Erratum: First Dark Matter Constraints from a SuperCDMS Single-Charge Sensitive Detector [Phys. Rev. Lett. 121 , 051301 (2018)]
Erratum: First Dark Matter Constraints from a SuperCDMS Single-Charge Sensitive Detector [Phys. Rev. Lett. 121 , 051301 (2018)]
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勘误表：来自 SuperCDMS 单电荷敏感探测器的第一个暗物质约束 [Phys。
DOI：
10.1103/physrevlett.122.069901
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发表时间：
2019
影响因子：
8.6
通讯作者：
Binder, T.
中科院分区：
文献类型：
--
作者：
Agnese, R.;Aralis, T.;Aramaki, T.;Arnquist, I. J.;Azadbakht, E.;Baker, W.;Banik, S.;Barker, D.;Bauer, D. A.;Binder, T.
如图。 1. 与 XENON10 和 SENSEI 结果相比，修正了 DM 粒子通过重暗光子（顶部，FDM= 1）或超轻暗光子（底部，FDM∝ 1= q 2）与电子相互作用的限制 [2, 3]。红线是电离模型中Fano因子为0.155的极限曲线。鲑鱼色区域表示由于 Fano 因子在数学上可能的最低值和 1 之间变化而导致的系统不确定性。有关信号模型以及其他天体物理约束，请参阅参考文献 [4]。此处显示的所有限制均假设局部 DM 密度为 0.3 GeV= cm 3。
FIG. 1. Corrected limit on DM particle interacting with electrons via a heavy dark photon (top, FDM= 1) or an ultralight dark photon (bottom, FDM∝ 1= q 2) compared to the XENON10 and SENSEI results [2, 3]. The red line is the limit curve with a Fano factor of 0.155 in the ionization model. The salmon colored region indicates the systematic uncertainties due to varying the Fano factor between the lowest mathematically possible value and 1. For signal models as well as additional astrophysical constraints, see Ref.[4]. All limits as shown here assume a local DM density of 0.3 GeV= cm 3.