Looking for high-mass young stellar objects: HO and OH masers in ammonia cores

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Table 1:

Coordinates used as phase centers for the VLA observations, LSR velocities of the cloud and distances.
Source	$\alpha$	$\delta$	$V_{\rm LSR}$ ^a	d^b
	(J2000)	(J2000)	(km s^-1)	(kpc)
G12.22-0.12	18:12:39.81	-18:24:16.8	+27.0	16.1^c
G12.22-0.12M	18:12:44.44	-18:24:24.6	+28.2	16.1^c
G14.17-0.06	18:16:26.00	-16:39:56.2	+38.3	2.5-13.0^d
G23.44-0.18	18:34:39.25	-08:31:38.8	+99.4	5.9^e
G31.24-0.11	18:48:45.08	-01:33:12.8	+21.8	1.7^e
G31.21-0.18	18:48:56.57	-01:36:43.4	-39.0	19.7^e
G31.28+0.06	18:48:11.91	-01:26:38.5	+108.6	8.5^c
G32.74-0.07	18:51:21.86	-00:12:06.2	+37.5	2.7^e
G35.03+0.35	18:54:00.65	+02:01:19.3	+52.9	3.6^e
G35.20-0.74	18:58:12.98	+01:40:38.0	+33.7	2.2^f
G35.20-1.74	19:01:45.69	+01:13:35.0	+42.6	3.3^f
G43.89-0.38	19:14:26.17	+09:22:34.0	+54.3	4.2^g
G48.61+0.02	19:20:31.19	+13:55:24.9	+19.5	9.7^e
G50.32+0.68	19:21:27.56	+15:44:21.3	+25.8	8.7^g
G75.78+0.34	20:21:44.11	+37:26:39.4	-0.5	4.1^g

Notes. ^(a) Based on the present single-dish survey for all sources but G14.17-0.06 (single-dish CS survey, Plume et al. 1992), G31.21-0.18 (based on the H₂O maser emission pattern, Anglada et al. 1996), G31.24-0.11 (present VLA data), and G50.32+0.68 (single-dish CS survey, Bronfman et al. 1996). ^(b) Whenever the near-far ambiguity is not resolved out both values are reported. ^(c) Walsh et al. (1997). ^(d) Plume et al. (1992). ^(e) Present work. ^(f) Zhang et al. (2009). ^(g) Hofner & Churchwell (1996).

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