A H2CO and H110α survey of H ii regions with the 25-m radio telescope of Nanshan Station

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Table 1

The sources with H₂CO absorption lines or H110α RRLs or both of them.

		RA(2000)	Dec(2000)	Rms^a	S_100 μm	S_6 cm^b
Source	Name	(^h m s)	(° ′ ″)	(Jy)	(10³Jy)	(Jy)	Note

IRAS 01202+6133		01 23 32.33	+ 61 48 48.7	0.124	1.72	0.90
IRAS 03271+3013		03 30 14.90	+ 30 23 48.5	0.125	0.01	...
IRAS 05375−0731	S235	05 39 56.06	−07 30 26.1	0.157	0.27	6.77
IRAS 05379+3550		05 41 20.53	+ 35 52 06.8	0.119	1.47	2.39
IRAS 05450+0019		05 47 34.62	+ 00 20 07.9	0.197	0.10	0.29
IRAS 05454+0034		05 47 59.22	+ 00 35 31.2	0.184	0.02	0.31
IRAS 06053−0622	Mon R2	06 07 46.67	−06 22 59.6	0.215	20.2	8.53
IRAS 06055+2039		06 08 32.82	+ 20 39 16.2	0.110	1.71	1.26
IRAS 17417−2851		17 44 53.42	−28 52 20.0	0.323	1.77	13.11
IRAS 17418−2927		17 44 59.55	−29 28 53.6	0.189	0.87	20.78
IRAS 17420−2902		17 45 14.80	−29 03 18.4	0.322	6.87	127.03
IRAS 17430−2900		17 46 16.07	−29 01 37.0	0.229	2.54	204.62
IRAS 17432−2855		17 46 26.73	−28 56 11.2	0.234	4.15	120.70
IRAS 17432−2835		17 46 27.43	−28 36 06.1	0.243	3.03	27.29
IRAS 17441−2822	Sgr B2	17 47 19.61	−28 23 07.3	0.237	66.7	54.63	^d^f
IRAS 17449−2855		17 48 10.47	−28 56 55.6	0.360	2.01	12.01	^d
G1.13−0.1		17 48 39.29	−28 01 57.5	0.181	...	10.17
IRAS 17455−2805		17 48 42.22	−28 06 49.3	0.240	5.39	7.99
IRAS 18035−2126		18 06 35.91	−21 26 00.7	0.194	1.05	2.58
IRAS 18048−2131		18 07 51.72	−21 30 53.2	0.204	0.14	...
IRAS 18060−2005	W31	18 08 58.52	−20 05 24.2	0.124	12.0	14.73	^f
G10.159−0.34	W31 A	18 09 23.52	−20 19 13.4	0.185	...	47.73	^d
IRAS 18064−2008		18 09 24.27	−20 08 07.4	0.242	1.16	13.40	^f
G12.807−0.20	W33	18 14 14.88	−17 55 44.1	0.175	...	38.57	^d^f
IRAS 18114−1718		18 14 23.26	−17 17 34.5	0.192	1.01	5.54
IRAS 18127−1717		18 15 38.13	−17 16 29.0	0.202	0.81	4.89
G14.626+0.08		18 16 48.35	−16 11 28.8	0.134	...	12.51
IRAS 18141−1615	RCW 157	18 17 02.22	−16 14 38.8	0.298	2.82	12.56	^f
G18.686+1.96	RCW 160	18 17 55.63	−11 43 36.8	0.177	...	13.26
G15.032−0.68	M17 S	18 20 26.74	−16 11 59.9	0.351	...	376.01
G15.181−0.62		18 20 30.64	−16 02 21.7	0.321	...	131.81	^d^f
G15.095−0.71	M17 N	18 20 40.19	−16 09 29.0	0.366	...	328.30
IRAS 18222−1317		18 25 02.27	−13 15 50.8	0.175	8.49	11.67	^d
G19.608−0.23		18 27 38.05	−11 56 41.5	0.202	...	9.46	^d^f
IRAS 18258−0737		18 28 34.15	−07 35 31.2	0.176	1.90	0.14
IRAS 18265−1517		18 29 24.80	−15 15 48.9	0.163	1.30	0.30
G23.421−0.21		18 34 43.95	−08 33 18.6	0.220	...	9.82	^d^f
IRAS 18328−0735		18 35 31.17	−07 33 22.1	0.195	2.98	10.02
IRAS 18406−0338		18 43 17.54	−03 35 45.4	0.186	3.13	4.59
IRAS 18408−0348		18 43 31.12	−03 44 57.5	0.209	0.87	5.37	^e^f
IRAS 18446−0150		18 47 13.96	−01 47 13.4	0.305	1.88	14.34
G30.776−0.03	W43	18 47 36.42	−01 55 54.8	0.220	...	69.35	^d^f
IRAS 18454−0158		18 48 01.30	−01 54 49.1	0.202	2.90	51.10
IRAS 18461−0136		18 48 44.59	−01 33 16.0	0.091	1.52	7.11
IRAS 18507+0110	NRAO 584	18 53 19.41	+ 01 14 34.7	0.179	32.5	13.72	^f
IRAS 18530+0215		18 55 34.19	+ 02 19 08.3	0.129	1.92	3.35
IRAS 18536+0753		18 56 03.75	+ 07 57 25.6	0.216	4.22	4.32
G40.505+2.54	S76	18 56 12.82	+ 07 53 39.3	0.245	...	5.09
IRAS 18566+0408		18 59 09.87	+ 04 12 13.6	0.143	1.03	3.66	^c
IRAS 18592+0108		19 01 46.95	+ 01 13 07.6	0.236	14.0	15.08
IRAS 19111+1048		19 13 27.81	+ 10 53 33.9	0.200	7.50	6.99
IRAS 19120+1103		19 14 21.73	+ 11 09 13.7	0.121	7.89	10.96	^d^f
IRAS 19124+1106		19 14 45.28	+ 11 11 58.3	0.162	0.58	6.03
G46.495−0.25		19 17 26.49	+ 11 55 54.4	0.136	...	4.20
IRAS 19181+1349		19 20 28.06	+ 13 55 26.0	0.138	5.23	8.50
G48.930−0.28		19 22 26.08	+ 14 07 08.1	0.115	...	39.98
G49.384−0.30		19 23 12.00	+ 14 27 31.2	0.149	...	41.69
G49.582−0.38	W51	19 23 42.06	+ 14 30 33.3	0.191	...	99.44	^f
IRAS 19598+3324	K3-50	20 01 45.60	+ 33 32 44.1	0.198	13.0	13.36
G79.293+1.30	DR 7	20 28 09.55	+ 40 51 42.5	0.122	...	13.48
G81.253+1.12		20 35 06.22	+ 42 20 23.6	0.214	...	14.20
IRAS 20332+4124		20 35 00.45	+ 41 34 48.2	0.098	1.38	...
IRAS 23033+5951		23 05 25.16	+ 60 08 11.6	0.108	1.83	1.09
IRAS 23116+6111	NGC 7538	23 13 45.63	+ 61 28 17.7	0.152	14.1	20.65

Notes.

^(a)

The rms of the spectral lines were obtained during our observation.

^(b)

The measurement results of the continuum flux densities at 6 cm;

^(c)

data reported by Araya et al. (2004);

^(d)

data reported by Downes et al. (1980);

^(e)

data reported by Wilson (1972);

^(f)

data reported by Whiteoak & Gardner (1974).

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