A [ITAL]HUBBLE SPACE TELESCOPE[/ITAL] Survey for Resolved Companions of Planetary Nebula Nuclei

Ciardullo, Robin; Bond, Howard E.; Sipior, M.; Fullton, L. K.; Zhang, C.-Y.; Schaefer, K. G.

doi:10.1086/300940

Cited by 182 publications

(250 citation statements)

References 72 publications

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“…The variability described here is not from a close companion, but rather reflects pulsations or variable winds. Ciardullo et al (1999) found no wide companion in NGC 6826, NGC 6543, NGC 2371 and NGC 5882, and only a possible association in NGC 2392. Hf 2-1 is a new discovery made from our deep AAOmega (Sharp et al 2006) observations described in Paper I (Fig.…”

Section: Can Low-ionisation Structures Be Used To Identify a Previousmentioning

confidence: 71%

Binary planetary nebulae nuclei towards the Galactic bulge

Miszalski

Acker

Parker

et al. 2009

A&A

146

218

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Considerable effort has been applied towards understanding the precise shaping mechanisms responsible for the diverse range of morphologies exhibited by planetary nebulae (PNe). A binary companion is increasingly gaining support as a dominant shaping mechanism, however morphological studies of the few PNe that we know for certain were shaped by binary evolution are scarce or biased. Newly discovered binary central stars (CSPN) from the OGLE-III photometric variability survey have significantly increased the sample of post common-envelope (CE) nebulae available for morphological analysis. We present Gemini South narrow-band images for most of the new sample to complement existing data in a qualitative morphological study of 30 post-CE nebulae. Nearly 30% of nebulae have canonical bipolar morphologies, however this rises to 60% once inclination effects are incorporated with the aid of geometric models. This is the strongest observational evidence yet linking CE evolution to bipolar morphologies. A higher than average proportion of the sample shows low-ionisation knots, filaments or jets suggestive of a binary origin. These features are also common around emission-line nuclei which may be explained by speculative binary formation scenarios for H-deficient CSPN.

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Section: Can Low-ionisation Structures Be Used To Identify a Previousmentioning

confidence: 71%

Binary planetary nebulae nuclei towards the Galactic bulge

Miszalski

Acker

Parker

et al. 2009

A&A

146

218

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“…The most likely solution is that this central star is a binary and the secondary, which is unseen in the visual, is of a much higher temperature and is responsible for the high degree of ionization found. The possible presence of a hotter star has been suspected earlier; Ciardullo et al (1999) have looked for it but have found only a very faint nearby star. If this is the source of ionization it cannot be a main sequence star because if this was so it would be too distant to be associated with the nebula.…”

Section: Discussionmentioning

confidence: 97%

“…(1) are the HST measurements of Wolff et al (2000), Col. (2) are HST measurements of Ciardullo et al (1999) and Col. (3) are the ground based measurements made by Heap & Hintzen (1990a). Very faint central stars are difficult to measure.…”

Section: Stellar Magnitudementioning

confidence: 99%

“…This in turn could introduce systematic errors in evolution calculations made using them. In addition Ciardullo et al (1999) measured accurate distances of a small sample of binary PNe and concluded that for these nebulae the statistical distances are overestimates. Instead we determine distances using three methods which, while giving somewhat more uncertain individual distances, are much less likely to have systematic errors.…”

Section: Pn Distancesmentioning

confidence: 99%

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Planetary nebulae abundances and stellar evolution II

Pottasch

Bernard─Salas

2010

A&A

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Context. In recent years mid-and far infrared spectra of planetary nebulae have been analysed and lead to more accurate abundances. It may be expected that these better abundances lead to a better understanding of the evolution of these objects. Aims. The observed abundances in planetary nebulae are compared to those predicted by the models of Karakas (2003, Thesis, Monash Univ. Melbourne) in order to predict the progenitor masses of the various PNe used. The morphology of the PNe is included in the comparison. Since the central stars play an important role in the evolution, it is expected that this comparison will yield additional information about them. Methods. First the nitrogen/oxygen ratio is discussed with relation to the helium/hydrogen ratio. The progenitor mass for each PNe can be found by a comparison with the models of Karakas. Then the present luminosity of the central stars is determined in two ways: first by computing the central star effective temperature and radius, and second by computing the nebular luminosity from the hydrogen and helium lines. This luminosity is also a function of the initial mass so that these two values of initial mass can be compared. Results. Six of the seven bipolar nebulae can be identified as descendants of high mass stars (4−6 M ) while the seventh is ambiguous. Most of the elliptical PNe have central stars which descend from low initial mass stars, although there are a few caveats which are discussed. There is no observational evidence for a higher mass for central stars which have a high carbon/oxygen ratio. The evidence provided by the abundance comparison with the models of Karakas is consistent with the HR diagram to which it is compared. In the course of this discussion it is shown how "optically thin" nebulae can be separated from those which are "optically thick".

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“…It is evidently a young PN (dynamical age ∼600 yr; Masson 1989) and displays a remarkably complex morphology. Optical imaging by the Hubble Space Telescope (HST; Bond et al 1997;Ciardullo et al 1999) reveals a bright, compact (∼5Љ radius) core region encircled by concentric rings of reflection nebulosity that extend to 15Љ in radius (Fig. 1a).…”

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confidence: 99%

Discovery of Extended X-Ray Emission from the Planetary Nebula NGC 7027 by the [ITAL]Chandra X-Ray Observatory[/ITAL]

Kastner

Vrtilek

Soker

2001

The Astrophysical Journal

116

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We report the discovery of X-ray emission from NGC 7027, a prototypical object for the study of the formation and evolution of planetary nebulae. Observations with the Advanced CCD Imaging Spectrometer (ACIS) aboard the Chandra X-Ray Observatory show that the X-ray emission from NGC 7027 is extended and is bipolar in morphology. The ACIS spectrum displays strong emission from highly ionized Ne and weaker emission features, which we attribute to O, Mg, and Si. Model fits to this spectrum suggest a characteristic temperature T ∼ 3 # X K and an intrinsic (unabsorbed) X-ray luminosity of ergs s Ϫ1 . The intranebular absorption of 6 32 10 L ∼ 1.3 # 10 X X-ray emission is highly nonuniform, but the modeling indicates an average column density cm Ϫ2 , 21 N ∼ 6 # 10 H consistent with previous measurements of relatively large visual extinction within the nebula. We suggest that the X-ray emission from NGC 7027 is or was generated by a hitherto undetected fast wind from the central star of NGC 7027 or from a companion to this star. Chandra's detection of extended, high-temperature X-ray emission from BD ϩ30Њ3639, NGC 6543, and now NGC 7027 suggests that such emission is a common feature of young planetary nebulae.

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A [ITAL]HUBBLE SPACE TELESCOPE[/ITAL] Survey for Resolved Companions of Planetary Nebula Nuclei

Cited by 182 publications

References 72 publications

Binary planetary nebulae nuclei towards the Galactic bulge

Binary planetary nebulae nuclei towards the Galactic bulge

Planetary nebulae abundances and stellar evolution II

Discovery of Extended X-Ray Emission from the Planetary Nebula NGC 7027 by the [ITAL]Chandra X-Ray Observatory[/ITAL]

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