The growth of brightest cluster galaxies and intracluster light over the past 10 billion years.

We constrain the evolution of the brightest cluster galaxy plus intracluster light (BCG + ICL) using an ensemble of 42 galaxy groups and clusters that span redshifts of z  = 0.05−1.75 and masses of M_{500, c} = 2 × 10¹³−10¹⁵ M_⊙. Specifically, we measure the relationship between the BCG + ICL stellar mass M_⋆ and M_{500, c} at projected radii 10 < r < 100 kpc for three different epochs. At intermediate redshift (⁠|$\bar{z}=0.40$|⁠), where we have the best data, we find M_⋆ ∝ M_{500, c} ^{0.48 ± 0.06}. Fixing the exponent of this power law for all redshifts, we constrain the normalization of this relation to be 2.08 ± 0.21 times higher at |$\bar{z}=0.40$| than at high redshift (⁠|$\bar{z}=1.55$|⁠). We find no change in the relation from intermediate to low redshift (⁠|$\bar{z}=0.10$|⁠). In other words, for fixed M_{500, c} , M_⋆ at 10 < r < 100 kpc increases from |$\bar{z}=1.55$| to |$\bar{z}=0.40$| and not significantly thereafter. Theoretical models predict that the physical mass growth of the cluster from z  = 1.5 to z  = 0 within r_{500, c} is 1.4×, excluding evolution due to definition of r_{500, c} . We find that M_⋆ within the central 100 kpc increases by ∼3.8× over the same period. Thus, the growth of M_⋆ in this central region is more than a factor of 2 greater than the physical mass growth of the cluster as a whole. Furthermore, the concentration of the BCG + ICL stellar mass, defined by the ratio of stellar mass within 10 kpc to the total stellar mass within 100 kpc, decreases with increasing M_{500, c} at all z. We interpret this result as evidence for inside–out growth of the BCG + ICL over the past 10 Gyr, with stellar mass assembly occurring at larger radii at later times. [ABSTRACT FROM AUTHOR]