New Physics beyond the Standard Model: from the Earth to the Sky

New Physics beyond the Standard Model: from the Earth to the Sky Shufang Su U. of Arizona Copyright S. Su CERN (Photo courtesy of Maruša Bradač.) APS4CS Oct 24, 2009

Let s start with the smallest scale: fundamental particles S. Su

Particle physics: the Standard Model S. Su Source: Fermilab media 3

Colliders: past and current Source: SLAC Source: CERN Source: Fermilab SLC@SLAC 19921998 (SLD) e+e Ecm up to 90 GeV LEP@CERN 19892000 e+e Ecm up to 209 GeV Tevatron @ Fermilab 19832010 ppbar Ecm up to 1.96 TeV S. Su 4

Success of the SM All quarks, leptons and gauge bosons have been found. latest: top quark 173 GeV, 1995 @ Tevatron top pair @ D0 S. Su 5 Source: D0

precision test: results from various experiments agree well m W [GeV] 80.5 80.4 80.3 August 2009 LEP2 and Tevatron (prel.) LEP1 and SLD 68% CL!" m H [GeV] 114 300 1000 Success of the SM Measurement Fit O meas!o fit /" meas 0 1 2 3 #$ (5) had (m Z ) 0.02758 ± 0.00035 0.02767 m Z [GeV] 91.1875 ± 0.0021 91.1874 % Z [GeV] 2.4952 ± 0.0023 2.4959 " 0 had [nb] 41.540 ± 0.037 41.478 R l 20.767 ± 0.025 20.742 A 0,l fb 0.01714 ± 0.00095 0.01643 A l (P & ) 0.1465 ± 0.0032 0.1480 R b 0.21629 ± 0.00066 0.21579 R c 0.1721 ± 0.0030 0.1723 A 0,b fb 0.0992 ± 0.0016 0.1038 A 0,c fb 0.0707 ± 0.0035 0.0742 A b 0.923 ± 0.020 0.935 A c 0.670 ± 0.027 0.668 A l (SLD) 0.1513 ± 0.0021 0.1480 sin 2 ' lept eff (Q fb ) 0.2324 ± 0.0012 0.2314 m W [GeV] 80.399 ± 0.025 80.378 % W [GeV] 2.098 ± 0.048 2.092 m t [GeV] 173.1 ± 1.3 173.2 150 175 200 S. Su March 2009 6 m t [GeV] LEPEWWG 0 1 2 3

Open questions SM only explains 4% of the Universe other 96%? dark matter, dark energy... (later) Antimatter? Unification? New symmetries, new physical laws? Extra dimensions? Why 3 generations of quarks and leptons? Neutrino masses? What is the origin of mass?... S. Su 7

Masses How do particles get masses? S. Su 8

Origin of the mass: Higgs mechanism S. Su 9

Origin of the mass: Higgs mechanism We have not found the Higgs boson yet... S. Su 9

Tevatron and the LHC LHC @ CERN 2009 xxx pp Ecm up to 14 TeV Source: Fermilab Tevatron @ Fermilab 19832010 ppbar Ecm up to 1.96 TeV S. Su 10 Source: CERN

Higgs events @ the LHC Higgs @ CMS S. Su 11 Source: CMS @ CERN

Higgs @ the LHC S. Su 12

Higgs @ the LHC NOT THAT EASY! S. Su 12

Higgs @ the LHC NOT THAT EASY! 1 Higgs in 800,000,000 particles S. Su 12

S. Su 13

Higgs with Higgs S. Su 13

New problems... SM is an effective theory below the electroweak scale mweak 10 2 GeV, Λcutoff = mpl 10 18 GeV Higgs is a fundamental scalar particle It receives huge quantum corrections from vacuum fluctuations (mh 2 )physical (mh 2 )bare + Λcutoff 2 +(10 18 GeV) 2 S. Su 14

Solutions: symmetry SM is an effective theory below the electroweak scale mew 10 2 GeV, Λcutoff = mpl 10 18 GeV Higgs is a fundamental scalar particle It receives huge quantum corrections from vacuum fluctuations (mh 2 )physical (mh 2 )bare + Λcutoff 2 = (10 2 GeV) 2 +(10 18 GeV) 2 S. Su 15

Solutions: symmetry SM is an effective theory below the electroweak scale mew 10 2 GeV, Λcutoff = mpl 10 18 GeV Higgs is a fundamental scalar particle It receives huge quantum corrections from vacuum fluctuations Λcutoff 2 (mh 2 )physical (mh 2 )bare + Λcutoff 2 = (10 2 GeV) 2 +(10 18 GeV) 2 (10 18 GeV) 2 S. Su 15

Solutions: symmetry SM is an effective theory below the electroweak scale mew 10 2 GeV, Λcutoff = mpl 10 18 GeV Higgs is a fundamental scalar particle It receives huge quantum corrections from vacuum fluctuations Λcutoff 2 (mh 2 )physical (mh 2 )bare + Λcutoff 2 = (10 2 GeV) 2 +(10 18 GeV) 2 (10 18 GeV) 2 Symmetry S. Su 15

Solutions: symmetry SM is an effective theory below the electroweak scale mew 10 2 GeV, Λcutoff = mpl 10 18 GeV Higgs is a fundamental scalar particle It receives huge quantum corrections from vacuum fluctuations Λcutoff 2 (mh 2 )physical (mh 2 )bare + Λcutoff 2 = (10 2 GeV) 2 +(10 18 GeV) 2 (10 18 GeV) 2 Symmetry Supersymmetry S. Su 15

Solutions: extra dimensions SM is an effective theory below the electroweak scale mew 10 2 GeV, Λcutoff = mpl 10 18 GeV Higgs is a fundamental scalar particle It receives huge quantum corrections from vacuum fluctuations (mh 2 )physical (mh 2 )bare + Λcutoff 2 = (10 2 GeV) 2 +(10 18 GeV) 2 S. Su 16

Solutions: strong dynamics SM is an effective theory below the electroweak scale mew 10 2 GeV, Λcutoff = mpl 10 18 GeV Higgs is a fundamental scalar particle It receives huge quantum corrections from vacuum fluctuations no fundamental scalar no hierarchy problem electroweak symmetry breaking (particles obtain masses) via strong dynamics: fermion condensates (mh 2 )physical (mh 2 )bare + Λcutoff 2 = (10 2 GeV) 2 technicor +(10 18 GeV) 2 S. Su 17

New Phenomenon supersymmetry: supersymmetric particles Extra dimensions: KluzaKlein particles Source: www.physics.gla.ac.uk/ ppt/susy.htm Technicolor: techni π, techni ρ Many other new scenarios, new particles and new forces... S. Su 18

the LHC LHC @ CERN 2009 xxx pp Ecm up to 14 TeV LHC is going to be a power pool for us to explore the energy frontier of particle physics in the coming decade. Source: CERN S. Su 19

Now let s look at the largest scale: the Universe S. Su

Observations Supernovae CMB (Photo courtesy of Maruša Bradač.) S. Su 21

Synthesis only 4% is known S. Su 22

Dark matter Source: Fermilab media CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting S. Su 23

Dark matter Source: Fermilab media CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting No good candidates for CDM in SM S. Su 23

Dark matter and new physics DM provide precise, unambiguous evidence for new physics In many BSM theories, DM is easier to explain than no DM Dark Matter: new stable particle there are usually many new weak scale particle constraints (proton decay, large EW corrections) discrete symmetry stability good dark matter candidate S. Su 24

Zoo of dark matter mass and interaction strengths span many, many orders of magnitude Some Dark Matter Candidate Particles! int (pb) 10 24 10 21 10 18 10 15 10 12 10 9 10 6 10 3 10 0 10 3 10 6 10 9 10 12 10 15 10 18 10 21 10 24 10 27 10 30 10 33 10 36 10 39 Roskowski (2004) Baer and Tata (2007) fuzzy CDM neutrinos axion WIMPs : neutralino KK photon branon LTP Qball axino SuperWIMPs : gravitino KK graviton wimp less wimpzilla 10 33 10 30 10 27 10 24 10 21 10 18 10 15 10 12 10 9 10 6 10 3 10 0 10 3 10 6 10 9 10 12 10 15 10 18 Black Hole Remnant S. Su mass (GeV) 25

WIMP WIMP: Weak Interacting Massive Particle Boltzmann equation WIMP Source: Kolb and Turner S. Su 26

WIMP miracle WIMP: Weak Interacting Massive Particle m WIMP m weak σ an α weak 2 m weak 2 Ω h 2 0.3 naturally around the observed value WIMP appears in many BSM scenarios lightest supersymmetric particles in SUSY models lightest KK particles in extra dimension models... S. Su 27

Study WIMP at colliders Produce and study WIMP properties (mass, coupling) at colliders Compare Ωproduced with Ωrelic: % level agreement LHC ILC WMAP (current) Battaglia (2005) Planck (~2010) S. Su 28

Study WIMP at colliders Produce and study WIMP properties (mass, coupling) at colliders Compare Ωproduced with Ωrelic: % level agreement LHC ILC WMAP (current) Confirmation of dark matter identity Battaglia (2005) Planck (~2010) S. Su 28

WIMPless? Ω X 1 σv m2 X g 4 X mx/gx 2 mweak/gweak 2, Ωh 2 0.3 only fixes one combination of dark matter mass and coupling could have mx mweak as long as the relation holds S. Su 29

WIMPless miracle Feng and Kumar (2008) Feng, Tu and Yu (2008) Dark matter is hidden no SM interactions DM sector has its own particle content, mass mx, coupling gx Connected to SUSY breaking sector WIMPs m X g 2 X m g 2 F 16π 2 M Ω X 1 σv m2 X g 4 X WIMPless DM right relic density! (irrespective of its mass) S. Su 30

Hidden dark matter signal @ collider DM p p Y Y b DM b Y particle appears at LHC as exotic 4th generation quarks S. Su

SuperWIMP / Extremely WIMP Not follow WIMP relation, DM interaction << Weak interaction. Possible? CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting (much weaker than weak interaction) S. Su 32

Nonthermal production: WIMP decay WIMP superwimp + SM particles Kim, Masiero, Nanopoulos (1984) Covi, Kim, Roszkowski (1999) Feng, Rajaraman, Takayama (2003); Bi, Li, Zhang (2003); Ellis, Olive, Santoso, Spanos (2003); Wang, Yang (2004); Feng, Su, Takayama (2004); Buchmuller, hamaguchi, Ratz, Yanagida (2004); Roszkowski, Ruiz de Austri, Choi (2004); Brandeburg, Covi, hamaguchi, Roszkowski, Steffen (2005);... S. Su 33

Nonthermal production: WIMP decay WIMP superwimp + SM particles WIMP S. Su 33

Nonthermal production: WIMP decay WIMP superwimp + SM particles SWIMP SM S. Su 33

Nonthermal production: WIMP decay WIMP superwimp + SM particles S. Su 33

Nonthermal production: WIMP decay WIMP superwimp + SM particles O(1) S. Su 33

Nonthermal production: WIMP decay WIMP superwimp + SM particles superwimp O(1) e.g. Gravitino LSP LKK graviton axino WIMP neutral charged S. Su 33

superwimp @ collider WIMP (slepton) could live for a year, so can be trapped then moved to a quiet environment to observe decays How to trap slepton? Hamaguchi, kuno, Nakaya, Nojiri, (2004) Feng and Smith, (2004) De Roeck et. al., (2005) Charged particle trap Reservoir S. Su 34

Synergy S. Su 35

Synergy Collider Inputs Weakscale Parameters DM Annihilation DMN Interaction S. Su 35

Synergy Collider Inputs Weakscale Parameters DM Annihilation DMN Interaction Relic Density Indirect Detection Direct Detection Astrophysical and Cosmological Inputs S. Su 35

Synergy parts per mille agreement for Ω χ discovery of dark matter Collider Inputs Weakscale Parameters DM Annihilation DMN Interaction Relic Density Indirect Detection Direct Detection Astrophysical and Cosmological Inputs S. Su 35

Synergy parts per mille agreement for Ω χ discovery of dark matter Collider Inputs Weakscale Parameters local DM density and velocity profile DM Annihilation DMN Interaction Relic Density Indirect Detection Direct Detection Astrophysical and Cosmological Inputs S. Su 35

Conclusion SM in particle physics is a successful framework S. Su 36

Conclusion SM in particle physics is a successful framework New physics beyond the SM: origin of masses Superymmetry, extra dimensions, strong dynamics... Current and future colliders: explore energy frontier We now know the composition of the Universe No known particle in the SM can be DM precise, unambiguous evidence for new physics New physics new stable particle as DM candidate Many dark matter candidates WIMP, WIMPless, superwimp,... Dark matter detection direct/indirect DM searches, collider studies S. Su 36

Conclusion SM in particle physics is a successful framework S. Su 36 New physics beyond the SM: origin of masses Superymmetry, extra dimensions, strong dynamics... Current and future colliders: explore energy frontier We now know the composition of the Universe No known particle in the SM can be DM precise, unambiguous evidence for new physics New physics new stable particle as DM candidate Many dark matter candidates WIMP, WIMPless, superwimp,... Dark matter detection direct/indirect DM searches, collider studies Synergy between astrophysics and particle phycics

The Coming decade is going to be very exciting in particle physics, astrophysics, and cosmology Stay tuned... S. Su 37