A Survey for Water Maser Emission toward Planetary Nebulae: New Detection in IRAS 17347−3139

Gregorio-Monsalvo, I. de; Gómez, Yolanda; Anglada, Guillem; Cesaroni, R.; Miranda, L. F.; Gómez, José F.; Torrelles, J. M.

doi:10.1086/380757

Cited by 45 publications

(67 citation statements)

References 36 publications

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“…A few other pPNe show H 2 O emission with low-velocity spots, more similar to that observed in our source (de Gregorio-Monsalvo et al 2004). Although the interpretation of the origin of the H 2 O emission in them is not straightforward, it seems to come from nebular regions that have not been accelerated during the post-AGB evolution.…”

Section: Resultssupporting

confidence: 85%

Water vapor and silicon monoxide maser observations in the protoplanetary nebula OH 231.8+4.2

Desmurs

Alcolea

Contreras

et al. 2007

A&A

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Context. OH 231.8+4.2 is a well studied preplanetary nebula (pPN) around a binary stellar system that shows a remarkable bipolar outflow. Aims. To study the structure and kinematics of the inner 10-80 AU nebular regions probed by SiO and H 2 O maser emission, where the agents of wind collimation are expected to operate, in order to gain insights into the, yet poorly known, processes responsible for the shaping of bipolar pPNe. Methods. We performed high-resolution observations of the H 2 O 6 1,6 -5 2,3 and 28 SiO v = 2, J = 1-0 maser emissions with the Very Long Baseline Array. The absolute position of both emission distributions were recovered using the phase referencing technique, and accurately registered in HST optical images. Results. Maps of both masers were produced and compared. H 2 O maser clumps are found to be distributed in two areas of 20 mas in size spatially displaced by ∼60 milli-arcs along an axis oriented nearly north-south. SiO masers are tentatively found to be placed between the two H 2 O maser emitting regions, probably indicating the position of the Mira component of the system. Conclusions. The SiO maser emission traces an inner equatorial component with a diameter of 12 AU, probably a disk rotating around the M-type star. Outwards, we detect in the H 2 O data a pair of polar caps, separated by 80 AU. We believe that the inner regions of the nebula probably have been altered by the presence of the companion, leading to an equator-to-pole density contrast that may explain the lack of H 2 O masers and strong SiO maser emission in the denser, equatorial regions.

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Section: Resultssupporting

confidence: 85%

Water vapor and silicon monoxide maser observations in the protoplanetary nebula OH 231.8+4.2

Desmurs

Alcolea

Contreras

et al. 2007

A&A

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“…Although such spectral indices may also arise from ionized jets, the flux density in IRAS 16333−4807 is too high to be explained in this way with reasonable mass-loss rates. As in the case of IRAS 17347−3139 (de Gregorio-Monsalvo et al 2004), a mass loss rate ofṀ ≃ 10 −4 (D/kpc) 3/2 M⊙ yr −1 , where D is the distance to the source, would be required for a spherical ionized wind to explain the observed radio continuum emission (Wright & Barlow 1975;Panagia & Felli 1975). Even assuming a collimated wind, and following the formulation by Reynolds (1986), the required mass loss rate is as high as ≃ 3 × 10 −6 (D/kpc) 3/2 M⊙ yr −1 , and this is a lower limit, assuming that the wind is fully ionized.…”

Section: The Nature Of Iras 16333−4807 As a Planetary Nebulamentioning

confidence: 92%

H2O maser emission associated with the planetary nebula IRAS 16333−4807

Uscanga

Gómez

Miranda

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present simultaneous observations of H 2 O maser emission and radio continuum at 1.3 cm carried out with the Australia Telescope Compact Array towards two sources, IRAS 16333−4807 and IRAS 12405−6219, catalogued as planetary nebula (PN) candidates, and where single-dish detections of H 2 O masers have been previously reported. Our goal was to unambiguously confirm the spatial association of the H 2 O masers with these two PN candidates. We detected and mapped H 2 O maser emission in both fields, but only in IRAS 16333−4807 the maser emission is spatially associated with the radio continuum emission. The properties of IRAS 16333−4807 provide strong support for the PN nature of the object, hereby confirming it as the fifth known case of a H 2 O maser-emitting PN. This source is bipolar, like the other four known H 2 O maser-emitting PNe, indicating that these sources might pertain to a usual, but short phase in the evolution of bipolar PNe. In IRAS 12405−6219, the H 2 O maser and radio continuum emission are not associated with each other and, in addition, the available data indicate that this source is an H ii region rather than a PN.

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“…4, we show the position in the IRAS two-colour diagram of the 9 sources with water masers detected in both surveys (Robledo and Parkes). We also include the post-AGB candidate IRAS 17088−4221, detected by Deacon et al (2007) and, for completeness, we also include the position of the other two H 2 O-PN, IRAS 17347−3139 (de Gregorio-Monsalvo et al 2004) and PN K3−35 (Miranda et al 2001). In this figure, we have used the same symbol for confirmed and candidate water-maser-emitting PNe, and analogously for confirmed and candidate post-AGB stars.…”

Section: Position Of the Detected Sources In The Iras And Msx Colour-mentioning

confidence: 99%

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

Suárez

Gómez

Miranda

et al. 2009

A&A

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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 o . 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.

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A Survey for Water Maser Emission toward Planetary Nebulae: New Detection in IRAS 17347−3139

Cited by 45 publications

References 36 publications

Water vapor and silicon monoxide maser observations in the protoplanetary nebula OH 231.8+4.2

Water vapor and silicon monoxide maser observations in the protoplanetary nebula OH 231.8+4.2

H2O maser emission associated with the planetary nebula IRAS 16333−4807

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

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