A low-mass dark matter search using ionization signals in XENON100
XENON100 Collaboration, E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, F. D. Amaro, M. Anthony, F. Arneodo, P. Barrow, L. Baudis, B. Bauermeister, M. L. Benabd… 展开作者
XENON100 Collaboration, E. Aprile, J. Aalbers, F. Agostini, M. Alfonsi, F. D. Amaro, M. Anthony, F. Arneodo, P. Barrow, L. Baudis, B. Bauermeister, M. L. Benabderrahmane, T. Berger, P. A. Breur, A. Brown, E. Brown S. Bruenner, G. Bruno, R. Budnik, A. Buss, L. Bütikofer, J. M. R. Cardoso, M. Cervantes, D. Cichon, D. Coderre, A. P. Colijn, J. Conrad, J. P. Cussonneau, M. P. Decowski, P. de Perio, P. Di Gangi, A. Di Giovanni, E. Duchovni, A. D. Ferella, A. Fieguth, D. Franco, W. Fulgione, M. Galloway, M. Garbini, C. Geis, L. W. Goetzke, Z. Greene, C. Grignon, E. Gross, C. Hasterok, E. Hogenbirk, R. Itay, B. Kaminsky, G. Kessler, A. Kish, H. Landsman, R. F. Lang, L. Levinson, M. Le Calloch, C. Levy, F. Linde, S. Lindemann, M. Lindner, J. A. M. Lopes, A. Lyashenko, A. Manfredini, T. Marrodán Undagoitia, J. Masbou, F. V. Massoli, D. Masson, D. Mayani, A. J. Melgarejo Fernandez, Y. Meng, M. Messina, K. Micheneau, B. Miguez, A. Molinario, M. Murra, J. Naganoma, U. Oberlack, S. E. A. Orrigo, P. Pakarha, B. Pelssers, R. Persiani, F. Piastra, J. Pienaar, G. Plante, N. Priel, L. Rauch, S. Reichard, C. Reuter, A. Rizzo, S. Rosendahl, N. Rupp, J. M. F. dos Santos, G. Sartorelli, M. Scheibelhut, S. Schindler, J. Schreiner, M. Schumann, L. Scotto Lavina, M. Selvi, P. Shagin, H. Simgen, A. Stein, D. Thers, A. Tiseni, G. Trinchero, C. D. Tunnell, M. von Sivers, R. Wall, H. Wang, M. Weber, Y. Wei, C. Weinheimer, J. Wulf, Y. Zhang
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6 pages; 7 figures; PRD. Additional file in source material, s2stot, contains the full list of events passing all selection cuts. Limit data points in TeX; Corrected LUX points used for comparison and respective reference in figure 5
We perform a low-mass dark matter search using an exposure of 30\,kg$\times$yr with the XENON100 detector. By dropping the requirement of a scintillation signal and using only the ionization signal to determine the interaction energy, we lowered the energy threshold for detection to 0.7\,keV for nuclear recoils. No dark matter detection can be claimed because a complete background model cannot be constructed without a primary scintillation signal. Instead, we compute an upper limit on the WIMP-nucleon scattering cross section under the assumption that every event passing our selection criteria could be a signal event. Using an energy interval from 0.7\,keV to 9.1\,keV, we derive a limit on the spin-independent WIMP-nucleon cross section that excludes WIMPs with a mass of 6\,GeV/$c^2$ above $1.4 \times 10^{-41}$\,cm$^2$ at 90\% confidence level.
Ionization of atoms by slow heavy particles, including dark matter
在慢重粒子与束缚电子的散射过程中，原子和分子会发生电离，这种涉及亲轻子的大质量弱相互作用粒子（WIMPs）的相互作用是DAMA暗物质直接探测实验中异常的9 σ年调制现象的一个有希望的可能解释[R. Bernabei等人，EUR. J. C 73，2648（2013）]。我们证明了这种相互作用的玻恩近似的适用性，通过显示其等效的半经典绝热处理慢移动的WIMPs的原子电离。传统观点认为，这样一个过程的电离概率应该是指数级的小。然而，我们发现，由于非解析，尖状行为的库仑函数靠近核这种抑制被删除，导致有效的原子结构增强。至关重要的是，我们还表明电子相对论效应实际上对这样的过程做出了主要贡献，将微分截面增强了1000倍。
Sub-keV dark matter can strongly ionize molecular clouds
Universidad Autónoma de Madrid（马德里自治大学）；Instituto de Física Teórica UAM-CSIC（UAM-CSIC理论物理研究所）；Stockholm University（斯德哥尔摩大学）；The Oskar Klein Centre for Cosmoparticle Physics（奥斯卡·克莱因宇宙粒子物理中心）
The Migdal effect in Semiconductors for the Effective Field Theory of Dark Matter Direct Detection
Karlsruhe Institute of Technology（卡尔斯鲁厄理工学院）；Walter Burke Institute for Theoretical Physics, California Institute of Technology（加州理工学院沃尔特·伯克理论物理研究所）；C.N. Yang Institute for Theoretical Physics, Stony Brook University（纽约州立大学石溪分校陈省身理论物理研究所）；Physics and Astronomy Department, Stony Brook University（纽约州立大学石溪分校物理与天文系）
Does the Reionization Model Influence the Constraints on Dark Matter Decay or Annihilation?
如果暗物质衰变或湮灭，大量的能量和粒子将被释放到宇宙等离子体中。因此，它们可以改变我们宇宙的热和电离历史，然后在宇宙微波背景功率谱上留下足迹。本文以暗物质湮灭为例，研究了不同的再电离模型对暗物质湮灭约束的影响。我们考虑了包括暗物质湮灭和恒星形成的电离历史，并对暗物质湮灭进行了限制。结合最新的普朗克数据、BAO数据、SNIa测量、类星体观测的$Q_\text{HII}$约束以及紫外和红外数据的恒星形成率密度，我们得到该星系的光学厚度为$τ=0.0571^{+0.0005}_{-0.0006}$，位于68 $\%$ C. L. $ε_0 f_d$的上限读数为$2.7765\times 10^{-24}$，在95 $\%$ C. L.。通过比较，我们也约束暗物质湮灭的瞬时再电离模型从相同的数据组合，除了$Q_\text{HII}$约束和恒星形成率密度。我们在68 $\%$ C. L.得到了$τ=0.0559^{+0.0069}_{-0.0076}$。$ε_0 f_d$的上限为95 $\%$ CL的$2.8468\times 10^{-24}$。%，比之前模型的结果高出$2.5\%$。这表明各种再电离模型对暗物质衰变或湮灭的约束参数影响很小。
Ultralight Boson Ionization from Comparable-Mass Binaries
Shanghai Jiao Tong University（上海交通大学）；CENTRA, Departamento de Física, Instituto Superior Técnico – IST, Universidade de Lisboa – UL（里斯本大学高级技术学院物理系CENTRA中心）；Tsung-Dao Lee Institute, Shanghai Jiao Tong University（上海交通大学李政道研究所）；Dipartimento di Fisica, Sapienza Università di Roma & INFN, Sezione di Roma（罗马第一大学物理系及罗马INFN分部）；Walter Burke Institute for Theoretical Physics, California Institute of Technology（加州理工学院沃尔特·伯克理论物理研究所）
