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

Suárez, Olga; Gómez, José F.; Miranda, L. F.; Torrelles, J. M.; Gómez, Yolanda; Anglada, Guillem; Morata, Ó.

doi:10.1051/0004-6361/200911777

Cited by 28 publications

(42 citation statements)

References 27 publications

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“…We note that the systemic velocity of the object is unknown and, therefore, we cannot establish whether the H2O masers arise in an equatorial structure or in a collimated outflow. Finally, the flux density of the H2O maser emission has increased from 1.8 Jy in 2007 (Parkes observations, Suárez et al 2009) to 4.8 Jy in 2013 (ATCA observations, this paper).…”

Section: Iras 16333−4807mentioning

confidence: 72%

“…Our main goal was to confirm the association of H2O maser emission, previously detected with the Parkes antenna (Suárez et al 2009), with these two PN candidates.…”

Section: Introductionmentioning

confidence: 85%

“…Moreover, these are the only three H2O-PNe in which the photoionized gas traced by the radio continuum emission shows a bipolar morphology similar to that seen in optical and infrared images. Gómez et al (2008) and Suárez et al (2009) proposed a simple evolutionary schema for H2O masers in evolved stars (5−8 M ⊙ ), considering their location in the nebula and their radial velocities. First, in the AGB phase, low-velocity H2O maser emission arises from the spherical shell.…”

Section: Comparison With Other H2o Maser-emitting Pnementioning

confidence: 99%

“…The observations of the northernmost sources (Suárez et al 2007) led to the detection of H2O maser emission towards the PN IRAS 18061−2505, later confirmed with the Very Large Array . For the southern part of the survey (Suárez et al 2009), two additional sources catalogued as possible PNe, IRAS 16333−4807 and IRAS 12405−6219 (van de Steene & Pottasch 1993), were found to be probably associated with H2O maser emission. However, the lack of enough angular resolution of the single-dish observations prevented to establish a clear association.…”

Section: Introductionmentioning

confidence: 98%

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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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Section: Iras 16333−4807mentioning

confidence: 72%

“…Our main goal was to confirm the association of H2O maser emission, previously detected with the Parkes antenna (Suárez et al 2009), with these two PN candidates.…”

Section: Introductionmentioning

confidence: 85%

Section: Comparison With Other H2o Maser-emitting Pnementioning

confidence: 99%

Section: Introductionmentioning

confidence: 98%

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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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“…Because of these maser properties, objects like I16342 are called "water fountain source (WFS)" (Likkel & Morris 1988;Imai et al 2007). So far, 14 objects are classified into this group (Imai et al 2007;Suárez et al 2009;Walsh et al 2009;Gómez et al 2011). Many PNs exhibit jets, which cannot be explained with only the generalised interacting stellar wind (GISW) model (Sahai & Trauger 1998).…”

Section: Introductionmentioning

confidence: 99%

Dust shell model of the water fountain source IRAS 16342–3814

Murakawa

Izumiura²

2012

A&A

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Aims. We investigate the circumstellar dust shell of the water fountain source IRAS 16342-3814. Methods. We performed two-dimensional radiative transfer modeling of the dust shell, taking into account previously observed spectral energy distributions (SEDs) and our new J-band imaging and H-and K S -band imaging polarimetry obtained using the VLT/NACO instrument. Results. Previous observations expect an optically thick torus in the equatorial plane because of a striking bipolar appearance and a large viewing angle of 30−40 • . However, models with such a torus as well as a bipolar lobe and an AGB shell cannot fit the SED and the images simultaneously. We find that an additional optically and geometrically thick disk located inside a massive torus solves this problem. The masses of the disk and the torus are estimated to be 0.01 M at the a max = 100 μm dust and 1 M at a max = 10 μm dust, respectively. Conclusions. We discuss a possible formation scenario for the disk and torus based on a similar mechanism to the equatorial back flow. IRAS 16342-3814 is expected to undergo mass loss at a high rate. The radiation from the central star is shielded by the dust that was ejected in the subsequent mass loss event. As a result, the radiation pressure on dust particles cannot govern the motion of the particles anymore. The mass loss flow can be concentrated in the equatorial plane by help of an interaction, which might be the gravitational attraction by the companion, if it exists in IRAS 16342-3814. A fraction of the ejecta is captured in a circum-companion or circum-binary disk and the remains are escaping from the central star(s) and form the massive torus.

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Maser emission in planetary nebulae

Gómez¹

2007

Proc. IAU

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Abstract. Stars at the top of the asymptotic giant branch (AGB) can exhibit maser emission from molecules like SiO, H2O and OH. These masers appear in general stratified in the envelope, with the SiO masers close to the central star and the OH masers farther out in the envelope. As the star evolves to the planetary nebula (PN) phase, mass-loss stops and ionization of the envelope begins, making the masers disappear progressively. The OH masers in PNe can be present in the envelope for periods of ∼1000 years but the H2O masers can survive only hundreds of years. Then, H2O maser emission is not expected in PNe and its detection suggests that these objects are in a very particular moment of its evolution in the transition from AGB to PNe. We discuss the unambiguous detection of H2O maser emission in two planetary nebulae: K 3-35 and IRAS 17347-3139. The water-vapor masers in these PNe are tracing disk-like structures around the core and in the case of K3-35 the masers were also found at the tip of its bipolar lobes. Kinematic modeling of the H2O masers in both PNe suggest the existence of a rotating and expanding disk. Both PNe exhibit a bipolar morphology and in the particular case of K 3-35 the OH masers are highly polarized close to the core in a disk-like structure. All these observational results are consistent with the models where rotation and magnetic fields have been proposed to explain the asymmetries observed in planetary nebulae.

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

Cited by 28 publications

References 27 publications

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

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

Dust shell model of the water fountain source IRAS 16342–3814

Maser emission in planetary nebulae

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