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Imaging the elusive H-poor gas in planetary nebulae with large abundance discrepancy factors

Published online by Cambridge University Press:  08 August 2017

Jorge García-Rojas Open the ORCID record for Jorge García-Rojas [Opens in a new window] ,
Romano L. M. Corradi ,
Henri M. J. Boffin ,
Hektor Monteiro ,
David Jones ,
Roger Wesson ,
Antonio Cabrera-Lavers  and
Pablo Rodríguez-Gil
Jorge García-Rojas
Affiliation:
Inst. de Astrofísica de Canarias, Vía Láctea, s/n, La Laguna, E-38205, Spain, email: jogarcia@iac.es Dept. de Astrofísica, Universidad de La Laguna, La Laguna, E-38205, Spain
Romano L. M. Corradi
Affiliation:
Inst. de Astrofísica de Canarias, Vía Láctea, s/n, La Laguna, E-38205, Spain, email: jogarcia@iac.es GRANTECAN, Cuesta de San José s/n, E-38712, Breña Baja, La Palma, Spain
Henri M. J. Boffin
Affiliation:
European Southern Observatory, Karl Schwarzschild Strasse 2, 85748 Garching, Germany
Hektor Monteiro
Affiliation:
Univ. Fed. Itajubá, Av. BPS 1303-Pinheirinho, 37500-903, Itajubá, Brazil
David Jones
Affiliation:
Inst. de Astrofísica de Canarias, Vía Láctea, s/n, La Laguna, E-38205, Spain, email: jogarcia@iac.es Dept. de Astrofísica, Universidad de La Laguna, La Laguna, E-38205, Spain
Roger Wesson
Affiliation:
Dept. of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, UK
Antonio Cabrera-Lavers
Affiliation:
Inst. de Astrofísica de Canarias, Vía Láctea, s/n, La Laguna, E-38205, Spain, email: jogarcia@iac.es GRANTECAN, Cuesta de San José s/n, E-38712, Breña Baja, La Palma, Spain
Pablo Rodríguez-Gil
Affiliation:
Inst. de Astrofísica de Canarias, Vía Láctea, s/n, La Laguna, E-38205, Spain, email: jogarcia@iac.es Dept. de Astrofísica, Universidad de La Laguna, La Laguna, E-38205, Spain
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Abstract

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The discrepancy between abundances computed using optical recombination lines (ORLs) and collisionally excited lines (CELs) is a major, unresolved problem with significant implications for the determination of chemical abundances throughout the Universe. In planetary nebulae (PNe), the most common explanation for the discrepancy is that two different gas phases coexist: a hot component with standard metallicity, and a much colder plasma enhanced in heavy elements. This dual nature is not predicted by mass loss theories, and direct observational support for it is still weak. In this work, we present our recent findings that demonstrate that the largest abundance discrepancies are associated with close binary central stars. OSIRIS-GTC tunable filter imaging of the faint O ii ORLs and MUSE-VLT deep 2D spectrophotometry confirm that O ii ORL emission is more centrally concentrated than that of [Oiii] CELs and, therefore, that the abundance discrepancy may be closely linked to binary evolution.

Keywords

binaries: closeISM: abundances(ISM:) planetary nebulae: generalstars: windsstars: outflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S323: Planetary Nebulae: Multi-Wavelength Probes of Stellar and Galactic Evolution , October 2016 , pp. 65 - 69
Copyright
Copyright © International Astronomical Union 2017 

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