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UCR 2019 Colloquium

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Flip Tanedo
Flip Tanedo

The overwhelming observational evidence for the existence of dark matter is only matched by the awkward scarcity of information about what it might actually be. Laboratory searches for dark matter now appear to exclude many of the "weakly interacting massive particle" models that were favored by particle physicists for decades. Where does that leave the hunt for dark matter? If we've left the WIMP behind, what are we looking for? We give a brief, biased, and largely fictional history of the WIMP in order to establish what has and has not been excluded, and why it matters. This general-interest presentation grew out of discussions with astronomers who wanted to understand why some of their particle physics colleagues are "searching for WIMPs" while the others have decided to live in a "post-WIMP world."

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@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM WH AT EVE R H A PPE N E D TO T H E WI M P O F T O M O R R OW ? A D A R K M A T T E R P U B L I C S E R V I C E A N N O U N C E M E N T @ f l i p . t a n e d o UCR PHYSICS & ASTRO COLLOQUIUM & 21 OCTOBER 2019 FLIP TANEDO
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 2 31 October darkmatterday.com
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 3 Outline
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 4 Assumptions: dark matter exists We Have No Idea, Cham & Whiteson
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 5 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 67UCR PHYSICS & ASTRO COLLOQUIUM 6 1. Rotation Curves Rubin, Ford & Thonnard 1978 What we learn: mass fraction distribution 2. Cluster Dynamics What we learn: mass fraction distribution Zwicky 1937 3. Cluster Gas What we learn: mass fraction distribution ~90% of the luminous matter in a cluster is hot gas 4. Strong Gravitational Lensing What we learn: mass fraction distribution 5.Weak Gravitational Lensing What we learn: distribution shape structure Dietrich et al. 2016 6. Cosmological Microlensing What we learn: mass fraction smoothness Lewis & Irwin 1996 Joachim Wambsganss 7. CMB Acoustic Peaks What we learn: ratio of DM/ collisional matter thermal history Hinshaw et al. 2013 WMAP 9 SPT ACT odd-numbered peaks boosted relative to even as baryon fraction increases 8. Matter Power Spectrum What we learn: ratio of DM/ collisional matter thermal history Chabanier et al. 2019 9. Large Scale Structure What we learn: ratio of DM/ collisional matter thermal history Paul Angel, Tiamat Simulation Excellent agreement between simulations and galaxy distribution on the largest scales 10. Galaxy/Cluster Collisions What we learn: distribution separation from collisional matter self-interaction NASA/Clowe et al. 2006 Difficult to explain without collisionless matter 11. Big Bang Nucleosynthesis What we learn: amount of baryonic matter PDG 2018 Remaining mystery: lithium abundance (but still need low baryon fraction) 12. Local Stellar Motions What we learn: local dark matter density Buser 2000 Estimates: ρDM ~ 0.3 GeV/cm3 ~ 0.008 MSun/pc3 Evidence… looks like an astro talk via Katie Mack (ACP Colloquium 2019)
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 7 Present status?
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 8 ` Present status?
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 9 Outline
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 10 Weakly Interacting Massive Particle how weak? “weak” or eak?W± <latexit sha1_base64="smXTBkHfQl+094B8aAuLaVLnUvk=">AAAB7HicbVDLSgNBEOyNrxhfUY9eBoPgKeyKoMegF48R3CSQrGF2MpsMmccyMyuEJd/gxYMiXv0gb/6Nk2QPmljQUFR1090Vp5wZ6/vfXmltfWNzq7xd2dnd2z+oHh61jMo0oSFRXOlOjA3lTNLQMstpJ9UUi5jTdjy+nfntJ6oNU/LBTlIaCTyULGEEWyeF7cdeKvrVml/350CrJChIDQo0+9Wv3kCRTFBpCcfGdAM/tVGOtWWE02mllxmaYjLGQ9p1VGJBTZTPj52iM6cMUKK0K2nRXP09kWNhzETErlNgOzLL3kz8z+tmNrmOcibTzFJJFouSjCOr0OxzNGCaEssnjmCimbsVkRHWmFiXT8WFECy/vEpaF/XArwf3l7XGTRFHGU7gFM4hgCtowB00IQQCDJ7hFd486b14797HorXkFTPH8Afe5w+0eI6a</latexit><latexit sha1_base64="smXTBkHfQl+094B8aAuLaVLnUvk=">AAAB7HicbVDLSgNBEOyNrxhfUY9eBoPgKeyKoMegF48R3CSQrGF2MpsMmccyMyuEJd/gxYMiXv0gb/6Nk2QPmljQUFR1090Vp5wZ6/vfXmltfWNzq7xd2dnd2z+oHh61jMo0oSFRXOlOjA3lTNLQMstpJ9UUi5jTdjy+nfntJ6oNU/LBTlIaCTyULGEEWyeF7cdeKvrVml/350CrJChIDQo0+9Wv3kCRTFBpCcfGdAM/tVGOtWWE02mllxmaYjLGQ9p1VGJBTZTPj52iM6cMUKK0K2nRXP09kWNhzETErlNgOzLL3kz8z+tmNrmOcibTzFJJFouSjCOr0OxzNGCaEssnjmCimbsVkRHWmFiXT8WFECy/vEpaF/XArwf3l7XGTRFHGU7gFM4hgCtowB00IQQCDJ7hFd486b14797HorXkFTPH8Afe5w+0eI6a</latexit><latexit sha1_base64="smXTBkHfQl+094B8aAuLaVLnUvk=">AAAB7HicbVDLSgNBEOyNrxhfUY9eBoPgKeyKoMegF48R3CSQrGF2MpsMmccyMyuEJd/gxYMiXv0gb/6Nk2QPmljQUFR1090Vp5wZ6/vfXmltfWNzq7xd2dnd2z+oHh61jMo0oSFRXOlOjA3lTNLQMstpJ9UUi5jTdjy+nfntJ6oNU/LBTlIaCTyULGEEWyeF7cdeKvrVml/350CrJChIDQo0+9Wv3kCRTFBpCcfGdAM/tVGOtWWE02mllxmaYjLGQ9p1VGJBTZTPj52iM6cMUKK0K2nRXP09kWNhzETErlNgOzLL3kz8z+tmNrmOcibTzFJJFouSjCOr0OxzNGCaEssnjmCimbsVkRHWmFiXT8WFECy/vEpaF/XArwf3l7XGTRFHGU7gFM4hgCtowB00IQQCDJ7hFd486b14797HorXkFTPH8Afe5w+0eI6a</latexit><latexit sha1_base64="smXTBkHfQl+094B8aAuLaVLnUvk=">AAAB7HicbVDLSgNBEOyNrxhfUY9eBoPgKeyKoMegF48R3CSQrGF2MpsMmccyMyuEJd/gxYMiXv0gb/6Nk2QPmljQUFR1090Vp5wZ6/vfXmltfWNzq7xd2dnd2z+oHh61jMo0oSFRXOlOjA3lTNLQMstpJ9UUi5jTdjy+nfntJ6oNU/LBTlIaCTyULGEEWyeF7cdeKvrVml/350CrJChIDQo0+9Wv3kCRTFBpCcfGdAM/tVGOtWWE02mllxmaYjLGQ9p1VGJBTZTPj52iM6cMUKK0K2nRXP09kWNhzETErlNgOzLL3kz8z+tmNrmOcibTzFJJFouSjCOr0OxzNGCaEssnjmCimbsVkRHWmFiXT8WFECy/vEpaF/XArwf3l7XGTRFHGU7gFM4hgCtowB00IQQCDJ7hFd486b14797HorXkFTPH8Afe5w+0eI6a</latexit> interacting with what? how massive? in what regime is it particle-y?
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 11 Weakly Interacting Massive Particle electroweak interactions electroweak particles electroweak mass yeah, it’s a particle F O R T H I S TA L K : This talk: what’s the value of this definition?
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 12 Defining the WIMP Bertone & Hooper, “History of Dark Matter,” 1605.04909, RMP original WIMP: neutrinos … it turns out that they don’t work.
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 13 Outline
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 14 A historical fiction about the WIMP … an imaginary story which told the final tale of the Silver Age Superman and his long mythology … via Wikipedia 6/2019 actual history grad students should cite this
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 15 Particle Physics, circa 1990s / / ¯ / − / ¯ / / / −/ ¯ / − / / ( ) ( ) fundamental forces matterparticles or something to explain unitarity of WW scattering ?
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 16 Particle Physics From We Have No Idea, Cham and Whiteson CMS
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 17Maximilien Brice, CERN via National Geographic (May 2012)
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 18 D. Overbye, New York Times, 4 July 2012
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 19 Known Unknowns in Particle Physics Why is the Higgs boson light? Hierarchy Problem an incomplete list! (Images: We Have No Idea, Cham and Whiteson) Why is there more matter than antimatter? Baryogenesis Problem Why is ϴYM small? Strong CP Problem What is the origin of neutrino mass? … What is dark matter? Missing Mass Problem Other puzzles (possibly related to dark matter?)
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 20 The Hierarchy Problem The Higgs has a snowball’s chance in hell of being 125 GeV. FT, Quantum Diaries, “The Hierarchy Problem” (2012) (and yet here we are)
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 21 The Hierarchy Problem FT, Quantum Diaries, “The Hierarchy Problem” (2012) supersymmetry or extra dimensions, compositeness…
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 22 A favorite answer: supersymmetry matter particle force particle force particle matter particle N E W PA R T I C L E SV I S I B L E S T U F F SUSY
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 23 For the most part, it works … a little bit of model-building required.
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 24 Preventing Proton Decay: R-parity ¯d ¯u e¯d,e¯s,e¯b 4 1 Q L ¯u ¯u y squarks. Arrows indicate helicity and should not be confus rac spinors [14]. Tildes indicate superpartners while bars a les into left-chiral fields in the conjugate representation. perfield Matter parity on of this is to impose the above constrain PR = ( )3(B L)+2s , of the field. Conservation of matter parity 2s factor always cancels in any interaction m has an even number of fermions. Obs rpartner fields have R-parity 1. (This i grams assocaited with electroweak precisio parity requires pair-production of superp ns cannot occur at tree-level and must co PR[ ordinary matter ] = + PR[ superpartner ] = − Added bonus:
 lightest superpartner is stable. ?
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 25 Known Unknowns mh ? Missing Mass
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 26 The story so far: SUSY mh ? SUSY New Particles p+ stability R-parity ? Dark Matter ! Missing Mass
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 27 Weakly-Interacting Massive Particle mh ? Dark Matter ! Weak scale mass ~100 GeV
 Weak scale interaction strength GF 
 No additional parameters (roughly) Missing Mass
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 28 One thing that we do know: density Dark Matter ! Missing Mass Approx. 1 WIMP per mug of coffee ~ GeV / cm3
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 29 Weakly-Interacting Massive Particle mh ? Dark Matter ! Weak scale mass ~100 GeV
 Weak scale interaction strength GF 
 No additional parameters (roughly) Missing Mass How much dark matter do we predict?
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 30 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 67UCR PHYSICS & ASTRO COLLOQUIUM 31 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 67UCR PHYSICS & ASTRO COLLOQUIUM 32 The “WIMP Miracle” capture annihilation SM SM Z “WEAK SCALE” MASS WEAK FORCE annihilation ⌦ h2 ⇠ 0.1 pb h annvi “WEAK SCALE” ANNIHILATION RATE PRESENT ABUNDANCE automatically get the correct abundance (almost) expansion of universe
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 33 SUSY WIMP bible 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 198 206 206 209 211 211 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 7.2. Axial-vector (spin) interaction 252 256 258 259 260 260 261
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 34 The story so far: SUSY mh ? SUSY New Particles p+ stability R-parity ? Dark Matter
 with correct abundance !
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 35 extra dimensions mh ? XD New Particles precision observables KK-parity ? ! free in flat XD warped XD Dark Matter
 with correct abundance !
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 36 compositeness mh ? composite New Particles T-parity ? ! precision observables Dark Matter
 with correct abundance !
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 37 mh ? new symmetry New Particles new parity ? dangerous processes WIMP Dark Matter
 with correct abundance !
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 38 A great love story Andrew Grant, Science News, June 2013
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 39 WIMP story predictions nomorefreeparameters mh ? new symmetry New Particles new parity ? dangerous processes Dark Matter
 with correct abundance !
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 40 WIMP Complementarity χ χ χ χ χ χ ANNIHIL ATION DI RECT DETECTION COLLIDER Ωχh2 INDIRECT DIRECT COLLIDER telescopes underground high energy & abundance
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 41via LUX-LZ (kipac.stanford.edu/research/topics/direct-dark-matter-detection) Direct Detection Underground, 
 high-volume, 
 high-sensitivity. Recoil of dark matter off nuclei.
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM Figure 27.1: WIMP cross sections (normalized to a single nucleon) for spin42 Direct Detection PDG Dark Matter Review 2018
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 43Figure 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 67UCR PHYSICS & ASTRO COLLOQUIUM A great love story… and break up 44
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM χ χ χ χ χ χ ANNIHIL ATION DI RECT DETECTIO N COLLIDER INDIRECT DIRECT COLLIDER 45 WIMP Complementarity Dark matter searches related by crossing symmetry: Standard ModelDark Matter 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 67UCR PHYSICS & ASTRO COLLOQUIUM A great love story… and break up 46
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 47 Is the neutralino WIMP really dead? Technically? No. Linguistically? No. Experimentally? No. Emotionally? Yes. The WIMP is dead to me. “weak” vs “electroweak” Experimental program is robust! n.b. analogous to “SUSY is dead” ways to ‘hide’ a neutralino-esque WIMP
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 48 Seven Samurai
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 49 Recap: WIMP mh ? SUSY New Particles p+ stability R-parity ? Dark Matter with correct abundance predictions nomorefreeparameters 49
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 50 “WIMP is dead… to me” mh ? SUSY New Particles p+ stability R-parity ? Dark Matter with correct abundance predictions nomorefreeparameters 50
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 51 Outline
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 52 Known Unknowns in Particle Physics Why is the Higgs boson light? Hierarchy Problem an incomplete list! Why is there more matter than antimatter? Baryogenesis Problem Why is ϴYM small? Strong CP Problem What is the origin of neutrino mass? … What is dark matter? Missing Mass Problem Other puzzles (possibly related to dark matter?)
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 53 What can we look for? ? Dark Matter with correct abundance predictions 53 ?
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 54 The elephant in the room How did it get here? Why is it still here?
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 55 Recap: WIMP + WIMP Miracle mh ? New Particles ? ! small
 problem Dark Matter
new symmetry Why is it still here? How did it get here?
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 56 Beyond the WIMP Dark Matter with correct abundance predictions 56 Fix couplings How’d it 
 get here? Why is it still here? new particlesUV theory? pheno. theory
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 57 How do we move forward? What is the theory of dark matter? 
 Write down a bunch of [probably] wrong theories of not-WIMPS, see what we learn from them. How do we discover dark matter?
 On a budget! Using the experiments and telescopes that we have.
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 58 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 67UCR PHYSICS & ASTRO COLLOQUIUM 59 Earth capture of dark matter 1 2 3 4 J. Feng, J. Smolinsky, FT 1509.07525, 1602.01465, 1701.03168 ; A. Green, FT 1808.03700 
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 60 Holographic Dark Sectors Brax, Fichet, Tanedo 1906.02199 Costantino, Fichet, Tanedo 1910.02972 UV IR STAN AR ARSTAT S hiding in momentum-dependence
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 61 No point in looking where it’s light! Search where it’s dark! Yojimbo
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 62 Vector Self-Interacting Dark Matter I. Chaffey and FT 1907.10217 
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 63 Neutron Star Dark Matter Collider A. Joglekar, N. Raj, FT, HBY Figure 1: Illustration of contrast between fixed targets and moving targets in NS frame. Left: Heavy targets (e.g. neutrons) are fixed and have “geometric” cross section in NS frame. Right:
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 64 Dark Matter at First Light https:// www.google.com/ imgres? imgurl=https%3A %2F%2Fphysics.s https://cat.ucr.edu/ Home_files/webpage.jpg Supermassive Primordial Black Holes?
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 65 How do we move forward? What is the theory of dark matter? 
 Write down a bunch of [probably] wrong theories of not-WIMPS, see what we learn from them. How do we discover dark matter?
 On a budget! Using the experiments and telescopes that we have.
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 66 Thanks!
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 67 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 67UCR PHYSICS & ASTRO COLLOQUIUM 68 f l i p . t a n e d o @ u c r . e d u The second dark matter: Vulcan LOUISIANA PHYSICS DEPARTMENT SEMINAR
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 69 Looks like a duck, vaguely aquatic… via Dmitry Ulitin (@dm_dm) on unsplash.com; @leonello, Getty Images
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 70 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 67UCR PHYSICS & ASTRO COLLOQUIUM 71 Effects on molecules, isotopes, … UCI IPC 1608.03591 1.03 MeV 10 keV width 18.15 MeV 138 keV width STATUS: INDEPENDENT EXP. CHECK REQUIRED
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 72 Diffuse Supernova Neutrino Background Nirmal
 Raj Gopi Mohlabeng
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM χ χ χ χ 73 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 67UCR PHYSICS & ASTRO COLLOQUIUM 74 Remixing dark phenomenology
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 75 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 67UCR PHYSICS & ASTRO COLLOQUIUM 76 Step 2: Mediator Decay
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 77Adapted 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 67UCR PHYSICS & ASTRO COLLOQUIUM 78 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 MZ'=6 effM / 2 Darkonium territory Monojet territory 14TeV (300fb-1) 14TeV (3ab-1) Z' dijet search excl. 50 100 500 1000 20 50 100 200 500 M (GeV) MZ'(GeV) D=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 67UCR PHYSICS & ASTRO COLLOQUIUM 79 Dark Monopoles Work in progress with C. Kilic, M. Martone visible matter picks up small dark charge dark stuff stays dark visible magnetic charge picks up small dark magnetic monopole Kinetic Mixing: Implies: millimagnetic charge
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 80 A counterpoint arXiv:1904.02769
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 81Andrew Grant, Science News, June 2013
@ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 82 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, …

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UCR 2019 Colloquium

  • 1. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM WH AT EVE R H A PPE N E D TO T H E WI M P O F T O M O R R OW ? A D A R K M A T T E R P U B L I C S E R V I C E A N N O U N C E M E N T @ f l i p . t a n e d o UCR PHYSICS & ASTRO COLLOQUIUM & 21 OCTOBER 2019 FLIP TANEDO
  • 2. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 2 31 October darkmatterday.com
  • 3. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 3 Outline
  • 4. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 4 Assumptions: dark matter exists We Have No Idea, Cham & Whiteson
  • 5. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 5 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!
  • 6. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 6 1. Rotation Curves Rubin, Ford & Thonnard 1978 What we learn: mass fraction distribution 2. Cluster Dynamics What we learn: mass fraction distribution Zwicky 1937 3. Cluster Gas What we learn: mass fraction distribution ~90% of the luminous matter in a cluster is hot gas 4. Strong Gravitational Lensing What we learn: mass fraction distribution 5.Weak Gravitational Lensing What we learn: distribution shape structure Dietrich et al. 2016 6. Cosmological Microlensing What we learn: mass fraction smoothness Lewis & Irwin 1996 Joachim Wambsganss 7. CMB Acoustic Peaks What we learn: ratio of DM/ collisional matter thermal history Hinshaw et al. 2013 WMAP 9 SPT ACT odd-numbered peaks boosted relative to even as baryon fraction increases 8. Matter Power Spectrum What we learn: ratio of DM/ collisional matter thermal history Chabanier et al. 2019 9. Large Scale Structure What we learn: ratio of DM/ collisional matter thermal history Paul Angel, Tiamat Simulation Excellent agreement between simulations and galaxy distribution on the largest scales 10. Galaxy/Cluster Collisions What we learn: distribution separation from collisional matter self-interaction NASA/Clowe et al. 2006 Difficult to explain without collisionless matter 11. Big Bang Nucleosynthesis What we learn: amount of baryonic matter PDG 2018 Remaining mystery: lithium abundance (but still need low baryon fraction) 12. Local Stellar Motions What we learn: local dark matter density Buser 2000 Estimates: ρDM ~ 0.3 GeV/cm3 ~ 0.008 MSun/pc3 Evidence… looks like an astro talk via Katie Mack (ACP Colloquium 2019)
  • 7. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 7 Present status?
  • 8. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 8 ` Present status?
  • 9. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 9 Outline
  • 10. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 10 Weakly Interacting Massive Particle how weak? “weak” or eak?W± <latexit sha1_base64="smXTBkHfQl+094B8aAuLaVLnUvk=">AAAB7HicbVDLSgNBEOyNrxhfUY9eBoPgKeyKoMegF48R3CSQrGF2MpsMmccyMyuEJd/gxYMiXv0gb/6Nk2QPmljQUFR1090Vp5wZ6/vfXmltfWNzq7xd2dnd2z+oHh61jMo0oSFRXOlOjA3lTNLQMstpJ9UUi5jTdjy+nfntJ6oNU/LBTlIaCTyULGEEWyeF7cdeKvrVml/350CrJChIDQo0+9Wv3kCRTFBpCcfGdAM/tVGOtWWE02mllxmaYjLGQ9p1VGJBTZTPj52iM6cMUKK0K2nRXP09kWNhzETErlNgOzLL3kz8z+tmNrmOcibTzFJJFouSjCOr0OxzNGCaEssnjmCimbsVkRHWmFiXT8WFECy/vEpaF/XArwf3l7XGTRFHGU7gFM4hgCtowB00IQQCDJ7hFd486b14797HorXkFTPH8Afe5w+0eI6a</latexit><latexit sha1_base64="smXTBkHfQl+094B8aAuLaVLnUvk=">AAAB7HicbVDLSgNBEOyNrxhfUY9eBoPgKeyKoMegF48R3CSQrGF2MpsMmccyMyuEJd/gxYMiXv0gb/6Nk2QPmljQUFR1090Vp5wZ6/vfXmltfWNzq7xd2dnd2z+oHh61jMo0oSFRXOlOjA3lTNLQMstpJ9UUi5jTdjy+nfntJ6oNU/LBTlIaCTyULGEEWyeF7cdeKvrVml/350CrJChIDQo0+9Wv3kCRTFBpCcfGdAM/tVGOtWWE02mllxmaYjLGQ9p1VGJBTZTPj52iM6cMUKK0K2nRXP09kWNhzETErlNgOzLL3kz8z+tmNrmOcibTzFJJFouSjCOr0OxzNGCaEssnjmCimbsVkRHWmFiXT8WFECy/vEpaF/XArwf3l7XGTRFHGU7gFM4hgCtowB00IQQCDJ7hFd486b14797HorXkFTPH8Afe5w+0eI6a</latexit><latexit sha1_base64="smXTBkHfQl+094B8aAuLaVLnUvk=">AAAB7HicbVDLSgNBEOyNrxhfUY9eBoPgKeyKoMegF48R3CSQrGF2MpsMmccyMyuEJd/gxYMiXv0gb/6Nk2QPmljQUFR1090Vp5wZ6/vfXmltfWNzq7xd2dnd2z+oHh61jMo0oSFRXOlOjA3lTNLQMstpJ9UUi5jTdjy+nfntJ6oNU/LBTlIaCTyULGEEWyeF7cdeKvrVml/350CrJChIDQo0+9Wv3kCRTFBpCcfGdAM/tVGOtWWE02mllxmaYjLGQ9p1VGJBTZTPj52iM6cMUKK0K2nRXP09kWNhzETErlNgOzLL3kz8z+tmNrmOcibTzFJJFouSjCOr0OxzNGCaEssnjmCimbsVkRHWmFiXT8WFECy/vEpaF/XArwf3l7XGTRFHGU7gFM4hgCtowB00IQQCDJ7hFd486b14797HorXkFTPH8Afe5w+0eI6a</latexit><latexit sha1_base64="smXTBkHfQl+094B8aAuLaVLnUvk=">AAAB7HicbVDLSgNBEOyNrxhfUY9eBoPgKeyKoMegF48R3CSQrGF2MpsMmccyMyuEJd/gxYMiXv0gb/6Nk2QPmljQUFR1090Vp5wZ6/vfXmltfWNzq7xd2dnd2z+oHh61jMo0oSFRXOlOjA3lTNLQMstpJ9UUi5jTdjy+nfntJ6oNU/LBTlIaCTyULGEEWyeF7cdeKvrVml/350CrJChIDQo0+9Wv3kCRTFBpCcfGdAM/tVGOtWWE02mllxmaYjLGQ9p1VGJBTZTPj52iM6cMUKK0K2nRXP09kWNhzETErlNgOzLL3kz8z+tmNrmOcibTzFJJFouSjCOr0OxzNGCaEssnjmCimbsVkRHWmFiXT8WFECy/vEpaF/XArwf3l7XGTRFHGU7gFM4hgCtowB00IQQCDJ7hFd486b14797HorXkFTPH8Afe5w+0eI6a</latexit> interacting with what? how massive? in what regime is it particle-y?
  • 11. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 11 Weakly Interacting Massive Particle electroweak interactions electroweak particles electroweak mass yeah, it’s a particle F O R T H I S TA L K : This talk: what’s the value of this definition?
  • 12. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 12 Defining the WIMP Bertone & Hooper, “History of Dark Matter,” 1605.04909, RMP original WIMP: neutrinos … it turns out that they don’t work.
  • 13. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 13 Outline
  • 14. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 14 A historical fiction about the WIMP … an imaginary story which told the final tale of the Silver Age Superman and his long mythology … via Wikipedia 6/2019 actual history grad students should cite this
  • 15. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 15 Particle Physics, circa 1990s / / ¯ / − / ¯ / / / −/ ¯ / − / / ( ) ( ) fundamental forces matterparticles or something to explain unitarity of WW scattering ?
  • 16. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 16 Particle Physics From We Have No Idea, Cham and Whiteson CMS
  • 17. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 17Maximilien Brice, CERN via National Geographic (May 2012)
  • 18. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 18 D. Overbye, New York Times, 4 July 2012
  • 19. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 19 Known Unknowns in Particle Physics Why is the Higgs boson light? Hierarchy Problem an incomplete list! (Images: We Have No Idea, Cham and Whiteson) Why is there more matter than antimatter? Baryogenesis Problem Why is ϴYM small? Strong CP Problem What is the origin of neutrino mass? … What is dark matter? Missing Mass Problem Other puzzles (possibly related to dark matter?)
  • 20. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 20 The Hierarchy Problem The Higgs has a snowball’s chance in hell of being 125 GeV. FT, Quantum Diaries, “The Hierarchy Problem” (2012) (and yet here we are)
  • 21. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 21 The Hierarchy Problem FT, Quantum Diaries, “The Hierarchy Problem” (2012) supersymmetry or extra dimensions, compositeness…
  • 22. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 22 A favorite answer: supersymmetry matter particle force particle force particle matter particle N E W PA R T I C L E SV I S I B L E S T U F F SUSY
  • 23. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 23 For the most part, it works … a little bit of model-building required.
  • 24. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 24 Preventing Proton Decay: R-parity ¯d ¯u e¯d,e¯s,e¯b 4 1 Q L ¯u ¯u y squarks. Arrows indicate helicity and should not be confus rac spinors [14]. Tildes indicate superpartners while bars a les into left-chiral fields in the conjugate representation. perfield Matter parity on of this is to impose the above constrain PR = ( )3(B L)+2s , of the field. Conservation of matter parity 2s factor always cancels in any interaction m has an even number of fermions. Obs rpartner fields have R-parity 1. (This i grams assocaited with electroweak precisio parity requires pair-production of superp ns cannot occur at tree-level and must co PR[ ordinary matter ] = + PR[ superpartner ] = − Added bonus:
 lightest superpartner is stable. ?
  • 25. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 25 Known Unknowns mh ? Missing Mass
  • 26. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 26 The story so far: SUSY mh ? SUSY New Particles p+ stability R-parity ? Dark Matter ! Missing Mass
  • 27. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 27 Weakly-Interacting Massive Particle mh ? Dark Matter ! Weak scale mass ~100 GeV
 Weak scale interaction strength GF 
 No additional parameters (roughly) Missing Mass
  • 28. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 28 One thing that we do know: density Dark Matter ! Missing Mass Approx. 1 WIMP per mug of coffee ~ GeV / cm3
  • 29. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 29 Weakly-Interacting Massive Particle mh ? Dark Matter ! Weak scale mass ~100 GeV
 Weak scale interaction strength GF 
 No additional parameters (roughly) Missing Mass How much dark matter do we predict?
  • 30. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 30 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
  • 31. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 31 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 ]
  • 32. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 32 The “WIMP Miracle” capture annihilation SM SM Z “WEAK SCALE” MASS WEAK FORCE annihilation ⌦ h2 ⇠ 0.1 pb h annvi “WEAK SCALE” ANNIHILATION RATE PRESENT ABUNDANCE automatically get the correct abundance (almost) expansion of universe
  • 33. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 33 SUSY WIMP bible 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 198 206 206 209 211 211 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 7.2. Axial-vector (spin) interaction 252 256 258 259 260 260 261
  • 34. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 34 The story so far: SUSY mh ? SUSY New Particles p+ stability R-parity ? Dark Matter
 with correct abundance !
  • 35. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 35 extra dimensions mh ? XD New Particles precision observables KK-parity ? ! free in flat XD warped XD Dark Matter
 with correct abundance !
  • 36. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 36 compositeness mh ? composite New Particles T-parity ? ! precision observables Dark Matter
 with correct abundance !
  • 37. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 37 mh ? new symmetry New Particles new parity ? dangerous processes WIMP Dark Matter
 with correct abundance !
  • 38. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 38 A great love story Andrew Grant, Science News, June 2013
  • 39. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 39 WIMP story predictions nomorefreeparameters mh ? new symmetry New Particles new parity ? dangerous processes Dark Matter
 with correct abundance !
  • 40. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 40 WIMP Complementarity χ χ χ χ χ χ ANNIHIL ATION DI RECT DETECTION COLLIDER Ωχh2 INDIRECT DIRECT COLLIDER telescopes underground high energy & abundance
  • 41. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 41via LUX-LZ (kipac.stanford.edu/research/topics/direct-dark-matter-detection) Direct Detection Underground, 
 high-volume, 
 high-sensitivity. Recoil of dark matter off nuclei.
  • 42. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM Figure 27.1: WIMP cross sections (normalized to a single nucleon) for spin42 Direct Detection PDG Dark Matter Review 2018
  • 43. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 43Figure 27.1: WIMP cross sections (normalized to a single nucleon) for spin PDG Dark Matter Review 2018 weak scale coupling weak scale mass
  • 44. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM A great love story… and break up 44
  • 45. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM χ χ χ χ χ χ ANNIHIL ATION DI RECT DETECTIO N COLLIDER INDIRECT DIRECT COLLIDER 45 WIMP Complementarity Dark matter searches related by crossing symmetry: Standard ModelDark Matter 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
  • 46. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM A great love story… and break up 46
  • 47. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 47 Is the neutralino WIMP really dead? Technically? No. Linguistically? No. Experimentally? No. Emotionally? Yes. The WIMP is dead to me. “weak” vs “electroweak” Experimental program is robust! n.b. analogous to “SUSY is dead” ways to ‘hide’ a neutralino-esque WIMP
  • 48. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 48 Seven Samurai
  • 49. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 49 Recap: WIMP mh ? SUSY New Particles p+ stability R-parity ? Dark Matter with correct abundance predictions nomorefreeparameters 49
  • 50. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 50 “WIMP is dead… to me” mh ? SUSY New Particles p+ stability R-parity ? Dark Matter with correct abundance predictions nomorefreeparameters 50
  • 51. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 51 Outline
  • 52. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 52 Known Unknowns in Particle Physics Why is the Higgs boson light? Hierarchy Problem an incomplete list! Why is there more matter than antimatter? Baryogenesis Problem Why is ϴYM small? Strong CP Problem What is the origin of neutrino mass? … What is dark matter? Missing Mass Problem Other puzzles (possibly related to dark matter?)
  • 53. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 53 What can we look for? ? Dark Matter with correct abundance predictions 53 ?
  • 54. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 54 The elephant in the room How did it get here? Why is it still here?
  • 55. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 55 Recap: WIMP + WIMP Miracle mh ? New Particles ? ! small
 problem Dark Matter
new symmetry Why is it still here? How did it get here?
  • 56. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 56 Beyond the WIMP Dark Matter with correct abundance predictions 56 Fix couplings How’d it 
 get here? Why is it still here? new particlesUV theory? pheno. theory
  • 57. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 57 How do we move forward? What is the theory of dark matter? 
 Write down a bunch of [probably] wrong theories of not-WIMPS, see what we learn from them. How do we discover dark matter?
 On a budget! Using the experiments and telescopes that we have.
  • 58. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 58 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!
  • 59. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 59 Earth capture of dark matter 1 2 3 4 J. Feng, J. Smolinsky, FT 1509.07525, 1602.01465, 1701.03168 ; A. Green, FT 1808.03700 
  • 60. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 60 Holographic Dark Sectors Brax, Fichet, Tanedo 1906.02199 Costantino, Fichet, Tanedo 1910.02972 UV IR STAN AR ARSTAT S hiding in momentum-dependence
  • 61. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 61 No point in looking where it’s light! Search where it’s dark! Yojimbo
  • 62. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 62 Vector Self-Interacting Dark Matter I. Chaffey and FT 1907.10217 
  • 63. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 63 Neutron Star Dark Matter Collider A. Joglekar, N. Raj, FT, HBY Figure 1: Illustration of contrast between fixed targets and moving targets in NS frame. Left: Heavy targets (e.g. neutrons) are fixed and have “geometric” cross section in NS frame. Right:
  • 64. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 64 Dark Matter at First Light https:// www.google.com/ imgres? imgurl=https%3A %2F%2Fphysics.s https://cat.ucr.edu/ Home_files/webpage.jpg Supermassive Primordial Black Holes?
  • 65. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 65 How do we move forward? What is the theory of dark matter? 
 Write down a bunch of [probably] wrong theories of not-WIMPS, see what we learn from them. How do we discover dark matter?
 On a budget! Using the experiments and telescopes that we have.
  • 66. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 66 Thanks!
  • 67. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 67 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
  • 68. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 68 f l i p . t a n e d o @ u c r . e d u The second dark matter: Vulcan LOUISIANA PHYSICS DEPARTMENT SEMINAR
  • 69. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 69 Looks like a duck, vaguely aquatic… via Dmitry Ulitin (@dm_dm) on unsplash.com; @leonello, Getty Images
  • 70. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 70 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!
  • 71. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 71 Effects on molecules, isotopes, … UCI IPC 1608.03591 1.03 MeV 10 keV width 18.15 MeV 138 keV width STATUS: INDEPENDENT EXP. CHECK REQUIRED
  • 72. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 72 Diffuse Supernova Neutrino Background Nirmal
 Raj Gopi Mohlabeng
  • 73. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM χ χ χ χ 73 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
  • 74. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 74 Remixing dark phenomenology
  • 75. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 75 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
  • 76. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 76 Step 2: Mediator Decay
  • 77. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 77Adapted 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
  • 78. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 78 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 MZ'=6 effM / 2 Darkonium territory Monojet territory 14TeV (300fb-1) 14TeV (3ab-1) Z' dijet search excl. 50 100 500 1000 20 50 100 200 500 M (GeV) MZ'(GeV) D=0.5, gq=0.1 Figure 1: Colorful curves show the future high-energy pp collider constraints on the model where 0
  • 79. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 79 Dark Monopoles Work in progress with C. Kilic, M. Martone visible matter picks up small dark charge dark stuff stays dark visible magnetic charge picks up small dark magnetic monopole Kinetic Mixing: Implies: millimagnetic charge
  • 80. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 80 A counterpoint arXiv:1904.02769
  • 81. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 81Andrew Grant, Science News, June 2013
  • 82. @ f l i p . t a n e d o 67UCR PHYSICS & ASTRO COLLOQUIUM 82 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, …