  We report on the results of an I-band time-series photometric survey of NGC
2547 using the MPG/ESO 2.2m telescope with WFI, achieving better than 1%
photometric precision per data point over 14 <~ I <~ 18. Candidate cluster
members were selected from a V vs V-I colour magnitude diagram over 12.5 < V <
24 (covering masses from 0.9 Msol down to below the brown dwarf limit), finding
800 candidates, of which we expect ~330 to be real cluster members, taking into
account contamination from the field (which is most severe at the extremes of
our mass range). Searching for periodic variations in these gave 176 detections
over the mass range 0.1 <~ M/Msol <~ 0.9. The rotation period distributions
were found to show a clear mass-dependent morphology, qualitatively
intermediate between the distributions obtained from similar surveys in NGC
2362 and NGC 2516, as would be expected from the age of this cluster. Models of
the rotational evolution were investigated, finding that the evolution from NGC
2362 to NGC 2547 was qualitatively reproduced (given the uncertainty in the age
of NGC 2547) by solid body and core-envelope decoupled models from our earlier
NGC 2516 study without need for significant modification.
