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

In order to explore local large-scale structures and velocity fields, accurate galaxy distance measures are needed. We now extend the well-tested recipe for calibrating the correlation between galaxy rotation rates and luminosities -- capable of providing such distance measures -- to the all-sky, space-based imaging data from the Wide-field Infrared Survey Explorer (WISE) W1 ($3.4mu$m) and W2 ($4.6mu$m) filters. We find a linewidth to absolute magnitude correlation (known as the Tully-Fisher Relation, TFR) of $mathcal{M}^{b,i,k,a}_{W1} = -20.35 - 9.56 (log W^i_{mx} - 2.5)$ (0.54 magnitudes 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 the I-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 magnitudes rms). The WISE TFRs show evidence of curvature. Quadratic fits give $mathcal{M}^{b,i,k,a}_{W1} = -20.48 - 8.36 (log W^i_{mx} - 2.5) + 3.60 (log W^i_{mx} - 2.5)^2$ (0.52 magnitudes rms) and $mathcal{M}^{b,i,k,a}_{W2} = -19.91 - 8.40 (log W^i_{mx} - 2.5) + 4.32 (log W^i_{mx} - 2.5)^2$ (0.55 magnitudes rms). We apply an I-band -- WISE color correction to lower the scatter 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 0.46 magnitudes rms). Using our three independent TFRs (W1 curved, W2 curved and I-band), we calibrate the UNION2 supernova Type Ia sample distance scale and derive $H_0 = 74.4 pm 1.4$(stat) $pm 2.4$(sys) kms$^{-1}$ Mpc$^{-1}$ with 4% total error.