Merging of Low-Mass Systems and the Origin of the Fundamental Plane

Abstract

We present a new set of dissipationless N-body simulations to examine the feasibility of creating bright ellipticals (following the Kormendy relation) by hierarchically merging present-day early-type dwarf galaxies, and to study how the encounter parameters affect the location of the end-product in the $<{\mu }_e>-R_e$ plane. We investigate the merging of one-component galaxies of both equal and different masses, the merging of two-component galaxy models to explore the effect of dark halos on the final galaxy characteristics, and the merging of ultracompact dwarf galaxies. We find that the increase of $<{\mu }_e>$ with $R_e$ is attributable to an increase in the initial orbital energy. The merger remnants shift down in the $<{\mu }_e>-R_e$ plane and fail to reach the KR. Thus, the KR is not reproducable by mergers of dwarf early-type systems, rendering untenable the theory that present-day dwarfs are responsible for even a small fraction of the present-day ellipticals, unless a considerable amount of dissipation is invoked. However, we do find that present-day dwarfs can be formed by the merger of ultra-compact dwarfs.

arXiv comment10 pages, 8 figures. Accepted for publication in MNRAS

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