Karen B. Kwitter (1), Emma M. M. Lehman (2), Bruce Balick (3) & R.B.C. Henry (4) ((1)Department of Astronomy, Williams College, Williamstown, MA 01267, USA; (2) Department of Astronomy, Williams College, Williamstown, MA 01267, USA; (3) Department of Astronomy, University of Washington, Seattle, WA 98195, USA); (4) H.L. Dodge Department of Physics & Astronomy, University of Oklahoma, Norman, OK 73019, USA)
We present spectroscopic observations and chemical abundances of 16 planetary nebulae (PNe) in the outer disk of M31. The [O III] 4363 line is detected in all objects, allowing a direct measurement of the nebular temperature essential for accurate abundance determinations. Our results show that the abundances in these M31 PNe display the same correlations and general behaviors as Type II PNe in the Milky Way Galaxy. We also calculate photoionization models to derive estimates of central star properties. From these we infer that our sample PNe, all near the peak of the Planetary Nebula Luminosity Function, originated from stars near 2 M_sun. Finally, under the assumption that these PNe are located in M31’s disk, we plot the oxygen abundance gradient, which appears shallower than the gradient in the Milky Way.
Complete preprint ==> http://arxiv.org/abs/1202.4933