Physics Beyond the SM Wim de Boer KIT

Physics Beyond the SM Wim de Boer, KIT Institut für Experimentelle Kernphysik KIT – University of the State of Baden-Wuerttemberg and National Research Center of the Helmholtz Association www. kit. edu

Outline Ø Lecture I (SM+Cosmology) Ø What are the essentials of a Grand Unified Theory (GUT)? Ø Which predictions follow from a GUT? Ø Dark energy and dark matter Ø Inflation and accelerated expansion of the universe Ø Lecture II (Supersymmetry) Ø Gauge and Yukawa coupling unification in SUSY Ø Prediction of electroweak symmetry breaking in SUSY Ø Prediction of the top mass in SUSY Ø Prediction of the Higgs mass in SUSY Ø Prospects for discovering SUSY Details in Many summerschool lectures on Supersymmetry in: http: //www-ekp. physik. uni-karlsruhe. de/~deboer/html/Lehre/Susy/ W. de Boer, hep-ph/9402266, ar. Xiv: 1309. 0721 Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 2

H Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 3

Force mediators Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 4

The SM particles Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 5

24 years of e+e- colliders 10 - u, d s Cross section [cm 2] 29 31 J/ Each peak described by Breit-Wigner resonance: Z c 10 - with width G=ħ t b 33 10 - 35 10 - At resonance: E=M, so high peak means long lifetime t WW + ZZ 37 10 -1 Wim de Boer 100 101 102 103 E [Ge. V] KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 6

LHC: broad range of CM energies and high luminosity (1 day LHC) Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 7

The SM interactions Gluons couple to colour (quarks, gluons) Particles in colour triplets, hence interactions invariant under global SU(3) rotations W, Z couple to weak isospin (quarks, leptons, W, Z) Particles in isospin doublets, hence interactions invariant under global SU(2) rotations Photons couple to electric charge (quarks, charged leptons, W). Invariant under U(1) rotations (=phase). Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 8

SM BASICS The SM is a relativistic field theory, based on local gauge invariance of the SU(n) groups. A shamrock is invariant under global SU(3) rotations What does this mean? Take the rotation group SU(3) A proton is a colour singlet, i. e. it has a red, green and blue quark. The proton is invariant under global SU(3) rotations, but requiring nature to be invariant under local rotations requires the introduction of coloured gluons, which counteract the local rotation. Mathematically local gauge invariance accomplished by introducing the covariant derivative Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 9

The Standard Model agrees with experiment Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 10

SU(n) needs n 2 -1 gauge bosons Since one can rotate locally any quark, one needs a gauge boson for countracting all possible local rotations for 3 colours (or 3 leafs) Need 9 Ggluons, since lin. comb. RR+GG+NBB inv. ->8 gluons ok RR RG RB GR GG GB BR BG BB Similarly for weak interaction: transitions of weak isospin in isospin doublets. Need for weak interactions only n 2 -1= 3 gauge bosons (W+, W-, Z 0) Wim de Boer e- n e- g, Z W´ n W- g, Z KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 11

Could Nature have SU(5)=SU(3)x. SU(2)XU(1) symmetry? e- n RR RG RB X 1 Y 1 GR GG GB X 2 Y 2 BR BG BB X 3 Y 3 e- X 1 X 2 X 3 g, Z W´ n Y 1 Y 2 Y 3 W- g, Z SU(5) symmetry suggested by Georgi&Glashow in 1974, thus unifying all SM forces (GUT). Predicts proton decay. Searched for, but not found. ( neutrino osc. discovered instead) Proton lifetime: Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 12

Could Nature have SU(5)=SU(3)x. SU(2)XU(1) symmetry? Correct linear combinations: Unification of gauge couplings in SM around 1015 Ge. V tp around 1031 a Idea: SU(5) breaks to SU(3)x. SU(2)XU(1) at unification scale, so X, Y get mass and do not play a role any more. Grand Unified Theory disappears. Non-observation of proton decay erased hope for GUT. In Supersymmetry: MX=2. 1016 Ge. V tp around 1034 a. Still being searched for. Wim de Boer LATER MORE ON RUNNING GAUGE COUPLINGS KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 13

Summary on GUTs A Grand Unified Theory unifies all SM interactions in a larger gauge group A larger gauge group has necessarily more gauge bosons and hence NEW FORCES (so additional forces present in early universe!) These forces not observed at low energy, so presumably new gauge bosons got mass, like W, Z bosons got mass via interactions with Higgs bosons after spontaneous breaking of the electroweak gauge symmetry SU(2)x. U(1) to U(1) Likewise new Higgs bosons at GUT scale by breaking SU(5) (or larger group like SO(10)) to SU(3)x. SU(2)XU(1), which gives mass to X, Y bosons Expect all interactions to have the same SU(5) gauge coupling as long as symmetry is not broken and all gauge bosons massless. We will work this out after 1) discussing need for physics beyond the SM from cosmology 2) why Supersymmetry fits so nicely all requirements for physics needed beyond the SM Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 14

Outline § Questions from Cosmology § Answers from Supersymmetry Details in Many lsummerschool ectures on Supersymmetry in: http: //www-ekp. physik. uni-karlsruhe. de/~deboer/html/Lehre/Susy/ W. de Boer, hep-ph/9402266, ar. Xiv: 1309. 0721 Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 15

The Big Bang and its energy 13. 7 billion years 95% of energy in universe of unknown nature Cosmology 380. 000 yrs Astroparticle physics Astronomy 1 ps Particle physics 10 -34 s Big Bang Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 16

Universe is a very active place During this lecture: 108 stars are created (in 1011 galaxies with 1011 stars each) The sun loses by radiation 1010 tons of its weight The sun radiates 1023 k. Wh The earth receives 1014 k. Wh This is the equivalent of 1013 Euros The energy prices are clearly too high Question: does Sun radiate also neutrinos? If yes, how would you calculate the flux? Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 17

Energy in the Universe From Planck satellite The „complete“ SM describes only 4. 9% of the energy in our universe. We know it is only 4. 9% from ratio of photons/baryons≈1010 which determines ratio heavy/light nuclei and CMB acoustic peaks (photons: 412/cm 3 everywhere for a CMB temperature of 2. 7 K) Repulsive gravity is caused by a constant energy density, like vacuum energy (Higgs field? ) or a cosmological constant Wim de Boer The dark side divided in two classes: Dark Matter with attractive gravity Dark Energy with repulsive gravity (Nobel prize 2011) KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 18

Energy density components in expanding universe Energy density ρradiation R-4 ρatom=0. 05 ρmatter R-3 =0. 27 ρcrit ρWIMP=0. 27 ρΛ =const. =0. 68ρcrit or ΩΛ = ρvacuum/ ρcrit =0. 68 Time Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 19

SDSS : ⅓ million galaxies Doppler shifts give galaxy velocities 3 b (~2 illion 0% lig to “ ht ye ars the edg e ”) Our galaxy is here Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 20

The Universe is EXPANDING (discovered already by Hubble some 80 years ago!) Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 21

View from galaxy A B A Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 22

View from galaxy B or car B overtaking A: B sees A moving away B A Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 23

Evolution of the universe R(t) determined by gravity It can be reconstructed from SNIa supernovae remnants, since R can be determined from luminosity and velocity (= slope d. R/dt) from the Doppler shift. One observes first a decelerating phase (attractive gravity) followed by an accelerating phase (repulsive gravity). Gravity repulsive if constant energy density (= vacuum energy? ) dominates. Can be calculated with non-rel. Newtonian mechanics Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 24

Gravity repulsive if CONSTANT energy dominates! Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 25

What is the critical density? (i. e. E=0) H=R/R Etot=0 H 2=8πGρcrit/3 ρcrit=3 H 2/8πG=2. 10 -29 g/cm 3 Define dimensionless density parameter: Ω=ρ/ρcrit=8πG/3 H 2 = ρ / ρcrit = B+ DM + =1 for flat universe Open univ. flat univ. closed univ. Wim de Boer Compare with rocket with U<T, U=T und U>T KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 26

Separation of DM and DE ( ) Perlmutter, Schmidt and Ries got NP for measuring acceleration of universe prop. to a M = 0. 7 Mather and Smoot got NP for measuring CMB anisotropy which later revealed that the universe is flat or 1 + M Combining results of the two orthogonal graphs yields M = 0. 3, DE = 0. 7 Matter = 0. 3 Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 27

Newest Planck Satellite data (2013) CMB without SNIa data already very precise Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 28

What is Dark Matter? a) DM is neutral (else electric fields) b) DM is weakly interacting (else it would clump in galactic center as baryonic matter c) DM is massive Therefore DM consists of WIMPs (Weakly Interacting Massive Particles) Wimps are Neutrinos? No, Galaxies cluster on small scales (in gravitational potential wells of DM) DM = non relativistic (“Cold DM”). Neutrinos would be “warm” or “hot” DM. WIMPs ARE NEW PARTICLES outside Standard Model NOT PRODUCED AT ACCELERATORS. BEST EVIDENCE FOR PHYSICS BEYOND THE SM! Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 29

Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 From M. Steinmetz, Potsdam 30

Discovery of DM in 1933 Zwicky, Fritz (1898 -1974 Center of the Coma Cluster by Hubble space telescope ©Dubinski Zwicky notes in 1933 that outlying galaxies in Coma cluster moving much faster than mass calculated for the visible galaxies would indicate Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 DM attracts galaxies with more force-> higher speed. But still bound! 31

Colliding Clusters Shed Light on Dark Matter Blue: dark matter from gravitationallensing Red: hot gas dunkel Rot: sichtbares Gas Observations with bullet cluster: • Chandra X-ray telescope shows distribution of hot gas • Hubble Space Telescope and others show distribution of dark matter from weak gravitational lensing • Distributions are clearly different after collision-> dark matter is weakly interacting! Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 32

Simulation of “Colliding Clusters” http: //www. sciam. com/ August 22, 2006 Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 33

Do we have Dark Matter in our Galaxy? rotation curve aolar system 1/ r Wim de Boer rotation curve Milky Way KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 34

Solution for flat rotation curve: non-baryonic DM Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 35

How do we measure the total energy density of the universe? In principle: the bending of light determines the energy density. In a flat universe the light moves on straight lines, which corresponds to the critical energy density This picture made Einstein famous Stars Sun Mond Moon Earth In 1919 moon in front of sun (eclipse), so Eddington could observe positions of stars behind the sun (expeditions to West-Africa and Brasil) According to Newton the angle : δ=0. 87 Grad According to Einstein: δ= 2 x 0. 87 Grad because of additional time dilatation by gravity Light on straight lines, if averaged energy zero or universe “FLAT” Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 36

Light from early universe visible as cosmic microwave background (CMB) CMB perfect for tracing flatness of universe Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 37

Universe at Big Bang 14 B yrs from R(t) 14 Universe today rs y t h B lig What we witness Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 38

CMB (Cosmic Microwave Background) (measured with COBE Satellite (1991) perfect black-body spectrum Mather(left) (NASA), Smoot (LBL, Berkeley) Nobelpreis 2006 T = 2. 728 ± 0. 004 K Photondensity 412 per cm 3 312 neutrinos/cm 3 Wavelength of photons ca. 1, 5 mm, so volume densely packed (10 mm / 1. 5 mm)3 =. 300/cm 3, so 412 means MANY photons/cm 3 Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 39

CMB Anisotropy (Temp. Fluctuations) The oval shapes show a spherical surface, as in a global map. The whole sky can be thought of as the inside of a sphere. Patches in the brightness are about 1 part in 100, 000 = a bacterium on a bowling ball Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 40

Evolution of the universe DT Early Universe /T ~ D The Cosmic screen Present Universe Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 41

DT / T ~ D Question: why sign negative? Expect: higher density = higher temperature Answer: gravitational redshift „cools“ photons if they escape from hot spot. They becomer cooler than average. Result: Temperatur anisotropy much smaller than expected. Indirect proof of DM, which determines depth of potential well Question: Gravitational redshift first observed by Pound and Repka by measuring frequency shift in 45 m high tower. How would you estimate the expected shift? How could one measure such a shift? Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 42

Can the density fluct. be acoustic waves? • Expect: the vacuum of “space” must be silent ? Not for the young Universe: • Shortly after the big bang (eg @ CMB: 380, 000 yrs) • • • all matter is spread out evenly (no stars or galaxies yet) Universe is smaller everything closer together (by × 1000) the density is much higher (by × 109 = a billion) 7 trillion photons & 7000 protons/electrons per cubic inch all at 5400ºF with pressure 10 -7 (ten millionth) Earth’s atm. There is a hot thin atmosphere for sound waves • • unusual fluid intimate mix of gas & light sound waves propagate at ~50% speed of light Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 43

Acoustic waves ARE density fluctuations Modern Flute Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 44

Model of acoustic waves in early universe Model of acoustic waves: DM determines depth of potential well Baryons (yellow) fall into well Photon pressure (spring) drives them out of well Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 45

t=trec t=1/2 trec 2 nd harmonic t=1/3 trec Wim de Boer 3 rd harmonic KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 Pho and ton pre s g ra v. in sure pha se 1. harmonic Pho ton t a o n n and d g press pre rav. in ure pha grav. ssure o pha se ut o se f Acoustic peaks in detail 46

Sound of Big Bang reconstructed from CMB anisotropy ©Mark Whittle (transposed by 50 octaves) A 220 Hz Frequency (in Hz) Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 47

Why is the frequency of the Big Bang so low? WEIL DAS UNIVERSUM SO GROß IST! Organ Universe Pan Flute ©Mark Whittle 0 0 0 , 0 0 4 s r a e y t h g li Beware: during the big bang, there was no bang, but perfect silence. Sound waves were created later by the interaction between matter and radiation. Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 48

Position of first acoustic peak determines curvature of universe http: //wmap. gsfc. nasa. gov/resources/camb_tool/index. html Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 49

WMAP results agree with Nuclear Synthesis Planck: Ωb=4. 9% Nucleosynthesis: Ωb≈ 5% Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 50

Evolution of the universe St sh ruc di ou tur ga stri ld b e in la bu e xi ti vi CM es on si B of ble in Early Universe The Cosmic screen Present Universe Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 51

Powerspectrum at small scales sensitive to neutrino mass! Sum of neutrino masses < 0. 23 e. V at 95% C. L. Planck 2013 Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 52

Energy density components in expanding universe Energy density ρradiation R-4 ρatom=0. 05 ρmatter R-3 =0. 27 ρcrit ρWIMP=0. 27 ρΛ =const. =0. 68ρcrit or ΩΛ = ρvacuum/ ρcrit =0. 68 teq= 50. 000 a Wim de Boer Time KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 53

Indirect limits on neutrino masses from cosmology ★ The cosmological mass upper limits are complemented by the limits from neutrino oscillation experiments ‣ Atmospheric neutrino oscillations show that there is at least one neutrino whose mass exceeds a lower limit around 0. 05 e. V ‣ Solar neutrino oscillations occur at smaller mass scale, perhaps around 0. 008 e. V ★ Sterile neutrinos are currently disfavored, it can be assumed that only three neutrino flavors are present in the neutrino background; this means that none of the three neutrinos can weigh more than about 0. 23/3 = 0. 08 e. V ★ The mass of the heaviest neutrino would therefore be in the range 0. 05 − 0. 08 e. V BEWARE: fits done in concordance CDM model Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 54

Summary on energy content We know the invisible 96% has 2 components: One with repulsive gravity –called dark energy (68%)If it is not dark, it does not matter one with normal gravity, called dark matter (26%) Ω= ρ/ρcrit 1. 0± 0. 01 ΩM= ρM/ρcrit ΩCDM= ρCDM/ρcrit ΩΛ= ρΛ/ρcrit =68% Ω= ΩM + ΩCDM + ΩΛ=1 Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 55

Time evolution of Universe Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 56

The ouroborus http: //emergent-culture. com Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 57

Summary on CMB How do we know baryon density? How do we know dark energy density? How do we know averaged dark matter density? How do we know local dark matter density? How do we know photon density? How do we know that our universe is flat? Does a flat universe mean that we have zero-energy universe? Where did energy for critical energy density come from? Wim de Boer KSETA Lecturese „Beyond the SM“ Kalsrsuhe, Oct. 2014 58