Kinematics of the H<sub>2</sub>O masers at the centre of the planetary nebula K3-35

Uscanga, L.; Gómez, Yolanda; Raga, A. C.; Cantó, J.; Anglada, Guillem; Gómez, José F.; Torrelles, J. M.; Miranda, L. F.

doi:10.1111/j.1365-2966.2008.13815.x

Cited by 28 publications

(36 citation statements)

References 36 publications

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“…However, most of these masers, and the overall distribution of all OH and H 2 O masers (Figure 4), seem to trace an equatorial structure, perpendicular to the lobes. This could be related to the low-velocity equatorial flows seen in some "water fountains" (Imai 2007) and the toroidal distribution of H 2 O masers in other maser-emitting PNe (de Gregorio- Monsalvo et al 2004;Uscanga et al 2008). The spatial distribution of the 1720 MHz OH maser spots and the presence of clear Zeeman pairs suggest that OH emission at 1720 MHz in IRAS 16333−4807 arises from an energetic ejection of material along the equatorial plane, probably in the form of an expanding, magnetized torus.…”

Section: The Origin Of Oh Maser Emissionmentioning

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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Section: The Origin Of Oh Maser Emissionmentioning

confidence: 99%

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

Qiao

Walsh

Gómez

et al. 2016

ApJ

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“…The solutions were based on the minimisation of the χ 2 V function expressed in Eq. (8) by Uscanga et al (2008) …”

Section: Rotating and Expanding Ringmentioning

confidence: 99%

“…There is a tendency for flatter structures to have a larger velocity width, in all sources apart from G23.657−00.127, (see Table 5), which suggests that we observe the effects of inclination and all motion is intrinsic to the plane of the ring. To test this hypothesis, we applied the model of a rotating and expanding thin disc (Uscanga et al 2008) to the nine ring-like masers. First, the coordinates of the spots (x j , y j ) were transformed to a reference system (x j , y j ) in which the origin was the center of the ellipse and the x'-axis was directed along the major axis of the projected ellipse (see Fig.…”

Section: Rotating and Expanding Ringmentioning

confidence: 99%

“…First, the coordinates of the spots (x j , y j ) were transformed to a reference system (x j , y j ) in which the origin was the center of the ellipse and the x'-axis was directed along the major axis of the projected ellipse (see Fig. 1 in Uscanga et al 2008). We then attempted to reproduce the kinematics using the LSR velocities (V LSR ) of the maser spots to determine rotation (V rot ), expansion (V exp ), and systemic (V sys ) velocities of each source.…”

Section: Rotating and Expanding Ringmentioning

confidence: 99%

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The diversity of methanol maser morphologies from VLBI observations

Bartkiewicz

Szymczak

Langevelde

et al. 2009

A&A

113

255

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Context. The 6.7 GHz methanol maser marks an early stage of high-mass star formation, but the origin of this maser is currently a matter of debate. In particular it is unclear whether the maser emission arises in discs, outflows or behind shocks running into rotating molecular clouds. Aims. We investigated which structures the methanol masers trace in the environment of high-mass protostar candidates by observing a homogenous sample of methanol masers selected from Torun surveys. We also probed their origins by looking for associated H II regions and IR emission. Methods. We selected 30 methanol sources with improved position accuracies achieved using MERLIN and another 3 from the literature. We imaged 31 of these using the European VLBI Network's expanded array of telescopes with 5-cm (6-GHz) receivers. We used the VLA to search for 8.4 GHz radio continuum counterparts and inspected Spitzer GLIMPSE data at 3.6-8 μm from the archive. Results. High angular resolution images allowed us to analyze the morphology and kinematics of the methanol masers in great detail and verify their association with radio continuum and mid-infrared emission. A new class of "ring-like" methanol masers in starforming regions appeared to be suprisingly common, 29% of the sample. Conclusions. The new morphology strongly suggests that methanol masers originate in the disc or torus around a proto-or a young massive star. However, the maser kinematics indicate the strong influence of outflow or infall. This suggests that they form at the interface between the disc/torus and a flow. This is also strongly supported by Spitzer results because the majority of the masers coincide with 4.5 μm emission to within less than 1 . Only four masers are associated with the central parts of UC H II regions. This implies that 6.7 GHz methanol maser emission occurs before H II region observable at cm wavelengths is formed.

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“…Recently, Velázquez et al (2007) have modeled the morphology of this PN by considering a precessing jet evolving in a dense AGB circumstellar medium. Uscanga et al (2008) re-analyzed the 22 GHz VLA data, and modeled the kinematics of the water maser emission from the central region. They claim the detection of a circular ring with a radius of ∼100 AU with an inclination to the line of sight of 55 • , almost perpendicular to the observed outflows.…”

Section: K 3-35mentioning

confidence: 99%

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

Desmurs¹,

Baudry²,

Sivagnanam³

et al. 2010

A&A

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Aims. The aim of this study is to investigate the physical properties of molecular envelopes of planetary nebulae (PNe) in their earliest stages of evolution. Methods. Using the 100 m telescope at Effelsberg, we have undertaken a high sensitivity discrete source survey for the first excited state of OH maser emission (J = 5/2, 2 Π 3/2 at 6 GHz) in the direction of PNe and proto-planetary nebulae (PNe) exhibiting 18 cm OH emission (main and/or satellite lines), and we further validate our detections using the Nançay radio telescope at 1.6-1.7 GHz and MERLIN interferometer at 1.6-1.7 and 6 GHz. Results. Two sources have been detected at 6035 MHz (5 cm), both of them are young (or very young) PNe. The first one is a confirmation of the detection of a weak 6035 MHz line in Vy 2-2. The second one is a new detection, in K 3-35, which was already known to be an exceptional late type star because it exhibits 1720 MHz OH emission. The detection of 6035 MHz OH maser emission is confirmed by subsequent observations made with the MERLIN interferometer. These lines are very rarely found in evolved stars. The 1612 MHz masers surround but are offset from the 1720 and 6035 MHz masers which in turn lie close to a compact 22 GHz continuum source embedded in the optical nebula.

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Kinematics of the H₂O masers at the centre of the planetary nebula K3-35

Cited by 28 publications

References 36 publications

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

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

The diversity of methanol maser morphologies from VLBI observations

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

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Kinematics of the H2O masers at the centre of the planetary nebula K3-35

Cited by 28 publications

References 36 publications

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

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

The diversity of methanol maser morphologies from VLBI observations

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

Contact Info

Product

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About

Kinematics of the H₂O masers at the centre of the planetary nebula K3-35