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Since z~1, the stellar mass density locked in low mass groups and clustershas grown by a factor of ~8. Here we make the first statistical measurements ofthe stellar mass content of low mass X-ray groups at 0.5<z<1, enabling thecalibration of stellar-to-halo mass scales for wide-field optical and infraredsurveys. Groups are selected from combined Chandra and XMM-Newton X-rayobservations in the Chandra Deep Field South (CDFS). These ultra-deepobservations allow us to identify bona fide low mass groups at high redshiftand enable measurements of their total halo masses. We compute aggregatestellar masses for these halos using galaxies from the Carnegie-Spitzer-IMACS(CSI) spectroscopic redshift survey. Stars comprise ~3-4% of the total mass ofgroup halos with masses 10^{12.8}<M200/Msun<10^{13.5} (about the mass of Fornaxand 1/50th the mass of Virgo). Complementing our sample with higher mass halosat these redshifts, we find that the stellar-to-halo mass ratio decreasestoward higher halo masses, consistent with other work in the local and highredshift universe. The observed scatter about the stellar-halo mass relation is~0.25 dex, which is relatively small and suggests that total group stellar masscan serve as a rough proxy for halo mass. We find no evidence for anysignificant evolution in the stellar-halo mass relation since z<1. Quantifyingthe stellar content in groups since this epoch is critical given thathierarchical assembly leads to such halos growing in number density and hostingincreasing shares of quiescent galaxies.

The Stellar Mass - Halo Mass Relation for Low Mass X-ray Groups at 0.5