Electroweak Baryogenesis after LHC8

Electroweak Baryogenesis after LHC8 Gláuber Carvalho Dorsch with S. Huber and J. M. No University of Sussex arxiv:135.661 JHEP 131, 29(213) What NExT? Southampton November 27, 213 G. C. Dorsch EWBG after LHC8 What NExT? 1 / 19

The problem of baryogenesis I Observed BAU: n B s 1 1. G. C. Dorsch EWBG after LHC8 What NExT? 2 / 19

The problem of baryogenesis I Observed BAU: n B s 1 1. I Assume BAU as initial condition of Universe? Inflation & sphaleron processes would wash out the initial asymmetry. G. C. Dorsch EWBG after LHC8 What NExT? 2 / 19

The problem of baryogenesis I Observed BAU: n B s 1 1. I Assume BAU as initial condition of Universe? Inflation & sphaleron processes would wash out the initial asymmetry. I Baryogenesis ) Sakharov conditions: B number violation; X chiral anomaly and non-trivial SU(2) topology; G. C. Dorsch EWBG after LHC8 What NExT? 2 / 19

Baryogenesis in SM I Observed BAU: n B s 1 1. I Assume BAU as initial condition of Universe? Inflation & sphaleron processes would wash out the initial asymmetry. I Baryogenesis ) Sakharov conditions: B number violation; C/CP violation; thermodynamical non-equilibrium; G. C. Dorsch EWBG after LHC8 What NExT? 3 / 19

Baryogenesis in SM I Observed BAU: n B s 1 1. I Assume BAU as initial condition of Universe? Inflation & sphaleron processes would wash out the initial asymmetry. I Baryogenesis ) Sakharov conditions: B number violation; X chiral anomaly and non-trivial SU(2) topology; C/CP violation; thermodynamical non-equilibrium; G. C. Dorsch EWBG after LHC8 What NExT? 3 / 19

Baryogenesis in SM I Observed BAU: n B s 1 1. I Assume BAU as initial condition of Universe? Inflation & sphaleron processes would wash out the initial asymmetry. I Baryogenesis ) Sakharov conditions: B number violation; X chiral anomaly and non-trivial SU(2) topology; C/CP violation; X CKM matrix; thermodynamical non-equilibrium; G. C. Dorsch EWBG after LHC8 What NExT? 3 / 19

Baryogenesis in SM I Observed BAU: n B s 1 1. I Assume BAU as initial condition of Universe? Inflation & sphaleron processes would wash out the initial asymmetry. I Baryogenesis ) Sakharov conditions: B number violation; X chiral anomaly and non-trivial SU(2) topology; C/CP violation; X CKM matrix; thermodynamical non-equilibrium; Xexpansion of Universe; XEW phase transition. G. C. Dorsch EWBG after LHC8 What NExT? 3 / 19

Electroweak baryogenesis in SM I B-number violating processes suppressed at T =... Probability e 16 2 /g 2 1 162 G. C. Dorsch EWBG after LHC8 What NExT? 4 / 19

Electroweak baryogenesis in SM I B-number violating processes suppressed at T =... Probability e 16 2 /g 2 1 162 I...but there is a threshold T. T c (EW scale) above which the rate of B violation Universe s expansion. I If T>T after EW phase transition, the generated asymmetry is washed out. I Successful baryogenesis requires a strong first order phase transition: v c T c & 1. Sphaleron CP χ L + χ L B χ R Sphaleron <φ> = <φ> = Bubble Wall Morrissey, Ramsey-Musolf [arxiv:126.2942] G. C. Dorsch EWBG after LHC8 What NExT? 4 / 19

Electroweak baryogenesis in SM I EWPT in SM is strongly first order only if m h. m W. G. C. Dorsch EWBG after LHC8 What NExT? 5 / 19

Electroweak baryogenesis in SM I EWPT in SM is strongly first order only if m h. m W. I CKM matrix alone does not supply sufficient CP violation. Even with a first order phase transition, BAU prediction would be 1 orders of magnitude below observed value. I EWBG requires BSM physics at EW scale with moderately large couplings to SM sector and new sources of CP! G. C. Dorsch EWBG after LHC8 What NExT? 5 / 19

EWBG in the MSSM MSSM Higgs sector ) two SU(2) L scalar doublets 1, 2: ' + i = i. h i + i i V MSSM tree = µ 2 1 1 1 µ 2 2 1 1 + g2 + g 2 8 EW minimum: h 1 i = v cos 2 2 µ 2 1 2 + H.c. + 2 2 g 2 + 2 2, h 2 i = 2 v sin 2 1 2. Mass eigenstates: G,G ± {z } + h,h,a,h ±. {z } Goldstone bosons physical Higgs states. G. C. Dorsch EWBG after LHC8 What NExT? 6 / 19

EWBG in MSSM (?) I New scalars increase strength of phase transition ) light stop scenario (LSS): 8 GeV. m t R. 12 GeV. Many new sources of CP violation. However... G. C. Dorsch EWBG after LHC8 What NExT? 7 / 19

EWBG in MSSM (?) I New scalars increase strength of phase transition ) light stop scenario (LSS): 8 GeV. m t R. 12 GeV. Many new sources of CP violation. However... I m h = m Z cos(2 ) + R.C.. 13 GeV. m h 125 GeV + LSS ) heavy stop 1 TeV (naturalness?) I This scenario allows for rather definite predictions on SM Higgs production and branching ratios, with severe tension with experimental data! [Curtin, Jaiswal, Meade, arxiv:123.2932] G. C. Dorsch EWBG after LHC8 What NExT? 7 / 19

2HDM I Two-Higgs-doublet models are the minimal SM extension able to account for BAU. I Generalization of the MSSM Higgs sector. I Extra heavy bosons (h,h,a,h ± ) may strengthen the EW phase transition. I Additional sources of CP (explicit and/or spontaneous). I Correct BAU can be obtained for simplified cases and for particular combinations of parameters. [Fromme, Huber, Seniuch, hep-ph/65242] G. C. Dorsch EWBG after LHC8 What NExT? 8 / 19

2HDM I General fermionic couplings: L Yukawa = Q L ( 1 1 + 2 2 ) n R +... G. C. Dorsch EWBG after LHC8 What NExT? 9 / 19

2HDM I General fermionic couplings: L Yukawa = Q L ( 1 1 + 2 2 ) n R +... I Diagonalizing mass matrix M n = 1 h' 1i + 2 h' 2i does not diagonalize 1,2 simultaneously, so induces tree-level FCNC. L FCNC = d L e 1 ' 1d R +... I Avoid this with Z 2 symmetry: 1! 1, 2! 2. u R d R e R Type I + + + Type II + Type X + + Type Y + + Only top-quark is significant for phase transition. Then models differ only in phenomenological constraints on their parameter space. These come mainly from B-physics, so Type I Type X, Type II Type Y. G. C. Dorsch EWBG after LHC8 What NExT? 9 / 19

2HDM I For simplicity, consider CP conserving case only. V tree( 1, 2) = µ 2 1 1 1 µ 2 2 µ 2 2 2 1 2 + H.c. + 2 + 1 2 2 1 1 + 2 2 2 + 3 1 1 2 2 + 2 2 apple + 4 1 2 2 1 + 5 2 1 2 + H.c.. 2 I EW minimum: h 1 i = I parameters: I v cos v 174 GeV and M, h 2 i = p µ. sin(2 ) I Masses: mh,m H,m A,m H ±. v sin I is the mixing angle between (G +,H + ) and (G,A ).. I Likewise, is the mixing angle between (h,h ). It is here defined such that = () h = h SM. G. C. Dorsch EWBG after LHC8 What NExT? 1 / 19

V = Vtree + VCW + VCT + VT. Fix mh = 125 GeV.4 tan 2 I Constraints: < 2 EW precision: 1 ; i < 4 ; metastability; B B (red/dashed) and B! Xs (black/full). I 1, I, I GeV µ 1 TeV, I 1 GeV ma, mh ± 1 TeV, 15 GeV mh 1 TeV. Type I/X Type II/Y 1 1 9 9 8 8 7 7 6 6 tan tan I 5 4 5 4 3 3 2 2 1 1 1 2 3 4 5 6 7 8 9 1 1 mh ± [GeV ] Type II/Y: mh ± G. C. Dorsch 2 3 4 5 6 7 8 9 1 mh ± [GeV ] 36 GeV [Hermann et al., arxiv:128.2788]. EWBG after LHC8 What NExT? 11 / 19

Results: tan 25 2 15 1 5 Type I/X.3.2.1 14 12 1 8 6 4 2 Type II/Y.3.2.1 1 2 3 4 5 6 7 8 9 1 tan Preference for tan 1 2 3 4 5 6 7 8 9 1 tan. 3 is excellent for baryogenesis, since n B (tan ) 2. G. C. Dorsch EWBG after LHC8 What NExT? 12 / 19

Results: Masses 3 25 2 15 1 5 (a).3.2.1 14 12 1 8 6 4 2 (f).5.4.3 15 125 1 75.2 5.1 25 (b).4.3.1 1 2 3 4 5 6 7 8 9 1 mh ± [GeV] 1 2 3 4 5 6 7 8 9 1 ma [GeV] 2 3 4 5 6 7 8 9 1 mh [GeV] 14 12 1 8 6 (e).5.4.3.2 8 6 4 (d) 1.8.6.4 16 12 8 (c).4.3 4 2.1 2.2 4.1-4 -2 2 4 6 8 ma mh± [GeV] m H ± -4-2 2 4 6 ma mh [GeV] -4-3 -2-1 1 2 3 4 mh mh± [GeV] hardly influences the phase transition. G. C. Dorsch EWBG after LHC8 What NExT? 13 / 19

Results: Masses 3 25 2 15 1 5 (a).3.2.1 14 12 1 8 6 4 2 (f).5.4.3 15 125 1 75.2 5.1 25 (b).4.3.1 1 2 3 4 5 6 7 8 9 1 mh ± [GeV] 1 2 3 4 5 6 7 8 9 1 ma [GeV] 2 3 4 5 6 7 8 9 1 mh [GeV] 14 12 1 8 6 (e).5.4.3.2 8 6 4 (d) 1.8.6.4 16 12 8 (c).4.3 4 2.1 2.2 4.1-4 -2 2 4 6 8 ma mh± [GeV] -4-2 2 4 6 ma mh [GeV] -4-3 -2-1 1 2 3 4 mh mh± [GeV] m H ± hardly influences the phase transition. Large pseudo-scalar masses, m A & 4 GeV, are favoured. G. C. Dorsch EWBG after LHC8 What NExT? 13 / 19

Results: Masses 3 25 2 15 1 5 (a).3.2.1 14 12 1 8 6 4 2 (f).5.4.3 15 125 1 75.2 5.1 25 (b).4.3.1 1 2 3 4 5 6 7 8 9 1 mh ± [GeV] 1 2 3 4 5 6 7 8 9 1 ma [GeV] 2 3 4 5 6 7 8 9 1 mh [GeV] 14 12 1 8 6 (e).5.4.3.2 8 6 4 (d) 1.8.6.4 16 12 8 (c).4.3 4 2.1 2.2 4.1-4 -2 2 4 6 8 ma mh± [GeV] -4-2 2 4 6 ma mh [GeV] -4-3 -2-1 1 2 3 4 mh mh± [GeV] m H ± hardly influences the phase transition. Large pseudo-scalar masses, m A & 4 GeV, are favoured. s also prefer hierarchy m A >m H ' m H ±. G. C. Dorsch EWBG after LHC8 What NExT? 13 / 19

Results: Couplings 4 = 1 2v 2 M 2 + m 2 A 2m2 H ±, 5 = 1 2v 2 M 2 m 2 A. 1 8 6 4 2 Type I/X.4.3.1 7 6 5 4 3 2 1 Type II/Y.6.4.2-1 -5 5 1-1 -5 5 1 4 4 16.6 6.6 12 8 4 Type I/X.4.2 4 2 Type II/Y.4.2-12 -1-8 -6-4 -2 2 4-12 -1-8 -6-4 -2 2 4 5 5 G. C. Dorsch EWBG after LHC8 What NExT? 14 / 19

Results: 1 8 Type I/X.4.3 1 8 Type II/Y.4.3 6 4 6 4 2.1 2.1 - /4 /4 /2 3 /4 - /4 /4 /2 3 /4 A strong PT favours a SM-like h. G. C. Dorsch EWBG after LHC8 What NExT? 15 / 19

Results: 1 8 Type I/X.4.3 1 8 Type II/Y.4.3 6 4 6 4 2.1 2.1 - /4 /4 /2 3 /4 - /4 /4 /2 3 /4 A strong PT favours a SM-like h. Put another way, the observation of a SM-like h constrains the parameter space of 2HDMs in favour of strong PTs. G. C. Dorsch EWBG after LHC8 What NExT? 15 / 19

Conclusions I 2HDMs are robust candidates to explain BAU in light of LHC8 results. G. C. Dorsch EWBG after LHC8 What NExT? 16 / 19

Conclusions I 2HDMs are robust candidates to explain BAU in light of LHC8 results. I h h SM favours a strong PT scenario. G. C. Dorsch EWBG after LHC8 What NExT? 16 / 19

Conclusions I 2HDMs are robust candidates to explain BAU in light of LHC8 results. I h h SM favours a strong PT scenario. I also prefers: G. C. Dorsch EWBG after LHC8 What NExT? 16 / 19

Conclusions I 2HDMs are robust candidates to explain BAU in light of LHC8 results. I h h SM favours a strong PT scenario. I also prefers: I tan 1; G. C. Dorsch EWBG after LHC8 What NExT? 16 / 19

Conclusions I 2HDMs are robust candidates to explain BAU in light of LHC8 results. I h h SM favours a strong PT scenario. I also prefers: I tan 1; I ma & 4 GeV; G. C. Dorsch EWBG after LHC8 What NExT? 16 / 19

Conclusions I 2HDMs are robust candidates to explain BAU in light of LHC8 results. I h h SM favours a strong PT scenario. I also prefers: I tan 1; I ma & 4 GeV; I mass hierarchy ma >m H ' m H ±. I What does this tell us about probing the 2HDM in LHC? Are there hidden scalars in current LHC data? [Arhrib, Ferreira, Santos, arxiv:1311.152] How would a discovery impact the phase transition? G. C. Dorsch EWBG after LHC8 What NExT? 16 / 19

Appendix h! 12 1 8 6 4 2 Type I.3.2.1 5 4 3 2 1 Type II.4.3.1.5 1 1.5 2 2.5 BR(h! ).5 1 1.5 2 2.5 BR(h! ) Coupling of h to b and : Type I: sin sin, Type II: cos cos. G. C. Dorsch EWBG after LHC8 What NExT? 17 / 19

Appendix µ parameter V tree µ 2 2 1 2 + H.c. 3 25 2 15 1 Type I/X.3.2.1 7 6 5 4 3 2 Type II/Y.3.2.1 5 1 1 2 3 4 5 6 7 8 9 1 µ [GeV] 1 2 3 4 5 6 7 8 9 1 µ [GeV] Type II/Y: m H ± 36 GeV. G. C. Dorsch EWBG after LHC8 What NExT? 18 / 19

Appendix Surviving points after each step of tests: Total EW precision i < 4 Metastability Absolute 6.3 1 6 1.2 1 6 1.4 1 5 2.6 1 4 4.3 1 3 Relative 1% 19.1% 2.3%.41%.69% fields: G + = cos ' + 1 +sin '+ 2 (charged Goldstone), H + = sin ' + 1 + cos '+ 2 (charged scalar), G = cos 1 +sin 2 (neutral Goldstone), A = sin 1 + cos 2 (pseudo-scalar), h = cos h 1 +sin h 2 (lightest scalar), H = sin h 1 + cos h 2 (heaviest scalar). where i = ' + i h i + i i. G. C. Dorsch EWBG after LHC8 What NExT? 19 / 19