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For refcode 1993A&A...279..343P:
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Copyright by European Southern Observatory (ESO). Reproduced by permission
1993A&A...279..343P Dark matter in spiral galaxies and the Arimoto-Jablonka photometric model M. Persic, P. Salucci, and K.M. Ashman SISSA, Strada Costiera 11, I-34014 Trieste, Italy CITA, University of Toronto, 60 St. George St., Toronto, Ontario M5S 1A1, Canada Received September 28, accepted December 10, 1992 Abstract. We use the recent stellar population synthesis models by Arimoto & Jablonka (1991), which by introducing the bulge into the calculation of galaxy masses mark a significant improvement over previous one-component models, to show that low-luminosity spiral galaxies have a higher dark matter fraction within the optical radius than high- luminosity spirals. In fact, the derived dark- to-visible mass ratio increases with decreasing luminosity, approximately as L_B_^- 1/2^. This conclusion agrees with previous results based on dynamical disc/halo decompositions of galaxy rotation curves (e.g. Persic & Salucci 1988). On the other hand, we do not find any strong trend between dark matter content and galaxy B - V colours, although we cannot exclude a weak one. Our results agree with Jablonka & Arimoto's (1992) conclusion that colours are not a primary indicator of the dark matter content of spiral galaxies. Instead, we confirm that the luminosity is a fundamental indicator of the dark mass fraction of spiral galaxies. Key words: dark matter - galaxy: fundamental parameters galaxies: spiral
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