The physics of halos surrounding planetary nebulae in the Large Magellanic Cloud

Details The physics of halos surrounding planetary nebulae in the Large Magellanic Cloud The physics of halos surrounding planetary nebulae in the Large Magellanic Cloud

Aug 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005noao.prop..308s&link_type=abstract

NOAO Proposal ID #2005B-0308

Physics

Scientific paper

A new deep, high resolution H-alpha and matching R-band map of the central 25 deg^2 of the Large Magellanic Cloud (LMC) has enabled us to identify extended ionized halos around many planetary nebulae (PNe). A Gemini South - GMOS pilot program executed in February 2005 confirmed the veracity of these LMC PN halos, and allowed for the first time the detection of the halo density. This will provide excellent leverage for solving the progenitor-to-final mass relation for low-mass stars through an accurate determination of the total remnant mass. We propose to use GMOS-S to obtain high resolution spectroscopy for a strategic sample of our newly discovered LMC PN halos. All proposed targets have HST images, thus the characteristics of the inner nebulae and the (brightest) central stars are known. These halos may account for most of the mass lost during the asymptotic giant branch (AGB) evolutionary stage, according to recent hydrodynamic models. The proposed data-set will enable us to determine the key properties of the AGB halos. Together with the available properties of stars and inner nebulae, we will be able to ascertain the applicability of the hydrodynamic and stellar evolutionary models for AGB and post-AGB evolution.

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