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COD95B - IRAS-selected Galactic star-forming regions - II. Water maser detections in the extended sample

Short title: Codella et al. (1995b)
Authors: Codella, C.Palumbo, G. G. C.Pareschi, G.Scappini, F.Caselli, P.Attolini, M. R.
Journal: Monthly Notices of the Royal Astronomical Society, Volume 276, Issue 1, pp. 57-73.
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Target type: IRAS
Observations category: SF.general
Facility type: single-dish

Abstract
The results of the analysis of the occurrence of 22.2-GHz H_2O maser emission in a sample of 1409 IRAS sources north of declination -30 deg associated with star-forming regions are presented. Our sample contains all the IRAS sources that satisfy Emerson criteria for selecting molecular cores associated with the earliest evolutionary stages of the star-forming process. In a previous paper, we have reported the results of the observations of about one third of the sample. In the present paper the observations of the remaining IRAS sources are presented: 18 of them are newly detected maser sources. The results show that 20 per cent of all IRAS sources that satisfy the Wood & Churchwell criteria have H_2O water masers. This is in agreement with the assumption that these criteria select objects that are connected with the early phases of the evolution of high-mass star-forming regions. Moreover, about one third of the whole sample selected according to Emerson criteria contains IRAS sources that are not associated with massive star-forming processes, but probably with molecular cores in low-mass star-forming regions.

Abstract

The results of the analysis of the occurrence of 22.2-GHz H_2O maser emission in a sample of 1409 IRAS sources north of declination -30 deg associated with star-forming regions are presented. Our sample contains all the IRAS sources that satisfy Emerson criteria for selecting molecular cores associated with the earliest evolutionary stages of the star-forming process. In a previous paper, we have reported the results of the observations of about one third of the sample. In the present paper the observations of the remaining IRAS sources are presented: 18 of them are newly detected maser sources. The results show that 20 per cent of all IRAS sources that satisfy the Wood & Churchwell criteria have H_2O water masers. This is in agreement with the assumption that these criteria select objects that are connected with the early phases of the evolution of high-mass star-forming regions. Moreover, about one third of the whole sample selected according to Emerson criteria contains IRAS sources that are not associated with massive star-forming processes, but probably with molecular cores in low-mass star-forming regions.

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Detection table from Codella et al. (1995b)

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ID	Obs. RA	Obs. Dec	l	b	Group id	grpv	Source name	Image	Line	V_peak	F_peak	∫F dv	Telescope	V_step	RMS	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)					H₂O	(km/s)	(Jy)	(Jy*km/s)		(km/s)	(Jy)	(arcsec)	Yes/No		(kpc)
1	07 04 45.6	-11 07 14.5	224.3396	-2.1326	G224.340-2.133	G224.3396-2.1326	07024-1102	Image	22 GHz;	18.1	29	34.7	MED	0.33	1.000	102	+H₂O -CH₃OH II	SFR_MIXED		920106
2	17 47 44.4	-29 01 31.5	0.1644	-0.4425	G0.167-0.446	G0.1644-0.4425	17445-2900	Image	22 GHz;	13.1	171	416.5	MED	0.33	19.300	102	+H₂O -CH₃OH I +CH₃OH II	SFR_MIXED		921230
3	18 08 18	-22 05 12.3	8.4903	-0.9823	G8.490-0.982	G8.4901-0.9820	18052-2205	Image	22 GHz;	14.2	82.9	90.2	MED	0.33	5.900	102	+H₂O	SFR_MIXED		911221
4	18 09 07	-19 27 22.6	10.8836	0.1261	G10.885+0.123	G10.8855+0.1227	18061-1927	Image	22 GHz;	24.5	38.9	33.2	MED	0.33	2.200	102	+H₂O -CH₃OH I +CH₃OH II +OH	SFR		930130
5	18 14 7.8	-18 00 20.6	12.7263	-0.2162	G12.721-0.216	G12.7263-0.2162	18112-1801	Image	22 GHz;	117.5	5.7	9.9	MED	0.33	1.400	102	+H₂O +CH₃OH I -CH₃OH II -OH -SiO	SFR_MIXED		930119
6	18 18 7.5	-13 45 06	16.9249	0.9638	G16.927+0.960	G16.9249+0.9638	18152-1346	Image	22 GHz;	-65.7	434	2558.2	MED	0.33	7.900	102	+H₂O +CH₃OH I -CH₃OH II	SFR		930121
7	18 33 30.4	-05 01 6.7	26.4202	1.6850	G26.422+1.685	G26.4213+1.6852	18308-0503	Image	22 GHz;	53.6	42	108.6	MED	0.33	2.800	102	+H₂O -CH₃OH I +CH₃OH II -OH			930118
8	18 34 37.8	-08 00 00	23.9021	0.0640	G23.901+0.066	G23.8984+0.0645	18319-0802	Image	22 GHz;	74.1	10.4	18.2	MED	0.33	2.300	102	+H₂O -CH₃OH I +CH₃OH II +OH	SFR_MIXED		930130
9	18 34 51.8	-08 51 40	23.1643	-0.3839	G23.162-0.382	G23.1623-0.3819	18321-0854	Image	22 GHz;	78.7	40.7	25.6	MED	0.33	1.500	102	+H₂O +CH₃OH II +OH	EVOLVED		930131
10	18 37 50.5	-01 45 47.8	29.8108	2.2184	G29.811+2.220	G29.8130+2.2195	18352-0148	Image	22 GHz;	43.7	14.7	10.3	MED	0.33	1.800	102	+H₂O -CH₃OH I -CH₃OH II -SiO	SFR_MIXED		920502
11	18 43 01	-04 37 32.6	27.8563	-0.2399	G27.869-0.236	G27.8563-0.2399	18403-0440	Image	22 GHz;	10.1	15.4	15.7	MED	0.33	2.400	102	+H₂O +CH₃OH II -OH	SFR_MIXED		920102
12	18 42 59.9	-04 41 59.7	27.7882	-0.2697	G27.783-0.260	G27.7882-0.2697	18403-0445	Image	22 GHz;	80.9	7.9	9.4	MED	0.33	1.400	102	+H₂O +CH₃OH I +CH₃OH II -OH	SFR		930119
13	18 44 07	-03 36 46.9	28.8823	-0.0208	G28.881-0.024	G28.8810-0.0244	18414-0339	Image	22 GHz;	137.8	13.7	33.3	MED	0.33	1.400	102	+H₂O +CH₃OH I -CH₃OH II	SFR		930131
14	18 47 35.6	-01 55 25.9	30.7815	-0.0222	G30.760-0.050	G30.7815-0.0222	18449-0158	Image	22 GHz;	115.6	8.9	23.1	MED	0.33	1.000	102	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		930421
15	18 57 52.9	+04 18 6.2	37.4943	0.5300	G37.498+0.530	G37.4979+0.5299	18553+0414	Image	22 GHz;	11.8	112	307	MED	0.33	7.400	102	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		921230
16	18 58 52.6	+04 32 12.4	37.8166	0.4170	G37.820+0.412	G37.8166+0.4170	18563+0428	Image	22 GHz;	18.8	218	158.7	MED	0.33	7.600	102	+H₂O +CH₃OH I -CH₃OH II +OH	SFR		930116
17	19 08 36.8	+06 57 1.5	41.0722	-0.6285	G41.078-0.637	G41.0722-0.6285	19061+0652	Image	22 GHz;	70.8	5.8	4.5	MED	0.33	1.000	102	+H₂O -CH₃OH I -CH₃OH II	UNK		920502
18	19 08 36.8	+06 57 1.5	41.0722	-0.6285	G41.078-0.637	G41.0722-0.6285	190874-0900	Image	22 GHz;	9.7	21.7	101.8	MED	0.33	2.000	102	+H₂O -CH₃OH I -CH₃OH II	UNK		921025

Non-detection table from Codella et al. (1995b)