The power spectrum of the galaxy distribution is accurately measured up to wavelengths over $100;h^{-1}$ 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 (${Omega}h$ = 0.2 and ${delta}_8$ = 1; see below for definitions) best approximates the observed power spectrum. The power spectrum of the standard COM model (${Omega}h$ = 0.5 and ${delta}_8$ = 1) is inconsistent with the observed one at the 99% confidence level. Our best estimation of the corresponding correlation function in real space is ${xi}(r);=;(r/6.2h^{-1}Mpc)^{-1.8}$ for r < $20h^{-1}$ Mpc.