 16d | − | (1) |
| A5 | 39.39 | +5.12 | − | − | − | 0.5 | +0.75 ± 0.13d | > 15d | − | (1) | |
| B1 | 95.38 | +7.23 | − | − | − | 0.4 | +0.53 ± 0.04d | > 10d | − | (1) | |
| NGC 7538 | E02 | 16.82 | −50.49 | 1.0 | 9.41 |  |
1.7 | +2.7 ± 0.3d | > 53d | > 104 | (2) |
| E26 | 95.15 | −55.92 | 0.5 | 11.39 |  |
1.0 | +1.6 ± 0.3d | > 31d | > 62 | (2) | |
| E48 | 23.68 | −58.03 | 1.2 | 9.26 |  |
1.7 | −2.7 ± 0.3d | > 53d | > 65 | (2) | |
| W51-e2 | W51E.13 | 65.78 | +57.86 | 1.7 | 8.9 |  |
0.4 | −0.9 ± 0.2 | > 17 | > 21 | (3) |
| W51E.14 | 217.32 | +59.26 | 1.7 | 8.8 |  |
0.1 | +0.26 ± 0.06 | > 5 | > 5 | (3) | |
| W51E.18 | 27.56 | +59.35 | − | − | − | 1.1 | −2.1 ± 0.5e | > 42e | > 51e | (3) | |
| W51E.32 | 8.11 | +57.86 | 0.6 | 8.8 |  |
−f | −f | −f | −f | (3) | |
| W48 | W48.14 | 294.68 | +44.49 | 1.0 | 9.5 |  |
0.7 | −1.1 ± 0.2 | > 22 | > 27 | (3) |
| W3(OH) | W3OH.11 | 212.03 | −42.60 | − | − | − | 2.9 | −4.5 ± 0.7 | > 89g | > 111g | (3) |
| W3OH.22 | 2051.30 | −45.41 | 1.0 | 10.0 |  |
2.1 | +4.5 ± 0.7 | > 88 | > 182 | (3) | |
| W3OH.25 | 156.18 | −43.74 | 1.1 | 8.8 |  |
2.3 | +3.4 ± 0.5 | > 66 | > 70 | (3) | |
| W3OH.35 | 347.43 | −42.86 | 0.9 | 9.2 |  |
3.8 | +5.8 ± 0.9 | > 113 | > 136 | (3) | |
| W3OH.37 | 110.11 | −42.51 | 1.4 | 9.2 |  |
5.0 | −10.9 ± 1.6 | > 213 | > 260 | (3) | |
| W3OH.40 | 178.62 | −45.14 | − | − | − | 1.3 | −2.0 ± 0.3 | > 39h | − | (3) | |
| W3OH.48 | 19.97 | −41.81 | 1.0 | 9.0 |  |
1.5 | +8.4 ± 1.8 | > 165 | > 195 | (3) | |
| IRAS 06058+2138-IRS 1 | IRAS06.22 | 93.29 | +10.86 | 1.2 | 9.6 |  |
0.2 | +0.4 ± 0.2 | > 9 | > 17 | (4) |
| S255-IR | S255.30 | 10.64 | +4.61 | 1.1 | 9.5 |  |
0.3 | +0.4 ± 0.1 | > 9 | > 16 | (4) |
| IRAS 20126+4104 | M05 | 27.84 | −6.10 | 2.0 | 8.8 |  |
0.7 | −1.8 ± 0.3 | > 36 | > 41 | (5) |
| G24.78+0.08 | G24.16 | 13.70 | +110.41 | 1.7 | 8.6 |  |
0.3 | −0.6 ± 0.2 | > 11 | > 13 | (6) |
| G24.23 | 9.79 | +107.69 | 1.9 | 8.8 |  |
0.7 | +1.7 ± 0.3 | > 34 | > 36 | (6) | |
| G24.43 | 11.48 | +114.23 | 1.6 | 8.9 |  |
0.7 | −1.5 ± 0.3 | > 30 | > 60 | (6) | |
| G24.52 | 32.97 | +113.40 | 1.8 | 8.8 |  |
0.3 | −3.7 ± 0.6 | > 73 | > 84 | (6) | |
| G29.86−0.04 | G29.09 | 19.26 | +100.39 | 1.8 | 8.6 |  |
0.6 | −1.2 ± 0.2 | > 24 | > 28 | (6) |
| G213.70−12.6 | G213.15 | 91.58 | +12.57 | 1.1 | 9.5 |  |
0.7 | −1.1 ± 0.2 | > 22 | > 42 | (6) |
| IRAS 06058+2138-IRS 1 | IRAS06.22 | 93.29 | +10.86 | 1.2 | 9.6 |  |
0.2 | +0.4 ± 0.2 | > 9 | > 17 | (4) |
| S255-IR | S255.30 | 10.64 | +4.61 | 1.1 | 9.5 |  |
0.3 | +0.4 ± 0.1 | > 9 | > 16 | (4) |
| IRAS 20126+4104 | M05 | 27.84 | −6.10 | 2.0 | 8.8 |  |
0.7 | −1.8 ± 0.3 | > 36 | > 41 | (5) |
| G24.78+0.08 | G24.16 | 13.70 | +110.41 | 1.7 | 8.6 |  |
0.3 | −0.6 ± 0.2 | > 11 | > 13 | (6) |
| G24.23 | 9.79 | +107.69 | 1.9 | 8.8 |  |
0.7 | +1.7 ± 0.3 | > 34 | > 36 | (6) | |
| G24.43 | 11.48 | +114.23 | 1.6 | 8.9 |  |
0.7 | −1.5 ± 0.3 | > 30 | > 60 | (6) | |
| G24.52 | 32.97 | +113.40 | 1.8 | 8.8 |  |
0.3 | −3.7 ± 0.6 | > 73 | > 84 | (6) | |
| G29.86−0.04 | G29.09 | 19.26 | +100.39 | 1.8 | 8.6 |  |
0.6 | −1.2 ± 0.2 | > 24 | > 28 | (6) |
| G213.70−12.6 | G213.15 | 91.58 | +12.57 | 1.1 | 9.5 |  |
0.7 | −1.1 ± 0.2 | > 22 | > 42 | (6) |
Notes.
Values used to model the circularly polarized emission as evaluated from the linearly polarized emission.
The lower limit of the magnetic field strength along the line of sight was determined by modeling the circularly polarized emission assuming that the favored hyperfine transition is F = 3 → 4 (Lankhaar et al. 2018). The Landé g-factor for this transition is gl = −1.135 Hz mG−1 (or αZ = −0.051 km s−1 G−1).
Due to the scarce spectral resolution, B|| was determined from the cross-correlation between the RR and LL spectra, i.e., 
.
To model the circularly polarized emission we considered the values of TbΔΩ = 1.1 × 109 K sr, ΔVi = 0.7 km s−1, and 
measured for W51-e2.
To model the circularly polarized emission we considered the error-weighted values of ⟨TbΔΩ⟩ = 1.8 × 109 K sr, ⟨ΔVi⟩ = 0.6 km s−1, and 
measured for Group VI in W3(OH).
To model the circularly polarized emission we considered the values of TbΔΩ = 2.2 × 109 K sr and ΔVi = 0.5 km s−1 that best fit the total intensity spectrum.
References. (1) Surcis et al. (2009); (2) Surcis et al. (2011a); (3) Paper I; (4) Paper II; (5) Surcis et al. (2014b); (6) Paper III.
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