Abundances of Planetary Nebulae in M31 and M32

Details Abundances of Planetary Nebulae in M31 and M32 Abundances of Planetary Nebulae in M31 and M32

Oct 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000jkas...33...97h&link_type=abstract

Journal of the Korean Astronomical Society, vol. 33, no. 2, pp. 97-110

Astronomy and Astrophysics

Astronomy

1

Ism: Galaxies (M31, M32), Planetary Nebulae: Photoionization Model: Chemical Abundance

Scientific paper

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, Hα, HeI, [OIII],[NII], [SII] and [NeIII]. From the [OIII]4363/5007 line ratio and the [OII] 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 M31 and M32. The derived chemical abundances are compared with those of the well-known Galactic planetary nebulae or the Sun. The chemical abundances of M32 appear to be less enhanced compared to the Galaxy or M31.

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