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Studies of the Planetary Nebulae in NGC 5128

Published online by Cambridge University Press:  26 May 2016

J. R. Walsh ,
G. H. Jacoby ,
R. F. Peletier  and
N. A. Walton
J. R. Walsh
Affiliation:
ST-ECF, ESO, Karl-Schwarzschild Strasse 2, D-85748 Garching, Germany
G. H. Jacoby
Affiliation:
KPNO, P.O. Box 26732, Tucson, AZ 85726, USA
R. F. Peletier
Affiliation:
Department of Physics & Astronomy, University of Nottingham, University Park, Nottingham NG7 2RD, UK
N. A. Walton
Affiliation:
Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 OHA, UK

Extract

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As the nearest large elliptical galaxy, NGC 5128 is ideal for planetary nebula studies. Its size, favourable aspect, small distance and reddening allow low mass stellar evolution in a whole galaxy to be surveyed. The surface density and properties of the PN can be compared with stars of various ages, metallicities and components (bulge, halo). The PN provide the α-element abundances whilst stellar photometry is calibrated against Fe/H; applied to the same stellar population, the PN abundances can be related to those of the stars. Gradients and non-radial trends in the abundance can be mapped using spectral observations of a large number of PN, allowing star formation history to be studied.

Type
Part VIII: Planetary Nebulae as Galaxy Probes
Information
Symposium - International Astronomical Union , Volume 209: Planetary Nebulae: Their Evolution and Role in the Universe , 2003 , pp. 593
Copyright
Copyright © Astronomical Society of the Pacific 2003