用Super-Kamiokande探测器间接寻找银河系中心和晕的暗物质
Indirect Search for Dark Matter from the Galactic Center and Halo with the Super-Kamiokande Detector
摘要：
基于1996年至2016年的Super-Kamiokande-I，-II，-III和-IV数据集，我们提出了一个寻找由于暗物质以弱相互作用大质量粒子（WIMPs）形式在银河系中心或晕中湮灭而导致的过量中微子相互作用的研究。假设WIMP自湮灭对$ν\overlineν$、$μ^+μ^-$、$b\overline{b}$或$W^+W^-$起主导作用，我们模拟了中微子通量、能量和味分布。过量是在比较大气中微子相互作用的详细建模和拟合数据。导出了质量在1 - 10 TeV范围内的WIMP自湮没截面$\langle σ_{A} V \rangle$的极限，对于5 GeV的WIMP在$b\bar b$模式下可达$9.6 \times10^{-23}$ cm $^3$ s $^{-1}$，对于1 GeV的WIMP在$ν\bar ν$模式下可达$1.2 \times10^{-24}$ cm $^3$ s $^{-1}$.所获得的灵敏度的超级神冈探测器的WIMP质量低于几十个GeV是最好的类似的间接搜索到目前为止。
英文摘要：
We present a search for an excess of neutrino interactions due to dark matter in the form of Weakly Interacting Massive Particles (WIMPs) annihilating in the galactic center or halo based on the data set of Super-Kamiokande-I, -II, -III and -IV taken from 1996 to 2016. We model the neutrino flux, energy, and flavor distributions assuming WIMP self-annihilation is dominant to $ν\overlineν$, $μ^+μ^-$, $b\overline{b}$, or $W^+W^-$. The excess is in comparison to atmospheric neutrino interactions which are modeled in detail and fit to data. Limits on the self-annihilation cross section $\langle σ_{A} V \rangle$ are derived for WIMP masses in the range 1 GeV to 10 TeV, reaching as low as $9.6 \times10^{-23}$ cm$^3$ s$^{-1}$ for 5 GeV WIMPs in $b\bar b$ mode and $1.2 \times10^{-24}$ cm$^3$ s$^{-1}$ for 1 GeV WIMPs in $ν\bar ν$ mode. The obtained sensitivity of the Super-Kamiokande detector to WIMP masses below several tens of GeV is the best among similar indirect searches to date.
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