通过互相关对Fermi-LAT gamma-ray天空的层析成像：更广泛和更深入的观察
Tomographic imaging of the Fermi-LAT gamma-ray sky through cross-correlations: A wider and deeper look
摘要：
我们调查的性质，河外未解决的伽玛射线背景（UGRB）交叉相关的几个星系目录与天空地图的UGRB建立从78个月的通行证8费米大面积望远镜的数据。本研究在几个方面更新和改进了以往的类似分析。首先，使用更大的伽马射线数据集使我们能够更详细地研究互相关的能量依赖性，在[0.25-500] GeV的宽能量范围内使用多达8个能量箱。其次，我们考虑更大和更深的目录（2 MASS光度红移目录，2 MPZ; WISE x SuperCOSMOS，WISC;和SDSS-DR 12光度红移数据集）除了在以前的研究中使用的目录（NVSS和SDSS-QSO）。第三，我们利用上述星表的红移信息，将它们划分为红移仓，并分别在每个仓中进行互相关。我们的研究结果证实，具有较高的统计意义，互相关信号之间的UGRB地图和所有考虑的目录，在小于1度的角尺度的检测。NVSS的显著性范围为16.3 sigma，SDSS-DR 12和WISC为7 sigma，2 MPZ为5 sigma，SDSS-QSO为4 sigma。此外，包括红移层析成像，SDSS-DR 12信号的显著性显著上升至12 σ，WISC的显著性显著上升至10.6 σ。我们提供了一个简单的解释晕模型的框架中的信号。精确的红移和能量信息使我们能够清楚地检测到对UGRB有贡献的伽马射线源的光谱和聚集行为的红移变化。
英文摘要：
We investigate the nature of the extragalactic unresolved gamma-ray background (UGRB) by cross-correlating several galaxy catalogs with sky-maps of the UGRB built from 78 months of Pass 8 Fermi-Large Area Telescope data. This study updates and improves similar previous analyses in several aspects. Firstly, the use of a larger gamma-ray dataset allows us to investigate the energy dependence of the cross-correlation in more detail, using up to 8 energy bins over a wide energy range of [0.25-500] GeV. Secondly, we consider larger and deeper catalogs (2MASS Photometric-Redshift catalog, 2MPZ; WISE x SuperCOSMOS, WISC; and SDSS-DR12 photometric-redshift dataset) in addition to the ones employed in the previous studies (NVSS and SDSS-QSOs). Thirdly, we exploit the redshift information available for the above catalogs to divide them into redshift bins and perform the cross-correlation separately in each of them. Our results confirm, with higher statistical significance, the detection of cross-correlation signal between the UGRB maps and all the catalogs considered, on angular scales smaller than 1 degree. Significances range from 16.3 sigma for NVSS, 7 sigma for SDSS-DR12 and WISC, 5 sigma for 2MPZ and 4 sigma for SDSS-QSOs. Furthermore, including redshift tomography, the significance of the SDSS-DR12 signal strikingly rises up to 12 sigma and the one of WISC to 10.6 sigma. We offer a simple interpretation of the signal in the framework of the halo model. The precise redshift and energy information allows us to clearly detect a change over redshift in the spectral and clustering behavior of the gamma-ray sources contributing to the UGRB.
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