Download or read book Using MiniCLEAN and Measurements of Microphysical Material Properties in the Vacuum Ultraviolet Regime to Inform Next generation Dark Matter and Neutrino Detectors written by Christopher Pete Benson and published by . This book was released on 2018 with total page 192 pages. Available in PDF, EPUB and Kindle. Book excerpt: Many compelling pieces of indirect evidence pointing to the existence of dark matter. While a confirmed and direct signature of dark matter has yet to be observed, many theoretical models have been developed in an attempt to explain the indirect evidence and to provide phenomenological models that can be tested with targeted experiments. The WIMP is a well-motivated dark matter candidate currently being sought for by several experiments. A variety of detector technologies are utilized, including liquid noble detectors, to look for WIMP scattering as a direct signature of dark matter. The CLEAN experiment is a proposed single-phase, monolithic, large-scale liquid argon experiment designed to look for high-mass WIMPs. A liquid neon target could be exchanged with the argon target to study solar neutrinos and to test the A2 dependence of a possible dark matter signal. Before scaling up to the multi-tonne scale of the full CLEAN detector, the design philosophy and background rejection capabilities required for the next-generation project are being tested using the MiniCLEAN prototype. As of mid-2018, MiniCLEAN has been constructed at SNOLAB and is currently being filled with natural liquid argon for a dark matter run. Following a short dark matter run, MiniCLEAN will be spiked with elevated levels of 39Ar to test the scaling limits of pulse shape discrimination, the primary method for electronic background rejection. These results will inform existing experiments and the next-generation of large-scale liquid argon detectors. A good understanding of light propagation is critical for optical experiments such as CLEAN, whose event reconstruction and background rejection relies primarily on scintillation light collection. This work presents two classes of complementary results which are expected to improve the modeling of scintillation light collection in current and future neutrino and dark matter detectors. These are, first, the dependence of the scintillation light time structure (triplet lifetime) and relative light yield of gaseous argon as a function of impurity level and, second, the measurement of several parameters critical to constructing a microphysically-motivated model of tetraphenyl butadiene (TPB) wavelength shifting thin films - a technology which is commonly used in many existing and proposed liquid noble gas experiments.
Download or read book Low Temperature Detectors for Neutrinos and Dark Matter written by Klaus Pretzl and published by Springer Science & Business Media. This book was released on 2012-12-06 with total page 169 pages. Available in PDF, EPUB and Kindle. Book excerpt: For the last few years astrophysicists and elementary particle physicists have been working jointly on the following fascinating phenomena: 1. The solar neutrino puzzle and the question: What happens to the neutrinos on their way from the sun to the earth? 2. The growing evidence that our universe is filled with about 10 times more matter than is visible and the question: What is dark matter made of? 3. The supernovae explosions and the question: What do neutrinos tell us about such explosions and vice versa? The experimental investigation of these phenomena is difficult and involves unconventional techniques. These are presently under development, and bring together such seemingly disparate disciplines as astrophysics and elementary particle physics on the one hand and superconductivity and solid-state physics on the other. This book contains the proceedings of a workshop held in March 1987 at which the above subjects and their experimental investigation were discussed. The proposed experimental methods are very new. They involve frontier developments in low temperature and solid-state physics. The book should be useful to researchers and students who actively work on these subjects or plan to enter the field. It also offers the non-expert reader with some physics background a good survey of the activities in this field.
Download or read book Dark Matter Neutrinos and Our Solar System written by Nirmala Prakash and published by World Scientific. This book was released on 2013 with total page 674 pages. Available in PDF, EPUB and Kindle. Book excerpt: This book describes these issues in terms of links, between cosmology, particle and nuclear physics, as well as between cosmology, atmospheric and terrestrial physics. It studies the constituents of dark matter (classified as hot warm and cold) first in terms of their individual structures, and second, in terms of facilities available to detect these structures. Neutrinos are treated as a separate entity. The last chapter details the real-time stories about the "regions" that were not explored thus far, for lack of advanced technology. Their untold stories (which span up to 2010) are illustrated here datewise in full. The book concludes with the latest news that the Large Hadron Collider team at CERN has finally succeeded in producing 7 trillion electronic Volts of energy by creating head-on-collisions of protons and more protons (in search of God-particle).
Download or read book Determining Properties of Neutralino Dark Matter Using High energy Neutrino Events microform written by Stefan H. P. Elieff and published by National Library of Canada = Bibliothèque nationale du Canada. This book was released on 1998 with total page 162 pages. Available in PDF, EPUB and Kindle. Book excerpt:
Download or read book Using the Dark to See written by Ranjan Laha and published by . This book was released on 2014 with total page 289 pages. Available in PDF, EPUB and Kindle. Book excerpt: We discuss two important research avenues in astroparticle physics: dark matter and neutrinos. We discuss both direct and indirect detection of dark matter. We calculate the signatures of dark matter annihilation from galaxy clusters in neutri- nos. We show the constraints on dark matter annihilation from radio measurements near the Galactic Center. We consider the dark matter annihilation contribution to the isotropic diffuse gamma-ray background and show how to determine the mini- mum dark matter halo mass for a given dark matter mass and annihilation channel. Motivated by recent hints on dark matter self-interactions, we calculate the nuclear recoil spectrum from a bound state dark matter scattering with a nuclei at rest in a dark matter direct detection experiment. We discuss non-standard interactions of neutrinos and astrophysical neutrino detection in the second part of the thesis. We derive strong constraints on a light Abelian gauge boson coupling to Standard Model leptons. In light of the recent detection of high energy neutrinos in IceCube, we discuss the cascade detection of high energy astrophysical neutrinos in IceCube and point out the benefits of this detection channel. We propose a new method to detect supernova electron neutrino in gadolinium loaded Super-Kamiokande detector and show that it can be used to measure the supernova electron neutrino spectrum to ~ 20% accuracy.
Download or read book Characterizing the Peripheral Dynamics of Xenon Dark Matter Detectors written by Jacob Edward Cutter and published by . This book was released on 2020 with total page 0 pages. Available in PDF, EPUB and Kindle. Book excerpt: One of the most important fundamental problems in physics today is to understand the nature of dark matter. The landscape of explanations for observed dark matter phenomena is vast and still expanding, and an impressive number of experiments have been built to probe the dark sector of the universe. A prominent class of detectors is aimed at discovering (or excluding) a particular kind of dark matter: the Weakly Interacting Massive Particle (WIMP). Searching for this popular dark matter candidate requires an ultra-sensitive, low-background target; xenon detectors serve as such a target for dark matter interactions. The Large Underground Xenon (LUX) detector is a dual-phase xenon time-projection chamber (TPC) which was operated underground at the Homestake Mine in Lead, South Dakota from 2013 to 2016, and was able to achieve the world's leading WIMP exclusion limit. However, successful reconstruction of WIMP-nucleus scatters in such detectors requires thorough understanding of the detection medium, which is made difficult by various confounding effects near the detector walls. Field-fringing is a major component of confusion in the periphery, and the large electric field non-uniformities in Run 4 of LUX provided a significant challenge in the dark matter analysis. Here is presented an algorithm to bijectively map between reconstructed event positions and true spatial coordinates, which serves as an important tool for studying field effects and fiducialization in LUX. Additionally, a successful dark matter search must model interfering background events in the WIMP search region which can't be directly vetoed. One class of unavoidable backgrounds comes from nuclear decay chain daughters in detector materials themselves, which may produce WIMP-like signals (an effect which is amplified due to various detector effects). The Davis Xenon (DAX) test bed system and a dual-phase TPC have been assembled and operated at UC Davis to characterize these common "wall backgrounds", as well as perform other R&D studies for the next-generation LUX-ZEPLIN (LZ) experiment. The DAX TPC specifically measures the xenon response to heavy nuclei produced by custom [alpha] decay sources created using novel chemical deposition procedures. In this thesis, results will be presented for the light and charge yields of immersed localized sources of 206Pb ions in liquid xenon, as well as a method for tagging such recoil events in situ by using PIN diodes as charged particle detectors to capture the correlated [alpha] particles. We also compare our isolated 206Pb events with previous WIMP search data from LUX, and discuss the significance of 206Pb as a WIMP background. Such information is most useful to future experiments if it can improve existing background models and simulations. The Noble Element Simulation Technique (NEST) is the ultimate software package for calculating expected signal yields in xenon detectors, but is an empirical framework that relies on experimental data to inform the models. We discuss the development of current NEST v2 models, specifically the heavy nuclear recoil models, as well as our current understanding of the xenon microphysics. We also show NEST predictions for mono-energetic 206Pb recoils, and discuss how our most recent DAX 206Pb measurements may inform NEST models in future work.
Download or read book Direct Search for Dark Matter by Using Dual phase Liquid Xenon Detector and Measurement of Nuclear Recoils in Liquid Argon written by Yixiong Meng and published by . This book was released on 2015 with total page 217 pages. Available in PDF, EPUB and Kindle. Book excerpt: Cosmological and Astrophysical observations provide compelling evidences for the existence of dark matter in the universe. One class of dark matter candidates, the Weakly Interacting Massive Particles (WIMPs), has been predicted in many particle physics theories. Direct detection experiments using dual- phase liquid noble element detectors report the best sensitivities to the detection of the dark matter particles. The next generation direct detection experiments using the same technology, are actively been built and expected to give a factor of 100 improvement on the current best sensitivity. This thesis discusses the measurement of nuclear recoils in a dual-phase liquid argon detector using a bunched neutron beam generated by linear accelerator facility at accelerator laboratory in Notre Dame University. Nuclear recoils of en- ergy ranging from 10.8 keVnr to 49.9 keVnr are measured under different drift field configurations. An electric field quenching on nuclear recoils in liquid argon is dis- covered and quantified for the first time. This quenching effect is also found to be drift field and recoil energy dependent. By varying the drift field amplitude from 100 V/cm to 1000 V/cm for each nuclear recoil energy, the quenching effect are measured as a function of nuclear recoil energy and drift field amplitude. Results from this measurement is used in the direct dark matter detection experiment to calculate the final sensitivity of direct dark matter search. A separate work on the optimization of detector design for the XENON1T detector is also discussed in detail. Finite element simulation tool is used to design and optimize the electric field in XENON1T time projection chamber. As part of the design of XENON1T detector, electron transparency across metal grids of different geometrical configurations are also studied.
Download or read book Deep Underground Science and Engineering Lab written by H. Nelson and published by . This book was released on 2006 with total page pages. Available in PDF, EPUB and Kindle. Book excerpt: In this report we have described the broad and compelling range of astrophysical and cosmological evidence that defines the dark matter problem, and the WIMP hypothesis, which offers a solution rooted in applying fundamental physics to the dynamics of the early universe. The WIMP hypothesis is being vigorously pursued, with a steady march of sensitivity improvements coming both from astrophysical searches and laboratory efforts. The connections between these approaches are profound and will reveal new information from physics at the smallest scales to the origin and workings of the entire universe. Direct searches for WIMP dark matter require sensitive detectors that have immunity to electromagnetic backgrounds, and are located in deep underground laboratories to reduce the flux from fast cosmic-ray-muon-induced neutrons which is a common background to all detection methods. With US leadership in dark matter searches and detector R & D, a new national laboratory will lay the foundation of technical support and facilities for the next generation of scientists and experiments in this field, and act as magnet for international cooperation and continued US leadership. The requirements of depth, space and technical support for the laboratory are fairly generic, regardless of the approach. Current experiments and upgraded versions that run within the next few years will probe cross sections on the 10{sup -45}-10{sup -44} cm{sup 2} scale, where depths of 3000-4000 m.w.e. are sufficient to suppress the neutron background. On the longer term, greater depths on the 5000-6000 level are desirable as cross sections down to 10{sup -46} cm{sup 2} are probed, and of course, if WIMPs are discovered then building up a statistical sample free of neutron backgrounds will be essential to extracting model parameters and providing a robust solution to the dark matter problem. While most of the detector technologies are of comparable physical scale, i.e., the various liquid and solid-state detector media under consideration have comparable density, a notable exception is the low-pressure gaseous detectors. These detectors are very likely to play a critical role in establishing the galactic origin of a signal, and so it is important to design the lab with this capability in mind. For example, for a WIMP-nucleon cross section of 10{sup -43} cm{sup 2} (just below the present limit [20]), 100 of the current DRIFT-II modules of 1 m{sup 3} at 40 torr CS{sub 2} [63] would require a two-year exposure [61] to get the approximately 200 events [64] required to establish the signal's galactic origin. While detector improvements are under investigation, a simple scaling for the bottom of the MSSM region at 10{sup -46} cm{sup 2} would require a 100,000 m{sup 3} detector volume. If a factor of 10 reduction in required volume is achieved (e.g., higher pressure operation, more detailed track reconstruction, etc.) then an experimental hall of (50 m){sup 3} could accommodate the experiment. Because the WIMP-nucleon cross section is unknown, it is impossible to make a definitive statement as to the ultimate requirements for a directional gaseous dark matter detector, or any other device, for that matter. What is clear, however, is that whatever confidence one gives to specific theoretical considerations, the foregoing discussion clearly indicates the high scientific priority of, broad intellectual interest in, and expanding technical capabilities for increasing the ultimate reach of direct searches for WIMP dark matter. Upcoming experiments will advance into the low-mass Supersymmetric region and explore the most favored models in a complementary way to the LHC, and on a similar time scale. The combination of astrophysical searches and accelerator experiments stands to check the consistency of the solution to the dark matter problem and provide powerful constraints on the model parameters. Knowledge of the particle properties from laboratory measurements will help to isolate and reduce the astrophysical uncertainties, which will allow a more complete picture of the galactic halo and could eventually differentiate between, say, infall versus isothermal models of galaxy formation. The scientific landscape of dark matter, which spans particle physics, astrophysics and cosmology, is very rich and interwoven. Exploring this exciting program following an initial detection will need many observables and hence a range of capabilities for followup experiments including different targets to sort out the mass and coupling of the WIMP, and directional sensitivity to confirm its galactic origin and open the age of WIMP astronomy. Clearly, this broad and fascinating program is ideally suited to the multi-decade span of DUSEL.
Download or read book Indirect Dark Matter Search with Neutrinos in JUNO and THEIA written by David Samuel Blum and published by . This book was released on 2022 with total page pages. Available in PDF, EPUB and Kindle. Book excerpt: Extensive evidence from various astrophysical observations suggests that most of the matter in the universe is dark matter. However, the nature of dark matter is still unknown and remains one of the most prominent unanswered questions in physics today. A potential way to search for dark matter is the indirect dark matter search with neutrinos. It is based on the hypothesis that dark matter particles self-annihilate into neutrinos. This would result in a neutrino flux, which could be measured by neutrino detectors at Earth. In case of no excess signal is observed, a limit on the dark matter self-annihilation cross section can be set. The future neutrino detectors JUNO and THEIA can search for dark matter, especially for light dark matter particles with masses ranging from MeV to GeV. The search for such light dark matter particles has gained in importance in the last years as it extends the typical WIMP search to the sub-GeV mass range. In this work, the sensitivities of JUNO and THEIA to measure neutrinos from dark matter self-annihilation in the Milky Way as an excess over backgrounds are determined in detail for the first time. The work focuses on direct self-annihilation of light dark matter particles with masses ranging from 15 MeV to 100 MeV into neutrino-antineutrino pairs. The expected electron antineutrino signal measured through the inverse beta decay (IBD) reaction and all background contributions occurring in the visible energy region from 10 MeV to 100 MeV are determined for both detectors. To effectively reduce IBD-like background events of atmospheric neutrinos interacting via neutral current and of fast neutrons in JUNO, pulse shape discrimination is studied and applied in this work. THEIA would feature the separate measurement of Cherenkov and scintillation light. As a consequence, selection cuts on the ratio of measured Cherenkov to scintillation light and on the number of reconstructed Cherenkov rings are determined in this work, which can suppress atmospheric neutral current and fast neutron background events in THEIA with high efficiency. The sensitivities of JUNO and THEIA are determined using a Bayesian analysis and Markov Chain Monte Carlo sampling for dark matter masses ranging from 15 MeV to 100 MeV. JUNO will achieve the highest sensitivity for indirect dark matter search with neutrinos among existing neutrino detectors and will take a leading role in the indirect dark matter search in the upcoming years. The results of this work show for the first time that JUNO will improve the best currently existing 90 % C.L. upper limit of neutrino detectors on the dark matter self-annihilation cross section by a factor of 2 to 9 for 10 years of data taking. JUNO's potential to discover an electron antineutrino signal from dark matter self-annihilation in the Milky Way as an excess over backgrounds will be between 3 sigma and 5 sigma for most dark matter masses from 15 MeV to 100 MeV assuming an annihilation cross section that corresponds to the 90 % C.L. upper limit on the annihilation cross section of Super-K. This work moreover demonstrates that THEIA, if realized, could achieve a sensitivity comparable to JUNO.
Download or read book Detecting WIMPs Neutrinos and Axions in the Next Generation of Dark Matter Experiment written by Ciaran A. J. O'Hare and published by . This book was released on 2017 with total page pages. Available in PDF, EPUB and Kindle. Book excerpt:
Download or read book Detection of Neutrino Electromagnetic Properties and Dark Matter Via Atomic Ionization written by 吳致樑 and published by . This book was released on 2014 with total page pages. Available in PDF, EPUB and Kindle. Book excerpt:
Download or read book The Low mass Limit written by Noah Kurinsky and published by . This book was released on 2018 with total page pages. Available in PDF, EPUB and Kindle. Book excerpt: The SuperCDMS SNOLAB experiment will be a 20-kg scale Si and Ge direct dark matter detection experiment designed to probe down to 300 MeV in dark matter (DM) mass through DM-nucleus scattering and 500 keV in DM electron scattering. In order to reach these low masses with appreciable sensitivity to dark matter, it needs to achieve very low energy resolution (≤ 10 ev) for nuclear recoils in both detector materials, which will be achieved using a new detector design and operating mode, CDMS HV. This detector is designed to operate at a bias of 100V to convert charges liberated in our detector targets to into phonon energy in order to resolve individual electron-hole pairs. This has never before been achieved in a kg-scale detector. In this thesis, I cover three elements of the design of the CDMS HV detectors. I discuss the detector physics controlling how charges and phonons are generated in our detector crystals, com- paring theory to results of recent experiments carried out at Stanford. I move on to describe the operating principles of our phonon-mediated charge readout, as well as the design of the CDMS HV detector. I then describe the performance tests of early CDMS HV prototypes in conjunction with the SuperCDMS SNOLAB electronics, and discuss the path towards achieving single electron-hole pair resolving detectors at the kg-scale given the performance obtained thus far. As a result of these tests, we were able to refine our noise and sensor dynamics models, and develop new metrics for diagnosing non-ideal sources of noise to aid in reducing coupling of the external environment to our detectors. In order to study the microphysics of phonon and charge production in our target crystals, we fabricated a number of gram-scale devices with various sensor designs in order to separate sensor and environmental effects from intrinsic crystal properties. These devices provided the first successful demonstrating of using voltage to amplify charge energy by production of phonons (the Neganov-Trofimov-Luke effect) in order to resolve electron-hole pairs, and opened up a new regime of dark matter and photon science at the gram-scale that we are just beginning to explore. A first dark matter search was carried out with one of these gram-scale devices, producing world-leading limits on electron-recoiling dark matter between 0.5 and 5 MeV in dark matter mass for multiple form factors. This device achieved a phonon resolution of 10 eV, allowing a single gram-day of exposure to rival kg-days of exposure in the competing liquid-noble based electron-recoil search.
Download or read book Prospects for Detecting Dark Matter with Neutrino Telescopes in Light of Recent Results from Direct Detection Experiments written by and published by . This book was released on 2005 with total page 13 pages. Available in PDF, EPUB and Kindle. Book excerpt: Direct detection dark matter experiments, lead by the CDMS collaboration, have placed increasingly stronger constraints on the cross sections for elastic scattering of WIMPs on nucleons. These results impact the prospects for the indirect detection of dark matter using neutrino telescopes. With this in mind, we revisit the prospects for detecting neutrinos produced by the annihilation of WIMPs in the Sun. We find that the latest bounds do not seriously limit the models most accessible to next generation kilometer-scale neutrino telescopes such as IceCube. This is largely due to the fact that models with significant spin-dependent couplings to protons are the least constrained and, at the same time, the most promising because of the efficient capture of WIMPs in the Sun. We identify models where dark matter particles are beyond the reach of any planned direct detection experiments while within reach of neutrino telescopes. In summary, we find that, even when contemplating recent direct detection results, neutrino telescopes still have the opportunity to play an important as well as complementary role in the search for particle dark matter.
Download or read book A Proposal for a Ton Scale Bubble Chamber for Dark Matter Detection written by and published by . This book was released on 2010 with total page 36 pages. Available in PDF, EPUB and Kindle. Book excerpt: The nature of non-baryonic dark matter is one of the most intriguing questions for particle physics at the start of the 21st century. There is ample evidence for its existence, but almost nothing is known of its properties. WIMPs are a very appealing candidate particle and several experimental campaigns are underway around the world to search for these particles via the nuclear recoils that they should induce. The COUPP series of bubble chambers has played a significant role in the WIMP search. Through a sequence of detectors of increasing size, a number of R & D issues have arisen and been solved, and the technology has now been advanced to the point where the construction of large chambers requires a modest research effort, some development, but mostly just engineering. It is within this context that we propose to build the next COUPP detector - COUPP-500, a ton scale device to be built over the next three years at Fermilab and then deployed deep underground at SNOLAB. The primary advantages of the COUPP approach over other technologies are: (1) The ability to reject electron and gamma backgrounds by arranging the chamber thermodynamics such that these particles do not even trigger the detector. (2) The ability to suppress neutron backgrounds by having the radioactively impure detection elements far from the active volume and by using the self-shielding of a large device and the high granularity to identify multiple bubbles. (3) The ability to build large chambers cheaply and with a choice of target fluids. (4) The ability to increase the size of the chambers without changing the size or complexity of the data acquisition. (5) Sensitivity to spin-dependent and spin-independent WIMP couplings. These key advantages should enable the goal of one background event in a ton-year of exposure to be achieved. The conceptual design of COUPP-500 is scaled from the preceding devices. In many cases all that is needed is a simple scaling up of components previously used. Calibration and R & D are still needed on some aspects of the system. We know we have the ability to distinguish alpha-induced events from nuclear recoils, but we do not yet know whether the combination of material purity and rejection are good enough to run for a year with no alpha background. We also need to have more detailed measurements of the detector threshold and a better understanding of its high gamma rejection. In addition, there are important checks to make on the longevity of the detector components in the hydraulic fluid and on the chemistry of the active fluid. The 2009 PASAG report explicitly supported the construction of the COUPP-500 device in all funding scenarios. The NSF has shown similar enthusiasm. It awarded one of its DUSEL S4 grants to assist in the engineering needed to build COUPP-500. The currently estimated cost of COUPP-500 is $8M, about half the $15M-$20M price tag expected by the PASAG report for a next generation dark matter search experiment. The COUPP-500 device will have a spin independent WIMP-nucleus cross-section sensitivity of 6 x 10−47 cm2 after a background-free year of running. This device should then provide the benchmark against which all other WIMP searches are measured.
Download or read book A Search for Solar Dark Matter with the IceCube Neutrino Detector written by and published by . This book was released on 2016 with total page 189 pages. Available in PDF, EPUB and Kindle. Book excerpt:
Download or read book Report of the Solar and Atmospheric Neutrino Working Group written by and published by . This book was released on 2005 with total page pages. Available in PDF, EPUB and Kindle. Book excerpt: The highest priority of the Solar and Atmospheric Neutrino Experiment Working Group is the development of a real-time, precision experiment that measures the pp solar neutrino flux. A measurement of the pp solar neutrino flux, in comparison with the existing precision measurements of the high energy [sup 8]B neutrino flux, will demonstrate the transition between vacuum and matter-dominated oscillations, thereby quantitatively testing a fundamental prediction of the standard scenario of neutrino flavor transformation. The initial solar neutrino beam is pure [nu][sub e], which also permits sensitive tests for sterile neutrinos. The pp experiment will also permit a significantly improved determination of [theta][sub 12] and, together with other solar neutrino measurements, either a measurement of [theta][sub 13] or a constraint a factor of two lower than existing bounds. In combination with the essential pre-requisite experiments that will measure the [sup 7]Be solar neutrino flux with a precision of 5%, a measurement of the pp solar neutrino flux will constitute a sensitive test for non-standard energy generation mechanisms within the Sun. The Standard Solar Model predicts that the pp and [sup 7]Be neutrinos together constitute more than 98% of the solar neutrino flux. The comparison of the solar luminosity measured via neutrinos to that measured via photons will test for any unknown energy generation mechanisms within the nearest star. A precise measurement of the pp neutrino flux (predicted to be 92% of the total flux) will also test stringently the theory of stellar evolution since the Standard Solar Model predicts the pp flux with a theoretical uncertainty of 1%. We also find that an atmospheric neutrino experiment capable of resolving the mass hierarchy is a high priority. Atmospheric neutrino experiments may be the only alternative to very long baseline accelerator experiments as a way of resolving this fundamental question. Such an experiment could be a very large scale water Cerenkov detector, or a magnetized detector with flavor and antiflavor sensitivity. Additional priorities are nuclear physics measurements which will reduce the uncertainties in the predictions of the Standard Solar Model, and similar supporting measurements for atmospheric neutrinos (cosmic ray fluxes, magnetic fields, etc.). We note as well that the detectors for both solar and atmospheric neutrino measurements can serve as multipurpose detectors, with capabilities of discovering dark matter, relic supernova neutrinos, proton decay, or as targets for long baseline accelerator neutrino experiments.
Download or read book Low Background Science with the Next Generation SuperCDMS HV eV Dark Matter Detector written by Corey Bathurst and published by . This book was released on 2023 with total page 0 pages. Available in PDF, EPUB and Kindle. Book excerpt: limiting setting and provided a clear idea of what can be improved for dark matter-electron searches moving forward.
