scholarly journals Characterization of the Hamamatsu R11410-10 3-in. photomultiplier tube for liquid xenon dark matter direct detection experiments

2012 ◽  
Vol 696 ◽  
pp. 32-39 ◽  
Author(s):  
K. Lung ◽  
K. Arisaka ◽  
A. Bargetzi ◽  
P. Beltrame ◽  
A. Cahill ◽  
...  
Keyword(s):  
Dark Matter ◽  
Direct Detection ◽  
Photomultiplier Tube ◽  
Liquid Xenon

scholarly journals A Review of Basic Energy Reconstruction Techniques in Liquid Xenon and Argon Detectors for Dark Matter and Neutrino Physics Using NEST

Instruments ◽  
2021 ◽  
Vol 5 (1) ◽  
pp. 13
Author(s):  
Matthew Szydagis ◽  
Grant A. Block ◽  
Collin Farquhar ◽  
Alexander J. Flesher ◽  
Ekaterina S. Kozlova ◽  
...  
Keyword(s):  
Dark Matter ◽  
Neutrino Physics ◽  
Electric Fields ◽  
Direct Detection ◽  
Profile Likelihood ◽  
Liquid Argon ◽  
Energy Scale ◽  
Liquid Xenon ◽  
Nuclear Recoils ◽  
Available Information

Detectors based upon the noble elements, especially liquid xenon as well as liquid argon, as both single- and dual-phase types, require reconstruction of the energies of interacting particles, both in the field of direct detection of dark matter (weakly interacting massive particles WIMPs, axions, etc.) and in neutrino physics. Experimentalists, as well as theorists who reanalyze/reinterpret experimental data, have used a few different techniques over the past few decades. In this paper, we review techniques based on solely the primary scintillation channel, the ionization or secondary channel available at non-zero drift electric fields, and combined techniques that include a simple linear combination and weighted averages, with a brief discussion of the application of profile likelihood, maximum likelihood, and machine learning. Comparing results for electron recoils (beta and gamma interactions) and nuclear recoils (primarily from neutrons) from the Noble Element Simulation Technique (NEST) simulation to available data, we confirm that combining all available information generates higher-precision means, lower widths (energy resolution), and more symmetric shapes (approximately Gaussian) especially at keV-scale energies, with the symmetry even greater when thresholding is addressed. Near thresholds, bias from upward fluctuations matters. For MeV-GeV scales, if only one channel is utilized, an ionization-only-based energy scale outperforms scintillation; channel combination remains beneficial. We discuss here what major collaborations use.

Dark matter direct detection based on liquid xenon

2011 ◽  
Vol 41 (12) ◽  
pp. 1414-1422
Author(s):  
YueHuan WEI ◽  
KaiXuan NI
Keyword(s):  
Dark Matter ◽  
Direct Detection ◽  
Liquid Xenon

PandaX: A deep underground dark matter search experiment in China using liquid xenon

2018 ◽  
Vol 33 (30) ◽  
pp. 1830013 ◽  
Author(s):  
Li Zhao ◽  
Jianglai Liu
Keyword(s):  
Dark Matter ◽  
Direct Detection ◽  
Underground Laboratory ◽  
Liquid Xenon ◽  
Detection Experiment ◽  
Dark Matter Search ◽  
The Future ◽  
Search Experiment ◽  
Deep Underground ◽  
Scientific Results

The nature of dark matter is one of the most fundamental scientific unknowns. Particle physicists have spent decades searching for evidence of dark matter particles. The PandaX project is a staged xenon-based dark matter direct detection experiment located at the China Jinping Underground Laboratory. In this paper, we give an overview of the PandaX experiment, discuss its recent scientific results, and outline the plan for the future.

scholarly journals Interplay and characterization of Dark Matter searches at colliders and in direct detection experiments

2015 ◽  
Vol 9-10 ◽  
pp. 51-58 ◽  
Author(s):  
Sarah A. Malik ◽  
Christopher McCabe ◽  
Henrique Araujo ◽  
Alexander Belyaev ◽  
Céline Bœhm ◽  
...  
Keyword(s):  
Dark Matter ◽  
Direct Detection

scholarly journals Characterization of new photo-detectors for the future dark matter experiments with liquid xenon

2020 ◽  
Vol 1468 ◽  
pp. 012238
Author(s):  
Kosuke Ozaki ◽  
Shingo Kazama ◽  
Masaki Yamashita ◽  
Yoshitaka Itow ◽  
Shigetaka Moriyama
Keyword(s):  
Dark Matter ◽  
Liquid Xenon ◽  
The Future ◽  
Photo Detectors

scholarly journals The impact of inelastic self-interacting dark matter on the dark matter structure of a Milky Way halo

2020 ◽  
Author(s):  
Kun Ting Eddie Chua ◽  
Karia Dibert ◽  
Mark Vogelsberger ◽  
Jesús Zavala
Keyword(s):  
Dark Matter ◽  
High Speed ◽  
Cold Dark Matter ◽  
Milky Way ◽  
Direct Detection ◽  
Major Axis ◽  
Inelastic Collisions ◽  
Axis Ratio ◽  
Lower Velocity ◽  
The Impact

Abstract We study the effects of inelastic dark matter self-interactions on the internal structure of a simulated Milky Way (MW)-size halo. Self-interacting dark matter (SIDM) is an alternative to collisionless cold dark matter (CDM) which offers a unique solution to the problems encountered with CDM on sub-galactic scales. Although previous SIDM simulations have mainly considered elastic collisions, theoretical considerations motivate the existence of multi-state dark matter where transitions from the excited to the ground state are exothermic. In this work, we consider a self-interacting, two-state dark matter model with inelastic collisions, implemented in the Arepo code. We find that energy injection from inelastic self-interactions reduces the central density of the MW halo in a shorter timescale relative to the elastic scale, resulting in a larger core size. Inelastic collisions also isotropize the orbits, resulting in an overall lower velocity anisotropy for the inelastic MW halo. In the inner halo, the inelastic SIDM case (minor-to-major axis ratio s ≡ c/a ≈ 0.65) is more spherical than the CDM (s ≈ 0.4), but less spherical than the elastic SIDM case (s ≈ 0.75). The speed distribution f(v) of dark matter particles at the location of the Sun in the inelastic SIDM model shows a significant departure from the CDM model, with f(v) falling more steeply at high speeds. In addition, the velocity kicks imparted during inelastic collisions produce unbound high-speed particles with velocities up to 500 km s−1 throughout the halo. This implies that inelastic SIDM can potentially leave distinct signatures in direct detection experiments, relative to elastic SIDM and CDM.

scholarly journals Generalized blind spots for dark matter direct detection in the 2HDM

2020 ◽  
Vol 2020 (2) ◽  
Author(s):  
M. E. Cabrera ◽  
J. A. Casas ◽  
A. Delgado ◽  
S. Robles
Keyword(s):  
Dark Matter ◽  
Direct Detection ◽  
Blind Spots

scholarly journals Sensitivity of direct detection experiments to neutrino magnetic dipole moments

2020 ◽  
Vol 2020 (12) ◽  
Author(s):  
D. Aristizabal Sierra ◽  
R. Branada ◽  
O. G. Miranda ◽  
G. Sanchez Garcia
Keyword(s):  
Dark Matter ◽  
Magnetic Dipole ◽  
Direct Detection ◽  
Dipole Moments ◽  
Nuclear Recoil ◽  
Active Volume ◽  
Electron Recoil ◽  
Flux Measurements ◽  
Neutrino Fluxes ◽  
One Year

Abstract With large active volume sizes dark matter direct detection experiments are sensitive to solar neutrino fluxes. Nuclear recoil signals are induced by 8B neutrinos, while electron recoils are mainly generated by the pp flux. Measurements of both processes offer an opportunity to test neutrino properties at low thresholds with fairly low backgrounds. In this paper we study the sensitivity of these experiments to neutrino magnetic dipole moments assuming 1, 10 and 40 tonne active volumes (representative of XENON1T, XENONnT and DARWIN), 0.3 keV and 1 keV thresholds. We show that with nuclear recoil measurements alone a 40 tonne detector could be as competitive as Borexino, TEXONO and GEMMA, with sensitivities of order 8.0 × 10−11μB at the 90% CL after one year of data taking. Electron recoil measurements will increase sensitivities way below these values allowing to test regions not excluded by astrophysical arguments. Using electron recoil data and depending on performance, the same detector will be able to explore values down to 4.0 × 10−12μB at the 90% CL in one year of data taking. By assuming a 200-tonne liquid xenon detector operating during 10 years, we conclude that sensitivities in this type of detectors will be of order 10−12μB. Reducing statistical uncertainties may enable improving sensitivities below these values.

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