248 keV LUX-ZEPLIN反冲候选事件中的核干涉与暗区激发
Nuclear interference versus dark sector excitation in the 248 keV LUX-ZEPLIN recoil candidate
- Zhejiang Normal University（浙江师范大学）
- Khazar University（哈扎尔大学）
- Università di Napoli “Federico II”（那不勒斯费德里科二世大学）
- Istituto Nazionale di Fisica Nucleare (INFN), sez. di Napoli（意大利国家核物理研究所（INFN）那不勒斯分部）
- Scuola Superiore Meridionale（南方高等学院）
- Harbin Institute of Technology（哈尔滨工业大学）
- University of Tashkent for Applied Sciences（塔什干应用科学大学）
- National University of Uzbekistan（乌兹别克斯坦国立大学）
机构由 AI 辅助整理，请以论文原文为准。
AI总结：
研究LZ实验248 keV反冲候选事件，对比弹性核响应与吸热暗区激发，发现核消零位置及年调制差异可区分两种机制，为暗物质探测提供判别依据。
AI中文摘要：
2026年LUX-ZEPLIN（LZ）高能核反冲搜索报告了一个能量为$248\pm23_{\rm stat}\pm23_{\rm sys}~\mathrm{keV}$的事件，并发现弹性同位旋矢量相互作用$\mathcal L_6^v$在重暗物质区域约$3.3\sigma$的局部置信水平上受到青睐。我们考察了这一反冲能标是否可源于弹性相互作用中的可分辨核响应，并将其谱形、靶核及年调制行为与吸热暗区激发进行比较。协变匹配关联了四个伽利略算符，代数地消除了纵向自旋响应，并确定了密度与轨道自旋-轨道振幅之间的干涉。GCN和JJ55氙壳模型计算给出了第二个自然的氙消零位置，分别为$211$和$214~\mathrm{keV}$。在重质量区域，该位置从暗物质质量$200~\mathrm{GeV}$到渐近极限的变化小于$0.01~\mathrm{keV}$。曲率加权的同位素质心重现了自然氙极小值的位置和剩余深度。直接的$^{40}$Ar计算将核特征移至约$350$和$425~\mathrm{keV}$，而吸热激发则遵循由暗态分裂设定的约化质量标度。在暗物质质量为$1~\mathrm{TeV}$时，吸热Ar与Xe的标度比为$1.082$，而核计算的对应比值为$1.63$至$2.01$。在所采用的晕模型中，弹性散射给出百分之几的年调制，而接近最大实验室晕速度的吸热解则显示出大得多的季节变化。这些标度和时间行为提供了对靶依赖的核消零与由暗区运动学设定的激发能的检验。
英文摘要：
The 2026 LUX-ZEPLIN (LZ) high energy nuclear recoil search reports one event at $248\pm23_{\rm stat}\pm23_{\rm sys}~\mathrm{keV}$ and finds the elastic isovector interaction $\mathcal L_6^v$ locally favored at about $3.3σ$ in the heavy dark matter regime. We examine whether this recoil scale can arise from resolved nuclear response within the elastic interaction and compare its spectral, target, and annual modulation behavior with endothermic dark sector excitation. Covariant matching correlates four Galilean operators, removes the longitudinal spin response algebraically, and fixes interference between density and orbital spin orbit amplitudes. The GCN and JJ55 xenon shell model calculations give a second natural xenon cancellation at $211$ and $214~\mathrm{keV}$. In the heavy mass regime, its position changes by less than $0.01~\mathrm{keV}$ from a dark matter mass of $200~\mathrm{GeV}$ to the asymptotic limit. A curvature weighted isotope centroid reproduces the position and residual depth of the natural xenon minimum. Direct $^{40}$Ar calculations shift the nuclear feature to about $350$ and $425~\mathrm{keV}$, whereas endothermic excitation follows reduced mass scaling set by the dark state splitting. At a dark matter mass of $1~\mathrm{TeV}$, the endothermic Ar to Xe scale ratio is $1.082$, compared with $1.63$ to $2.01$ for the nuclear calculations. Elastic scattering gives a few percent annual modulation in the adopted halo model, while endothermic solutions near the maximum laboratory halo speed show much larger seasonal variation. These scaling and timing behaviors provide tests of a target-dependent nuclear cancellation against an excitation energy set by dark sector kinematics.
