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In order to explore local large-scale structures and velocity fields,accurate galaxy distance measures are needed. We now extend the well-testedrecipe for calibrating the correlation between galaxy rotation rates andluminosities -- capable of providing such distance measures -- to the all-sky,space-based imaging data from the Wide-field Infrared Survey Explorer (WISE) W1($3.4\mu$m) and W2 ($4.6\mu$m) filters. We find a linewidth to absolutemagnitude correlation (known as the Tully-Fisher Relation, TFR) of$\mathcal{M}^{b,i,k,a}_{W1} = -20.35 - 9.56 (\log W^i_{mx} - 2.5)$ (0.54magnitudes rms) and $\mathcal{M}^{b,i,k,a}_{W2} = -19.76 - 9.74 (\log W^i_{mx}- 2.5)$ (0.56 magnitudes rms) from 310 galaxies in 13 clusters. We update theI-band TFR using a sample 9% larger than in Tully & Courtois (2012). We derive$\mathcal{M}^{b,i,k}_I = -21.34 - 8.95 (\log W^i_{mx} - 2.5)$ (0.46 magnitudesrms). The WISE TFRs show evidence of curvature. Quadratic fits give$\mathcal{M}^{b,i,k,a}_{W1} = -20.48 - 8.36 (\log W^i_{mx} - 2.5) + 3.60 (\logW^i_{mx} - 2.5)^2$ (0.52 magnitudes rms) and $\mathcal{M}^{b,i,k,a}_{W2} =-19.91 - 8.40 (\log W^i_{mx} - 2.5) + 4.32 (\log W^i_{mx} - 2.5)^2$ (0.55magnitudes rms). We apply an I-band -- WISE color correction to lower thescatter and derive $\mathcal{M}_{C_{W1}} = -20.22 - 9.12 (\log W^i_{mx} - 2.5)$and $\mathcal{M}_{C_{W2}} = -19.63 - 9.11 (\log W^i_{mx} - 2.5)$ (both 0.46magnitudes rms). Using our three independent TFRs (W1 curved, W2 curved andI-band), we calibrate the UNION2 supernova Type Ia sample distance scale andderive $H_0 = 74.4 \pm 1.4$(stat) $\pm\ 2.4$(sys) kms$^{-1}$ Mpc$^{-1}$ with 4%total error.

The Calibration of the WISE W1 and W2 Tully-Fisher Relation