Searching for nascent planetary nebulae: OHPNe candidates in the SPLASH survey

Cala, Roldán A.; Gómez, José F.; Miranda, L. F.; Uscanga, L.; Breen, S. L.; Dawson, J. R.; Gregorio‐Monsalvo, I. de; Imai, Hiroshi; Qiao, Hai-Hua; Suárez, Olga

doi:10.1093/mnras/stac2341

Cited by 4 publications

(3 citation statements)

References 103 publications

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“…We have processed all the continuum data associated with the interferometric follow-up of SPLASH (see Qiao et al 2020), which was carried out with Australia Telecope Compact Array. We found three previously identified bona fide OHPNe, and four new OHPNe candidates (Cala et al 2022). The new OHPNe candidates present characteristics that are similar to those observed in bona fide OHPNe (see Cala et al 2022).…”

Section: New Identificationssupporting

confidence: 59%

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Nascent planetary nebulae: new identifications and extraordinary evolution

Cala,

Gómez,

Miranda

2022

Proc. IAU

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Planetary nebulae (PNe) harbouring masers of H2O (H2OPNe) and/or OH (OHPNe) are thought to be nascent PNe. They are extremely scarce, and so far only eight members are know to date. Here we explain our current effort to identify new H2OPNe and/or OHPNe. We report IRAS 07027–7934 as a new bona fine OHPN. Its 1612 MHz OH spectrum seems to be changing from double- to single-peaked since the redshifted emission has vanished almost completely, and the 1667 MHz OH maser emission has disappeared. For the OHPN Vy 2-2, we found that its central star is unexpectedly carbon (C)-rich, has a low-mass progenitor, and could be a post-common envelope binary system. Moreover, we confirm Vy 2-2 as a nascent PN. We speculate that low-mass C-rich central stars in post-common envelope systems could be a common end of H2OPNe and OHPNe.

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Section: New Identificationssupporting

confidence: 59%

“…We found three previously identified bona fide OHPNe, and four new OHPNe candidates (Cala et al 2022). The new OHPNe candidates present characteristics that are similar to those observed in bona fide OHPNe (see Cala et al 2022). We aim to confirm the new OHPNe candidates as bona fide PNe by means of optical/infrared spectroscopy.…”

Section: New Identificationsmentioning

confidence: 80%

Nascent planetary nebulae: new identifications and extraordinary evolution

Cala,

Gómez,

Miranda

2022

Proc. IAU

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“…An alternative explanation for the origin of the radio continuum emission is the onset of photoionization at which this source is entering the PN phase. An increase in the flux density at radio wavelengths has also been observed in several young PNe (Kwok et al 1981;Knapp et al 1995;Christianto & Seaquist 1998;Gómez et al 2005;Tafoya et al 2009;Cala et al 2022). Such a flux density increase has been interpreted as an expansion of the ionized region.…”

Section: Characteristics Of the Radio Continuum Emission In I18043mentioning

confidence: 67%

Evolution of the Outflow in the Water Fountain Source IRAS 18043–2116*

Uscanga

Imai

Gómez

et al. 2023

ApJ

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We present the spectral and spatial evolution of H2O masers associated with the water fountain source IRAS 18043−2116, found in observations with the Nobeyama 45 m Telescope and the Australia Telescope Compact Array. We have found new highest-velocity components of the H2O masers (at the redshifted side V LSR ≃ 376 km s−1 and at the blueshifted side V LSR ≃ −165 km s−1), and the resulting velocity spread of ≃540 km s−1 breaks the speed record of fast jets/outflows in this type of sources. The locations of those components have offsets from the axis joining the two major maser clusters, indicating a large opening angle of the outflow (∼60°). The evolution of the maser cluster separation of ∼2.9 mas yr−1 and the compact (∼0.″2) CO emission source mapped with the Atacama Large Millimeter-submillimeter Array suggest a very short (∼30 yr) timescale of the outflow. We also confirmed an increase in the flux density of the 22 GHz continuum source. The properties of the jet and the continuum sources and their possible evolution in the transition to the planetary nebula phase are further discussed.

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An interferometric search for SiO maser emission in planetary nebulae

Cala,

Gómez,

Miranda

et al. 2024

A&A

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Maser emission of SiO, H$_2$O, and OH is widespread in asymptotic giant branch (AGB) stars with oxygen- (O-) rich envelopes. This emission quickly disappears during the post-AGB phase and is extremely rare in planetary nebulae (PNe). So far, only eight PNe have been confirmed to show OH and/or H$_2$O maser emission, and none have ever been found to show SiO maser emission. We intend to obtain the first detection of a SiO maser from a PN. Such a detection would provide us with a useful tool to probe mass loss in PNe at a scales of a few AU from the central star, much shorter than the scales traced by H$_2$ or OH masers. We compiled two different samples. The first one comprises all known PNe with confirmed OH and/or H$_2$O maser emission, as well as two candidate PNe showing OH masers. For the second sample, we compiled single-dish SiO maser detections in the literature, and compared them with catalogs of PNe and radio continuum emission (which could trace photoionized gas in PNe). We identified five targets (either PN or radio continuum sources) within the beam of the single-dish SiO maser observations. We then carried out interferometric observations of both samples with the Australia Telescope Compact Array, to confirm the spatial association between continuum and SiO maser emission. We find no SiO maser emission associated with any confirmed or candidate PN. In all targets, except IRAS 17390$-$3014, there is no spatial coincidence between SiO masers and radio continuum emission. While in IRAS 17390$-$3014 we cannot completely rule out a possible association, it is unlikely that the radio continuum emission arises from a PN. The absence of SiO maser emission in PNe showing OH or H$_2$O masers is of special interest, since thermal SiO emission has been reported in at least one of these targets, indicating that SiO molecules can be present in the gas phase. Since some maser-emitting PNe show evidence of having O-rich outer envelopes, and carbon- (C-) rich central stars and inner envelopes, we speculate that SiO abundance could be very low in the central regions where physical conditions are optimal for maser pumping, and C-bearing molecules may be dominant in the gas phase at those locations.

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Searching for nascent planetary nebulae: OHPNe candidates in the SPLASH survey

Cited by 4 publications

References 103 publications

Nascent planetary nebulae: new identifications and extraordinary evolution

Nascent planetary nebulae: new identifications and extraordinary evolution

Evolution of the Outflow in the Water Fountain Source IRAS 18043–2116*

An interferometric search for SiO maser emission in planetary nebulae

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