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Table 3

All 6.7 GHz CH3OH maser features detected in NGC 7538-IRS 1 with the EVN.

     (1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13)
Maser group RA Dec Peak flux Vlsr ΔvL Pl χ ΔVia TbΔΩa ΔVZb θc
offset offset Density(I)
(mas) (mas) (Jy beam-1) (km s-1) (km s-1) (%) (°) (km s-1) (log K sr) (m s-1) (°)
E01 D  −286.910  −282.502 0.55 ± 0.02  −60.40 0.12  −  −  −  −  −  −
E02 D  −272.725  −279.037 16.82 ± 0.03  −60.49 0.21 4.5 ± 0.8  + 13 ± 16  + 2.7 ± 0.3
E03d D  −255.344  −273.992 4.72 ± 0.03  −60.58 0.24 5.6 ± 0.9  + 58 ± 5  −
E04 C  −93.660  −222.357 10.39 ± 0.02  −61.28 0.24 3.6 ± 0.2  + 81 ± 22  −
E05 C  −86.171  −200.790 0.73 ± 0.02  −61.28 0.20  −  −  −  −  −  −
E06 A  −80.377 22.786 15.21 ± 0.03  −57.24 0.20 3.6 ± 0.2  −66 ± 10  −
E07 C  −74.392  −213.730 16.41 ± 0.03  −61.28 0.29 4.1 ± 0.5  −83 ± 20  −
E08 A  −61.547 18.163 4.08 ± 0.02  −57.15 0.23 4.3 ± 1.4  −48 ± 40  −
E09 C  −57.174  −207.658 9.48 ± 0.02  −61.46 0.27 2.5 ± 0.7  −90 ± 4  −
E10 C  −52.938  −248.180 0.73 ± 0.02  −60.84 0.31  −  −  −  −  −  −
E11 C  −49.085  −205.700 1.12 ± 0.03  −60.75 1.08  −  −  −  −  −  −
E12 C  −48.483  −245.093 1.21 ± 0.02  −60.67 0.28  −  −  −  −  −  −
E13 C  −44.930  −222.357 4.65 ± 0.02  −60.84 0.25 1.4 ± 0.4  −86 ± 83  −
E14 C  −41.350  −198.801 1.11 ± 0.01  −61.02 0.49  −  −  −  −  −  −
E15 C  −40.421  −255.891 0.59 ± 0.02  −60.84 0.33  −  −  −  −  −  −
E16 C  −39.082  −181.780 0.57 ± 0.03  −60.75 0.18  −  −  −  −  −  −
E17 A  −37.661 12.650 14.31 ± 0.02  −56.80 0.33 1.4 ± 0.2  + 58 ± 12  −
E18 C  −27.986  −199.362 0.80 ± 0.03  −60.75 0.19  −  −  −  −  −  −
E19 C  −25.963  −230.701 1.29 ± 0.02  −60.84 0.26  −  −  −  −  −  −
E20 C  −22.083  −211.354 3.19 ± 0.03  −60.58 0.27 2.4 ± 1.0  −87 ± 23  −
E21 C  −18.147  −226.401 2.53 ± 0.03  −60.75 0.22 2.41 ± 0.04  −83 ± 12  −
E22 C  −15.769  −242.950 0.51 ± 0.02  −60.84 0.25  −  −  −  −  −  −
E23 A  −13.091  −56.523 1.43 ± 0.05  −55.75 0.26  −  −  −  −  −  −
E24 C  −8.172  −220.826 1.83 ± 0.02  −60.67 0.29 2.5 ± 0.3  −84 ± 14  −
E25 C  −7.762  −238.071 0.42 ± 0.02  −60.84 0.32  −  −  −  −  −  −
E26d A 0 0 95.15 ± 0.08  −55.92 0.33 5.83 ± 0.03  −87 ± 17  + 1.6 ± 0.3
E27 E 71.113  −503.039 0.19 ± 0.01  −58.56 0.12  −  −  −  −  −  −
E28 E 81.252  −497.234 0.37 ± 0.01  −58.56 0.27  −  −  −  −  −  −
E29 E 85.297  −557.914 1.06 ± 0.01  −58.91 0.27  −  −  −  −  −  −
E30 E 97.923  −513.329 0.30 ± 0.01  −58.38 0.18  −  −  −  −  −  −
E31 E 99.399  −489.943 2.26 ± 0.01  −58.38 0.21  −  −  −  −  −  −
E32 B 110.386  −235.856 4.37 ± 0.02  −57.77 0.31 2.4 ± 0.6  + 74 ± 44  −
E33 B 116.016  −175.760 10.11 ± 0.02  −57.86 0.30 2.5 ± 0.7  −81 ± 83  −
E34 B 121.782  −203.613 0.54 ± 0.02  −57.42 0.55  −  −  −  −  −  −
E35 E 122.083  −511.884 0.80 ± 0.02  −58.21 0.22  −  −  −  −  −  −
E36 B 123.859  −173.165 6.46 ± 0.02  −57.59 0.32 2.3 ± 0.6  −28 ± 42  −
E37 B 125.062  −233.976 0.68 ± 0.02  −57.07 0.28  −  −  −  −  −  −
E38 E 126.893  −540.110 0.93 ± 0.03  −58.12 0.21  −  −  −  −  −  −
E39 E 127.303  −546.631 0.21 ± 0.06  −58.73 0.26  −  −  −  −  −  −
E40 B 129.927  −218.961 8.98 ± 0.02  −57.51 0.37 2.1 ± 0.7  −69 ± 10  −
E41d B 132.550  −163.392 1.81 ± 0.02  −57.24 0.34 4.3 ± 1.1  + 76 ± 42  −
E42 E 134.190  −506.261 1.10 ± 0.03  −58.12 0.20  −  −  −  −  −  −
E43d B 137.196  −209.274 1.69 ± 0.03  −57.24 0.37 6.2 ± 2.0  −18 ± 17  −
E44 B 137.552  −181.682 1.05 ± 0.02  −57.33 0.24  −  −  −  −  −  −
E45 B 143.509  −164.852 0.98 ± 0.02  −56.72 0.32  −  −  −  −  −  −
E46 E 144.083  −537.047 0.12 ± 0.01  −58.73 0.28  −  −  −  −  −  −
E47 B 149.112  −203.584 0.71 ± 0.02  −57.42 0.27  −  −  −  −  −  −
E48 E 156.163  −503.223 23.68 ± 0.03  −58.03 0.24 3.5 ± 0.6  + 89 ± 44  −2.7 ± 0.3
E49 B 162.558  −154.095 1.50 ± 0.05  −56.19 0.16  −  −  −  −  −  −

Notes. 

(a)

The best-fitting results obtained by using a model based on the radiative transfer theory of CH3OH masers for Γ + Γν = 1s-1 (Vlemmings et al. 2010). The errors were determined by analyzing the full probability distribution function. For Γ + Γν = 0.6s-1 (Minier et al. 2002) TbΔΩ has to be adjusted by adding  − 0.22.

(b)

The Zeeman-splittings are determined from the cross-correlation between the RR and LL spectra.

(c)

The angle between the magnetic field and the maser propagation direction is determined by using the observed Pl and the fitted emerging brightness temperature. The errors were determined by analyzing the full probability distribution function.

(d)

Because of the degree of the saturation of these H2O masers, TbΔΩ is underestimated, ΔVi and θ are overestimated.

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