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For refcode 1996AJ....112.1415J:
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1996AJ....112.1415J THE LUMINOSITY-METALLICITY RELATION FOR BULGES OF SPIRAL GALAXIES P. JABLONKA URA 173 CNRS-DAFC, Observatoire de Paris, 92195 Meudon Principal Cedex, France Electronic mnil: jablonka@obspm.fr P. MARTIN Steward Observatory, University of Arizona, Tucson, Arizona 85721 Electronic mnil: pmartin@eso.org N. ARIMOTO Institute of Astronomy, University of Tokyo, Mitaka, Tokyo 181, Japan Electronic mnil: arimoto@mtk.ioa.s.u-tokyo.ac.jp Received 1996 January 16; revised 1996 April 19 ABSTRACT Optical integrated spectra of bulges have been obtained for 28 spiral galaxies for which the surface brightness profiles were decomposed into disk and bulge contributions by Kent (ApJS, 59, 115(1985)] and Simien & de Vaucouleurs [ApJ, 302, 564 (1986)]. By applying an appropriate aperture size for each galaxy, the unavoidable contamination of disk starlight has been carefully minimized and set to ~1/7 of the total stellar light. The sample covers a wide range in bulge luminosity and morphology. The Mg_2_ index shows a tight correlation with the bulge intrinsic luminosity, similar-and extended at fainter magnitudes-to the relationship known for ellipticals. Other features such as CaII K, CN, G- band, and TiO show similar trend with the bulge luminosity. On the contrary, the Fe5270 and Fe5335 iron lines are constant-within some dispersion-for all bulges. A simple application of a stellar population synthesis model suggests that magnesium should be most enhanced with respect to iron in the brightest bulges. Concerning the structural parameters, bulges do occupy the same region in the fundamental plane as ellipticals. In conclusion, the present study favors the idea that the bulk of stars in bulges have formed with only moderate or negligible influence of the disk material, likely by very similar processes as those driving the formation of elliptical galaxies.
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