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 ( \mbox { [ Z / H ] } \la - 1.1 ) , except for the GCs Hubble V in NGC 205 ( T = 1.2 \pm 0.6 Gyr , \mbox { [ Z / H ] } = -0.6 \pm 0.2 ) , Hubble VI in NGC 205 ( T = 4 \pm 2 Gyr , \mbox { [ Z / H ] } = -0.8 \pm 0.2 ) , and FJJVII in NGC 185 ( T = 7 \pm 3 Gyr , \mbox { [ Z / H ] } = -0.8 \pm 0.2 ) .
The majority of our GC sample has solar [ \alpha /Fe ] enhancement 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 .