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SUA07 - New detections of H2O masers in planetary nebulae and post-AGB stars using the Robledo-70 m antenna

Short title: Suarez et al. (2007)
Authors: Suarez, O. Gomez, J. F. Morata, O.
Journal: Astronomy and Astrophysics, Volume 467, Issue 3, June I 2007, pp.1085-1091
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Non-detection table: Show non-detection table
Detection table: Show detection table (11 detection)
Target type: pAGB_PN

Abstract
Aims:We investigated the possible relationship between the evolutionary stage of post-AGB stars and planetary nebulae (PNe) and the presence of water masers in their envelopes Methods: We have used NASA's 70-m antenna in Robledo de Chavela (Spain) to search for the water maser transition at 22 235.08 MHz, towards a sample of 105 sources with IRAS colour characteristic of post-AGB stars and PNe at declination >-32. 83% of the sources in the sample are post-AGB stars, 15% PNe or PN candidates, while only 2% seem to be HII regions. Results: We have detected five water masers, of which four are reported for the first time: two in PNe (IRAS 17443-2949 and IRAS 18061-2505), a ``water fountain'' in a post-AGB star (IRAS 16552-3050), and one in a source previously catalogued as a PN, but whose classification is uncertain (IRAS 17580-3111). Conclusions: The unexpected detections of water masers in two objects among the small subset of PNe led us to suggest that the PNe harbouring water masers are a special type of massive, rapidly evolving PNe. Tables 1 and 3 are only available in electronic form at http://www.aanda.org eprintid: arXiv:astro-ph/0703502

Abstract

Aims:We investigated the possible relationship between the evolutionary stage of post-AGB stars and planetary nebulae (PNe) and the presence of water masers in their envelopes Methods: We have used NASA's 70-m antenna in Robledo de Chavela (Spain) to search for the water maser transition at 22 235.08 MHz, towards a sample of 105 sources with IRAS colour characteristic of post-AGB stars and PNe at declination >-32. 83% of the sources in the sample are post-AGB stars, 15% PNe or PN candidates, while only 2% seem to be HII regions.
Results: We have detected five water masers, of which four are reported for the first time: two in PNe (IRAS 17443-2949 and IRAS 18061-2505), a ``water fountain'' in a post-AGB star (IRAS 16552-3050), and one in a source previously catalogued as a PN, but whose classification is uncertain (IRAS 17580-3111). Conclusions: The unexpected detections of water masers in two objects among the small subset of PNe led us to suggest that the PNe harbouring water masers are a special type of massive, rapidly evolving PNe. Tables 1 and 3 are only available in electronic form at eprintid: arXiv:astro-ph/0703502

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Detection table from Suarez et al. (2007)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	V_peak	F_peak	∫F dv	Detection	Class	Dist. (parallax)
	(J2000)	(J2000)	(deg.)	(deg.)			H₂O	(km/s)	(Jy)	(Jy*km/s)	Yes/No		(kpc)
1	07 35 41.2	+00 14 58	217.8018	9.9477	G217.801+9.947	IRAS 07331+0021	22 GHz;	28.1	0.21	2.2	+H₂O +OH	EVOLVED
2	16 58 27.8	-30 55 06	352.5669	7.2976	G352.567+7.298	IRAS 16552-3050	22 GHz;	89.5	5.54	212.9	+H₂O -OH	EVOLVED
	16 58 27.8	-30 55 06	352.5669	7.2976	G352.567+7.298	IRAS 16552-3050	22 GHz;	-66.8	1.55	125.3	+H₂O -OH	EVOLVED
	16 58 27.8	-30 55 06	352.5669	7.2976	G352.567+7.298	IRAS 16552-3050	22 GHz;	88.6	2.84	132	+H₂O -OH	EVOLVED
5	17 47 35.3	-29 50 57	359.4423	-0.8405	G359.442-0.840	IRAS 17443-2949	22 GHz;	-6.4	10.58	114.2	+H₂O +OH	SFR_MIXED
	17 47 35.3	-29 50 57	359.4423	-0.8405	G359.442-0.840	IRAS 17443-2949	22 GHz;	-6.3	8.67	100.1	+H₂O +OH	SFR_MIXED
7	18 01 19.6	-31 11 22	359.7780	-4.0710	G359.778-4.071	IRAS 17580-3111	22 GHz;	21.3	1.09	9.6	+H₂O +OH	EVOLVED
8	18 09 12.4	-25 04 34	5.9737	-2.6110	G5.974-2.611	IRAS 18061-2505	22 GHz;	57.2	2.4	45.2	+H₂O -OH	EVOLVED
	18 09 12.4	-25 04 34	5.9737	-2.6110	G5.974-2.611	IRAS 18061-2505	22 GHz;	57.3	2.4	27.4	+H₂O -OH	EVOLVED
	18 09 12.4	-25 04 34	5.9737	-2.6110	G5.974-2.611	IRAS 18061-2505	22 GHz;	60.5	6.95	66	+H₂O -OH	EVOLVED
	18 09 12.4	-25 04 34	5.9737	-2.6110	G5.974-2.611	IRAS 18061-2505	22 GHz;	60.9	3.01	56.4	+H₂O -OH	EVOLVED

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 SUA07

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