Robin Ciardullo
Published 2004-07-14Version 1
The [O III] 5007 planetary nebula luminosity function (PNLF) occupies an important place on the extragalactic distance ladder: it is the only standard candle that can be applied to all the large galaxies of the Local Supercluster. We review the method's precision, and use it to show that the distance scale defined by Cepheids and the Surface Brightness Fluctuation method is likely too large by ~ 7%. We also discuss some of the physics underlying the phenomenon, and present clues as why the technique is so resilient.
Comments: 12 pages and 5 figures - A contribution to the ESO Intl. Workshop on "Planetary Nebulae beyond the Milky Way", Garching (Germany), May 19-21, 2004 - Conference proceedings will appear in the Springer-Verlag series of ESO Astrophysics Symposia (eds. J.R. Walsh, L. Stanghellini & N. Douglas)
Potential of the Surface Brightness Fluctuation method to measure distances to dwarf ellipticals in nearby clusters
Calibrating Type Ia Supernovae using the Planetary Nebula Luminosity Function I. Initial Results
Improved simulations of the planetary nebula luminosity function
