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James L. Pinfold University of Alberta

AstroCollider Physics. ASTROPARTICLE PHYSICS AND THE LHC. James L. Pinfold University of Alberta. Menu. The LHC and its multi-purpose detectors, for high p t physics (and forward physics?) Forward physics at the LHC and Cosmic Ray physics The cosmic ray energy spectrum

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James L. Pinfold University of Alberta

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  1. AstroCollider Physics ASTROPARTICLE PHYSICS AND THE LHC James L. Pinfold University of Alberta

  2. Menu • The LHC and its multi-purpose detectors, for high pt physics (and forward physics?) • Forward physics at the LHC and Cosmic Ray physics • The cosmic ray energy spectrum • Understanding cosmic ray air showers & the NEEDS project • Exotic physics (already seen in CR emulsions?) • UHECR and SUSY • The synergy between astroparticle physics and high pT LHC physics • WMAP & SUSY dark matter (MSUGRA, GMSB and split SUSY) • LHC and dark matter (eg neutralino Dark Matter) • Direct detection of dark matter • Indirect detection of dark matter • A brief look at gravitino dark matter • Extra dimensions • Collider signatures of Extra Dimensions • Evidence for Extra Dimensions from the cosmos • Mini black hole production at the LHC and in HECR interactions • COSMOLHC – the direct detection of cosmic rays with LHC detectors • Conclusions

  3. The LHC Collider LHC ring ~26km in circ. • SCHEDULE • LHC install by the end of 2006 • First beam: April 2007 • First collisions: ~July 2007 • 2007: First physics = 4 fb-1 • 2008-09: Low lumi = 20 fb-1/y • 2010+: High lumi = 100 fb-1/y

  4. The LHC Detectors • PHYSICS TARGETS • ATLAS, CMS: • - Higgs boson(s) • - SUSY particles • …?? • ALICE: • Quark Gluon Plasma • LHC-B: • CP violation in the B sector • TOTEM: • Total pp x-section • MoEDAL: • Monopole search • (LoI stage only) CMS MoEDAL

  5. Measuring the Forward Region at the LHC ? CMS The present LHC coverage TOTEM • TOTEM (at the CMS IP)~ 3 Roman Pot stations at both sides of IP to detect leading proton in elastic scattering and in diffractive interactions plus 2 telescopes (3<||<7) to study inelastic interactions in forward region • Similar coverage being planned for ATLAS

  6. A Benchmark Measurement of stot(pp) Goal of CMS/TOTEM and ATLAS: ~ 1 % precision Measured by TOTEM -t  (4-mom. transfer)2  (pscat)2 (p=7 TeV) Nel, Ninel : no’s of elastic & inelastic events (dNel/dt)|t=0: (extrap.of) diff. elastic rate at t=0   Re[forward amp.] /Im[forward amp.] = 0.10 0.01 Curves are ~ (log s) To achieve ~ 1% accuracy on tot need to Measure Ninel over large rapidity range to minimize acceptance correction For ||  7 acceptance is 99 % measure dNel/dt down to -t ~ 2 x 10-2 GeV2 to minimize extrapolation to t=0  Of particular interest for cosmic ray physics is the measurement of the total & inelastic X-section as well as the ratio of sdiff/sinel

  7. Forward physics at the LHC and Cosmic Ray Physics

  8. The LHC & HECR Energy Spectrum • Studies of LHC collisions with pp (& pA, AA) x-sections are important in refining our understanding the HECR energy spectrum. • Is there something that colliders can contribute to understanding of the knee? For example, a new threshold: • The sextet quark model where enhanced WW/ ZZ production has a threshold at the knee (~1015 eV) • The Tevatron energy is just too low but the LHC could see a clear effect. • Is the CR spectrum, beyond the GZK cut-off, due to physics beyond the SM? • From monopoles • From extra dimensions that induce strong n x-sections • Originating from massive relic particle decay with MX >1012 GeV, • From SUSY particles such as the S0 (uds-gluino) High energy CRs consist of protons, nuclei, gammas,… GZK Cut-off HECR manifest themselves as extended air showers (EAS)

  9. Forward Physics - the LHC & CRs • Forward directions (| |>5): few particles with low pT but very high energy (>90% of the event energy) relevant to HECR • Collider physics measurement emphasis: • High Transverse energy: Jets, Leptons, Leptonic secondaries & ETmiss • Cosmic Ray Extended Air Shower (EAS) measurements involve primarily: • Total/inelastic x-section; fraction of diffractive dissociation; energy flow; particle multiplicity distributions; hadronic secondaries • The study of hA interaction is mostly limited to fixed target (FT) energies, (sNN)hA < 0.03 TeV (new data from RHIC (Au-Au) is at~0.2 TeV) but Feynman Scaling breaks down at higher energies (eg Tevatron, LHC). • Uncertainties in the MC prediction of the development EAS are due to uncertainties in the calculation of hadronic interactions. ET E  EAS EAS

  10. Colliders & CR EAS - The NEEDS Meeting • Major uncertainties in our understanding of Cosmic ray observables still exist • The NEEDS workshop - held in Karlsruhre in 2002 - discussed which measurements of hadronic interactions are key to our understanding of CR physics. Some central questions were: • How important are the uncertainties in our knowledge of hadronic interactions in the determination of CR flux & comp. • Will planned expts reduce these uncertainties. • What additional expts are necessary. • A brief list of some of the most important measurements for shower development: • A precise measurement of the stot & sinel. proton cross-sections • Energy distribution of the leading nucleon in the final state • Measurement of sdiff/sinel • Inclusive p-spectra in the frag. region xF >0.1 • Ideally make these measurements for pp, AA, and pA at the LHC. EG-1 The HECR Energy spectrum EG-2 World data:<log mass>

  11. Cosmic Ray Exotics at the LHC • Centauro events have been predominantly observed in CR emulsion exposures in balloons • Centauros all characterized by: • Abnormal hadron dominance in multiplicity/energy. • Low hadron mult. (wrt AA collisions of similar energy) • PT of produced particles more than “normal” (PT~1.7 GeV/c) • Pseudorapidity distributions consistent with formation & isotropic decay of a fireball • The CASTOR (CMS) proposal makes charge particle mult. & EM/HAD E-flow up to |h| ~8 • A tungsten/quartz fibre calorimeter • CASTOR’s objectives, measure: • EEM/Ehad • Longitudinal shower evolution • Search for Centauros, etc. • L=1.5m, 8 sectors ~ 9

  12. HECRs and SUSY • A possible origin of UHECRs is the decay of a supermassive particle Mx with mass related to the unification mass scale 1024 GeV • Schematic view of a ‘jet’ for an initial squark from the decay of the ‘X’ particle • Particles with mass of order mSUSY decay at the 1st vertical line. For mSUSY< Q < 0.1 light QCD DOFs still contribute to the evolution of the cascade. • At the second vertical line, all partons hadronize and unstable hadrons + leptons decay. • At best we would only detect on earth one particle of the ~104’s of particles produced in the decay of an ‘X-particle’. • Thus, we will only be able to make studies of the single-particle inclusive spectra of protons, n’s, LSPs & g’s. • Thus, input from the LHC wouldl be vital to study physics at energies up to 1012 GeV. hep-ph/0210142)

  13. The Synergy Between Astroparticle Physics and High pT LHC physics

  14. WMAP & Dark Matter • Launch of WMAP satellite in June 2001  1st data, February 2003. • The vastly increased precision of the WMAP CMB data, revealed temperature fluctuations that vary by only millionths of a degree. • Best fit cosmological model (including CB, ACBAR, 2dF Galaxy Redshift Survey and Lyman alpha forest data) give the following energy densities (units of the critical density): • ΩL = 0.73±0.04 (Vacuum energy) • Ωb = 0.044±0.004 (baryon density) • Ωm = 0.27±0.04 (Matter density • One can derive the cold dark matter density • 0.94 < ΩCDM h2 < 0.129 (95% CL) (Cold dark matter) – normalized Hubble Constant =0.71 ± 0.04 • Little or no hot dark matter

  15. Constraining Dark Matter Candidates Disfavoured by BR (b  s) from CLEO, BaBar BELLE BR (b  s) = (3.2  0.5)  10-4 used Favoured by g-2 (E821) Favoured by cosmology assuming 0.1    h2  0.3 Favoured by cosmology assuming 0.094    h2  0.129 i.e. new WMAP results        b s • Dark matter candidates are legion: axions, gravitinos, neutralinos, KK particles, Q balls, superWIMPs, self-interacting particles, branons… SUSY DARK MATTER (MSUGRA) (5 params m0- common scalar mass; m1/2 – common gaugino mass; A0 - common trilinear coupling; tanb; m - Higgsino mass parameter) mSUGRA A0=0 , Ellis et al., hep-ph/0303043 Co-annihilation region Focus point region Forbidden LSP = stau Bulk region “co-annihilation region” “bulk region”

  16. Investigating DM at the LHC SUSY studies at the ATLAS/LHC will proceed in four steps: • SUSY Discovery phase (inclusive searches) success assumed! • Inclusive Studies (comparison of significance in inclusive channels etc). • First rough predictions of Wch2 within specific model framework (e.g. Constrained MSSM / mSUGRA). • Exclusive studies (calculation of model-independent SUSY masses) and interpretation within specific model framework. • Model-independent calculation of LSP mass for comparison with e.g. direct searches; detailed model-dependent calculations of DM quantities (Wch2, scp, fsun etc.) • Less model-dependent interpretation. • Approach to model-independent measurement of Wch2 etc. through measurement of all relevant masses etc.

  17. First Step - Inclusive Constraints ATLAS constraints Direct Detection jets+ETmiss+X channel in ATLAS Dan Tovey WIMP-N x-section (pb). Dan Tovey M0 (GeV) The next direct DM searches (~1tonne) could probe cosmologically favoured regions (s~10-10 pb) not accessible to the LHC: 1) Focus point scenarios (large m0); 2) models with large tan(b). 5s reach of the inclusive SUSY searches at ATLAS for mSUGRA with large tanb probing regions inaccessible to the current DM expts

  18. Step 2 Inclusive Studies LHC Point 5 (Physics TDR) • Assuming that SUSY is revealed at the LHC the next step will be to test broad features of the potential DM candidate. • 1st Question: is R-Parity Conserved? • If YES possible DM candidate • LHC experiments sensitive only to LSP lifetimes < 1 ms (<< tU ~ 13.7 Gyr) • 2nd Question: is the neutralino the LSP? • Natural in many MSSM models • If YES then test for consistency with astrophysics • If NO then what is it? • e.g. Light Gravitino DM from GMSB models (not considered here) R-Parity Conserved R-Parity Violated ATLAS Non-pointing photons from c01gGg GMSB Point 1b (Physics TDR) ATLAS

  19. Stage 2/3: Model-Dependent DM CMSSM A0=0 , Ellis et al. hep-ph/0303043 Disfavoured by BR (b  s) = (3.2  0.5)  10-4 (CLEO, BELLE) Favoured by g-2 (E821) Assuming  = (26  10)  10 -10 from SUSY ( 2  band) 0.094    h2  0.129 (WMAP) Forbidden (LSP = stau) • If a viable DM candidate is found initially assume specific consistent model • e.g. CMSSM / mSUGRA. • Measure model parameters (m0, m1/2, tan(b), sign(m), A0 in CMSSM): Stage 2/3. • Check consistency with accelerator constraints (mh, gm-2, bgsg etc.) • Estimate Wch2g consistency check with astrophysics (WMAP etc.) • Ultimate test of DM at LHC only possible in conjunction with astroparticle experiments gmeasure mc , scp, fsunetc.

  20. Step 3 - Mass Measurements e+e- + m+m- 30 fb-1 Point 5 ATLAS TDR llq threshold lq edge llq edge 2% error (100 fb-1) 1% error (100 fb-1) 1% error (100 fb-1) p p ~ c01 TDR, Point 5 ~ ~ ~ ~ q c02 g lR TDR, Point 5 TDR, Point 5 ATLAS ATLAS ATLAS q q l l • Model parameters estimated using fit to measured positions of kinematic end-points observed in the chain of decays in SUSY event. Model independent estimate of masses will also be made • At point 5 expected precisions after 30 fb-1on M0, M1/2 & Tan b are ± 2.3%, ± 0.9% and 0.5% respectively

  21. Stage 2/3: Model Parameters Point m0 m1/2 A0 tan(b) sign(m) LHC Point 5 100 300 300 2 +1 SPS1a 100 250 -100 10 +1 LHC Point 5 (A0 =300 GeV, tan(b)=2, m>0) Sparticle Mass (LHC Point 5)Mass (SPS1a) qL~690 GeV ~530 GeV 02233 GeV 177 GeV lR157 GeV 143 GeV 01122 GeV 96 GeV Point SPS1a (A0 =-100 GeV, tan(b)=10, m>0) ~ ~ ~ ~ • First indication (Stage 2) of CMSSM parameters from inclusive channels • Compare significance in jets + ETmiss + n leptons channels • Detailed measurements (Stage 3) from exclusive channels when accessible. • Consider here two specific example points: ATLAS

  22. Step 34 Relic Density Scenarios • Use parameter measurements to estimate Wch2 , direct detection cross-section etc. (e.g. for 300 fb-1, SPS1a) • W c h2 = 0.1921  0.0053 & log10(scp/pb) = - 8.17  0.04

  23. dR =p.Af(A) .S(A,ER).I(A).F2(A,ER).g(A).e(Ev) dEv Direct Searches for WIMPs • Predicted nuclear recoil energy spectrum depends on astrophysics (DM halo model), nuclear physics (form-factors, coupling enhancements) and particle physics (WIMP mass and coupling). p = WIMP-nucleon scattering cross-section, f(A) = mass fraction of element A in target, S(A,ER) ~ exp(-ER/E0r) for recoil energy ER, I(A) = spin/coherence enhancement (model-dep.), F2(A,ER) = nuclear form-factor, g(A) = quenching factor (Ev/ER), (Ev)= event identification efficiency.

  24. Direct DM Searches EDELWEISS CDMS DAMA ZEPLIN-I CRESST-II ZEPLIN-2 EDELWEISS 2 ZEPLIN-4 GENIUS XENON ZEPLIN-MAX • Next generation of tonne-scale direct Dark Matter detection experiments should give sensitivity to scalar WIMP-nucleon cross-sections ~ 10-10 pb. (Slide supplied from D. Tovey)

  25. Indirect Dark Matter Searches • Indirect neutralino dark matter can be detected via neutralino annihilations giving rise to 3 main signals. • The 1st of these signals arises from n’s produced by neutralino annihilation in the sun’s/earth’s core. These n’s detected via CC interactions (ν µ conv’s) in n-telescopes such as AMANDA. • The planned neutrino telescopes ANTARES & IceCube are sensitive to Eµ > 10 GeV & Eµ > 25–50 GeV, respect. • The 2nd signal stems from g-rays originating from neutralino annihilations in the galactic core & halo producing hadrons, giving rise to g’s primarily from p0 decays. • These signals can be detected by space- based detectors such as EGRET or GLAST with thresholds as low as 100’s of MeV and in atmospheric Cerenkov telescopes on the ground, with detection thresholds in the range 20100 GeV. • The 3rd signal is provided by hard cosmic ray positrons produced in the decays of leptons, heavy quarks & gauge bosons from neutralino annihilations in our galactic halo. A “clumpy halo” is required to get sufficient s/n. • Space-based anti-matter detectors such as AMS-02 and PAMELA will provide precise measurements of the positron spectrum and may be able to detect a possible positron signal from neutralino annihilation. • All of these measurements are prone to large systematic uncertainties, for example on quantities such as neutralino densities and density variations in the core & halo of the galaxy.

  26. Putting it All Together The black contour depicts the exclusion that we can expect from the planned future direct detection (DD) dark matter experiments (σSI> 10-9 pb). The S/B > 0.01 contour for halo produced positrons (blue-green contour) and The LHC (100 fb-1) can cover the HB/FP region up to m1/2 ∼ 700 GeV, which corresponds to a reach in mgluino of ~1.8 TeV Reach of IceCube ν telescope with Fsun(μ) = 40 μ’s/km2/yr and Eμ > 25 covering the FP region to 1400GeV The Tevatron (10 fb-1) could cover the Higgs annihilation corridor as shown by red dashed line If SUSY lies in the upper FP region, then it may be discovered 1st by IceCube (+ possibly Antares), & confirmed later by direct DM detection and the LC1000.

  27. What if the Graviton is the LSP? • Assume gravitino is LSP. Early universe behaves as usual, WIMP freezes out with desired thermal relic density • Gravitinos are superweakly-interacting massive particles –“superWIMPs” as all interactions are suppressed by MW/MPl ~ 10-16 • Current scenarios favour a long lifetime for the WIMP (~1 year) - A year passes…then all WIMPs decay to gravitinos • Are there observable consequences? Well late decays, t̃→ t G̃ can modify light element abundances • Independent 7Li measurements are all low by factor of 3 - SuperWIMP DM naturally explains 7Li ! MPl2/MW3 ~ year

  28. Collider Phenomenology • Each SUSY event produces 2 metastable sleptons with a spectacular signature: highly-ionizing charged tracks • Current bound (LEP): ml̃ > 99 GeV • Tevatron Run II reach: ml̃ ~ 150GeV • LHC reach: ml̃ ~ 700 GeV in 1 year • Slepton trapping: • Sleptons live for roughly a year, so can be trapped for the decays to be observed later • LHC: 106 sleptons/yr possible, but most are fast. By optimizing trap location and shape, can catch ~100/yr in 1000 m3we. (a 1000 a year at the LC) • Measurement of G  mG̃ • WG̃. SuperWIMP contribution to dark matter • SUSY breaking scale • Early universe (BBN, CMB) in the lab

  29. Extra Dimensions • The broad features of theories of Extra Dimensions (EDs) are as follows: • Compactification of the n EDs generates a KK (Kaluza-Klein) tower of states - a generic feature of models with compactified EDs. • Most of the ED models fall into 3 classes • 1st, the large extra dimension (LED) ADD scenario in which: • Gravity propagates in the bulk, the matter gauge forces live on the 3-brane. • There is an emission and exchange of large KK towers of gravitons finely spaced in mass. • 2nd - In the RS scenario where the hierarchy is generated by the large curvature of the EDs: • There exists 1 ED and the TeV+Planck branes within a 5-D space of constant -ve curvature that forms the bulk - where gravity can propagate. • All of the SM particles and forces are confined to the TeV brane • 3rd - The UED scenario all fields can propagate in the bulk and branes do not need to be present Often assume that EDs have a common size R (3+1+n ) dimensions (3+1) dimensions

  30. Searching for EDs at Colliders • Searches for LEDs have usually assumed the ADD scenario. EG at LEP graviton emission & virtual graviton effects from LEDs have been sought • Hadron collider reach (ADD scenario) for real graviton emission and virtual graviton effects • In RS scenario there are KK excitations of the SM gauge fields with masses ~TeV, that would manifest themselves at the LHC as resonances. • The constraints from data + theoretical asssumptions/ requirements mean that the RS scenario could be ruled out completely at the LHC N=27 ~80 pb-1

  31. Astrophysical/Cosmological Limits on EDs Anomalous heating of neutron stars by gravitionally trapped KK graviton modes SN cooling via graviton emission Radiative decay of gravitons to g’s, contribute to the diffuse g back-grounds • Although some of these limits are stringent they are indirect and contain large systematic errors. Although the n =2 scenario looks to be in trouble. • Ignoring these limitations we see that the astrophysical constraints allow low-gravity models with MD ~1TeV, n  4. • If extra dimensions are discovered at the LHC it would provide useful input to our understanding of astrophysics/cosmology.

  32. Extra Dimensions & the Radion • In the RS scenario the radion field is a scalar field which stabilizes the size of the extra-dimensions. Parameters: radion mass (m ), radion vev ( ), h- mixing () • The presence of the radion is one of the key phenomenological consequences of theories of warped EDs such as RS. • Similar couplings as SM Higgs but with different strengths ( gg is enhanced wrt the Higgs , WW/ZZ suppressed in some cases);   HH important if open. << H • Precise measurements of couplings needed to disentangle /H. The determination at the LHC would be ~10%. • The experimental efforts to determine the properties of the radion field have a cosmological significance since the size of the interaction of the radion field with SM particles determines whether it can decay quickly enough to avoid overclosure by the beginning of BBN. • The ADD scenario also admits a light radion (10 MeV > Mf > 10-3 eV) that is a potential source of dark matter similar to axionic dark matter

  33. Searching for the Radion at ATLAS •  = 1 TeV mH=125 GeV (For 100 fb-1 of data)

  34. Black Hole Production at the LHC • Big surprise: BH production is not an exotic remote possibility, but the dominant effect! (Limitation:lack of knowledge of quantum gravity effects ) • Main idea: when the Ecm reaches the fundamental “Planck”scale, a BH is formed; x-section is given by the black disk; σ ~ πRS2 ~ 1 TeV-2 ~ 10-38 m2 ~ 100 pb • The underlying assumptions rely on 2 simple qualitative properties: the absence of small couplings; the “democratic” nature of BH decays • Black holes decay immediately ( ~ 10-26 s) by Hawking radiation: large multiplicity, small Etmiss, jets/leptons ~ 5 • Black holes to hadrons/leptons/g,W,Z/Higgs ~ 75%/20%/3%/2% James Pinfold ATLAS Athens Physics Workshop 20

  35. Black Holes in ATLAS Preliminary studies : reach is MD ~ 6 TeV for any  in one year at low luminosity. MBH ~ 8 TeV By testing Hawking formula  proof that it is BH + measure of MD,  Precise measurements of MBH & TH needed (TH from lepton & g spectra) • The end of short-distance physics? Naively – yes, once the event horizon is larger than a proton, a HEP collider would only produce BHs! • But, gravity couples universally, so each new particle, which can appear in the BH decay would be produced with ~1% probability (if its mass is less thanTH ~ 100 GeV) • Time required for a 5s Higgs discovery: MP = 1/3/5 TeV 1 hr/1 wk/1yr. SUSY particles would also enjoy a similar rapid discovery mode • Black hole decays open a new window into new physics! Hence, rebirth of the short-distance physics! Clean BH samples would make LHC a new physics factory as well

  36. Black Hole Production by Cosmic Rays (Feng and Shapere, hep-ph/0109106) hep-ph/0311365 • Consider BH production deep in the atmosphere by UHE neutrinos - detect them, e.g. in PAO, Ice3 or AGASSA • OFO 100 BHs can be detected before the LHC turns on • But can the BH signature be uniquely established? nD=6 PAO limit (96% CL)

  37. COSMOLHC – the Direct Detection of Cosmic Rays with LHC Detectors

  38. Cosmo-LHC • The LHC detectors will deploy unprecedented areas of precision muon tracking, tracking and calorimetry ~100m underground • In the spirit of Cosmo-LEP the LHC detectors could be used to detect and measure cosmic ray events directly

  39. Muon Physics Plus with CosmoLHC • CosmoLHC – carrying on CosmoLEP (L3+C, CosmoALEPH). Topics to study: • Single/inclusive m’s (pt spectrum >20 GeV 2TeV, angular dist. 0 < q < 50o, charge ratio, etc.) • Upward going m’s (E spectrum, angular distribution, etc.) • Multi-m’s (composition measurements, etc.) • Muon bundles (evidence for new physics?) • Isoburst events seen in LVD, KGF (an hyp. is that they are due to the decay of WIMPS (M> 10 GeV) – better measured at the LHC.) • These measurements will yield data on: • Forward physics of hadronic showers • Primary composition of cosmic rays • Non-uniformities (sidereal anisotropies, bursts, point sources, GRBs) • New physics (eg anomalous muon bundles)? • One can also place detectors in coincidence (cosmic strings) L3+C Single muon data L3+C A muon “bundle” event

  40. Concluding Remarks • There is a considerable and growing synergy between collider & astroparticle physics A good example of this partnership is the search for dark matter. Ultimate test of DM at LHC only possible in conjunction with astroparticle experiments g measure mc , scp,, fsunetc. • The nature of discovery physics is that it often occurs when it is least expected  astrocollider physics maximizes the coverage of “possibility space”

  41. Extra SLIDES

  42. ATLAS Weight 7K tonnes 46m 25m Scale

  43. LHC- Direct Search for Monopoles • An LOI for the MoEDAL experiment to search for monopoles, dyons & other highly ionizing objects has been accepted by the LHCC. • The MoEDAL detector is essentially a “partial” plastic ball deployed around the LHCb vertex chamber region. • Highly ionizing objects are detected by etching the plastic’s “ionization damage” zones • Threshold Z/b > ~10. (Z/b for a highly relativistic monopole ~1500) • Advantages: • Minimizes assumptions about the nature of the monopole or dyon • Essentially no SM background. In principle 1 event should be enough for a discovery • Very Very cost effective (plastic ball) Detection medium, plastic track-etch detectors (CR39)

  44. Indirect Search for Monopoles/Dyons pT1 + pT2 Also searched in cosmic rays ATLAS, 100 fb-1 Caveat: there will be large form factor suppression in the cross-section if the monopole is not point-like

  45. The Mysteries of an Opaque Universe • The universe is opaque to UHECR • In the case of the GZK cut-off a 5x1019 eV proton has a mfp of 50 mpc due to interaction with photons in the the CMB. • But no nearby sources have been identified • How are the protons with energy > EGZK getting to us? There are two scenarios: • BOTTOM UP: acceleration in AGNs, g-ray bursters, etc. Then production of a neutral (n, so,etc). • BOTTOM UP with GZK cut-off relaxed by violation of Lorentz Invariance, etc. • Or TOP DOWN: topological defects (cosmic strings, monopoles, etc.) or massive relics, etc. Region restricted by GZK cut-off ~100 Mpc 10,000Mpc Size of observable universe

  46. Cosmic Ray Exotica • Centauro, Mini-Centauros, Chirons, Geminions are all characterized by: • Abnormal hadron dominance in multiplicity/energy. • Low total hadron multiplicity compared to that expected for A-A collisions in that energy range • PT of produced particles higher than “normal” • PT ~1.7 GeV/c for centauros • PT of 10-15 GeV/c for chirons • Pseudorapidity distributions consistent with formation and isotropic decay of a fireball with: • Nh ~100 & MFB for centauros and chirons • Nh ~15 and MFB ~ 35 GeV for mini-centauros • Anti-Centauros: • Events with abnormal EM dominance • Long Flying Component: • Unusually penetrating cascades, clusters of showers… • Halo Events: • Dense EM cascade containing several hadronic cores spaced closely together (small rel. PT)– in many multi-halo events the halos are aligned, where halos are EM showers in jets. • Muon Bundles: • Events where bundles of muons with very small lateral separation as if produced in a process with very small PT A Centauro Model Does the production of strangelets play a role in Centauro-type phenomena?

  47. Focus Point Region • Relic density can also be reduced if c has significant Higgsino component to enhance Feng, Matchev, Wilczek (2000) • Motivates SUSY with multi-TeV g̃, q̃, l̃ c±/c0 highly degenerate • Such SUSY would be missed at LHC, discovered at LC Baer, Belyaev, Krupovnickas, Tata (2003) James Pinfold Fermilab June 2005

  48. DM Detectors (as of summer 2004) • CDMS (Stanford/Soudan) • CDMS I Shallow site (Stanford) • punch through fast neutrons from cosmic ray µ spallation. • Subtraction by MC checks on multiple scatters limit at 3x10-6pb. • CDMS II underground operation at Soudan mine from April 2003 • 56 live days data collected, blind analysis completed, limit at 4x10-7pb • CRYO-ARRAY tonne scale detector in planning stages • XENON (DUSEL) • R&D programme to develop two phase xenon target completed • Proposal submitted for construction of 100kg module for 2007 deployment • Intend tonne scale final detector for deployment at DUSEL • XMASS (Kamioka) • 3kg two phase xenon dark matter detector in operation. • High background due to radon contamination (200 Bq/m3!) • 20kg module under construction • DAMA (Gran Sasso) • 9x9.7 kg crystals in shield: 7 years data analysed • Annual variation observed in total event rate < 6keV (+ noise rej.) • LIBRA (250kg) NaI array construction completed • Edelweiss (Frejus) • Ge thermal/ionisation detector. 50 kg.days data from 4x320g units • 2002 no events in recoil region (one on boundary) giving ~10-6pb limit. • 2003 data runs see neutron events in nuclear recoil region, confirms limit. • 28x320g array expected operation in 2004: 40kg array planned • CRESST (Gran Sasso) • CRESST I: Sapphire bolometer: low WIMP mass, spin interaction reach • CRESST II: CaWO4 thermal/scint: 300g demonstrator operated • Engineering runs completed: neutrons observed, no shielding • 10kg (33x330g) stack in construction: SQUID readout incorporated

  49. Parameter Expected precision 30 fb-1 300 fb-1 m0 3.2% 1.4% m1/2 0.9%  0.6% tan(b)  0.5%  0.5% Point m0 m1/2 A0 tan(b) sign(m) LHC Point 5 100 300 300 2 +1 SPS1a 100 250 -100 10 +1 Point m0 m1/2 A0 tan(b) sign(m) LHC Point 5 100 300 300 2 +1 SPS1a 100 250 -100 10 +1 Sparticle Mass (LHC Point 5)Mass (SPS1a) qL~690 GeV ~530 GeV 02233 GeV 177 GeV lR157 GeV 143 GeV 01122 GeV 96 GeV ~ ~ ~ ~

  50. Colour Sextet Quark Model - Notes Dfirectly rom Mike Albrow’s talk - “GTEV Gluon Physics at the Tevatron”

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