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SUA09 - Water maser detections in southern candidate post-AGB stars and planetary nebulae

Short title: Suarez et al. (2009)
Authors: Suarez, O. Gomez, J. F. Miranda, L. F. Torrelles, J. M. Gómez, Y. Anglada, G. Morata, O.
Journal: Astronomy and Astrophysics, Volume 505, Issue 1, 2009, pp.217-225
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Detection table: Show detection table (6 detection)

Abstract
Aims: We study the incidence and characteristics of water masers in the envelopes of stars in the post-AGB and PN evolutionary stages. Methods: We used the 64-m antenna in Parkes (Australia) to search for water maser emission at 22 GHz, towards a sample of 74 sources with IRAS colours characteristic of post-AGB stars and PNe, at declination < -32 deg. In our sample, 39% of the sources are PNe or PNe candidates, and 50% are post-AGB stars or post-AGB candidates. Results: We detected four new water masers, all of them in optically obscured sources: three are in PNe candidates (IRAS 12405-6219, IRAS 15103-5754, and IRAS 16333-4807) and one is in a post-AGB candidate (IRAS 13500-6106). The PN candidate IRAS 15103-5754 has water fountain characteristics and could be the first PN of this class found. Conclusions: We confirm the trend suggested in Paper I that water maser emission during the post-AGB phase is more likely to be present in obscured sources with massive envelopes than in objects with optical counterpart. We propose an evolutionary scenario for water masers in the post-AGB and PNe stages, in which ""water fountain"" masers could develop during the post-AGB and early PN stages. Later PNe would exhibit lower velocity maser emission, both along jets and close to the central objects, with only the central masers remaining in more evolved PNe. eprintid: arXiv:0906.3031

Abstract

Aims: We study the incidence and characteristics of water masers in the envelopes of stars in the post-AGB and PN evolutionary stages.
Methods: We used the 64-m antenna in Parkes (Australia) to search for water maser emission at 22 GHz, towards a sample of 74 sources with IRAS colours characteristic of post-AGB stars and PNe, at declination < -32 deg. In our sample, 39% of the sources are PNe or PNe candidates, and 50% are post-AGB stars or post-AGB candidates.
Results: We detected four new water masers, all of them in optically obscured sources: three are in PNe candidates (IRAS 12405-6219, IRAS 15103-5754, and IRAS 16333-4807) and one is in a post-AGB candidate (IRAS 13500-6106). The PN candidate IRAS 15103-5754 has water fountain characteristics and could be the first PN of this class found.
Conclusions: We confirm the trend suggested in Paper I that water maser emission during the post-AGB phase is more likely to be present in obscured sources with massive envelopes than in objects with optical counterpart. We propose an evolutionary scenario for water masers in the post-AGB and PNe stages, in which ""water fountain"" masers could develop during the post-AGB and early PN stages. Later PNe would exhibit lower velocity maser emission, both along jets and close to the central objects, with only the central masers remaining in more evolved PNe. eprintid:

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Detection table from Suarez et al. (2009)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	V_range	V_peak	F_peak	∫F dv	RMS	Detection
	(J2000)	(J2000)	(deg.)	(deg.)			(km/s)	(km/s)	(Jy)	(Jy*km/s)	(Jy)	Yes/No
1	12 43 31.5	-62 36 14	302.0218	0.2539	G302.022+0.254	IRAS 12405-6219		-23.6	0.94	11.1	0.120	+H₂O -CH₃OH II
2	13 53 34.5	-61 20 52	310.3104	0.6306	G310.310+0.631	IRAS 13500-6106		39.9	0.8	8.9	0.150	+H₂O -CH₃OH II -OH
	13 53 34.5	-61 20 52	310.3104	0.6306	G310.310+0.631	IRAS 13500-6106		40.0	1.6	6.7	0.230	+H₂O -CH₃OH II -OH
3	15 14 18.5	-58 05 20	320.9066	-0.2928	G320.906-0.293	IRAS 15103-5754	80.0	-35.8	60.3	1327.6	0.240	+H₂O -OH
	15 14 18.5	-58 05 20	320.9066	-0.2928	G320.906-0.293	IRAS 15103-5754	80.0	-35.8	36.7	704.6	0.600	+H₂O -OH
4	16 37 6.1	-48 13 42	336.6430	-0.6944	G336.644-0.695	IRAS 16333-4807		-42.2	1.8	26	0.200	+H₂O +OH

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 SUA09

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