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Whatever happened to the WIMP of tomorrow?

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Flip Tanedo
Flip Tanedo

The document discusses a physics colloquium presentation about dark matter. It begins with an outline comparing the talk to fictional stories of Superman. The talk then reviews evidence that dark matter exists from astronomical observations. Next, it discusses the status of the weakly interacting massive particle (WIMP) as a leading dark matter candidate. The talk provides historical context for the WIMP hypothesis from the 1990s and outlines several open questions in particle physics that a WIMP could potentially address, such as the hierarchy problem. It describes how supersymmetry is a favored theoretical framework that could explain a WIMP through the introduction of superpartner particles.

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@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM Whatever happened to the WIMP of tomorrow? Flip Tanedo October 12, 2020 The Silver Age of Dark Matter
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Outline … with my apologies to DC comics Images: Cham & Whiteson We Have No Idea + The Guardian (Adam West Obituary), Johns Action Comics #858, Moore Whatever Happened to the Man of Tomorrow, Jurgens et al, Superman: Reign of the Supermen 2
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Outline … with my apologies to DC comics Images: Cham & Whiteson We Have No Idea + The Guardian (Adam West Obituary), Johns Action Comics #858, Moore Whatever Happened to the Man of Tomorrow, Jurgens et al, Superman: Reign of the Supermen 3
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Assumption for this talk: dark matter exists Cham & Whiteson , We Have No Idea 4 And we know roughly how much there is
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Astronomy and Cosmology tell us Dark Matter Exists Images: Jeff Filippini (Berkeley Cosmology 2005), NASA APOD 2006, NASA WMAP 5 5% 27% 68% Standard Model is not complete ROTATION CURVES GRAVITATIONAL LENSING COSMIC MICROWAVE BACKGROUND This talk: new particle(s) Conservative assumption
 could be other options And we know roughly how much there is
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 6 Evidence… looks like an astro talk 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 via Katie Mack (ACP Colloquium 2019) 6 Astronomy and Cosmology tell us Dark Matter Exists
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Outline … with my apologies to DC comics Images: Cham & Whiteson We Have No Idea + The Guardian (Adam West Obituary), Johns Action Comics #858, Moore Whatever Happened to the Man of Tomorrow, Jurgens et al, Superman: Reign of the Supermen 7
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Present Status 8 Adapted from “Dewey Defeats Truman,” via history.com originally from the St. Louis Globe-Democrat
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Hooper, CfA Colloquium: youtube.com/watch?v=j3Wmvijk70E 9
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Weakly Interacting Massive Particle 10 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 CORNELL PHYSICS COLLOQUIUM 64 Weakly Interacting Massive Particle Cham & Whiteson We Have No Idea 11 electroweak interactions electroweak Particles electroweak Mass particle; certainly in electroweak regime definition for this talk why this definition?
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Defining the WIMP Bertone & Hooper, “History of Dark Matter,” 1605.04909, RMP 12 original WIMP: neutrinos … it turns out that they don’t work. why this definition?
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Outline … with my apologies to DC comics Images: Cham & Whiteson We Have No Idea + The Guardian (Adam West Obituary), Johns Action Comics #858, Moore Whatever Happened to the Man of Tomorrow, Jurgens et al, Superman: Reign of the Supermen 13
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 A historical fiction about the WIMP Whatever happened to the man of tomorrow? 14 … an imaginary story which told the final tale of the Silver Age Superman and his long mythology … Wikipedia 6/2019 actual history grad students should cite this
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Particle Physics, circa 1990s 15 / / ¯ / − / ¯ / / / −/ ¯ / − / / ( ) ( ) fundamental forces matter particles or something to explain unitarity of WW scattering ? Image: Stanford ATLAS website
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Particle Physicists Cham and Whiteson, We Have No Idea 16 CMS
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 17 Maximilien Brice, CERN via National Geographic (May 2012)
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 D. Overbye, New York Times, 4 July 2012 18
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Known Unknowns in Particle Physics 1990s - 2020; incomplete list Images: Cham and Whiteson, We Have No Idea 19 Why is the Higgs boson light? Hierarchy Problem Why is there more matter than antimatter? 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 CORNELL PHYSICS COLLOQUIUM 64 The Hierarchy Problem FT, Quantum Diaries, “The Hierarchy Problem” (2012) 20 The Higgs has a snowball’s chance in hell of being 125 GeV. (and yet here we are)
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 One favorite answer: supersymmetry See also extra dimensions, compositeness… 21 matter particle force particle force particle matter particle N E W PA R T I C L E S V I S I B L E S T U F F SUSY
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 How it works Idealized version 22 a little bit of model-building required. In practice: It has been well known since lep that in order to pu stop masses, me t ⇠ 1 1.4 tev. Pushing the stop The stops contribute not only to the Higgs quartic— also to the soft mass m2 Hu from loops of the form + 24 tops contribute not only to the Higgs quartic—which we need to push the Hi o the soft mass m2 Hu from loops of the form + 24
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 A little bit of patching up: R-Parity Preventing proton decay 23 ¯ d ū ē d,ē s,ē b 4 1 Q L ū ū by squarks. Arrows indicate helicity and should not be confused Dirac spinors [14]. Tildes indicate superpartners while bars are ticles into left-chiral fields in the conjugate representation. ariation of this is to impose the above constraint using PR = ( )3(B L)+2s , e spin of the field. Conservation of matter parity implies e ( )2s factor always cancels in any interaction term sin h term has an even number of fermions. Observe tha superpartner fields have R-parity 1. (This is simila e diagrams assocaited with electroweak precision obser e R-parity requires pair-production of superpartners, rections cannot occur at tree-level and must come from PR[ ordinary matter ] = + PR[ superpartner ] = − Added bonus:
 lightest superpartner is stable. ?
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The story so far: supersymmetry Images: Cham and Whiteson, We Have No Idea 24 mh ? ! Missing Mass
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The story so far: supersymmetry 25 mh ? SUSY New Particles p+ stability R-parity ? Dark Matter ? Missing Mass
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The story so far: supersymmetry 26 mh ? Dark Matter ? Missing Mass Weak scale mass ~100 GeV
 Weak scale interaction strength GF 
 No additional parameters (roughly)
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Ingredients for a model of dark matter? Anticipating how the WIMP became larger than life 1. At least one new particle. 2. Mechanism to produce 𝜌DM. 3. Experimental viability. 4. Strategy to test the model. 27 ? Moore Whatever Happened to the Man of Tomorrow
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 28 Approx. 1 WIMP per mug of coffee ~ GeV / cm3
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Weakly-Interacting Massive Particle 29 mh ? Dark Matter ? Missing Mass Weak scale mass ~100 GeV
 Weak scale interaction strength GF 
 No additional parameters (roughly) How much dark matter?
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 How much dark matter is there? 30 1 10 equilibrium time ~ mass / temp [comoving] number density 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 CORNELL PHYSICS COLLOQUIUM 64 How much dark matter is there? 31 1 10 equilibrium time ~ mass / temp [comoving] number density A N N I H I L AT I O N SM SM H U B B L E freeze out
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The WIMP Miracle Automatically obtain [almost] the correct abundance 32 c a p t u r e annihilation SM SM Z “WEAK SCALE” MASS WEAK FORCE annihilation ⌦ h2 ⇠ 0.1 pb h annvi “WEAK SCALE” ANNIHILATION RATE PRESENT ABUNDANCE expansion of universe
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 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 198 6.4. Fermion final states 252 Supersymmetric WIMP Bible 33
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The story so far: supersymmetry 34 mh ? SUSY New Particles p+ stability R-parity ? Dark Matter with correct abundance !
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The story so far: extra dimensions 35 mh ? Extra Dimensions New Particles precision observables KK-parity ? Dark Matter with correct abundance ! free in flat XD warped extra dim.
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The story so far: composite Higgs 36 mh ? composite New Particles precision observables T-parity ? Dark Matter with correct abundance !
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The general story 37 mh ? new symmetry New Particles precision observables new parity ? Dark Matter with correct abundance !
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 A great love story Andrew Grant, Science News, June 2013 38
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 What is a model of dark matter? Ingredients 1. At least one new particle. 2. Mechanism to produce 𝜌DM. 3. Experimental viability. 4. Strategy to test the model. 39 ?
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The general story 40 mh ? new symmetry New Particles precision observables new parity ? Dark Matter with correct abundance ! predictions no more free parameters
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 WIMP Complementarity 41 χ χ χ χ χ χ A N N I H I L ATION D I RECT DETECTIO N COLLIDER Ωχh2 INDIRECT DIRECT COLLIDER telescopes underground high energy & abundance Dark matter searches related by crossing symmetry
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM Direct Detection Underground, 
 high-volume, 
 high-sensitivity. Recoil of dark matter off nuclei via LUX-LZ (kipac.stanford.edu/research/topics/direct-dark-matter-detection)
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 PDG Dark Matter Review 2018 43 Figure 27.1: WIMP cross sections (normalized to a single nucleon) for spin- direct detection
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 PDG Dark Matter Review 2018 44 Figure 27.1: WIMP cross sections (normalized to a single nucleon) for spin- weak scale coupling weak scale mass
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 A great love story . . . and a break up 45
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 WIMP Complementarity 46 χ χ χ χ χ χ A N N I H I L ATION D I RECT DETECTIO N COLLIDER 2 INDIRECT Standard Model Dark Matter WEAK FORCE W I M P M I R AC L 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 DIRECT COLLIDE
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 A great love story . . . and a break up 47
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Are WIMPs dead? 48
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Are WIMPs dead? 49 (Like asking “is SUSY dead?”) Technically? No. Linguistically? No. Experimentally? No. Emotionally? Yes. The WIMP is dead to me. “weak” vs “electroweak” Experimental program is robust! ways to ‘hide’ a neutralino-esque WIMP This is the wrong question!
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The general story 50 mh ? new symmetry New Particles precision observables new parity ? Dark Matter with correct abundance ! predictions no more free parameters
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The general story 51 mh ? new symmetry New Particles precision observables new parity ? Dark Matter with correct abundance ! predictions no more free parameters
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Known Unknowns in Particle Physics 1990s - 2020; incomplete list Images: Cham and Whiteson, We Have No Idea 52 Why is the Higgs boson light? Hierarchy Problem Why is there more matter than antimatter? 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 CORNELL PHYSICS COLLOQUIUM 64 Outline … with my apologies to DC comics Images: Cham & Whiteson We Have No Idea + The Guardian (Adam West Obituary), Johns Action Comics #858, Moore Whatever Happened to the Man of Tomorrow, Jurgens et al, Superman: Reign of the Supermen 53
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 54 Chris Burden, Urban Light, 2008, Los Angeles County Museum of Art; photo courtesy of @neohumanity via Instagram Have we been looking under the wrong lamp-post? 1. At least one new particle. 2. Mechanism to produce 𝜌DM. 3. Experimental viability. 4. Strategy to test the model.
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The Elephant in the Room The abundance of dark matter 55 How did it get here? Why is it still here?
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Recap: WIMP Miracle 56 mh ? new symmetry New Particles new parity ? dangerous processes Dark Matter ! How did it get here? Why is it still here?
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 A phenomenological approach How do we cast the widest net? 57 Dark Matter with correct abundance predictions UV theory? pheno. theory start here What is the theory of dark matter? 
 Explore broad possibilities without top- down theory prejudice. 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 CORNELL PHYSICS COLLOQUIUM 64 A phenomenological approach How do we cast the widest net? 58 Dark Matter with correct abundance predictions Fix couplings How’d it 
 get here? Why is it still here? new particles UV theory? pheno. theory start here What is the theory of dark matter? 
 Explore broad possibilities without top- down theory prejudice. 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 CORNELL PHYSICS COLLOQUIUM 64 Example: Dark Sector with Light Mediator Non-WIMP lamp-post 59 e e e e e e e e e e capture a n n i h i l a t i o n x x A0 A0 INDIRECT DIRECT COLLIDER Standard Model Mediator N N q q A N N I H I L ATION COLLIDER D I R E C T Dark Matter Halo Morpholo • SIDM particles follow the 0 2 4 6 8 0 2 4 6 8 R HkpcL z HkpcL constant density contours Kaplinghat, Linden, Keeley, HBY (2013) (PR Co dis SELF
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 e.g. Earth capture of dark matter Not possible with neutralinos J. Feng, J. Smolinsky, FT 1509.07525, 1602.01465, 1701.03168 ; A. Green, FT 1808.03700  60 1 2 3 4
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 e.g. Holographic Dark Sectors Non-minimal mediators Brax, Fichet, Tanedo 10906.02199; Costantino, Fichet, Tanedo 19010.02972 61
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 62 Chris Burden, Urban Light, 2008, Los Angeles County Museum of Art; photo courtesy of @neohumanity via Instagram Have we been looking under the wrong lamp-post? non-thermal production complicated dark sectors decaying dark matter macroscopic dark matter lumps primordial black holes axions, ultralight dark matter gravity is very weird many other possibilities… 1. At least one new particle. 2. Mechanism to produce 𝜌DM. 3. Experimental viability. 4. Strategy to test the model.
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Big Picture: why this matters More interdisciplinary than ever Hunt for dark matter is multi-frontier. Each sub-community has its own jargon. WIMP is jargon whose meaning has drifted to mean something slightly different to different people. This gets in the way of seeing why certain ideas were well-motivated, and why/how we are moving beyond them. US particle physics community’s decadal strategic planning process: snowmass21.org 63
@ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Thanks Csáki group, September 2012; Photo Courtesy of Cornell 64

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Whatever happened to the WIMP of tomorrow?

  • 1. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM Whatever happened to the WIMP of tomorrow? Flip Tanedo October 12, 2020 The Silver Age of Dark Matter
  • 2. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Outline … with my apologies to DC comics Images: Cham & Whiteson We Have No Idea + The Guardian (Adam West Obituary), Johns Action Comics #858, Moore Whatever Happened to the Man of Tomorrow, Jurgens et al, Superman: Reign of the Supermen 2
  • 3. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Outline … with my apologies to DC comics Images: Cham & Whiteson We Have No Idea + The Guardian (Adam West Obituary), Johns Action Comics #858, Moore Whatever Happened to the Man of Tomorrow, Jurgens et al, Superman: Reign of the Supermen 3
  • 4. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Assumption for this talk: dark matter exists Cham & Whiteson , We Have No Idea 4 And we know roughly how much there is
  • 5. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Astronomy and Cosmology tell us Dark Matter Exists Images: Jeff Filippini (Berkeley Cosmology 2005), NASA APOD 2006, NASA WMAP 5 5% 27% 68% Standard Model is not complete ROTATION CURVES GRAVITATIONAL LENSING COSMIC MICROWAVE BACKGROUND This talk: new particle(s) Conservative assumption
 could be other options And we know roughly how much there is
  • 6. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 6 Evidence… looks like an astro talk 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 via Katie Mack (ACP Colloquium 2019) 6 Astronomy and Cosmology tell us Dark Matter Exists
  • 7. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Outline … with my apologies to DC comics Images: Cham & Whiteson We Have No Idea + The Guardian (Adam West Obituary), Johns Action Comics #858, Moore Whatever Happened to the Man of Tomorrow, Jurgens et al, Superman: Reign of the Supermen 7
  • 8. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Present Status 8 Adapted from “Dewey Defeats Truman,” via history.com originally from the St. Louis Globe-Democrat
  • 9. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Hooper, CfA Colloquium: youtube.com/watch?v=j3Wmvijk70E 9
  • 10. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Weakly Interacting Massive Particle 10 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 CORNELL PHYSICS COLLOQUIUM 64 Weakly Interacting Massive Particle Cham & Whiteson We Have No Idea 11 electroweak interactions electroweak Particles electroweak Mass particle; certainly in electroweak regime definition for this talk why this definition?
  • 12. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Defining the WIMP Bertone & Hooper, “History of Dark Matter,” 1605.04909, RMP 12 original WIMP: neutrinos … it turns out that they don’t work. why this definition?
  • 13. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Outline … with my apologies to DC comics Images: Cham & Whiteson We Have No Idea + The Guardian (Adam West Obituary), Johns Action Comics #858, Moore Whatever Happened to the Man of Tomorrow, Jurgens et al, Superman: Reign of the Supermen 13
  • 14. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 A historical fiction about the WIMP Whatever happened to the man of tomorrow? 14 … an imaginary story which told the final tale of the Silver Age Superman and his long mythology … Wikipedia 6/2019 actual history grad students should cite this
  • 15. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Particle Physics, circa 1990s 15 / / ¯ / − / ¯ / / / −/ ¯ / − / / ( ) ( ) fundamental forces matter particles or something to explain unitarity of WW scattering ? Image: Stanford ATLAS website
  • 16. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Particle Physicists Cham and Whiteson, We Have No Idea 16 CMS
  • 17. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 17 Maximilien Brice, CERN via National Geographic (May 2012)
  • 18. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 D. Overbye, New York Times, 4 July 2012 18
  • 19. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Known Unknowns in Particle Physics 1990s - 2020; incomplete list Images: Cham and Whiteson, We Have No Idea 19 Why is the Higgs boson light? Hierarchy Problem Why is there more matter than antimatter? 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 CORNELL PHYSICS COLLOQUIUM 64 The Hierarchy Problem FT, Quantum Diaries, “The Hierarchy Problem” (2012) 20 The Higgs has a snowball’s chance in hell of being 125 GeV. (and yet here we are)
  • 21. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 One favorite answer: supersymmetry See also extra dimensions, compositeness… 21 matter particle force particle force particle matter particle N E W PA R T I C L E S V I S I B L E S T U F F SUSY
  • 22. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 How it works Idealized version 22 a little bit of model-building required. In practice: It has been well known since lep that in order to pu stop masses, me t ⇠ 1 1.4 tev. Pushing the stop The stops contribute not only to the Higgs quartic— also to the soft mass m2 Hu from loops of the form + 24 tops contribute not only to the Higgs quartic—which we need to push the Hi o the soft mass m2 Hu from loops of the form + 24
  • 23. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 A little bit of patching up: R-Parity Preventing proton decay 23 ¯ d ū ē d,ē s,ē b 4 1 Q L ū ū by squarks. Arrows indicate helicity and should not be confused Dirac spinors [14]. Tildes indicate superpartners while bars are ticles into left-chiral fields in the conjugate representation. ariation of this is to impose the above constraint using PR = ( )3(B L)+2s , e spin of the field. Conservation of matter parity implies e ( )2s factor always cancels in any interaction term sin h term has an even number of fermions. Observe tha superpartner fields have R-parity 1. (This is simila e diagrams assocaited with electroweak precision obser e R-parity requires pair-production of superpartners, rections cannot occur at tree-level and must come from PR[ ordinary matter ] = + PR[ superpartner ] = − Added bonus:
 lightest superpartner is stable. ?
  • 24. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The story so far: supersymmetry Images: Cham and Whiteson, We Have No Idea 24 mh ? ! Missing Mass
  • 25. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The story so far: supersymmetry 25 mh ? SUSY New Particles p+ stability R-parity ? Dark Matter ? Missing Mass
  • 26. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The story so far: supersymmetry 26 mh ? Dark Matter ? Missing Mass Weak scale mass ~100 GeV
 Weak scale interaction strength GF 
 No additional parameters (roughly)
  • 27. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Ingredients for a model of dark matter? Anticipating how the WIMP became larger than life 1. At least one new particle. 2. Mechanism to produce 𝜌DM. 3. Experimental viability. 4. Strategy to test the model. 27 ? Moore Whatever Happened to the Man of Tomorrow
  • 28. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 28 Approx. 1 WIMP per mug of coffee ~ GeV / cm3
  • 29. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Weakly-Interacting Massive Particle 29 mh ? Dark Matter ? Missing Mass Weak scale mass ~100 GeV
 Weak scale interaction strength GF 
 No additional parameters (roughly) How much dark matter?
  • 30. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 How much dark matter is there? 30 1 10 equilibrium time ~ mass / temp [comoving] number density 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 CORNELL PHYSICS COLLOQUIUM 64 How much dark matter is there? 31 1 10 equilibrium time ~ mass / temp [comoving] number density A N N I H I L AT I O N SM SM H U B B L E freeze out
  • 32. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The WIMP Miracle Automatically obtain [almost] the correct abundance 32 c a p t u r e annihilation SM SM Z “WEAK SCALE” MASS WEAK FORCE annihilation ⌦ h2 ⇠ 0.1 pb h annvi “WEAK SCALE” ANNIHILATION RATE PRESENT ABUNDANCE expansion of universe
  • 33. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 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 198 6.4. Fermion final states 252 Supersymmetric WIMP Bible 33
  • 34. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The story so far: supersymmetry 34 mh ? SUSY New Particles p+ stability R-parity ? Dark Matter with correct abundance !
  • 35. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The story so far: extra dimensions 35 mh ? Extra Dimensions New Particles precision observables KK-parity ? Dark Matter with correct abundance ! free in flat XD warped extra dim.
  • 36. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The story so far: composite Higgs 36 mh ? composite New Particles precision observables T-parity ? Dark Matter with correct abundance !
  • 37. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The general story 37 mh ? new symmetry New Particles precision observables new parity ? Dark Matter with correct abundance !
  • 38. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 A great love story Andrew Grant, Science News, June 2013 38
  • 39. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 What is a model of dark matter? Ingredients 1. At least one new particle. 2. Mechanism to produce 𝜌DM. 3. Experimental viability. 4. Strategy to test the model. 39 ?
  • 40. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The general story 40 mh ? new symmetry New Particles precision observables new parity ? Dark Matter with correct abundance ! predictions no more free parameters
  • 41. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 WIMP Complementarity 41 χ χ χ χ χ χ A N N I H I L ATION D I RECT DETECTIO N COLLIDER Ωχh2 INDIRECT DIRECT COLLIDER telescopes underground high energy & abundance Dark matter searches related by crossing symmetry
  • 42. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM Direct Detection Underground, 
 high-volume, 
 high-sensitivity. Recoil of dark matter off nuclei via LUX-LZ (kipac.stanford.edu/research/topics/direct-dark-matter-detection)
  • 43. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 PDG Dark Matter Review 2018 43 Figure 27.1: WIMP cross sections (normalized to a single nucleon) for spin- direct detection
  • 44. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 PDG Dark Matter Review 2018 44 Figure 27.1: WIMP cross sections (normalized to a single nucleon) for spin- weak scale coupling weak scale mass
  • 45. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 A great love story . . . and a break up 45
  • 46. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 WIMP Complementarity 46 χ χ χ χ χ χ A N N I H I L ATION D I RECT DETECTIO N COLLIDER 2 INDIRECT Standard Model Dark Matter WEAK FORCE W I M P M I R AC L 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 DIRECT COLLIDE
  • 47. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 A great love story . . . and a break up 47
  • 48. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Are WIMPs dead? 48
  • 49. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Are WIMPs dead? 49 (Like asking “is SUSY dead?”) Technically? No. Linguistically? No. Experimentally? No. Emotionally? Yes. The WIMP is dead to me. “weak” vs “electroweak” Experimental program is robust! ways to ‘hide’ a neutralino-esque WIMP This is the wrong question!
  • 50. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The general story 50 mh ? new symmetry New Particles precision observables new parity ? Dark Matter with correct abundance ! predictions no more free parameters
  • 51. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The general story 51 mh ? new symmetry New Particles precision observables new parity ? Dark Matter with correct abundance ! predictions no more free parameters
  • 52. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Known Unknowns in Particle Physics 1990s - 2020; incomplete list Images: Cham and Whiteson, We Have No Idea 52 Why is the Higgs boson light? Hierarchy Problem Why is there more matter than antimatter? 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 CORNELL PHYSICS COLLOQUIUM 64 Outline … with my apologies to DC comics Images: Cham & Whiteson We Have No Idea + The Guardian (Adam West Obituary), Johns Action Comics #858, Moore Whatever Happened to the Man of Tomorrow, Jurgens et al, Superman: Reign of the Supermen 53
  • 54. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 54 Chris Burden, Urban Light, 2008, Los Angeles County Museum of Art; photo courtesy of @neohumanity via Instagram Have we been looking under the wrong lamp-post? 1. At least one new particle. 2. Mechanism to produce 𝜌DM. 3. Experimental viability. 4. Strategy to test the model.
  • 55. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 The Elephant in the Room The abundance of dark matter 55 How did it get here? Why is it still here?
  • 56. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Recap: WIMP Miracle 56 mh ? new symmetry New Particles new parity ? dangerous processes Dark Matter ! How did it get here? Why is it still here?
  • 57. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 A phenomenological approach How do we cast the widest net? 57 Dark Matter with correct abundance predictions UV theory? pheno. theory start here What is the theory of dark matter? 
 Explore broad possibilities without top- down theory prejudice. 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 CORNELL PHYSICS COLLOQUIUM 64 A phenomenological approach How do we cast the widest net? 58 Dark Matter with correct abundance predictions Fix couplings How’d it 
 get here? Why is it still here? new particles UV theory? pheno. theory start here What is the theory of dark matter? 
 Explore broad possibilities without top- down theory prejudice. How do we discover dark matter?
 On a budget! Using the experiments and telescopes that we have.
  • 59. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Example: Dark Sector with Light Mediator Non-WIMP lamp-post 59 e e e e e e e e e e capture a n n i h i l a t i o n x x A0 A0 INDIRECT DIRECT COLLIDER Standard Model Mediator N N q q A N N I H I L ATION COLLIDER D I R E C T Dark Matter Halo Morpholo • SIDM particles follow the 0 2 4 6 8 0 2 4 6 8 R HkpcL z HkpcL constant density contours Kaplinghat, Linden, Keeley, HBY (2013) (PR Co dis SELF
  • 60. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 e.g. Earth capture of dark matter Not possible with neutralinos J. Feng, J. Smolinsky, FT 1509.07525, 1602.01465, 1701.03168 ; A. Green, FT 1808.03700  60 1 2 3 4
  • 61. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 e.g. Holographic Dark Sectors Non-minimal mediators Brax, Fichet, Tanedo 10906.02199; Costantino, Fichet, Tanedo 19010.02972 61
  • 62. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 62 Chris Burden, Urban Light, 2008, Los Angeles County Museum of Art; photo courtesy of @neohumanity via Instagram Have we been looking under the wrong lamp-post? non-thermal production complicated dark sectors decaying dark matter macroscopic dark matter lumps primordial black holes axions, ultralight dark matter gravity is very weird many other possibilities… 1. At least one new particle. 2. Mechanism to produce 𝜌DM. 3. Experimental viability. 4. Strategy to test the model.
  • 63. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Big Picture: why this matters More interdisciplinary than ever Hunt for dark matter is multi-frontier. Each sub-community has its own jargon. WIMP is jargon whose meaning has drifted to mean something slightly different to different people. This gets in the way of seeing why certain ideas were well-motivated, and why/how we are moving beyond them. US particle physics community’s decadal strategic planning process: snowmass21.org 63
  • 64. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64 Thanks Csáki group, September 2012; Photo Courtesy of Cornell 64