Can One Determine TR at the LHC with a or G Dark Matter? e Leszeek Roszkowski Astro–Particle Theory and Cosmology Group Sheffield, England with K.-Y. Choi and R. Ruiz de Austri arXiv:0710.3349 ! JHEP'08 L. Roszkowski, COSMO'08 – p.1 Non-commercial advert L. Roszkowski, COSMO'08 – p.2 MCMC scan + Bayesian study of SUSY models new development, led by two groups: B. Allanach (Cambridge), and us prepare tools for data from LHC and dark matter searches e.g.: Constrained MSSM: scan over m1=2, m0, tan β, A0 + 4 SM (nuisance) param's software package available from SuperBayes.org SuperBayes L. Roszkowski, COSMO'08 – p.3 e.g.: Constrained MSSM: scan over m1=2, m0, tan β, A0 + 4 SM (nuisance) param's software package available from SuperBayes.org SuperBayes MCMC scan + Bayesian study of SUSY models new development, led by two groups: B. Allanach (Cambridge), and us prepare tools for data from LHC and dark matter searches L. Roszkowski, COSMO'08 – p.3 software package available from SuperBayes.org SuperBayes MCMC scan + Bayesian study of SUSY models new development, led by two groups: B. Allanach (Cambridge), and us prepare tools for data from LHC and dark matter searches e.g.: Constrained MSSM: scan over m1=2, m0, tan β, A0 + 4 SM (nuisance) param's arXiv:0705.2012 (flat priors) Roszkowski, Ruiz & Trotta (2007) 4 3.5 3 2.5 (TeV) 2 0 m 1.5 1 0.5 CMSSM µ>0 0.5 1 1.5 2 m (TeV) 1/2 Relative probability density 0 0.2 0.4 0.6 0.8 1 L. Roszkowski, COSMO'08 – p.3 software package available from SuperBayes.org SuperBayes MCMC scan + Bayesian study of SUSY models new development, led by two groups: B. Allanach (Cambridge), and us prepare tools for data from LHC and dark matter searches e.g.: Constrained MSSM: scan over m1=2, m0, tan β, A0 + 4 SM (nuisance) param's arXiv:0705.2012 (flat priors) SI direct detection: σp Roszkowski, Ruiz & Trotta (2007) Roszkowski, Ruiz & Trotta (2007) 4 −4 CMSSM, µ > 0 3.5 −5 EDELWEISS−I 3 ZEPLIN−II −6 XENON−10 2.5 CDMS−II (pb)] −7 SI p (TeV) 2 σ 0 −8 m 1.5 Log[ −9 1 −10 0.5 CMSSM µ>0 −11 0.5 1 1.5 2 0.2 0.4 0.6 0.8 1 m (TeV) m (TeV) 1/2 χ L. Roszkowski, COSMO'08 – p.3 software package available from SuperBayes.org SuperBayes MCMC scan + Bayesian study of SUSY models new development, led by two groups: B. Allanach (Cambridge), and us prepare tools for data from LHC and dark matter searches e.g.: Constrained MSSM: scan over m1=2, m0, tan β, A0 + 4 SM (nuisance) param's arXiv:0705.2012 (flat priors) GLAST and γ–ray flux from GC Roszkowski, Ruiz & Trotta (2007) 4 3.5 3 2.5 (TeV) 2 0 m 1.5 1 0.5 CMSSM µ>0 0.5 1 1.5 2 m (TeV) 1/2 L. Roszkowski, COSMO'08 – p.3 software package available from SuperBayes.org SuperBayes MCMC scan + Bayesian study of SUSY models new development, led by two groups: B. Allanach (Cambridge), and us prepare tools for data from LHC and dark matter searches e.g.: Constrained MSSM: scan over m1=2, m0, tan β, A0 + 4 SM (nuisance) param's arXiv:0705.2012 (flat priors) PAMELA and positron flux Roszkowski, Ruiz & Trotta (2007) Roszkowski, Ruiz, Silk & Trotta (2008) 4 −1 CAPRICE 94 10 HEAT 94+95 3.5 HEAT 00 −2 Moore+ac 10 3 ) −3 NFW+ac e− 10 2.5 Φ + −4 10 e+ NFW (TeV) 2 Φ 0 −5 /( m 10 68% 1.5 e+ NFW profile, BF = 1 Φ −6 CMSSM, µ > 0 10 1 −7 95% 10 0.5 CMSSM µ>0 −8 10 0.5 1 1.5 2 0.1 1 10 100 400 m (TeV) E (GeV) 1/2 e+ L. Roszkowski, COSMO'08 – p.3 SuperBayes MCMC scan + Bayesian study of SUSY models new development, led by two groups: B. Allanach (Cambridge), and us prepare tools for data from LHC and dark matter searches e.g.: Constrained MSSM: scan over m1=2, m0, tan β, A0 + 4 SM (nuisance) param's arXiv:0705.2012 (flat priors) PAMELA and positron flux Roszkowski, Ruiz & Trotta (2007) Roszkowski, Ruiz, Silk & Trotta (2008) 4 −1 CAPRICE 94 10 HEAT 94+95 3.5 HEAT 00 −2 Moore+ac 10 3 ) −3 NFW+ac e− 10 2.5 Φ + −4 10 e+ NFW (TeV) 2 Φ 0 −5 /( m 10 68% 1.5 e+ NFW profile, BF = 1 Φ −6 CMSSM, µ > 0 10 1 −7 95% 10 0.5 CMSSM µ>0 −8 10 0.5 1 1.5 2 0.1 1 10 100 400 m (TeV) E (GeV) 1/2 e+ software package available from SuperBayes.org L. Roszkowski, COSMO'08 – p.3 End of advert L. Roszkowski, COSMO'08 – p.4 SUSY neutralino and other superpartners + Higgs discovered; 2 neutralino's density Ωχh , as determined with LHC data, is consistent with 0:1 WIMP signal detected in DM searches; SI direct detection c.s. σp consistent with value determined from LHC data neutralino is DM! ) Alternatively (potentially more interesting): WIMP signal not found in DM searches down to σSI 10 10 pb p ∼ − and 2 neutralino seemingly stable but its density Ωχh (determined with LHC data) convincingly different from Ω h2 0:1 (WMAP, etc) CDM ' or lightest superpartner at LHC not electrically neutral (e.g. stau) DM is made up of exotic WIMP (axino a or gravitino G) or another ) E–WIMP/superWIMP e e it may become possible to determine T from LHC data alone ) R (TR – highest temp. at which, after inflation, the Universe reaches thermal equilibrium) Possible outcomes from LHC... L. Roszkowski, COSMO'08 – p.5 Alternatively (potentially more interesting): WIMP signal not found in DM searches down to σSI 10 10 pb p ∼ − and 2 neutralino seemingly stable but its density Ωχh (determined with LHC data) convincingly different from Ω h2 0:1 (WMAP, etc) CDM ' or lightest superpartner at LHC not electrically neutral (e.g. stau) DM is made up of exotic WIMP (axino a or gravitino G) or another ) E–WIMP/superWIMP e e it may become possible to determine T from LHC data alone ) R (TR – highest temp. at which, after inflation, the Universe reaches thermal equilibrium) Possible outcomes from LHC... SUSY neutralino and other superpartners + Higgs discovered; 2 neutralino's density Ωχh , as determined with LHC data, is consistent with 0:1 WIMP signal detected in DM searches; SI direct detection c.s. σp consistent with value determined from LHC data neutralino is DM! ) L. Roszkowski, COSMO'08 – p.5 DM is made up of exotic WIMP (axino a or gravitino G) or another ) E–WIMP/superWIMP e e it may become possible to determine T from LHC data alone ) R (TR – highest temp. at which, after inflation, the Universe reaches thermal equilibrium) Possible outcomes from LHC... SUSY neutralino and other superpartners + Higgs discovered; 2 neutralino's density Ωχh , as determined with LHC data, is consistent with 0:1 WIMP signal detected in DM searches; SI direct detection c.s. σp consistent with value determined from LHC data neutralino is DM! ) Alternatively (potentially more interesting): WIMP signal not found in DM searches down to σSI 10 10 pb p ∼ − and 2 neutralino seemingly stable but its density Ωχh (determined with LHC data) convincingly different from Ω h2 0:1 (WMAP, etc) CDM ' or lightest superpartner at LHC not electrically neutral (e.g. stau) L. Roszkowski, COSMO'08 – p.5 Possible outcomes from LHC... SUSY neutralino and other superpartners + Higgs discovered; 2 neutralino's density Ωχh , as determined with LHC data, is consistent with 0:1 WIMP signal detected in DM searches; SI direct detection c.s. σp consistent with value determined from LHC data neutralino is DM! ) Alternatively (potentially more interesting): WIMP signal not found in DM searches down to σSI 10 10 pb p ∼ − and 2 neutralino seemingly stable but its density Ωχh (determined with LHC data) convincingly different from Ω h2 0:1 (WMAP, etc) CDM ' or lightest superpartner at LHC not electrically neutral (e.g. stau) DM is made up of exotic WIMP (axino a or gravitino G) or another ) E–WIMP/superWIMP e e it may become possible to determine T from LHC data alone ) R (TR – highest temp. at which, after inflation, the Universe reaches thermal equilibrium) L. Roszkowski, COSMO'08 – p.5 axino and gravitino E-WIMPs their properties and relic production LSP relic abundance and LHC TR for axino LSP upper bound on LSP mass TR for gravitino LSP distinguishing axinos from gravitinos at LHC summary Outline L. Roszkowski, COSMO'08 – p.6 their properties and relic production LSP relic abundance and LHC TR for axino LSP upper bound on LSP mass TR for gravitino LSP distinguishing axinos from gravitinos at LHC summary Outline axino and gravitino E-WIMPs L. Roszkowski, COSMO'08 – p.6 LSP relic abundance and LHC TR for axino LSP upper bound on LSP mass TR for gravitino LSP distinguishing axinos from gravitinos at LHC summary Outline axino and gravitino E-WIMPs their properties and relic production L. Roszkowski, COSMO'08 – p.6 TR for axino LSP upper bound on LSP mass TR for gravitino LSP distinguishing axinos from gravitinos at LHC summary Outline axino and gravitino E-WIMPs their properties and relic production LSP relic abundance and LHC L. Roszkowski, COSMO'08 – p.6 upper bound on LSP mass TR for gravitino LSP distinguishing axinos from gravitinos at LHC summary Outline axino and gravitino E-WIMPs their properties and relic production LSP relic abundance and LHC TR for axino LSP L.