Hubble-type outflows of the high-excitation poly-polar planetary nebula NGC 6302 - from expansion proper motions

Meaburn, J.; Lloyd, M.; Vaytet, N.; López, J. A.

doi:10.1111/j.1365-2966.2007.12782.x

Cited by 43 publications

(93 citation statements)

References 11 publications

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“…The line profile from slit g, which passes close to the central star, shows both sides of the high-speed bipolar outflow, covering a velocity range of over 400 km s −1 . The high-velocity components in all slits display their maximum velocity close to the star and this decreases with distance from it, contrary to what is usually observed in the so-called Hubble flows where the outflow increases its velocity with distance from the source (see, e.g., Meaburn et al 2008). …”

Section: Discussioncontrasting

confidence: 75%

The Outflows and Three-Dimensional Structure of NGC 6337: A Planetary Nebula With a Close Binary Nucleus

García-Díaz¹,

Clark²,

López³

et al. 2009

ApJ

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NGC 6337 is a member of the rare group of planetary nebulae where a close binary nucleus has been identified. The nebula's morphology and emission line profiles are both unusual, particularly the latter. We present a thorough mapping of spatially resolved, long-slit echelle spectra obtained over the nebula that allows a detailed characterization of its complex kinematics. This information, together with narrowband imagery, is used to produce a three-dimensional (3D) model of the nebula using the code SHAPE. The 3D model yields a slowly expanding toroid with large density fluctuations in its periphery that are observed as cometary knots. A system of bipolar expanding caps of low ionization is located outside the toroid. In addition, an extended high velocity and tenuous bipolar collimated outflow is found emerging from the core and sharply bending in opposite directions, a behavior that cannot be accounted for by pure magnetic launching and collimation unless the source of the outflow is precessing or rotating, as could be expected from a close binary nucleus.

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Section: Discussioncontrasting

confidence: 75%

The Outflows and Three-Dimensional Structure of NGC 6337: A Planetary Nebula With a Close Binary Nucleus

García-Díaz¹,

Clark²,

López³

et al. 2009

ApJ

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“…For comparison, similar lobes of the PN NGC 6302 were conclusively shown to have been ejected at high velocity (630 km s −1 ; Meaburn et al 2005Meaburn et al , 2008 and formed over a period of ≈2000 yr. The bipolar outflow from Mira A revealed here could easily develop into such features over a similar timescale.…”

Section: Evolutionmentioning

confidence: 98%

A high-speed bipolar outflow from the archetypical pulsating star Mira A

Meaburn

López

Boumis

et al. 2009

A&A

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Optical images and high-dispersion spectra have been obtained of the ejected material surrounding the pulsating AGB star Mira A. The two streams of knots on either side of the star, found in far-ultraviolet (FUV) GALEX images, have now been imaged clearly in the light of Hα. Spatially resolved profiles of the same line reveal that the bulk of these knots form a bipolar outflow with radial velocity extremes of ±150 km s −1 with respect to the central star. The south stream is approaching and the north stream receding from the observer. A displacement away from Mira A between the position of one of the south-stream knots in the new Hα image and its position in the previous Palomar Observatory Sky Survey (POSS I) red plate was noted. If interpreted as a consequence of expansion proper motions, the bipolar outflow is tilted at 69 • ± 15 • to the plane of the sky, has an outflow velocity of 160 ± 10 km s −1 and is ≈1000 y old.

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“…Precise HST optical parallaxes, also based on multi-epoch nebular images, have become available in the last decade (Reed et al 1999;Palen et al 2002;Li, Harrington & Borkowski 2002;Hajian 2006) which promise to have a significant impact on the local PN distance scale. Furthermore, Meaburn et al (2008) and Boumis & Meaburn (2013) have used the proper motions of fast-moving outer optical knots (assuming ballistic motion) to derive distances for NGC 6302 of 1170 ± 140 pc, and KjPn 8 of 1800 ± 300 pc, respectively, though the extended nebula of KjPn 8 does only as a rough integrated Hα flux available, so has been excluded as a calibrator (but see §A1).…”

Section: Expansion Parallaxesmentioning

confidence: 99%

The H surface brightness-radius relation: a robust statistical distance indicator for planetary nebulae

Frew¹,

Parker²,

Bojičić³

2015

Monthly Notices of the Royal Astronomical Society

166

127

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Measuring the distances to Galactic planetary nebulae (PNe) has been an intractable problem for many decades. We have now established a robust optical statistical distance indicator, the Hα surface brightness -radius or S Hα -r relation, which addresses this problem. We developed this relation from a critically evaluated sample of primary calibrating PNe. The robust nature of the method results from our revised calibrating distances with significantly reduced systematic uncertainties, and the recent availability of high-quality data, including updated nebular diameters and integrated Hα fluxes. The S Hα -r technique is simple in its application, requiring only an angular size, an integrated Hα flux, and the reddening to the PN. From these quantities, an intrinsic radius is calculated, which when combined with the angular size, yields the distance directly. Furthermore, we have found that optically thick PNe tend to populate the upper bound of the trend, while optically-thin PNe fall along the lower boundary in the S Hα -r plane. This enables sub-trends to be developed which offer even better precision in the determination of distances, as good as 18 per cent in the case of optically-thin, high-excitation PNe. This is significantly better than any previous statistical indicator. We use this technique to create a catalogue of statistical distances for over 1100 Galactic PNe, the largest such compilation in the literature to date. Finally, in an appendix, we investigate both a set of transitional PNe and a range of PN mimics in the S Hα -r plane, to demonstrate its use as a diagnostic tool. Interestingly, stellar ejecta around massive stars plot on a tight locus in S Hα -r space with the potential to act as a separate distance indicator for these objects.

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Hubble-type outflows of the high-excitation poly-polar planetary nebula NGC 6302 - from expansion proper motions

Cited by 43 publications

References 11 publications

The Outflows and Three-Dimensional Structure of NGC 6337: A Planetary Nebula With a Close Binary Nucleus

The Outflows and Three-Dimensional Structure of NGC 6337: A Planetary Nebula With a Close Binary Nucleus

A high-speed bipolar outflow from the archetypical pulsating star Mira A

The H surface brightness-radius relation: a robust statistical distance indicator for planetary nebulae

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