Tully-Fisher and Dn-sigma distances, radial velocities, and associated catalog and observational data for the spiral, irregular, and elliptical galaxies that comprise the Mark 3 catalog are given in 5 different kinds of tables for seven separate data sets. Users interested only in the resulting distances need use only the files listed in sections 3 (Grouped spiral distance files), 4 (Elliptical galaxy distance files), and 5 (Comparison of galaxy distances). Introduction: The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; 1982ApJ...258...64A): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; 1982ApJ...258...64A): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; 1982ApJ...258...64A): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match Disclaimer Note: IMPORTANT NOTE/DISCLAIMER In all cases, the Basic data files try to give the data as either published or otherwise given to us by the original author(s). In contrast, the Spiral Galaxy distance files contain data as homogenized by the authors' methodology. In many cases, value of radial velocity may differ by up to 50 km/sec (in the case of Local Group velocities), owing to both round-off errors in our computer programs and to differences in how to transform from one velocity reference frame to another. Similar, values of eta may differ in the last decimal place by up to 0.004. Only if much larger differences are found do the originators of these files wish the user to contact them. As errors are inevitable in a compendium of this size, notice of large errors found is much appreciated.