Rotation curves and dark matter in early type disk galaxies

Details Rotation curves and dark matter in early type disk galaxies Rotation curves and dark matter in early type disk galaxies

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004bdmh.confe..68n&link_type=abstract

"Proceedings of "Baryons in Dark Matter Halos". Novigrad, Croatia, 5-9 Oct 2004. Editors: R. Dettmar, U. Klein, P. Salucci. Publ

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We are studying the rotation curves and mass distribution in a sample of 16 early type disk galaxies, with morphological type between S0 and Sab and B-band absolute magnitude between -17 and -22; they form the massive and high-surface brightness extreme of the disk galaxy population. Our study is designed to investigate the relation between dark and luminous matter in these systems, of which little yet is known. From a combination of WSRT HI observations and long-slit optical spectra, we have obtained high-quality rotation curves which probe the dynamical mass distribution from small to large scales. Due to the presence of the massive bulges, the rotation curves rise extremely rapidly in the centers; even in the optical spectra the central velocity gradients are often barely resolved. Many of our galaxies have declining rotation curves, with the outermost measured velocity up to 40% lower than the maximum. Some of the galaxies in our sample have very high rotation velocities, with Vmax ˜ 400 km/s. We decompose the rotation curves into contributions from the luminous (stellar and gaseous) and dark matter. The stellar bulges always dominate the rotation curves in the inner regions and are at least partly responsible for the decline at larger radii. We are able to put both upper and lower limits on their stellar mass-to-light ratios. Dark matter is needed to explain the shape of rotation curves in the outer parts. As an example, we present here the mass models for UGC 9133.

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