The Star Formation Histories of Red-Sequence Galaxies, Mass-to-Light Ratios and the Fundamental Plane

TL;DR

This study investigates the star formation histories of red-sequence galaxies using spectral lines and mass-to-light ratios, revealing insights into galaxy evolution, the Fundamental Plane, and the role of dark matter and stellar populations.

Contribution

It introduces simple parametric models of star formation history fitted to spectral data, clarifying the impact on mass-to-light ratios and the tilt of the Fundamental Plane.

Findings

Downsizing trend confirmed for giant galaxies

Models with recent star formation are inconsistent with observed mass-to-light ratios

Stellar populations significantly influence the Fundamental Plane tilt

Abstract

This paper addresses the challenge of understanding the typical star formation histories of red sequence galaxies, using linestrength indices and mass-to-light ratios as complementary constraints on their stellar age distribution. We construct simple parametric models of the star formation history that bracket a range of scenarios, and fit these models to the linestrength indices of low-redshift cluster red-sequence galaxies. For giant galaxies, we confirm the downsizing trend. We find, however, that this trend flattens or reverses at sigma < 70 km/s. We then compare predicted stellar mass-to-light ratios with dynamical mass-to-light ratios derived from the Fundamental Plane (FP), or by the SAURON group. For galaxies with sigma ~ 70 km/s, models with a "frosting" of young stars and models with exponential star formation histories have stellar mass-to-light ratios that are larger than observed dynamical mass-to-light ratios by factors of 1.7 and 1.4, respectively, and so are rejected. The SSP model is consistent with the FP, and requires a modest amount of dark matter (20-30%) to account for the difference between stellar and dynamical mass-to-light ratios. A model in which star formation was "quenched" at intermediate ages is also consistent with the observations. We find that the contribution of stellar populations to the "tilt" of the FP is highly dependent on the assumed star-formation history: for the SSP model, the tilt of the FP is driven primarily by stellar-population effects. For a quenched model, two-thirds of the tilt is due to stellar populations and only one third is due to dark matter or non-homology.