Using a volume-limited sample of 550 groups from the Galaxy And Mass Assembly (GAMA) Galaxy Group Catalogue spanning the halo mass range $12.8 < \log [M_{ h}/M] < 14.2$, we investigate the merging potential of central Brightest Group Galaxies (BGGs). We use spectroscopically-confirmed close-companion galaxies as an indication of the potential stellar mass build-up of low-redshift BGGs, $z \leq 0.2$. We identify 17 close-companion galaxies with projected separations $r_{ p} < 30$ kpc, relative velocities $\Delta v \leq 300$ km s$^{ -1}$, and stellar-mass ratios $M_{ BGG}/M_{ CC} \leq 4$ relative to the BGG. These close-companion galaxies yield a total pair fraction of $0.03 \pm 0.01$. Overall, we find that BGGs in our sample have the potential to grow in stellar mass due to mergers by $2.2 \pm 1.5\%$ Gyr$^{ -1}$. This is lower than the stellar mass growth predicted by current galaxy evolution models.
Categories: astro-ph.GA