Higgs field as the main character in the early Universe Dmitry Gorbunov Institute for Nuclear Research, Moscow, Russia Dual year Russia-Spain, Particle Physics, Nuclear Physics and Astroparticle Physics Barcelona University, 11.11.2011 Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 1 / 24
Outline Outline 1 Motivation: phenomena observed but unexplained within the SM 2 Top-down approach: starting from Higgs-inflation (no new fields!) Chaotic inflation: preliminaries Higgs field with nonminimal coupling to gravity: inflation and reheating Strong coupling Possible role of nonrenormalizable operators 3 Summary Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 2 / 24
Motivation: phenomena observed but unexplained within the SM Outline 1 Motivation: phenomena observed but unexplained within the SM 2 Top-down approach: starting from Higgs-inflation (no new fields!) Chaotic inflation: preliminaries Higgs field with nonminimal coupling to gravity: inflation and reheating Strong coupling Possible role of nonrenormalizable operators 3 Summary Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 3 / 24
Motivation: phenomena observed but unexplained within the SM Neutrino oscillations: masses and mixing angles Solar 2 2 subsector Atmospheric 2 2 subsector 10 4.0 4 3 ) 2 ev 3 (10 2 m 3.5 3.0 3 2.5 2.0 2 1.5 MINOS best oscillation fit MINOS 90% Super K 90% MINOS 68% Super K L/E 90% K2K 90% 1.01 0.6 0.7 0.8 0.9 1 sin 2 (2θ) http://hitoshi.berkeley.edu/neutrino/ m 1 > 0.008 ev MINOS, T2K, SNO,..., global fits: sin 2 2θ 13 0.3 arxiv:0806.2237 m 2 > 0.05 ev Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 4 / 24
Motivation: phenomena observed but unexplained within the SM Baryons and Dark Matter in Astrophysics Rotation curves Gravitational lensing X-rays from clusters Bullet cluster Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 5 / 24
Motivation: phenomena observed but unexplained within the SM Baryons and Dark Matter in Cosmology Standard candles Angular distance BBN (m-m) (mag) (m-m) (mag) 1.0 0.5 0.0-0.5-1.0 0.5 0.0-0.5 Ground Discovered HST Discovered Empty (Ω=0) Ω M=0.27, Ω Λ=0.73 "replenishing" gray Dust high-z gray dust (+Ω M=1.0) Ω M=1.0, Ω Λ=0.0 Evolution ~ z, (+Ω M=1.0) θ (mas) 10 2 10 1 10 0 0.27 0.26 0.25 Yp D 0.24 H 0.23 10 3 10 4 10 5 10 9 5 7 Li/H p 0.005 4 He D/H p 3 He/H p Baryon density Ω b h 2 0.01 0.02 0.03 BBN CMB 0.0 0.5 1.0 1.5 2.0 z 10 2 10 1 10 0 10 1 10 2 10 3 z 2 10 10 1 2 3 4 5 6 7 8 9 10 Baryon-to-photon ratio η 10 10 Structures BAO CMB fluctuations Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 6 / 24
Cosmological parameters: Ω DM = 0.22, Ω B = 0.046 2.0 Baryon density Ω b h 2 0.005 0.01 0.02 0.03 No Big Bang 0.27 0.26 4 He 0.25 1.5 Y p D 0.24 H 0.23 10 3 Motivation: phenomena observed but unexplained within the SM 1.0 SNe 10 4 10 5 D/H p 3 He/H p BBN CMB 0.5 7 Li/H p 10 9 5 BAO Flat CMB 0.0 0.0 0.5 1.0 arxiv:0804.4142 2 10 10 1 2 3 4 5 6 7 8 9 10 Baryon-to-photon ratio η 10 10 http://pdg.lbl.gov Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 7 / 24
Motivation: phenomena observed but unexplained within the SM Inflationary solution of Hot Big Bang problems Temperature fluctuations δt /T 10 5 Universe is uniform! conformal time conformal time space coordinate particle horizon casually connected regions inflationary expansion δρ/ρ 10 5 space coordinate Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 8 / 24
Motivation: phenomena observed but unexplained within the SM True Extension of the Standard Model should Reproduce the correct neutrino oscillations Contain the viable DM candidate Be capable of explaining the baryon asymmetry of the Universe Have the inflationary mechanism operating at early times Guiding principle: use as little new physics as possible Why? No any hints observed so far! No FCNC No WIMPs No...... Nothing new at all Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 9 / 24
Motivation: phenomena observed but unexplained within the SM Standard Model: Success and Problems Gauge fields (interactions): γ, W ±, Z, g Three generations of matter: L = ( ν L e L ), er ; Q = ( ul d L ), d R, u R Describes all experiments dealing with electroweak and strong interactions Does not describe Neutrino oscillations Dark matter (Ω DM ) Baryon asymmetry (ΩB ) Inflationary stage Dark energy (ΩΛ ) Strong CP: boundary terms, new topology,... Gauge hierarchy: No new fields at new scales! Quantum gravity Try to explain all above Planck-scale physics saves the day Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 10 / 24
Top-down approach: starting from Higgs-inflation (no new fields!) Outline 1 Motivation: phenomena observed but unexplained within the SM 2 Top-down approach: starting from Higgs-inflation (no new fields!) Chaotic inflation: preliminaries Higgs field with nonminimal coupling to gravity: inflation and reheating Strong coupling Possible role of nonrenormalizable operators 3 Summary Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 11 / 24
Top-down approach: starting from Higgs-inflation (no new fields!) Chaotic inflation: preliminaries Chaotic inflation: simple realization S = d 4 x ( ) g M2 P 2 R + ( µ X) 2 βx 4 2 Chaotic inflation, A.Linde (1983) Ẍ+3HẊ + V (X) = 0 H 2 = 1 MP 2 V (X), a(t) e Ht slow roll conditions get satisfied at X e > M Pl MP 2 = M2 Pl /(8π) generation of scale-invariant scalar (and tensor) perturbations from exponentially stretched quantum fluctuations of X X δρ/ρ 10 5 requires = V = βx 4 : β 10 13 Gravity solves all problems No scale, no problem We have scalar in the SM! The Higgs field! ( In a unitary gauge H T = 0,(h + v)/ ) 2 (and neglecting v = 246 GeV) λ 0.1 1 S = d 4 x ( ) g M2 P 2 R + ( µ h) 2 λ h4 2 4 Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 12 / 24
Top-down approach: starting from Higgs-inflation (no new fields!) Chaotic inflation: preliminaries Chaotic inflation: simple realization S = d 4 x ( ) g M2 P 2 R + ( µ X) 2 βx 4 2 Chaotic inflation, A.Linde (1983) Ẍ+3HẊ + V (X) = 0 H 2 = 1 MP 2 V (X), a(t) e Ht slow roll conditions get satisfied at X e > M Pl MP 2 = M2 Pl /(8π) generation of scale-invariant scalar (and tensor) perturbations from exponentially stretched quantum fluctuations of X X δρ/ρ 10 5 requires = V = βx 4 : β 10 13 Gravity solves all problems No scale, no problem We have scalar in the SM! The Higgs field! ( In a unitary gauge H T = 0,(h + v)/ ) 2 (and neglecting v = 246 GeV) λ 0.1 1 S = d 4 x ( ) g M2 P 2 R + ( µ h) 2 λ h4 2 4 Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 12 / 24
Top-down approach: starting from Higgs-inflation (no new fields!) Higgs-driven inflation Higgs field with nonminimal coupling to gravity: inflation and reheating S = d 4 x ( g M2 P ( In a unitary gauge H T = 0,(h + v)/ ) 2 2 R ξ H HR + L SM (and neglecting v = 246 GeV) S = d 4 x ( g M2 P + ξ ) h2 R + ( µ h) 2 λ h4 2 2 4 F.Bezrukov, M.Shaposhnikov (2007) ) slow roll behavior due to modified kinetic term even for λ 1 Go to the Einstein frame: (M 2 P + ξ h2 )R M 2 P R g µν = Ω 2 g µν, Ω 2 = 1 + ξ h2 M 2 P with canonically normalized χ: dχ dh = M P MP 2 + (6ξ + 1)ξ h2 MP 2 + ξ, U(χ) = h2 λm 4 P h4 (χ) 4(M 2 P + ξ h2 (χ)) 2. we have a flat potential at large fields: U(χ) const @ h M P / ξ Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 13 / 24
Top-down approach: starting from Higgs-inflation (no new fields!) Higgs field with nonminimal coupling to gravity: inflation and reheating U(χ) MP λm 4 /ξ 2 /4 log(χ) MP /ξ MP /ξ exact h 3/2ξh 2 /MP 6 log( ξh/mp ) log(h) MP / ξ Reheating by Higgs field after inflation: effective dynamics : M P /ξ < h < M P / ξ h 2 χ L = 1 2 µ χ µ χ λ 6 M 2 P ξ 2 χ2 Advantage: NO NEW interactions to reheat the Universe inflaton couples to all SM fields! λm 4 /ξ 2 /16 λ v 4 /4 0 0 v 0 0 χ end χ WMAP χ exponentially flat potential! @ h M P / ξ : U(χ) = λm4 P 4ξ 2 ( ( )) 2 2 χ 1 exp 3MP coincides (apart of T reh 10 14 GeV) with R 2 -model! But NO NEW d.o.f. 0812.3622 n s = 0.97, r = 0.0034, N = 59 from WMAP-normalization: ξ 47000 λ Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 14 / 24
Top-down approach: starting from Higgs-inflation (no new fields!) Higgs field with nonminimal coupling to gravity: inflation and reheating U(χ) MP λm 4 /ξ 2 /4 log(χ) MP /ξ MP /ξ exact h 3/2ξh 2 /MP 6 log( ξh/mp ) log(h) MP / ξ Reheating by Higgs field after inflation: effective dynamics : M P /ξ < h < M P / ξ h 2 χ L = 1 2 µ χ µ χ λ 6 M 2 P ξ 2 χ2 Advantage: NO NEW interactions to reheat the Universe inflaton couples to all SM fields! λm 4 /ξ 2 /16 λ v 4 /4 0 0 v 0 0 χ end χ WMAP χ exponentially flat potential! @ h M P / ξ : U(χ) = λm4 P 4ξ 2 ( ( )) 2 2 χ 1 exp 3MP coincides (apart of T reh 10 14 GeV) with R 2 -model! But NO NEW d.o.f. 0812.3622 n s = 0.97, r = 0.0034, N = 59 from WMAP-normalization: ξ 47000 λ Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 14 / 24
Top-down approach: starting from Higgs-inflation (no new fields!) Higgs field with nonminimal coupling to gravity: inflation and reheating F.Bezrukov, D.G., M.Shaposhnikov, 0812.3622 log(χ) MP MP /ξ MP /ξ exact h 3/2ξh 2 /MP 6 log( ξh/mp ) log(h) MP / ξ Reheating by Higgs field after inflation: M P /ξ < h < M P / ξ mw 2 (χ) = g2 2 6 m t (χ) = y t M P χ (t) ξ M P χ (t) sign χ(t) 6ξ reheating via W + W, ZZ production at zero crossings then nonrelativistic gauge bosons scatter to light fermions W + W f f effective dynamics : h 2 χ L = 1 2 µ χ µ χ λ 6 M 2 P ξ 2 χ2 Advantage: NO NEW interactions to reheat the Universe inflaton couples to all SM fields! Hot stage starts almost from T = M P /ξ 10 14 GeV: ( ) λ 1/4 3.4 10 13 GeV < T r < 1.1 10 14 GeV 0.25 from WMAP-normalization: ξ 47000 λ Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 15 / 24
Top-down approach: starting from Higgs-inflation (no new fields!) Strong coupling U(χ) Fine theoretical descriptions both in UV: ( χ M P, U = const + O exp ( 2 χ/ )) 3M P λm 4 /ξ 2 /4 and in IR: h M P /ξ, U = λ 4 h4 Obvious problem with QFT-description of IR/UV matching at intermediate χ < χ end and h < M P / ξ Hence no reliable prediction for the SM Higgs boson mass m h = 2λ v upto that from the absence of Landau pole and wrong minimum of Higgs potential (well) below M P /ξ 130GeV m h 190GeV λm 4 /ξ 2 /16 λ v 4 /4 0 0 v 0 0 χ end χ WMAP χ exponentially flat potential! @ h M P / ξ : U(χ) = λm4 P 4ξ 2 ( ( )) 2 2 χ 1 exp 3MP coincides (apart of T reh 10 14 GeV) with R 2 -model! But NO NEW d.o.f. 0812.3622 n s = 0.97, r = 0.0034, N = 59 from WMAP-normalization: ξ 47000 λ Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 16 / 24
Top-down approach: starting from Higgs-inflation (no new fields!) Strong coupling U(χ) Fine theoretical descriptions both in UV: ( χ M P, U = const + O exp ( 2 χ/ )) 3M P λm 4 /ξ 2 /4 and in IR: h M P /ξ, U = λ 4 h4 Obvious problem with QFT-description of IR/UV matching at intermediate χ < χ end and h < M P / ξ Hence no reliable prediction for the SM Higgs boson mass m h = 2λ v upto that from the absence of Landau pole and wrong minimum of Higgs potential (well) below M P /ξ 130GeV m h 190GeV λm 4 /ξ 2 /16 λ v 4 /4 0 0 v 0 0 χ end χ WMAP χ exponentially flat potential! @ h M P / ξ : U(χ) = λm4 P 4ξ 2 ( ( )) 2 2 χ 1 exp 3MP coincides (apart of T reh 10 14 GeV) with R 2 -model! But NO NEW d.o.f. 0812.3622 n s = 0.97, r = 0.0034, N = 59 from WMAP-normalization: ξ 47000 λ Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 16 / 24
Top-down approach: starting from Higgs-inflation (no new fields!) Strong coupling Strong coupling in Higgs-inflation: scatterings Jordan frame Einstein frame E Strong coupling E Strong coupling Λ Planck Λ g-s Λ Planck M P M P Λ g-s Λ gauge Λ gauge M P /ξ Weak coupling M P /ξ Weak coupling M P /ξ M P / ξ h gravity-scalar sector: M P ξ, for h M P ξ, ξ h Λ g s (h) 2 M, for M P P ξ h M P, ξ ξ h, for h M P. ξ 1008.5157 M P /ξ M P / ξ h gravitons: Λ 2 Planck M2 P + ξ h2 gauge interactions: Λ gauge (h) { MP ξ, for h M P ξ, h, for M P ξ h, Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 17 / 24
Top-down approach: starting from Higgs-inflation (no new fields!) Strong coupling at M P /ξ... Strong coupling Can it change the initial conditions of the Hot Big Bang? 1 reheating temperature 2 baryon (lepton) asymmetry of the Universe 3 dark matter abundance Let s test these options adding all possible nonrenormalizable operators to the model Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 18 / 24
Top-down approach: starting from Higgs-inflation (no new fields!) Possible role of nonrenormalizable operators What can nonrenormalizable operators do? F.Bezrukov, D.G., Shaposhnikov (2011) δl NR = a 6 Λ 2 (H H) 3 + + β L 4Λ F αβ L α HH L c β + β B Λ 2 O baryon violating + + h.c. + β N 2Λ H H N c N + b L α Λ L α ( /DN) c H +, L α are SM leptonic doublets, α = 1,2,3, N stands for right handed sterile neutrinos potentially present in the model, H a = ε ab Hb, a,b = 1,2; and Λ = Λ(h) = { Λ g s (h), Λ gauge (h), Λ Planck (h) } couplings can differ significantly in different regions of h: today h < M P /ξ, at preheating M P /ξ < h < M P / ξ Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 19 / 24
Top-down approach: starting from Higgs-inflation (no new fields!) Possible role of nonrenormalizable operators LFV, BV nonrenormalizable operators today Neutrino masses: easily hence L νν (5) = β Lv 2 F αβ 4Λ 2 ν ανβ c + h.c. ( ) Λ 3 10 14 3 10 3 ev 2 1/2 GeV β L matm 2 when Λ = M P ξ can explain with 0.6 1014 GeV β L 0.2 Proton decay: probably then from experiments L (6) β B Λ 2 QQQL Λ ( ) β B 10 16 τ 1/4 p π GeV 0 e + 1.6 10 33 years with the same one needs Λ = M P ξ 0.6 1014 GeV β B < 0.4 10 4 Either B and L α are significantly different or we will observe proton decay in the next generation experiment Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 20 / 24
Top-down approach: starting from Higgs-inflation (no new fields!) Possible role of nonrenormalizable operators LFV, BV nonrenormalizable operators today Neutrino masses: easily hence L νν (5) = β Lv 2 F αβ 4Λ 2 ν ανβ c + h.c. ( ) Λ 3 10 14 3 10 3 ev 2 1/2 GeV β L matm 2 when Λ = M P ξ can explain with 0.6 1014 GeV β L 0.2 Proton decay: probably then from experiments L (6) β B Λ 2 QQQL Λ ( ) β B 10 16 τ 1/4 p π GeV 0 e + 1.6 10 33 years with the same one needs Λ = M P ξ 0.6 1014 GeV β B < 0.4 10 4 Either B and L α are significantly different or we will observe proton decay in the next generation experiment Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 20 / 24
Top-down approach: starting from Higgs-inflation (no new fields!) Possible role of nonrenormalizable operators LFV, BV nonrenormalizable operators today Neutrino masses: easily hence L νν (5) = β Lv 2 F αβ 4Λ 2 ν ανβ c + h.c. ( ) Λ 3 10 14 3 10 3 ev 2 1/2 GeV β L matm 2 when Λ = M P ξ can explain with 0.6 1014 GeV β L 0.2 Proton decay: probably then from experiments L (6) β B Λ 2 QQQL Λ ( ) β B 10 16 τ 1/4 p π GeV 0 e + 1.6 10 33 years with the same one needs Λ = M P ξ 0.6 1014 GeV β B < 0.4 10 4 Either B and L α are significantly different or we will observe proton decay in the next generation experiment Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 20 / 24
Top-down approach: starting from Higgs-inflation (no new fields!) Possible role of nonrenormalizable operators Leptogenesis, B L /3: can be successful i d dt ˆQ L = [Ĥint, ˆQ ] L, n L n L n L = Q L L Y = Y α Lα HE α + h.c., L νν (5) = β L 4Λ F αβ L α HH L c β + h.c. ( )) ( ) d n L /dt Im (βl 4 Tr FF FYYF YY βl 4 y τ 4 Im F 3β Fαβ F α3f33 for the gauge cutoff Λ = h one has β 4 L ( yτ 0.01 ) 4 ( 0.25 λ for gravity-scalar cutoff Λ = ξ h 2 /M P ( βl 4 yτ ) ( 4 0.25 0.01 λ ) 5/4 ( 10 10 < L < βl 4 yτ 0.01 ) 13/4 ( 6.3 10 13 < L < βl 4 yτ 0.01 ) ( ) 4 0.25 10 9, λ In both cases the asymmetry can be (significantly) increased with operator δl τ = y τ L τ HE τ + β y L τ HE τ H H Λ 2 + ) ( ) 4 0.25 2 2.4 10 10 λ one can fancy the hierarchy gives a factor up to 10 8! 1 β y y τ 10 2. Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 21 / 24
Top-down approach: starting from Higgs-inflation (no new fields!) Possible role of nonrenormalizable operators Leptogenesis, B L /3: can be successful i d dt ˆQ L = [Ĥint, ˆQ ] L, n L n L n L = Q L L Y = Y α Lα HE α + h.c., L νν (5) = β L 4Λ F αβ L α HH L c β + h.c. ( )) ( ) d n L /dt Im (βl 4 Tr FF FYYF YY βl 4 y τ 4 Im F 3β Fαβ F α3f33 for the gauge cutoff Λ = h one has β 4 L ( yτ 0.01 ) 4 ( 0.25 λ for gravity-scalar cutoff Λ = ξ h 2 /M P ( βl 4 yτ ) ( 4 0.25 0.01 λ ) 5/4 ( 10 10 < L < βl 4 yτ 0.01 ) 13/4 ( 6.3 10 13 < L < βl 4 yτ 0.01 ) ( ) 4 0.25 10 9, λ In both cases the asymmetry can be (significantly) increased with operator δl τ = y τ L τ HE τ + β y L τ HE τ H H Λ 2 + ) ( ) 4 0.25 2 2.4 10 10 λ one can fancy the hierarchy gives a factor up to 10 8! 1 β y y τ 10 2. Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 21 / 24
Top-down approach: starting from Higgs-inflation (no new fields!) Possible role of nonrenormalizable operators Dark matter: an example of sterile fermion L int = β N H H 2Λ N c N = β N 4 can be produced at preheating or at the hot stage h 2 Λ(h) N c N DM fermion has to be light! (WDM?) Indeed, today b Lα Λ L α ( /DN) c H f α b Lα M N Λ. So, N is unstable with the γν partial width of the order Γ N γν 9b2 L α αg 2 F 512π 4 v 2 M 5 N Λ 2. EGRET gives τ γν > 10 27 s, hence 0709.2299 for Λ = M P : M N 200MeV, for Λ = M P /ξ : M N 4MeV Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 22 / 24
Outline Summary 1 Motivation: phenomena observed but unexplained within the SM 2 Top-down approach: starting from Higgs-inflation (no new fields!) Chaotic inflation: preliminaries Higgs field with nonminimal coupling to gravity: inflation and reheating Strong coupling Possible role of nonrenormalizable operators 3 Summary Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 23 / 24
Summary Summary on Higgs-inflation Guiding principle: use as little new physics as possible Predicted n s, r can be tested experimentally Can explain neutrino oscillations with nonrenormalizable operators Can explain BAU with nonrenormalizable operators Need a new field to be DM Fermion DM is light (?) and can be searched for in cosmic X- or γ-rays (?) Proton decays (???) The main character in the early Universe...? It can solve all the phenomenological problems we are aware of... It would be great to describe IR/UV matching in RH H Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 24 / 24
Summary Summary on Higgs-inflation Guiding principle: use as little new physics as possible Predicted n s, r can be tested experimentally Can explain neutrino oscillations with nonrenormalizable operators Can explain BAU with nonrenormalizable operators Need a new field to be DM Fermion DM is light (?) and can be searched for in cosmic X- or γ-rays (?) Proton decays (???) The main character in the early Universe...? It can solve all the phenomenological problems we are aware of... It would be great to describe IR/UV matching in RH H Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 24 / 24
Backup slides Dmitry Gorbunov (INR) Higgs field: the main character in Universe 11.11.11, Barcelona University 25 / 24