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We combine the globular cluster data for fifteen Brightest Cluster Galaxiesand use this material to trace the mass-metallicity relations (MMR) in theirglobular cluster systems (GCSs). This work extends previous studies whichcorrelate the properties of the MMR with those of the host galaxy. Our combineddata sets show a mean trend for the metal-poor (MP) subpopulation whichcorresponds to a scaling of heavy-element abundance with cluster mass Z ~M^(0.30+/-0.05). No trend is seen for the metal-rich (MR) subpopulation whichhas a scaling relation that is consistent with zero. We also find that thescaling exponent is independent of the GCS specific frequency and host galaxyluminosity, except perhaps for dwarf galaxies.  We present new photometry in (g',i') obtained with Gemini/GMOS for theglobular cluster populations around the southern giant ellipticals NGC 5193 andIC 4329. Both galaxies have rich cluster populations which show up as normal,bimodal sequences in the colour-magnitude diagram.  We test the observed MMRs and argue that they are statistically real, and notan artifact caused by the method we used. We also argue against asymmetriccontamination causing the observed MMR as our mean results are no differentfrom other contamination-free studies. Finally, we compare our method to thestandard bimodal fitting method (KMM or RMIX) and find our results areconsistent.  Interpretation of these results is consistent with recent models for globularcluster formation in which the MMR is determined by GC self-enrichment duringtheir brief formation period.

Further Definition of the Mass-Metallicity Relation in Globular Cluster Systems Around Brightest Cluster Galaxies