Title: Galactic Dynamics and Planetary Nebulae

Abstract: Efforts to determine the mass distribution of early-type 
galaxies are generally hampered by the scarcity of useful tracers of the 
potential at large radii. Planetary Nebulae (PNe) offer a way around 
this problem: as remants of intermediate mass stars we expect them to 
follow the stellar light distribution and be numerous enough to be an 
effective tracer. PNe radiate hundreds of solar luminosities in a few 
emission lines (mostly [OIII] 5007λ ), making it possible to detect them 
over extragalactic distances and measure their radial velocities. I 
report on observations of four early-type galaxies performed with the 
Rutgers Fabry-Perot (RFP). I briefly discuss the RFP, our observations 
and selection procedure. In addition, I constructed simple mass models 
for the two galaxies with a sufficiently large PN sample, the Leo 
galaxies NGC 3379 and NGC 3384. Using a Monte Carlo Markov Chain method 
we explored the space of likely mass models. Our spherical model for the 
E1 galaxy NGC 3379 shows that mass follows light within five half-light 
radii with an overall B band mass-to-light ratio ∼ 6 (solar units). Our 
model for the SB0 galaxy NGC 3384 is not as successful, although it does 
seem to indicate that mass follows light as well.