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

AbstractWater maser emission has been detected only toward three planetary nebulae (PNe). In particular, in K3-35, the first PN where water vapor maser emission was detected, the components are located in a torus-like structure with a radius of 85 AU and also at the surprisingly large distance of 5000 AU from the star, in the tips of the bipolar lobes. The existence of these water molecules in PNe is puzzling, probably related to some unknown mechanism shielding them against the ionizing radiation. We report the detection of HCO+ (J = 1 − 0) emission toward K 3-35, that not only suggests that dense molecular gas (~105 cm−3) is present in this PN, but also that this kind of PN can enrich their surroundings with organic molecules.

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Imaging the water masers toward the H2O-PN IRAS 18061–2505

Proceedings of the International Astronomical Union ◽

10.1017/s1743921312007090 ◽

2012 ◽

Vol 8 (S287) ◽

pp. 258-259

Author(s):

Yolanda Gómez ◽

Daniel Tafoya ◽

Olga Suárez ◽

Jose F. Gómez ◽

Luis F. Miranda ◽

...

Keyword(s):

Planetary Nebulae ◽

Central Star ◽

Large Array ◽

Maser Emission ◽

Very Large Array ◽

Kinematical Model ◽

Water Masers ◽

Central Stars ◽

Water Maser

AbstractIt has been suggested that the presence of disks or tori around the central stars of pre Planetary Nebulae and Planetary Nebulae is related to the collimation of the jet that are frequently observed in these sources. These disks or tori can be traced by the maser emission of some molecules such as water. In this work we present Very Large Array (VLA) observations of the water maser emission at 22 GHz toward the PN IRAS 18061–2505, for which the masers appear located on one side of the central star. For comparison with the observations, we present a simple kinematical model of a disk rotating and expanding around the central star. The model matches qualitatively the observations. However, since the masers appear only on one side of the disk, these results are not conclusive.

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Erratum: “Discovery of Water Maser Emission in Eight AGNs with 70 m Antennas of NASA’s Deep Space Network” (ApJ, 638, 100 [2006])

The Astrophysical Journal ◽

10.1086/504978 ◽

2006 ◽

Vol 649 (1) ◽

pp. 561-561 ◽

Cited By ~ 1

Author(s):

P. T. Kondratko ◽

L. J. Greenhill ◽

J. M. Moran ◽

J. E. J. Lovell ◽

T. B. H. Kuiper ◽

...

Keyword(s):

Deep Space ◽

Deep Space Network ◽

Maser Emission ◽

Space Network ◽

Water Maser

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A new jet/outflow maser in the nucleus of the Compton-thick AGN IRAS 15480-0344

Proceedings of the International Astronomical Union ◽

10.1017/s1743921317010596 ◽

2017 ◽

Vol 13 (S336) ◽

pp. 129-132

Author(s):

Paola Castangia ◽

Andrea Tarchi ◽

Alessandro Caccianiga ◽

Paola Severgnini ◽

Gabriele Surcis ◽

...

Keyword(s):

Detection Rate ◽

Radio Continuum ◽

Continuum Emission ◽

Maser Emission ◽

X Ray ◽

Vlbi Observations ◽

S0 Galaxies ◽

Water Maser

AbstractInvestigations of H2O maser galaxies at X-ray energies reveal that most harbor highly absorbed AGN. Possible correlations between the intrinsic X-ray luminosity and the properties of water maser emission have been suggested. With the aim of looking into these correlations on a more solid statistical basis, we have search for maser emission in a well-defined sample of Compton-thick AGN. Here we report the results of the survey, which yielded a surprisingly high maser detection rate, with a particular focus on the newly discovered luminous water maser in the lenticular (field) S0 galaxy IRAS 15480-0344. Recently, VLBI observations have been obtained to image the line and continuum emission in the nucleus of this galaxy. The radio continuum emission at VLBI scales is resolved into two compact components that are interpreted as jet knots. Based on the single-dish profile, the variability of the maser emission, and the position of the maser spots with respect to these continuum sources, we favor of a jet/outflow origin for the maser emission, consistent with similar cases found in other radio-quiet AGN. This scenario is consistent with the hypothesis of the presence of strong nuclear winds recently invoked to explain the main characteristics of field S0 galaxies.

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RADIO INTERFEROMETRIC OBSERVATIONS OF CANDIDATE WATER-MASER-EMITTING PLANETARY NEBULAE

The Astronomical Journal ◽

10.1088/0004-6256/135/6/2074 ◽

2008 ◽

Vol 135 (6) ◽

pp. 2074-2083 ◽

Cited By ~ 18

Author(s):

José F. Gómez ◽

Olga Suárez ◽

Yolanda Gómez ◽

Luis F. Miranda ◽

José M. Torrelles ◽

...

Keyword(s):

Planetary Nebulae ◽

Water Maser

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Water masers as signposts of extremely young planetary nebulae

Proceedings of the International Astronomical Union ◽

10.1017/s1743921317009577 ◽

2017 ◽

Vol 13 (S336) ◽

pp. 377-380

Author(s):

José F. Gómez ◽

Luis F. Miranda ◽

Lucero Uscanga ◽

Olga Suárez

Keyword(s):

Planetary Nebulae ◽

Radio Continuum ◽

Continuum Emission ◽

Water Masers ◽

Water Maser

AbstractOnly five planetary nebulae (PNe) have been confirmed to emit water masers. They seem to be very young PNe. The water emission in these objects preferentially traces circumstellar toroids, although in K 3-35 and IRAS 15103-5754, it may also trace collimated jets. We present water maser observations of these two sources at different epochs. The water maser distribution changes on timescales of months to a few years. We speculate that these changes may be due to the variation of the underlying radio continuum emission, which is amplified by the maser process in the foreground material.

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OH Maser Emission from Young Planetary Nebulae

Planetary Nebulae ◽

10.1007/978-94-009-0865-9_79 ◽

1989 ◽

pp. 210-210

Author(s):

A. Zijlstra ◽

S. R. Pottasch ◽

P. te Lintel ◽

C. Bignell

Keyword(s):

Planetary Nebulae ◽

Maser Emission

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A search for water maser emission toward obscured post-AGB star and planetary nebula candidates

Astronomy and Astrophysics ◽

10.1051/0004-6361/201526009 ◽

2015 ◽

Vol 578 ◽

pp. A119 ◽

Cited By ~ 7

Author(s):

J. F. Gómez ◽

J. R. Rizzo ◽

O. Suárez ◽

A. Palau ◽

L. F. Miranda ◽

...

Keyword(s):

Planetary Nebula ◽

Maser Emission ◽

Water Maser

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Mainline and water maser observations of OH/IR stars in the Arecibo sky

Symposium - International Astronomical Union ◽

10.1017/s0074180900131316 ◽

1997 ◽

Vol 180 ◽

pp. 356-356

Author(s):

B. M. Lewis

Keyword(s):

Detection Rate ◽

Planetary Nebulae ◽

Complete Sample ◽

Detection Rates ◽

Ir Stars ◽

Circumstellar Shells ◽

Water Masers ◽

The Many ◽

Water Maser

A complete sample of color selected IRAS sources with S(25) ≥ 2 Jy in the Arecibo sky and(0° ≤ δ ≤ 37°) was examined previously for 1612 MHz masers. The resulting set of OH/IR stars has now been searched for mainline OH masers at Arecibo (Lewis 1997) and for 22 GHz water masers at Effelsberg (Engels & Lewis 1996). The high overall detection rate of 61.6% for the mainlines and 54.8% for water is partly a result of deployed sensitivity, and partly due to the many blue objects in the sample. But the detectability of both masers improves when S(25)> 20 Jy, as the accompanying tables show. Still the bluest objects exhibit higher (usually ≥80%) detection rates, while there is a clear decrease in detections from redder shells: this decrease begins circa (25–12) μm=–0.55 for mainline masers, and abruptly circa (25–12) μm = −0.35 for water. These trends adhere to the descriptive sequence of the chronological scenario for masers in circumstellar shells, though a few proto planetary nebulae and very red OH/IR stars have water masers and a few mainline masers are detected in shells with (25-12) μm ≥ −0.2.

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