Titlebook: Dark Matter in Astro- and Particle Physics; Proceedings of the I H. V. Klapdor-Kleingrothaus Conference proceedings 2001 Springer-Verlag Be

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The Distribution of Dark Matter in Galaxies: Constant-Density Dark Halos Envelop the Stellar Disksalaxies. Their rotation curves, coadded according to the galaxy luminosity, conform to an Universal profile which can be represented as the sum of an exponential thin disk term plus a spherical halo term with a flat density core. From dwarfs to giants, these halos feature a constant density region o

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The Amount of Dark Matter in Spiral Galaxies198, 6503, and 7184 are analyzed. For these galaxies the radial velocity dispersions of the stars have been measured. If the parameters of the decompositions are chosen according to the ‘maximum’ disk hypothesis, the Toomre . stability parameter is sytematically less than one, which is a strong argu

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Measuring Stellar and Dark Mass Fractions in Spiral Galaxies of spiral galaxies. We perform hydrodynamical simulations of the gas flow in a sequence of potentials with varying the stellar contribution to the total potential. The stellar portion of the potential was derived empirically from K-band photometry. The output of the simulations — namely the gas den

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Contribution to Dark Matter from Extragalactic Duste formation of molecules. Many of the grain properties had to be derived from the extinction of starlight, but it has become possible to map its emission in continuum and spectral lines. New, sensitive instruments even allow to map large extragalactic systems..It was found that cold dust (. ≤ 20K) i

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The Sloan Digital Sky Survey at the Millenniums a smaller area in the south. An array of CCD detectors is used in drift-scan mode to image the sky in five passbands to a limiting magnitude of . ~ 23. Selected from the imaging survey, 10. galaxies, 10. quasars and ~ 10. stars will be observed spectroscopically. To date we have imaged 1700 square

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perjury

Can Dark Matter See Itself?iles. This is in stark contrast with observations of both low- and high-surface brightness galaxies, which indicate that the dark matter has almost constant density in the central parts of halos. Basically there are three possible avenues to a solution to the problem, which we discuss in turn. Obser