Dark matter in spiral galaxies and the Arimoto-Jablonka photometric model

Details Dark matter in spiral galaxies and the Arimoto-Jablonka photometric model Dark matter in spiral galaxies and the Arimoto-Jablonka photometric model

Nov 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...279..343p&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 279, no. 2, p. 343-350

Astronomy and Astrophysics

Astrophysics

8

Astronomical Models, Astronomical Photometry, Dark Matter, Galactic Evolution, Spiral Galaxies, Star Formation, Accretion Disks, Galactic Halos, Galactic Rotation, Mathematical Models, Stellar Luminosity

Scientific paper

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 1/(square root of LB). This conclusion agrees with previous results based on dynamical disk 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 colors, although we cannot exclude a weak one. Our results agree with Jablonka & Arimoto's (1992) conclusion that colors 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.

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