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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

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


Angular power spectrum in temperature wmap 2006
Angular Power Spectrum in Temperature WMAP (2006)

2nd Sino-French Workshop on the Dark Universe

Daniel Santos


L cdm model

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


2nd Sino-French Workshop on the Dark Universe

Daniel Santos


Galactic Halo existence justifies local measurements

2nd Sino-French Workshop on the Dark Universe

Daniel Santos


Direct detection strategies
Direct detection strategies

2nd Sino-French Workshop on the Dark Universe

Daniel 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

2nd Sino-French Workshop on the Dark Universe

Daniel 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 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


Direct detection of susy particles
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


Cross section 3 he and event rate in mimac he3 10kg
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


Complementarity with scalar detection

sSDandsSI

not correlated

2nd Sino-French Workshop on the Dark Universe

Daniel Santos


Ionization ratio simulation (SRIM)

2nd Sino-French Workshop on the Dark Universe

Daniel 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

2nd Sino-French Workshop on the Dark Universe

Daniel Santos


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


Range vs energy he3 recoils electrons
Range vs. EnergyHe3 recoils Electrons

2nd Sino-French Workshop on the Dark Universe

Daniel Santos


A b ratio f pressure l 10 cm
a/b ratio = f (pressure)L~10 cm

2nd Sino-French Workshop on the Dark Universe

Daniel Santos


Time collection f pressure
Time collection = f(pressure)

2nd Sino-French Workshop on the Dark Universe

Daniel Santos


Diffusion of primary electrons
Diffusion of primary electrons

2nd Sino-French Workshop on the Dark Universe

Daniel Santos


Source 3He, 4He, 1H

( LPSC-Grenoble)

2nd Sino-French Workshop on the Dark Universe

Daniel Santos


Mimac source spectrum at 14kv
MIMAC source spectrum at 14kV

2nd Sino-French Workshop on the Dark Universe

Daniel Santos


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


Time of flight measurement of the ion coming out of the mimac source at 50 kv
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


2 MIMAC source at 50 kVnd Sino-French Workshop on the Dark Universe

Daniel Santos


Ionization measured in the range of a few kev in 4 he
Ionization measured in the range of a few keV (in MIMAC source at 50 kV4He )

2nd Sino-French Workshop on the Dark Universe

Daniel Santos


2 MIMAC source at 50 kVnd Sino-French Workshop on the Dark Universe

Daniel Santos


Conclusions
Conclusions MIMAC source at 50 kV

  • 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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