Planetary Nebula Luminosity Function Distances to M 33, NGC 2403 and NGC 3627 and a Comparison to the Cepheid Distance Scale

Details Planetary Nebula Luminosity Function Distances to M 33, NGC 2403 and NGC 3627 and a Comparison to the Cepheid Distance Scale Planetary Nebula Luminosity Function Distances to M 33, NGC 2403 and NGC 3627 and a Comparison to the Cepheid Distance Scale

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aas...195.1103k&link_type=abstract

American Astronomical Society, 195th AAS Meeting, #11.03; Bulletin of the American Astronomical Society, Vol. 31, p.1391

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Scientific paper

We report the results of an [O III] λ 5007 survey for planetary nebulae (PNe) in three spiral galaxies: M33 (NGC 598), NGC 2403, and NGC 3627. By comparing on-band/off-band [O III] λ 5007 images with images taken in Hα , we identify 58, 40, and 73 PNe candidates in each galaxy, respectively. From these data, an adopted M31 distance of 770 kpc, and the empirical planetary nebula luminosity function (PNLF), we derive preliminary distances to M33, NGC 2403, and NGC 3627 of .85+0.07-0.10, 3.26+0.27-0.30, 10.41+0.68-0.67 Mpc. With the addition of M33, NGC 2403, and NGC 3627, there are now 11 galaxies with both PNLF and Cepheid distance measurements: 4 galaxies in the Local Group (the SMC, the LMC, M31, and M33), two M81 group galaxies (M81 and NGC 2403), two Leo Group galaxies (M96 and NGC 3627), and three others (M101, NGC 300, and NGC 5253). We examine the systematic behavior between the PNLF and Cepheid distance estimates, and show that for large, metal-rich galaxies, the two distance scales are in excellent agreement. However, we also show that there is a systematic offset between the two scales for low-luminosity, metal-poor galaxies. For these objects, the PNLF method gives distances that are 10% larger than the distances derived from Cepheids. We model this behavior, and provide a metallicity correction for the PNLF technique.

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