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Table 3

All 6.7 GHz methanol maser features detected in W48.

     (1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12)
Maser RA Dec Peak flux Vlsr ΔvL Pl χ ΔVia TbΔΩa ΔVZb θc
offset offset density(#I)
(mas) (mas) (Jy/beam) (km s-1) (km s-1) (%) (°) (km s-1) (log K sr) (m/s) (°)

W48.01 –138.785 –87.692 19.00 ± 0.40 43.78 0.22  −  −  −  −  −  −
W48.02 –110.296 –57.672 6.84 ± 0.06 44.13 0.19  −  −  −  −  −  −
W48.03 –109.953 –128.784 14.07 ± 0.26 41.41 0.23  −  −  −  −  −  −
W48.04d –101.143 –70.511 60.05 ± 1.46 42.91 0.29 5.1 ± 0.2 23 ± 8  −
W48.05 –99.026 –134.666 23.28 ± 0.95 40.89 0.29  −  −  −  −  −  −
W48.06 –94.621 –117.296 8.38 ± 0.14 42.03 0.24  −  −  −  −  −  −
W48.07 –90.502 –158.745 78.93 ± 1.40 41.50 0.22  −  −  −  −  −  −
W48.08 –89.072 –140.818 1.58 ± 0.02 40.18 0.35  −  −  −  −  −  −
W48.09 –82.093 –128.763 3.82 ± 0.09 40.18 0.35  −  −  −  −  −  −
W48.10 –81.635 –122.286 202.87 ± 6.56 42.47 0.26 4.4 ± 1.3 22 ± 6  −
W48.11 –81.235 –157.660 47.04 ± 0.08 40.97 0.31  −  −  −  −  −  −
W48.12 –77.974 –200.914 22.79 ± 0.18 41.76 0.37  −  −  −  −  −  −
W48.13 –75.171 –192.154 11.58 ± 0.26 41.41 0.17  −  −  −  −  −  −
W48.14d 0 0 294.68 ± 1.11 44.49 0.24 4.6 ± 1.5 12 ± 6 3.8 ± 0.4
W48.15 13.158 –65.594 2.48 ± 0.12 43.34 0.15  −  −  −  −  −  −
W48.16 27.631 –0.439 26.15 ± 0.41 44.57 0.26  −  −  −  −  −  −
W48.17 27.631 –29.171 22.64 ± 1.11 44.49 0.12  −  −  −  −  −  −
W48.18 34.267 –20.596 3.05 ± 0.17 45.36 0.24  −  −  −  −  −  −
W48.19d 47.082 –62.460 101.52 ± 1.30 43.70 0.25 5.4 ± 0.6 16 ± 4  −
W48.20d 58.352 6.796 32.74 ± 0.23 44.84 0.25 6.5 ± 0.6 27 ± 1  −

Notes. 

(a)

The best-fitting results obtained by using a model based on the radiative transfer theory of methanol masers for Γ + Γν = 1 (Vlemmings et al. 2010; Surcis et al. 2011b). The errors were determined by analyzing the full probability distribution function.

(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 CH3OH masers TbΔΩ is underestimated, ΔVi and θ are overestimated.

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