Spatially resolved spectroscopy of planetary nebulae and their halos

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

doi:10.1051/0004-6361:200809635

Cited by 37 publications

(56 citation statements)

References 86 publications

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“…Typical values needed for the final AGB mass-loss rates areṀ agb 10 −4 M yr −1 with wind velocities between about 10−15 km s −1 . Values of about 10 −4 M yr −1 for the final AGB mass-loss rates from four well-known Galactic PNe have recently been derived by Sandin et al (2008) using integral field spectroscopy of the respective PN haloes.…”

Section: Discussionmentioning

confidence: 99%

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The evolution of planetary nebulae

Schönberner

Jacob

Sandín

et al. 2010

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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: Discussionmentioning

confidence: 99%

“…Marten (1993aMarten ( , 1995 demonstrated that non-equilibrium may become important for rapidly expanding, low-density nebular shells, and also for cases with quickly evolving central stars. Well-known examples are the hot PN haloes that are extremely out of thermal and ionisation equilibrium (Marten 1993b;Sandin et al 2008).…”

Section: Introductionmentioning

confidence: 99%

The evolution of planetary nebulae

Schönberner

Jacob

Sandín

et al. 2010

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“…In Fig. 14 we show wavelength-calibrated and flat-fielded spectra of data of LARR and PPAK from the central regions of two planetary nebulae: NGC 2392 for PPAK and M 2-2 for LARR, whose outcome is presented in Sandin et al (2008). In the first case we reduced the LARR data using MOX (without correcting for cross-talk) and aperture extraction.…”

Section: Accuracy Of Spectra Extracted Using the Three Different Methodsmentioning

confidence: 99%

“…The required information is mostly found in the data header. For more details on this issue see Sandin et al (2008) and the spatial interpolation procedure of Arribas et al (1999).…”

Section: Object Extractionmentioning

confidence: 99%

P3D: a general data-reduction tool for fiber-fed integral-field spectrographs

Sandín¹,

Becker²,

Roth³

et al. 2010

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The reduction of integral-field spectrograph (IFS) data is demanding work. Many repetitive operations are required to convert raw data into, typically, a large number of spectra. This effort can be markedly simplified through the use of a tool or pipeline, which is designed to complete many of the repetitive operations without human interaction. Here we present our semi-automatic data-reduction tool p3d, which is designed to be used with fiber-fed IFSs. Important components of p3d include a novel algorithm for automatic finding and tracing of spectra on the detector and two methods of optimal spectrum extraction in addition to standard aperture extraction. p3d also provides tools to combine several images, perform wavelength calibration and flat field data. p3d is at the moment configured for four IFSs. To evaluate its performance, we tested the different components of the tool. For these tests we used both simulated and observational data. We demonstrate that a correction for so-called cross-talk due to overlapping spectra on the detector is required for three of the IFSs. Without such a correction, spectra will be inaccurate, in particular if there is a significant intensity gradient across the object. Our tests showed that p3d is able to produce accurate results. p3d is a highly general and freely available tool. It is easily extended to include improved algorithms, new visualization tools, and support for additional instruments. The program code can be downloaded from the p3d-project web site http://p3d.sourceforge.net.

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“…This can be tessellated a posteriori, preserving the relevant spatial information as best possible, but at the same time optimizing the quality of the signal by co-adding the spectra belonging to a given portion of the mapped area -the tile -(e.g. Monreal-Ibero et al 2005;Sandin et al 2008). Here, we use this principle to explore the capabilities of MUSE to obtain spatially resolved information of extragalactic DIBs.…”

Section: Introductionmentioning

confidence: 99%

Towards DIB mapping in galaxies beyond 100 Mpc

Monreal-Ibero

Weilbacher

Wendt

et al. 2015

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Context. Diffuse interstellar bands (DIBs) are non-stellar weak absorption features of unknown origin found in the spectra of stars viewed through one or several clouds of the interstellar medium (ISM). Research of DIBs outside the Milky Way is currently very limited. In particular, spatially resolved investigations of DIBs outside of the Local Group are, to our knowledge, inexistent. Aims. In this contribution, we explore the capability of the high-sensitivity integral field spectrograph, MUSE, as a tool for mapping diffuse interstellar bands at distances larger than 100 Mpc. Methods. We used MUSE commissioning data for AM 1353-272 B, the member with the highest extinction of the Dentist's Chair, an interacting system of two spiral galaxies. High signal-to-noise spectra were created by co-adding the signal of many spatial elements distributed in a geometry of concentric elliptical half-rings. Results. We derived decreasing radial profiles for the equivalent width of the λ5780.5 DIB both in the receding and approaching side of the companion galaxy up to distances of ∼4.6 kpc from the centre of the galaxy. The interstellar extinction as derived from the Hα/Hβ line ratio displays a similar trend, with decreasing values towards the external parts. This translates into an intrinsic correlation between the strength of the DIB and the extinction within AM 1353-272 B, consistent with the currently existing global trend between these quantities when using measurements for Galactic and extragalactic sightlines. Conclusions. It seems feasible to map the DIB strength in the Local Universe, which has up to now only been performed for the Milky Way. This offers a new approach to studying the relationship between DIBs and other characteristics and species of the ISM in addition to using galaxies in the Local Group or sightlines towards very bright targets outside the Local Group.

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Spatially resolved spectroscopy of planetary nebulae and their halos

Cited by 37 publications

References 86 publications

The evolution of planetary nebulae

The evolution of planetary nebulae

P3D: a general data-reduction tool for fiber-fed integral-field spectrographs

Towards DIB mapping in galaxies beyond 100 Mpc

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