  We present high-quality, Keck spectroscopic data for a sample of 20 globular
clusters (GCs) in the massive E0 galaxy NGC1407. A subset of twenty
line-strength indices of the Lick/IDS system have been measured for both the GC
system and the central integrated star-light of the galaxy. Ages, metallicities
and [alpha/Fe] ratios have been derived using several different approaches. The
majority GCs in NGC1407 studied are old, follow a tight metallicity sequence
reaching values slightly above solar, and exhibit mean [alpha/Fe] ratios of ~
0.3 dex. In addition, three GCs are formally derived to be young (~ 4 Gyr), but
we argue that they are actually old GCs hosting blue horizontal branches. We
report, for the first time, evidence for the existence of two
chemically-distinct subpopulations of metal-rich (MR) GCs. We find some MR GCs
exhibit significantly larger [Mg/Fe] and [C/Fe] ratios. Different star
formation time-scales are proposed to explain the correlation between Mg and C
abundances. We also find striking CN overabundances over the entire GC
metallicity range. Interestingly, the behavior of C and N in metal-poor (MP)
GCs clearly deviates from the one in MR GCs. In particular, for MR GCs, N
increases dramatically while C essentially saturates. This may be interpreted
as a consequence of the increasing importance of the CNO cycle with increasing
metallicity.
