Massive galaxy clusters undergo strong evolution from z \sim 1.6 to z \sim 0.5 , with overdense environments at high- z characterized by abundant dust-obscured star formation and stellar mass growth which rapidly give way to widespread quenching .
Data spanning the near- to far- infrared ( IR ) spectrum can directly trace this transformation ; however , such studies have largely been limited to the massive galaxy end of cluster populations .
In this work , we present ‘ ‘ total light '' stacking techniques spanning 3.4 - 500 \mu m aimed at revealing the total cluster infrared emission , including low mass members and any potential intracluster dust .
We detail our procedures for WISE , Spitzer , and Herschel imaging , including corrections to recover the total stacked emission in the case of high fractions of detected galaxies .
We apply our stacking techniques to 232 well-studied massive ( log M _ { 200 } / M _ { \odot } \sim 13.8 ) clusters across multiple redshift bins , recovering extended cluster emission at all wavelengths , typically at > 5 \sigma .
We measure the averaged near- to far-IR radial profiles and spectral energy distributions ( SEDs ) , quantifying the total stellar and dust content .
The near-IR radial profiles are well described by an NFW model with a high ( c \sim 7 ) concentration parameter .
Dust emission is similarly concentrated , albeit suppressed at small radii ( r < 0.2 Mpc ) .
The measured SEDs lack warm dust , consistent with the colder SEDs expected for low mass galaxies .
We derive total stellar masses consistent with the theoretical M _ { halo } - M _ { \star } relation and specific-star formation rates that evolve strongly with redshift , echoing that of massive ( log M _ { \star } / M _ { \odot } \gtrsim 10 ) cluster galaxies .
Separating out the massive galaxy population reveals that the majority of cluster far-IR emission ( \sim 70 - 80 \% ) is provided by the low mass constituents , which differs from field galaxies .
This effect may be a combination of mass-dependent quenching and excess dust in low mass cluster galaxies .