Titlebook: Dark Matter in Astro- and Particle Physics; Proceedings of the I H. V. Klapdor-Kleingrothaus,R. D. Viollier Conference proceedings 2002 Spr

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Androgen

The Dark Mass at the Center of the Milky Waybital accelerations for some of the most central stars of our Galaxy confirming the results obtained by Ghez et al. (2000) with NIRC at the Keck telescope. A detailed analysis combining the high precision but shorter time scale NIRC/Keck data with the lower precision but longer time scale SHARP/NTT

心痛

Dim Matter in the Disks of Low Surface Brightness Galaxiestions due to the various components of the galaxies. For this purposegalaxies are selected which show clear spiral structure. Arguments of density wave theory of galactic spiral arms are then used to estimate the masses of the galactic disks. These estimates seem to indicate that the disks of low su

detach

Black Holes in Active Galactic Nucleithe galaxian matter from its vicinity. The release of the gravitational energy of the infalling matter is ultimately responsible for the large radiative output of those objects, and in some cases, for formation and acceleration of powerful relativistic jets. This paper outlines our current understan

harmony

contrast-medium

contrast-medium

Baryonic Dark Matter and Machosr halo consisting of baryons in the form of Machos is ruled out, leaving an elementary particle as the prime candidate for the dark matter. The observed microlensing events may make up around 20% of the dark matter in the Milky Way, or may indicate an otherwise undetected component of the Large Mage

狂怒

白楊

icipants gave very nice professional talks during the conference. We are grateful to John Ellis for doing an incredible job preparing his excellent summary talk during the sessions. Some specia978-3-642-62920-4978-3-642-55739-2

overhaul

The Dark Mass at the Center of the Milky Wayly inclined (60° < . < 80°), and eccentric (0.4 < . < 0.95) orbits around a central dark mass. The combination of both data sets results in a position of this central mass of .. E and .. S of the nominal radio position of Sgr A.. In particular it is possible to statistically correct the observed acc