  We apply state-of-the art data analysis methods to a number of fictitious CMB
mapping experiments, including 1/f noise, distilling the cosmological
information from time-ordered data to maps to power spectrum estimates, and
find that in all cases, the resulting error bars can we well approximated by
simple and intuitive analytic expressions. Using these approximations, we
discuss how to maximize the scientific return of CMB mapping experiments given
the practical constraints at hand, and our main conclusions are as follows.
  (1) For a given resolution and sensitivity, it is best to cover a sky area
such that the signal-to-noise ratio per resolution element (pixel) is of order
unity.
  (2) It is best to avoid excessively skinny observing regions, narrower than a
few degrees.
  (3) The minimum-variance mapmaking method can reduce the effects of 1/f noise
by a substantial factor, but only if the scan pattern is thoroughly
interconnected.
  (4) 1/f noise produces a 1/l contribution to the angular power spectrum for
well connected single-beam scanning, as compared to virtually white noise for a
two-beam scan pattern such as that of the MAP satellite.
