(Sub)millimeter emission lines of molecules in born-again stars

D. Tafoya; J. A. Toalá; W. H. T. Vlemmings; M. A. Guerrero; E. De Beck; M. González; S. Kimeswenger; A. A. Zijlstra; Á. Sánchez-Monge; S. P. Treviño-Morales

doi:10.1051/0004-6361/201630074

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Volume 600 (April 2017)

A&A, 600 (2017) A23

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Table 2

Detected line emission.

Molecule	Transition	Rest frequency	Line peak(T_MB,peak)^a^b	Line peak(S_ν,peak)^c	v _LSR ^a^d	Δv ^a^f	I ^f	rms^c^g
		(GHz)	(mK)	(mJy)	(km s^-1)	(km s^-1)	(K km s^-1)	(mJy)

V4334 Sgr

HCN	J = 4 → 3	354.50548	16.5±1.8	490±52	181±16	298±37	4.9±0.8	139
HCN	J = 1 → 0	88.63185	6.2±0.4	31±2	128±14	405±34	2.5±0.3	7
H¹³CN	J = 4 → 3	345.33976	7.2±0.8	215±24	123±13	236±30	1.7±0.3	57

V605 Aql

CO	J = 3 → 2	345.79599	4.0±0.5	119±16	96±11	164±25	0.7 ± 0.1	29

Notes.

^(a)

Nominal value and standard error obtained from fitting a Gaussian model to the emission line.

^(b)

The main-beam brightness temperature was obtained as /η_MB, where is the antenna temperature corrected for the atmospheric attenuation.

^(c)

The flux density can be obtained as (or equivalently, S_ν = η_MBT_MB/ Γ).

^(d)

Central LSR velocity.

^(e)

Fullwidth at half maximum.

^(f)

Velocity-integrated intensity of the line.

^(g)

Channel-to-channel 1σ rms noise of the line-free channels for a velocity resolution of 20 km s^-1.

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