Scalings between physical and their observationally related quantities of merger remnants

We present scaling relations between the virial velocity (V) and the one-dimensional central velocity dispersion (sigma(0)); the gravitational radius (R-v) and the effective radius (R-e); and the total mass (M) and the luminous mass (M-L) found in N-body simulations of binary mergers of spiral galaxies. These scalings are of the form V-2 proportional to sigma(alpha)(0), R-v proportional to R-e(beta) and M proportional to M-L(gamma). The particlar values obtained for {alpha, beta, gamma} depend on the method of fitting used [ordinary least-squares (OLS) or orthogonal distance regression (ODR)], the assumed profile [de Vaucouleurs (deV) or Sersic (S)], and the size of the radial interval where the fit is done. The alpha and gamma indexes turn out more sensitive to the fitting procedure, resulting for the OLS in a mean <alpha >(ols) = 1.51 and <gamma >(ols) = 0.69, whiletfor the ODR <alpha >(odr) = 2.35 and <gamma >(odr) = 0.76. The beta index depends more on the adopted type of profile, with <beta >(deV) = 0.13 and <beta >(s) = 0.27. We conclude that dissipationless formed remnants of mergers have a strong breaking of structural and kinematical homology.