New Physics beyond the Standard Model: from the Earth to the Sky
|
|
|
- Bridget Baker
- 6 years ago
- Views:
Transcription
1 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
2 Let s start with the smallest scale: fundamental particles S. Su
3 Particle physics: the Standard Model S. Su Source: Fermilab media 3
4 Colliders: past and current Source: SLAC Source: CERN Source: Fermilab (SLD) e+e Ecm up to 90 GeV e+e Ecm up to 209 GeV Fermilab ppbar Ecm up to 1.96 TeV S. Su 4
5 Success of the SM All quarks, leptons and gauge bosons have been found. latest: top quark 173 GeV, Tevatron top D0 S. Su 5 Source: D0
6 precision test: results from various experiments agree well m W [GeV] August 2009 LEP2 and Tevatron (prel.) LEP1 and SLD 68% CL!" m H [GeV] Success of the SM Measurement Fit O meas!o fit /" meas #$ (5) had (m Z ) ± m Z [GeV] ± % Z [GeV] ± " 0 had [nb] ± R l ± A 0,l fb ± A l (P & ) ± R b ± R c ± A 0,b fb ± A 0,c fb ± A b ± A c ± A l (SLD) ± sin 2 ' lept eff (Q fb ) ± m W [GeV] ± % W [GeV] ± m t [GeV] ± S. Su March m t [GeV] LEPEWWG
7 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
8 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
9 Masses How do particles get masses? S. Su 8
10 Origin of the mass: Higgs mechanism S. Su 9
11 Origin of the mass: Higgs mechanism We have not found the Higgs boson yet... S. Su 9
12 Tevatron and the LHC CERN 2009 xxx pp Ecm up to 14 TeV Source: Fermilab Fermilab ppbar Ecm up to 1.96 TeV S. Su 10 Source: CERN
13 Higgs the LHC CMS S. Su 11 Source: CERN
14 the LHC S. Su 12
15 the LHC NOT THAT EASY! S. Su 12
16 the LHC NOT THAT EASY! 1 Higgs in 800,000,000 particles S. Su 12
17 S. Su 13
18 Higgs with Higgs S. Su 13
19 New problems... SM is an effective theory below the electroweak scale mweak 10 2 GeV, Λcutoff = mpl GeV Higgs is a fundamental scalar particle It receives huge quantum corrections from vacuum fluctuations (mh 2 )physical (mh 2 )bare + Λcutoff 2 S. Su 14
20 New problems... SM is an effective theory below the electroweak scale mweak 10 2 GeV, Λcutoff = mpl 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
21 New problems... SM is an effective theory below the electroweak scale mweak 10 2 GeV, Λcutoff = mpl 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 14
22 New problems... SM is an effective theory below the electroweak scale mweak 10 2 GeV, Λcutoff = mpl 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 +(10 18 GeV) 2 S. Su 14
23 New problems... SM is an effective theory below the electroweak scale mweak 10 2 GeV, Λcutoff = mpl 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 +(10 18 GeV) 2 cancellation of 32 orders of magnitude: unnatural naturalness problem/hierarchy problem S. Su 14
24 Solutions: symmetry SM is an effective theory below the electroweak scale mew 10 2 GeV, Λcutoff = mpl 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
25 Solutions: symmetry SM is an effective theory below the electroweak scale mew 10 2 GeV, Λcutoff = mpl 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
26 Solutions: symmetry SM is an effective theory below the electroweak scale mew 10 2 GeV, Λcutoff = mpl 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
27 Solutions: symmetry SM is an effective theory below the electroweak scale mew 10 2 GeV, Λcutoff = mpl 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
28 Solutions: symmetry SM is an effective theory below the electroweak scale mew 10 2 GeV, Λcutoff = mpl 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
29 Solutions: extra dimensions SM is an effective theory below the electroweak scale mew 10 2 GeV, Λcutoff = mpl 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
30 Solutions: extra dimensions SM is an effective theory below the electroweak scale mew 10 2 GeV, Λcutoff = mpl 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
31 Solutions: extra dimensions SM is an effective theory below the electroweak scale mew 10 2 GeV, Λcutoff = mpl 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
32 Solutions: extra dimensions SM is an effective theory below the electroweak scale mew 10 2 GeV, Λcutoff = mpl 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 + (10 2 GeV) 2 Λcutoff 10 2 GeV S. Su 16
33 Solutions: extra dimensions SM is an effective theory below the electroweak scale mew 10 2 GeV, Λcutoff = mpl 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 + (10 2 GeV) 2 Λcutoff 10 2 GeV Extra dimension S. Su 16
34 Solutions: strong dynamics SM is an effective theory below the electroweak scale mew 10 2 GeV, Λcutoff = mpl 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 17
35 Solutions: strong dynamics SM is an effective theory below the electroweak scale mew 10 2 GeV, Λcutoff = mpl 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 17
36 Solutions: strong dynamics SM is an effective theory below the electroweak scale mew 10 2 GeV, Λcutoff = mpl 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
37 New Phenomenon supersymmetry: supersymmetric particles Extra dimensions: KluzaKlein particles Source: ppt/susy.htm Technicolor: techni π, techni ρ Many other new scenarios, new particles and new forces... S. Su 18
38 the 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
39 Now let s look at the largest scale: the Universe S. Su
40 Observations Supernovae CMB (Photo courtesy of Maruša Bradač.) S. Su 21
41 Synthesis only 4% is known S. Su 22
42 Synthesis only 4% is known S. Su 22
43 Dark matter Source: Fermilab media CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting S. Su 23
44 Dark matter Source: Fermilab media CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting S. Su 23
45 Dark matter Source: Fermilab media CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting S. Su 23
46 Dark matter Source: Fermilab media CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting S. Su 23
47 Dark matter Source: Fermilab media CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting S. Su 23
48 Dark matter Source: Fermilab media CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting S. Su 23
49 Dark matter Source: Fermilab media CDM requirements Stable Nonbaryonic Neutral Cold (massive) Correct density Gravitational interacting S. Su 23
50 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
51 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
52 Zoo of dark matter mass and interaction strengths span many, many orders of magnitude Some Dark Matter Candidate Particles! int (pb) 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 Black Hole Remnant S. Su mass (GeV) 25
53 Zoo of dark matter mass and interaction strengths span many, many orders of magnitude Some Dark Matter Candidate Particles! int (pb) 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 Black Hole Remnant S. Su mass (GeV) 25
54 Zoo of dark matter mass and interaction strengths span many, many orders of magnitude Some Dark Matter Candidate Particles! int (pb) 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 Black Hole Remnant S. Su mass (GeV) 25
55 Zoo of dark matter mass and interaction strengths span many, many orders of magnitude Some Dark Matter Candidate Particles! int (pb) 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 Black Hole Remnant S. Su mass (GeV) 25
56 Zoo of dark matter mass and interaction strengths span many, many orders of magnitude Some Dark Matter Candidate Particles! int (pb) 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 Black Hole Remnant appear in particle physics models motivated independently by attempts to solve EWSB relic density are determined by m pl and m weak naturally around the observed value no need to introduce and adjust new energy scale S. Su mass (GeV) 25
57 WIMP WIMP: Weak Interacting Massive Particle Boltzmann equation WIMP Source: Kolb and Turner S. Su 26
58 WIMP miracle WIMP: Weak Interacting Massive Particle m WIMP m weak σ an α weak 2 m weak 2 Ω h 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
59 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
60 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
61 WIMPless? Ω X 1 σv m2 X g 4 X mx/gx 2 mweak/gweak 2, Ωh only fixes one combination of dark matter mass and coupling could have mx mweak as long as the relation holds S. Su 29
62 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
63 Hidden dark matter collider DM p p Y Y b DM b Y particle appears at LHC as exotic 4th generation quarks S. Su
64 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
65 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
66 Nonthermal production: WIMP decay WIMP superwimp + SM particles WIMP S. Su 33
67 Nonthermal production: WIMP decay WIMP superwimp + SM particles WIMP S. Su 33
68 Nonthermal production: WIMP decay WIMP superwimp + SM particles SWIMP SM S. Su 33
69 Nonthermal production: WIMP decay WIMP superwimp + SM particles S. Su 33
70 Nonthermal production: WIMP decay WIMP superwimp + SM particles O(1) S. Su 33
71 Nonthermal production: WIMP decay WIMP superwimp + SM particles superwimp O(1) e.g. Gravitino LSP LKK graviton axino WIMP neutral charged S. Su 33
72 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
73 Synergy S. Su 35
74 Synergy Collider Inputs Weakscale Parameters DM Annihilation DMN Interaction S. Su 35
75 Synergy Collider Inputs Weakscale Parameters DM Annihilation DMN Interaction Relic Density Indirect Detection Direct Detection Astrophysical and Cosmological Inputs S. Su 35
76 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
77 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
78 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 eliminate particle physics uncertainty do real astrophysics S. Su 35
79 Conclusion SM in particle physics is a successful framework S. Su 36
80 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 S. Su 36
81 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
82 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
83 The Coming decade is going to be very exciting in particle physics, astrophysics, and cosmology Stay tuned... S. Su 37
Dark Matter WIMP and SuperWIMP
Dark Matter WIMP and SuperWIMP Shufang Su U. of Arizona S. Su Dark Matters Outline Dark matter evidence New physics and dark matter WIMP candidates: neutralino LSP in MSSM direct/indirect DM searches,
DARK MATTERS. Jonathan Feng University of California, Irvine. 2 June 2005 UCSC Colloquium
DARK MATTERS Jonathan Feng University of California, Irvine 2 June 2005 UCSC Colloquium 2 June 05 Graphic: Feng N. Graf 1 WHAT IS THE UNIVERSE MADE OF? An age old question, but Recently there have been
Beyond the WIMP Miracle
Beyond the WIMP Miracle Shufang Su U. of Arizona S. Su PittPACC LDM workshop Nov 16, 2011 Beyond the WIMP Miracle WIMP miracle WIMPless general framework light dark matter collider signature superwimp
Kaluza-Klein Theories - basic idea. Fig. from B. Greene, 00
Kaluza-Klein Theories - basic idea Fig. from B. Greene, 00 Kaluza-Klein Theories - basic idea mued mass spectrum Figure 3.2: (Taken from [46]). The full spectrum of the UED model at the first KK level,
Dark matter: evidence and candidates
.... Dark matter: evidence and candidates Zhao-Huan Yu ( 余钊焕 ) Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, CAS March 14, 2014 Zhao-Huan Yu (IHEP) Dark matter: evidence and
SUPERSYMMETRIC DARK MATTER
SUPERSYMMETRIC DARK MATTER Jonathan Feng University of California, Irvine 11 May 2007 Fermilab Wine & Cheese Hunt for DM Workshop 11 May 07 Feng 1 Dark Matter Ω DM h 2 = 0.105 ± 0.004 (WMAP, SDSS) Best
RECENT DEVELOPMENTS IN PARTICLE DARK MATTER
RECENT DEVELOPMENTS IN PARTICLE DARK MATTER KISS Dark Matter Workshop 15 July 2009 Jonathan Feng UC Irvine Feng 1 EVIDENCE FOR DARK MATTER There is now overwhelming evidence that normal (standard model)
The Standard Model and Beyond
The Standard Model and Beyond Nobuchika Okada Department of Physics and Astronomy The University of Alabama 2011 BCVSPIN ADVANCED STUDY INSTITUTE IN PARTICLE PHYSICS AND COSMOLOGY Huê, Vietnam, 25-30,
SUPERSYMETRY FOR ASTROPHYSICISTS
Dark Matter: From the Cosmos to the Laboratory SUPERSYMETRY FOR ASTROPHYSICISTS Jonathan Feng University of California, Irvine 29 Jul 1 Aug 2007 SLAC Summer Institute 30 Jul 1 Aug 07 Feng 1 Graphic: N.
SUSY AND COSMOLOGY. Jonathan Feng UC Irvine. SLAC Summer Institute 5-6 August 2003
SUSY AND COSMOLOGY Jonathan Feng UC Irvine SLAC Summer Institute 5-6 August 2003 Target Audience From the organizers: graduate students, junior postdocs ¾ experimentalists, ¼ theorists Students enjoy the
DARK MATTER. Martti Raidal NICPB & University of Helsinki Tvärminne summer school 1
DARK MATTER Martti Raidal NICPB & University of Helsinki 28.05.2010 Tvärminne summer school 1 Energy budget of the Universe 73,4% - Dark Energy WMAP fits to the ΛCDM model Distant supernova 23% - Dark
COSMOLOGY AT COLLIDERS
COSMOLOGY AT COLLIDERS Jonathan Feng University of California, Irvine 23 September 2005 SoCal Strings Seminar 23 September 05 Graphic: Feng N. Graf 1 COSMOLOGY NOW We are living through a revolution in
Dark Matter in Particle Physics
High Energy Theory Group, Northwestern University July, 2006 Outline Framework - General Relativity and Particle Physics Observed Universe and Inference Dark Energy, (DM) DM DM Direct Detection DM at Colliders
IMPLICATIONS OF PARTICLE PHYSICS FOR COSMOLOGY
IMPLICATIONS OF PARTICLE PHYSICS FOR COSMOLOGY Jonathan Feng University of California, Irvine 28-29 July 2005 PiTP, IAS, Princeton 28-29 July 05 Feng 1 Graphic: N. Graf OVERVIEW This Program anticipates
Kaluza-Klein Dark Matter
Kaluza-Klein Dark Matter Hsin-Chia Cheng UC Davis Pre-SUSY06 Workshop Complementary between Dark Matter Searches and Collider Experiments Introduction Dark matter is the best evidence for physics beyond
Theoretical Aspects on Dark Matter and Its Detection
Theoretical Aspects on Dark Matter and Its Detection Shufang Su U. of Arizona S. Su Dark Matters IWDD09, Shanghai June 15, 2009 Outline Dark matter evidence New physics and dark matter Dark matter candidates
MICROPHYSICS AND THE DARK UNIVERSE
MICROPHYSICS AND THE DARK UNIVERSE Jonathan Feng University of California, Irvine CAP Congress 20 June 2007 20 June 07 Feng 1 WHAT IS THE UNIVERSE MADE OF? Recently there have been remarkable advances
Lecture 18 - Beyond the Standard Model
Lecture 18 - Beyond the Standard Model Why is the Standard Model incomplete? Grand Unification Baryon and Lepton Number Violation More Higgs Bosons? Supersymmetry (SUSY) Experimental signatures for SUSY
Search for SUperSYmmetry SUSY
PART 3 Search for SUperSYmmetry SUSY SUPERSYMMETRY Symmetry between fermions (matter) and bosons (forces) for each particle p with spin s, there exists a SUSY partner p~ with spin s-1/2. q ~ g (s=1)
LHC Impact on DM searches
LHC Impact on DM searches Complementarity between collider and direct searches for DM Outline Introduction (complementarity of DM searches) Dark Matter signals at the LHC (missing ET, jets, etc... ) Particular
RECENT PROGRESS IN SUSY DARK MATTER
RECENT PROGRESS IN SUSY DARK MATTER Jonathan Feng University of California, Irvine 12 April 2006 Texas A&M Mitchell Symposium 12 Apr 06 Graphic: Feng N. Graf 1 Supersymmetric dark matter has been around
November 24, Scalar Dark Matter from Grand Unified Theories. T. Daniel Brennan. Standard Model. Dark Matter. GUTs. Babu- Mohapatra Model
Scalar from November 24, 2014 1 2 3 4 5 What is the? Gauge theory that explains strong weak, and electromagnetic forces SU(3) C SU(2) W U(1) Y Each generation (3) has 2 quark flavors (each comes in one
Dark Matter Implications for SUSY
Dark Matter Implications for SUSY Sven Heinemeyer, IFCA (CSIC, Santander) Madrid, /. Introduction and motivation. The main idea 3. Some results 4. Future plans Sven Heinemeyer, First MultiDark workshop,
DARK MATTER MEETS THE SUSY FLAVOR PROBLEM
DARK MATTER MEETS THE SUSY FLAVOR PROBLEM Work with Manoj Kaplinghat, Jason Kumar, John Learned, Arvind Rajaraman, Louie Strigari, Fumihiro Takayama, Huitzu Tu, Haibo Yu Jonathan Feng University of California,
Constraining minimal U(1) B L model from dark matter observations
Constraining minimal U(1) B L model from dark matter observations Tanushree Basak Physical Research Laboratory, India 10th PATRAS Workshop on Axions, WIMPs and WISPs CERN Geneva, Switzerland July 3, 2014
Beyond the SM: SUSY. Marina Cobal University of Udine
Beyond the SM: SUSY Marina Cobal University of Udine Why the SM is not enough The gauge hierarchy problem Characteristic energy of the SM: M W ~100 GeV Characteristic energy scale of gravity: M P ~ 10
Astroparticle Physics at Colliders
Astroparticle Physics at Colliders Manuel Drees Bonn University Astroparticle Physics p. 1/29 Contents 1) Introduction: A brief history of the universe Astroparticle Physics p. 2/29 Contents 1) Introduction:
New Physics at the TeV Scale and Beyond Summary
New Physics at the TeV Scale and Beyond Summary Machine and Detector Issues 1. Correlated Beamstrahlung David Strom New Theoretical Ideas: 1. Signatures for Brane Kinetic Terms at the LC Tom Rizzo 2. Implementing
SuperWeakly Interacting Massive Particle Dark Matter
SuperWeakly Interacting Massive Particle Dark Matter Fumihiro Takayama Institute for High Energy Phenomenology, Cornell University @Chicago(12 th December 2005) Dark matter is one of the best evidence
Physics at e + e - Linear Colliders. 4. Supersymmetric particles. M. E. Peskin March, 2002
Physics at e + e - Linear Colliders 4. Supersymmetric particles M. E. Peskin March, 2002 In this final lecture, I would like to discuss supersymmetry at the LC. Supersymmetry is not a part of the Standard
The WIMPless Miracle and the DAMA Puzzle
The WIMPless Miracle and the DAMA Puzzle Jason Kumar University of Hawaii w/ Jonathan Feng, John Learned and Louis Strigari (0803.4196,0806.3746,0808.4151) Relic Density matter in early universe in thermal
WIMPs and superwimps. Jonathan Feng UC Irvine. MIT Particle Theory Seminar 17 March 2003
WIMPs and superwimps Jonathan Feng UC Irvine MIT Particle Theory Seminar 17 March 2003 Dark Matter The dawn (mid-morning?) of precision cosmology: Ω DM = 0.23 ± 0.04 Ω total = 1.02 ± 0.02 Ω baryon = 0.044
Neutralino Dark Matter and SUSY Spectroscopy. M. E. Peskin June 2004 YITP
Neutralino Dark Matter and SUSY Spectroscopy M. E. Peskin June 2004 YITP - 2004 The prediction of cosmic dark matter is an important argument for the presence of SUSY in Nature. This is a robust prediction
Physics at the TeV Scale Discovery Prospects Using the ATLAS Detector at the LHC
Physics at the TeV Scale Discovery Prospects Using the ATLAS Detector at the LHC Peter Krieger Carleton University Physics Motivations Experimental Theoretical New particles searches Standard Model Higgs
Astroparticle Physics and the LC
Astroparticle Physics and the LC Manuel Drees Bonn University Astroparticle Physics p. 1/32 Contents 1) Introduction: A brief history of the universe Astroparticle Physics p. 2/32 Contents 1) Introduction:
SUSY Phenomenology & Experimental searches
SUSY Phenomenology & Experimental searches Slides available at: Alex Tapper http://www.hep.ph.ic.ac.uk/~tapper/lecture.html Objectives - Know what Supersymmetry (SUSY) is - Understand qualitatively the
Staus at the LHC. Koichi Hamaguchi (Tokyo U.) based on the works. KH, M.M.Nojiri, A.de Roeck (hep-ph/ );
Staus at the LHC Koichi Hamaguchi (Tokyo U.) at KEKPH 7, based on the works KH, M.M.Nojiri, A.de Roeck (hep-ph/6126); KH, M.M.Nojiri, Y.Kuno, T.Nakaya ( 4); W.Buchmüller, KH, M.Ratz, T.Yanagida ( 4); Mar.
Why SUSY? Key Words LECTURE OUTLINE. Between Supersymmetry and Dark Matter Teruki Kamon KNU/TAMU. Probing the Connection.
Why SUSY? Beyond the SM: Probing the Connection Between Supersymmetry and Dark Matter Teruki Kamon KNU/TAMU This is what I said at Lecture 00. Course Description Since March 00, the Large Hadron Collider
Physics at the ILC. Ariane Frey, MPI München 38. Herbstschule Maria Laach Ariane Frey, MPI München
Physics at the ILC Beyond the Standard Model: Supersymmetry Extra Dimensions Heavy Z, Z, Strong EWSB Precision Physics (top, W, ) CLIC top, W LHC ILC Synergy Ariane Frey, MPI München 1 Higgs Profile Use
Cosmological Constraint on the Minimal Universal Extra Dimension Model
Cosmological Constraint on the Minimal Universal Extra Dimension Model Mitsuru Kakizaki (Bonn University) September 7, 2007 @ KIAS In collaboration with Shigeki Matsumoto (Tohoku Univ.) Yoshio Sato (Saitama
Supersymmetry and other theories of Dark Matter Candidates
Supersymmetry and other theories of Dark Matter Candidates Ellie Lockner 798G Presentation 3/1/07 798G 3/1/07 1 Overview Why bother with a new theory? Why is Supersymmetry a good solution? Basics of Supersymmetry
Searches for Physics Beyond the Standard Model. Jay Wacker. APS April Meeting SLAC. A Theoretical Perspective. May 4, 2009
Searches for Physics Beyond the Standard Model A Theoretical Perspective Jay Wacker SLAC APS April Meeting May 4, 2009 1 The Plan Motivations for Physics Beyond the Standard Model New Hints from Dark Matter
Discovery Physics at the Large Hadron Collider
+ / 2 GeV N evt 4 10 3 10 2 10 CMS 2010 Preliminary s=7 TeV -1 L dt = 35 pb R > 0.15 R > 0.20 R > 0.25 R > 0.30 R > 0.35 R > 0.40 R > 0.45 R > 0.50 10 1 100 150 200 250 300 350 400 [GeV] M R Discovery
Contributions by M. Peskin, E. Baltz, B. Sadoulet, T. Wizansky
Contributions by M. Peskin, E. Baltz, B. Sadoulet, T. Wizansky Dark Matter established as major component of the Universe: CMB determination of its relic density further confirmed by SNs and galaxy clusters;
Probing Supersymmetric Connection with Dark Matter
From サイエンス 82 Probing Supersymmetric Connection with Dark Matter Taken from Science, 1982 Teruki Kamon Department of Physics Texas A&M University November 3, 2005 Physics Colloquium, Texas Tech University
Beyond the Standard Model
Beyond the Standard Model The Standard Model Problems with the Standard Model New Physics Supersymmetry Extended Electroweak Symmetry Grand Unification References: 2008 TASI lectures: arxiv:0901.0241 [hep-ph]
Testing the Standard Model and Search for New Physics with CMS at LHC
Dezső Horváth: Search for New Physics with CMS FFK2017, Warsaw, Poland p. 1 Testing the Standard Model and Search for New Physics with CMS at LHC FFK-2017: International Conference on Precision Physics
Models of New Physics for Dark Matter
Models of New Physics for Dark Matter Carlos Muñoz instituto de física teórica ift-uam/csic departamento de física teórica dft-uam 1 PPC 2010, Torino, July 12-16 Crucial Moment for SUSY in next few years:
Little Higgs Models Theory & Phenomenology
Little Higgs Models Theory Phenomenology Wolfgang Kilian (Karlsruhe) Karlsruhe January 2003 How to make a light Higgs (without SUSY) Minimal models The Littlest Higgs and the Minimal Moose Phenomenology
Particle Physics and Cosmology II: Dark Matter
Particle Physics and Cosmology II: Dark Matter Mark Trodden Center for Particle Cosmology University of Pennsylvania Second Lecture Puerto Vallarta Mexico 1/13/2011 Problems of Modern Cosmology Is cosmic
Open Questions in Particle Physics. Carlos Wagner Physics Department, EFI and KICP, Univ. of Chicago HEP Division, Argonne National Laboratory
Open Questions in Particle Physics Carlos Wagner Physics Department, EFI and KICP, Univ. of Chicago HEP Division, Argonne National Laboratory Society of Physics Students, Univ. of Chicago, Nov. 21, 2016
components Particle Astrophysics, chapter 7
Dark matter and dark energy components Particle Astrophysics, chapter 7 Overview lecture 3 Observation of dark matter as gravitational ti effects Rotation curves galaxies, mass/light ratios in galaxies
DARK MATTER FROM THE EARLY UNIVERSE AND PARTICLE PHYSICS CANDIDATES
DARK MATTER FROM THE EARLY UNIVERSE AND PARTICLE PHYSICS CANDIDATES Jonathan Feng, UC Irvine Dark Matter Universe: On the Threshold of Discovery NAS Sackler Colloquium, Irvine, 18-20 October 2012 19 Oct
The first year of the LHC and Theory. G.G.Ross, Krakow, December 09
The first year of the LHC and Theory G.G.Ross, Krakow, December 09 The LHC a discovery machine The gauge sector : new gauge bosons? The maber sector : new quarks and leptons? The scalar sector : the hierarchy
Foundations of Physics III Quantum and Particle Physics Lecture 13
Foundations of Physics III Quantum and Particle Physics Lecture 13 Frank Krauss February 27, 2012 1 Construction of the Standard Model 2 The Standard Model: Tests and status 3 Beyond the Standard Model?
PHY323:Lecture 11 SUSY and UED Higgs and Supersymmetry The Neutralino Extra Dimensions How WIMPs interact
PHY323:Lecture 11 SUSY and UED Higgs and Supersymmetry The Neutralino Extra Dimensions How WIMPs interact Candidates for Dark Matter III The New Particle Zoo Here are a few of the candidates on a plot
SUSY or not, what is the evidence? Status and perspectives of collider searches Part III
SUSY or not, what is the evidence? Status and perspectives of collider searches Part III (pralavor@cppm.in2p3.fr) CPPM/IN2P3 Univ. de la Méditerranée (Marseille, FRANCE) Lectures at Niels Bohr Institute
Beyond the Standard Model Phenomenology. DOE Review 2008 Progress Report. Shufang Su U. of Arizona
Beyond the Standard Model Phenomenology DOE Review 2008 Progress Report Shufang Su U. of Arizona S. Su DOE Review, 2008 Low energy Precision measurement LEP Experiments Tevatron (now) LC LHC (2008( 2008)
Dark Matter Decay and Cosmic Rays
Dark Matter Decay and Cosmic Rays Christoph Weniger Deutsches Elektronen Synchrotron DESY in collaboration with A. Ibarra, A. Ringwald and D. Tran see arxiv:0903.3625 (accepted by JCAP) and arxiv:0906.1571
Searches for Beyond SM Physics with ATLAS and CMS
Searches for Beyond SM Physics with ATLAS and CMS (University of Liverpool) on behalf of the ATLAS and CMS collaborations 1 Why beyond SM? In 2012 the Standard Model of Particle Physics (SM) particle content
Pseudo-Dirac Bino as Dark Matter and Signatures of D-Type G
and Signatures of D-Type Gauge Mediation Ken Hsieh Michigan State Univeristy KH, Ph. D. Thesis (2007) ArXiv:0708.3970 [hep-ph] Other works with M. Luty and Y. Cai (to appear) MSU HEP Seminar November 6,
Kiwoon Choi (KAIST) 3 rd GCOE Symposium Feb (Tohoku Univ.)
Exploring New Physics beyond the Standard Model of Particle Physics Kiwoon Choi (KAIST) 3 rd GCOE Symposium Feb. 2011 (Tohoku Univ.) We are confronting a critical moment of particle physics with the CERN
Potential Discoveries at the Large Hadron Collider. Chris Quigg
Potential Discoveries at the Large Hadron Collider Chris Quigg Fermilab quigg@fnal.gov XXIII Taiwan Spring School Tainan 31 March - 3 April 2010 Electroweak theory successes Theoretical Physics Department,
MSSM4G: MOTIVATIONS AND ALLOWED REGIONS
MSSM4G: MOTIVATIONS AND ALLOWED REGIONS ATLAS SUSY WG Meeting CERN Jonathan Feng, University of California, Irvine 31 January 2018 Based on 1510.06089, 1608.00283 with Mohammad Abdullah (Texas A&M), Sho
Higgs Physics. Yasuhiro Okada (KEK) November 26, 2004, at KEK
Higgs Physics Yasuhiro Okada (KEK) November 26, 2004, at KEK 1 Higgs mechanism One of two principles of the Standard Model. Gauge invariance and Higgs mechanism Origin of the weak scale. Why is the weak
Naturalness and mixed axion-higgsino dark matter
Naturalness and mixed axion-higgsino dark matter Howard Baer University of Oklahoma UCLA DM meeting, Feb. 18, 2016 ADMX What is the connection? LZ The naturalness issue: Naturalness= no large unnatural
SUSY at Accelerators (other than the LHC)
SUSY at Accelerators (other than the LHC) Beate Heinemann, University of Liverpool Introduction Final LEP Results First Tevatron Run 2 Results Summary and Outlook IDM 2004, Edinburgh, September 2004 Why
Week 3 - Part 2 Recombination and Dark Matter. Joel Primack
Astro/Phys 224 Spring 2012 Origin and Evolution of the Universe Week 3 - Part 2 Recombination and Dark Matter Joel Primack University of California, Santa Cruz http://pdg.lbl.gov/ In addition to the textbooks
Searching for sneutrinos at the bottom of the MSSM spectrum
Searching for sneutrinos at the bottom of the MSSM spectrum Arindam Chatterjee Harish-Chandra Research Insitute, Allahabad In collaboration with Narendra Sahu; Nabarun Chakraborty, Biswarup Mukhopadhyay
Physics 662. Particle Physics Phenomenology. February 21, Physics 662, lecture 13 1
Physics 662 Particle Physics Phenomenology February 21, 2002 Physics 662, lecture 13 1 Physics Beyond the Standard Model Supersymmetry Grand Unified Theories: the SU(5) GUT Unification energy and weak
Probing the Connection Between Supersymmetry and Dark Matter
Probing the Connection Between Supersymmetry and Dark Matter Bhaskar Dutta Texas A&M University Physics Colloquium, OSU, March 30, 2006 March 30, 2006 Probing the Connection Between SUSY and Dark Matter
The Matter-Antimatter Asymmetry and New Interactions
The Matter-Antimatter Asymmetry and New Interactions The baryon (matter) asymmetry The Sakharov conditions Possible mechanisms A new very weak interaction Recent Reviews M. Trodden, Electroweak baryogenesis,
Determination of Non-Universal Supergravity Models at the LHC
Determination of Non-Universal Supergravity Models at the LHC B. Dutta 1, T. Kamon 1, 2, 3, N. Kolev 4, *, A. Krislock 1, Y. Oh 3 1 Texas A&M U., 2 Fermilab, 3 Kyungpook National U., 4 U. of Regina * kolev20n@uregina.ca
Gravitino LSP as Dark Matter in the Constrained MSSM
Gravitino LSP as Dark Matter in the Constrained MSSM Ki Young Choi The Dark Side of the Universe, Madrid, 20-24 June 2006 Astro-Particle Theory and Cosmology Group The University of Sheffield, UK In collaboration
SUSY and Exotics. UK HEP Forum"From the Tevatron to the LHC, Cosener s House, May /05/2009 Steve King, UK HEP Forum '09, Abingdon 1
SUSY and Exotics Standard Model and the Origin of Mass Puzzles of Standard Model and Cosmology Bottom-up and top-down motivation Extra dimensions Supersymmetry - MSSM -NMSSM -E 6 SSM and its exotics UK
Searches for New Phenomena with Lepton Final States at the Tevatron
Searches for New Phenomena with Lepton Final States at the Tevatron including charginos, neutralinos,, excited leptons and unexpected signatures Todd Adams Florida State University for the CDF and DØ Collaborations
Crosschecks for Unification
Crosschecks for Unification Hans Peter Nilles Physikalisches Institut Universität Bonn Crosschecks for Unification, Planck09, Padova, May 2009 p. 1/39 Questions Do present observations give us hints for
Project Paper May 13, A Selection of Dark Matter Candidates
A688R Holly Sheets Project Paper May 13, 2008 A Selection of Dark Matter Candidates Dark matter was first introduced as a solution to the unexpected shape of our galactic rotation curve; instead of showing
PAMELA from Dark Matter Annihilations to Vector Leptons
PAMELA from Dark Matter Annihilations to Vector Leptons phalendj@umich.edu With Aaron Pierce and Neal Weiner University of Michigan LHC and Dark Matter Workshop 2009 University of Michigan Outline PAMELA
Astronomy 182: Origin and Evolution of the Universe
Astronomy 182: Origin and Evolution of the Universe Prof. Josh Frieman Lecture 12 Nov. 18, 2015 Today Big Bang Nucleosynthesis and Neutrinos Particle Physics & the Early Universe Standard Model of Particle
Beyond the Standard Model Phenomenology. Shufang Su U. of Arizona
Beyond the Standard Model Phenomenology DOE Review 2009 Shufang Su U. of Arizona Copyright S. Su CERN DOE Review, 2009 (Photo courtesy of Maruša Bradač.) Low energy Precision measurement LEP Experiments
SUSY at Accelerators (other than the LHC)
SUSY at Accelerators (other than the LHC) Beate Heinemann, University of Liverpool Introduction Final LEP Results First Tevatron Run 2 Results Summary and Outlook IDM 2004, Edinburgh, September 2004 Why
IX. Electroweak unification
IX. Electroweak unification The problem of divergence A theory of weak interactions only by means of W ± bosons leads to infinities e + e - γ W - W + e + W + ν e ν µ e - W - µ + µ Divergent integrals Figure
Higgs Signals and Implications for MSSM
Higgs Signals and Implications for MSSM Shaaban Khalil Center for Theoretical Physics Zewail City of Science and Technology SM Higgs at the LHC In the SM there is a single neutral Higgs boson, a weak isospin
Axino Phenomenology in the Kim-Nilles mechanism
CP3, SDU, Odense, 11 Aug. 2014 Axino Phenomenology in the Kim-Nilles mechanism Eung Jin Chun Outline Introduction to strong CP problem & axion. KSVZ & DFSZ axion models. Supersymmetric axion models and
Electroweak and Higgs Physics
Electroweak and Higgs Physics Lecture 2 : Higgs Mechanism in the Standard and Supersymmetric Models Alexei Raspereza DESY Summer Student Program Hamburg August 2017 Standard Model (Summary) Building blocks
Lecture 12. Dark Matter. Part II What it could be and what it could do
Dark Matter Part II What it could be and what it could do Theories of Dark Matter What makes a good dark matter candidate? Charge/color neutral (doesn't have to be though) Heavy We know KE ~ kev CDM ~
The mass of the Higgs boson
The mass of the Higgs boson LHC : Higgs particle observation CMS 2011/12 ATLAS 2011/12 a prediction Higgs boson found standard model Higgs boson T.Plehn, M.Rauch Spontaneous symmetry breaking confirmed
Origin of the Universe - 2 ASTR 2120 Sarazin. What does it all mean?
Origin of the Universe - 2 ASTR 2120 Sarazin What does it all mean? Fundamental Questions in Cosmology 1. Why did the Big Bang occur? 2. Why is the Universe old? 3. Why is the Universe made of matter?
Supersymmetry Basics. J. Hewett SSI J. Hewett
Supersymmetry Basics J. Hewett SSI 2012 J. Hewett Basic SUSY References A Supersymmetry Primer, Steve Martin hep-ph/9709356 Theory and Phenomenology of Sparticles, Manual Drees, Rohini Godbole, Probir
Introduction to particle physics Lecture 13: The Standard Model
Introduction to particle physics Lecture 13: The Standard Model Frank Krauss IPPP Durham U Durham, Epiphany term 2010 1 / 23 Outline 1 The Standard Model: Construction 2 The Standard Model: Tests and status
A Century of Physics
A Century of Physics The 20th century witnessed the triumph physics From the discovery of the electron and the nucleus To the development of relativity and quantum mechanics We now have an understanding
Is SUSY still alive? Dmitri Kazakov JINR
2 1 0 2 The l o o h c S n a e p o r Eu y g r e n E h g i of H s c i s y PAnhjou, France 2 1 0 2 e n 6 19 Ju Is SUSY still alive? Dmitri Kazakov JINR 1 1 Why do we love SUSY? Unifying various spins SUSY
Dark Matter and Dark Energy components chapter 7
Dark Matter and Dark Energy components chapter 7 Lecture 3 See also Dark Matter awareness week December 2010 http://www.sissa.it/ap/dmg/index.html The early universe chapters 5 to 8 Particle Astrophysics,
The Linear Collider and the Preposterous Universe
The Linear Collider and the Preposterous Universe Sean Carroll, University of Chicago 5% Ordinary Matter 25% Dark Matter 70% Dark Energy Why do these components dominate our universe? Would an Apollonian
Introduction Motivation WIMP models. WIMP models. Sebastian Belkner. University of Bonn - University of Cologne. June 24, 2016
WIMP models Sebastian Belkner University of Bonn - University of Cologne June 24, 2016 1 / 27 A brief history of the universe 2 / 27 Outline 1 Motivation On galactic scales On cosmological scales 2 WIMP
Early SUSY Searches in Events with Leptons with the ATLAS-Detector
Early SUSY Searches in Events with Leptons with the ATLAS-Detector Timo Müller Johannes Gutenberg-Universität Mainz 2010-29-09 EMG Annual Retreat 2010 Timo Müller (Universität Mainz) Early SUSY Searches
Lecture 03. The Standard Model of Particle Physics. Part III Extensions of the Standard Model
Lecture 03 The Standard Model of Particle Physics Part III Extensions of the Standard Model Where the SM Works Excellent description of 3 of the 4 fundamental forces Explains nuclear structure, quark confinement,
A SUPERSYMMETRIC VIEW OF THE HIGGS HUNTING
UC @ Santa Barbara Feb. 2nd, 2011 A SUPERSYMMETRIC VIEW OF THE HIGGS HUNTING Tao Liu UC @ Santa Barbara Higgs Boson And Particle Physics The Standard Model (SM) is a successful theory of describing the
The Physics of Heavy Z-prime Gauge Bosons
The Physics of Heavy Z-prime Gauge Bosons Tevatron LHC LHC LC LC 15fb -1 100fb -1 14TeV 1ab -1 14TeV 0.5TeV 1ab -1 P - =0.8 P + =0.6 0.8TeV 1ab -1 P - =0.8 P + =0.6 χ ψ η LR SSM 0 2 4 6 8 10 12 2σ m Z'