天体粒子天空的宇宙学模型

J. Biteau, S. Marafico, Y. Kerfis, O. Deligny
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引用次数: 2

摘要

对河外天体粒子天空的建模包括重建宇宙中最极端源的三维分布。近红外波段的全天层析成像调查已经使天体粒子界能够绑定天体物理中微子和超高宇宙射线(uhecr)源的密度,约束二元黑洞合并的分布,并确定河外伽玛射线背景的一些成分。这篇文章总结了清理和补充引力波和近红外社区所开发的星表的努力,以获得恒星质量(“∗”)和恒星形成率(SFR)的宇宙学观点。前所未有的宇宙学是由350 Mpc内约40万个星系的样本提供的,光谱和光度距离,“*”,SFR和随距离增加和星系纬度减少而不完整的校正比例为50-50。推断出的“*”和“SFR”的三维分布与“宇宙流”一致。*和SFR密度趋同于与100 Mpc以上的深场观测相一致的值,表明较远源的分布接近各向同性。除了强调四种天体粒子群落的相关应用外,这篇论文还探索了从物质的三维分布推断出的Mpc尺度上的-场分布,这被认为是塑造超高能量天空的关键。这些努力为模拟UHECR各向异性提供了新的基础,这对确定其长期寻找的来源来说是一个好兆头。
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Cosmographic model of the astroparticle skies
Modeling the extragalactic astroparticle skies involves reconstructing the 3D distribution of the most extreme sources in the Universe. Full-sky tomographic surveys at near-infrared wavelengths have already enabled the astroparticle community to bind the density of sources of astrophysical neutrinos and ultra-high cosmic rays (UHECRs), constrain the distribution of binary black-hole mergers and identify some of the components of the extragalactic gamma-ray background. This contribution summarizes the efforts of cleaning and complementing the catalogs developed by the gravitational-wave and near-infrared communities, in order to obtain a cosmographic view on stellarmass ("∗) and star formation rate (SFR).Unprecedented cosmography is offered by a sample of about 400,000 galaxies within 350 Mpc, with a 50-50 ratio of spectroscopic and photometric distances, "∗, SFR and corrections for incompleteness with increasing distance and decreasing Galactic latitude. The inferred 3D distribution of "∗ and SFR is consistent with Cosmic Flows. The "∗ and SFR densities converge towards values compatible with deep-field observations beyond 100 Mpc, suggesting a close-to-isotropic distribution of more distant sources. In addition to highlighting relevant applications for the four astroparticle communities, this contribution explores the distribution of -fields at Mpc scales deduced from the 3D distribution of matter, which is believed to be crucial in shaping the ultra-high-energy sky. These efforts provide a new basis for modeling UHECR anisotropies, which bodes well for the identification of their long-sought sources.
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