  We have used a proper combination of multiband high-resolution {\it
HST-WFPC2} and wide-field ground based observations to image the galactic
globular cluster NGC 6266 (M62). The extensive photometric data set allows us
to determine the center of gravity and to construct the most extended radial
profile ever published for this cluster including, for the first time, detailed
star counts in the very inner region. The star density profile is well
reproduced by a standard King model with an extended core ($\sim 19''$) and a
modest value of the concentration parameter ($c=1.5$), indicating that the
cluster has not-yet experienced core collapse.
  The millisecond pulsar population (whose members are all in binary systems)
and the X-ray emitting population (more than 50 sources within the cluster half
mass radius) suggest that NGC 6266 is in a dynamical phase particularly active
in generating binaries through dynamical encounters. UV observations of the
central region have been used to probe the population of blue straggler stars,
whose origin might be also affected by dynamical interactions. The comparison
with other globular clusters observed with a similar strategy shows that the
blue straggler content in NGC 6266 is relatively low, suggesting that the
formation channel that produces binary systems hosting neutron stars or white
dwarfs is not effective in significantly increasing the blue straggler
population. Moreover, an anticorrelation between millisecond pulsar content and
blue straggler specific frequency in globular cluster seems emerging with
increasing evidence.
