# Presentation: 433621

## Dan Hooper
Particle Astrophysics Center
Fermi National Laboratory
dhooper@fnal.gov

*Particle Astrophysics Center*
*Fermi National Laboratory*
*dhooper@fnal.gov*

- Implications of Direct Dark Matter Experiments for
- MSSM Higgs Searches at the Tevatron

- Pheno 06 Symposium University of Wisconsin                May 15, 2006

## How To Search For Supersymmetry     and Neutralino Dark Matter

**Indirect Detection **
**Colliders**
**    **
**       **
** **

**How To Search For Supersymmetry     and Neutralino Dark Matter**

## Direct Dark Matter Detection

**Prospects depend on the neutralino’s elastic scattering cross section with nuclei**
**Leading experiments include CDMS (Minnesota), Edelweiss (France), and Zeplin (UK)**
** **

**Direct Dark Matter Detection**

## Direct Dark Matter Detection

** **

**Direct Dark Matter Detection**

**q**

**q**

****

****

**h,H**

**q**

**q**

****

****

**q**

**~**

**Cross section depends on numerous SUSY parameters: neutralino mass and composition, tan********, squark masses and mixings, Higgs masses and mixings**

**SUSY Models**

## Direct Dark Matter Detection

** **

**Direct Dark Matter Detection**

**Current Status**

**CDMS**

**Zeplin, Edelweiss**

**DAMA**

**Supersymmetric **
**Models**

## Direct Dark Matter Detection

** **

**Direct Dark Matter Detection**

**Near-Future Prospects**

**CDMS**

**Zeplin, Edelweiss**

**DAMA**

**Supersymmetric **
**Models**

**CDMS, Edelweiss Projections**

## Direct Dark Matter Detection

** **

**Direct Dark Matter Detection**

**Long-Term Prospects**

**CDMS**

**Zeplin, Edelweiss**

**DAMA**

**Supersymmetric **
**Models**

**Super-CDMS, Zeplin-Max**

## Direct Dark Matter Detection

** **

**Direct Dark Matter Detection**

**What does direct detection tell us?**
**Models with large cross sections                              are dominated by Higgs exchange,                  couplings to b, s quarks**
**Squark exchange contribution                      substantial only below ~10****-8**** pb **
**Leads to correlation between                         neutralino composition, tan ********, m****A****	****	****	****        ****and the elastic scattering rate**
**Direct detection searches depend                               on the quantity: **
**          ****|N****11****|****2**** |N****13****|****2 **** tan****2******** / m****A****4**** **

**A. Taylor, Hooper, in preparation**

## Searches For Heavy MSSM Higgs at the Tevatron

**            **p p  A/H X + - X                                	                                                              	p p  A/H bb bb bb
** **
** **

**Searches For Heavy MSSM Higgs at the Tevatron**

## Searches For Heavy MSSM Higgs at the Tevatron

** **
** **

**Searches For Heavy MSSM Higgs at the Tevatron**

## Searches For Heavy MSSM Higgs at the Tevatron

** **
** **

**Searches For Heavy MSSM Higgs at the Tevatron**

## Searches For Heavy MSSM Higgs at the Tevatron

** **
** **

**Searches For Heavy MSSM Higgs at the Tevatron**

**Both depend on tan********, m****A**

## Direct Detection and Collider Searches

** **
** **

**Direct Detection and Collider Searches**

**Current CDMS Limit**

**For a wide range of M****2**** and ********,  much stronger current limits on tan********, m****A**** from CDMS than from the Tevatron **

**M. Carena, Hooper, P. Skands, hep-ph/0603180**

## Direct Detection and Collider Searches

** **
** **

**Direct Detection and Collider Searches**

**M. Carena, Hooper, P. Skands, hep-ph/0603180**

**Limits from CDMS imply heavy Higgs (H/A) is beyond the reach of the Tevatron, unless LSP has a very small higgsino fraction (********>>M****2****)**** **

**3******** discovery reach, 4 fb****-1**

**Projected 2007 CDMS Limit (assuming no detection)**

## Direct Detection and Collider Searches

** **
** **

**Direct Detection and Collider Searches**

**H/A discovery (3********) not possible given current CDMS limits**

**H/A discovery (3********) not possible given projected 2007 CDMS limits (assuming no detection) **

**M. Carena, Hooper, P. Skands, hep-ph/0603180**

**Constrained heavy Higgs (A/H) discovery potential at the Tevatron (4 pb****-1****) **

## Caveats

** **
** **

**Caveats**

**The LSP is a neutralino**
**R-parity is conserved**
**GUT relations for M****1****, M****2 ****(LSP not mostly wino)**
**No large CP-violating phase of ******** (can reduce elastic scattering)**
**Local dark matter (neutralino) density of ~0.3 GeV/cm****3**
**Standard dark matter velocity distribution (no tidal steams, etc.) **

**Our Results depend on the following assumptions:**

## Interplay Between Collider and Astrophysics Experiments

**Astrophysics and collider experiments are highly complementary and should be used to assist each other**
**       **
** **

**Interplay Between Collider and Astrophysics Experiments**

## Putting It All Together

**Putting It All Together**

- LHC+Relic Density

- Actual Value

- +CDMS

**(Hooper, A. Taylor, In preparation)**

## Putting It All Together

**Putting It All Together**

** ****I  C  E  C  U  B  E**

**GLAST**

**A**

**I   C  E**

**P**

**M  E  L  A**

**M S**

**D M S**

**ANTA**

**RES**

**A  T  L        S**

**ZEPLIN**

**DZERO**

**VERITAS**

**M A  G  I   C**

**CDF**

**CMS**

**H   E  S**

## Let’s use all of the tools we have to solve the puzzle of supersymmetry!

** ****I  C  E  C  U  B  E**

**GLAST**

**A**

**I   C  E**

**P**

**M  E  L  A**

**M S**

**D M S**

**ANTA**

**RES**

**A  T  L        S**

**ZEPLIN**

**DZERO**

**VERITAS**

**M A  G  I   C**

**CDF**

**CMS**

**H   E  S**

**Let’s use all of the tools we have to solve the puzzle of supersymmetry!**