SIMBAD references

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 (3.4 µm) and W2 (4.6 µm) filters. We find a correlation of line width to absolute magnitude (known as the Tully-Fisher relation, TFR) of M_W1^b,i,k,a = -20.35 - 9.56(logW_mxⁱ - 2.5) (0.54 mag rms) andi M_W2^b,i,k,a = -19.76 - 9.74(log W_mxⁱ - 2.5) (0.56 mag rms) from 310 galaxies in 13 clusters. We update the I-band TFR using a sample 9% larger than in Tully & Courtois. We derive M_l^b,i,k = -21.34 - 8.95(logW_mxⁱ -2.5) (0.46 mag rms). The WISE TFRs show evidence of curvature. Quadratic fits give M_W1^b,i,k,a = -20.48 - 8.36(logW_mxⁱ -2.5) + 3.60(loglogW_mxⁱ -2.5)² (0.52 mag rms) and M_W2^b,i,k,a = -19.91 - 8.40(logW_mxⁱ -2.5) + 4.32(loglogW_mxⁱ -2.5)² (0.55 mag rms). We apply an I-band -WISE color correction to lower the scatter and derive M_Cw1 = -20.22 -9.12(log W_mxⁱ -2.5) and M_Cw2 = -19.63 -9.11(log W_mxⁱ -2.5) (both 0.46 mag rms). Using our three independent TFRs (W1 curved, W2 curved, and I band), we calibrate the UNION2 Type Ia supernova sample distance scale and derive H₀= 74.4±1.4(stat)±2.4(sys) km/s./Mpc with 4% total error.