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GOM08 - Radio Interferometric Observations of Candidate Water-Maser-Emitting Planetary Nebulae

Short title: Gomez et al. (2008)
Authors: Gómez, José F. Suárez, Olga Gómez, Yolanda Miranda, Luis F. Torrelles, José M. Anglada, Guillem Morata, Óscar
Journal: The Astronomical Journal, Volume 135, Issue 6, pp. 2074-2083 (2008).
Bibcode:

Target type: pAGB_PN

Abstract
We present Very Large Array observations of H₂O and OH masers as well as radio continuum emission at 1.3 and 18 cm toward three sources previously cataloged as planetary nebulae (PNe) and in which single-dish detections of H₂O masers have been reported: IRAS 17443-2949, IRAS 17580-3111, and IRAS 18061-2505. Our goal was to unambiguously confirm their nature as water-maser-emitting PNe, a class of objects of which only two bona fide members were previously known. We detected and mapped H₂O maser emission toward all three sources, while OH maser emission is detected in IRAS 17443-2949 and IRAS 17580-3111 as well as in other two objects within the observed fields: IRAS 17442-2942 (unknown nature) and IRAS 17579-3121 (also cataloged as a possible PN). We found radio continuum emission associated only with IRAS 18061-2505. Our results confirm IRAS 18061-2505 as the third known case of a PN associated with H₂O maser emission. The rest of the studied sources are not likely to trace PNe. The three known water-maser-emitting PNe have clear bipolar morphologies, which suggests that water maser emission in these objects is related to non-spherical mass-loss episodes. We speculate that these bipolar water-maser-emitting PNe would have ""water-fountain"" asymptotic giant branch (AGB) and post-AGB stars as their precursors. A note of caution is given for other objects that have been classified as OHPNe (objects with both OH maser and radio continuum emission that could be extremely young PNe) based on single-dish observations, since interferometric data of both OH masers and continuum are necessary for a proper identification as members of this class. eprintid: arXiv:0803.1644

Abstract

We present Very Large Array observations of H₂O and OH masers as well as radio continuum emission at 1.3 and 18 cm toward three sources previously cataloged as planetary nebulae (PNe) and in which single-dish detections of H₂O masers have been reported: IRAS 17443-2949, IRAS 17580-3111, and IRAS 18061-2505. Our goal was to unambiguously confirm their nature as water-maser-emitting PNe, a class of objects of which only two bona fide members were previously known. We detected and mapped H₂O maser emission toward all three sources, while OH maser emission is detected in IRAS 17443-2949 and IRAS 17580-3111 as well as in other two objects within the observed fields: IRAS 17442-2942 (unknown nature) and IRAS 17579-3121 (also cataloged as a possible PN). We found radio continuum emission associated only with IRAS 18061-2505. Our results confirm IRAS 18061-2505 as the third known case of a PN associated with H₂O maser emission. The rest of the studied sources are not likely to trace PNe. The three known water-maser-emitting PNe have clear bipolar morphologies, which suggests that water maser emission in these objects is related to non-spherical mass-loss episodes. We speculate that these bipolar water-maser-emitting PNe would have ""water-fountain"" asymptotic giant branch (AGB) and post-AGB stars as their precursors. A note of caution is given for other objects that have been classified as OHPNe (objects with both OH maser and radio continuum emission that could be extremely young PNe) based on single-dish observations, since interferometric data of both OH masers and continuum are necessary for a proper identification as members of this class. eprintid:

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Detection table from Gomez et al. (2008)

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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	18 01 19.6	-31 11 22	359.7780	-4.0710	G359.778-4.071	IRAS 17580-3111	1612	15.9	12.7	0.912	ENG15	+H₂O +OH	EVOLVED		GOM08
2	18 01 13.4	-31 21 57	359.6130	-4.1384	G359.613-4.139	IRAS 17579-3121	1612	20.4	1.4	2.100	ENG15	+OH	EVOLVED		GOM08
3	17 47 35.3	-29 50 57	359.4423	-0.8405	G359.442-0.840	IRAS 17443-2949	1612	11.3	-16.1	1.215	ENG15	+H₂O +OH	SFR_MIXED		GOM08
	17 47 35.3	-29 50 57	359.4423	-0.8405	G359.442-0.840	IRAS 17443-2949	1665	17.6	-15.0	0.141	ENG15	+H₂O +OH	SFR_MIXED		GOM08
5	17 47 28.9	-29 43 38	359.5346	-0.7575	G359.534-0.757	IRAS 17442-2942	1612	31.8	-55.9	0.229	ENG15	+OH -SiO	EVOLVED		GOM08

Non-detection table from Gomez et al. (2008)