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 4

Properties of the cores with velocity gradients detected with ALMA.

Name	d	HPBW^a	L_bol/M_gas	disc^b
	(kpc)	(AU)	(L_⊙/M_⊙)

G17.64+0.16	2.2	332	300	N
G24.78+0.08 A1	7.7	1205	15	?
G29.96−0.02 HMC	5.26	1168	300^c	Y
G31.41+0.31	7.9	1707	17	?
G345.49+1.47 M	2.4	483	22	?
G345.50+0.35 M	2.0	402	84	Y
G345.50+0.35 S	2.0	1217	84	Y
AFGL 4176^d	4.2	1205	120	Y

Notes.

^(a)

Half-power width of the synthesized beam at the distance of the source.

^(b)

Y = disc candidate; ? = questionable disc; N = no evidence for a molecular disc.

^(c)

A significant fraction of L_bol from G29.96 is known to be contributed by the O5–O6 star associated with the nearby UC Hii region (see Sect. 2).

^(d)

Revealed with ALMA by Johnston et al. (2015). The values of L_bol (1.7 × 10⁵L_⊙) and M_gas (1400 M_⊙) have been taken from Beltrán et al. (2007), after correcting for the different distance (4.7 kpc instead of 5.3 kpc) and dust temperature (50 K instead of 30 K).

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