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Dark Matter Particle Physics View

Dark Matter Particle Physics View. Outline DM candidates Direct DM Search Indirect DM Search Possible Manifestations DM Profile of the Milky Way. Dmitri Kazakov JINR/ITEP. Problem # 3. What is Dark Matter ?. ?. ?. ?. DARK. TRANSPARENT. INVISIBLE. What is it made of ?.

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Dark Matter Particle Physics View

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  1. Dark MatterParticle Physics View • Outline • DM candidates • Direct DM Search • Indirect DM Search • Possible Manifestations • DM Profile of the Milky Way Dmitri Kazakov JINR/ITEP

  2. Problem # 3 What is Dark Matter ? ? ? ? DARK TRANSPARENT INVISIBLE What is it made of ?

  3. DM Candidates The Dark Matter is made of: • Macro objects – Not seen • New particles – right neutrino - neutralino - sneutrino - axion (axino) - gravitino - heavy photon - heavy pseudo-goldstone - light sterile higgs Non from the SM

  4. SU(3) The Standard Model SU(2) U(1) Forces Electromagnetic Particles Strong Weak H Gravity The Higgs boson

  5. SUSY Dark Matter Neutralino = SUSY candidate for the cold Dark Matter Neutralino = the Lightest Superparticle (LSP) = WIMP photino zino higgsino higgsino • Superparticles are created in pairs • The lightest superparticle is stable

  6. DM Detection Direct detection Indirect detection • EGRET -> GLAST • Diffuse Gamma Rays • HEAT, AMS01 -> PAMELA • Positrons in Cosmic Rays • BESS -> AMS02 • Antiprotons in Cosmic Rays DAMA, Zeplin, CDMS, Edelweiss No convincing evidence so far Hope for new results soon First Evidence of DM annihilation!

  7. DAMA ZEPLIN Edelweiss CDMS Projections DIRECT DM SEARCHES Spin-dependent Spin-independent Predictions from EGRET data assuming Supersymmetry

  8. Recent Results on Direct Detection Spin Independent Spin Dependent 10-36 cm2 The Chicagoland Observatory for Underground Particle Physics (COUPP) Cryogenic Dark Matter Search (CDMS)

  9. DM Annihilation Dominant annihilation x-section:  +   A  bb quark pair B-fragmentation well studied at LEP! Yield and spectra of positrons, gammas and antiprotons well known!

  10. DM Annihilation X-Sections S-wave dominant P-wave dominant

  11. DM Interactions with Matter Main Diagrams Cross-section for quark subprocess

  12. Diffuse Gamma Rays from the Sky

  13. Excess of Diffuse Gamma Rays Above 1 GEV A: inner Galaxy (l=±300, |b|<50) B: Galactic plane avoiding A C: Outer Galaxy D: low latitude (10-200) E: intermediate lat. (20-600) F: Galactic poles (60-900)

  14. Analysis of EGRET Data in 6 Sky Directions

  15. Background + Signal Describe EGRET Data

  16. Diffuse Gamma Rays in EGRET Energy Range

  17. H H2 4 R [kpc] Fitted Halo Parameters Gamma Ray Flux: (<v> from WMAP) Enhancement of rings over 1/r2 profile 2 and 7, respectively. Mass in rings 1.6 and 0.3% of total DM 14 kpc coincides with ring of stars at 14-18 kpc due to infall of dwarf galaxy 4 kpc coincides with ring of neutral hydrogen molecules!

  18. halo DM bulge disk Inner Ring Outer Ring Halo Profile and Rotation Curve Halo profile with rings of DM Rotation curve of the Milky Way

  19. Halo density on scale of 30 kpc Sideview Topview

  20. Support for the Ring Structure Thegas layer of the Galactic Disk as function of the distancefrom theGalactic center. N-body simulation of the tidal disruptionof the Canis Major dwarf Galaxyfitted to the observed stars (red points). The simulationpredicts a ringlike structure of dark matter with a radiusof 13 kpc

  21. Positron Fraction and Anatiprotons from DM Annihilation PAMELA First Data 2008 AMS On ISS

  22. DM is the Window to the Physics beyond the SM What the future may bring?

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