Integral Field Spectroscopy of Faint Halos of Planetary Nebulae

Monreal-Ibero, A.; Roth, Martin; Schönberner, D.; Steffen, M.; Böhm, P.

doi:10.1086/432664

Cited by 33 publications

(29 citation statements)

References 10 publications

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“…From the highest to the lowest metal content A&A 523, A86 (2010) Guided by our simulations, we expect metal-poor PNe to show a more smooth or diffuse morphology without a clear-cut signature of a central cavity (or hole) and a sharp outer boundary. The surface brightness profile of NGC 4361 shows indeed neither a pronounced central cavity nor a bright, distinct rim (Monreal-Ibero et al 2005). The metal content of this object is, on the average, 0.1 Z GD (Howard et al 1997, Table 4 of the whole Howard et al sample (see Fig.…”

Section: Structures and Kinematics Of The Modelsmentioning

confidence: 86%

The evolution of planetary nebulae

Schönberner

Jacob

Sandín

et al. 2010

A&A

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Aims. By means of hydrodynamical models we do the first investigations of how the properties of planetary nebulae are affected by their metal content and what can be learned from spatially unresolved spectrograms of planetary nebulae in distant stellar systems. Methods. We computed a new series of 1D radiation-hydrodynamics planetary nebulae model sequences with central stars of 0.595 M surrounded by initial envelope structures that differ only by their metal content. At selected phases along the evolutionary path, the hydrodynamic terms were switched off, allowing the models to relax for fixed radial structure and radiation field into their equilibrium state with respect to energy and ionisation. The analyses of the line spectra emitted from both the dynamical and static models enabled us to systematically study the influence of hydrodynamics as a function of metallicity and evolution. We also recomputed selected sequences already used in previous publications, but now with different metal abundances. These sequences were used to study the expansion properties of planetary nebulae close to the bright cut-off of the planetary nebula luminosity function. Results. Our simulations show that the metal content strongly influences the expansion of planetary nebulae: the lower the metal content, the weaker the pressure of the stellar wind bubble, but the faster the expansion of the outer shell because of the higher electron temperature. This is in variance with the predictions of the interacting-stellar-winds model (or its variants) according to which only the central-star wind is thought to be responsible for driving the expansion of a planetary nebula. Metal-poor objects around slowly evolving central stars become very dilute and are prone to depart from thermal equilibrium because then adiabatic expansion contributes to gas cooling. We find indications that photoheating and line cooling are not fully balanced in the evolved planetary nebulae of the Galactic halo. Expansion rates based on widths of volume-integrated line profiles computed from our radiation-hydrodynamics models compare very well with observations of distant stellar system. Objects close to the bright cut-off of the planetary nebula luminosity function consist of rather massive central stars (>0.6 M ) with optically thick (or nearly thick) nebular shells. The halfwidth-half-maximum velocity during this bright phase is virtually independent of metallicity, as observed, but somewhat depends on the final AGB-wind parameters. Conclusions. The observed expansion properties of planetary nebulae in distant stellar systems with different metallicities are explained very well by our 1D radiation-hydrodynamics models. This result demonstrates convincingly that the formation and acceleration of a planetary nebula occurs mainly because of ionisation and heating of the circumstellar matter by the stellar radiation field, and that the pressure exerted by the shocked stellar wind is less important. Determinations of nebular abundances by means of photoionisa...

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Section: Structures and Kinematics Of The Modelsmentioning

confidence: 86%

The evolution of planetary nebulae

Schönberner

Jacob

Sandín

et al. 2010

A&A

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“…Although NGC 3242 is a well-known PN, with about 350 references from 1990 to date, and even though different diagnostics were clearly determined, only few works investigated its characteristics using some kind of spatially resolved data, from a range of wavelengths. Monreal-Ibero et al (2005), the only work apart from ours that used IFU data for this object, succeeded in determining some properties of the halo, but did not perform a detailed analysis of the physical and chemical properties.…”

Section: Introductionmentioning

confidence: 99%

Spatially resolved physical and chemical properties of the planetary nebula NGC 3242

Monteiro

Gonçalves

Leal-Ferreira

et al. 2013

A&A

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Aims. Optical integral-field spectroscopy was used to investigate the planetary nebula NGC 3242. We analysed the main morphological components of this source, including its knots, but not the halo. In addition to revealing the properties of the physical and chemical nature of this nebula, we also provide reliable spatially resolved constraints that can be used for future photoionisation modelling of the nebula. The latter is ultimately necessary to obtain a fully self-consistent 3D picture of the physical and chemical properties of the object. Methods. The observations were obtained with the VIMOS instrument attached to VLT-UT3. Maps and values for specific morphological zones for the detected emission-lines were obtained and analysed with routines developed by the authors to derive physical and chemical conditions of the ionised gas in a 2D fashion. Results. We obtained spatially resolved maps and mean values of the electron densities, temperatures, and chemical abundances for specific morphological structures in NGC 3242. These results show the pixel-to-pixel variations of the the small-and large-scale structures of the source. These diagnostic maps provide information free from the biases introduced by traditional single long-slit observations. Conclusions. In general, our results are consistent with a uniform abundance distribution for the object, whether we look at abundance maps or integrated fluxes from specified morphological structures. The results indicate that special care should be taken with the calibration of the data and that only data with extremely good signal-to-noise ratio and spectral coverage should be used to ensure the detection of possible spatial variations.

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“…Spectral H 2 imaging in the infrared has been applied mostly to map the morphology of post-AGB stars and the AGB remnant halo of Planetary Nebulae (Hrivnak et al 2008(Hrivnak et al , 2006Sahai & Trauger 1998;Kastner et al 2001;Cox et al 2003;Davis et al 2005; Van de Steene et al 2008). The novel technique of Integral Field Spectroscopy has been applied for these evolved objects to obtain higher spatial and spectral resolution in molecular hydrogen and other lines (Tsamis et al 2008;Sandin et al 2008;Santander-García et al 2007Sharp et al 2006;Lowe & Gledhill 2006;Monreal-Ibero et al 2005).…”

Section: The Molecular Envelopesmentioning

confidence: 99%