  We study the globular clusters M3 and Palomar 3 as a "second parameter (2ndP)
pair," showing that:
  i) M3 has a surprisingly strong *internal* 2ndP;
  ii) The dispersion in mass on the Pal 3 horizontal branch (HB) is
intrinsically very small, leading to the most apparent differences in HB
morphology between M3 and Pal 3;
  iii) Ignoring the difference in HB mass dispersion between M3 and Pal 3,
their relative HB types can be accounted for by a fairly small difference in
age, of order 0.5-1 Gyr.
