用H.E.S.S对Milky Way最近探测到的DES矮星系卫星的暗物质信号的搜索
Search for dark matter signals towards a selection of recently-detected DES dwarf galaxy satellites of the Milky Way with H.E.S.S
摘要：
银河系的矮球状星系卫星是用伽马射线间接探测暗物质的主要目标，因为它们的距离很近，暗物质含量很高，而且没有非热发射过程。最近，暗能量调查（DES）揭示了南半球天空中新的超微弱矮球状星系的存在，因此非常适合使用成像大气切伦科夫望远镜阵列H.E.S.S.进行地面观测。我们提出了一个非常高的能量（$E\gtrsim100$ GeV）的伽玛射线辐射的搜索使用H.E.S. S。最近对Reticulum II、Tucana II、Tucana III、Tucana IV和Grus II卫星进行了观测。从对任何单个物体的观测中，以及对所有数据集的综合分析中，都没有发现明显的超高能伽马射线。使用最新的建模的暗物质分布在矮星系晕，我们计算DES卫星上的第一次个人和联合约束切伦科夫望远镜观测的湮灭截面的暗物质粒子的形式弱相互作用的大质量粒子。95%的C.L.对于质量为1.5 TeV的暗物质，观测到的上限在$W^+W^-$通道中达到$\langle σv \rangle \simeq 1 \times 10^{-23}$ cm $^3$ s $^{-1}$，在$γγ$通道中达到$4 \times 10^{-26}$ cm $^3$ s $^{-1}$。H.E.S.S.约束很好地补充了Fermi-LAT，HAWC，MAGIC和VERITAS的结果，目前是多GeV/多TeV质量范围内$γγ$通道中最严格的。
英文摘要：
Dwarf spheroidal galaxy satellites of the Milky Way are prime targets for indirect detection of dark matter with gamma rays due to their proximity, high dark matter content and absence of non-thermal emission processes. Recently, the Dark Energy Survey (DES) revealed the existence of new ultra-faint dwarf spheroidal galaxies in the southern-hemisphere sky, therefore ideally located for ground-based observations with the imaging atmospheric Cherenkov telescope array H.E.S.S. We present a search for very-high-energy ($E\gtrsim100$ GeV) gamma-ray emission using H.E.S.S. observations carried out recently towards Reticulum II, Tucana II, Tucana III, Tucana IV and Grus II satellites. No significant very-high-energy gamma-ray excess is found from the observations on any individual object nor in the combined analysis of all the datasets. Using the most recent modeling of the dark matter distribution in the dwarf galaxy halo, we compute for the first time on DES satellites individual and combined constraints from Cherenkov telescope observations on the annihilation cross section of dark matter particles in the form of Weakly Interacting Massive Particles. The combined 95% C.L. observed upper limits reach $\langle σv \rangle \simeq 1 \times 10^{-23}$ cm$^3$s$^{-1}$ in the $W^+W^-$ channel and $4 \times 10^{-26}$ cm$^3$s$^{-1}$ in the $γγ$ channels for a dark matter mass of 1.5 TeV. The H.E.S.S. constraints well complement the results from Fermi-LAT, HAWC, MAGIC and VERITAS and are currently the most stringent in the $γγ$ channels in the multi-GeV/multi-TeV mass range.
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