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We describe a program of surface brightness fluctuation (SBF) measurementsfor determining galaxy distances. This paper presents the photometriccalibration of our sample and of SBF in general. Basing our zero point onobservations of Cepheid variable stars, we find that the absolute SBF magnitudein the Kron-Cousins I band correlates well with the mean (V-I)o color of agalaxy according to  M_Ibar = (-1.74 +/- 0.07) + (4.5 +/- 0.25) [ (V-I)o - 1.15 ]  for 1.0 < (V-I) < 1.3. This agrees well with theoretical estimates fromstellar population models. Comparisons between SBF distances and a variety ofother estimators, including Cepheid variable stars, the Planetary NebulaLuminosity Function (PNLF), Tully-Fisher (TF), Dn-sigma, SNII, and SNIa,demonstrate that the calibration of SBF is universally valid and that SBF errorestimates are accurate. The zero point given by Cepheids, PNLF, TF (bothcalibrated using Cepheids), and SNII is in units of Mpc; the zero point givenby TF (referenced to a distant frame), Dn-sigma and SNIa is in terms of aHubble expansion velocity expressed in km/s. Tying together these two zeropoints yields a Hubble constant of H_0 = 81 +/- 6 km/s/Mpc. As part of thisanalysis, we present SBF distances to 12 nearby groups of galaxies whereCepheids, SNII, and SNIa have been observed.Comment: 29 pages plus 8 figures; LaTeX (AASTeX) uses aaspp4.sty (included);  To appear in The Astrophysical Journal, 1997 February 1 issue; Compressed  PostScript available from ftp://mars.tuc.noao.edu/sbf

The SBF Survey of Galaxy Distances. I. Sample Selection, Photometric Calibration, and the Hubble Constant