Supersymmetric Dark Matter Candidates in Light of Constraints from Collider and Astroparticle Observables
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Report of the Supersymmetry Theory Subgroup
Report of the Supersymmetry Theory Subgroup J. Amundson (Wisconsin), G. Anderson (FNAL), H. Baer (FSU), J. Bagger (Johns Hopkins), R.M. Barnett (LBNL), C.H. Chen (UC Davis), G. Cleaver (OSU), B. Dobrescu (BU), M. Drees (Wisconsin), J.F. Gunion (UC Davis), G.L. Kane (Michigan), B. Kayser (NSF), C. Kolda (IAS), J. Lykken (FNAL), S.P. Martin (Michigan), T. Moroi (LBNL), S. Mrenna (Argonne), M. Nojiri (KEK), D. Pierce (SLAC), X. Tata (Hawaii), S. Thomas (SLAC), J.D. Wells (SLAC), B. Wright (North Carolina), Y. Yamada (Wisconsin) ABSTRACT Spacetime supersymmetry appears to be a fundamental in- gredient of superstring theory. We provide a mini-guide to some of the possible manifesta- tions of weak-scale supersymmetry. For each of six scenarios These motivations say nothing about the scale at which nature we provide might be supersymmetric. Indeed, there are additional motiva- tions for weak-scale supersymmetry. a brief description of the theoretical underpinnings, Incorporation of supersymmetry into the SM leads to a so- the adjustable parameters, lution of the gauge hierarchy problem. Namely, quadratic divergences in loop corrections to the Higgs boson mass a qualitative description of the associated phenomenology at future colliders, will cancel between fermionic and bosonic loops. This mechanism works only if the superpartner particle masses comments on how to simulate each scenario with existing are roughly of order or less than the weak scale. event generators. There exists an experimental hint: the three gauge cou- plings can unify at the Grand Uni®cation scale if there ex- I. INTRODUCTION ist weak-scale supersymmetric particles, with a desert be- The Standard Model (SM) is a theory of spin- 1 matter tween the weak scale and the GUT scale. -
Dark Energy and Dark Matter As Inertial Effects Introduction
Dark Energy and Dark Matter as Inertial Effects Serkan Zorba Department of Physics and Astronomy, Whittier College 13406 Philadelphia Street, Whittier, CA 90608 [email protected] ABSTRACT A disk-shaped universe (encompassing the observable universe) rotating globally with an angular speed equal to the Hubble constant is postulated. It is shown that dark energy and dark matter are cosmic inertial effects resulting from such a cosmic rotation, corresponding to centrifugal (dark energy), and a combination of centrifugal and the Coriolis forces (dark matter), respectively. The physics and the cosmological and galactic parameters obtained from the model closely match those attributed to dark energy and dark matter in the standard Λ-CDM model. 20 Oct 2012 Oct 20 ph] - PACS: 95.36.+x, 95.35.+d, 98.80.-k, 04.20.Cv [physics.gen Introduction The two most outstanding unsolved problems of modern cosmology today are the problems of dark energy and dark matter. Together these two problems imply that about a whopping 96% of the energy content of the universe is simply unaccounted for within the reigning paradigm of modern cosmology. arXiv:1210.3021 The dark energy problem has been around only for about two decades, while the dark matter problem has gone unsolved for about 90 years. Various ideas have been put forward, including some fantastic ones such as the presence of ghostly fields and particles. Some ideas even suggest the breakdown of the standard Newton-Einstein gravity for the relevant scales. Although some progress has been made, particularly in the area of dark matter with the nonstandard gravity theories, the problems still stand unresolved. -
Dark Matter and the Early Universe: a Review Arxiv:2104.11488V1 [Hep-Ph
Dark matter and the early Universe: a review A. Arbey and F. Mahmoudi Univ Lyon, Univ Claude Bernard Lyon 1, CNRS/IN2P3, Institut de Physique des 2 Infinis de Lyon, UMR 5822, 69622 Villeurbanne, France Theoretical Physics Department, CERN, CH-1211 Geneva 23, Switzerland Institut Universitaire de France, 103 boulevard Saint-Michel, 75005 Paris, France Abstract Dark matter represents currently an outstanding problem in both cosmology and particle physics. In this review we discuss the possible explanations for dark matter and the experimental observables which can eventually lead to the discovery of dark matter and its nature, and demonstrate the close interplay between the cosmological properties of the early Universe and the observables used to constrain dark matter models in the context of new physics beyond the Standard Model. arXiv:2104.11488v1 [hep-ph] 23 Apr 2021 1 Contents 1 Introduction 3 2 Standard Cosmological Model 3 2.1 Friedmann-Lema^ıtre-Robertson-Walker model . 4 2.2 A quick story of the Universe . 5 2.3 Big-Bang nucleosynthesis . 8 3 Dark matter(s) 9 3.1 Observational evidences . 9 3.1.1 Galaxies . 9 3.1.2 Galaxy clusters . 10 3.1.3 Large and cosmological scales . 12 3.2 Generic types of dark matter . 14 4 Beyond the standard cosmological model 16 4.1 Dark energy . 17 4.2 Inflation and reheating . 19 4.3 Other models . 20 4.4 Phase transitions . 21 5 Dark matter in particle physics 21 5.1 Dark matter and new physics . 22 5.1.1 Thermal relics . 22 5.1.2 Non-thermal relics . -
Letter of Interest Cosmic Probes of Ultra-Light Axion Dark Matter
Snowmass2021 - Letter of Interest Cosmic probes of ultra-light axion dark matter Thematic Areas: (check all that apply /) (CF1) Dark Matter: Particle Like (CF2) Dark Matter: Wavelike (CF3) Dark Matter: Cosmic Probes (CF4) Dark Energy and Cosmic Acceleration: The Modern Universe (CF5) Dark Energy and Cosmic Acceleration: Cosmic Dawn and Before (CF6) Dark Energy and Cosmic Acceleration: Complementarity of Probes and New Facilities (CF7) Cosmic Probes of Fundamental Physics (TF09) Astro-particle physics and cosmology Contact Information: Name (Institution) [email]: Keir K. Rogers (Oskar Klein Centre for Cosmoparticle Physics, Stockholm University; Dunlap Institute, University of Toronto) [ [email protected]] Authors: Simeon Bird (UC Riverside), Simon Birrer (Stanford University), Djuna Croon (TRIUMF), Alex Drlica-Wagner (Fermilab, University of Chicago), Jeff A. Dror (UC Berkeley, Lawrence Berkeley National Laboratory), Daniel Grin (Haverford College), David J. E. Marsh (Georg-August University Goettingen), Philip Mocz (Princeton), Ethan Nadler (Stanford), Chanda Prescod-Weinstein (University of New Hamp- shire), Keir K. Rogers (Oskar Klein Centre for Cosmoparticle Physics, Stockholm University; Dunlap Insti- tute, University of Toronto), Katelin Schutz (MIT), Neelima Sehgal (Stony Brook University), Yu-Dai Tsai (Fermilab), Tien-Tien Yu (University of Oregon), Yimin Zhong (University of Chicago). Abstract: Ultra-light axions are a compelling dark matter candidate, motivated by the string axiverse, the strong CP problem in QCD, and possible tensions in the CDM model. They are hard to probe experimentally, and so cosmological/astrophysical observations are very sensitive to the distinctive gravitational phenomena of ULA dark matter. There is the prospect of probing fifteen orders of magnitude in mass, often down to sub-percent contributions to the DM in the next ten to twenty years. -
Effective Description of Dark Matter As a Viscous Fluid
Motivation Framework Perturbation theory Effective viscosity Results FRG improvement Conclusions Effective Description of Dark Matter as a Viscous Fluid Nikolaos Tetradis University of Athens Work with: D. Blas, S. Floerchinger, M. Garny, U. Wiedemann . N. Tetradis University of Athens Effective Description of Dark Matter as a Viscous Fluid Motivation Framework Perturbation theory Effective viscosity Results FRG improvement Conclusions Distribution of dark and baryonic matter in the Universe Figure: 2MASS Galaxy Catalog (more than 1.5 million galaxies). N. Tetradis University of Athens Effective Description of Dark Matter as a Viscous Fluid Motivation Framework Perturbation theory Effective viscosity Results FRG improvement Conclusions Inhomogeneities Inhomogeneities are treated as perturbations on top of an expanding homogeneous background. Under gravitational attraction, the matter overdensities grow and produce the observed large-scale structure. The distribution of matter at various redshifts reflects the detailed structure of the cosmological model. Define the density field δ = δρ/ρ0 and its spectrum hδ(k)δ(q)i ≡ δD(k + q)P(k): . N. Tetradis University of Athens Effective Description of Dark Matter as a Viscous Fluid 31 timation method in its entirety, but it should be equally valid. 7.3. Comparison to other results Figure 35 compares our results from Table 3 (modeling approach) with other measurements from galaxy surveys, but must be interpreted with care. The UZC points may contain excess large-scale power due to selection function effects (Padmanabhan et al. 2000; THX02), and the an- gular SDSS points measured from the early data release sample are difficult to interpret because of their extremely broad window functions. -
Supersymmetry Breaking and Inflation from Higher Curvature
Prepared for submission to JHEP Supersymmetry Breaking and Inflation from Higher Curvature Supergravity I. Dalianisa, F. Farakosb, A. Kehagiasa;c, A. Riottoc and R. von Ungeb aPhysics Division, National Technical University of Athens, 15780 Zografou Campus, Athens, Greece bInstitute for Theoretical Physics, Masaryk University, 611 37 Brno, Czech Republic cDepartment of Theoretical Physics and Center for Astroparticle Physics (CAP) 24 quai E. Ansermet, CH-1211 Geneva 4, Switzerland E-mail: [email protected], [email protected], [email protected], [email protected], [email protected] Abstract: The generic embedding of the R + R2 higher curvature theory into old- minimal supergravity leads to models with rich vacuum structure in addition to its well-known inflationary properties. When the model enjoys an exact R-symmetry, there is an inflationary phase with a single supersymmetric Minkowski vacuum. This appears to be a special case of a more generic set-up, which in principle may include R- symmetry violating terms which are still of pure supergravity origin. By including the latter terms, we find new supersymmetry breaking vacua compatible with single-field inflationary trajectories. We discuss explicitly two such models and we illustrate how arXiv:1409.8299v2 [hep-th] 22 Jan 2015 the inflaton is driven towards the supersymmetry breaking vacuum after the inflationary phase. In these models the gravitino mass is of the same order as the inflaton mass. Therefore, pure higher curvature supergravity may not only accommodate the proper inflaton field, but it may also provide the appropriate hidden sector for supersymmetry breaking after inflation has ended. -
TASI 2008 Lectures: Introduction to Supersymmetry And
TASI 2008 Lectures: Introduction to Supersymmetry and Supersymmetry Breaking Yuri Shirman Department of Physics and Astronomy University of California, Irvine, CA 92697. [email protected] Abstract These lectures, presented at TASI 08 school, provide an introduction to supersymmetry and supersymmetry breaking. We present basic formalism of supersymmetry, super- symmetric non-renormalization theorems, and summarize non-perturbative dynamics of supersymmetric QCD. We then turn to discussion of tree level, non-perturbative, and metastable supersymmetry breaking. We introduce Minimal Supersymmetric Standard Model and discuss soft parameters in the Lagrangian. Finally we discuss several mech- anisms for communicating the supersymmetry breaking between the hidden and visible sectors. arXiv:0907.0039v1 [hep-ph] 1 Jul 2009 Contents 1 Introduction 2 1.1 Motivation..................................... 2 1.2 Weylfermions................................... 4 1.3 Afirstlookatsupersymmetry . .. 5 2 Constructing supersymmetric Lagrangians 6 2.1 Wess-ZuminoModel ............................... 6 2.2 Superfieldformalism .............................. 8 2.3 VectorSuperfield ................................. 12 2.4 Supersymmetric U(1)gaugetheory ....................... 13 2.5 Non-abeliangaugetheory . .. 15 3 Non-renormalization theorems 16 3.1 R-symmetry.................................... 17 3.2 Superpotentialterms . .. .. .. 17 3.3 Gaugecouplingrenormalization . ..... 19 3.4 D-termrenormalization. ... 20 4 Non-perturbative dynamics in SUSY QCD 20 4.1 Affleck-Dine-Seiberg -
Pandax-II ! 2015.4.9 Sino-French PPL, Hefei Pandax Dark Matter Search Program
Jinping Mountain WIMPs PandaX Dark Matter Search with Liquid Xenon at Jinping Kaixuan Ni! (on behalf of the PandaX Collaboration)! Shanghai Jiao Tong University! from PandaX-I to PandaX-II ! 2015.4.9 Sino-French PPL, Hefei PandaX dark matter search program ❖ 2009.3 SJTU group visited Jinping for the first time! ❖ 2009.4 Proposals submitted for dark matter search with liquid xenon at Jinping! ❖ 2010.1 PandaX collaboration formed, funding supported by SJTU/MOST/NSFC, started to develop the PandaX-I detector at SJTU! ❖ 2012.8 PandaX-I detector moved to CJPL! ❖ 2012.9-2013.9 Two engineering runs carried out for system integration! ❖ 2014.3 Detector fully functional for data taking! ❖ 2014.8 PandaX-I first results (17 days) published! ❖ 2014.11 Another 63 days dark matter data were collected! ❖ 2015 Upgrading from PandaX-I (125-kg) to PandaX-II (500-kg) PandaX Collaboration for Dark Matter Search Shanghai Jiao Tong University! Shanghai Institute of Applied Physics, CAS! Shandong University! University of Maryland! University of Michigan! Peking University! http://pandax.org/ Yalong River Hydropower Development Co.! China Institute of Atomic Energy (new group joined 2015) Why Liquid Xenon? • Ultra-low background: using self-shielding with 3D fiducialization and ER/NR discrimination • Sensitive to both heavy and light dark matter • Sensitive to both Spin-independent and Spin-dependent (129Xe,131Xe) • Ultra-pure Xe target: xenon gas can be purified with sub-ppb (O2 etc.) and sub-ppt (Kr) impurities • Multi-ton target achievable: with reasonable cost ($1.5M/ton) and relative simple cryogenics (165K) Two-phase xenon for dark matter searches WIMPs/Neutrons. -
CP Violation Beyond the Standard Model*
INSTITUTE OF PHYSICS PUBLISHING JOURNAL OF PHYSICS G: NUCLEAR AND PARTICLE PHYSICS J. Phys. G: Nucl. Part. Phys. 28 (2002) 345–358 PII: S0954-3899(02)30104-X CP violation beyond the standard model* GLKane1 and D D Doyle2 1 Randall Physics Laboratory, University of Michigan, Ann Arbor, MI 48109, USA 2 CPES, University of Sussex, Falmer, Brighton BN1 9QJ, UK E-mail: [email protected] Received 25 October 2001 Published 21 January 2002 Online at stacks.iop.org/JPhysG/28/345 Abstract In this paper a number of broad issues are raised about the origins of CP violation and how to test the ideas. 1. Introduction The fundamental sources of CP violation in theories of physics beyond the standard model is an important issue which has not been sufficiently studied. In this paper, we begin by discussing the possible origins of CP violation in string theory and the potential influence of its phenomenology on string theory. This naturally develops into a consideration of supersymmetry breaking, specifically the soft-breaking supersymmetric Lagrangian, Lsoft. There exist two extreme scenarios which may realistically accommodate CP violation; the first involves small soft phases and a large CKM phase, δCKM, whereas the second contains large soft phases and small δCKM. We argue that there is reasonable motivation for δCKM to be almost zero and that the latter scenario should be taken seriously. Consequently, it is appropriate to consider what CP violating mechanisms could allow for large soft phases, and hence measurements of these soft phases (which can be deduced from collider results, mixings and decays, experiments exploring the Higgs sector or from electric dipole moment values) provide some interesting phenomenological implications for physics beyond the standard model. -
Atomic Electric Dipole Moments and Cp Violation
261 ATOMIC ELECTRIC DIPOLE MOMENTS AND CP VIOLATION S.M.Barr Bartol Research Institute University of Delaware Newark, DE 19716 USA Abstract The subject of atomic electric dipole moments, the rapid recent progress in searching for them, and their significance for fundamental issues in particle theory is surveyed. particular it is shown how the edms of different kinds of atoms and molecules, as well Inas of the neutron, give vital information on the nature and origin of CP violation. Special stress is laid on supersymmetric theories and their consequences. 262 I. INTRODUCTION In this talk I am going to discuss atomic and molecular electric dipole moments (edms) from a particle theorist's point of view. The first and fundamental point is that permanent electric dipole moments violate both P and T. If we assume, as we are entitled to do, that OPT is conserved then we may speak equivalently of T-violation and OP-violation. I will mostly use the latter designation. That a permanent edm violates T is easily shown. Consider a proton. It has a magnetic dipole moment oriented along its spin axis. Suppose it also has an electric edm oriented, say, parallel to the magnetic dipole. Under T the electric dipole is not changed, as the spatial charge distribution is unaffected. But the magnetic dipole changes sign because current flows are reversed by T. Thus T takes a proton with parallel electric and magnetic dipoles into one with antiparallel moments. Now, if T is assumed to be an exact symmetry these two experimentally distinguishable kinds of proton will have the same mass. -
Modified Newtonian Dynamics
J. Astrophys. Astr. (December 2017) 38:59 © Indian Academy of Sciences https://doi.org/10.1007/s12036-017-9479-0 Modified Newtonian Dynamics (MOND) as a Modification of Newtonian Inertia MOHAMMED ALZAIN Department of Physics, Omdurman Islamic University, Omdurman, Sudan. E-mail: [email protected] MS received 2 February 2017; accepted 14 July 2017; published online 31 October 2017 Abstract. We present a modified inertia formulation of Modified Newtonian dynamics (MOND) without retaining Galilean invariance. Assuming that the existence of a universal upper bound, predicted by MOND, to the acceleration produced by a dark halo is equivalent to a violation of the hypothesis of locality (which states that an accelerated observer is pointwise inertial), we demonstrate that Milgrom’s law is invariant under a new space–time coordinate transformation. In light of the new coordinate symmetry, we address the deficiency of MOND in resolving the mass discrepancy problem in clusters of galaxies. Keywords. Dark matter—modified dynamics—Lorentz invariance 1. Introduction the upper bound is inferred by writing the excess (halo) acceleration as a function of the MOND acceleration, The modified Newtonian dynamics (MOND) paradigm g (g) = g − g = g − gμ(g/a ). (2) posits that the observations attributed to the presence D N 0 of dark matter can be explained and empirically uni- It seems from the behavior of the interpolating function fied as a modification of Newtonian dynamics when the as dictated by Milgrom’s formula (Brada & Milgrom gravitational acceleration falls below a constant value 1999) that the acceleration equation (2) is universally −10 −2 of a0 10 ms . -
SUSY Phenomenology Circa 2020
SUSY phenomenology circa 2020 Howie Baer (baer at ou dot edu), Pheno2020 University of Oklahoma May 4, 2020 m(higgs) finetuned in SM for cuto↵ m(weak) • 120 cosmological constant 10− expected • 10 ✓¯ 10− (strong CP/QCD) • ⇠ ``The appearance of fine- tuning in a scientific theory is like a cry of distress from nature, complaining that something needs to be better explained’’ virtual Pitt PACC meeting 1 SUSY phenomenology of 20th century mediation: gravity (mSUGRA/CMSSM), gauge, anomaly • naturalness: sparticles 100 GeV scale • ⇠ dark matter: WIMP/neutralino via stau-co, A-funnel or FP • 2 21 century experiments meet 20th century theory m = 125.18 0.16 GeV • h ± m > 2.1 TeV • g˜ m˜ > 1.1 TeV • t1 no sign of WIMPs (via DD) • These values/limits lead to impression that Weak Scale SUSY largely excluded except for few remote regions of p-space 3 21 century physics 1. discrete R-symmetries: mu-problem,p-decay, R-parity, gravity-safe global PQ symmetry 2. naturalness: BG, HS, EW 3. DM: need axion for strong CP, SUSY mu-problem: mainly DFSZ axion plus higgsino-like WIMP 4. string landscape: solves CC problem, role in hierarchy problem? Yes 4 SUSY mu problem: The SUSY preserving mu-parameter is usually tuned within spectrum calculator computer codes and otherwise ignored. But more basically, it should be ~m(Planck), or else in string theory=0 (no arbitrary mass scales) But: phenomenologically, need mu~m(weak)~100-300 GeV (practical naturalness: independent contributions to observables should be of order of or less than the measured value).