# Presentation: 785147

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

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

- What Can We Learn About Supersymmetry
- From Astrophysical Experiments?

- University of Oregon          Cosmo/Astro Mini-Workshop        May 22-26, 2006

## Based On:

**M. Carena, DH, P. Skands, hep-ph/0603180**
**F. Halzen, DH, hep-ph/0510048, PRD **
**DH and Andrew Taylor (in preparation)**

## The Existence of Dark Matter

**Galaxy and cluster rotation curves have pointed to the presence of large quantities of non-luminous matter for many decades (compelling since the 1970’s)**
**White dwarfs, brown dwarfs, Jupiter-like planets, neutron stars, black holes, etc?**

## The Dark Matter Density

**WMAP best-fit ********CDM model (for a flat Universe):**
**73 % Dark energy (************= 0.73) **
**27 % Matter (********M****h****2 ****= 0.27)**
**********h****2  ******** 0.0076**

**Big Bang nucleosynthesis combined with cosmic microwave background determine ********B****h****2**** ******** 0.024**
**But, we also know ********M**** ~ 0.3, so most of the matter in the Universe is ****non-baryonic dark matter!**

**Fields and Sarkar, 2004**

**Baryonic**** ****Abundance**

**Notes:**
Basic facts

**Observations of the large scale structure of our Universe can be compared to computer simulations**
**Simulation results depend primarily on whether the dark matter is hot (relativistic) or cold (non-relativistic) when structures were formed**
**Most of the Universe’s matter must be ****Cold Dark Matter**

**Cold Dark Matter and Structure Formation**

**Notes:**
Basic facts

## “The world is full of obvious things which nobody by any chance ever observes.”

**“****The world is full of obvious things which nobody by any chance ever observes.”**
**-Sherlock Holmes**

## The Particle Nature of Dark Matter

**A virtual zoo of dark matter candidates have been proposed over the years.  100’s of viable candidates.**
**Weakly Interacting Massive Particles (WIMPs) are a particularly attractive class of dark matter candidates. **

**The Particle Nature of Dark Matter**

## Introduces new bosons for fermions and vice versa
Elegant extension of the Standard Model
Natural solution to hierarchy problem (stabilizes quadradic divergences to Higgs mass)
Restores unification of couplings
Requirement of proton stability implies the stability of the Lightest Supersymmetric Particle (LSP) by the virtue of R-parity
The lightest neutralino is among the most natural possibilities for the LSP 

*Elegant extension of the Standard Model*
*Natural solution to hierarchy problem (stabilizes quadradic divergences to Higgs mass)*
*Restores unification of couplings*
*Requirement of proton stability implies the stability of the Lightest Supersymmetric Particle (LSP) by the virtue of R-parity*
*The lightest neutralino is among the most natural possibilities for the LSP *

**Supersymmetry**

## The Lightest Neutralino

**Properties of the lightest neutralino can vary wildly depending on its composition**
**The composition of the lightest neutralino will likely not be determined at the LHC**
**Annihilation and elastic scattering cross sections with nucleons can vary over many orders of magnitude depending on LSP’s composition (and sparticle spectrum, tan ********, etc.)**
**By including astrophysical measurements with LHC data, it may be possible to determine the composition of the lightest neutralino**** **

**Bino**

**Wino**

**Higgsinos**

## Can Astrophysics Measure ?

**Can Astrophysics Measure ********?**

## Supersymmetry At The Tevatron

**For example,**
**For the case of light m****A**** and large tan********, heavy MSSM higgs bosons (A/H) are observable**
**Tevatron searches for light squarks and****	****	****	****	**** gluinos are also interesting**
**Tevatron SUSY searches only possible if****	****	****	****superpartners are rather light**

**Supersymmetry At The Tevatron**

## Supersymmetry At The LHC

**Squarks/gluinos decay to distinctive combinations of leptons, jets and missing energy (LSPs)**
**Capable of discoverying squarks/gluinos as heavy as  ~3 TeV**
**                   **

**Supersymmetry At The LHC**

## Supersymmetry At The LHC

**By studying decay kinematics, lightest neutralino mass to be measured to ~10% precision**
**Masses of sleptons and heavier neutralinos may also be determined if sufficiently light **
**But what is the nature of the LSP?**
**Is it dark matter?**
**                   **

**Supersymmetry At The LHC**

## Direct Detection 

**    ****- Momentum transfer to detector **
**          ****through elastic scattering **
**Indirect Detection **
**    ****- Observation of annihilation **
**           ****products (********, e****+****, p, ********, etc.)**
**       **
** **

**Astrophysical Dark Matter Experiments**

## Direct Detection

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

**Direct Detection**

## Direct Detection

** **

**Direct 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 Detection

** **

**Direct Detection**

**Current Status**

**CDMS**

**Zeplin, Edelweiss**

**DAMA**

**Supersymmetric **
**Models**

## Direct Detection

** **

**Direct Detection**

**Near-Future Prospects**

**CDMS**

**Zeplin, Edelweiss**

**DAMA**

**Supersymmetric **
**Models**

**CDMS, Edelweiss Projections**

## Direct Detection

** **

**Direct Detection**

**Long-Term Prospects**

**CDMS**

**Zeplin, Edelweiss**

**DAMA**

**Supersymmetric **
**Models**

**Super-CDMS, Zeplin-Max**

## Direct Detection

** **

**Direct Detection**

**But 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****              ****  **

## 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****) **

## Indirect Detection: Neutrinos

**Captured at a rate ~ 10****18**** s****-1****  (************p****/10****-8**** pb) (100 GeV/m********)****2**
**Over billions of years, annihilation/capture rates equilibrate**
**Annihilation products are absorbed, except for neutrinos**
** **

**Indirect Detection: Neutrinos**

## Indirect Detection: Neutrinos

**Full cubic kilometer instrumented volume**
**Technology proven with predecessor, AMANDA**
**First string of detectors deployed in 2004/2005, **
**8 more strings deployed in 2005/2006 (80 in total)**
**Sensitive to muon neutrinos above ~ 100 GeV**
**Similar physics reach to KM3 in **
**Mediterranean Sea**
** **

**Indirect Detection: Neutrinos**

## Indirect Detection: Neutrinos

**Direct detection limits impact rates anticipated in neutrino telescopes**
** **

**Indirect Detection: Neutrinos**

## Indirect Detection: Neutrinos

**Direct detection constraints on spin-dependent scattering are still very weak**
** **

**Indirect Detection: Neutrinos**

_**Spin-Independent**_

_**Spin-Dependent**_

## Indirect Detection: Neutrinos

**Indirect Detection: Neutrinos**

- q

- q

**Always Small**

******  ****|f****H1****|****2**** - |f****H2****|****2**

**Substantial Higgsino Component Needed**

- 

- q

- q

- Z

- q

- q

## Indirect Detection: Neutrinos

**Indirect Detection: Neutrinos**

**Hooper and A. Taylor;                             F. Halzen and Hooper (hep-ph/0510048)**

- High Neutrino Rates

## Indirect Detection: Neutrinos

**Indirect Detection: Neutrinos**

**Hooper and A. Taylor;                               F. Halzen and Hooper (hep-ph/0510048)**** **

**Current CDMS Constraint**

## Indirect Detection: Neutrinos

**Future bounds by CDMS will simplify neutrino rate considerably**

**Indirect Detection: Neutrinos**

**Hooper and A. Taylor;                               F. Halzen and Hooper (hep-ph/0510048)**** **

- High Neutrino Rates

**Current CDMS Constraint**

**100 Times Stronger Constraint**

## Indirect Detection: Gamma-Rays

**Indirect Detection: Gamma-Rays**

**Propagate undeflected (point sources possible)**
**Propagate without energy loss (spectral information)**
**Distinctive spectral features (lines), provide potential “smoking gun”**
**Wide range of experimental technology (ACTs, satellite-based)**

_**Disadvantages of Gamma-Rays**_

**Flux depends critically on poorly known inner halo profiles**
**       ******** ****predictions dramatically vary from model to model**
**Unknown astrophysical backgrounds **

## Indirect Detection: Gamma-Rays

**Indirect Detection: Gamma-Rays**

**Likely to be the brightest source of dark matter annihilation radiation **
**Detected in ~TeV gamma-rays by four ACTs:**
**   ****Cangaroo-II, Whipple, HESS and MAGIC **
**Possible evidence for dark matter?**

## Indirect Detection: Gamma-Rays

**Indirect Detection: Gamma-Rays**

**Consistent with WIMP in ~1-4 TeV mass range**
**Roughly consistent with Whipple/Veritas **

**Hooper, Perez, Silk, Ferrer and Sarkar, JCAP, astro-ph/0404205**

## Indirect Detection: Gamma-Rays

**Indirect Detection: Gamma-Rays**

**Consistent with WIMP in ~1-4 TeV mass range**
**Roughly consistent with Whipple/Veritas **

_**The HESS **__**Obsevation**_

**Superior telescope**
**Inconsistent with Cangaroo-II**
**Extends at least to ~10 TeV**
**WIMP of ~10-40 TeV mass needed **

**D. Horns, PLB, astro-ph/0408192**

## Indirect Detection: Gamma-Rays

**Indirect Detection: Gamma-Rays**

**Very heavy neutralinos tend to overclose the Universe**
**Largest annihilation cross sections (lowest relic abundance) are found for Wino-like or Higgsino-like neutralinos**
******h****2****~0.1 for ~1 TeV Higgsino, or ~3 TeV Wino**
**Significantly larger masses are possible only if coannihilations are carefully arranged ****(for example, S. Profumo, hep-ph/0508628)**

## Can A Neutralino Be As Heavy As 10-40 TeV?

**Indirect Detection: Gamma-Rays**

**Electroweak precision observables indicate the presence of a light higgs boson (near the EW scale)**
**Large contributions to the higgs mass come from particle loops:**

**In unbroken SUSY, boson and fermion loops exactly cancel**
** ****If m****SUSY**** >> m****Higgs ****, extreme fine tuning required**
**m****SUSY**** below ~1 TeV is strongly preferred**

## Messenger Sector Dark Matter

**Indirect Detection: Gamma-Rays**

**In Gauge Mediated SUSY Breaking (GMSB) models, SUSY is broken in ~100 TeV sector**
**LSP is a light gravitino (1-10 eV), ****	****	****	****	****poor DM candidate**
**Lightest messenger particle is naturally ****	****	****	****	****stable, multi-TeV scalar****	****neutrino is a ****	****	****	****	****viable dark matter candidate**
**Generated gamma-ray spectrum not ****	****	****	****	****inconsistent with HESS/MAGIC source**

**Dimopolous, Giudice, Pomarol; Han, Hemfling; Han, Marfatia, Zhang; Hooper and  March-Russell, PLB (hep-ph/0412048)**

## Astrophysical Origin of Galactic Center Source?

**Indirect Detection: Gamma-Rays**

**A region rich in extreme astrophysical objects**
**Particle acceleration associated with supermassive black hole?**
**Aharonian and Neronov (astro-ph/0408303), **
**Atoyan and Dermer (astro-ph/0410243)**
**Nearby Supernova Remnant to close **
**to rule out**
**If this source is of an astrophysical**
**nature, it would represent a extremely**
**challenging background for future **
**dark matter searches to overcome **
**(GLAST, AMS, etc.)**

**Hooper, Perez, Silk, Ferrer and Sarkar, JCAP, astro-ph/0404205**

## Dwarf Spheriodal Galaxies

**Indirect Detection: Gamma-Rays**

**Several very high mass-to-light dwarf galaxies in Milky Way**
**(Draco, Sagittarius, etc.)**
**Little is known for certain about the halo profiles of such objects**
**For example, draco mass estimates range from 10****7**** to 10****10**** solar masses**
**       ******** ****broad range of predictions for annihilation rate/gamma-ray flux**
**May provide several very bright sources of dark matter annihilation radiation... or very, very little **
**Detection of Draco by CACTUS experiment??? **
**(Bergstrom, Hooper, hep-ph/0512317; Profumo, Kamionkowski, astro-ph/0601249)**

## Indirect Detection: Gamma-Rays

**Indirect Detection: Gamma-Rays**

_**What Does the Gamma-Ray Spectrum Tell Us?**_
**Most annihilation modes generate very similar spectra**
******+********-**** mode is the most distinctive, although ****	****	****	****        still not identifiable with planned****	****	****	****	****	**** experiments (GLAST, etc.)**
**Neutralino mass and annihilation cross ****	****	****	****	****	****section may be roughly extracted**

## Indirect Detection: Gamma-Rays

**Indirect Detection: Gamma-Rays**

_**What Does the Gamma-Ray Spectrum Tell Us?**_
**At loop level, neutralinos annihilate to ******** and ********Z final states**
**Distinctive spectral line features**
**If bright enough, fraction of neutralino annihilations to lines can be measured**

## Indirect Detection: Gamma-Rays

**Indirect Detection: Gamma-Rays**

_**What Does the Gamma-Ray Spectrum Tell Us?**_
**Chargino-W****+/- ****loop diagrams ****	****	****	****	****	****	****provide largest contributions ****	****	****	****	****	****	****  in most models**
**Cross sections largest for ****	****	****	****	****	****	****higgsino-like (or wino-like)****	****	****	****	****	**** neutralinos**
**Knowledge of squark masses ****	****	****	****	****	****	****makes this correlation more ****	****	****	****	****	****	****powerful **

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

## Indirect Detection: Positrons

**Positron spectrum generated in neutralino annihilations is dominated by local dark matter distribution (within a few kpc)**
**Considerably less uncertainty in the local density than the density of inner halo profiles **
**Cosmic positron measurements can roughly measure the neutralino’s annihilation cross section **
** **

**Indirect Detection: Positrons**

## Indirect Detection: Positrons

** **

**Indirect Detection: Positrons**

**Positrons produced through a range of neutralino annihilation channels:**
**    ****(decays of heavy quarks, heavy leptons, gauge bosons, etc.)**
**Positrons move under influence of galactic magnetic fields**
**Energy losses through inverse compton and synchotron scattering with starlight, CMB**

## Indirect Detection: Positrons

** **

**Indirect Detection: Positrons**

**Determine positron spectrum at Earth by solving diffusion equation:**

**Diffusion Constant**

**Energy Loss Rate**

**Source Term**

**Inputs:  **
**Diffusion constant**
**Energy loss rate**
**Annihilation cross section/modes**
**Halo profile (inhomogeneities?)**
**Boundary conditions**
**Neutralino mass**

## Indirect Detection: Positrons

** **

**Indirect Detection: Positrons**

**The HEAT Excess(?)**
**The HEAT balloon flights have measured an excess in the cosmic positron fraction between 5-30 GeV, although considerable ambiguities exist**
**Neutralinos can generate ****	****	****	****	****	****	****the observed spectral shape,****	****	****	****	****	****	**** but requires an annihilation ****	****	****	****	****	****	****rate a factor of ~50 or more****	****	****	****	**** ****	****	****above the rate expected for ****	****	****	****	****	****	**** a thermal relic and a ****	****	****	****	****	****	****homogeneous dark matter ****	****	****	****	****	****distribution **

## Indirect Detection: Positrons

** **

**Indirect Detection: Positrons**

_**Where does this leave us?**_

**Future cosmic positron experiments hold great promise**
**PAMELA satellite, planned to be launched in 2006**
**AMS-02, planned for deployment **
**onboard the ISS (???)**

## Indirect Detection: Positrons

** **

**Indirect Detection: Positrons**

_**With a “HEAT sized” signal:**_

**Dramatic signal for either PAMELA or AMS-02**
**Clear, easily identifiable signature of dark matter **

**Hooper and J. Silk, PRD (hep-ph/0409104)**

## Indirect Detection: Positrons

** **

**Indirect Detection: Positrons**

_**With a smaller signal:**_

**More difficult for PAMELA or AMS-02**
**Still one of the most promising dark matter search techniques **

**Hooper and J. Silk, PRD (hep-ph/0409104)**

## Indirect Detection: Positrons

** **

**Indirect Detection: Positrons**

** **

**Hooper and J. Silk, PRD (hep-ph/0409104)**

**Value for thermal abundance**

**AMS-02 can detect a thermal   (s-wave) relic up to ~200 GeV, for *****any *****boost factor, and all likely annihilation modes**
**For modest boost factor of ~ 5, AMS-02 can detect dark matter as heavy as ~1 TeV**
**PAMELA, with modest boost factors, can reach masses of ~250 GeV**
**Non-thermal scenarios (AMSB, etc), can be easily tested**

**Prospects for Neutralino Dark Matter:**** **

## Putting It All Together

**Putting It All Together**

**Direct Detection**

**Neutrino Telescopes**

******-Rays + e****+**

## Putting It All Together

**Putting It All Together**

## SUSY Benchmark Models

**SUSY Benchmark Models**

## SUSY Benchmark Models

**SUSY Benchmark Models**

## SUSY Benchmark Models

**SUSY Benchmark Models**

**Squark decay kinematics **

**      ****A/H ******** ********+ ********-**

## SUSY Benchmark Models

**SUSY Benchmark Models**

**Uncertainty In Local Density **

**      ****Atmospheric ******** BG **

**BF < 10**

## Combining LHC With Astrophysics

**Combining LHC With Astrophysics**

**Benchmark model LT1:**
**M****2****=120 GeV, ********=302 GeV, m****A****=352 GeV, tan********=56, 1700 GeV squarks**
**LHC:   m********= 59 ± 10%, m****squark****=1700 ± 10%, tan********=56 ± 15%, m****A****=352 ± 1%**
**Astro:  ************N****=7 10****-8**** x/******** 2, R******** < 10 yr****-1****, ************+********Z ****/ ********tot ****< 10****-5**

## Combining LHC With Astrophysics

**Combining LHC With Astrophysics**

**Benchmark model LT1:**
**M****2****=120 GeV, ********=302 GeV, m****A****=352 GeV, tan********=56, 1700 GeV squarks**
**LHC:   m********= 59 ± 10%, m****squark****=1700 ± 10%, tan********=56 ± 15%, m****A****=352 ± 1%**
**Astro:  ************N****=7****.****10****-8**** x/******** 2, R******** < 10 yr****-1****, ************+********Z ****/ ********tot ****< 10****-5**

**What can be inferred about the lightest neutralino’s composition?**

## Combining LHC With Astrophysics

**Combining LHC With Astrophysics**

**Benchmark model LT1:**
**M****2****=120 GeV, ********=302 GeV, m****A****=352 GeV, tan********=56, ****	****	****1700 GeV squarks**
**LHC:   m********= 59 ± 10%, m****squark****=1700 ± 10%, ****	**** ****	****tan********=56 ± 15%, ****	****	****	****m****A****=352 ± 1%**
**Astro:  ************N****=7****.****10****-8**** x/******** 2, ****	****    ****	****R******** < 10 yr****-1****, ****	****	****    ****	************+********Z ****/ ********tot ****< 10****-5**

- LHC+Relic Density

- Actual Value

- +Astro(CDMS)

## Combining LHC With Astrophysics

**Combining LHC With Astrophysics**

**Benchmark model LT1:**
**M****2****=120 GeV, ********=302 GeV, m****A****=352 GeV, tan********=56, ****	****	****1700 GeV squarks**
**LHC:   m********= 59 ± 10%, m****squark****=1700 ± 10%, ****	**** ****	****tan********=56 ± 15%, ****	****	****	****m****A****=352 ± 1%**
**Astro:  ************N****=7****.****10****-8**** x/******** 2, ****	****    ****	****R******** < 10 yr****-1****, ****	****	****    ****	************+********Z ****/ ********tot ****< 10****-5**

- LHC+Relic Density

- +Astro(CDMS)

## Combining LHC With Astrophysics

**Combining LHC With Astrophysics**

**Benchmark model LT2:**
**M****2****=168 GeV, ********=351 GeV, m****A****=326 GeV, tan********=56, ****	****	****430 GeV squarks**

**Astrophysics adds little information in this case (beyond confirmation)**

## Slide 66

## Slide 67

## Combining LHC With Astrophysics

**Can break coannihilation/funnel/bulk degeneracies**
**Sign of ******** is not determined**
**In heavier SUSY models, LHC will measure few particles, making astrophysical measurements more valuable**

**Combining LHC With Astrophysics**

## Combining LHC With Astrophysics

**Can break coannihilation/funnel/bulk degeneracies**
**Sign of ******** is not determined**
**In heavier SUSY models, LHC will measure few particles, making astrophysical measurements more valuable**

**Combining LHC With Astrophysics**

**In Progress: constraints on tan********, m****A, ****stop/sbottom masses, etc.**

## A Few Caveats

**      ******** ****Perhaps astro can be used to confirm that we are in the MSSM?**
**M****1**** = M****2 ****/ 2   (what is relevant is M****1**** << M****2****)**
**Common sfermion mass scale (role of sleptons may be important)**
**Astrophysical uncertainties (local dark matter density, velocity dist, etc.)**
**No large CP-violating phases in ******** (can reduce direct rates)**
**Nature is supersymmetric (not easily distinguished from UED, little Higgs, etc. by LHC)**

**A Few Caveats**

## A Few Caveats

**      ******** ****Perhaps astro can be used to confirm that we are in the MSSM?**
**M****1**** = M****2 ****/ 2   (what is relevant is M****1**** << M****2****)**
**Common sfermion mass scale (role of sleptons may be important)**
**Astrophysical uncertainties (local dark matter density, velocity dist, etc.)**
**No large CP-violating phases in ******** (can reduce direct rates)**
**Nature is supersymmetric (not easily distinguished from UED, little Higgs, etc. by LHC)**

**A Few Caveats**

**DH, G. Kribs (soon to be in preparation)**

## Summary

**The LHC (or perhaps the Tevatron) are exceedingly likely to discover supersymmetry (****or whatever other new physics is associated with the electroweak scale), but is likely to tell us little about it (squark masses, LSP mass, perhaps some sleptons and heavy neutralinos, but not much else)**
**Astrophysical probes of neutralino dark matter can fill in some of the gaps in our post-LHC understanding of supersymmetry**

**Summary**

## Summary

**Kilometer scale neutrino telescopes (IceCube, KM3) will be capable of detecting mixed gaugino-higgsino neutralinos, or constrain the higgsino fraction**
**Cosmic anti-matter searches will be sensitive to (s-wave annihilating) neutralinos up to hundreds of GeV (PAMELA) or ~1 TeV (AMS-02)**
**Gamma-ray astronomy is improving rapidly, possibly enabling observations of gamma-ray lines; Dwarf spheriodals are among the most promising sources**

**Summary**

## 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!**