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The WIMP is dead, long live the WIMP

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Flip Tanedo
Flip Tanedo

This document is a summary of a physics colloquium given by Flip Tanedo at UC Riverside on October 22, 2018 about dark matter theory. The colloquium discussed the history of the weakly interacting massive particle (WIMP) as a leading dark matter candidate, treating it as a piece of historical fiction. It described how the WIMP arose from attempts to solve problems in particle physics in the 1990s, such as the hierarchy problem, and came to predict the correct abundance of dark matter through the "WIMP miracle." However, as WIMPs have yet to be directly detected, the talk suggests it is now more productive to explore non-WIMP dark matter models.

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f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 Flip Tanedo 22 OCT 2018 UC Riverside Particle Theory T H E W I M P I S D E A D 
 LO N G L I V E T H E W I M P T O W A R D A T H E O R Y O F D A R K M A T T E R f l i p . t a n e d o @ u c r . e d u USC PHYSICS COLLOQUIUM FALL 2018 &
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 2 the plan dark matter in dark times WIMP, from the lens of historical fiction post-WIMP dark matter Learning Objectives
 What we really mean by a “WIMP”
 What we really mean by “WIMPs are dead”
 Why it’s okay to move on from WIMPs
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 3 Who discovered water? https://quoteinvestigator.com/2013/12/23/water-fish/ I don’t know. But it probably wasn’t a fish. Status of dark matter.
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 4 The first dark matter: Neptune Astronomical observations + theory → missing stuff Image: Magnus Manske via Wikipedia U. Le Verrier; hubpages.com/ education/The-Drama-of-Neptunes-Discovery
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 5 f l i p . t a n e d o @ u c r . e d u USC PHYSICS COLLOQUIUM FALL 2018 The Second Dark Matter: Vulcan
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 6 Astro + Cosmo: Dark Matter Exists 5% 27% 68% Standard Model is not complete GALACTIC 
 ROTATION CURVES GRAVITATIONAL LENSING COSMIC MICROWAVE BACKGROUND Images: Jeff Filippini (Berkeley Cosmology 2005), NASA APOD 2006, NASA WMAP This talk: new particle(s) THIS IS A CONSERVATIVE ASSUMPTION
 BUT: THERE ARE OTHER OPTIONS!
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 7 Current status via Jorge Cham & Daniel Whiteson One of the top two recent books to use comic illustrations to share what it’s like to be a physicist. … this audience already knows the other one! now in paperback!
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 Figure 27.1: WIMP cross sections (normalized to a single nucleon) for spin8 Direct Detection PDG Dark Matter Review 2018
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 9 “WIMP Dark Matter is dead” Weakly-Interacting Massive Particle (This means different things to different people!)
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 10 A model of dark matter pixabay.com/en/crime-scene-chalk-outline-29055/ g Z DA R K M AT T E R I N T E R ACT I O N Properties: spin, mass Interactions with visible matter (has to stay dark) + a reason to be stable
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 11 “Just parameter fitting, right?” PDG 2018 16 27. Dark matter Figure 27.1: WIMP cross sections (normalized to a single nucleon) for spin- independent coupling versus mass. The DAMA/LIBRA [72], and CDMS-Si enclosed areas are regions of interest from possible signal events. References to the experimental results are given in the text. For context, the black contour shows a scan of the parameter space of 4 typical SUSY models, CMSSM, NUHM1, NUHM2, pMSSM10 [73], which integrates constraints set by ATLAS Run 1. Table 26.1 summarizes the best experimental performances in terms of the upper limit on cross sections for spin independent and spin dependent couplings, at the optimized WIMP mass of each experiment. Also included are some new significant results (using Argon for example). In summary, the confused situation at low WIMP mass has largely been cleared DA R K M AT T E R mass g Z interaction strength
 (which one?)
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 12 A model of dark matter pixabay.com/en/crime-scene-chalk-outline-29055/ g Z DA R K M AT T E R I N T E R ACT I O N Properties: spin, mass Interactions with visible matter (has to stay dark) + a reason to be stable model-building required
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 13 the plan dark matter in dark times WIMP, from the lens of historical fiction post-WIMP dark matter this is historical science fiction
 A collective mis-remembering of history
 whose fiction hopefully engenders a
 deeper truth.
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 14 A useful historical starting point PHYSICS REPORTS ELSEWIER Physics Reports 267 (1996) 195-373 Supersymmetric dark matter Gerard Jungmana, Marc Kamionkowskib,“, Kim Griestd aDepartment of Physics, syyacuse University, Syracuse, NY 13244, USA. jungman@npac.syr.edu, bDepartment of Physics, Columbia University, New York, NY 10027, USA. kamion@phys.columbia.edu, ‘School of Natural Sciences, Institute for Advanced Study, Princeton, NJ 08540. USA, aDepartment of Physics, University of California, San Diego, La Jolla, CA 92093, USA. kgriest@ucsd.edu Received June 1995; editor: D.N. Schramm Contents 1. Introduction 2. Dark matter in the Universe 2.1. Inventory of dark matter 2.2. Theoretical arguments 2.3. Baryonic content of the Universe 2.4. Distribution of dark matter in the Milky 198 206 206 209 211 6.4. Fermion final states 6.5. Gluon final states 6.6. Photon final states 6.7. Summary of neutralino annihilation 7. Elastic-scattering cross sections 7.1. The basic ingredients 252 256 258 259 260 260 Caveat emptor: what follows is a piece of historical fiction
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 15 Particle Physics, 1990s / / ¯ / − / ¯ / / / −/ ¯ / − / / ( ) ( ) fundamental forces matterparticles or something to explain unitarity of WW scattering
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 16 The Hierarchy Problem Why is the Higgs light? FT, Quantum Diaries, “The Hierarchy Problem” (2012)
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 17 A favorite answer: supersymmetry matter particle force particle force particle matter particle N E W PA R T I C L E SElegant solution to hierarchy problem
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 18 Preventing Proton Decay ¯d ¯u e¯d,e¯s,e¯b 4 1 Q L ¯u ¯u by squarks. Arrows indicate helicity and should not be confu Dirac spinors [14]. Tildes indicate superpartners while bars cles into left-chiral fields in the conjugate representation. ion of this is to impose the above constrai PR = ( )3(B L)+2s , n of the field. Conservation of matter parity )2s factor always cancels in any interaction rm has an even number of fermions. Ob erpartner fields have R-parity 1. (This grams assocaited with electroweak precisi parity requires pair-production of superp PR[ ordinary matter ] = + PR[ superpartner ] = − Added bonus: the lightest superpartner is stable.
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 19 The story so far: SUSY mh ? SUSY New Particles p+ stability R-parity ? Dark Matter !
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 20 Variant: extra dimensions mh ? XD New Particles precision observables KK-parity ? Dark Matter ! free in flat XD warped XD
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 21 Variant: compositeness mh ? composite New Particles T-parity ? Dark Matter ! precision observables
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 22 SUSY Dark Matter: Neutralino WIMP g Z DA R K M AT T E R I N T E R ACT I O N spin-1/2 mass ~ 100 GeV Stable due to R-parity ~ 0.6 “ W E A K S CA L E ” “ W E A K S CA L E ” lightest superpartner combination of photon, Z, Higgs partners weak scale mass weak scale couplings
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 23 How much dark matter is there? 1 10 equilibrium time ~ mass / temp [comoving]numberdensity SM SM SM SM = … so there is no dark matter E Q U I L I B R I U M A N N I H I L AT I O N SM SM
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 24 How much dark matter is there? 1 10 equilibrium freeze out time ~ mass / temp [comoving]numberdensity SM SM H U B B L E A N N I H I L AT I O N WIMP prediction: relic abundance of dark matter [ neutralino & cousins ]
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 25 The “WIMP Miracle” capture SM SM Z “WEAK SCALE” MASS ~100 GeV WEAK FORCE annihilation vs. expansion of universe ⌦ h2 ⇠ 0.1 pb h annvi “WEAK SCALE” ANNIHILATION RATE OBSERVED AMOUNT OF DARK MATTER TODAY If dark matter interacts through electroweak (W, Z, h) bosons, then it automatically has roughly the correct abundance
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 26 The “WIMP Miracle” mh ? SUSY New Particles p+ stability R-parity ? Dark Matter with correct abundance
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 27 The “WIMP Nightmare” mh ? SUSY New Particles p+ stability R-parity ? Dark Matter with correct abundance predictions nomorefreeparameters
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 28 “WIMP Complementarity” Dark matter searches related by crossing symmetry: How Dark Matter talks to the Standard Model .. χ . χ . sm . sm .. χ . sm . χ . sm .. sm . sm . χ . χ ANNIHIL ATION DI RECT DETECTIO N COLLIDER INDIRECT DIRECT COLLIDER Standard ModelDark MatterANNIHIL ATION COLLIDER D I R E C T WEAK FORCE
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 29 “WIMP Complementarity” Dark matter searches related by crossing symmetry: How Dark Matter talks to the Standard Model .. χ . χ . sm . sm .. χ . sm . χ . sm .. sm . sm . χ . χ ANNIHIL ATION DI RECT DETECTIO N COLLIDER INDIRECT DIRECT COLLIDER Standard ModelDark MatterANNIHIL ATION COLLIDER D I R E C T WEAK FORCE R E L I C A B U N DA N C E YO U ’ R E K I L L I N G M E N OT G R E AT, E I T H E R
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 30Figure 27.1: WIMP cross sections (normalized to a single nucleon) for spin PDG Dark Matter Review 2018 weak scale coupling weak scale mass
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 31 adapted from Getty Images * neutralinos with the most natural parameter choices
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 32 Is the neutralino WIMP dead? Technically? No. Linguistically? No. Experimentally? No. Emotionally? Yes. The WIMP is dead to me. Hiding places in mass, mixing;
 many parameters, conspiracies Ambiguity in meaning of “weak”
 not necessarily electroweak if dark matter is a WIMP, we know how to find it and we’re actively searching more interesting: what if dark
 matter isn’t a WIMP at all? Experimental program is probing previously unexplored models n.b. analogous to “SUSY is dead”
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 . er talks to the Standard Model .. χ . sm . χ . sm .. sm . sm . χ . χ 33 Defining the WIMP SPECIFIC GENERAL interacts through W and Z bosons interactions with visible matter have a “small” coupling interactions with visible matter are electroweak-scale “One parameter” contact interactions many interactions, only dark-visible must be small neutralinos e.g. axions? SM singlet
 particle e.g. connected
 to naturalness(motivated) (arbitrary) “everything is a WIMP!” WIMP Miracle
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 34 the plan dark matter in dark times WIMP, from the lens of historical fiction post-WIMP dark matter Why there are still theorists working on dark matter
 light mediators as an example of a better
 phenomenological framework
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 35Andrew Grant, Science News, June 2013
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 36 Phenomenology post-2013 1. Waiting for Godot. (Ambulance chasing mode) 2. Brave New World. (Lamp post mode) top-down model building
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 37 f l i p . t a n e d o @ u c r . e d u USC PHYSICS COLLOQUIUM FALL 2018 Ambulance Chasing Mode If this is true, then dark matter must …
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 38 f l i p . t a n e d o @ u c r . e d u USC PHYSICS COLLOQUIUM FALL 2018 Image: Alex Perez, via expertphotography.com/low-key-photography-dramatic-lighting/ Lamp-Post Mode Where can we look for dark matter? Where are we not looking?
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 39 Example: Light Mediators e e e e e capture annihilation x xA0 A0 INDIRECT DIRECT COLLIDER Standard ModelMediator N N q q ANNIHIL ATION COLLIDER D I R E C T Dark Matter can keep thermal relic!
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 40 New Searches with Light Mediators e e e e ee ee e e capture annihilation A0 A0 INDIRECT DIRECT MEDIATOR PRODUCTION N N ANNIHIL ATION COLLIDERD I R E C T A0 A0 Halo Morpholo • SIDM particles follow the 0 2 4 6 8 0 2 4 6 8 R HkpcL zHkpcL constant density contours Kaplinghat, Linden, Keeley, HBY (2013) (P C d SELF Standard ModelMediatorDark Matter SM SM SM SM accelerators astro R E L I C 
 A B U N DA N C E
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 41 Step 1: Mediator Production A A0 e e A e N N A0 e EXAMPLES OF LIGHT MEDIATOR PRODUCTION STRATEGIES annihilation bremsstrahlung Others: Drell-Yan, nuclear transitions, Higgs decays, … ⇡0 = 1 p 2 u¯u d ¯d meson decay
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 42 Step 2: Mediator Decay
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 43Adapted from 1608.08632, 1608.03591, N. Toro at Dark Sectors 2017 InteractionwithStandardModel Mediator Mass A0 prompt displaced vertex LIMITED BY STATISTICS LIMITED BY VERTEXING existing bounds
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 44 Remixing dark phenomenology UNCHANGED ANNIHILATION SCATTERING PRODUCTION HALO SHAPE INDIRECT DETECTION DIRECT DETECTION COLLIDER: MISSING ENERGY NUCLEAR TRANSITIONS NEUTRON STAR HEATING COMPOSITE MEDIATOR HALO PROFILES BEAM DUMP & FIXED-TARGET CAPTURE & ENHANCED ANNIHILATION PROCESS CLASSIFICATION ANNIHILATION TO ON-SHELL MEDIATORS LIGHT MEDIATORS SOME OF MY PERSONAL INTEREST... SELF INTERACTION
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 45 Example: remixing complementarity 1 2 3 4 J. Feng, J. Smolinsky, FT 1509.07525
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 46 Recap: WIMP mh ? SUSY New Particles p+ stability R-parity ? Dark Matter with correct abundance predictions nomorefreeparameters 46 x
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 47 “WIMP is dead… to me” mh ? SUSY New Particles p+ stability R-parity ? Dark Matter with correct abundance predictions nomorefreeparameters 47 x
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 48 “WIMP is dead… to me” ? Dark Matter with correct abundance predictions 48 ?
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 49 Beyond the WIMP Dark Matter with correct abundance predictions 49 Fix couplings How’d it 
 get here? Constraints?
 Anomalies? new particlesUV theory? etc … ANNIHIL ATION COLLIDER D I R E C T Halo Morphology: Milky Way • SIDM particles follow the stellar distribution 0 2 4 6 8 0 2 4 6 8 R HkpcL zHkpcL constant density contours Correlation between the stellar distribution and the SIDM distribution pheno. theory
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 50 f l i p . t a n e d o @ u c r . e d u USC PHYSICS COLLOQUIUM FALL 2018 Image: Alex Perez, via expertphotography.com/low-key-photography-dramatic-lighting/ post-WIMP lamp posts Dark sectors (light mediator) Low-mass dark matter Macroscopic dark matter Primordial black holes Gravity is very weird … opportunities for unique
 search strategies!
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 51 Extra Slides
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 52 Renormalizable Portals Dark Matter Mediator Standard ModelU(1)’ Standard ModelHiggs Dark Matter Mediator Standard Model ⌫R Kinetic Mixing Dark Matter USEFUL BENCHMARK + variations of each portal, motivated dim-5 portals, …
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 53 What is theoretical science? gravity from missing stuff Haven’t seen it in the lab current theory of particle physics
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 54 What is theoretical science? Haven’t seen it in the lab current theory of particle physics gravity from missing stuff new particle: dark matter
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 55 What is theoretical science? A “complete” theory that includes previous knowledge & new observations previous knowledge gravity from missing stuffprediction
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 56 Theorist’s roadmap to tenure HACK full theory predictions interpretation consistency
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 57 Example of an LHC Search Krovi, Low, Zhang (1807.07972) 27TeV (15ab-1) 27TeV (1.5ab-1) 100TeV (100ab-1) 100TeV (30ab-1)27TeV (15ab-1) 27TeV (1.5ab-1) MZ'=2M χ MZ'=6αeffM χ /π 2 Darkonium territory Monojet territory 14TeV (300fb-1) 14TeV (3ab-1) Z' dijet search excl. 50 100 500 1000 20 50 100 200 500 Mχ (GeV) MZ'(GeV) αD=0.5, gq=0.1 Figure 1: Colorful curves show the future high-energy pp collider constraints on the model where 0
f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 58 17 MeV Beryllium Bump UCI IPC 1608.03591 1.03 MeV 10 keV width 18.15 MeV 138 keV width STATUS: INDEPENDENT EXP. CHECK REQUIRED

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The WIMP is dead, long live the WIMP

  • 1. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 Flip Tanedo 22 OCT 2018 UC Riverside Particle Theory T H E W I M P I S D E A D 
 LO N G L I V E T H E W I M P T O W A R D A T H E O R Y O F D A R K M A T T E R f l i p . t a n e d o @ u c r . e d u USC PHYSICS COLLOQUIUM FALL 2018 &
  • 2. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 2 the plan dark matter in dark times WIMP, from the lens of historical fiction post-WIMP dark matter Learning Objectives
 What we really mean by a “WIMP”
 What we really mean by “WIMPs are dead”
 Why it’s okay to move on from WIMPs
  • 3. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 3 Who discovered water? https://quoteinvestigator.com/2013/12/23/water-fish/ I don’t know. But it probably wasn’t a fish. Status of dark matter.
  • 4. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 4 The first dark matter: Neptune Astronomical observations + theory → missing stuff Image: Magnus Manske via Wikipedia U. Le Verrier; hubpages.com/ education/The-Drama-of-Neptunes-Discovery
  • 5. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 5 f l i p . t a n e d o @ u c r . e d u USC PHYSICS COLLOQUIUM FALL 2018 The Second Dark Matter: Vulcan
  • 6. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 6 Astro + Cosmo: Dark Matter Exists 5% 27% 68% Standard Model is not complete GALACTIC 
 ROTATION CURVES GRAVITATIONAL LENSING COSMIC MICROWAVE BACKGROUND Images: Jeff Filippini (Berkeley Cosmology 2005), NASA APOD 2006, NASA WMAP This talk: new particle(s) THIS IS A CONSERVATIVE ASSUMPTION
 BUT: THERE ARE OTHER OPTIONS!
  • 7. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 7 Current status via Jorge Cham & Daniel Whiteson One of the top two recent books to use comic illustrations to share what it’s like to be a physicist. … this audience already knows the other one! now in paperback!
  • 8. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 Figure 27.1: WIMP cross sections (normalized to a single nucleon) for spin8 Direct Detection PDG Dark Matter Review 2018
  • 9. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 9 “WIMP Dark Matter is dead” Weakly-Interacting Massive Particle (This means different things to different people!)
  • 10. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 10 A model of dark matter pixabay.com/en/crime-scene-chalk-outline-29055/ g Z DA R K M AT T E R I N T E R ACT I O N Properties: spin, mass Interactions with visible matter (has to stay dark) + a reason to be stable
  • 11. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 11 “Just parameter fitting, right?” PDG 2018 16 27. Dark matter Figure 27.1: WIMP cross sections (normalized to a single nucleon) for spin- independent coupling versus mass. The DAMA/LIBRA [72], and CDMS-Si enclosed areas are regions of interest from possible signal events. References to the experimental results are given in the text. For context, the black contour shows a scan of the parameter space of 4 typical SUSY models, CMSSM, NUHM1, NUHM2, pMSSM10 [73], which integrates constraints set by ATLAS Run 1. Table 26.1 summarizes the best experimental performances in terms of the upper limit on cross sections for spin independent and spin dependent couplings, at the optimized WIMP mass of each experiment. Also included are some new significant results (using Argon for example). In summary, the confused situation at low WIMP mass has largely been cleared DA R K M AT T E R mass g Z interaction strength
 (which one?)
  • 12. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 12 A model of dark matter pixabay.com/en/crime-scene-chalk-outline-29055/ g Z DA R K M AT T E R I N T E R ACT I O N Properties: spin, mass Interactions with visible matter (has to stay dark) + a reason to be stable model-building required
  • 13. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 13 the plan dark matter in dark times WIMP, from the lens of historical fiction post-WIMP dark matter this is historical science fiction
 A collective mis-remembering of history
 whose fiction hopefully engenders a
 deeper truth.
  • 14. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 14 A useful historical starting point PHYSICS REPORTS ELSEWIER Physics Reports 267 (1996) 195-373 Supersymmetric dark matter Gerard Jungmana, Marc Kamionkowskib,“, Kim Griestd aDepartment of Physics, syyacuse University, Syracuse, NY 13244, USA. jungman@npac.syr.edu, bDepartment of Physics, Columbia University, New York, NY 10027, USA. kamion@phys.columbia.edu, ‘School of Natural Sciences, Institute for Advanced Study, Princeton, NJ 08540. USA, aDepartment of Physics, University of California, San Diego, La Jolla, CA 92093, USA. kgriest@ucsd.edu Received June 1995; editor: D.N. Schramm Contents 1. Introduction 2. Dark matter in the Universe 2.1. Inventory of dark matter 2.2. Theoretical arguments 2.3. Baryonic content of the Universe 2.4. Distribution of dark matter in the Milky 198 206 206 209 211 6.4. Fermion final states 6.5. Gluon final states 6.6. Photon final states 6.7. Summary of neutralino annihilation 7. Elastic-scattering cross sections 7.1. The basic ingredients 252 256 258 259 260 260 Caveat emptor: what follows is a piece of historical fiction
  • 15. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 15 Particle Physics, 1990s / / ¯ / − / ¯ / / / −/ ¯ / − / / ( ) ( ) fundamental forces matterparticles or something to explain unitarity of WW scattering
  • 16. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 16 The Hierarchy Problem Why is the Higgs light? FT, Quantum Diaries, “The Hierarchy Problem” (2012)
  • 17. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 17 A favorite answer: supersymmetry matter particle force particle force particle matter particle N E W PA R T I C L E SElegant solution to hierarchy problem
  • 18. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 18 Preventing Proton Decay ¯d ¯u e¯d,e¯s,e¯b 4 1 Q L ¯u ¯u by squarks. Arrows indicate helicity and should not be confu Dirac spinors [14]. Tildes indicate superpartners while bars cles into left-chiral fields in the conjugate representation. ion of this is to impose the above constrai PR = ( )3(B L)+2s , n of the field. Conservation of matter parity )2s factor always cancels in any interaction rm has an even number of fermions. Ob erpartner fields have R-parity 1. (This grams assocaited with electroweak precisi parity requires pair-production of superp PR[ ordinary matter ] = + PR[ superpartner ] = − Added bonus: the lightest superpartner is stable.
  • 19. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 19 The story so far: SUSY mh ? SUSY New Particles p+ stability R-parity ? Dark Matter !
  • 20. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 20 Variant: extra dimensions mh ? XD New Particles precision observables KK-parity ? Dark Matter ! free in flat XD warped XD
  • 21. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 21 Variant: compositeness mh ? composite New Particles T-parity ? Dark Matter ! precision observables
  • 22. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 22 SUSY Dark Matter: Neutralino WIMP g Z DA R K M AT T E R I N T E R ACT I O N spin-1/2 mass ~ 100 GeV Stable due to R-parity ~ 0.6 “ W E A K S CA L E ” “ W E A K S CA L E ” lightest superpartner combination of photon, Z, Higgs partners weak scale mass weak scale couplings
  • 23. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 23 How much dark matter is there? 1 10 equilibrium time ~ mass / temp [comoving]numberdensity SM SM SM SM = … so there is no dark matter E Q U I L I B R I U M A N N I H I L AT I O N SM SM
  • 24. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 24 How much dark matter is there? 1 10 equilibrium freeze out time ~ mass / temp [comoving]numberdensity SM SM H U B B L E A N N I H I L AT I O N WIMP prediction: relic abundance of dark matter [ neutralino & cousins ]
  • 25. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 25 The “WIMP Miracle” capture SM SM Z “WEAK SCALE” MASS ~100 GeV WEAK FORCE annihilation vs. expansion of universe ⌦ h2 ⇠ 0.1 pb h annvi “WEAK SCALE” ANNIHILATION RATE OBSERVED AMOUNT OF DARK MATTER TODAY If dark matter interacts through electroweak (W, Z, h) bosons, then it automatically has roughly the correct abundance
  • 26. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 26 The “WIMP Miracle” mh ? SUSY New Particles p+ stability R-parity ? Dark Matter with correct abundance
  • 27. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 27 The “WIMP Nightmare” mh ? SUSY New Particles p+ stability R-parity ? Dark Matter with correct abundance predictions nomorefreeparameters
  • 28. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 28 “WIMP Complementarity” Dark matter searches related by crossing symmetry: How Dark Matter talks to the Standard Model .. χ . χ . sm . sm .. χ . sm . χ . sm .. sm . sm . χ . χ ANNIHIL ATION DI RECT DETECTIO N COLLIDER INDIRECT DIRECT COLLIDER Standard ModelDark MatterANNIHIL ATION COLLIDER D I R E C T WEAK FORCE
  • 29. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 29 “WIMP Complementarity” Dark matter searches related by crossing symmetry: How Dark Matter talks to the Standard Model .. χ . χ . sm . sm .. χ . sm . χ . sm .. sm . sm . χ . χ ANNIHIL ATION DI RECT DETECTIO N COLLIDER INDIRECT DIRECT COLLIDER Standard ModelDark MatterANNIHIL ATION COLLIDER D I R E C T WEAK FORCE R E L I C A B U N DA N C E YO U ’ R E K I L L I N G M E N OT G R E AT, E I T H E R
  • 30. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 30Figure 27.1: WIMP cross sections (normalized to a single nucleon) for spin PDG Dark Matter Review 2018 weak scale coupling weak scale mass
  • 31. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 31 adapted from Getty Images * neutralinos with the most natural parameter choices
  • 32. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 32 Is the neutralino WIMP dead? Technically? No. Linguistically? No. Experimentally? No. Emotionally? Yes. The WIMP is dead to me. Hiding places in mass, mixing;
 many parameters, conspiracies Ambiguity in meaning of “weak”
 not necessarily electroweak if dark matter is a WIMP, we know how to find it and we’re actively searching more interesting: what if dark
 matter isn’t a WIMP at all? Experimental program is probing previously unexplored models n.b. analogous to “SUSY is dead”
  • 33. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 . er talks to the Standard Model .. χ . sm . χ . sm .. sm . sm . χ . χ 33 Defining the WIMP SPECIFIC GENERAL interacts through W and Z bosons interactions with visible matter have a “small” coupling interactions with visible matter are electroweak-scale “One parameter” contact interactions many interactions, only dark-visible must be small neutralinos e.g. axions? SM singlet
 particle e.g. connected
 to naturalness(motivated) (arbitrary) “everything is a WIMP!” WIMP Miracle
  • 34. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 34 the plan dark matter in dark times WIMP, from the lens of historical fiction post-WIMP dark matter Why there are still theorists working on dark matter
 light mediators as an example of a better
 phenomenological framework
  • 35. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 35Andrew Grant, Science News, June 2013
  • 36. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 36 Phenomenology post-2013 1. Waiting for Godot. (Ambulance chasing mode) 2. Brave New World. (Lamp post mode) top-down model building
  • 37. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 37 f l i p . t a n e d o @ u c r . e d u USC PHYSICS COLLOQUIUM FALL 2018 Ambulance Chasing Mode If this is true, then dark matter must …
  • 38. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 38 f l i p . t a n e d o @ u c r . e d u USC PHYSICS COLLOQUIUM FALL 2018 Image: Alex Perez, via expertphotography.com/low-key-photography-dramatic-lighting/ Lamp-Post Mode Where can we look for dark matter? Where are we not looking?
  • 39. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 39 Example: Light Mediators e e e e e capture annihilation x xA0 A0 INDIRECT DIRECT COLLIDER Standard ModelMediator N N q q ANNIHIL ATION COLLIDER D I R E C T Dark Matter can keep thermal relic!
  • 40. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 40 New Searches with Light Mediators e e e e ee ee e e capture annihilation A0 A0 INDIRECT DIRECT MEDIATOR PRODUCTION N N ANNIHIL ATION COLLIDERD I R E C T A0 A0 Halo Morpholo • SIDM particles follow the 0 2 4 6 8 0 2 4 6 8 R HkpcL zHkpcL constant density contours Kaplinghat, Linden, Keeley, HBY (2013) (P C d SELF Standard ModelMediatorDark Matter SM SM SM SM accelerators astro R E L I C 
 A B U N DA N C E
  • 41. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 41 Step 1: Mediator Production A A0 e e A e N N A0 e EXAMPLES OF LIGHT MEDIATOR PRODUCTION STRATEGIES annihilation bremsstrahlung Others: Drell-Yan, nuclear transitions, Higgs decays, … ⇡0 = 1 p 2 u¯u d ¯d meson decay
  • 42. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 42 Step 2: Mediator Decay
  • 43. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 43Adapted from 1608.08632, 1608.03591, N. Toro at Dark Sectors 2017 InteractionwithStandardModel Mediator Mass A0 prompt displaced vertex LIMITED BY STATISTICS LIMITED BY VERTEXING existing bounds
  • 44. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 44 Remixing dark phenomenology UNCHANGED ANNIHILATION SCATTERING PRODUCTION HALO SHAPE INDIRECT DETECTION DIRECT DETECTION COLLIDER: MISSING ENERGY NUCLEAR TRANSITIONS NEUTRON STAR HEATING COMPOSITE MEDIATOR HALO PROFILES BEAM DUMP & FIXED-TARGET CAPTURE & ENHANCED ANNIHILATION PROCESS CLASSIFICATION ANNIHILATION TO ON-SHELL MEDIATORS LIGHT MEDIATORS SOME OF MY PERSONAL INTEREST... SELF INTERACTION
  • 45. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 45 Example: remixing complementarity 1 2 3 4 J. Feng, J. Smolinsky, FT 1509.07525
  • 46. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 46 Recap: WIMP mh ? SUSY New Particles p+ stability R-parity ? Dark Matter with correct abundance predictions nomorefreeparameters 46 x
  • 47. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 47 “WIMP is dead… to me” mh ? SUSY New Particles p+ stability R-parity ? Dark Matter with correct abundance predictions nomorefreeparameters 47 x
  • 48. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 48 “WIMP is dead… to me” ? Dark Matter with correct abundance predictions 48 ?
  • 49. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 49 Beyond the WIMP Dark Matter with correct abundance predictions 49 Fix couplings How’d it 
 get here? Constraints?
 Anomalies? new particlesUV theory? etc … ANNIHIL ATION COLLIDER D I R E C T Halo Morphology: Milky Way • SIDM particles follow the stellar distribution 0 2 4 6 8 0 2 4 6 8 R HkpcL zHkpcL constant density contours Correlation between the stellar distribution and the SIDM distribution pheno. theory
  • 50. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 50 f l i p . t a n e d o @ u c r . e d u USC PHYSICS COLLOQUIUM FALL 2018 Image: Alex Perez, via expertphotography.com/low-key-photography-dramatic-lighting/ post-WIMP lamp posts Dark sectors (light mediator) Low-mass dark matter Macroscopic dark matter Primordial black holes Gravity is very weird … opportunities for unique
 search strategies!
  • 51. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 51 Extra Slides
  • 52. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 52 Renormalizable Portals Dark Matter Mediator Standard ModelU(1)’ Standard ModelHiggs Dark Matter Mediator Standard Model ⌫R Kinetic Mixing Dark Matter USEFUL BENCHMARK + variations of each portal, motivated dim-5 portals, …
  • 53. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 53 What is theoretical science? gravity from missing stuff Haven’t seen it in the lab current theory of particle physics
  • 54. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 54 What is theoretical science? Haven’t seen it in the lab current theory of particle physics gravity from missing stuff new particle: dark matter
  • 55. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 55 What is theoretical science? A “complete” theory that includes previous knowledge & new observations previous knowledge gravity from missing stuffprediction
  • 56. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 56 Theorist’s roadmap to tenure HACK full theory predictions interpretation consistency
  • 57. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 57 Example of an LHC Search Krovi, Low, Zhang (1807.07972) 27TeV (15ab-1) 27TeV (1.5ab-1) 100TeV (100ab-1) 100TeV (30ab-1)27TeV (15ab-1) 27TeV (1.5ab-1) MZ'=2M χ MZ'=6αeffM χ /π 2 Darkonium territory Monojet territory 14TeV (300fb-1) 14TeV (3ab-1) Z' dijet search excl. 50 100 500 1000 20 50 100 200 500 Mχ (GeV) MZ'(GeV) αD=0.5, gq=0.1 Figure 1: Colorful curves show the future high-energy pp collider constraints on the model where 0
  • 58. f l i p . t a n e d o @ u c r . e d u 50USC PHYSICS COLLOQUIUM FALL 2018 58 17 MeV Beryllium Bump UCI IPC 1608.03591 1.03 MeV 10 keV width 18.15 MeV 138 keV width STATUS: INDEPENDENT EXP. CHECK REQUIRED