  The interpretation that bimodal colour distributions of globular clusters
(GCs) reflect bimodal metallicity distributions has been challenged.
Non-linearities in the colour to metallicity conversions caused by the
horizontal branch (HB) stars may be responsible for transforming a unimodal
metallicity distribution into a bimodal (optical) colour distribution. We study
optical/near-infrared (NIR) colour distributions of the GC systems in 14 E/S0
galaxies. We test whether the bimodal feature, generally present in optical
colour distributions, remains in the optical/NIR ones. The latter colour
combination is a better metallicity proxy than the former. We use KMM and GMM
tests to quantify the probability that different colour distributions are
better described by a bimodal, as opposed to a unimodal distribution. We find
that double-peaked colour distributions are more commonly seen in optical than
in optical/NIR colours. For some of the galaxies where the optical (g-z)
distribution is clearly bimodal, the (g-K) and (z-K) distributions are better
described by a unimodal distribution. The two most cluster-rich galaxies in our
sample, NGC4486 and NGC4649, show some interesting differences. The (g-K)
distribution of NGC4649 is better described by a bimodal distribution, while
this is true for the (g-K) distribution of NGC4486 GCs only if restricted to a
brighter sub-sample with small K-band errors (< 0.05 mag). Formally, the K-band
photometric errors cannot be responsible for blurring bimodal metallicity
distributions to unimodal (g-K) colour distributions. However, simulations
including the extra scatter in the colour-colour diagrams (not fully accounted
for in the photometric errors) show that such scatter may contribute to the
disappearance of bimodality in (g-K) for the full NGC4486 sample. For the less
cluster-rich galaxies results are inconclusive due to poorer statistics.
[Abridged]
