Abstract
We present scaling relations between the virial velocity (V) and the one-dimensional central velocity dispersion (σ0); the gravitational radius (Rv) and the effective radius (Re); and the total mass (M) and the luminous mass (ML) found in N-body simulations of binary mergers of spiral galaxies. These scalings are of the form V2 ∝ σ0α, Rv ∝ Reβ and M∝ MLγ. The particlar values obtained for {α,β,γ} depend on the method of fitting used [ordinary least-squares (OLS) or orthogonal distance regression (ODR)], the assumed profile [de Vaucouleurs (deV) or Sérsic (S)], and the size of the radial interval where the fit is done. The α and γ indexes turn out more sensitive to the fitting procedure, resulting for the OLS in a mean < α >ols = 1.51% and < γ >ols= 0.69, while for the ODR < α >odr=2.35 and < γ >odr=0.76. The β index depends more on the adopted type of profile, with < β >deV=0.13 and < β >S=0.27. We conclude that dissipationless formed remnants of mergers have a strong breaking of structural and kinematical homology.
