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ZIJ89 - OH maser emission from young planetary nebulae

Short title: Zijlstra et al. (1989)
Authors: Zijlstra, A. A. te Lintel Hekkert, P. Pottasch, S. R. Caswell, J. L. Ratag, M. Habing, H. J.
Journal: Astronomy and Astrophysics (ISSN 0004-6361), vol. 217, no. 1-2, June 1989, p. 157-178. Research supported by ZWO.
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Abstract
OH emission, primarily in the 1612 MHz satellite line and also in the main lines, is detected in a number of young planetary nebulae. These objects form a direct observational link between the evolved OH/IR stars and planetary nebulae. In this paper, the observations are presented and the implications for various aspects of Post-Asymptotic Giant Branch evolution are discussed. Lifetimes and birthrates of this evolutionary stage are calculated. A scheme for classifying preplanetary nebula objects is proposed.	Comments: Velocity resolution: 0.8, 0.9 and 1.1 km/s Upper limit for non-detections: 0.2 Jy (3σ)

Abstract

OH emission, primarily in the 1612 MHz satellite line and also in the main lines, is detected in a number of young planetary nebulae. These objects form a direct observational link between the evolved OH/IR stars and planetary nebulae. In this paper, the observations are presented and the implications for various aspects of Post-Asymptotic Giant Branch evolution are discussed. Lifetimes and birthrates of this evolutionary stage are calculated. A scheme for classifying preplanetary nebula objects is proposed.

Comments:
Velocity resolution: 0.8, 0.9 and 1.1 km/s
Upper limit for non-detections: 0.2 Jy (3σ)

Input tables: Table 3 and Figure 1
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Detection table from Zijlstra et al. (1989)

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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 13 44.8	-37 06 13	349.5093	1.0546	G349.509+1.055	NGC6302	1612	40.0	-40.0	0.500	ENG15	-H₂O -CH₃OH II +OH	EVOLVED		ZIJ89
2	17 18 29	-37 58 01	349.3517	-0.2112	G349.352-0.211	OH349.36-0.20	1612	126.0	-126.0	0.500	ENG15	-H₂O -CH₃OH II +OH	EVOLVED		ZIJ89
	17 18 29	-37 58 01	349.3517	-0.2112	G349.352-0.211	OH349.36-0.20	1667	130.0	-130.0	0.800	ENG15	-H₂O -CH₃OH II +OH	EVOLVED		ZIJ89
	17 18 29	-37 58 01	349.3517	-0.2112	G349.352-0.211	OH349.36-0.20	1665	129.0	-129.0	0.100	ENG15	-H₂O -CH₃OH II +OH	EVOLVED		ZIJ89
5	17 23 55.6	-28 59 32	357.3844	3.9603	G357.385+3.960	IRAS 17207-2856	1612	18.0	-18.0	0.400	ENG15	-CH₃OH II +OH	EVOLVED		ZIJ89
6	17 25 18.9	-30 40 43	356.1541	2.7661	G356.154+2.766	IRAS 17221-3038	1612	33.0	-15.0	0.200	ENG15	-H₂O +OH	EVOLVED		ZIJ89
7	17 38 1.2	-31 40 58	356.8016	-0.0575	G356.802-0.055	IRAS 17347-3139	1612	120.0	-120.0	0.600	ENG15	+H₂O +OH	SFR_MIXED		ZIJ89
8	17 40 20.6	-27 49 11	0.3396	1.5742	G0.344+1.566	IRAS 17371-2747	1612	115.0	115.0	0.800	ENG15	-H₂O +OH	EVOLVED		ZIJ89
9	17 40 40.7	-28 01 06	0.2104	1.4062	G0.210+1.406	IRAS 17375-2759	1612	21.0	21.0	1.000	ENG15	+OH	EVOLVED		ZIJ89
10	17 40 44.3	-30 02 07	358.5066	0.3263	G358.507+0.326	IRAS 17375-3000	1612	20.0	-36.0	2.800	ENG15	-H₂O +OH	EVOLVED		ZIJ89
11	17 42 32.1	-27 28 28	0.8894	1.3445	G0.890+1.344	OH0.9+1.3	1612	31.0	-124.0	54.000	ENG15	+H₂O -CH₃OH I -CH₃OH II +OH	EVOLVED		ZIJ89
	17 42 32.1	-27 28 28	0.8894	1.3445	G0.890+1.344	OH0.9+1.3	1667	125.0	-125.0	1.200	ENG15	+H₂O -CH₃OH I -CH₃OH II +OH	EVOLVED		ZIJ89
13	17 47 35.2	-29 50 56	359.4424	-0.8400	G359.442-0.840	IRAS 17443-2949	1612	15.0	-15.0	1.200	ENG15	+H₂O +OH	SFR_MIXED		ZIJ89
14	18 01 19.5	-31 11 20	359.7783	-4.0705	G359.778-4.071	IRAS 17580-3111	1612	16.0	13.0	2.200	ENG15	+H₂O +OH	EVOLVED		ZIJ89
15	19 24 21.9	+09 53 54	45.4969	-2.7023	G45.497-2.702	Vy2-2	1612	62.0	-62.0	5.000	ENG15	-H₂O +OH	EVOLVED		ZIJ89

Non-detection table from Zijlstra et al. (1989)