Chasing discs around O-type (proto)stars: Evidence from ALMA observations

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Volume 602 (June 2017)

A&A, 602 (2017) A59

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Table 1

Targets for the ALMA observations with their main parameters, obtained from the literature.

Name	Other	α(J2000)	δ(J2000)	V_LSR	d	L_bol	M_gas^a	Ref.^c
	names	(h m s)	()	(km s^-1)	(kpc)	(10⁵L_⊙)	(10³M_⊙)

G17.64+0.16	AFGL 2136	18 22 26.370	−13 30 12.00	22.5	2.2	1.0	0.20	1
G24.78+0.08		18 36 12.661	−07 12 10.15	111.0	7.7	2.2	4.8	2, 3
G29.96−0.02	W43 S	18 46 03.665	−02 39 22.00	98.0	5.26	5.8	1.3	4, 5
G31.41+0.31		18 47 34.315	−01 12 45.90	96.5	7.9	2.6	5.2	3, 6
G345.49+1.47		16 59 41.610	−40 03 43.30	−12.6	2.4^b	1.5	1.2	1
G345.50+0.35		17 04 22.870	−40 44 23.50	−17.8	2.0	1.0	0.55	1

Notes.

^(a)

Computed from the flux density at 870 μm obtained from the ATLASGAL data, assuming a dust temperature of 50 K, a dust absorption coefficient κ_dust = 2 cm² g^-1 (Ossenkopf & Henning 1994), and a gas-to-dust mass ratio of 100.

^(b)

We prefer the spectrophotometric distance estimate by Moisés et al. (2011) to the kinematic distance of 1.6 ± 0.1 kpc by Urquhart et al. (2008).

^(c)

References for distance and luminosity: 1. RMS database; 2. Forster & Caswell (1989); 3. this paper; 4. Beltrán et al. (2013); 5. Zhang et al. (2014); 6. Cesaroni et al. (1994a).

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