stellar mass growth of the intracluster light between $z=0.3$ and $z=0$.'
author:
- |
    Danièl N. Groenewald$^{1,2}$[^1], Rosalind E. Skelton$^{1}$, David G. Gilbank$^1$ and S. Ilani Loubser$^2$\
    $^{1}$South African Astronomical Observatory, Observatory Road, 7925, Cape Town, South Africa\
    $^{2}$North-West University, Potchefstroom, 2520, South Africa
bibliography:
- 'ms.bib'
date: 'Accepted XXX. Received YYY; in original form ZZZ'
title: 'The close pair fraction of BCGs since $z=0.5$: major mergers dominate recent BCG stellar mass growth'
---

\[firstpage\]

galaxies: clusters: general – galaxies: clusters: intracluster medium – galaxies: elliptical and lenticular, cD – galaxies: evolution – galaxies: interactions.

Introduction {#sec:intro}
============

Brightest cluster galaxies (BCGs) are the most massive and luminous galaxies in the Universe. These galaxies are typically found close to, or at, the centres of their host clusters [@Jones1984; @Jones1999; @Beers1986; @Rhee1991]. In the hierarchical formation scenario BCGs are thought to form through the accretion of smaller galaxies [e.g. @Ostriker1977; @Richstone1983]. These massive galaxies are also known to have properties that are very different from that of other early-type galaxies (ETGs). In comparison to other ETGs of the same mass, BCGs are found to be larger [@Bernardi2007 and references therein] and have extended light profiles [@Matthews1964; @Tonry1987; @Schombert1988; @Gonzalez2000; @Gonzalez2003]. These 