arXiv 2205.131362022-05-26astro-ph.GAastro-ph.CO

WISE W1（$3.4μ\rm m$）和W2（$4.6μ\rm m$）波段中Tully-Fisher关系的校准

Calibration of the Tully-Fisher relation in the WISE W1 ($3.4μ\rm m$) and W2 ($4.6μ\rm m$) Bands

Rianna Bell, Khaled Said, Tamara Davis, T. H. Jarrett

备注：: 16 pages, 17 figures, 1 table, submitted to MNRAS, comments are welcome
DOI：: 10.1093/mnras/stac3407

摘要：

本文分别用848个和857个大样本的W_1和W_2波段的数据，对中红外W_1（$3.4μ$ m）和W_2（$4.6μ$ m）波段的TF关系进行了刻度。在这个校准中，我们进行了集群人口不完整性偏差的校正，和形态类型校正。使用新的迭代双变量拟合程序进行校准。对于这些校准，我们使用的总绝对星等，和HI线宽$W_{F50}$来自HI全球配置文件作为衡量的旋转速度。然后，我们进行了两个额外的校准相同的样品使用（i）等照度星等和（ii）平均旋转速度测量沿平面部分的空间分辨的旋转曲线的星系，这是从旋转速度定义之间的经验转换。我们比较了这三个校准，以确定是否使用等照度的幅度，或空间分辨的旋转速度有一个显着的影响周围的TF关系在W1和W2波段的散射。我们发现，使用总幅度和\hi线宽的原始校准具有最小的总散射。这些校准由$M_{\rm Tot, W1} = (2.02 \pm 0.44) - (10.08 \pm 0.17)\log_{10}(W_{F50})$和$M_{\rm Tot, W2} = (2.00 \pm 0.44) - (10.11 \pm 0.17)\log_{10}(W_{F50})$给出，并具有$σ_{W1} = 0.68$和$σ_{W2} = 0.69$的相关总散射。最后，我们比较了我们的校准在中红外波段与以前的校准在近红外J，H和K波段和长波长的光学I波段，其中使用相同的两个校正。这些关系之间的差异可以通过考虑由不同波长追踪的螺旋星系的不同区域和组成部分来解释。

英文摘要：

In this paper, we present our calibrations of the TF relation in the mid-infrared W1 ($3.4μ$m) and W2 ($4.6μ$m) bands, using large samples 848 galaxies and 857 galaxies in the W1 and W2 bands respectively. In this calibration we performed a correction for the cluster population incompleteness bias, and a morphological type correction. The calibration was performed using a new, iterative bivariate fitting procedure. For these calibrations we used the total absolute magnitudes, and HI linewidths $W_{F50}$ derived from the HI global profiles as a measure of the rotational velocities. We then performed two additional calibrations on the same sample using (i) the isophotal magnitudes and (ii) the average rotational velocities measured along the flat sections of the spatially resolved rotation curves of the galaxies, which were obtained from the empirical conversion between rotational velocity definitions. We compared these three calibrations to determine whether the use of isophotal magnitudes, or spatially resolved rotational velocities have a significant impact on the scatter around the TF relations in the W1 and W2 bands. We found that the original calibrations using total magnitudes and \hi linewidths had the smallest total scatters. These calibrations are given by $M_{\rm Tot, W1} = (2.02 \pm 0.44) - (10.08 \pm 0.17)\log_{10}(W_{F50})$ and $M_{\rm Tot, W2} = (2.00 \pm 0.44) - (10.11 \pm 0.17)\log_{10}(W_{F50})$, with associated total scatters of $σ_{W1} = 0.68$ and $σ_{W2} = 0.69$. Finally, we compared our calibrations in the mid-infrared bands with previous calibrations in the near-infrared J, H and K bands and the long-wavelength optical I band, which used the same two corrections. The differences between these relations can be explained by considering the different regions and components of spiral galaxies that are traced by the different wavelengths.

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摘要：

英文摘要：

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