We obtain an unbiased estimate of the global Hubble constant H0 in a volume of cz ≤ 12,000 km s-1 in the region of Pisces-Perseus. The Tully-Fisher (TF) relation is applied to a magnitude-limited sample of 441 spiral galaxies selected from the Arecibo 21 cm catalog. We improve the photometry data of the previous TF study by Ichikawa & Fukugita by using our original surface photometry data and local calibrators that have newly been made available in other works. The photometry data were calibrated with CCD observations, and we achieve 0.13 mag for a photometric internal error. We use a maximum likelihood method for the TF analysis. Monte Carlo simulations demonstrate that our method reproduces a given H0 at the 95% confidence level. By applying the method to our sample galaxies, we obtain the unbiased global Hubble constant H0=65±2?14+20 km s-1 Mpc-1; the first and the second terms represent the internal random error and the external uppermost and lowermost systematic errors, respectively. We also find a good agreement for our H0 with those recently obtained via Cepheid observation in the local universe and the TF relation and supernovae applied to a spatial volume comparable to or larger than ours. Hubble velocities of the spirals inferred from our H0 show no significant systematic differences from those given in the Mark III catalog. The same analysis for H0 is carried out using the r-band photometry data of the Pisces-Perseus region given by Willick et al. We obtain a global H0 that is consistent with that obtained from the B-band analysis. A bulk motion in the Pisces-Perseus region is briefly discussed, based on our calibration of H0. The B-band intrinsic TF scatter is too large to allow any determination of bulk motion. However, our r-band TF analysis supports the notion of a coherent streaming motion of the Pisces-Perseus ridge with a velocity of ~-200 km s-1 with respect to the CMB, in agreement with most modern studies.
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机译：我们在双鱼座-珀尔修斯地区的cz≤12,000 km s-1中获得了全球哈勃常数H0的无偏估计。 Tully-Fisher（TF）关系适用于从Arecibo 21 cm目录中选择的441个旋涡星系的幅度受限样本。通过使用我们最初的表面光度数据和其他工作中新近使用的本地校准器，我们改进了Ichikawa＆Fukugita先前TF研究的光度数据。用CCD观测值对光度数据进行了校准，对于光度内部误差，我们获得0.13 mag。我们使用最大似然法进行TF分析。蒙特卡洛模拟表明，我们的方法以95％的置信度再现了给定的H0。通过将该方法应用于我们的样本星系，我们获得了无偏全局哈勃常数H0 = 65±2？14 + 20 km s-1 Mpc-1;第一项和第二项分别代表内部随机误差和外部最高和最低系统误差。我们还发现H0与最近通过造父变星观测在当地宇宙中获得的H0有很好的一致性，并且TF关系和超新星应用于与我们相当或更大的空间体积。从H0推论得出的螺旋线的哈勃速度与Mark III目录中给出的系统速度没有明显的系统差异。使用Willick等人给出的双鱼座-英仙座区域的r波段测光数据对H0进行相同的分析。我们获得与从B波段分析获得的全局H0一致的全局H0。根据我们对H0的校准，简要讨论了双鱼座-英仙座区域的整体运动。 B波段固有TF散射太大，无法确定整体运动。然而，与大多数现代研究一致，我们的r波段TF分析支持双鱼座-珀耳修斯海岭相干流的连贯运动（相对于CMB约为-200 km s-1）的概念。
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