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ELL96B - A survey of the Galactic plane for 6.7-GHz methanol masers - I. l=325-335 b=-0.53-0.53

Short title: Ellingsen et al. (1996)
Authors: Ellingsen, S. P.von Bibra, M. L.McCulloch, P. M.Norris, R. P.Deshpande, A. A.Phillips, C. J.
Journal: Monthly Notices of the Royal Astronomical Society, Volume 280, Issue 2, pp. 378-396.
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (50 detection)
Target type: Blind
Transitions: CH3OH_6(II)

Abstract
We report the results of the first complete survey of an area of the Galactic plane for maser emission from the 6.7-GHz 5_1-->6_0 A^+ transition of CH_3OH. The survey covers a 10.6-deg^2 region of the Galactic plane in the longitude range 325 deg-335 deg and latitude range -0.Ë訙-0.Ë訙. The survey is sensitive to masers with a peak flux density greater than ~2.6 Jy. The weakest maser detected has a peak flux density of 2.3 Jy, and the strongest a peak flux density of 425 Jy. We detected a total of 50 distinct masers, 26 of which are new detections. We show that many 6.7-GHz CH_3OH masers are not associated with IRAS sources, and that some are associated with sources that have colours differing from those of a typical ultracompact HII (UCHII) region. We estimate that the number of UCHII regions in the Galaxy is significantly more than suggested by IRAS-based estimates, possibly by more than a factor of 2.

Abstract

We report the results of the first complete survey of an area of the Galactic plane for maser emission from the 6.7-GHz 5_1-->6_0 A^+ transition of CH_3OH. The survey covers a 10.6-deg^2 region of the Galactic plane in the longitude range 325 deg-335 deg and latitude range -0.Ë訙-0.Ë訙. The survey is sensitive to masers with a peak flux density greater than ~2.6 Jy. The weakest maser detected has a peak flux density of 2.3 Jy, and the strongest a peak flux density of 425 Jy. We detected a total of 50 distinct masers, 26 of which are new detections. We show that many 6.7-GHz CH_3OH masers are not associated with IRAS sources, and that some are associated with sources that have colours differing from those of a typical ultracompact HII (UCHII) region. We estimate that the number of UCHII regions in the Galaxy is significantly more than suggested by IRAS-based estimates, possibly by more than a factor of 2.

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Detection table from Ellingsen et al. (1996)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Image	Descr.	Line	V_range	V_peak	F_peak	∫F dv	Telescope	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)					CH₃OH (class II)	(km/s)	(km/s)	(Jy)	(Jy*km/s)		(arcsec)	Yes/No		(kpc)
1	15 43 40.7	-54 19 28	326.3976	0.5052	G326.398+0.505	326.40+0.51	Image	Descr	6.6 GHz (II);		-38.1	2.4	1.4	Hobart_26m	420	+CH₃OH II	UNK		1993 April - 1994 September
2	15 44 33.3	-54 06 23	326.6321	0.6001	G326.641+0.611	326.63+0.60	Image	Descr	6.6 GHz (II);	-44;-36	-43.1	18	18.8	Hobart_26m	420	+CH₃OH I +CH₃OH II	SFR		1993 April - 1994 September
3	15 44 52.1	-54 10 30	326.6265	0.5178	G326.627+0.518	326.63+0.52	Image	Descr	6.6 GHz (II);	-42;-38	-41	5.6	8.3	Hobart_26m	420	+CH₃OH II	SFR		1993 April - 1994 September
4	15 51 11.1	-54 59 01	326.8435	-0.6840	G326.843-0.684	326.84-0.68	Image		6.6 GHz (II);	-59;-57	-57.6	10	9.7	Hobart_26m	420	+CH₃OH II	UNK		1993 April - 1994 September
5	15 47 33.6	-53 52 35	327.1219	0.5102	G327.120+0.511	327.12+0.51	Image	Descr	6.6 GHz (II);	-90;-83	-87.1	80	49.8	Hobart_26m	420	+H₂O -CH₃OH I +CH₃OH II +OH	SFR		1993 April - 1994 September
6	15 49 14	-53 45 36	327.3878	0.4481	G327.402+0.444	327.40+0.44	Image	Descr	6.6 GHz (II);	-84;-75	-82.6	106	153.1	Hobart_26m	420	+H₂O -CH₃OH I +CH₃OH II +OH	SFR		1993 April - 1994 September
7	15 50 21.4	-53 56 25	327.4045	0.2039	G327.392+0.199	327.40+0.20	Image	Descr	6.6 GHz (II);	-86;-82	-84.6	9	9	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II	SFR		1993 April - 1994 September
8	15 52 34	-54 03 12	327.5857	-0.0884	G327.590-0.094	327.59-0.09	Image	Descr	6.6 GHz (II);		-86.2	3.2	1.7	Hobart_26m	420	+H₂O -CH₃OH I +CH₃OH II	SFR		1993 April - 1994 September
9	15 52 47.3	-54 03 15	327.6104	-0.1096	G327.618-0.111	327.61-0.11	Image	Descr	6.6 GHz (II);		-97.5	2.3	1.8	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II	EVOLVED		1993 April - 1994 September
10	15 54 34.8	-53 52 18	327.9298	-0.1362	G327.945-0.115	327.93-0.14	Image	Descr	6.6 GHz (II);	-52;-51	-51.7	6.6	3	Hobart_26m	420	+H₂O -CH₃OH I +CH₃OH II	SFR		1993 April - 1994 September
11	15 57 58.5	-53 59 23	328.2369	-0.5477	G328.237-0.547	328.24-0.55	Image	Descr	6.6 GHz (II);	-46;-34	-44.9	421	437.7	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 April - 1994 September
12	15 57 59.9	-53 58 01	328.2542	-0.5325	G328.237-0.547	328.25-0.53	Image	Descr	6.6 GHz (II);	-50;-36	-37.4	425	428.1	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 April - 1994 September
13	15 55 51.2	-52 42 36	328.8191	0.6351	G328.809+0.633	328.81+0.63	Image	Descr	6.6 GHz (II);	-47;-43	-44.5	278	353	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 April - 1994 September
14	16 00 22.1	-53 12 57	329.0098	-0.1906	G329.031-0.200	329.03-0.20	Image	Descr	6.6 GHz (II);	-47;-41	-41.9	25	38.2	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 April - 1994 September
15	16 00 36	-53 12 17	329.0433	-0.2048	G329.031-0.200	329.03-0.21	Image	Descr	6.6 GHz (II);	-41;-34	-37.5	275	360	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 April - 1994 September
16	16 01 12.7	-53 15 58	329.0723	-0.3112	G329.066-0.308	329.07-0.31	Image	Descr	6.6 GHz (II);	-48;-43	-43.9	24	17.4	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 April - 1994 September
17	16 01 36.3	-53 11 49	329.1621	-0.2976	G329.163-0.286	329.18-0.31	Image	Descr	6.6 GHz (II);	-60;-51	-55.7	13	18.6	Hobart_26m	420	+CH₃OH I +CH₃OH II	SFR		1993 April - 1994 September
18	16 00 29.3	-52 44 39	329.3317	0.1546	G329.339+0.148	329.33+0.15	Image	Descr	6.6 GHz (II);	-107;-10	-106.5	14	8.3	Hobart_26m	420	-H₂O -CH₃OH I +CH₃OH II +OH	SFR_MIXED		1993 April - 1994 September
19	16 03 36.5	-53 08 58	329.4192	-0.4598	G329.405-0.459	329.41-0.46	Image	Descr	6.6 GHz (II);	-71;-66	-66.8	144	106	Hobart_26m	420	+H₂O -CH₃OH I +CH₃OH II +OH	SFR		1993 April - 1994 September
20	15 59 39.9	-52 22 45	329.4751	0.5129	G329.469+0.503	329.48+0.51	Image	Descr	6.6 GHz (II);	-73;-65	-72.1	13	17.1	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II	SFR		1993 April - 1994 September
21	16 02 7.3	-52 35 13	329.6218	0.1109	G329.610+0.114	329.62+0.11	Image		6.6 GHz (II);	-69;-59	-60.1	30	26.5	Hobart_26m	420	-H₂O -CH₃OH I +CH₃OH II	SFR		1993 April - 1994 September
22	16 09 53.3	-51 55 38	330.9469	-0.1921	G330.954-0.182	330.95-0.18	Image	Descr	6.6 GHz (II);	-89;-87	-87.6	7	4.1	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 April - 1994 September
23	16 11 0.7	-51 51 18	331.1231	-0.2568	G331.132-0.244	331.13-0.24	Image	Descr	6.6 GHz (II);	-92;-84	-84.4	34	43.3	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 April - 1994 September
24	16 11 22.3	-51 42 26	331.2646	-0.1866	G331.278-0.188	331.28-0.19	Image	Descr	6.6 GHz (II);	-86;-78	-78.1	165	250.3	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 April - 1994 September
25	16 12 23.3	-51 46 11	331.3369	-0.3397	G331.342-0.346	331.34-0.35	Image	Descr	6.6 GHz (II);	-68;-64	-67.4	66	124.9	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		1993 April - 1994 September
26	16 10 10.3	-51 16 18	331.4238	0.2598	G331.425+0.264	331.42+0.26	Image	Descr	6.6 GHz (II);	-91;-88	-88.6	25	19.9	Hobart_26m	420	+H₂O -CH₃OH I +CH₃OH II	EVOLVED		1993 April - 1994 September
27	16 12 14.6	-51 34 39	331.4519	-0.1841	G331.442-0.187	331.45-0.18	Image	Descr	6.6 GHz (II);	-93;-84	-88.5	70	158	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 April - 1994 September
28	16 12 10.9	-51 25 24	331.5503	-0.0650	G331.543-0.066	331.54-0.07	Image	Descr	6.6 GHz (II);	-87;-83	-84.1	12	12.5	Hobart_26m	420	-H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 April - 1994 September
29	16 12 28.7	-51 27 04	331.5651	-0.1169	G331.556-0.121	331.56-0.12	Image	Descr	6.6 GHz (II);	-105;-94	-103.4	35	46	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 April - 1994 September
30	16 16 19.3	-51 17 50	332.1058	-0.4187	G332.094-0.421	332.11-0.42	Image	Descr	6.6 GHz (II);	-62;-58	-61.4	16	16.8	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II	SFR		1993 April - 1994 September
31	16 15 50.5	-50 55 26	332.3103	-0.0974	G332.295-0.094	332.31-0.10		Descr	6.6 GHz (II);	-47;-42	-47	6.3	8.3	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II	GALAXY		1993 April - 1994 September
32	16 17 29.3	-51 09 24	332.3348	-0.4447	G332.335-0.445	332.33-0.44		Descr	6.6 GHz (II);		-53.8	4	4.5	Hobart_26m	420	+CH₃OH II	SFR		1993 April - 1994 September
33	16 17 19.2	-50 46 33	332.5810	-0.1529	G332.581-0.153	332.58-0.15		Descr	6.6 GHz (II);	-56;-49	-51	5	5.6	Hobart_26m	420	+CH₃OH II	UNK		1993 April - 1994 September
34	16 21 19.9	-50 53 40	332.9495	-0.6816	G332.963-0.680	332.95-0.68		Descr	6.6 GHz (II);	-54;-52	-52.9	21	14.9	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II	SFR		1993 April - 1994 September
35	16 21 23.2	-50 53 02	332.9631	-0.6802	G332.963-0.680	332.96-0.68		Descr	6.6 GHz (II);	-48;-38	-45.9	41	49.2	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II	SFR		1993 April - 1994 September
36	16 18 47.3	-50 21 56	333.0343	-0.0219	G333.029-0.015	333.03-0.02		Descr	6.6 GHz (II);	-61;-53	-53.6	3	6.3	Hobart_26m	420	+CH₃OH I +CH₃OH II	SFR		1993 April - 1994 September
37	16 20 53.7	-50 37 32	333.0902	-0.4423	G333.090-0.442	333.07-0.45	Image	Descr	6.6 GHz (II);	-55;-53	-54.5	12	7.7	Hobart_26m	420	+CH₃OH II			1993 April - 1994 September
38	16 20 59.5	-50 35 47	333.1217	-0.4324	G333.127-0.434	333.12-0.43	Image	Descr	6.6 GHz (II);	-50;-48	-49.3	11	11.6	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 April - 1994 September
39	16 21 2.7	-50 35 54	333.1263	-0.4397	G333.127-0.434	333.13-0.44	Image	Descr	6.6 GHz (II);	-45;-42	-44.4	3	1.9	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 April - 1994 September
40	16 21 39.1	-50 40 06	333.1450	-0.5572	G333.130-0.560	333.15-0.56	Image	Descr	6.6 GHz (II);	-63;-52	-56.8	17	14.9	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II	SFR		1993 April - 1994 September
41	16 19 41.7	-50 19 53	333.1614	-0.0989	G333.163-0.101	333.16-0.10	Image	Descr	6.6 GHz (II);	-95;-91	-95.3	8	3.7	Hobart_26m	420	+CH₃OH I +CH₃OH II	SFR		1993 April - 1994 September
42	16 19 46.3	-50 17 20	333.2000	-0.0772	G333.184-0.091	333.20-0.08	Image	Descr	6.6 GHz (II);	-85;-81	-82	6.5	5	Hobart_26m	420	+CH₃OH I +CH₃OH II	SFR		1993 April - 1994 September
43	16 19 51	-50 15 18	333.2327	-0.0619	G333.234-0.061	333.23-0.06	Image	Descr	6.6 GHz (II);	-92;-81	-81.9	4.7	3	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 April - 1994 September
44	16 19 31.7	-50 04 03	333.3276	0.1078	G333.315+0.105	333.33+0.11	Image	Descr	6.6 GHz (II);	-50;-41	-43.7	9	24.7	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 April - 1994 September
45	16 21 18.1	-50 09 47	333.4624	-0.1601	G333.466-0.164	333.47-0.17	Image	Descr	6.6 GHz (II);	-49;-37	-42.4	41	39.2	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 April - 1994 September
46	16 21 13.7	-49 58 49	333.5830	-0.0223	G333.583-0.022	333.58-0.02	Image	Descr	6.6 GHz (II);	-37;-34	-35.9	39	58	Hobart_26m	420	+CH₃OH II	SFR		1993 April - 1994 September
47	16 23 32.6	-50 12 05	333.6885	-0.4414	G333.683-0.437	333.69-0.44	Image		6.6 GHz (II);	-6;-4	-5.2	19	13.2	Hobart_26m	420	+H₂O -CH₃OH I +CH₃OH II	SFR		1993 April - 1994 September
48	16 23 19.5	-49 48 14	333.9464	-0.1368	G333.931-0.135	333.95-0.14	Image		6.6 GHz (II);	-37;-36	-36.8	7	4.3	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II	SFR		1993 April - 1994 September
49	16 25 51.1	-49 13 07	334.6513	-0.0193	G334.635-0.015	334.65-0.02	Image		6.6 GHz (II);	-31;-27	-30.1	61	53.5	Hobart_26m	420	+H₂O -CH₃OH I +CH₃OH II	EVOLVED		1993 April - 1994 September
50	16 29 28.9	-49 11 36	335.0806	-0.4290	G335.060-0.427	335.08-0.43	Image		6.6 GHz (II);	-48;-39	-47	15	16.5	Hobart_26m	420	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		1993 April - 1994 September

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 ELL96B

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