Radio interferometric observations of candidate water-maser-emitting planetary nebulae

TL;DR

This study uses VLA observations to confirm water maser emission in three planetary nebulae, revealing their bipolar morphology and suggesting a link to non-spherical mass-loss episodes, thus expanding the known class of water-maser-emitting PNe.

Contribution

First interferometric confirmation of water masers in three planetary nebulae, establishing their bipolar morphology and potential evolutionary links.

Findings

IRAS 18061-2505 confirmed as water-maser-emitting PN

All three PNe show bipolar morphology

Water maser emission likely related to non-spherical mass loss

Abstract

We present Very Large Array (VLA) 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 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 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.