Transform analysis of the high-resolution Shane-Wirtanen catalog: The power spectrum and the bispectrum

To extract more statistical information from the high resolution (10') Shane-Wirtanen data, and in particular to gain information about the large-scale behavior of galaxy clustering, we have examined the two- and three-point galaxy correlation functions in Fourier transform space for wavelengths corresponding to 1/2 0< or approx. =theta< or approx. =700 (2 Mpc< or approx. =hr< or approx. =260 Mpc, h = Hubble's constant in units of 100 km s-1 Mpc-1). To the extent that our results can be compared to earlier works, we obtain rough agreement, but we are able to identify some systematic differences also. There is no evidence for any transition in behavior of the power spectrum corresponding to the break in the two-point function at 2.05 (9 h-1 Mpc), but this characteristic scale does appear in the bispectrum. The small k (large angle) behavior of the power spectrum is as k/sup n/, with nroughly-equal-1