The Dynamics of Poor Systems of Galaxies

Details The Dynamics of Poor Systems of Galaxies The Dynamics of Poor Systems of Galaxies

1999-01-08

arxiv.org/abs/astro-ph/9901095v1

Astrophys.J. 518 (1999) 69

Astronomy and Astrophysics

Astrophysics

36 pages, 20 figures, and 5 tables. To appear in the Astrophysical Journal

Scientific paper

10.1086/307280

We assemble and observe a sample of poor galaxy systems that is suitable for testing N-body simulations of hierarchical clustering (Navarro, Frenk, & White 1997; NFW) and other dynamical halo models (e.g., Hernquist 1990). We (1) determine the parameters of the density profile rho(r) and the velocity dispersion profile sigma(R), (2) separate emission-line galaxies from absorption-line galaxies, examining the model parameters and as a function of spectroscopic type, and (3) for the best-behaved subsample, constrain the velocity anisotropy parameter, beta, which determines the shapes of the galaxy orbits. The NFW universal profile and the Hernquist (1990) model both provide good descriptions of the spatial data. In most cases an isothermal sphere is ruled out. Systems with declining sigma(R) are well-matched by theoretical profiles in which the star-forming galaxies have predominantly radial orbits (beta > 0); many of these galaxies are probably falling in for the first time. There is significant evidence for spatial segregation of the spectroscopic classes regardless of sigma(R).

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