1. 29/09/2016Susy DM Tools1 SUSY DM TOOLS, ENTApP Visitor Program, DESY

2. 29/09/2016Susy DM Tools2 Outline MSSM NMSSM: Daniel Lopez Fogliani

3. 29/09/2016Susy DM Tools3 Motivation: computation of neutralino relic density (1) Early Universe dense and hot; WIMPs in thermal equilibrium Universe expands and cools; WIMP density is reduced through pair annihilation; Boltzmann suppression: n~e -m/T Temperature and density too low for WIMP annihilation to keep up with expansion rate → freeze out Final dark matter density:  h 2 ~ 1/ Thermally avaraged cross section of all annihilation channels

4. 29/09/2016Susy DM Tools4 MSSM: many possible processes Complete spectrum needed to compute  h 2 of the neutralino

5. 29/09/2016Susy DM Tools5 Ingredients for computation of Neutralino masses and decomposition bino, wino, higgsino admixture Sfermion masses (bulk, coannhilation)‏ or at least lower limits on them, and mixing angles Higgs masses and widths: h,H,A tan  Yukawa couplings, etc. General MSSM has ~120 free parameters. Models of SUSY-breaking give relations between the soft terms → more predictive, easier to analyse

6. 29/09/2016Susy DM Tools6 GUT scale EW scale Boundary conditions of SUSY breaking model e.g. m 0, m 1/2, A 0 Boundary conditions: Gauge and Yukawa couplings @ mZ Run gauge and Yukawa couplings up to GUT scale,  1 =  2 =  3, 2 x 10 16 GeV SUSY scale Run all parameters back down to SUSY scale Radiative electroweak symmetry breaking, threshold corrections to sparticle masses (= shift from running to pole masses)‏ Interation until required precision is achieved Run all parameters back down to EW scale Spectrum computation within a model of SUSY breaking

7. 29/09/2016Susy DM Tools7 Gaugino masses M 1 :M 2 :M 3 =       Higgs mass parameters m H2 2 < 0 due to heavy top effect → radiative EWSB !!  from minimalization condition Slepton masses stay ~ m 0 Squark masses driven ~ M 3

8. 29/09/2016Susy DM Tools8 State of the Art 2-loop RGEs for gauge and Yukawa couplings as well as for all SUSY-breaking parameters 1-loop SUSY corrections to gauge and Yukawa couplings Higgs potential at 2-loops Sparticle pole masses at 1-loop Quite a complicated task → public tools Isajet, Softsusy, Spheno, Suspect

9. 29/09/2016Susy DM Tools9 Comparison Codes

10. 29/09/2016Susy DM Tools10 SUSY Les Houches Accord (SLHA)‏ Text-file based I/O standard to interface SUSY tools P. Skands et al., hep-ph/0311123

11. 29/09/2016Susy DM Tools11 SLHA interface Block MODSEL # Select model 1 1 # sugra Block SMINPUTS # Standard Model inputs 1 1.279340000e+02 # alpha^(-1) SM MSbar(MZ)‏ 2 1.166370000e-05 # G_Fermi 3 1.172000000e-01 # alpha_s(MZ) SM MSbar 4 9.118760000e+01 # MZ(pole)‏ 54.250000000e+00 # mb(mb) SM MSbar 6 1.743000000e+02 # mtop(pole)‏ Block MINPAR # Input parameters 1 1.000000000e+02 # m0 2 2.500000000e+02 # m12 3 1.000000000e+01 # tanb 4 1.000000000e+00 # sign(mu)‏ 5 -1.000000000e+02 # A0

12. 29/09/2016Susy DM Tools12 SLHA Output fd

13. 29/09/2016Susy DM Tools13 SUSY Les Houches Accord + F77 I/O Library by T. Hahn (now also SLHA2)‏ SUSY MODEL MSSM SUGRA GMSB AMSB NMSSM RPV CPV FLV … CPSUPERH FEYNHIGGS ISASUSY NMHDECAY SOFTSUSY SPHENO SUSPECT … SPECTRUM CALCULATOR CALC/COMPHEP ILCSLEPTON GRACE HERWIG (++)‏ ISAJET PROSPINO PYTHIA SHERPA SMADGRAPH SUSYGEN WHIZARD … MC EVENT GEN / XS CALCULATOR MICRΩS DARKSUSY NEUTDRIVER PLATON (?)‏ CDM PACKAGE DECAY PACKAGE FEYNHIGGS FCHDECAY HDECAY NMHDECAY SDECAY SPHENO spectru m spc+de c sp c input spectru m      FITTINO, SFITTER, SUPERBAYESFITTERS  

14. 29/09/2016Susy DM Tools14 How is done in practice?

15. 29/09/2016Susy DM Tools15 Micromegas

16. 29/09/2016Susy DM Tools16....

17. 29/09/2016Susy DM Tools17 Code organization

18. 29/09/2016Susy DM Tools18 New developments

19. 29/09/2016Susy DM Tools19 Outlook

20. 29/09/2016Susy DM Tools20 DarkSusy Either all low-energy parameters can be given by the user, or MSSM or mSUGRA* parameters can be used. *) Interface to ISASUGRA, SUSPECT DarkSUSY is a set of Fortran routines for calculations of relic densities and different direct and indirect detection rates in supersymmetric models.

21. 29/09/2016Susy DM Tools21 Calculable quantities Vertices Mass spectrum Accelerator bounds Relic density Scattering cross sections Rates in neutrino telescopes Fluxes from the halo: antiprotons, positrons, continuum gammas, gamma lines (  and  ) and neutrinos.

22. 29/09/2016Susy DM Tools22 Accelerator bounds Routines to check current accelerator constraints are available: m H 2 b  s  m  + sfermion masses(g-2)  etc It is easy to replace the standard routines with your own ones.

23. 29/09/2016Susy DM Tools23 Scattering cross sections The scattering cross sections on protons and neutrons are calculated. The quark and spin content of the nucleons can be changed by the user.

24. 29/09/2016Susy DM Tools24 Neutrino telescopes From WIMP annihilation in the Earth/Sun, we can calculate: – the neutrino flux – the neutrino to muon conversion rate – the neutrino-induced muon flux Both differential and integrated fluxes/rates can be obtained. The new population of WIMPs (Damour-Krauss) that have scattered in the outskirts of the Sun can be included.

25. 29/09/2016Susy DM Tools25 Antiprotons from the halo Different propagation models can be used: Chardonnay et el, Bottino et al, Bergström et al *. Energy losses of antiprotons are included. Many diffusion model parameters are adjustable. Solar modulation can be included. Fluxes from a clumpy halo can be calculated. *) Default

26. 29/09/2016Susy DM Tools26 Positrons from the halo Different diffusion models included: Kamionkowski-Turner and Baltz-Edsjö with * and without a cut-off in the diffusion constant. Both integrated and differential fluxes can be obtained.

27. 29/09/2016Susy DM Tools27 Gammas from the halo The flux in a given direction (averaged or not averaged over detector resolution  ) can be obtained for – continuum gamma rays – monochromatic gamma lines from  – monochromatic gamma lines from Z  Both differential and integrated fluxes can be obtained.

28. 29/09/2016Susy DM Tools28 Neutrinos from the halo From a given direction (averaged or not averaged over detector resolution  ) we can obtain the – neutrino flux – neutrino to muon conversion rate – neutrino-induced muon flux Both differential and integrated fluxes/rates can be obtained.

29. 29/09/2016Susy DM Tools29 Code organization The code is written in Fortran. The user has to provide a main program – an example program is provided. Current Version 4.1: www.physto.se/~edsjo/darksusy

30. 29/09/2016Susy DM Tools30 Comparisons

31. 29/09/2016Susy DM Tools31 mSUGRA parameter space GUT-scale boundary conditions: m 0, m 1/2, A 0 [plus tan , sgn(  )] 4 regions with right  h 2  bulk (excl. by m h from LEP)  co-annihilation  Higgs funnel (tan  ~ 50)‏  focus point (higgsino scenario)‏

32. 29/09/2016Susy DM Tools32 Fixing SM parameters is not enough Impact on CDM varying mtop

33. 29/09/2016Susy DM Tools33 A popular approach: chi-square analysis tan  = 10 m 0 fitted to WMAP m t fixed to central value Ellis et al, JHEP 0605 (2006) 005 (hep-ph/0602220) tan  = 50 m 0 fitted to WMAP m t fixed to central value “In that framework [CMSSM with a neutralino LSP], the range of m 0 is very restricted by the CDM density determined by WMAP and other observations, for any set of assumed values of tan , m 1/2 and the trilinear soft supersymmetry-breaking parameter A 0 ” neutralino mass (GeV) ‏ Chi-squared grid

34. 29/09/2016Susy DM Tools34 Bayes’ Theorem prior posterior likelihood  Probability density Bayesian Parameter Estimation

35. 29/09/2016Susy DM Tools35 11 22 11 P 11 P 11 22  2 INTEGRATED OVER  2 FIXED Marginalization

36. 29/09/2016Susy DM Tools36 (1) Select a random point in parameter space,  0 Compute P(  0 ) = Like*Prior (2) Propose a new point,  1 with transition probability T, satisfying T(  0,  1 ) = T(  1,  0 )‏ (3) Evaluate P(  1 ) = Like*Prior (4) If P(  1 ) > P(  0 ) move to  1 else move to  1 with probability = P(  1 )/P(  o )‏ MCMC = Markov Chain Monte Carlo Obtain a Markov Chain:  i, i = 1,..., N The density of points is proportional to the target distribution, P(  ) Number of points scales as the number of model's parameters MCMC algorithm

37. 29/09/2016Susy DM Tools37 Bayesian Analysis of the CMSSM CMSSM parameters ‘Nuisance’ parameters Observables (with full likelihood)‏ SUSY mass limits (LEPII), Higgs limits, BR’s, g-2, EW observables, cosmological CDM abundance

38. 29/09/2016Susy DM Tools38 What we have?

39. 29/09/2016Susy DM Tools39 Not very much apart from setting an upper limit to m 1/2 ! (WMAP1 data) ‏ Ruiz de Austri, Trotta, Roszkowski (2006) ‏ Just how constraining is  m h 2 ?

40. 29/09/2016Susy DM Tools40 Fully marginalised constraints vs chi-sq fits m t fixed tan  = 10 fixed m 0 fitted to WMAP m t, m b,  S,  EM, tan , constrained through data excepting and integrated over Ellis et al (2005), hep-ph/0508169 Ruiz de Austri et al (2007 ‏ ) ‏ Telling the truth with statistics m0m0

41. 29/09/2016Susy DM Tools41 Higgs Searches

42. 29/09/2016Susy DM Tools42 Probability density 4 TeV prior 2 TeV prior 4 TeV prior, no g-2 Sleptons, squarks: prior and g-2 dependent Probability density SUSY at the LHC Eg, gluino mass < 2.7 TeV with 78%prob ROBUST

43. 29/09/2016Susy DM Tools43 Dark matter direct detection LHC 1 event/Ton/year LHC 1 event/Kg/year

44. 29/09/2016Susy DM Tools44 SuperBayeS.org

45. 29/09/2016Susy DM Tools45 Thank you !