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

Qiao, Hai-Hua; Walsh, A. J.; Gómez, José F.; Imai, Hiroshi; Green, James; Dawson, J. R.; Shen, Zhi; Ellingsen, S. P.; Breen, S. L.; Jones, P. A.; Gibson, Steven J.; Cunningham, M. R.

doi:10.3847/0004-637x/817/1/37

Cited by 19 publications

(34 citation statements)

References 46 publications

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“…We will discuss the transition overlap of the evolved star category and star formation category separately in more detail in Section 4.3. The only PN site (G336.644−0.695; in the evolved star category) has 1612, 1667, and 1720 MHz OH masers and shows variability in the 1720 MHz transition at two epochs (see Qiao et al 2016 for more details). The two SNR sites (G336.961−0.111, Frail et al 1996, from MAGMO; G337.802−0.053, Caswell 2004, from our data set) show single-peak 1720 MHz OH masers, which trace the interaction of the SNR and surrounding molecular clouds.…”

Section: The Identification Of Maser Sitesmentioning

confidence: 99%

“…One evolved star site only has 1665 and 1667 MHz masers (G341.083−1.084 from our data set) with two maser spots at each transition. One PN site (G336.644 −0.695; Qiao et al 2016) The bottom panel of Figure 5 is a Venn diagram illustrating the overlap between the four transitions in star formation regions. 70% of 1612 MHz OH masers (7/10) are solitary, i.e., not associated with other ground-state OH transitions.…”

Section: Overlap Between Transitionsmentioning

confidence: 99%

“…Star formation OH masers preferentially trace a later stage of the HMSF process, compared to methanol masers and water masers (e.g., Caswell & Haynes 1987;Caswell 1998;Breen et al 2010a). As mentioned above, OH masers in the 1720 MHz transition are quite rare and are commonly associated with shocked gas, which can be detected in SNRs (Goss & Robinson 1968), HMSF regions (Caswell 2004;Edris et al 2007), occasionally asymptotic giant branch (AGB) stars (Sevenster & Chapman 2001), and PNe (Qiao et al 2016).…”

Section: Introductionmentioning

confidence: 99%

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Accurate Oh Maser Positions From the Splash Pilot Region

Qiao¹,

Walsh²,

Green³

et al. 2016

ApJS

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We report on high spatial resolution observations, using the Australia Telescope Compact Array (ATCA), of ground-state OH masers. These observations were carried out toward 196 pointing centers previously identified in the Southern Parkes Large-Area Survey in Hydroxyl (SPLASH) pilot region, between Galactic longitudes of 334°a nd 344°and Galactic latitudes of −2°and +2°. Supplementing our data with data from the MAGMO (Mapping the Galactic Magnetic field through OH masers) survey, we find maser emission toward 175 of the 196 target fields. We conclude that about half of the 21 nondetections were due to intrinsic variability. Due to the superior sensitivity of the followup ATCA observations, and the ability to resolve nearby sources into separate sites, we have identified 215 OH maser sites toward the 175 fields with detections. Among these 215 OH maser sites, 111 are new detections. After comparing the positions of these 215 maser sites to the literature, we identify 122 (57%) sites associated with evolved stars (one of which is a planetary nebula), 64 (30%) with star formation, two sites with supernova remnants, and 27 (13%) of unknown origin. The infrared colors of evolved star sites with symmetric maser profiles tend to be redder than those of evolved star sites with asymmetric maser profiles, which may indicate that symmetric sources are generally at an earlier evolutionary stage.

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Section: The Identification Of Maser Sitesmentioning

confidence: 99%

Section: Overlap Between Transitionsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Accurate Oh Maser Positions From the Splash Pilot Region

Qiao¹,

Walsh²,

Green³

et al. 2016

ApJS

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“…When CEs enter the PN phase, H 2 O and OH masers will rapidly disappear (< 10 3 yrs), and thus can trace young PNe. To date, five PNe with H 2 O and seven with OH maser emission have been confirmed, among which only two exhibit both maser emission (Gomez et al 2015a, Uscanga et al 2012, Qiao et al 2016. Gomez et al (2015b) discovered the first "water fountain" PN that was speculated to be the youngest PN known so far.…”

Section: Small Gas-phase Moleculesmentioning

confidence: 99%

Molecular studies of Planetary Nebulae

Zhang

2016

Proc. IAU

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Abstract. Circumstellar envelopes (CEs) around evolved stars are an active site for the production of molecules. After evolving through the Asymptotic Giant Branch (AGB), proto-planetary nebula (PPN), to planetary nebula (PN) phases, CEs ultimately merge with the interstellar medium (ISM). The study of molecules in PNe, therefore, is essential to understanding the transition from stellar to interstellar materials. So far, over 20 molecular species have been discovered in PNe. The molecular composition of PNe is rather different from those of AGB and PPNe, suggesting that the molecules synthesized in PN progenitors have been heavily processed by strong ultraviolet radiation from the central star. Intriguingly, fullerenes and complex organic compounds having aromatic and aliphatic structures can be rapidly formed and largely survive during the PPN/PN evolution. The similar molecular compositions in PNe and diffuse clouds as well as the detection of C + 60 in the ISM reinforce the view that the mass-loss from PNe can significantly enrich the ISM with molecular species, some of which may be responsible for the diffuse interstellar bands. In this contribution, I briefly summarize some recent observations of molecules in PNe, with emphasis on their implications on circumstellar chemistry.

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“…The 1720-MHz ( 2 Π 3/2 J = 3/2, F = 2−1) OH maser transition is one of the ground-state satellite lines, and is primarily found in star forming sites (Caswell 1999) and supernova remnants (Green et al 1997a) but has also been seen towards a small number of post-AGB stars and PNe (e.g. Sevenster & Chapman 2001;Qiao et al 2016). Detections in star forming regions commonly accompany ground and excited-state OH main lines (e.g.…”

Section: Introductionmentioning

confidence: 99%

MAGMO: polarimetry of 1720-MHz OH masers towards southern star-forming regions

Ogbodo

Green

Dawson

et al. 2020

Monthly Notices of the Royal Astronomical Society

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From targeted observations of ground-state OH masers towards 702 Multibeam (MMB) survey 6.7-GHz methanol masers, between Galactic longitudes 186 • through the Galactic centre to 20 • , made as part of the 'MAGMO' project, we present the physical and polarisation properties of the 1720-MHz OH maser transition, including the identification of Zeeman pairs. We present 10 new and 23 previously catalogued 1720-MHz OH maser sources detected towards star formation regions. In addition, we also detected 16 1720-MHz OH masers associated with supernova remnants and two sites of diffuse OH emission. Towards the 33 star formation masers, we identify 44 Zeeman pairs, implying magnetic field strengths ranging from −11.4 to +13.2 mG, and a median magnetic field strength of |B LOS | ∼ 6 mG. With limited statistics, we present the in-situ magnetic field orientation of the masers and the Galactic magnetic field distribution revealed by the 1720-MHz transition. We also examine the association statistics of 1720-MHz OH SFR masers with other ground-state OH masers, excited-state OH masers, class I and class II methanol masers and water masers, and compare maser positions with mid-infrared images of the parent star forming regions. Of the 33 1720-MHz star formation masers, ten are offset from their central exciting sources, and appear to be associated with outflow activity.

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

Cited by 19 publications

References 46 publications

Accurate Oh Maser Positions From the Splash Pilot Region

Accurate Oh Maser Positions From the Splash Pilot Region

Molecular studies of Planetary Nebulae

MAGMO: polarimetry of 1720-MHz OH masers towards southern star-forming regions

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