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BLO94 - A deep VLA search for OH (1612 MHz) maser sources in the galactic plane

Short title: Blommaert et al. (1994)
Authors: Blommaert, J. A. D. L. van Langevelde, H. J. Michiels, W. F. P.
Journal: Astronomy and Astrophysics (ISSN 0004-6361), vol. 287, no. 2, p. 479-492
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (44 detection)

Abstract
The results of a Very Large Array (VLA) OH (1612 MHz) search for OH/IR stars in 7 fields along the galactic plane are presented. Forty-four sources were detected of which 35 were not previously known. It is shown that 'blind' radio interferometric observ- ations (such as with the VLA) are capable of filling up the gap in the IRAS based OH surveys near the galactic plane. This is important for the dynamical modeling of the disc and bulge of our Galaxy. It is also demonstrated that the high resolution of a synthesis telescope is needed to avoid confusion in the galactic plane. Most detected sources are likely to be young (approximately less than 1 Gyr) and massive (M_ms greater than 2-3 solar masses) evolved stars and have high expansion velocities (v_exp greater than 14.5 km/s) and small deviations (less than 10 km/s) from galactic rotation. Like Baud et al. (1981) we find a peak in the number of sources around l = 25 deg, a region associated with active star formation and a low number of stars at l = 5 deg and 10 deg.	Comments: Spectral type was set to: ""S"", where only one peak was found. ""D"", where two peaks were found. Velocity resolution: 2.27 km/s

Abstract

The results of a Very Large Array (VLA) OH (1612 MHz) search for OH/IR stars in 7 fields along the galactic plane are presented. Forty-four sources were detected of which 35 were not previously known. It is shown that 'blind' radio interferometric observ- ations (such as with the VLA) are capable of filling up the gap in the IRAS based OH surveys near the galactic plane. This is important for the dynamical modeling of the disc and bulge of our Galaxy. It is also demonstrated that the high resolution of a synthesis telescope is needed to avoid confusion in the galactic plane. Most detected sources are likely to be young (approximately less than 1 Gyr) and massive (M_ms greater than 2-3 solar masses) evolved stars and have high expansion velocities (v_exp greater than 14.5 km/s) and small deviations (less than 10 km/s) from galactic rotation. Like Baud et al. (1981) we find a peak in the number of sources around l = 25 deg, a region associated with active star formation and a low number of stars at l = 5 deg and 10 deg.

Comments:
Spectral type was set to:
""S"", where only one peak was found.
""D"", where two peaks were found.

Velocity resolution: 2.27 km/s

Input tables: Table 2
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Detection table from Blommaert et al. (1994)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Frequency	V_range	V_peak	F_peak	List	Detection	Class	Dist. (parallax)	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			(MHz)	(km/s)	(km/s)	(Jy)		Yes/No		(kpc)
1	17 55 40.3	-24 38 8.6	4.8420	0.2769	G4.842+0.277	OH4.843+0.277	1612	27.2	118.1	0.288	ENG15	+OH	EVOLVED		BLO94
2	17 56 50.2	-24 28 56.5	5.1078	0.1251	G5.108+0.125	OH5.104+0.122	1612	9.1	-11.3	0.062	ENG15	+OH	EVOLVED		BLO94
3	17 57 3.2	-24 40 50.6	4.9610	-0.0171	G4.961-0.017	OH4.961-0.017	1612	40.9	-74.9	0.177	ENG15	+OH	EVOLVED		BLO94
4	18 07 23.1	-20 25 51.2	9.8340	0.0086	G9.834+0.009	OH9.835+0.008	1612	38.6	59.1	0.037	ENG15	+OH	EVOLVED		BLO94
5	18 07 59	-20 27 33.6	9.8773	-0.1277	G9.877-0.128	OH9.878-0.127	1612	31.8	79.5	0.880	ENG15	+OH	EVOLVED		BLO94
6	18 08 3.2	-20 17 47.3	10.0276	-0.0629	G10.028-0.063	OH10.028-0.063	1612	20.4	-2.2	0.694	ENG15	+OH	EVOLVED		BLO94
7	18 08 16.3	-20 16 11.3	10.0758	-0.0947	G10.076-0.095	OH10.077-0.095	1612	54.5	25.0	0.948	ENG15	+H₂O +OH	EVOLVED		BLO94
8	18 16 41.6	-16 04 8.4	14.7209	0.1686	G14.721+0.168	OH14.724+0.168	1612	25.0	109.0	0.458	ENG15	-CH₃OH II +OH	EVOLVED		BLO94
9	18 16 57.9	-15 53 23.2	14.9096	0.1963	G14.910+0.196	OH14.910+0.196	1612	129.4	129.4	0.100	ENG15	+OH	EVOLVED		BLO94
10	18 17 20.7	-15 51 2.5	14.9874	0.1344	G14.987+0.134	OH14.988+0.134	1612	31.7	11.4	0.140	ENG15	+OH	EVOLVED		BLO94
11	18 17 36.2	-15 48 27.4	15.0548	0.1002	G15.053+0.086	OH15.059+0.099	1612	13.6	109.0	0.028	ENG15	-H₂O +OH	SFR_MIXED		BLO94
12	18 17 41.2	-16 00 05	14.8937	-0.0094	G14.894-0.009	OH14.895-0.009	1612	34.0	104.5	0.111	ENG15	+OH	EVOLVED		BLO94
13	18 18 10.5	-16 08 12.9	14.8300	-0.1769	G14.830-0.177	OH14.831-0.177	1612	22.7	-59.0	0.827	ENG15	+OH	EVOLVED		BLO94
14	18 18 45.4	-15 53 23.4	15.1138	-0.1830	G15.114-0.183	OH15.117-0.183	1612	38.6	72.7	0.086	ENG15	+OH	EVOLVED		BLO94
15	18 22 32	-13 23 56.8	17.7410	0.1853	G17.741+0.185	OH17.741+0.185	1612	34.0	6.9	0.549	ENG15	+OH	EVOLVED		BLO94
16	18 22 41.1	-13 40 58.1	17.5078	0.0196	G17.508+0.019	OH17.508+0.020	1612	29.5	52.3	1.141	ENG15	+OH +SiO	EVOLVED		BLO94
17	18 22 47.5	-14 06 35.7	17.1428	-0.2037	G17.140-0.198	OH17.146-0.200	1612	99.8	-99.8	0.906	ENG15	-CH₃OH II +OH	EVOLVED		BLO94
18	18 22 53.1	-13 47 45.3	17.4307	-0.0764	G17.432-0.077	OH17.434-0.077	1612	127.2	127.2	0.023	ENG15	+OH	SFR_MIXED		BLO94
19	18 23 17.8	-13 42 48.5	17.5504	-0.1260	G17.551-0.126	OH17.551-0.126	1612	31.8	27.3	1.522	ENG15	+H₂O +OH +SiO	EVOLVED		BLO94
20	18 23 23.6	-13 55 10.1	17.3795	-0.2433	G17.380-0.243	OH17.383-0.243	1612	118.1	118.1	0.125	ENG15	+OH	EVOLVED		BLO94
21	18 23 34.8	-13 55 52.3	17.3904	-0.2888	G17.391-0.289	OH17.392-0.289	1612	31.8	13.7	2.409	ENG15	+OH +SiO	EVOLVED		BLO94
22	18 31 38.2	-09 07 36.1	22.5611	0.2005	G22.559+0.201	OH22.560+0.201	1612	29.5	81.8	0.067	ENG15	+OH	EVOLVED		BLO94
23	18 31 49.2	-08 56 51.3	22.7408	0.2432	G22.741+0.240	OH22.742+0.237	1612	152.1	152.1	0.218	ENG15	+OH	EVOLVED		BLO94
24	18 32 0.6	-09 18 21.4	22.4447	0.0359	G22.445+0.035	OH22.446+0.035	1612	29.5	120.4	0.649	ENG15	+OH	EVOLVED		BLO94
25	18 32 7.3	-09 27 09	22.3275	-0.0562	G22.322-0.049	OH22.328-0.057	1612	38.6	52.3	0.210	ENG15	+OH -SiO	SFR_MIXED		BLO94
26	18 32 12.6	-09 18 54.6	22.4593	-0.0121	G22.459-0.012	OH22.458-0.011	1612	29.5	90.9	0.058	ENG15	+OH	SFR_MIXED		BLO94
27	18 32 22.6	-09 27 43.9	22.3479	-0.1165	G22.348-0.117	OH22.349-0.117	1612	40.9	25.0	0.875	ENG15	+OH	EVOLVED		BLO94
28	18 33 40.2	-09 09 6.2	22.7706	-0.2562	G22.766-0.253	OH22.772-0.256	1612	31.8	77.2	1.545	ENG15	-H₂O -CH₃OH II +OH	SFR_MIXED		BLO94
29	18 35 54.3	-06 56 47.5	24.9828	0.2683	G24.983+0.268	OH24.978+0.261	1612	36.3	22.8	0.129	ENG15	+OH	EVOLVED		BLO94
30	18 35 57.3	-07 18 55.3	24.6610	0.0876	G24.661+0.087	OH24.661+0.089	1612	31.8	40.9	4.001	ENG15	+OH +SiO	EVOLVED		BLO94
31	18 35 59	-06 53 14.1	25.0444	0.2783	G25.044+0.278	OH25.046+0.278	1612	40.9	72.7	0.245	ENG15	+H₂O +OH +SiO	EVOLVED		BLO94
32	18 36 3.6	-07 05 17.8	24.8746	0.1689	G24.875+0.168	OH24.875+0.170	1612	36.3	75.0	0.196	ENG15	+OH	EVOLVED		BLO94
33	18 36 19.8	-07 11 51.7	24.8083	0.0592	G24.809+0.058	OH24.809+0.060	1612	40.9	70.4	0.308	ENG15	+CH₃OH II +OH	SFR_MIXED		BLO94
34	18 36 30.1	-07 18 47.9	24.7252	-0.0318	G24.725-0.032	OH24.726-0.030	1612	25.0	-31.7	0.394	ENG15	+OH	SFR_MIXED		BLO94
35	18 36 45.8	-07 18 16.8	24.7627	-0.0855	G24.763-0.086	OH24.762-0.085	1612	45.4	63.6	0.444	ENG15	+H₂O -CH₃OH II +OH +SiO	SFR_MIXED		BLO94
36	18 36 57.8	-06 53 23.9	25.1538	0.0610	G25.156+0.060	OH25.154+0.061	1612	29.5	72.7	3.322	ENG15	-H₂O -CH₃OH I -CH₃OH II +OH	SFR_MIXED		BLO94
37	18 37 10.6	-07 06 43	24.9809	-0.0880	G24.981-0.088	OH24.981-0.088	1612	27.2	115.9	0.367	ENG15	+OH	EVOLVED		BLO94
38	18 37 13.2	-06 59 0.8	25.0999	-0.0385	G25.100-0.039	OH25.100-0.040	1612	52.2	75.0	0.423	ENG15	+H₂O -CH₃OH II +OH	EVOLVED		BLO94
39	18 37 25.2	-07 07 45.9	24.9931	-0.1496	G24.993-0.150	OH24.993-0.150	1612	36.3	106.7	0.949	ENG15	+OH	EVOLVED		BLO94
40	18 37 58.2	-06 52 28.6	25.2822	-0.1539	G25.279-0.153	OH25.284-0.156	1612	102.2	102.2	0.312	ENG15	-H₂O +OH +SiO	EVOLVED		BLO94
41	18 46 12.2	-02 41 21	29.9421	-0.0625	G29.933-0.064	OH29.938-0.062	1612	102.2	102.2	0.090	ENG15	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		BLO94
42	18 46 24.8	-02 59 27.1	29.6976	-0.2468	G29.697-0.242	OH29.699-0.241	1612	115.9	115.9	0.804	ENG15	+OH	SFR_MIXED		BLO94
43	18 46 33.3	-02 33 12.4	30.1029	-0.0787	G30.103-0.079	OH30.103-0.078	1612	27.2	22.8	0.977	ENG15	-H₂O +CH₃OH II +OH	SFR_MIXED		BLO94
44	18 47 9.8	-02 35 35.8	30.1368	-0.2320	G30.137-0.232	OH30.137-0.231	1612	34.0	34.1	12.095	ENG15	+H₂O -CH₃OH II +OH +SiO	SFR_MIXED		BLO94

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 BLO94

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