Neutralino Dark Matter in the NMSSM, D. E. L ´ opez-Fogliani. 1 ✬ ✫ ✩ ✪ Neutralino Dark Matter in the NMSSM Daniel E. L ´ opez-Fogliani Universidad Aut ´ onoma de Madrid Departamento de F´ ısica Te ´ orica and IFT D. Cerde ˜ no, C. Hugonie, D. L-F., C. Mu ˜ noz, A. Teixeira, JHEP 0412 (2004) 048 E. Gabrielli, D. L-F., C. Mu ˜ noz, A. Teixeira, hep-ph/06????? IRGAC 2006, Barcelona, 11-15 July
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Neutralino Dark Matter in the NMSSM, D. E. Lopez-Fogliani. 1'
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Neutralino Dark Matter in the NMSSM
Daniel E. Lopez-Fogliani
Universidad Autonoma de Madrid
Departamento de Fısica Teorica and IFT
D. Cerdeno, C. Hugonie, D. L-F., C. Munoz, A. Teixeira, JHEP 0412 (2004) 048
E. Gabrielli, D. L-F., C. Munoz, A. Teixeira, hep-ph/06?????
IRGAC 2006, Barcelona, 11-15 July
Neutralino Dark Matter in the NMSSM, D. E. Lopez-Fogliani. 2'
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Index
Introduction
Dark Matter in the NMSSM
• The NMSSM
• The DM-Nucleus Cross Section
• Experimental constraints
• Analysis of DM in the NMSSM
Conclusions
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The problem of galaxy rotation curves
Far from the center of the galaxy we expect: v =√
GMvis
R∼ 1√
R
But observation gives v ∼ cte
Solution
Dark Matter: Postulated for the first time by Zwicky (1933)
Neutralino Dark Matter in the NMSSM, D. E. Lopez-Fogliani. 4'
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WMAP
Energy composition of the Universe
• Ordinary Matter→ 4 %
• Dark Matter→ 23 %
• Dark Energy→ 73 %
Cold Dark Matter→ 0.094 . Ωh2 . 0.129 WMAP’06
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WIMPs
• WIMP’s very promising and exciting DM candidates:
stable, massive, weakly interacting particles;
enough WIMP’s left after Big Bang to acount for observed DM
SUSY
• R parity→ the LSP is absolutely stable
• SUSY provides good candidates to Dark Matter
From SUSY models→ the WIMP by excellence is the lightest Neutralino
Neutralino Dark Matter in the NMSSM, D. E. Lopez-Fogliani. 6'
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WIMP’s Direct Detection
Since 1987 there are a lot of experiments around the world