LkHα 101 at millimeter wavelengths | Astronomy & Astrophysics (A&A)

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Table 2

Recombination lines (rest frequency ν) observed and Gaussian fits.

Transition	ν [GHz]	S_C [mJy]^a			S_L [mJy]			υ_LSR [km s^-1]			w [km s^-1]			^b			L/C [km s^-1]^c			Remark

H40α	99.022958	230	±	3	141	±	3	–2.6	±	0.2	43.8	±	0.3	7.10	±	0.1	30.9	±	1.2	non-Gaussian wings
H50β	99.225214	231	±	3	22	±	3	–1.5	±	0.8	60.0	±	2.2	1.56	±	0.1
H57γ	98.671897	229	±	3	7.4	±	0.7	5.2	±	2.3	64.1	±	6.5	0.54	±	0.05
H62δ	100.539631	233	±	3	<3.0
H67ϵ	98.199388	228	±	3	≲2.5
H39α	106.737363	275	±	18	226	±	8	0.4	±	0.4	32.8	±	1.2	7.80	±	0.28	28.4	±	2.5	non-Gaussian wings
H49β	105.301864	274	±	18	38	±	10	−2.0	±	2.0	32.9	±	5.0	1.35	±	0.20
H29α	256.302051	428	±	34	1250	±	34	−1.6	±	0.2	30.3	±	0.5	42.3	±	0.6	98.8	±	7.0	non-Gaussian wings
H41γ	257.635490	430	±	34	<85

Notes.S_L is the peak line flux density, υ_LSR the LSR velocity of the center of the line, and w its full width at half power. S_C is the continuum flux density.

^(a)

30 m values are derived from the spectroscopic baseline;

^(b)

derived from numerical integration over the line profile, in units of [Jy km s^-1];

^(c)

velocity-integrated line-to-continuum ratio.

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