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In clusters of galaxies, the red sequence is believed to be a consequence ofa correlation between stellar mass and chemical abundances, with more massivegalaxies being more metal-rich and, as a consequence, redder. However, there isa color scatter around the red sequence that holds even with precisionphotometry, implying that the galaxy population is more complicated than asdescribed by a mass-metallicity relation. We use precision photometry from theCluster Lensing and Supernova survey with Hubble (CLASH) to investigate whatdrives this scatter. In four CLASH clusters at $z=0.355 \pm 0.007$, we findthat the optical-IR galaxy colors confirm the previously known trend ofmetallicity along the red sequence but also show a strong connection betweenstellar age and red sequence offset, with ages ranging from 3 to 8 Gyr.Starting with fixed-age color-magnitude relations motivated by themass-metallicity correlations of CLASH cluster galaxies, and by adjustinggalaxy colors through stellar population models to put them all at the age ofour red sequence, we are able to reduce the, e.g., F625W $-$ F814W scatter from0.051 mag to 0.026 mag with median photometric errors of 0.029 mag. While wewill extend this analysis to the full CLASH sample, in four clusters ourtechnique already provides a color precision in near-total-light apertures toresolve the spread in stellar population formation ages that drives the scatterin the red sequence.

On the Origin of the Scatter in the Red Sequence: An Analysis of Four CLASH Clusters