Constraints on dark matter-nucleon effective couplings in the presence of kinematically distinct halo substructures using the DEAP-3600 detector
Constraints on dark matter-nucleon effective couplings in the presence of kinematically distinct halo substructures using the DEAP-3600 detector
复制标题
DOI：
10.1103/physrevd.102.082001
复制
发表时间：
2020-05
影响因子：
5
通讯作者：
P. Adhikari;R. Ajaj;D. Auty;C. E. Bina;W. Bonivento;M. Boulay;M. Cadeddu;B. Cai;M. C'ardenas-Montes-M.
中科院分区：
文献类型：
--
作者：
P. Adhikari;R. Ajaj;D. Auty;C. E. Bina;W. Bonivento;M. Boulay;M. Cadeddu;B. Cai;M. C'ardenas-Montes-M.
DEAP-3600 是一款单相液氩探测器，旨在直接检测弱相互作用大质量粒子 (WIMP)，位于 SNOLAB（加拿大萨德伯里）。在分析第一年运行期间获取的数据后，使用无效结果为 WIMP 核子自旋无关的等标量横截面设置上限。这项研究在非相对论有效场论框架内重新解释了这一结果，并进一步研究了局部暗物质晕中各种可能的子结构如何影响这些约束。盖亚卫星和其他最近的天文观测观测到的当地恒星分布的运动结构暗示了这种子结构。其中包括盖亚香肠（或土卫二），以及最近研究中发现的许多不同的溪流。考虑等标量、等向量和等量关系，对有效接触交互算子 $\mathcal{O}_1$、$\mathcal{O}_3$、$\mathcal{O}_5$、$\mathcal{O}_8$ 和 $\mathcal{O}_{11}$ 的耦合强度给出限制。 仇外场景，以及与毫电荷、磁偶极子、电偶极子和阿纳极相互作用相对应的特定算子。还探讨了晕子结构对每个算子的影响，表明 $\mathcal{O}_5$ 和 $\mathcal{O}_8$ 算子对速度分布特别敏感，即使在暗物质质量高于 100 GeV/$c^2$ 时也是如此。
DEAP-3600 is a single-phase liquid argon detector aiming to directly detect Weakly Interacting Massive Particles (WIMPs), located at SNOLAB (Sudbury, Canada). After analyzing data taken during the first year of operation, a null result was used to place an upper bound on the WIMP-nucleon spin-independent, isoscalar cross section. This study reinterprets this result within a Non-Relativistic Effective Field Theory framework, and further examines how various possible substructures in the local dark matter halo may affect these constraints. Such substructures are hinted at by kinematic structures in the local stellar distribution observed by the Gaia satellite and other recent astronomical surveys. These include the Gaia Sausage (or Enceladus), as well as a number of distinct streams identified in recent studies. Limits are presented for the coupling strength of the effective contact interaction operators $\mathcal{O}_1$, $\mathcal{O}_3$, $\mathcal{O}_5$, $\mathcal{O}_8$, and $\mathcal{O}_{11}$, considering isoscalar, isovector, and xenonphobic scenarios, as well as the specific operators corresponding to millicharge, magnetic dipole, electric dipole, and anapole interactions. The effects of halo substructures on each of these operators are explored as well, showing that the $\mathcal{O}_5$ and $\mathcal{O}_8$ operators are particularly sensitive to the velocity distribution, even at dark matter masses above 100 GeV/$c^2$.