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Non-Baryonic Dark Matter: From the CMB and axial direct detection

Non-Baryonic Dark Matter: From the CMB and axial direct detection. Daniel Santos Laboratoire de Physique Subatomique et de Cosmologie Grenoble (CNRS/IN2P3-UJF-ENSPG). Angular Power Spectrum in Temperature WMAP (2006).  tot. 1.02 ± 0.02.  L. 0.73 ± 0.04.  b h 2. 0.022 ± 0.001.  m.

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Non-Baryonic Dark Matter: From the CMB and axial direct detection

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  1. Non-Baryonic Dark Matter:From the CMB and axial direct detection Daniel Santos Laboratoire de Physique Subatomique et de Cosmologie Grenoble (CNRS/IN2P3-UJF-ENSPG) 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  2. Angular Power Spectrum in Temperature WMAP (2006) 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  3. tot 1.02 ± 0.02 L 0.73 ± 0.04 bh2 0.022 ± 0.001 m 0.27 ± 0.04 h 0.71 ± 0.04 ns 0.93 ± 0.03 LCDM model CMB + Lyman-alpha + clusters + supernovae Age : 13.7 Gyr Composition : Geometry : flat  inflation (?) 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  4. 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  5. Galactic Halo existence justifies local measurements 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  6. Direct detection strategies 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  7. The lightest neutralino • lowest mass linear superposition of superpartners of the gauge and higgs bosons: ~ ~ ~ ~ ~ = a1B + a2W3 + a3H1 + a4H2 • neutral, colorless, only weak interaction • stable with R-parity conservation • non-relativistic at decoupling  CDM • relic density can be compatible with cosmological observations 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  8. 3He for axial detection of non-baryonic dark matter • spin 1/2 nucleus axial interaction with • high signal/noise ratio : energy range ~ 1-5 keV • sensitive to M (WIMP) > 6 GeV • neutron capturesignature: n + 3He p + 3H + 764 keV • very low sensivity to -rays • nointrinsic X-rays 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  9. Direct Detection of SUSY particles • Elastic diffusion -quark : • spin dependent (axial) • SD(AX) αSD(p) × A2 • spin independent (scalar) • SI(AX) αSI (p) × A4 For 3He and 19F : SD » SI 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  10. Cross section 3He-and event rate in MIMAC-He3 (10kg) • 0.02< Ωh2<0.15 • Accelerator constrains Exclusion curve for background 10-3 kg-1jour-1 Neutralino mass (GeV/c2) 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  11. Complementarity with scalar detection sSDandsSI not correlated 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  12. Ionization ratio simulation (SRIM) 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  13. R&D: MIMAC-He3: (MIcro-tpc MAtrix of Chambers of Helium 3) LPSC (Grenoble) : D. Santos, F. Mayet, R. Brissot Coordinateur technique : O. Guillaudin - Electronique : O. Bourrion, G. Bosson, J-P. Richer - Mécanique : Ch. Fourel, T. Cabanel - Source d’ions : T. Lamy, J-C. Curdy, , P. Sole ILL (Grenoble) : P. Van Esch, B. Guerard, G. Manzin Dapnia-Saclay : P. Colas, I. Giomataris 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  14. MIMAC-He3: (MIcroTPC MAtrix of Chambers of He 3) • spatial • High temporalresolution • energetic • recoil track projection • energy threshold < 1 keV • electron/recoil discrimination 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  15. Range vs. EnergyHe3 recoils Electrons 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  16. a/b ratio = f (pressure)L~10 cm 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  17. Time collection = f(pressure) 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  18. Diffusion of primary electrons 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  19. Source 3He, 4He, 1H ( LPSC-Grenoble) 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  20. MIMAC source spectrum at 14kV 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  21. Recoil energy distribution after a polypropilene foil of 0.44μg/cm2for acceleration energies of 45 and 50 keV 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  22. Time of flight measurement of the ion coming out of the MIMAC source at 50 kV 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  23. 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  24. Ionization measured in the range of a few keV (in 4He ) 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  25. 2nd Sino-French Workshop on the Dark Universe Daniel Santos

  26. Conclusions • The nBDM search is an open problem • The axial interaction should be explored • 3He is a very interesting target • A matrix with different targets including 19F at high pressure (2 bar ) is a natural possible extension • The quenching factor measurement in 3He and 4He is inminent • The collaboration is open to people interested ! 2nd Sino-French Workshop on the Dark Universe Daniel Santos

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