A search for the favored hyperfine transition of a 6.7 GHz methanol maser line

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Volume 701 (September 2025)

A&A, 701 (2025) A101

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Table A.1

Parameters of the 6.7 GHz CH₃OH maser features detected in G 69.540–0.976 (ON 1).

(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)	(12)	(13)
Maser	RA^a	Dec^a	Peak	V_LSR	(Δ_{v_L}	$P_{1}^{b}$ $P_{1}^{b}$	χ^b	$Δ V_{i}^{c}$ $\Delta V_{\mathrm{i}}^{c}$	$T_{b} Δ Ω^{c}$ $T_{\mathrm{b}} \Delta \Omega^{c}$	P_V	Δ V_Z	θ^d
	offset	offset	Intensity (I)
	(mas)	(mas)	(Jy beam ⁻¹)	(kms⁻¹)	kms⁻¹)	(%)	°	(km s⁻¹)	(log K sr)	(%)	(m s⁻¹)	(°)
G69.M01	−44.763	127.548	0.100 ± 0.005	15.65	0.19	–	–	–	–	–	–	–
G69.M02	−9.487	−4.536	0.355 ± 0.047	14.51	0.19	–	–	–	–	–	–	–
G69.M03	−1.024	6.649	1.746 ± 0.008	14.81	0.19	–	–	–	–	–	–	–
G69.M04	0.000	0.000	11.022 ± 0.049	14.68	0.21	0.4 ± 0.1	−58 ± 6	${0.85}_{- 0.3}^{+ 0.2}$ $0.85_{-0.3}^{+0.2}$	${8.4}_{- 0.5}^{+ 1.0}$ $8.4_{-0.5}^{+1.0}$	0.6	3.2 ± 0.6	$75_{- 37}^{+ 13}$ $75_{-37}^{+13}$
G69.M05	340.544	885.803	1.361 ± 0.010	0.06	0.54	–	–	–	–	–	–	–
G69.M06	343.715	924.751	0.438 ± 0.006	1.25	0.26	–	–	–	–	–	–	–
G69.M07	378.442	944.389	0.218 ± 0.005	2.30	0.25	–	–	–	–	–	–	–
G69.M08	390.989	952.068	0.049 ± 0.004	2.61	0.16	–	–	–	–	–	–	–
G69.M09	401.805	−135.044	4.730 ± 0.047	14.51	0.18	–	–	–	–	–	–	–
G69.M10	411.694	−129.734	0.943 ± 0.053	14.60	0.20	–	–	–	–	–	–	–
G69.M11	428.595	−129.059	0.133 ± 0.013	–	–	–	–	–	–	–	–	–

Notes. ^aThe reference position is RA(J2000) =20^h 10^m09^s.04272 ± 0^s.00007 and Dec(J2000)=+31° 31^′ 34^′′.9736 ± 0^′.0009. ^bP₁ and χ are the mean values of the linear polarization percentage and the linear polarization angle measured across the spectrum, respectively. ^cThe best-fitting results obtained by using a model based on the radiative transfer theory of CH₃OH masers for Γ+Γ_v=1 s⁻¹ (Vlemmings et al. 2010; Surcis et al. 2011a). The errors were determined by analyzing the full probability distribution function. ^dThe angle between the magnetic field and the maser propagation direction is determined by using the observed P₁ and the fitted emerging brightness temperature. The errors were determined by analyzing the full probability distribution function.

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