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The Large Magellanic Cloud PN population

Published online by Cambridge University Press:  11 May 2017

Warren A. Reid
Warren A. Reid*
Affiliation:
Department of Physics and Astronomy, Macquarie University Sydney, NSW, 2109Australia email: warren.reid@outlook.com Western Sydney University, Locked Bag 1797, Penrith South DC, NSW 1797, Australia
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Abstract

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The Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) allow us to study late stellar evolution in environments that are respectively about a half and a quarter the metallicity of the Milky Way. With a known distance and low reddening, the LMC is an excellent environment to study PNe and conduct multiple studies. Over the past twelve months we have used the UKST Hα survey to complete our search for faint PNe in the outer most LMC beyond the 64 deg2 area previously covered. Follow-up spectroscopy using AAOmega on the AAT and the 2.3-m telescope at Siding Spring Observatory have yielded a further 22 new LMC PNe while confirming the 8 previously known in the outer LMC. Medium- and high-resolution spectra have been used to measure fluxes and derive densities, mass and central star temperatures. A strong correlation is found between PNe and stellar density. This is visually displayed and given an empirical value of α = 1 PN / 2.5 × 106 L⊙. The current [O iii]-based PNLF, apart from providing an excellent standard candle, contains information about the parent population. The new PNLF, which extends down nine magnitudes, permits investigation of the faint end, the overall effects of internal extinction and provides clues to explain the insensitivity of the PNLF cutoff. When compared to the ionised density and mass of LMC PNe, the PNLF reveals it’s bimodal characteristics. Two separate evolutionary paths are evident for young, evolving PNe.

Keywords

Planetary nebulae: GeneralMagellanic Cloudssurveyskinematics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , General Assembly A29B , August 2015 , E6
Copyright
Copyright © International Astronomical Union 2017 

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