未分辨伽马射线源的聚集偏置
On the Clustering Bias of Unresolved Gamma-Ray Sources
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中文总结 AI 辅助
本研究通过弱引力透镜与未分辨伽马射线背景的互相关，推断出未分辨耀变体种群的平均偏置和宿主暗物质晕质量，发现信号由中等偏置源主导，且结果不依赖于具体源模型。
中文摘要 AI 辅助
未分辨伽马射线背景（UGRB）编码了那些太暗而无法单独探测的源种群的集体辐射，其与大尺度结构示踪物的互相关已成为表征这些种群的有力工具。在本工作中，我们使用参考耀变体模型分析了弱引力透镜-UGRB互相关。通过模拟耀变体伽马射线光度与宿主暗物质晕质量之间的关系，我们推断出未分辨耀变体种群的平均线性偏置⟨b(z)⟩和宿主暗物质晕质量⟨M(z)⟩。我们发现该信号由中等偏置的源主导，在z≃1处⟨b⟩≳2，其宿主暗物质晕质量为⟨M⟩∼O(10^13 M_⊙)。使用非对齐活动星系核模型重复分析得到一致的偏置值，表明该结果由UGRB的聚集性质决定，而非伽马射线源模型的细节决定。
英文摘要
The Unresolved $γ$-Ray Background (UGRB) encodes the collective emission of source populations that are too faint to be detected individually, and its cross-correlation with tracers of the large-scale structure has emerged as a powerful tool to characterize those populations. In this work, we analyze the weak-lensing--UGRB cross-correlation using a reference blazar model. By modeling the relation between blazar $γ$-ray luminosity and host-halo mass, we infer the average linear bias $\langle b(z) \rangle$ and host-halo mass $\langle M(z) \rangle$ of the unresolved blazar population. We find that the signal is dominated by moderately biased sources, with $\langle b \rangle \gtrsim 2$ at $z\simeq 1$, hosted by halos with $\langle M \rangle \sim \mathcal{O}(10^{13}\,M_\odot)$. Repeating the analysis with a misaligned-AGN model yields consistent bias values, indicating that the result is determined by the clustering properties of the UGRB rather than by the details of the $γ$-ray source model.
发表机构
- Università degli Studi di Torino（都灵大学）
- INFN – Istituto Nazionale di Fisica Nucleare, Sezione di Torino（意大利国家核物理研究所都灵分部）
- University of Amsterdam（阿姆斯特丹大学）
- Louisiana State University（路易斯安那州立大学）
- INAF – Istituto Nazionale di Astrofisica, Osservatorio Astrofisico di Torino（意大利国家天体物理研究所都灵天文台）
- Department of Physics & Astronomy, University of the Western Cape（西开普大学物理与天文学系）
- Ludwig-Maximilians-Universität（慕尼黑大学）
机构由 AI 辅助整理，请以论文原文为准。
