Neutralino Dark Matter Detection in Split Supersymmetry Scenarios
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PHY323:Lecture 11 SUSY and UED
PHY323:Lecture 11 SUSY and UED •Higgs and Supersymmetry •The Neutralino •Extra Dimensions •How WIMPs interact Candidates for Dark Matter III The New Particle Zoo Here are a few of the candidates on a plot showing cross section vs. mass. An enormous range. We will focus on WIMPs thanks to L. Roszkowski (Sheffield) Freeze Out of Thermal DM Particles WIMP Candidate 1 Supersymmetric Dark Matter Each particle gets a “sparticle” counterpart. Bosons get fermions and vice versa. e.g. Photon Photino W Wino Z Zino etc The Lightest Supersymmetric Particle (LSP) is predicted to be stable. This is called the NEUTRALINO. Supersymmetry Theory What we are aiming to do, e.g.: At higher energies, where symmetries are unbroken, you might expect a unified theory should have a single coupling constant Supersymmetry Theory and the Higgs To make things simpler, it would be nice if all the forces of nature were unified under the same theoretical framework. The energy at which this is likely called the Planck energy (1019 GeV). This was started in the 1970s - the result is the electroweak theory. The theory is intricate and complicated, partly because the photon is massless, but the W & Z are heavy. The electroweak theory posits that the very different carriers, and therefore properties, of these forces at energy scales present in nature today are actually the result of taking a much more symmteric theory at higher energies, above the ‘electroweak scale’ of 90GeV (the W and Z rest energy) and ‘spontaneously breaking’ it. The theoretical mechanism for spontaneous symmetry breaking requires yet another new particle, a spin zero particle called the HIGGS BOSON. -
CERN Courier–Digital Edition
CERNMarch/April 2021 cerncourier.com COURIERReporting on international high-energy physics WELCOME CERN Courier – digital edition Welcome to the digital edition of the March/April 2021 issue of CERN Courier. Hadron colliders have contributed to a golden era of discovery in high-energy physics, hosting experiments that have enabled physicists to unearth the cornerstones of the Standard Model. This success story began 50 years ago with CERN’s Intersecting Storage Rings (featured on the cover of this issue) and culminated in the Large Hadron Collider (p38) – which has spawned thousands of papers in its first 10 years of operations alone (p47). It also bodes well for a potential future circular collider at CERN operating at a centre-of-mass energy of at least 100 TeV, a feasibility study for which is now in full swing. Even hadron colliders have their limits, however. To explore possible new physics at the highest energy scales, physicists are mounting a series of experiments to search for very weakly interacting “slim” particles that arise from extensions in the Standard Model (p25). Also celebrating a golden anniversary this year is the Institute for Nuclear Research in Moscow (p33), while, elsewhere in this issue: quantum sensors HADRON COLLIDERS target gravitational waves (p10); X-rays go behind the scenes of supernova 50 years of discovery 1987A (p12); a high-performance computing collaboration forms to handle the big-physics data onslaught (p22); Steven Weinberg talks about his latest work (p51); and much more. To sign up to the new-issue alert, please visit: http://comms.iop.org/k/iop/cerncourier To subscribe to the magazine, please visit: https://cerncourier.com/p/about-cern-courier EDITOR: MATTHEW CHALMERS, CERN DIGITAL EDITION CREATED BY IOP PUBLISHING ATLAS spots rare Higgs decay Weinberg on effective field theory Hunting for WISPs CCMarApr21_Cover_v1.indd 1 12/02/2021 09:24 CERNCOURIER www. -
Wimps and Machos ENCYCLOPEDIA of ASTRONOMY and ASTROPHYSICS
WIMPs and MACHOs ENCYCLOPEDIA OF ASTRONOMY AND ASTROPHYSICS WIMPs and MACHOs objects that could be the dark matter and still escape detection. For example, if the Galactic halo were filled –3 . WIMP is an acronym for weakly interacting massive par- with Jupiter mass objects (10 Mo) they would not have ticle and MACHO is an acronym for massive (astrophys- been detected by emission or absorption of light. Brown . ical) compact halo object. WIMPs and MACHOs are two dwarf stars with masses below 0.08Mo or the black hole of the most popular DARK MATTER candidates. They repre- remnants of an early generation of stars would be simi- sent two very different but reasonable possibilities of larly invisible. Thus these objects are examples of what the dominant component of the universe may be. MACHOs. Other examples of this class of dark matter It is well established that somewhere between 90% candidates include primordial black holes created during and 99% of the material in the universe is in some as yet the big bang, neutron stars, white dwarf stars and vari- undiscovered form. This material is the gravitational ous exotic stable configurations of quantum fields, such glue that holds together galaxies and clusters of galaxies as non-topological solitons. and plays an important role in the history and fate of the An important difference between WIMPs and universe. Yet this material has not been directly detected. MACHOs is that WIMPs are non-baryonic and Since extensive searches have been done, this means that MACHOS are typically (but not always) formed from this mysterious material must not emit or absorb appre- baryonic material. -
Analysis and Instrumentation for a Xenon-Doped Liquid Argon System
Analysis and instrumentation for a xenon-doped liquid argon system Ryan Gibbons Work completed under the advisement of Professor Michael Gold Department of Physics and Astronomy The University of New Mexico May 27, 2020 1 Abstract Liquid argon is a scintillator frequently used in neutrino and dark matter exper- iments. In particular, is the upcoming LEGEND experiment, a neutrinoless double beta decay search, which will utilize liquid argon as an active veto system. Neutri- noless double beta decay is a theorized lepton number violating process that is only possible if neutrinos are Majorana in nature. To achieve the LEGEND background goal, the liquid argon veto must be more efficient. Past studies have shown the ad- dition of xenon in quantities of parts-per-million in liquid argon improves the light yield, and therefore efficiency, of such a system. Further work, however, is needed to fully understand the effects of this xenon doping. I present a physical model for the light intensity of xenon-doped liquid argon. This model is fitted to data from various xenon concentrations from BACoN, a liquid argon test stand. Additionally, I present preliminary work on the instrumentation of silicon photomultipliers for BACoN. 2 Contents 1 Introduction 4 1.1 Neutrinos and double beta decay . 4 1.2 LEGEND and BACoN . 5 1.3 Liquid argon . 6 2 Physical modeling of xenon-doped liquid argon 8 2.1 Model . 8 2.2 Fits to BACoN Data . 9 2.3 Analysis of Rate Constant . 12 3 Instrumentation of SiPMs 12 4 Conclusions and Future Work 13 3 1 Introduction 1.1 Neutrinos and double beta decay Neutrinos are neutral leptons that come in three flavors: electron, muon, and tao. -
Dark Energy and Dark Matter
Dark Energy and Dark Matter Jeevan Regmi Department of Physics, Prithvi Narayan Campus, Pokhara [email protected] Abstract: The new discoveries and evidences in the field of astrophysics have explored new area of discussion each day. It provides an inspiration for the search of new laws and symmetries in nature. One of the interesting issues of the decade is the accelerating universe. Though much is known about universe, still a lot of mysteries are present about it. The new concepts of dark energy and dark matter are being explained to answer the mysterious facts. However it unfolds the rays of hope for solving the various properties and dimensions of space. Keywords: dark energy, dark matter, accelerating universe, space-time curvature, cosmological constant, gravitational lensing. 1. INTRODUCTION observations. Precision measurements of the cosmic It was Albert Einstein first to realize that empty microwave background (CMB) have shown that the space is not 'nothing'. Space has amazing properties. total energy density of the universe is very near the Many of which are just beginning to be understood. critical density needed to make the universe flat The first property that Einstein discovered is that it is (i.e. the curvature of space-time, defined in General possible for more space to come into existence. And Relativity, goes to zero on large scales). Since energy his cosmological constant makes a prediction that is equivalent to mass (Special Relativity: E = mc2), empty space can possess its own energy. Theorists this is usually expressed in terms of a critical mass still don't have correct explanation for this but they density needed to make the universe flat. -
ANTIMATTER a Review of Its Role in the Universe and Its Applications
A review of its role in the ANTIMATTER universe and its applications THE DISCOVERY OF NATURE’S SYMMETRIES ntimatter plays an intrinsic role in our Aunderstanding of the subatomic world THE UNIVERSE THROUGH THE LOOKING-GLASS C.D. Anderson, Anderson, Emilio VisualSegrè Archives C.D. The beginning of the 20th century or vice versa, it absorbed or emitted saw a cascade of brilliant insights into quanta of electromagnetic radiation the nature of matter and energy. The of definite energy, giving rise to a first was Max Planck’s realisation that characteristic spectrum of bright or energy (in the form of electromagnetic dark lines at specific wavelengths. radiation i.e. light) had discrete values The Austrian physicist, Erwin – it was quantised. The second was Schrödinger laid down a more precise that energy and mass were equivalent, mathematical formulation of this as described by Einstein’s special behaviour based on wave theory and theory of relativity and his iconic probability – quantum mechanics. The first image of a positron track found in cosmic rays equation, E = mc2, where c is the The Schrödinger wave equation could speed of light in a vacuum; the theory predict the spectrum of the simplest or positron; when an electron also predicted that objects behave atom, hydrogen, which consists of met a positron, they would annihilate somewhat differently when moving a single electron orbiting a positive according to Einstein’s equation, proton. However, the spectrum generating two gamma rays in the featured additional lines that were not process. The concept of antimatter explained. In 1928, the British physicist was born. -
Neutralino Dark Matter in Supersymmetric Models with Non--Universal Scalar Mass Terms
CERN{TH 95{206 DFTT 47/95 JHU{TIPAC 95020 LNGS{95/51 GEF{Th{7/95 August 1995 Neutralino dark matter in sup ersymmetric mo dels with non{universal scalar mass terms. a b,c d e,c b,c V. Berezinsky , A. Bottino , J. Ellis ,N.Fornengo , G. Mignola f,g and S. Scop el a INFN, Laboratori Nazionali del Gran Sasso, 67010 Assergi (AQ), Italy b Dipartimento di FisicaTeorica, UniversitadiTorino, Via P. Giuria 1, 10125 Torino, Italy c INFN, Sezione di Torino, Via P. Giuria 1, 10125 Torino, Italy d Theoretical Physics Division, CERN, CH{1211 Geneva 23, Switzerland e Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, Maryland 21218, USA. f Dipartimento di Fisica, Universita di Genova, Via Dodecaneso 33, 16146 Genova, Italy g INFN, Sezione di Genova, Via Dodecaneso 33, 16146 Genova, Italy Abstract Neutralino dark matter is studied in the context of a sup ergravityscheme where the scalar mass terms are not constrained by universality conditions at the grand uni cation scale. We analyse in detail the consequences of the relaxation of this universality assumption on the sup ersymmetric parameter space, on the neutralino relic abundance and on the event rate for the direct detection of relic neutralinos. E{mail: b [email protected], b [email protected], [email protected], [email protected], [email protected], scop [email protected] 1 I. INTRODUCTION The phenomenology of neutralino dark matter has b een studied extensively in the Mini- mal Sup ersymmetric extension of the Standard Mo del (MSSM) [1]. -
Non–Baryonic Dark Matter V
Non–Baryonic Dark Matter V. Berezinsky1 , A. Bottino2,3 and G. Mignola3,4 1INFN, Laboratori Nazionali del Gran Sasso, 67010 Assergi (AQ), Italy 2Universit`a di Torino, via P. Giuria 1, I-10125 Torino, Italy 3INFN - Sezione di Torino, via P. Giuria 1, I-10125 Torino, Italy 4Theoretical Physics Division, CERN, CH–1211 Geneva 23, Switzerland (presented by V. Berezinsky) The best particle candidates for non–baryonic cold dark matter are reviewed, namely, neutralino, axion, axino and Majoron. These particles are considered in the context of cosmological models with the restrictions given by the observed mass spectrum of large scale structures, data on clusters of galaxies, age of the Universe etc. 1. Introduction (Cosmological environ- The structure formation in Universe put strong ment) restrictions to the properties of DM in Universe. Universe with HDM plus baryonic DM has a Presence of dark matter (DM) in the Universe wrong prediction for the spectrum of fluctuations is reliably established. Rotation curves in many as compared with measurements of COBE, IRAS galaxies provide evidence for large halos filled by and CfA. CDM plus baryonic matter can ex- nonluminous matter. The galaxy velocity distri- plain the spectrum of fluctuations if total density bution in clusters also show the presence of DM in Ω0 ≈ 0.3. intercluster space. IRAS and POTENT demon- There is one more form of energy density in the strate the presence of DM on the largest scale in Universe, namely the vacuum energy described the Universe. by the cosmological constant Λ. The correspond- The matter density in the Universe ρ is usually 2 ing energy density is given by ΩΛ =Λ/(3H0 ). -
Ten Years of PAMELA in Space
Ten Years of PAMELA in Space The PAMELA collaboration O. Adriani(1)(2), G. C. Barbarino(3)(4), G. A. Bazilevskaya(5), R. Bellotti(6)(7), M. Boezio(8), E. A. Bogomolov(9), M. Bongi(1)(2), V. Bonvicini(8), S. Bottai(2), A. Bruno(6)(7), F. Cafagna(7), D. Campana(4), P. Carlson(10), M. Casolino(11)(12), G. Castellini(13), C. De Santis(11), V. Di Felice(11)(14), A. M. Galper(15), A. V. Karelin(15), S. V. Koldashov(15), S. Koldobskiy(15), S. Y. Krutkov(9), A. N. Kvashnin(5), A. Leonov(15), V. Malakhov(15), L. Marcelli(11), M. Martucci(11)(16), A. G. Mayorov(15), W. Menn(17), M. Mergè(11)(16), V. V. Mikhailov(15), E. Mocchiutti(8), A. Monaco(6)(7), R. Munini(8), N. Mori(2), G. Osteria(4), B. Panico(4), P. Papini(2), M. Pearce(10), P. Picozza(11)(16), M. Ricci(18), S. B. Ricciarini(2)(13), M. Simon(17), R. Sparvoli(11)(16), P. Spillantini(1)(2), Y. I. Stozhkov(5), A. Vacchi(8)(19), E. Vannuccini(1), G. Vasilyev(9), S. A. Voronov(15), Y. T. Yurkin(15), G. Zampa(8) and N. Zampa(8) (1) University of Florence, Department of Physics, I-50019 Sesto Fiorentino, Florence, Italy (2) INFN, Sezione di Florence, I-50019 Sesto Fiorentino, Florence, Italy (3) University of Naples “Federico II”, Department of Physics, I-80126 Naples, Italy (4) INFN, Sezione di Naples, I-80126 Naples, Italy (5) Lebedev Physical Institute, RU-119991 Moscow, Russia (6) University of Bari, I-70126 Bari, Italy (7) INFN, Sezione di Bari, I-70126 Bari, Italy (8) INFN, Sezione di Trieste, I-34149 Trieste, Italy (9) Ioffe Physical Technical Institute, RU-194021 St. -
Observation of High-Energy Gamma-Rays with the Calorimetric
Louisiana State University LSU Digital Commons LSU Doctoral Dissertations Graduate School 10-22-2018 Observation of High-Energy Gamma-Rays with the Calorimetric Electron Telescope (CALET) On-board the International Space Station Nicholas Wade Cannady Louisiana State University and Agricultural and Mechanical College, [email protected] Follow this and additional works at: https://digitalcommons.lsu.edu/gradschool_dissertations Part of the Instrumentation Commons, and the Other Astrophysics and Astronomy Commons Recommended Citation Cannady, Nicholas Wade, "Observation of High-Energy Gamma-Rays with the Calorimetric Electron Telescope (CALET) On-board the International Space Station" (2018). LSU Doctoral Dissertations. 4736. https://digitalcommons.lsu.edu/gradschool_dissertations/4736 This Dissertation is brought to you for free and open access by the Graduate School at LSU Digital Commons. It has been accepted for inclusion in LSU Doctoral Dissertations by an authorized graduate school editor of LSU Digital Commons. For more information, please [email protected]. OBSERVATION OF HIGH-ENERGY GAMMA-RAYS WITH THE CALORIMETRIC ELECTRON TELESCOPE (CALET) ON-BOARD THE INTERNATIONAL SPACE STATION A Dissertation Submitted to the Graduate Faculty of the Louisiana State University and Agricultural and Mechanical College in partial fulfillment of the requirements for the degree of Doctor of Philosophy in The Department of Physics and Astronomy by Nicholas Wade Cannady B.S., Louisiana State University, 2011 December 2018 To Laura and Mom ii Acknowledgments First and foremost, I would like to thank my partner, Laura, for the constant and unconditional support that she has provided during the research described in this thesis and my studies in general. Without her, this undertaking would not have been possible. -
Rethinking “Dark Matter” Within the Epistemologically Different World (EDW) Perspective Gabriel Vacariu and Mihai Vacariu
Chapter Rethinking “Dark Matter” within the Epistemologically Different World (EDW) Perspective Gabriel Vacariu and Mihai Vacariu The really hard problems are great because we know they’ll require a crazy new idea. (Mike Turner in Panek 2011, p. 195) Abstract In the first part of the article, we show how the notion of the “universe”/“world” should be replaced with the newly postulated concept of “epistemologically different worlds” (EDWs). Consequently, we try to demonstrate that notions like “dark matter” and “dark energy” do not have a proper ontological basis: due to the correspondences between two EDWs, the macro-epistemological world (EW) (the EW of macro-entities like planets and tables) and the mega-EW or the macro– macro-EW (the EW of certain entities and processes that do not exist for the ED entities that belong to the macro-EW). Thus, we have to rethink the notions like “dark matter” and “dark energy” within the EDW perspective. We make an analogy with quantum mechanics: the “entanglement” is a process that belongs to the wave- EW, but not to the micro-EW (where those two microparticles are placed). The same principle works for explaining dark matter and dark energy: it is about entities and processes that belong to the “mega-EW,” but not to the macro-EW. The EDW perspective (2002, 2005, 2007, 2008) presupposes a new framework within which some general issues in physics should be addressed: (1) the dark matter, dark energy, and some other related issues from cosmology, (2) the main problems of quantum mechanics, (3) the relationship between Einstein’s general relativity and quantum mechanics, and so on. -
R-Parity Violation and Light Neutralinos at Ship and the LHC
BONN-TH-2015-12 R-Parity Violation and Light Neutralinos at SHiP and the LHC Jordy de Vries,1, ∗ Herbi K. Dreiner,2, y and Daniel Schmeier2, z 1Institute for Advanced Simulation, Institut f¨urKernphysik, J¨ulichCenter for Hadron Physics, Forschungszentrum J¨ulich, D-52425 J¨ulich, Germany 2Physikalisches Institut der Universit¨atBonn, Bethe Center for Theoretical Physics, Nußallee 12, 53115 Bonn, Germany We study the sensitivity of the proposed SHiP experiment to the LQD operator in R-Parity vi- olating supersymmetric theories. We focus on single neutralino production via rare meson decays and the observation of downstream neutralino decays into charged mesons inside the SHiP decay chamber. We provide a generic list of effective operators and decay width formulae for any λ0 cou- pling and show the resulting expected SHiP sensitivity for a widespread list of benchmark scenarios via numerical simulations. We compare this sensitivity to expected limits from testing the same decay topology at the LHC with ATLAS. I. INTRODUCTION method to search for a light neutralino, is via the pro- duction of mesons. The rate for the latter is so high, Supersymmetry [1{3] is the unique extension of the ex- that the subsequent rare decay of the meson to the light ternal symmetries of the Standard Model of elementary neutralino via (an) R-parity violating operator(s) can be particle physics (SM) with fermionic generators [4]. Su- searched for [26{28]. This is analogous to the production persymmetry is necessarily broken, in order to comply of neutrinos via π or K-mesons. with the bounds from experimental searches.