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arXiv 1407.7528astro-ph.COastro-ph.GA
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WISE W1和W2 Tully-Fisher关系的校正

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

J. D. Neill, Mark Seibert, R. Brent Tully, Hélène Courtois, Jenny G. Sorce, T. H. Jarrett, Victoria Scowcroft, Frank J. Masci

备注：
22 page, 21 figures, accepted to ApJ, Table 1 data at http://spartan.srl.caltech.edu/~neill/tfwisecal/table1.txt
发表信息：
ApJ v792 p129, 2014
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摘要：

为了探索局部大尺度结构和速度场，需要精确的星系距离测量。现在，我们将校准星系旋转速率和光度之间的相关性的久经考验的配方-能够提供这种距离测量-扩展到来自宽场红外巡天探测器（WISE）W1（$3.4μ$ m）和W2（$4.6μ$ m）过滤器的全天空天基成像数据。我们从13个星系团的310个星系中发现了$\mathcal{M}^{b,i,k,a}_{W1} = -20.35 - 9.56 (\log W^i_{mx} - 2.5)$（0.54星等rms）和$\mathcal{M}^{b,i,k,a}_{W2} = -19.76 - 9.74 (\log W^i_{mx} - 2.5)$（0.56星等rms）的线宽与绝对星等的相关性（Tully-Fisher关系，TFR）。我们使用比Tully & Courtois（2012）大9%的样本更新了I波段TFR。我们推导出$\mathcal{M}^{b,i,k}_I = -21.34 - 8.95 (\log W^i_{mx} - 2.5)$（0.46幅度均方根）。WISE TFR显示弯曲迹象。二次拟合给出了$\mathcal{M}^{b,i,k,a}_{W1} = -20.48 - 8.36 (\log W^i_{mx} - 2.5) + 3.60 (\log W^i_{mx} - 2.5)^2$（0.52幅度rms）和$\mathcal{M}^{b,i,k,a}_{W2} = -19.91 - 8.40 (\log W^i_{mx} - 2.5) + 4.32 (\log W^i_{mx} - 2.5)^2$（0.55幅度rms）。我们应用I波段- WISE颜色校正来降低散射，并导出$\mathcal{M}_{C_{W1}} = -20.22 - 9.12 (\log W^i_{mx} - 2.5)$和$\mathcal{M}_{C_{W2}} = -19.63 - 9.11 (\log W^i_{mx} - 2.5)$（均为0.46幅度rms）。使用我们的三个独立的TFRs（W1弯曲，W2弯曲和I波段），我们校准UNION 2超新星Ia型样本距离尺度和导出$H_0 = 74.4 \pm 1.4$（stat）$\pm\ 2.4$（sys）kms $^{-1}$ Mpc $^{-1}$与4%的总误差。

英文摘要：

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 ($3.4μ$m) and W2 ($4.6μ$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.

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