Discrete Source Survey of 6 GHz OH emission from PNe and pPNe and first 6 GHz images of K 3–35

Desmurs, J. F.; Baudry, A.; Sivagnanam, P.; Henkel, C.; Richards, A. M. S.; Bains, Indra

doi:10.1051/0004-6361/200913387

Cited by 12 publications

(17 citation statements)

References 38 publications

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“…Regarding the maser environment, Yoon et al (2014) reported no detection of 22 GHz H 2 O and 43 GHz SiO masers. Until our work, hydroxyl (OH) masers had not been detected either: Desmurs et al (2010) reported no detection of the 6 GHz OH excited lines, while Silverglate et al (1979) reported no detection of the 1612, 1665 or 1667 MHz OH lines. The absence of masers from oxygen-species is not surprising because of the carbon-rich nature of CRL 618.…”

Section: Introductionmentioning

confidence: 72%

“…They found 1720 MHz masers to have very similar velocity and location to the H 2 O masers. An excited OH maser of the 6035 MHz transition has also been detected toward K3-35, and, as for the 1720 MHz OH masers, the excited OH maser in K3-35 is coincident in position and velocity with H 2 O masers and may originate from the inner circumstellar envelope (Gómez et al 2009, Desmurs et al 2010. According to the model by Herpin & Cernicharo (2000), the region where OH and H 2 O are located in CRL 618 is within 1,400 a.u.…”

Section: Scenarios For the Origin Of The 4765 Mhz Oh Maser In Crl 618mentioning

confidence: 86%

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Detection of 4765 MHz OH Emission in a Preplanetary Nebula: CRL 618

Strack

Araya

Lebrón

et al. 2019

ApJ

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Jets and outflows are ubiquitous phenomena in astrophysics, found in our Galaxy in diverse environments, from the formation of stars to late-type stellar objects. We present observations conducted with the 305m Arecibo Telescope of the pre-planetary nebula CRL 618 (Westbrook Nebula) − a well studied late-type star that has developed bipolar jets. The observations resulted in the first detection of 4765 MHz OH in a late-type stellar object. The line was narrow (FWHM ∼ 0.6 km s −1 ) and ∼40 km s −1 blueshifted with respect to the systemic velocity, which suggests association with the expanding jets/bullets in CRL 618. We also report non-detection at Arecibo of any other OH transition between 1 and 9 GHz. The non-detections were obtained during the observations in 2008, when the 4765 MHz OH line was first discovered, and also in 2015 when the 4765 MHz OH line was not detected. Our data indicate that the 4765 MHz OH line was a variable maser. Modeling of the 4765 MHz OH detection and non-detection of the other transitions is consistent with the physical conditions expected in CRL 618. The 4765 MHz OH maser could originate from dissociation of H 2 O by shocks after sublimation of icy objects in this dying carbon-rich stellar system, although other alternatives such as OH in an oxygen-rich circumstellar region associated with a binary companion are also possible.

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Section: Introductionmentioning

confidence: 72%

Section: Scenarios For the Origin Of The 4765 Mhz Oh Maser In Crl 618mentioning

confidence: 86%

Detection of 4765 MHz OH Emission in a Preplanetary Nebula: CRL 618

Strack

Araya

Lebrón

et al. 2019

ApJ

View full text Add to dashboard Cite

show abstract

“…Seaquist & Davis (1983) detected radio continuum (at 2, 6, and 20 cm) and OH (1612 MHz) maser emission with the VLA toward this source. Moreover, OH maser emission at 6035 MHz was detected toward this source with single-dish observations (Jewell et al 1985;Desmurs et al 2002Desmurs et al , 2010. However, References.…”

Section: Iras 19219+0947 (Vy 2−2)mentioning

confidence: 79%

An updated catalog of OH-maser-emitting planetary nebulae

Uscanga

Gómez

Suárez

et al. 2012

A&A

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Aims. We studied the characteristics of planetary nebulae (PNe) that show both OH maser and radio continuum emission (hereafter OHPNe). These have been proposed to be very young PNe, and therefore, they could be key objects for understanding the formation and evolution of PNe. Methods. We consulted the literature searching for interferometric observations of radio continuum and OH masers toward evolved stars, including the information from several surveys. We also processed radio continuum and OH maser observations toward PNe in the Very Large Array data archive. The high positional accuracy provided by interferometric observations allow us to confirm or reject the association between OH maser and radio continuum emission. Results. We found a total of six PNe that present both OH maser and radio continuum emissions, as confirmed with radio interferometric observations. These are bona fide OHPNe. The confirmed OHPNe present a bipolar morphology in resolved images of their ionized emission at different wavelengths, suggesting that the OH maser emission in PNe is related to nonspherical mass-loss phenomena. The OH maser spectra in PNe present a clear asymmetry, tending to show blueshifted emission with respect to the systemic velocity. Their infrared colors suggest that most of these objects are very young PNe. OHPNe do not form a homogeneous group, and seem to represent a variety of different evolutionary stages. We suggest that OH masers pumped in the asymptotic giant branch (AGB) phase may disappear during the post-AGB phase, but reappear once the source becomes a PN and its radio continuum emission is amplified by the OH molecules. Therefore, OH maser emission could last significantly longer than the previously assumed 1000 yr after the end of the AGB phase. This maser lifetime may be longer in PNe with more massive central stars, which ionize a larger amount of gas in the envelope.

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“…They all show maser emission with strong asymmetry, i.e., preferentially blueshifted emission with respect to the stellar velocity (Uscanga et al 2012). One of them, K 3−35, shows OH maser emission at all four ground-state transitions (1612, 1665, 1667, 1720 MHz; Gómez et al 2009), as well as excited-state masers at 6035 MHz (Desmurs et al 2010). It is so far the only PN known to exhibit OH maser lines at 1720 MHz.…”

Section: Introductionmentioning

confidence: 99%

Unusual Shock-Excited Oh Maser Emission in a Young Planetary Nebula

Qiao

Walsh

Gómez

et al. 2016

ApJ

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We report on OH maser emission toward G336.644−0.695 (IRAS 16333−4807), which is a H 2 O maser-emitting Planetary Nebula (PN). We have detected 1612, 1667, and 1720 MHz OH masers at two epochs using the Australia Telescope Compact Array, hereby confirming it as the seventh known case of an OH-maser-emitting PN. This is only the second known PN showing 1720 MHz OH masers after K 3−35 and the only evolved stellar object with 1720 MHz OH masers as the strongest transition. This PN is one of a group of very young PNe. The 1612 MHz and 1667 MHz masers are at a similar velocity to the 22 GHz H 2 O masers, whereas the 1720 MHz masers show a variable spectrum, with several components spread over a higher velocity range (up to 36 km s −1 ). We also detect Zeeman splitting in the 1720 MHz transition at two epochs (with field strengths of ∼2 to ∼10 mG), which suggests the OH emission at 1720 MHz is formed in a magnetized environment. These 1720 MHz OH masers may trace short-lived equatorial ejections during the formation of the PN.

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Discrete Source Survey of 6 GHz OH emission from PNe and pPNe and first 6 GHz images of K 3–35

Cited by 12 publications

References 38 publications

Detection of 4765 MHz OH Emission in a Preplanetary Nebula: CRL 618

Detection of 4765 MHz OH Emission in a Preplanetary Nebula: CRL 618

An updated catalog of OH-maser-emitting planetary nebulae

Unusual Shock-Excited Oh Maser Emission in a Young Planetary Nebula

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