Temperature variations from Hubble Space Telescope imagery and spectroscopy of NGC 7009

Rubin, R. H.; Bhatt, Nishant; Dufour, R. J.; Buckalew, B.; Barlow, M. J.; Liu, X.-W.; Storey, P. J.; Balick, Bruce; Ferland, Gary J.; Harrington, J. P.; Martín, P. G.

doi:10.1046/j.1365-8711.2002.05567.x

Cited by 42 publications

(38 citation statements)

References 32 publications

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“…Many papers have been published about the physical properties of NGC 7009 (Gonçalves et al 2003;Rubin et al 2002;Liu et al 1995;Barker 1983;Czyzak & Aller 1979), and in general our estimates are compatible with previous determinations of temperatures and densities. Rubin et al (2002) have evaluated the [O iii] electron temperature variation along the major axis of NGC 7009, with spectrophotometric data obtained with the Hubble Space Telescope at a spatial resolution of 0.05 arcsec.…”

Section: Ngc 7009supporting

confidence: 88%

“…Recently, direct determinations of electron temperature fluctuations have been obtained for the planetary nebulae NGC 4361 (Liu 1998) and NGC 7009 (Rubin et al 2002), and for the H ii regions 30 Doradus (Krabbe & Copetti 2002) and Orion Nebula (Rubin et al 2003;O'Dell et al 2003) from pointto-point measurements of electron temperature and very low temperature fluctuations have been measured. Up to now these four objects are the only ones for which direct estimations of electron temperature fluctuations have been published.…”

Section: Introductionmentioning

confidence: 99%

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Electron temperature fluctuations in planetary nebulae

Krabbe¹,

Copetti²

2005

A&A

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An observational study of the spatial variation of the electron temperature and density in 10 galactic planetary nebulae is presented. The data consist of long-slit spectra of high signal-to-noise ratio in the 3100 to 6900 Å range. Electron temperatures were determined from the . An anti-correlation between temperature and density was found for NGC 2438 and NGC 3132, with the electron temperature increasing with the decrease of electron density and a correlation between temperature and density was found for NGC 2440, NGC 3242, NGC 6302, and NGC 7009, with the electron temperature increasing with the increase of electron density. These relationships seem to be associated with the structure of the nebula. The nebulae in which the correlation between temperature and density is present are ring shaped. The anti-correlation between temperature and density is found in bipolar planetary nebulae that are denser in the centre of the nebula.

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Section: Ngc 7009supporting

confidence: 88%

Section: Introductionmentioning

confidence: 99%

Electron temperature fluctuations in planetary nebulae

Krabbe¹,

Copetti²

2005

A&A

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“…4, right hand plot. No clear evidence for such large changes in T e have been seen in previous observations (e.g., Rubin et al 2002;Tsamis et al 2008), nor in the MUSE [S III] T e map (to be presented in Paper II).…”

Section: Investigation Of C Across the Inner Shellmentioning

confidence: 70%

“…9), but, since this occurred close to the boundary of the IFU area, its reality could not be confirmed. Examination of the HST WFPC2 F487N (Hβ) and F656N (Hα) images of NGC 7009, taken in Programme 8114, also shows evidence for the wave feature at the edge of the inner shell from the simple ratio of the images; a feature not remarked on by Rubin et al (2002).…”

Section: Derivation Of Extinction Mapmentioning

confidence: 95%

The extinction and dust-to-gas structure of the planetary nebula NGC 7009 observed with MUSE

Walsh

Monreal-Ibero

Barlow

et al. 2016

A&A

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Context. Dust plays a significant role in planetary nebulae. Dust ejected with the gas in the asymptotic giant branch (AGB) phase is subject to the harsh environment of the planetary nebula (PN) while the star is evolving towards a white dwarf. Dust surviving the PN phase contributes to the dust content of the interstellar medium. Aims. The morphology of the internal dust extinction has been mapped for the first time in a PN, the bright nearby Galactic nebula NGC 7009. The morphologies of the gas, dust extinction and dust-to-gas ratio are compared to the structural features of the nebula. Methods. Emission line maps in H Balmer and Paschen lines were formed from analysis of MUSE cubes of NGC 7009 observed during science verification of the instrument. The measured electron temperature and density from the same cube were employed to predict the theoretical H line ratios and derive the extinction distribution across the nebula. After correction for the interstellar extinction to NGC 7009, the internal A V /N H has been mapped for the first time in a PN. Results. The extinction map of NGC 7009 has considerable structure, broadly corresponding to the morphological features of the nebula. The dust-to-gas ratio, A V /N H , increases from 0.7 times the interstellar value to >5 times from the centre towards the periphery of the ionized nebula. The integrated A V /N H is about 2× the mean ISM value. A large-scale feature in the extinction map is a wave, consisting of a crest and trough, at the rim of the inner shell. The nature of this feature is investigated and instrumental and physical causes considered; no convincing mechanisms were identified to produce this feature, other than AGB mass loss variations. Conclusions. Extinction mapping from H emission line imaging of PNe with MUSE provides a powerful tool for revealing the properties of internal dust and the dust-to-gas ratio.

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“…One potential explanation to these discrepancies would be the presence of temperature fluctuations inside of H II regions and planetary nebulae (Peimbert 1967). However, the observed values of electron temperature fluctuations have been lower than the ones necessary to Table 1 is only available in electronic form at http://www.edpsciences.org reconcile the abundances derived from forbidden and permitted lines (Liu 1998;Rubin et al 2002;Krabbe & Copetti 2002;Rubin et al 2003;O'Dell et al 2003;Krabbe & Copetti 2005). Other solution that was suggested by Liu et al (2000) would be the presence inside the nebula of hydrogen deficient clumps with high density and rich in heavy elements.…”

Section: Introductionmentioning

confidence: 99%

Chemical abundances in seven galactic planetary nebulae

Krabbe

Copetti

2006

A&A

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An observational study of chemical abundances in the galactic planetary nebulae NGC 1535, NGC 2438, NGC 2440, NGC 3132, NGC 3242, NGC 6302, and NGC 7009 based on long-slit spectra of high signal-to-noise ratio in the 3100 to 6900 Å range is presented. We determined the N, O, Ne, S, and Cl abundances from collisionally excited lines and the He and O ++ abundances from recombination lines. ++ /H + derived from recombination and from forbidden lines present smooth variations along the nebular surface of NGC 7009, with the differences decreasing from the center to the edges of the nebula. If these abundance differences are explained by the presence of electron temperature fluctuations, quantified by the parameter t 2 , a value of about t 2 = 0.09 is required for NGC 3242 and NGC 7009.

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Temperature variations from Hubble Space Telescope imagery and spectroscopy of NGC 7009

Cited by 42 publications

References 32 publications

Electron temperature fluctuations in planetary nebulae

Electron temperature fluctuations in planetary nebulae

The extinction and dust-to-gas structure of the planetary nebula NGC 7009 observed with MUSE

Chemical abundances in seven galactic planetary nebulae

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