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James L. Pinfold University of Alberta

AstroCollider Physics. ASTROPARTICLE PHYSICS AND THE LHC. James L. Pinfold University of Alberta. James Pinfold ISMD 2005. Astro-Collider Physics – The Synergies. Direct Detection of Cosmic Rays in Collider Detectors. High P T Collider Physics

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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 James Pinfold ISMD 2005

  2. Astro-Collider Physics – The Synergies Direct Detection of Cosmic Rays in Collider Detectors High PT Collider Physics Involving ETmiss, jet production, lepton ID, etc Relevant to Dark Matter, Extra Dimensions, etc. Forward (|h|>5) Collider Physics Few particles with low pT but very high energy ( >90% of Eevent) relevant to HECR Astroparticle Physics & Cosmology James Pinfold ISMD 2005

  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 James Pinfold ISMD 2005

  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 accepted) • LHCF: • Forward pion production X-section • measurement (Proposal) CMS James Pinfold ISMD 2005

  5. Forward Physics at the LHC & Astroparticle Physics Forward (|h|>5) Collider Physics Few particles with low pT but very high energy ( >90% of Eevent) relevant to HECR Astroparticle Physics & Cosmology James Pinfold ISMD 2005

  6. Measuring the Forward Region at the LHC see Risto's talk on Totem • Extended coverage being planned for ATLAS (with pots out to 420m?) • The LHC benchmark measurement in this area is that of stot(pp) to ~1% James Pinfold ISMD 2005

  7. Colliders & CR Extended Air Showers • Major uncertainties in our understanding of Cosmic ray observables still exist • The NEEDS workshop (2002) discussed which measurements of hadronic interactions are key to our understanding of CR physics. Eg: • A precise measure of stot /sinel. p-p x-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 • Make these measurement for pp, pA, and AA • To answer these questions ATLAS, CMS TOTEM, CASTOR have been joined by the proposed LHCF Project: “ To Measure Very Forward Particles at the LHC in order to Understand the Highest Energy Cosmic Rays ” • To achieve its aim LHCF aims to measure the production x-section of pions in p-p collisions at the highest energy (≡ 1017eV CR proton) EG-1 The HECR energy spectrum LHCF Detector

  8. The LHC & HECR Energy Spectrum • Studies of forward LHC collisions with pp, pA & AA collisions are needed to refine our understanding of the HECR energy spectrum. • Can colliders can contribute to our understanding of the knee? • Eg the Colour Sextet quark model - 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 inducing strong n x-sections • From massive relic particle (MRP) 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 James Pinfold ISMD 2005

  9. Cosmic Ray Exotics at the LHC • Centauro events have been mostly observed in CR emulsion exposures in balloons – they are 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) • .h distributions consistent with fireball formation & isotropic decay • The LHC CASTOR (CMS) proposal measure 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. One of the mysterious "Centauro" events seen by the Brazil ­ Japan collab. in X-ray emulsion chambers on Mt Chacaltaya • L=1.5m, 8 sectors ~ 9 James Pinfold ISMD 2005

  10. High PT Collider Physics + Cosmology and Astroparticle Physics High PT Collider Physics Involving ETmiss, jet production, lepton ID, etc Relevant to Dark Matter, Extra Dimensions, etc. Astroparticle Physics & Cosmology James Pinfold ISMD 2005

  11. Very High Energy CosmicRays & SUSY • A possible origin of UHECRs is the decay of a MRP, Mx, with mass related to the unification mass scale. • 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. • 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 produced in the ‘X-particle’ decay • Thus we will only be able to study single -particle inclusive spectra of p’s, n’s, LSPs & g’s. • Input from the LHC on SUSY cascade studies are vital to study this physics - at energies up to 1012 GeV. hep-ph/0210142) James Pinfold ISMD 2005

  12. 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) (CDM) – normalized Hubble Constant =0.71 ± 0.04 • Little or no hot dark matter James Pinfold ISMD 2005

  13. Constraining Dark Matter Candidates Disfavoured by BR (b  s) from CLEO, BaBar BELLE BR (b  s) = (3.2  0.5)  10-4 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, branons… • SUSY dark matter (MSUGRA) a good candidate is the neutralino  LHC can explore a lot of the parameter space • MSUGRA would be discovered in one year at the LHC using jets + ETmiss +X mSUGRA A0=0 , Ellis et al., hep-ph/0303043 Co-annihilation region Focus point (FP) region Forbidden LSP = stau Bulk region “co-annihilation region” “bulk region” James Pinfold ISMD 2005

  14. 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. James Pinfold ISMD 2005

  15. 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. James Pinfold ISMD 2005

  16. Indirect Dark Matter Searches • Indirect neutralino dark matter can be detected via neutralino annihilations, giving rise to 3 main signals: • 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, respectively • .g-rays originating from neutralino annihilations in the galactic core & halo producing hadrons, which give rise to g’s mostly from p0 decays. • Detected by space- based detectors such as EGRET/GLAST with thresholds as low as 100’s MeV and in atmospheric Cerenkov telescopes, with thresholds in the range 20100 GeV. • 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 positron signal from neutralino annihilation. • The predicted detection rates are very dependent on the models of neutralino densities, etc. and thus subject to large systematic uncertainties. James Pinfold ISMD 2005

  17. 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 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. James Pinfold ISMD 2005

  18. Extra Dimensions • A broad features of theories of Extra Dimensions (EDs) is that compactification of the n EDs generates a KK (Kaluza-Klein) tower of states • 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. • 2nd - The RS scenario, the hierarchy is generated by the large curvature of the EDs: • There exists 1 ED + the TeV & Planck branes within a 5-D space of constant -ve curvature forming the bulk - where gravity propagates. • SM particles & 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 James Pinfold ISMD 2005

  19. 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, manifested as resonances. • The constraints from data + theoretical requirements mean that the RS scenario could be ruled out completely at the LHC N=27 ~80 pb-1 James Pinfold ISMD 2005

  20. 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 like it’s in trouble. • Ignoring these limitations we see that the astrophysical constraints allow low-gravity models with MD ~1 TeV, n  4. • If EDs are discovered at the LHC it would provide useful input to our understanding of astrophysics/cosmology. James Pinfold ISMD 2005

  21. Black Hole Production at the LHC • In theories with large EDs BH production is not an remote possibility, but could be the dominant effect when the Ecm reaches the “Planck” scale • The Cross-section is given by the black disk; σ ~ πRS2 ~ 1 TeV-2 ~ 10-38 m2 ~100 pb. • Two qualitative assumptions: the absence of small couplings; the “democratic” nature of BH decays • BHs decay to give large multiplicity, small ETmiss, jets/leptons ~5  hadrons/leptons/g,W,Z/Higgs ~ 75%/20%/3%/2% • BH decays open a window into new physics! Clean BH samples would make LHC a new physics factory. EG SUSY particles produced ~1% level James Pinfold ISMD 2005

  22. Black Holes at the LHC • The LHC reach is MD ~ 6 TeV for any  in one year at low luminosity • Once the event horizon is larger than a proton, the LHC would only produce BHs! An example of an ATLAS BH event is shown below. ATLAS MBH ~ 8 TeV James Pinfold ISMD 2005

  23. Black Hole Production by Cosmic Rays • 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? hep-ph/0311365 nD=6 (Feng and Shapere, hep-ph/0109106) PAO limit (96% CL) James Pinfold ISMD 2005

  24. Direct Detection of CRs at the LHC Direct Detection of Cosmic Rays in Collider Detectors Astroparticle Physics & Cosmology James Pinfold ISMD 2005

  25. 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

  26. Muon Physics Plus with CosmoLHC L3+C • CosmoLHC – carrying on CosmoLEP (L3+C, CosmoALEPH). Topics to study: • Single/inclusive m’s • Upward going m’s (E spectrum, angular distribution, etc.) • Multi-m’s + Muon bundles • Isoburst events seen in LVD, KGF (due to the decay of WIMPS with M> 10 GeV??) • 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 large area coincidence (cosmic strings) Single muon data L3+C A muon “bundle” event

  27. 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”

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