non-baryonic dark matter: from the cmb and axial direct detection
DESCRIPTION
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. - PowerPoint PPT PresentationTRANSCRIPT
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
Non-Baryonic Dark Matter:From the CMB and axial direct detection
Daniel SantosLaboratoire de Physique Subatomique et de Cosmologie
Grenoble
(CNRS/IN2P3-UJF-ENSPG)
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
Angular Power Spectrum in Temperature WMAP (2006)
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
CDM modelCMB + Lyman-alpha + clusters + supernovae
Age : 13.7 Gyr
Composition :
Geometry : flat inflation (?)
0.93 ± 0.03ns
0.71 ± 0.04h
0.27 ± 0.04m
0.022 ± 0.001bh2
0.73 ± 0.04
1.02 ± 0.02tot
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
Galactic Halo existence justifies local measurements
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
Direct detection strategies
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
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
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
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 capture signature: n + 3He p + 3H + 764 keV
very low sensivity to -rays
no intrinsic X-rays
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
Direct Detection of SUSY particlesElastic 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
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
Cross section 3He- and event rate in MIMAC-He3 (10kg)
• 0.02< Ωh2< 0.15• Accelerator constrains
Exclusion curve for background 10-3 kg-1jour-1
Neutralino mass (GeV/c2)
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
Complementarity with scalar detection
SD and SI not correlated
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
Ionization ratio simulation (SRIM)
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
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
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
MIMAC-He3: (MIcroTPC MAtrix of Chambers of He 3)
spatial High temporal resolution energetic
recoil track projection energy threshold < 1 keV electron/recoil discrimination
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
Range vs. EnergyHe3 recoils Electrons
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
a/b ratio = f (pressure)L~10 cm
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
Time collection = f(pressure)
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
Diffusion of primary electrons
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
Source 3He, 4He, 1H ( LPSC-Grenoble)
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
MIMAC source spectrum at 14kV MIMAC source spectrum at 14kV
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
Recoil energy distribution after a polypropilene foil of 0.44μg/cm2
for acceleration energies of 45 and 50 keV
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
Time of flight measurement of the ion coming out of the MIMAC source at 50 kV
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
Ionization measured in the range of a few keV (in 4He )
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
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Beijing, August 28th 2006 2nd Sino-French Workshop on the Dark UniverseDaniel Santos
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 !