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CAS95B - Methanol and hydroxyl maser positions

Short title: Caswell et al. (1995)
Authors: Caswell, J. L.Vaile, R. A.Forster, J. R.
Journal: Monthly Notices of the Royal Astronomical Society, Volume 277, Issue 1, pp. 210-216.
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (38 detection)
Target type: Known_Class_II,OH
Transitions: OH_1665,CH3OH_6(II)

Abstract
The Australia Telescope Compact Array has been used to study more than 40 sites of 1.665-GHz hydroxyl masers and 36 sites of 6.668-GHz methanol masers. Maser positions accurate to better than 1 arcsec have been derived. At each maser site both species are commonly present, and comparisons have been made between the methanol and OH. In 28 of the 29 cases where we have accurate measurements of both species, the methanol and OH coincide to within the errors, with nominal separations of less than 1.4 arcsec. In only one case do the two species apparently arise from different sites, the separation in this instance exceeding 3 arcsec. 1.665-GHz OH masers are known to be excellent indicators of the sites of ultra-compact HII regions which envelop recently formed massive stars our results confirm with high accuracy that masers of 1.665-GHz OH and 6.6-GHz methanol generally pinpoint identical HII regions. Thus the same evolutionary phase of the HII region is conducive to both OH and methanol maser emission. We briefly discuss the precise distribution of the masing molecules relative to the embedded star and its HII region, but this requires further study.

Abstract

The Australia Telescope Compact Array has been used to study more than 40 sites of 1.665-GHz hydroxyl masers and 36 sites of 6.668-GHz methanol masers. Maser positions accurate to better than 1 arcsec have been derived. At each maser site both species are commonly present, and comparisons have been made between the methanol and OH. In 28 of the 29 cases where we have accurate measurements of both species, the methanol and OH coincide to within the errors, with nominal separations of less than 1.4 arcsec. In only one case do the two species apparently arise from different sites, the separation in this instance exceeding 3 arcsec. 1.665-GHz OH masers are known to be excellent indicators of the sites of ultra-compact HII regions which envelop recently formed massive stars our results confirm with high accuracy that masers of 1.665-GHz OH and 6.6-GHz methanol generally pinpoint identical HII regions. Thus the same evolutionary phase of the HII region is conducive to both OH and methanol maser emission. We briefly discuss the precise distribution of the masing molecules relative to the embedded star and its HII region, but this requires further study.

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Detection table from Caswell et al. (1995)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	V_peak	F_peak	Telescope	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)			CH₃OH (class II)	(km/s)	(Jy)		(arcsec)	Yes/No		(kpc)
1	13 11 13.7	-62 34 41.5	305.2083	0.2060	G305.208+0.206	305.21+0.21	6.6 GHz (II);	-38.3	320	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
2	13 11 10.5	-62 34 39	305.2021	0.2072	G305.208+0.206	305.20+0.21	6.6 GHz (II);	-44	20	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
3	13 50 41.8	-61 35 10.1	309.9205	0.4789	G309.921+0.479	309.92+0.48	6.6 GHz (II);	-59.7	710	ATCA	2	-H₂O +CH₃OH II +OH	SFR		1993 February 2-6
4	15 00 55.4	-58 58 52.9	318.9478	-0.1962	G318.948-0.196	318.95-0.20	6.6 GHz (II);	-34.7	690	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
5	15 18 34.6	-56 38 25	322.1583	0.6361	G322.161+0.635	322.16+0.64	6.6 GHz (II);	-63	178	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
6	15 31 45.5	-56 30 50.2	323.7401	-0.2627	G323.740-0.263	323.74-0.26	6.6 GHz (II);	-51.1	3000	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		1993 February 2-6
7	15 57 58.4	-53 59 23.1	328.2366	-0.5475	G328.237-0.547	328.24-0.55	6.6 GHz (II);	-44.5	360	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
8	15 57 59.8	-53 58 0.8	328.2541	-0.5323	G328.237-0.547	328.25-0.53	6.6 GHz (II);	-37.5	440	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
9	15 55 48.6	-52 43 6.2	328.8087	0.6328	G328.809+0.633	328.81+0.63	6.6 GHz (II);	-43.9	340	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
10	16 00 31.8	-53 12 49.7	329.0295	-0.2048	G329.031-0.200	329.03-0.21	6.6 GHz (II);	-37.4	138	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
11	16 00 30.3	-53 12 27.4	329.0308	-0.1977	G329.031-0.200	329.03-0.20	6.6 GHz (II);	-45.5	1 1	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
12	16 01 9.9	-53 16 2.7	329.0663	-0.3076	G329.066-0.308	329.07-0.31	6.6 GHz (II);	-44	2.3	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
13	16 11 26.6	-51 41 56.6	331.2783	-0.1882	G331.278-0.188	331.28-0.19	6.6 GHz (II);	-78.2	190	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
14	16 21 20.2	-50 09 48.4	333.4660	-0.1643	G333.466-0.164	333.47-0.16	6.6 GHz (II);	-42.5	63	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
15	16 30 57.3	-48 43 39.7	335.5851	-0.2846	G335.585-0.290	335.59-0.28	6.6 GHz (II);	-49.3	19.8	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		1993 February 2-6
16	16 30 58.7	-48 43 50.7	335.5855	-0.2894	G335.585-0.290	335.59-0.29	6.6 GHz (II);	-51.7	26	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		1993 February 2-6
17	16 30 58.8	-48 43 53.4	335.5851	-0.2902	G335.585-0.290	335.59-0.29se	6.6 GHz (II);	-47.4	92	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		1993 February 2-6
18	16 29 27.4	-48 17 53	335.7265	0.1910	G335.726+0.191	335.73+0.19	6.6 GHz (II);	-44.4	23.3	ATCA	2	+H₂O +CH₃OH II	SFR		1993 February 2-6
19	16 29 47.3	-48 15 51.6	335.7891	0.1741	G335.789+0.174	335.79+0.17	6.6 GHz (II);	-47.6	118	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
20	16 38 29.6	-47 00 35.3	337.7053	-0.0531	G337.705-0.053	337.71-0.05	6.6 GHz (II);	-54.6	98	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
21	16 51 6.2	-46 16 2.9	339.6805	-1.2081	G339.681-1.207	339.68-1.21	6.6 GHz (II);	-21.5	41	ATCA	2	+H₂O +CH₃OH II +OH	SFR		1993 February 2-6
22	16 52 4.7	-46 08 34.2	339.8840	-1.2588	G339.884-1.259	339.88-1.26	6.6 GHz (II);	-38.7	1650	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
23	16 50 14.9	-44 42 26.4	340.7850	-0.0960	G340.785-0.096	340.78-0.10	6.6 GHz (II);	-106.9	340	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
24	16 52 17.8	-44 26 52.1	341.2177	-0.2118	G341.218-0.212	341.22-0.21	6.6 GHz (II);	-37.9	137	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
25	17 04 7.8	-42 18 39.5	344.2275	-0.5687	G344.228-0.569	344.23-0.57	6.6 GHz (II);	-26.2	68	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
26	17 04 7.7	-42 18 38.8	344.2275	-0.5684	G344.228-0.569	344.23-0.57	6.6 GHz (II);	-19.8	90	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
27	16 56 47.6	-40 14 26.2	345.0094	1.7924	G345.010+1.792	345.01+1.79	6.6 GHz (II);	-17.9	500	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
28	16 56 46.8	-40 14 9.1	345.0116	1.7972	G345.010+1.792	345.01+1.80	6.6 GHz (II);	-13	30	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
29	17 04 22.9	-40 44 22.4	345.5045	0.3482	G345.505+0.348	345.50+0.35	6.6 GHz (II);	-17.7	172	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
30	17 19 20.4	-39 03 51.3	348.5498	-0.9787	G348.550-0.979	348.55-0.98	6.6 GHz (II);	-10.3	35	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
31	17 19 20.4	-39 03 52.1	348.5497	-0.9790	G348.550-0.979	348.55-0.98	6.6 GHz (II);	-12.9	29	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
32	17 19 20.4	-39 03 49.1	348.5504	-0.9785	G348.550-0.979	348.55-0.98n	6.6 GHz (II);	-20.1	33	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
33	17 26 42.5	-36 09 17.7	351.7746	-0.5364	G351.775-0.537	351.77-0.54	6.6 GHz (II);	1.2	290	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
34	17 30 26.1	-34 41 45.6	353.4097	-0.3600	G353.410-0.360	353.41-0.36	6.6 GHz (II);	-20	50	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
35	17 30 17.1	-33 13 55.1	354.6148	0.4719	G354.615+0.472	354.61+0.47	6.6 GHz (II);	-24.6	151	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
36	18 08 44.9	-19 54 38.2	10.4441	-0.0183	G10.444-0.018	10.44-0.02	6.6 GHz (II);	73	14.8	ATCA	2	+H₂O -CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
37	18 08 38.2	-19 51 50	10.4723	0.0273	G10.472+0.027	10.47+0.03	6.6 GHz (II);	75	120	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6
38	18 08 37.9	-19 51 15.9	10.4799	0.0330	G10.472+0.027	10.48+0.03	6.6 GHz (II);	65	9.7	ATCA	2	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 February 2-6

Distribution of sources in all sky (l,b)

Distribution of sources in all sky using Aladin

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Distribution of sources in IRAS color-color diagram

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Original color diagram is taken form van der Veen & Habing (1987)

Type	Description
I	Oxygen-rich non-variable stars without circumstellar shells
II	Variable stars with "young" O-rich circumstellar shells
IIIa	Variable stars with more evolved O-rich circumstellar shells
IIIb	Variable stars with thick O-rich circumstellar shells
IV	Variable stars with very thick O-rich circumstellar shells
V	Planetary nebulae and non- variable stars with very cool circumstellar shells
VIa	Variable stars with relatively cold dust at large distances; a significant part of the stars is carbon-rich
VIb	Variable stars with relatively hot dust close to the star and relatively cold dust at large distances; Some of the objects have proven to be O-rich
VII	Variable stars with more evolved C-rich circumstellar shells
VIII	Different sort of objects

Distribution of the detection velocities versus galactic longitude from CAS95B

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