On Mass Concentrations & Magnitude Gaps of Galaxy Systems in the CS82
  Survey
  Galaxy systems with large magnitude gaps - defined as the difference in
magnitude between the central galaxy and the brightest satellite in the central
region - have been claimed to have earlier formation histories. In this study
we measure the mass concentration, as an indicator of early formation, of
ensembles of galaxy systems divided by redshift and magnitude gaps in the $r$
band. We use cross-correlation weak lensing measurements with NFW parametric
mass profiles to measure masses and concentrations of these ensembles from a
catalogue of systems built from the SDSS Coadd by the redMaPPer algorithm. The
lensing shear data come from the CFHT Stripe 82 (CS82) survey, and consists of
$i$-band images of the SDSS Stripe 82 region. We find that the stack made up of
systems with larger magnitude gaps has a high probability of being more
concentrated on average, in the lowest redshift slice ($0.2<z<0.4$), both when
dividing in quartiles ($P=0.98$) and terciles ($P=0.85$). These results lend
credibility to the claim that the magnitude gap is an indicator of earlier
formed systems.
