ALMA observations of CO isotopologues towards six obscured post-asymptotic giant branch stars

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Volume 694 (February 2025)

A&A, 694 (2025) A222

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Table 2.

Parameters obtained from the literature and measured values of the continuum emission for the sample stars.

Source	d	L	Chem.	Spec.	υ_LSR	S_ν^cont	α^cont	δ^cont	FWHM and PA of cont.
	[kpc]	[10³ L_⊙]	type	type	[km s⁻¹]	[mJy]			[″ × ″/°]
GLMP 950	3.9 ^(a)	6	C ^(c)	?	22	5.2 ± 0.6	$19^{h} 47^{m} 24 \overset{s}{.} 43$ ${19^{\text{ h}}47^{\text{ m}}24{{\overset{\text{ s}}{.}}}43}$	$+ 29^{°} 28' 13 \overset{″}{.} 6$ ${+29^{\circ}28{\prime}13{{\overset{\prime\prime}{.}}}6}$	0.48(0.04)×0.39(0.03)/170(20)
GLMP 953	3.8 ^(a)	6	C ^(c)	?	42	119 ± 12	$19^{h} 50^{m} 08 \overset{s}{.} 20$ ${19^{\text{ h}}50^{\text{ m}}08{{\overset{\text{ s}}{.}}}20}$	$+ 25^{°} 11' 57 \overset{″}{.} 1$ ${+25^{\circ}11{\prime}57{{\overset{\prime\prime}{.}}}1}$	0.24(0.02)×0.26(0.01)/170(70)
AFGL 5385	3.4 ^(a)	12	C ^(d)	F4I ^(f)	7	12.9 ± 1.4	$17^{h} 47^{m} 13 \overset{s}{.} 50$ ${17^{\text{ h}}47^{\text{ m}}13{{\overset{\text{ s}}{.}}}50}$	$- 24^{°} 12' 51 \overset{″}{.} 6$ ${-24^{\circ}12{\prime}51{{\overset{\prime\prime}{.}}}6}$	1.4(0.1)×0.79(0.09)/59(8)
HD 187885	2.4 ^(a)	6	C ^(e)	F0Ie ^(f)	25	6.3 ± 0.7	$19^{h} 52^{m} 52 \overset{s}{.} 70$ ${19^{\text{ h}}52^{\text{ m}}52{{\overset{\text{ s}}{.}}}70}$	$- 17^{°} 01' 50 \overset{″}{.} 3$ ${-17^{\circ}01{\prime}50{{\overset{\prime\prime}{.}}}3}$	1.67(0.06)×1.43(0.06)/39(12)
Hen 3-1475	5.8 ^(b)	11	O	B7e ^(b)	49	29 ± 3	$17^{h} 45^{m} 14 \overset{s}{.} 18$ ${17^{\text{ h}}45^{\text{ m}}14{{\overset{\text{ s}}{.}}}18}$	$- 17^{°} 56' 46 \overset{″}{.} 9$ ${-17^{\circ}56{\prime}46{{\overset{\prime\prime}{.}}}9}$	1.10(0.09)×1.00(0.07)/–
M1-92	2.6 ^(a)	6	O	B0.5IV ^(g)	2	127 ± 13	$19^{h} 36^{m} 18 \overset{s}{.} 88$ ${19^{\text{ h}}36^{\text{ m}}18{{\overset{\text{ s}}{.}}}88}$	$+ 29^{°} 32' 49 \overset{″}{.} 6$ ${+29^{\circ}32{\prime}49{{\overset{\prime\prime}{.}}}6}$	–/–

Notes. Adopted distances and corresponding luminosities, chemical types, spectral types, systemic velocities measured from the spectra, and measured integrated continuum flux densities at 1.31 mm (S_ν^cont), continuum-peak positions, and FWHM sizes and position angle from Gaussian fit to continuum images.

References. (a) Vickers et al. (2015); (b) Riera et al. (1995); (c) Omont et al. (1993); (d) Su et al. (1998); (e) Van Winckel & Reyniers (2000); (f) Suárez et al. (2006); (g) Allen & Swings (1976).

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