Split SUSY at LHC and a 100 TeV collider

Transcription

1 Split SUSY at LHC and a 100 TeV collider Thomas Grégoire With Hugues Beauchesne and Kevin Earl GGI

2 Status of Supersymmetry

3 stop searches gluino searches m t & 700GeV m g & 1.4TeV

4 What does it mean for naturalness? natural SUSY (stop,gluino,higgsino) Papucci, Ruderman,Weiler 11 m 2 h = y2 t q m 2 t 1 + m 2 t 2 stop m 2 Q 3 + m 2 u 3 + A t 2 log. 600GeV 1 1/2 20% TeV gluino m 2 h = 2 2 y2 t s M3 2 log 2 TeV M GeV sin 1 1/2 20%

5 125 Gev Higgs : prefers heavy stops m 2 h = 3G F p 2 2 m4 t log m 2 t m 2 t! ~ 1-10 TeV stop depending on A-term More complete models generally yield %-level fine-tuning 2.5 CMSSM parameter space with tanb = 3, A 0 = experimentally excluded CMSSM m 0 êm excluded vev = 0 allowed excluded by LHC Strumia M 1ê2 êm excluded vev =

6 NMSSM, split generation, low-scale mediation, Dirac gaugino, and R-parity breaking are generically tuned. Arvanitaki, Baryakhtar, Huang, Tiburg, Villadoro 13 Better model building might save the day Scherk-Schwartz SUSY breaking Compressed spectrum Stealth supersymmetry Twin Higgs Dimopoulos, March-Russell 14 LeComte, Martin 11 Dimopoulos, March-Russell, Scoville 14 Fan, Reece,Ruderman 11 Chacko, Goh, Harnik 05 Craig, Howe 13

7 Dirac gauginos In the MSSM gauginos are Majorana M F X 2 Z d 2 XW W Can be Dirac if new superfields are added W 1,W 2,W 3 M D S, T, G N=2 supersymmetry extra-dimension

8 Supersoft SUSY breaking Fox, Nelson, Weiner 02 D 0 Z D-term breaking d 2 W 0 W i i Dirac gauginos do not feed into scalar masses through renormalization m 2 = C i (r) i m 2 i log 2 m 2 i

9 They can be naturally heavier than scalars LHC will have a harder time seeing the gluino... M. Heikinheimo, M. Kellerstein, V. Sanz 12 Kribs, Martin 12...and squarks u ũ g u ũ

10 Squark production 1 shq é q é* L M g é = 2 TeV 10-1 Dirac Gluino Majorana Gluino m q Frugiuele, T.G., Kumar, Ponton

11 R-symmetry With Dirac gaugino: possible to impose an U(1) R-symmetry M D Kribs,Poppitz,Weiner 02 Bounds from FCNC are weaker: off diagonal m ij R[Q, U c,d c,l,e c ]=1 R[H u,h d ]=0 µh u H d

12 Higgs mass Tree-level: Reduced quartic, usual of Dirac gauginos Z d 2 W 0 W i i D 2 = M 2 T a + H u a H u +... When the scalar T is integrated out: h h T h h! 0 Higgs quartic If the mass of is set by and T M 2 T =0

13 No help (at tree-level) from T H u TR d + S H u SR d don t get a vev (In the limit of exact R-symmetry) But do help in models without an R-symmetry Benakli, Goodsell, Staub

14 Loop-level Usual stop correction (but A-terms are 0) h t h 2 t 2 t h h Similar loop from the triplet h 2 T T h 2 T h T h

15 V CW T log m2 T M t log m2 t m 2 t! Very sensitive to T.but so are electroweak precision measurements

16 allowed by EWPT B T =B S = 1 3 I-m 2 adj - M D 2 M GeV 2, m=300 GeV m t = 300GeV 80 madj HGeVL m t = m adj M D HGeVL Bertuzzo, Frugiuele, T.G., Ponton

17 Arkani-Hamed, Dimopoulos 05 Split Supersymmetry Naturalness might not be a good guide SUSY might still be relevant Dark matter Gauge coupling unification UV reasons Gauginos and scalars might not be at the same mass scale natural in for example anomaly mediation

18 Prediction for the Higgs mass The Higgs quartic coupling is predicted at a high scale: (m scalar )= 1 4 (g2 + g 02 ) cos 2 tree-level SUSY Split SUSY MSSM thresholds running thresholds Bagnaschi, Giudice,Slavich,Strumia 14

19 tanb = 50 tanb = 4 tanb = 2 tanb = 1 Split-SUSY Bagnaschi, Giudice,Slavich,Strumia 14 Higgs mass in GeV Observed M h M 1 = M 2 = M 3 = m = 1 TeV Degenerate SUSY scale in GeV

20 Mini-split in anomaly mediation Arvanitaki, Craig, Dimopoulos, Villadoro 12 scalar masses are generated by gravity mediation Z d 4 X XQ Q M 2 pl m 2 = m 2 3/2 but the gaugino masses are generated by AMSB M i = b i 16 2 g2 i m 3/2 Z d 2 XW W M pl

21 µ -term generated through Giudice-Masiero Z d 4 conformal compensator H u H d µ B µ µ m 3/2 Heavy Higgsino

22 Similar spectrum could also arise in gauge mediation Arvanitaki, Craig, Dimopoulos, Villadoro 12 Buican, Meade, Seiberg, Shih 09 W = M R X 1 2 M i g2 i 16 2 M F 3 M R MR 3 = g2 i 16 2 We take the scalars at

23 Gaugino spectrum (deflected AMSB) apple M B = M 1 1+ C µ 11 + Higgsino threshold M W = M 2 [1 + C µ + ] M g = M 3 [1 + ] M i = i g i m 3/2 C µ = µ m 2 A sin2 m 3/2 µ 2 ln m2 A µ 2 m 2 A

24 AMSB Gaugino spectrum Beauchesne, Earl, T.G Gaugino masses M B, W, G GeV M G M B M W C Μ Parametrize deflection from AMSB spectrum

25 Similar expressions for gauge mediation apple M B = M C0 µ 5 + M W = M 2 1+C 0 µ + M g = M 3 [1 + ] M i = g2 i 16 2 C 0 µ = µ m 2 A sin2 m 2 A µ 2 ln m2 A µ 2

26 Similar expressions for gauge mediation 2000 Gaugino masses M B, W, G GeV M W M B M G C' Μ

27 Assume that gluino decay to 3rd generation quarks g é Æ c 1 0 t t g é Æ c 2 0 t t g é Æ c 1 0 b b g é Æ c 2 0 b b g é Æ c 1 + b t + h.c. m B =0GeV m G =1.5 TeV BR M W

28 Electroweakino decays W 0! Bh W +! W + B bino LSP B! W 0 h W +! W 0 + soft wino LSP

29 Parameter space parameters of the model: m 3/2 µ tan m scalar choose: m scalar m 3/2 set tan to reproduce the Higgs mass results in term of C µ and m 3/2

30 Recasting LHC bounds Gaugino spectrum and branching ratios are obtained as a m 3/2 C µ function of and. we simulate the signal using MadGraph- Pythia-Delphes and recast LHC searches ATLAS multi-leptons+b-jets ATLAS 0-1 lepton+b-jets CMS high jets multiplicity CMS 2 OS leptons+jets

31 AMSB M W contours color breaking vacuum Beauchesne, Earl, T.G. 15

32 Gauge mediation

33 LHC 14 prospects looked at 2 sets of cuts same-sign dilepton cohen et al SSDL 2 b-jets or more 6 jets or more H T > 700GeV ET miss > 250GeV 8 signal regions High missing energy CMS-PAS-FTR lepton 6 jets or more 1 b-jet H T > 500GeV E miss T + P lep T 4 signal regions > 450GeV

34 AMSB (discovery) at LHC 14 M W contours 3000 fb 300 fb

35 GMSB (discovery) at LHC 14 M Bcontours

36 Prospect for a 100 TeV collider same-sign dilepton cohen et al High missing energy adapted from Jung, Wells 13 SSDL 3 b-jets or more 7 jets or more H T > 3000GeV ET miss > 800GeV 8 signal regions 2 jets with no lepton > 0.2M e M e > 15TeV E miss T p T > 0.1M e 3 or more b-jest 5 signal regions

37 AMSB at a 100 TeV collider ( 3ab 1 )

38 GMSB at a 100 TeV collider

39 Dark matter If the LSP is a wino: need M W 2.7TeV 100 TeV collider

40 If the LSP is a bino: need dilution If the LSP is a bino-wino mixture ( C µ 4): M ~ several 100 GeV well-tempered neutralino Arkani- Hamed,Delgado,Giudice

41 Gauge couplings unification modified by heavy Higgsino, but seems to work a 1-1 a 2-1 a 3 a HGeVL Arkani-Hamed, Gupta, Kaplan, Weiner, Zowarski