ABUNDANCES OF PLANETARY NEBULAE IN M 31 AND M 32

  • HYUNG SIEK (Korea Astronomy Observatory) ;
  • ALLER LAWRENCE H. (Dept. of Physics and Astronomy, UCLA) ;
  • HAN SOO-RYEON (Dept. of Earth Science Education, Korea National University of Education) ;
  • KIM YOUNG-KWANG (Korea Astronomy Observatory) ;
  • HAN WONYONG (Korea Astronomy Observatory) ;
  • CHOI YOUNGJUN (Korea Astronomy Observatory)
  • Published : 2000.10.01

Abstract

Planetary nebulae provide a direct way to probe elemental abundances, their distributions and their gradients in populations in nearby galaxies. We investigate bulge planetary nebulae in M 31 and M 32 using the strong emission lines, H$\alpha$, He I, [O III], [N II], [S II] and [Ne III]. From the [O III] 4363/5007 line ratio and the [O II] 3727/3729, we determine the electron temperatures and number densities. With a standard modeling procedure (Hyung, 1994), we fit the line intensities and diagnostic temperatures, and as a result, we derive the chemical abundances of individual planetary nebulae in M 31 and M 32. The derived chemical abundances are compared with those of the well-known Galactic planetary nebulae or the Sun. The chemical abundances of M 32 appear to be less enhanced compared to the Galaxy or M 31.

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