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Non-accelerator particle and astroparticle physics

Non-accelerator particle and astroparticle physics. - Dark matter - Proton decay - Particle Astrophysics Ultra high energy cosmic rays Gamma rays Neutrinos - Dark energy. Cosmological evidence for DM. CMB + SNs + LSS concordance model. Stable relic from big bang :

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Non-accelerator particle and astroparticle physics

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  1. Non-accelerator particle andastroparticle physics - Dark matter - Proton decay - Particle Astrophysics Ultra high energy cosmic rays Gamma rays Neutrinos - Dark energy Non accelerator physics Nathalie Palanque-Delabrouille

  2. Cosmological evidence for DM CMB + SNs + LSS concordance model Stable relic from big bang : 1 / A v  = 23%  A weak Stars (0.5%) Dark Energy (72%) Baryonic DM (4%) Natural candidate with SUSY theories: the LSP (neutralino) M > 50 GeV from searches at colliders Non-baryonic DM (23%) Non accelerator physics Nathalie Palanque-Delabrouille

  3. A non-baryonic dark halo Microlensing  baryonic matter not the solution Excluded by MACHO MACHO detection Milky Way: Mhalo ~ 10 x Mvisible A dark non-baryonic halo,  ~ 0.3 GeV / cm3 v ~ 220 km / s Non accelerator physics Nathalie Palanque-Delabrouille

  4. Liquid Xe ZEPLIN Ionization Scintillation DAMA NaI EDELWEISS, CDMS CRESST Heat CaWO4 Ge Detection challenge WIMP: elastic scattering on detector nucleus 1evt / kg / day  - Deep underground - Low radioactivity of materials - Discrimination against radioactive background Nuclear (vs. electronic) recoil discrimination: event by event or statistical WIMP signal Radioactive background Non accelerator physics Nathalie Palanque-Delabrouille

  5. Event by event discriminationEdelweiss / CDMS : heat + ionization Edelweiss (Modane lab) CDMS (Soudan mine) 1.5 1.5 Electronic recoil (g) Few (no) events in signal region 1 1 Ionization / recoil Ionization / recoil Surf. evts? 0.5 0.5 Nuclear recoil band (WIMP, n) 0 0 0 50 100 0 50 100 150 200 Recoil energy (keV) Recoil energy (keV) - 250g Ge or 100g Si crystal - sensors to detect vibration & charge - Allows surface event rejection based on pulse shape veto - Edelweiss I 1kg - Edelweiss II 9 kg (up to 36 kg) Non accelerator physics Nathalie Palanque-Delabrouille

  6. 0.1 0.1 0.01 0.01 0.001 0.001 0.0001 0.0001 10 100 10 100 Other technologiesCRESST: scintillation + heat, ZEPLIN: scintillation + charge CRESST : event by event light + phonon discrimination works with many absorber materials (CaWO4, PbWO4, BGO…) ZEPLIN : statistical light + charge discrimination liquid scintillators (Xe) gammas neutrons Pulse time constant (ns) Pulse time constant (ns) some caveats : - no calibration in range of interest for WIMP recoils - no low en. nuclear recoils observed in presence of neutron source  overestimated sensitivity ? Non accelerator physics Nathalie Palanque-Delabrouille

  7. Annual modulationa possible WIMP signature Motion of Earth in the c wind d = 30o Modulation of annual rate ± 7% Max in June vSun = 220 km/s vEarth = 30 km/s DAMA: Total exposure of 295 kg.yr Annual modulation at 6.3 mc ~ 44-62 GeV BUT 1 signature only Result in contradiction with other expts. 2nd phase 250 kg (NaI) LIBRA running Non accelerator physics Nathalie Palanque-Delabrouille

  8. Current limits on WIMP CRESST, EDELWEISS CDMS CDMS-II, EDELWEISS-II, CRESST-II XENON, XMASS - sensitivity goal Testing most SUSY param. space (MSSM) requires 3 orders of magnitude beyond present best performances 1-ton sensitivity goal Non accelerator physics Nathalie Palanque-Delabrouille

  9. Future 1-ton projects EURECA (Europe) EDELWEISS + CRESST collaborations + CERN + … First studies: cryogeny, electronics, shielding Multi target approach: Ge (phonon ionization) CaWO4 (phonon scintillation) Detector R&D ongoing Super-CDMSGe, Si (US) XENON (US), XMASS (Japan) Liquid Xenon (an easier target than a crystal) XENON: 10 kg proto at Gran Sasso ArDM, WARP (Europe) Liquid Argon OK on the paper, feasibility study (calibration w/ source) Non accelerator physics Nathalie Palanque-Delabrouille

  10. 10-6 ga (GeV-1) 10-8 PVLAS 10-10 10-12 10-14 CAST 10-5 10-3 10-1 10 Ma (eV) Axion : a DM candidate? Postulated to solve the strong CP problem Interesting CDM candidates if ma in 10-5 eV - 10-3 eV (a~ 1) Primakoff effect: 2-photon interaction in external B field ADMX CAST PVLAS Microwave cavity for galactic axions 9T field to convert solar axions into X-rays  strong upper limit 6.6T field to search for ellipticity in laser polarization due to axion-induced birefringence  axion-like signal? Non accelerator physics Nathalie Palanque-Delabrouille

  11. Rare processes : proton decay Test of GUTs (MGUT~ 1016 GeV) at low energy 1st generation (IMB, Fréjus,Kamiokande: ~1 kton)  non supersymmetric SU(5) excluded 2nd generation (SuperKamiokande: ~50 kton)  minimal supersymmetric SU(5) excluded Next generation  more general supersymmetric models Need to reach ~ 1035 yrs  1035 nucleons With 6x1023 nucleons / g  Megaton scale detectors Non accelerator physics Nathalie Palanque-Delabrouille

  12. Current limits on proton decay Dominant decay channel in SS GUTs:p  K+  a few x 1034 yrs (in many models) SK limit: 1.6 x 1033 yrs expected sensitivity (MEMPHYS): 2 x 1034 yrs after 10 yrs but model-dependent decay mode Most model independent decay channel:p  e+0 ~ a few x 1034 yrs — 1035 yrs SK limit: 5 x 1033 yrs expected sensitivity (MEMPHYS): 1035 yrs after 10 yrs Within reach of next generation experiments ! Non accelerator physics Nathalie Palanque-Delabrouille

  13. Proton decay : future initiatives UNO(Underground Nucleon decay and neutrino Observatory) Mine in US 440 kT MEMPHYS(MEgaton Mass PHYSics) Fréjus 440 kT HyperK Japan 550 kT Liquid Argon TPCs (FLARE (US), GLACIER (Europe)) ? 100 kT p  e+0  e+ Complementarity liquid argon vs. water Cerenkov p  K+ (higher detection eff.) p  e+0 (larger mass) Non accelerator physics Nathalie Palanque-Delabrouille

  14. Physics with Megaton detectors - Proton decay -  from SN II (20  from SN1987A) out to Galactic Center (spectrum, ms timing structure in collapse) out to the Andromeda galaxy (~10) - diffuse flux of SN relic neutrinos ( insight on history of star formation in Universe) -  properties - atmospheric osc. parameters determined with better resolution - (13, ) finally within reach with  super- and beta- beams (~100 km away) - The Unexpected Non accelerator physics Nathalie Palanque-Delabrouille

  15. Particle astrophysicsor the use of multi-messengers The high energy Universe as seen with Cosmic rays Charged ( do not point except at UHE) Highest energies observed Gamma rays Traditional messenger yet unexplained phenomena (GRBs…) Neutrinos Most challenging to detect, but no GZK Non accelerator physics Nathalie Palanque-Delabrouille

  16. Galactic (SNR) cross calibration needed not confined by galactic B  Extragalactic LEP LHC Complete mystery! On the Ultra High Energy side AGASA: 17 events above 6x1019 eV HiRes : 2 events (~ 20 expected) Emax = 3.2 1020 eV = 50 J ! Non accelerator physics Nathalie Palanque-Delabrouille

  17. Detection techniques for UHECR Primary cosmic ray UV fluorescence Isotropic emission Hadronic and electromagnetic showers Height where shower is maximal  E Xmax Cerenkov radiation forward emission Auger Cerenkov telescope X Air fluorescence HiRes Ground detectors AGASA Non accelerator physics Nathalie Palanque-Delabrouille

  18. GZK cut-off? 1022 Auger: neither cut-off nor ankle (not much stat above 50 EeV) Energy loss due to interaction on CMB photons Not solved yet 1022 eV 1021 eV 1021 Energy (eV) Nb @ E>3 EeV 1020 eV 1020 1019 10 100 103 Propagation distance (Mpc) Non accelerator physics Nathalie Palanque-Delabrouille

  19. Status on experiments Auger South (as of August 2005) - 3 fluorescence stations (out of 4) - 60% of ground detectors (out of a total of 3000 km2) - Emax = 86 EeV (one at 140 EeV but not selected by cuts) Auger North? Would allow - improved statistics - test of isotropy - more possible sources (North: local supercluster) EUSO on ISS: stopped OWL (Orbiting Wide-angle Light-collectors): design with 2 satellites to measure atmospheric scintillation Non accelerator physics Nathalie Palanque-Delabrouille

  20. Gamma ray astronomy Photon = traditional astronomy Straight propagation  allows study of sources Interacts with CMB… backgrounds  existence of a gamma horizon Gamma ray “telescopes” keV — GeV : satellites GeV — TeV : ground-based (IACTs) Recent results with INTEGRAL, HESS, MAGIC, SWIFT Non accelerator physics Nathalie Palanque-Delabrouille

  21. INTEGRAL (20 keV - 10 MeV)INTErnational Gamma Ray Astrophysics Laboratory Very strong 511 keV emission (e+e-) in Galactic Center Dark matter? e+ annihilation at rest (positronium)  New form of DM particle? (1-100 MeV) Hypernovae? needs 1 / 5000 yrs e+ from radioactive decay of CO56 90% of “gamma fog” = 91 sources (47 binary stars, 3 pulsars, … 37 new sources) Non accelerator physics Nathalie Palanque-Delabrouille

  22. H.E.S.S. Radio Contour 20 TeV Neutralino 20 TeV KK particle Systematic pointing error Radio H.E.S.S.: Dark Matter at GC?High Energy Stereoscopic System Preliminary based on early data proposed before H.E.S.S. data  Unlikely pure DM Astrophysical source candidates: - 3x106 Msun black hole SgR A - Supernova Remnant Sgr A East Non accelerator physics Nathalie Palanque-Delabrouille

  23. H.E.S.S. HESS + ASCA HESS + Rosat X and  from same source  first confirmation of SNRs as particle accelerators up to 1014 eV (~knee of CR spectrum) Are they protons/nuclei or e-? Survey of galactic plane 14 new sources (+ 3 already known ones): - SNRs, X-ray binaries, pulsars - 3 with no counterpart at any  Non accelerator physics Nathalie Palanque-Delabrouille

  24. Gamma Ray Bursts Galaxies Quasars GRBs swift Optical counterparts 6 4 Redshift record Cosmological phenomena! out to z = 6.3 (Sept. 2005) 2 0 +6.5h Fading afterglow in X-ray 1960 1980 2000 +12h Afterglow in optical +52h Non accelerator physics Nathalie Palanque-Delabrouille

  25. Future in gamma ray astronomy - GLAST satellite (launch in 2007): 20 MeV - 100 GeV imager 10 keV - 25 MeV GRB detector - HESS 2 with a 5th larger telescope lower threshold (50-100 GeV): overlap with satellites improved sensitivity at high E in coïncidence mode - VERITAS (Arizona), CANGAROO III (Australia) - MAGIC 2 x 17m telescopes Dark Matter searches : gamma rays from neutralino annihilation Several thousand sources (GLAST)  study of source populations Non accelerator physics Nathalie Palanque-Delabrouille

  26. Neutrinos in astronomy Photons: absorbed (GZK) Neutrons: t ~ 15 mn dmax=10 kpc (E=1018 eV) Protons: absorbed (GZK) & deviated (E<1018 eV) Neutrinos:no charge, “no” interaction with matter nor radiation Ideal probes of: dense regions, sources on cosmological scales, acceleration processes Non accelerator physics Nathalie Palanque-Delabrouille

  27. e- g p g g po g p+ - High energy n sources ! nm m+ - nmnee+ - Acceleration processes Low energy emission (X-ray) : Synchrotron emission of e- in jet • High energy emission (g-ray): • self-compton (electro-magnetic) ? • p0 decay (hadronic) ? e- g Non accelerator physics Nathalie Palanque-Delabrouille

  28. Neutrino telescopes Low fluxes @ high E Low cross-sections Large volume (lake, sea, polar ice) High background (atmospheric m) Good shielding (> 1000m water eq.) Non accelerator physics Nathalie Palanque-Delabrouille

  29. ANTARES / AMANDA ANTARES ANTARES (43o North) deployment by end 2007 Better angular resolution (~0.2°) <25% exposure ANTARES/AMANDA 0.6p sr overlap AMANDA AMANDA (South pole) taking data Better sensitivity (less absorption) not visible Non accelerator physics Nathalie Palanque-Delabrouille

  30. Science reach Medium Energy (10 GeV - 1 TeV): - Dark matter searches from dense regions (neutralino concentration & annihilation) AMANDA: reaching the level of direct searches nfrom supernovae High Energy (> 1 TeV): - n from (extra-)galactic sources (cf. gamma rays) - PeV & EeV n - ndetection 1 PeV  Double-bang signature Typical 10 TeV  Non accelerator physics Nathalie Palanque-Delabrouille

  31. Status & future of  astronomy ANTARES, AMANDA: 0,1 km2 arrays Allow assessment of under-ice, under-water  telescopes Possible observation of diffuse neutrino fluxes (from AGN) (current limits from AMANDA reaching predictions from some models) No point sources so far Actual  astronomy (point sources) requires 1 km3 IceCube: 80 1-km long strings over ~1 km2 January 2006: 6 lines deployed KM3: design study in FP6 through network KM3Net Joint study from ANTARES, NESTOR, NEMO Non accelerator physics Nathalie Palanque-Delabrouille

  32. (0,1) (.5,.5) (1,0) (1.5,-.5) (M, ) = (0,0) (1,0) (2,0) Stars Dark Energy Non baryo. DM Baryo DM Revolutions in cosmology Great achievements in past decade with observations of Cosmic Microwave Background Type Ia Supernovae 3K black body (COBE)  expansion of Universe Anisotropies (balloons, WMAP)  composition of Universe + seeds for structure formation Hubble diagram of SNIa (flux vs. redshift)  accelerated expansion Magnitude m Redshift z Non accelerator physics Nathalie Palanque-Delabrouille

  33. reference discovery SNLS SuperNova Legacy Survey : 2003-2008 Megacam (380 million pixels) SN discovery & follow-up simultaneously  Evolution of expansion of Universe since explosion  dark energy Homogeneous set of SN (systematics) Larger statistics: ~150 SN after 1 year of data taking  exceeds previous world stat of SNIa Non accelerator physics Nathalie Palanque-Delabrouille

  34. A dark UniverseA challenge for cosmology and fundamental physics • - Nature of dark matter ? • - What is dark energy ? • Vacuum energy, quintessence, modified gravity, more exotic field? • - Cosmological constant problem: • field theory tends to predict quantum vacuum energy • 1060 - 10120 times higher than closure density • - Coincidence problem: • just at transition (Dark) Matter / Dark Energy • - … or … • - are we totally wrong? Non accelerator physics Nathalie Palanque-Delabrouille

  35. Dark energy status Cosmological equation of state : p = w  matter: w = 0 cosmological constant: w = -1 radiation: w = 1/3 quintessence: w > -1 SNLS, 2008 w = p/ SNLS, 2008 2002 M Aim of SNLS Non accelerator physics Nathalie Palanque-Delabrouille

  36. Future with DUNE, SNAP … Dark energy modifies: expansion rate of the Universe  supernovae growth rate of structures gravitational distortions Future : caracterization of dark energy  Space projects SNAP SNAP: several thousand SNIa Population study (environment, spectral features …) to reduce intrinsic dispersion > 2015 (NASA : Beyond Einstein) DUNE: weak shear analysis Statistics of grav. distortions depend on geometry of universe ~ 2012 (french CNES) or ~ 2015 (ESA) Gravitationally distorted galaxies Non accelerator physics Nathalie Palanque-Delabrouille

  37. The cost of knowledge… *(per experiment) 500 - 1000 M€ proton decay 100 - 500 M€ Space-based dark energy missions 1 km3 neutrino telescopes Other space missions (AMS, EUSO) 10 - 100 M€ Each gamma astro experiment Cosmic rays (per detection site) Direct dark matter detection Much less expensive than particle physics at the energy frontier, yet requires at least regional (world-wide?) coordination * Based on inputs from ApPEC, courtesy of C. Spiering Non accelerator physics Nathalie Palanque-Delabrouille

  38. Do nucleons decay? What physics is there at 1016 GeV? How large can detectors become? Dark energy: Quantum field? New laws of gravity? Messages from the sky: Nature of most energetic phenomena (AGN, GRBs…)? Origin of cosmic rays? Acceleration processes? Dark matter: WIMPS? axions? What knowledge will come from accelerators (LHC, ILC or CLIC)? direct detection (sensitive enough)? sky (gamma rays or UHECR)? Questions as conclusions… Non accelerator physics Nathalie Palanque-Delabrouille

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