Non baryonic dark matter from the cmb and axial direct detection
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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

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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)

2nd Sino-French Workshop on the Dark Universe

Daniel Santos


Angular Power Spectrum in Temperature WMAP (2006)

2nd Sino-French Workshop on the Dark Universe

Daniel Santos


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

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

  • 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 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. EnergyHe3 recoils Electrons

2nd Sino-French Workshop on the Dark Universe

Daniel Santos


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

2nd Sino-French Workshop on the Dark Universe

Daniel Santos


Time collection = f(pressure)

2nd Sino-French Workshop on the Dark Universe

Daniel Santos


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

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

2nd Sino-French Workshop on the Dark Universe

Daniel Santos


2nd Sino-French Workshop on the Dark Universe

Daniel Santos


Ionization measured in the range of a few keV (in 4He )

2nd Sino-French Workshop on the Dark Universe

Daniel Santos


2nd Sino-French Workshop on the Dark Universe

Daniel 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 !

2nd Sino-French Workshop on the Dark Universe

Daniel Santos


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