Characterizing Intra-cluster light in the Hubble Frontier Fields
  We investigate the intra-cluster light (ICL) in the 6 Hubble Frontier Field
clusters at $0.3<z<0.6$. We employ a new method, which is free from any
functional form of the ICL profile, and exploit the unprecedented depth of this
Hubble Space Telescope imaging to map the ICL's diffuse light out to
clustrocentric radii $R\sim300$kpc ($\mu_{\rm ICL}\sim27$mag arcsec$^{-2}$).
From these maps, we construct radial color and stellar mass profiles via SED
fitting and find clear negative color gradients in all systems with increasing
distance from the Brightest Cluster Galaxy (BCG). While this implies older/more
metal rich stellar components in the inner part of the ICL, we find the ICL
mostly consists of a $<2$Gyr population, and plausibly originated with $\log
M_*/M_\odot<10$ cluster galaxies. Further, we find 10-15% of the ICL's mass at
large radii ($>150$kpc) lies in a younger/bluer stellar population
($\sim1$Gyr), a phenomenon not seen in local samples. We attribute this light
to the higher fraction of starforming/(post-)starburst galaxies in clusters at
$z\sim0.5$. Ultimately, we find the ICL's total mass to be $\log M_{\rm *}^{\rm
ICL}/M_\odot\sim11$-12, constituting 5%-20% of the clusters' total stellar
mass, or about a half of the value at $z\sim0$. The above implies distinct
formation histories for the ICL and BCGs/other massive cluster galaxies; i.e.
the ICL at this epoch is still being constructed rapidly
($\sim40M_\odot$yr$^{-1}$), while the BCGs have mostly completed their
evolution. To be consistent with the ICL measurements of local massive
clusters, such as the Virgo, our data suggest mass acquisition mainly from
quiescent cluster galaxies is the principal source of ICL material in the
subsequent $\sim$5 Gyr of cosmic time.
