  We present measurements of ages, metallicities, and [alpha/Fe] ratios for 16
globular clusters (GC) in NGC 147, NGC 185, and NGC 205 and of the central
regions of the diffuse galaxy light in NGC 185, and NGC 205. Our results are
based on spectra obtained with the SCORPIO multi-slit spectrograph at the 6-m
telescope of the Russian Academy of Sciences. We include in our analysis
high-quality HST/WFPC2 photometry of individual stars in the studied GCs to
investigate the influence of their horizontal branch (HB) morphology on the
spectroscopic analysis. All our sample GCs appear to be old (T>8 Gyr) and
metal-poor ([Z/H] <~ -1.1), except for the globular clusters Hubble V in NGC
205 (T=1.2+/-0.6 Gyr, [Z/H]=-0.6+/-0.2), Hubble VI in NGC 205 (T=4+/-2 Gyr,
[Z/H]=-0.8+/-0.2), and FJJVII in NGC 185 (T=7+/-3 Gyr, [Z/H]=-0.8+/-0.2). The
majority of our GC sample has solar [alpha/Fe] enhancements in contrast to the
halo population of GCs in M31 and the Milky Way. The HB morphologies for our
sample GCs follow the same behavior with metallicity as younger halo Galactic
globular clusters. We show that it is unlikely that they bias our spectroscopic
age estimates based on Balmer absorption line indices. Spectroscopic ages and
metallicities of the central regions in NGC 205 and NGC 185 coincide with those
obtained from color-magnitude diagrams. The central field stellar populations
in these galaxies have approximately the same age as their most central GCs
(Hubble V in NGC 205 and FJJIII in NGC 185), but are more metal-rich than the
central globular clusters.
