Baryogenesis and dark matter in the nmssm
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1 Baryogenesis and dark matter in the nmssm C.Balázs, M.Carena, A. Freitas, C.Wagner Phenomenology of the nmssm from colliders to cosmology arxiv: C. Balázs, Monash U Melbourne BG & DM in the nmssm DSU, June 6, /18
2 Minimal Supersymmetric Standard Model Explains the origin of è mass: radiative dynamics Ø electroweak symmetry breaking è dark matter: R-parity Ø stable, neutral WIMP LSP è baryons: lepto-, baryogenesis Ø è... baryon-antibaryon asymmetry But the Higgs sector of the MSSM is problematic C. Balázs, Monash U Melbourne BG & DM in the nmssm DSU, June 6, /18
3 Problems with the Higgs sector of the SSM è the m problem: W m H` 1.H` 2 in not natural è the fine-tuning problem: tension between m h > 114 GeV and... stops è the baryogenesis problem: electroweak baryogenesis demands m h d 120 GeV è... put your own problem here Fortunately, it's is easy to fix these problems while keeping radiative EWSB intact C. Balázs, Monash U Melbourne BG & DM in the nmssm DSU, June 6, /18
4 nmssm: nearly MSSM Discreet symmetries of super- & Kahler potentials Z 5 R, Z 7 R Õ U 1 R' where R' = 3R + "PQ" to prevent domain walls and large tadpoles è Superpotential è Scalar potential W = W MSSM + m 12 2 S` ÄÄÄÄÄÄÄÄÄÄÄÄÄÄÄÄ +l S` H` l 1.H` 2 V = V MSSM + t S S + h.c. + m S 2 S 2 + a l SH 1.H 2 + h.c. è New parameters v S, l, a l, m 12, m S, t S C. Balázs, Monash U Melbourne BG & DM in the nmssm DSU, June 6, /18
5 Positive features of the nmssm Solves m problem naturally W = W MSSM + m 12 2 S` ÄÄÄÄÄÄÄÄÄÄÄÄÄÄÄÄ + l S` H` l 1.H` 2 è m = l S = l v S set by EW scale Alleviates fine tuning in Higgs/stop sector m h 2 m Z 2 cos 2 2 b+ 2 l2 ÄÄÄÄÄÄÄÄÄÄÄÄÄÄÄÄ g èèè 2 sin2 2 b è tree level lightest Higgs mass limit relaxed Tree level cubic term of scalar potential V = V MSSM + t S S + h.c. + m S 2 S 2 + a l SH 1.H 2 + h.c. è assists a strongly 1 st order EW phase transition C. Balázs, Monash U Melbourne BG & DM in the nmssm DSU, June 6, /18
6 l Electroweak baryogenesis in the nmssm Measured h B strongly 1 st order EWPT large OP f C /T C t 1 è strength of EWPT minimum of finite T eff. potential V eff (f,t) = ( m 2 +at 2 )f 2 g T f 3 + ÅÅÅÅÅ 4 l f è V eff minimal for 0 <f if f C T C ÅÅÅÅÅÅÅ ÅÅÅÅ Ø g affects OP è g generated by l SM : bosonic loops Øg~g 3 ~ g l l MSSM : sc. loops Øg~ y 3 l nmssm : tree level Ø g~a l è MSSM: light stop induces strongly 1 st order EWPT nmssm: tree level a l SH 1.H 2 coupling does the same C. Balázs, Monash U Melbourne BG & DM in the nmssm DSU, June 6, /18
7 Dark matter in nmssm Neutralinos M M 2... Z é = -c b s w m Z c b s w m Z 0.. s b c w m Z -s b c w m Z l v S l v 2 l v 1 0 è unification assumption: M 2 = a 2 /a 1 M 1 è EWBG Ø low tanb & Arg(M 1 ) = Arg(M 2 ) = f M ~ 0.1 è typical lightest neutralino (Z è 1): mostly singlino m Z é 1 ~ 2lv 1v 2 v S /(v 1 2 +v 2 2 +v S 2 ) d 60 GeV C. Balázs, Monash U Melbourne BG & DM in the nmssm DSU, June 6, /18
8 All matter in nmssm Neutralino relic density è Z è 1 light Ø no coannihilations dominant annihilation channel: Z è 1 Z è 1 Ø Z * Ø SM Menon, Morrissey, Wagner 2004 C. Balázs, Monash U Melbourne BG & DM in the nmssm DSU, June 6, /18
9 Can we "measure" W Z è 1 at colliders? W è (m è Z 1 Z, sv ) under standard thermal assumptions 1 nmssm benchmark: point "A" tanb l v S a l m a M 2 f M GeV GeV GeV GeV Extracting physical parameters from cross sections è generate LHC & ILC events (tree & parton level w/ BGs, jet broadening,...) è construct appropriate invariant mass distributions è reconstruct masses (couplings) from distributions è determine central values and precision è scan around the central value in a precision window C. Balázs, Monash U Melbourne BG & DM in the nmssm DSU, June 6, /18
10 Mass determination at the LHC Typical production/decay chain: squarks/gluinos Ø charginos/neutralinos Ø leptons/jets è typical invariant mass spectra (lumi 300 fb -1 ) C. Balázs, Monash U Melbourne BG & DM in the nmssm DSU, June 6, /18
11 Mass determination at the LHC è four kinematic (mass) edges Ø four mass parameters m ll,max = m é m é Z 2 Z = 73.5±0.6 GeV 1 2 = (m 2 é Z m 2 é 2 Z )(m 2 é 1 b1 m 2 é Z )/m 2 é 2 Z = 447.0±20.0 GeV 2 2 m jll,min,3 = f 1 (m é,m é Z 1 Z,m é 3 Z,m é 2 b )= 256.2±7.0 GeV 1 2 m jll,max,3 = f 2 (m é,m é Z 1 Z,m é 3 Z,m é 2 b )= 463.5±9.0 GeV 1 m jll,max,2 è results for individual masses m Z é m Z é = GeV m é Z = GeV m é b = GeV 1 = GeV è absolute precision is reasonable but Z è 1 is very light! C. Balázs, Monash U Melbourne BG & DM in the nmssm DSU, June 6, /18
12 LHC "precision" C. Balázs, Monash U Melbourne BG & DM in the nmssm DSU, June 6, /18
13 Mass determination at the ILC Processes utilized at ILC (lumi 500 fb -1 ) e + e - Ø W è + 1 W è - 1 e + e - Ø Z è 2 Z è 4 e + e - Ø Z è 3 Z è 4 è results for individual masses m Z é m Z é 1 = 33.3±1.1 GeV m Z é 3 = 181.5±5.2 GeV m W è = GeV += 165 ± 0.3 GeV 1 è after inclusion of e + e - Ø W è + 1 W è - 1 threshold scan m Z é 1 = GeV è resulting precision of W Z é 1 is comparable to WMAP! C. Balázs, Monash U Melbourne BG & DM in the nmssm DSU, June 6, /18
14 ILC precision C. Balázs, Monash U Melbourne BG & DM in the nmssm DSU, June 6, /18
15 ILC precision C. Balázs, Monash U Melbourne BG & DM in the nmssm DSU, June 6, /18
16 Dark matter direct detection C. Balázs, Monash U Melbourne BG & DM in the nmssm DSU, June 6, /18
17 Dark matter indirect detection C. Balázs, Monash U Melbourne BG & DM in the nmssm DSU, June 6, /18
18 Conclusions nmssm improves on MSSM: no m problem, less fine-tuning, looser constraints on EWBG All matter in the Universe can be simultaneously generated in the nmssm Model can be discovered at LHC, direct detection, and low energy experiments (e - EDM) ILC precision is critical for determining astrophysical parameters: relic density, WIMP-nucleon scattering,... C. Balázs, Monash U Melbourne BG & DM in the nmssm DSU, June 6, /18
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