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LIN96 - A search for OH maser emission from post-asymptotic giant branch stars.

Short title: te Lintel Hekkert & Chapman (1996)
Authors: te Lintel Hekkert, P. Chapman, J. M.
Journal: Astronomy and Astrophysics Supplement, v.119, p.459-481
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Abstract
We present a survey for OH maser emission at 18cm in the direction of 196 IRAS point sources. The primary aim of the survey was to detect OH maser emission from post-asymptotic giant branch (post-AGB) stars. OH emission and/or absorption was detected in the direction of 77 sources of which 57 OH detections were previously unknown, giving an overall detection rate of 39 per cent. Fourteen maser sources associated with evolved stars or planetary nebulae were found, corresponding to 7 per cent of the total observed. These included three planetary nebulae (two new OH detections), nine post-AGB stars (three new OH detections) and two cold OH/IR stars (both previously known). Two sources were of uncertain identification (both new OH detections). The remainder of the OH sources were identified with young stellar objects and with HII regions. The survey included the detection of OH maser emission from HD 101584, an early-type supergiant at high Galactic latitude. For several of the post-AGB stars, changes have occurred in the OH spectral profiles over a period of several years. This is interpreted as evidence for rapid changes in the stellar winds, due either to interactions with stellar companions, novae-like events or rapid stellar evolution.	Comments: IRAS 15103-5754, classified as HII region, is included, as it is now considered to be a post-AGB star. Velocity resolution: 0.90 km/s Upper limit for non-detections: mostly <0.300 Jy (3σ) Entries for IRAS 15103-5754 and 17423-1755 taken from the spectrum.

Abstract

We present a survey for OH maser emission at 18cm in the direction of 196 IRAS point sources. The primary aim of the survey was to detect OH maser emission from post-asymptotic giant branch (post-AGB) stars. OH emission and/or absorption was detected in the direction of 77 sources of which 57 OH detections were previously unknown, giving an overall detection rate of 39 per cent. Fourteen maser sources associated with evolved stars or planetary nebulae were found, corresponding to 7 per cent of the total observed. These included three planetary nebulae (two new OH detections), nine post-AGB stars (three new OH detections) and two cold OH/IR stars (both previously known). Two sources were of uncertain identification (both new OH detections). The remainder of the OH sources were identified with young stellar objects and with HII regions. The survey included the detection of OH maser emission from HD 101584, an early-type supergiant at high Galactic latitude. For several of the post-AGB stars, changes have occurred in the OH spectral profiles over a period of several years. This is interpreted as evidence for rapid changes in the stellar winds, due either to interactions with stellar companions, novae-like events or rapid stellar evolution.

Comments:
IRAS 15103-5754, classified as HII region, is included, as it is now considered to be a post-AGB star.

Velocity resolution: 0.90 km/s
Upper limit for non-detections: mostly <0.300 Jy (3σ)
Entries for IRAS 15103-5754 and 17423-1755 taken from the spectrum.

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Detection table from te Lintel Hekkert & Chapman (1996)

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ID	Obs. RA	Obs. Dec	l	b	Group id	grpv	Source name	Line	Frequency	V_range	V_peak	F_peak	List	Detection	Class	Dist. (parallax)	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)				OH	(MHz)	(km/s)	(km/s)	(Jy)		Yes/No		(kpc)
1	07 42 17.1	-14 42 50	231.8355	4.2208	G231.835+4.220	G231.8354+4.2204	IRAS 07399-1435	1612 MHz;	1612	21.1	21.1	0.550	ENG15	+H₂O -CH₃OH II +OH +SiO	EVOLVED		LIN96
2	07 42 17.1	-14 42 50	231.8355	4.2208	G231.835+4.220	G231.8354+4.2204	IRAS 07399-1435	1667 MHz;	1667	19.0	19.0	13.730	ENG15	+H₂O -CH₃OH II +OH +SiO	EVOLVED		LIN96
3	14 50 42.1	-60 16 52	317.2032	-0.7566	G317.203-0.757	G317.2032-0.7566	IRAS 14468-6004	1612 MHz;	1612	87.9	-87.9	2.000	ENG15	-CH₃OH II +OH	UNK		LIN96
4	15 44 11.1	-49 55 20	329.1424	3.9498	G329.142+3.950	G329.1424+3.9498	IRAS 15405-4945	1665 MHz;	1665	37.8	37.8	2.310	ENG15	-CH₃OH II +OH	EVOLVED		LIN96
5	15 44 11.1	-49 55 20	329.1424	3.9498	G329.142+3.950	G329.1424+3.9498	IRAS 15405-4945	1667 MHz;	1667	15.7	-15.7	0.670	ENG15	-CH₃OH II +OH	EVOLVED		LIN96
6	16 37 40	-38 20 17	344.0737	5.8466	G344.074+5.847	G344.0737+5.8466	IRAS 16342-3814	1612 MHz;	1612	10.2	-10.2	9.000	ENG15	+H₂O +OH -SiO	EVOLVED		LIN96
7	16 37 40	-38 20 17	344.0737	5.8466	G344.074+5.847	G344.0737+5.8466	IRAS 16342-3814	1667 MHz;	1667	6.1	6.1	2.220	ENG15	+H₂O +OH -SiO	EVOLVED		LIN96
8	17 03 55.9	-41 23 59	344.9287	0.0145	G344.929+0.014	G344.9291+0.0137	IRAS 17004-4119	1612 MHz;	1612	21.1	-21.1	115.000	ENG15	+H₂O +OH	SFR_MIXED		LIN96
9	17 13 44.8	-37 06 13	349.5093	1.0546	G349.509+1.055	G349.5093+1.0555	IRAS 17103-3702	1667 MHz;	1667	45.7	-45.7	0.160	ENG15	-H₂O -CH₃OH II +OH	UNK		LIN96
10	17 21 11.4	-27 11 38	358.5355	5.4710	G358.536+5.471	G358.5355+5.4710	IRAS 17180-2708	1667 MHz;	1667	85.6	85.6	1.320	ENG15	-CH₃OH II +OH	UNK		LIN96
11	17 45 14.1	-17 56 47	9.3641	5.7789	G9.364+5.779	G9.3641+5.7789	IRAS 17423-1755	1667 MHz;	1667	47.0	47.0	0.700	ENG15	-H₂O -CH₃OH I +OH	UNK		LIN96
12	18 51 46.8	-02 04 09	31.1292	-1.0194	G31.127-1.016	G31.1292-1.0194	IRAS 18491-0207	1667 MHz;	1667	63.1	63.1	1.350	ENG15	-H₂O -CH₃OH II +OH	EVOLVED		LIN96
13	19 45 52.1	+24 17 40	60.5740	-0.1858	G60.574-0.186	G60.5750-0.1862	IRAS 19437+2410	1665 MHz;	1665	1.7	1.7	0.780	ENG15	+H₂O -CH₃OH I +CH₃OH II +OH	SFR_MIXED		LIN96
14	20 29 7.9	+35 45 39	75.2660	-1.8413	G75.268-1.842	G75.2678-1.8419	IRAS 20272+3535	1612 MHz;	1612	15.0	-15.0	6.600	ENG15	-H₂O -CH₃OH II +OH	EVOLVED		LIN96
15	22 05 30.5	+53 21 33	99.6338	-1.8356	G99.634-1.836	G99.6338-1.8356	IRAS 22036+5306	1612 MHz;	1612	66.9	-66.9	0.830	ENG15	-H₂O -CH₃OH II +OH	EVOLVED		LIN96
16	22 05 30.5	+53 21 33	99.6338	-1.8356	G99.634-1.836	G99.6338-1.8356	IRAS 22036+5306	1667 MHz;	1667	68.1	-68.1	0.630	ENG15	-H₂O -CH₃OH II +OH	EVOLVED		LIN96

Non-detection table from te Lintel Hekkert & Chapman (1996)