Erratum: “Propagation of Ultra-High-Energy Cosmic Rays above 1019 eV in a Structured Extragalactic Magnetic Field and Galactic Magnetic Field” (ApJ, 639, 803 [2006])
Erratum: “Propagation of Ultra-High-Energy Cosmic Rays above 1019 eV in a Structured Extragalactic Magnetic Field and Galactic Magnetic Field” (ApJ, 639, 803 [2006])
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勘误表：“1019 eV 以上超高能宇宙射线在结构化河外磁场和银河磁场中的传播”（ApJ, 639, 803 [2006]）
DOI：
10.1086/508700
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发表时间：
2006
期刊：
影响因子：
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通讯作者：
Katsuhiko Sato
中科院分区：
文献类型：
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作者：
H. Takami;Hiroyuki Yoshiguchi;Katsuhiko Sato
由于在计算超高能宇宙射线(UHECR)到达分布时存在数值误差，图9和图14是错误的。我们考虑了10Y106MPC的UHECR源的数密度；然而，最能再现AGASA结果的UHECR源的数密度超出了这个范围，为104MPC。使用调和分析估计了大尺度各向同性(见原始图7和图8)。当我们重新计算一次和二次谐波时，对于103Mpc到106Mpc的所有数密度，这些幅度与AGASA得到的各向同性在1个统计误差内是一致的。这里给出的修正后的图9显示了公式(18)中定义的10，作为UHECR源的数密度的函数。图10显示了计算的两点相关函数与AGASA得到的函数的拟合优度。修正后的数字显示，最能再现AGASA结果的震源的数密度为10 Mpc，因为这是最小的10 Mpc。修正后的图14显示了根据再现AGASA观测到的大尺度各向同性的震源分布计算的两点关联函数。在未经校正的计算中，这样的源分布的数量为20个。然而，在这里，21个数密度为104 Mpc 3的震源分布再现了大尺度各向同性。大多数不能再现大尺度各向同性的震源分布都有非常近和明亮的震源。这些来源对到达的宇宙射线流量的贡献导致了强烈的各向异性。在修订后的图14的左图中，可以看到两点相关函数实际上与AGASA的结果是一致的，尽管它与我们的原始论文不一致。这种差异是由于增加了震源数密度造成的。综上所述，AGASA观测到的大尺度各向同性和小尺度各向异性是在局域结构的河外磁场和银河系磁场作用下，以104MpC的源密度再现的。请注意，我们采用了光度加权源模型，如公式(12)中所示。由于发光源是宇宙射线的主要贡献者，UHECR源的数密度比源模型中增加的更多，与源的光度无关。
Because of a numerical error in computing the arrival distribution of ultraYhigh-energy cosmic rays (UHECRs), Figures 9 and 14 are incorrect. We considered number densities of UHECR sources with 10 Y10 6 Mpc ; however, the number density of UHECR sources that best reproduces the AGASA results is outside this range, at 10 4 Mpc . The large-scale isotropy was estimated using harmonic analysis (see our original Figs. 7 and 8). When we recalculate the first and second harmonics, for all number densities from 10 3 to 10 6 Mpc , these amplitudes are consistent with the isotropy obtained by AGASAwithin 1 total statistical errors. The corrected Figure 9 given here shows 10, defined in equation (18), as a function of the number density of UHECR sources. The 10 plot shows the goodness of fit of the calculated two-point correlation functions and the function obtained by AGASA. The revised figure shows that the number density of the sources that best reproduces the AGASA results is 10 Mpc , since this has the smallest 10. The corrected Figure 14 shows the two-point correlation functions calculated from source distributions that reproduce the largescale isotropy observed by AGASA. The number of such source distributions is 20 in the uncorrected calculation. Here, however, 21 source distributions with number densities of 10 4 Mpc 3 reproduce the large-scale isotropy. Most of the source distributions that do not reproduce the large-scale isotropy have very near and bright sources. The contributions to arriving cosmic-ray flux from such sources result in strong anisotropies. In the left panel of the revised Figure 14, it can be seen that the two-point correlation function is in fact consistent with the AGASA result, although it is not consistent in our original paper. This difference results from increasing the source number density. In summary, the large-scale isotropy and small-scale anisotropy observed by AGASA are reproduced with a source number density of 10 4 Mpc 3 with a locally structured extragalactic magnetic field and a Galactic magnetic field. Note that we have adopted a luminosity-weighted source model, as in equation (12). The number density of UHECR sources increases more than in the source model independent of source luminosity, since luminous sources are the main contributors of cosmic-rays.