Context : Globular clusters are representative of the oldest stellar populations .
It is thus essential to have a complete census of these systems in dwarf galaxies , from which more massive galaxies are progressively formed in the hierarchical scenario .

Aims : We present the results of spectroscopic observations of eight globular cluster candidates in NGC 147 , a satellite dwarf elliptical galaxy of M31 .
Our goal is to make a complete inventory of the globular cluster system of this galaxy , determine the properties of their stellar populations , and compare these properties with those of systems of globular clusters in other dwarf galaxies .

Methods : The candidates were identified on Canada-France-Hawaii telescope photographic plates .
Medium resolution spectra were obtained with the SCORPIO spectrograph at the prime focus of the 6m telescope of the Russian Academy of Sciences .
They were analyzed using predictions of stellar population synthesis models .

Results : We were able to confirm the nature of all eight candidates , three of which ( GC5 , GC7 , and GC10 ) are indeed globular clusters , and to estimate evolutionary parameters for the two brightest ones and for Hodge II .
The bright clusters GC5 and GC7 appear to have metallicities ( [ Z/H ] \sim - 1.5 \div - 1.8 ) that are lower than the oldest stars in the galaxy .
The fainter GC Hodge II has a metallicity [ Z/H ] = -1.1 , similar to that of the oldest stars in the galaxy .
The clusters GC5 and GC7 have low alpha-element abundance ratios .
The mean age of the globular clusters in NGC 147 is 9 \pm 1 Gyr .
We also measured the radial velocities of Hodge II and IV , and derived a mass of NGC 147 in good agreement with the value from the literature .
The frequency , S _ { n } = 6.4 , and mass fraction , T = 14 of globular clusters in NGC 147 appear to be higher than those for NGC 185 and 205 .

Conclusions : Our results indicate that the bright clusters GC5 , GC7 , and Hodge III formed in the main star-forming period \sim 8-10 Gyr ago , while the fainter clusters Hodge I and II formed together with the second generation of field stars .