The ALMA detection of CO rotational line emission in AGB stars in the Large Magellanic Cloud

M. A. T. Groenewegen; W. H. T. Vlemmings; P. Marigo; G. C. Sloan; L. Decin; M. W. Feast; S. R. Goldman; K. Justtanont; F. Kerschbaum; M. Matsuura; I. McDonald; H. Olofsson; R. Sahai; J. Th. van Loon; P. R. Wood; A. A. Zijlstra; J. Bernard-Salas; M. L. Boyer; L. Guzman-Ramirez; O. C. Jones; E. Lagadec; M. Meixner; M. G. Rawlings; S. Srinivasan

doi:10.1051/0004-6361/201629590

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Volume 596 (December 2016)

A&A, 596 (2016) A50

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Table 2

Results of the CO J = 2−1 observations.

Identifier	v _⋆	v _exp	A	T _peak	rms	Gas Ṁ^b
	(km s^-1)	(km s^-1)	(K km s^-1)	(K)	(K)	(M_⊙ yr^-1)

OH/IR stars

IRAS 05298	280^a	10.5^a	< 0.36	< 0.027	0.028	< 2.8 × 10^-6
IRAS 04545	250^a	7.7^a	0.53 ± 0.09	0.053 ± 0.009	0.026	3.3 × 10^-6

Carbon-rich stars

IRAS 05506	251.6 ± 0.3	23.63 ± 0.42	8.94 ± 0.19	0.284 ± 0.006	0.027	3.5 ×10^-5
IRAS 05125	207.1 ± 0.3	11.77 ± 0.15	2.85 ± 0.12	0.183 ± 0.007	0.024	1.0 ×10^-5
ERO 0529379	232.7 ± 0.3	11.04 ± 0.41	2.61 ± 0.09	0.178 ± 0.007	0.019	8.9 ×10^-6
ERO 0518117	164.0 ± 0.3	8.87 ± 0.52	3.01 ± 0.15	0.257 ± 0.013	0.033	9.0 ×10^-6

Notes.

^(a)

Stellar velocity and expansion velocity for the OH/IR stars from Goldman et al. (2016), and fixed in the fitting.

^(b)

Gas MLR based on Eq. (2); see text for assumed parameters.

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