  Fluctuations in the CMB have now been detected over a wide range of angular
scales, and a consistent picture seems to be emerging. The data cannot
currently constrain a large number of cosmological parameters, but it is clear
that there is more information than just the normalization of the models. Here
we use the data to constrain a second parameter, namely the amplitude of the
Doppler peak, using a phenomenological approach to the power spectrum. We find
that the data prefer a peak of height ~3, with a purely flat spectrum ruled out
at the 95%CL. Although there are concerns about possible foregrounds and
non-Gaussian fluctuations, we believe that the existence of a peak at
degree-scales is established by the data. This immediately implies that
reionization was unimportant for the CMB. It also potentially leads to
difficulties for models where the fluctuations were produced by topological
defects. Independent constraints on Omega_B, on the slope n, etc. will need to
wait for further data. At the moment, the simple presence of a Doppler peak
should be seen as strong supporting evidence for standard dark matter-dominated
models with some few percent of baryons at z=1000.
