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Appendix A: Tables

In Tables A.1–A.4 we list all the CH₃OH maser features detected towards the four massive star-forming regions observed with the EVN. The Tables are organized as follows. The name of the feature is reported in Col. 1 and the group to which they belong is in Col. 2. The positions, Cols. 3 and 4, are referred to the maser feature used for self-calibration, no absolute positions were measured. The peak flux density (I), the LSR velocity (V_lsr), and the FWHM (Δv_L) of the total intensity spectra of the maser features are reported in Cols. 5–7, respectively. I, V_lsr, and Δv_L are obtained using a Gaussian fit. The linear polarization fraction (P_l) and the linear polarization angles (χ) are instead reported in Cols. 8 and 9, respectively. The best-fitting results obtained by using a model based on the radiative transfer theory of methanol masers for Γ + Γ_ν = 1  s^-1 (Vlemmings et al. 2010; Surcis et al. 2011b) are reported in Cols. 10 (the emerging brightness temperature) and 11 (the intrinsic thermal linewidth). The errors were determined by analyzing the full probability distribution function. The angle between the magnetic field and the maser propagation direction (θ, Col. 14) is determined by using the observed P_l and the fitted emerging brightness temperature. Also for θ the errors were determined by analyzing the full probability distribution function. The circular polarization fraction (P_V) and the Zeeman-splitting (ΔV_Z) are finally in Cols. 12 and 13, respectively. The Zeeman-splitting is determined by fitting the V stoke spectra by using the best-fitting results (ΔV_i and T_bΔΩ).

© ESO, 2013