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The Teerikorpi incompleteness bias in the distance modulus of a galaxycluster that is determined from incomplete data using the Tully-Fisher (TF)method is discussed differently than has been done in earlier papers of thisseries. A toy cluster is made with zero intrinsic TF dispersion but with slopesthat differ between the calibrators and the cluster data, showing the biascaused by incorrect slopes. Intrinsic dispersion is added to the model and twostrategies are used to analyze the data; first by binning the data by linewidth and then by apparent magnitude (the direct method), and second by binningby magnitude and then summing over all line widths (the inverse method). Toillustrate these strategies, a composite cluster is made by combining theobservations of Virgo A and B subclusters with those for the Ursa Major I andII clusters, corrected to the Virgo A distance. The cluster data are calibratedusing Cepheid distances to 25 galaxies that have adequate TF properties.Different moduli calculated with varying completeness limits are displayed. Thecluster modulus derived from the complete cluster sample gives (m-M) = 31.42+/- 0.2 (external) for Virgo A, 31.80 +/- 0.16 for Virgo B, 31.26 +/- 0.13 forUMa I, and 31.58 +/- 0.17 for UMa II. Combining the Virgo A distance (D = 19.2Mpc that has a range from 17.5 to 21.1 Mpc with its expansion velocity of 1175+/- 50 km/s as tied to the remote kinematic frame gives a Hubble constant of61km/s/Mpc with a range from 53 to 70.

Bias Properties of Extragalactic Distance Indicators XII: Bias Effects  of Slope Differences and Intrinsic Dispersion on Tully-Fisher Distances to  Galaxy Clusters with Application to the Virgo Cluster