CMB mapping experiments: a designer's guide

We apply state-of-the art data analysis methods to a number of ficticious 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 strategy is thoroughly interconnected. (4)If each pixel is scanned through in fairly perpendicular directions, the noise correlations in the resulting map reveal no stripiness, but are quite isotropic. (5) 1/f-noise produces a $1/\l$ contribution to the angular power spectrum for single-beam scanning, as compared to virtually white noise for a two-beam scan pattern such as that of the MAP satellite.