The power spectrum of the galaxy distribution is accurately measured up to wavelengths over 100h−1 100h−1 Mpc from the CfA 1 and 2 catalogs. We find that our results agree with power spectra calculated by others from smaller samples of optical, radio and infrared galaxies. The power spectrum of an open CDM model (Ωh Ωh = 0.2 and δ8 δ8 = 1; see below for definitions) best approximates the observed power spectrum. The power spectrum of the standard COM model (Ωh Ωh = 0.5 and δ8 δ8 = 1) is inconsistent with the observed one at the 99% confidence level. Our best estimation of the corresponding correlation function in real space is ξ(r)=(r/6.2h−1Mpc)−1.8 ξ(r)=(r/6.2h−1Mpc)−1.8 for r < 20h−1 20h−1 Mpc.