We present 0.55 × 106-particle simulations of the accretion of high-density dwarf galaxies by low-density giant galaxies, using models that contain both power-law central density cusps and point masses representing supermassive black holes. The cusp of the dwarf galaxy is disrupted during the merger, producing a remnant with a central density that is only slightly higher than that of the giant galaxy initially. Removing the black hole from the giant galaxy allows the dwarf galaxy to remain intact and leads to a remnant with a high central density, contrary to what is observed. Our results support the hypothesis that the persistence of low-density cores in giant galaxies is a consequence of supermassive black holes (Refer to PDF file for exact formulas).

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Also archived in: arXiv:astro-ph/0101194 v2 12 Mar 2001 AND Rutgers Astrophysics Preprint Series No. 299 The work described here was supported by NSF grants AST 96-17088 and 00-71099, NASA grants NAG5-6037 and NAG5-9046, and by a fellowship from the Consejo Nacional de Ciencia y Tecnologia de Mexico. This work was partially supported by the National Computational Science Alliance under grant no. MCA00N010N. Note: imported from RIT’s Digital Media Library running on DSpace to RIT Scholar Works in February 2014.

Document Type


Department, Program, or Center

School of Physics and Astronomy (COS)


RIT – Main Campus