  The current enthusiam to measure fluctuations in the CMB power spectrum at
angular scales between 0.1 and 1 degree is largely motivated by the expectation
that CMB determinations of cosmological parameters will be of unprecedented
precision. In such circumstances it is important to estimate what we can
already say about the cosmological parameters. In two recent papers (Lineweaver
etal 1997a & 1997b) we have compiled the most recent CMB measurements, used a
fast Boltzmann code to calculate model power spectra (Seljak & Zaldarriaga
1996) and, with a chi-squared analysis, we have compared the data to the power
spectra from several large regions of parameter space. In the context of the
flat models tested we obtain the following constraints on cosmological
parameters: $Ho = 30^{+13}_{-9}$, $n=0.93^{+0.17}_{-0.16}$ and
$Q=17.5^{+3.5}_{-2.5}$ uK. The n and Q values are consistent with previous
estimates while the Ho result is surprisingly low.
