论文标题
使用X射线光谱和成像卫星实验和未来卫星任务的前景搜索原始黑洞暗物质
Search for primordial black hole dark matter with X-ray spectroscopic and imaging satellite experiments and prospects for future satellite missions
论文作者
论文摘要
当前观察值允许超光原始黑洞（PBHS（PBH）10 $^{16} $ -10 $ -10 $^{22} $ g允许构成宇宙中的暗物质的很大一部分，即使不是全部。在这项工作中，我们提出了对超轻质，非旋转PBH的限制，这些PBH是由Kev-Mev能量带中此类物体的鹰辐射信号的未检测而产生的。也就是说，我们考虑了当前代代任务XMM-Newton和Integrall/SPI的观察结果，并讨论了未来Missions Missions Athena，Extp和Theseus的观察观点，以进行PBH搜索。基于3.4毫秒的总暴露时间XMM-Newton对Draco矮球的观察结果，我们得出结论，具有质量$ \ Lessim 10^{16} $ g的PBH无法在95％的置信度下使所有暗物质都能使所有暗物质的变化。我们对银河系中$> 100 $ MSEC的积分/SPI数据的开放式分析对Halo的速度产生了更大的约束。只有$ \ Lessim 10 $％的暗物质才能由质量$ \ sillesim 3 \ cdot 10^{16} $ g提出，而大多数暗物质不能由$ 7 \ cdot 10^{16} $ g的$ 7 \ cdot 10^{16} $ G表示95％。我们讨论了系统不确定性与工具性和天体物理积分/SPI背景的变化相关的对派生结果的变化并估算其水平的强烈影响。我们还表明，根据这些仪器系统的系统控制水平，未来的大型视野任务（例如Theseus/X-GI）将能够提高约束10-100倍。
Ultra-light primordial black holes (PBHs) in the mass range of 10$^{16}$ - 10$^{22}$ g are allowed by current observations to constitute a significant fraction, if not all, of the dark matter in the Universe. In this work, we present limits on ultra-light, non-rotating PBHs which arise from the non-detection of the Hawking radiation signals from such objects in the keV-MeV energy band. Namely, we consider observations from the current-generation missions XMM-Newton and INTEGRAL/SPI and discuss the observational perspectives of the future missions Athena, eXTP, and THESEUS for PBH searches. Based on 3.4 Msec total exposure time XMM-Newton observations of Draco dwarf spheroidal galaxy, we conclude that PBH with masses $\lesssim 10^{16}$ g can not make all dark matter at 95% confidence level. Our ON-OFF-type analysis of $>100$ Msec of INTEGRAL/SPI data on the Milky Way halo puts significantly stronger constraints. Only $\lesssim 10$% dark matter can be presented by PBHs with masses $\lesssim 3\cdot 10^{16}$ g while the majority of dark matter can not be represented by PBHs lighter than $7\cdot 10^{16}$ g at 95% confidence level. We discuss the strong impact of systematic uncertainty related to the variations of instrumental and astrophysical INTEGRAL/SPI background on the derived results and estimate its level. We also show that future large-field-of-view missions such as THESEUS/X-GIS will be able to improve the constraints by a factor of 10-100 depending on the level of control under the systematics of these instruments.
