Dynamically Hot Galaxies. II. Global Stellar Populations

The global relationship between the stellar populations and structural properties of hot galaxies is studied using the same sample of objects analyzed in Bender, Burstein, and Faber. Two measures of global stellar population are used: the Mg_2_ index at the center of a galaxy and (B - V)_0_ color measured over a much larger volume. The sample of galaxies studied includes luminous ellipticals that span a wide range in luminosity, compact ellipticals, dwarf ellipticals, and the bulges of S0 galaxies. The degree of anisotropy of internal stellar motions is known for most of these objects. The total sample spans a range of over four orders of magnitude in mass and surface brightness, and the various subclasses populate the fundamental plane in very different ways. Despite this, all galaxies follow the same mean relationship between Mg_2_ and velocity dispersion σ_0_. The relative tightness of this relation is impressive: galaxies show a mean scatter of only 0.025 mag in Mg_2_, versus a full range of nearly 0.35 mag in Mg_2_. At least some of the scatter is intrinsic, but the residuals do not correlate with any of the structural properties studied (e.g., velocity anisotropy; effective radius, surface brightness or mass). The residuals also do not show any relation with the positions of the objects within or perpendicular to the fundamental plane. The only properties that do correlate are the morphological and kinematical peculiarities of a handful of disturbed ellipticals, as shown both in this paper and in the study of Schweizer et al. The observed scatter sets an upper limit of 15% on the rms variation of both age and metallicity at fixed σ_0_ for bright ellipticals. The Mg_2_-(B - V)_0_ relation is also examined and found to be tight and consistent for all dynamically hot galaxies. Several S0 galaxies have much bluer global colors compared to central Mg_2_ than do other hot galaxies, but these exceptions are likely due to contamination of the global color by young disk light. The generally tight relation between central Mg_2_ and global (B - V)_0_ means that variations in the internal color and line-strength gradients from galaxy to galaxy must be small. The Mg_2_-σ_0_ relationship can be reformulated as a function of the mass of the galaxy M and the average volume density of baryonic matter ρ as defined by the stars. This new relation can be expressed as Mg_2_ = (M^2^rho)^0.033^. Though ρ is used here to denote average volume density, this relation might also be interpreted as a correlation between the local stellar population and local volume density within each dynamically hot galaxy. This prediction will be tested against observed color and line strength gradients in the next paper of this series.