Dan Hooper

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Studying Supersymmetry With Dark Matter

• Dan Hooper
• Theoretical Astrophysics Group
• dhooper_at_fnal.gov

Fermilab Wine and Cheese Seminar September 1, 2006
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Dark Matter

• Evidence from a wide range of astrophysical
  observations including rotation curves, CMB,
  lensing, clusters, BBN, SN1a, large scale
  structure

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NASA/Chandra Press Release, August 21, 2006
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Dark Matter

• Evidence from a wide range of astrophysical
  observations including rotation curves, CMB,
  lensing, clusters, BBN, SN1a, large scale
  structure
• Each observes dark matter through its
  gravitational influence
• Still no (reliable) observations of dark matters
  electroweak interactions (or other
  non-gravitational interactions)
• Still no (reliable) indications of dark matters
  particle nature

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The Dark Matter Candidate Zoo
Axions, Neutralinos, Gravitinos, Axinos,
Kaluza-Klein Photons, Kaluza-Klein Neutrinos,
Heavy Fourth Generation Neutrinos, Mirror
Photons, Mirror Nuclei, Stable States in Little
Higgs Theories, WIMPzillas, Cryptons, Sterile
Neutrinos, Sneutrinos, Light Scalars, Q-Balls,
D-Matter, Brane World Dark Matter, Primordial
Black Holes,
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Weakly Interacting Massive Particles (WIMPs)

• As a result of the thermal freeze-out process, a
  relic density of WIMPs is left behind
• ? h2 xF / lt?vgt
• For a particle with a GeV-TeV mass, to obtain a
  thermal abundance equal to the observed dark
  matter density, we need an annihilation cross
  section of lt?vgt pb
• Generic weak interaction yields
• lt?vgt ?2 (100 GeV)-2 pb

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Weakly Interacting Massive Particles (WIMPs)

• As a result of the thermal freeze-out process, a
  relic density of WIMPs is left behind
• ? h2 xF / lt?vgt
• For a particle with a GeV-TeV mass, to obtain a
  thermal abundance equal to the observed dark
  matter density, we need an annihilation cross
  section of lt?vgt pb
• Generic weak interaction yields
• lt?vgt ?2 (100 GeV)-2 pb

Numerical coincidence? Or an indication that
dark matter originates from EW physics?
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Supersymmetry

• Perhaps the most theoretically appealing
  (certainly the most well studied) extension of
  the Standard Model
• Natural solution to hierarchy problem (stabilizes
  quadradic divergences to Higgs mass)
• Restores unification of couplings
• Vital ingredient of string theory
• Naturally provides a compelling candidate for
  dark matter

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Supersymmetric Dark Matter

• R-parity must be introduced in supersymmetry to
  prevent rapid proton decay
• Another consequence of R-parity is that
  superpartners can only be created and destroyed
  in pairs, making the lightest supersymmetric
  particle (LSP) stable
• Possible WIMP candidates from supersymmetry
  include

?
, Z, h, H
4 Neutralinos

3 Sneutrinos
?
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Supersymmetric Dark Matter

• R-parity must be introduced in supersymmetry to
  prevent rapid proton decay
• Another consequence of R-parity is that
  superpartners can only be created and destroyed
  in pairs, making the lightest supersymmetric
  particle (LSP) stable
• Possible WIMP candidates from supersymmetry
  include

?
, Z, h, H
4 Neutralinos

3 Sneutrinos
?
Excluded by direct detection
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Supersymmetry at the Tevatron

• Most promising channel is through
  neutralino-chargino production
• For example
• Currently sensitive to charginos as heavy as 140
  GeV
• Tevatron searches for light squarks and gluinos
  are also very interesting
• For the case of light mA and large tan?, heavy
  MSSM higgs bosons (A/H) may be observable

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Supersymmetry at the LHC

• Squarks and gluinos produced prolifically at the
  LHC
• Subsequent decays result in distinctive
  combinations of leptons, jets and missing energy

T. Plehn, Prospino 2.0

• Squarks and gluinos up to 1 TeV can be discovered
  with 1 of the first year design luminosity
• Ultimately, LHC can probe squarks and gluinos up
  to 3 TeV

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Supersymmetry at the LHC
What Can We Learn About Supersymmetry At The LHC?

• Kinematics of squark/gluino decays can reveal
  masses of squarks, gluinos, sleptons and
  neutralinos involved
• If many superpartners are light (bulk region),
  much of the sparticle spectrum could be
  reconstructed at the LHC

E. Baltz, et al, hep-ph/0602187
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Supersymmetry at the LHC
What Can We Learn About Supersymmetry At The LHC?

• Kinematics of squark/gluino decays can reveal
  masses of squarks, gluinos, sleptons and
  neutralinos involved
• If many superpartners are light (bulk region),
  most/much of the sparticle spectrum could be
  reconstructed at the LHC

But we might not be so lucky!
E. Baltz, et al, hep-ph/0602187
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Supersymmetry at the LHC
What Can We Learn About Supersymmetry At The LHC?

• For moderate and heavy SUSY models, the LHC will
  reveal far fewer superpartners
• It is not at all unlikely that the LHC could
  uncover a spectrum of squarks, gluinos and one
  neutralino
• Other than one mass, this would tell us next to
  nothing about the neutralino sector

E. Baltz, et al, hep-ph/0602187
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Studying Supersymmetry With Neutralino Dark Matter

• Unless several of the neutralinos are light
  enough to be discovered at the LHC, we will learn
  very little about the composition and couplings
  of the lightest neutralino
• Astrophysical dark matter experiments provide
  another way to probe these couplings
• Potentially enable us to constrain/measure
  parameters appearing in the neutralino mass
  matrix ?, M1, M2, tan?

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Astrophysical Probes of Particle Dark Matter

• Direct Detection -Momentum transfer to
  detector through elastic scattering
• Indirect Detection -Observation of
  annihilation products (?, ?, e, p, etc.)

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Direct Detection

• Neutralino-nuclei elastic scattering can occur
  through Higgs and squark exchange diagrams

• Cross section depends on numerous SUSY
  parameters neutralino mass and composition,
  tan?, squark masses and mixings, Higgs masses and
  mixings

SUSY Models
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Direct Detection

• Current Status

Zeplin, Edelweiss
DAMA
CDMS
Supersymmetric Models
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Direct Detection

• Near-Future Prospects

Zeplin, Edelweiss
DAMA
CDMS
Supersymmetric Models
CDMS 2007 Projection
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Direct Detection

• Long-Term Prospects

Zeplin, Edelweiss
DAMA
CDMS
Supersymmetric Models
Super-CDMS, Zeplin-Max
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Direct Detection
But what does direct detection tell us?

• Neutralino is dark matter (?sec
  vs. cosmological time scales)
• 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?, mA and the elastic scattering
  rate

Hooper and A. Taylor, hep-ph/0607086
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Direct Detection And The Tevatron

• Correlation between neutralino composition, tan?,
  mA and the elastic scattering rate (large tan?,
  small mA leads to a large elastic scattering
  rate)
• MSSM Higgs searches at the Tevatron are also most
  sensitive to large tan?, small mA

M. Carena, Hooper and P. Skands, PRL,
hep-ph/0603180
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Direct Detection And The Tevatron
Current CDMS Limit
For a wide range of M2 and ?, much stronger
current limits on tan?, mA from CDMS than from
the Tevatron
M. Carena, Hooper and P. Skands, PRL,
hep-ph/0603180
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Direct Detection And The Tevatron
3? discovery reach, 4 fb-1
Projected 2007 CDMS Limit (assuming no detection)
Limits from CDMS imply heavy, neutral MSSM Higgs
(H/A) are beyond the reach of the Tevatron,
unless the LSP has a very small higgsino fraction
(?gtgtM2)
M. Carena, Hooper and P. Skands, PRL,
hep-ph/0603180
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Direct Detection And The Tevatron
H/A discovery (3?, 4 fb-1) not expected given
current CDMS limit
H/A discovery (3?, 4 fb-1) not expected given
projected 2007 CDMS limits (assuming no
detection)
M. Carena, Hooper and P. Skands, PRL,
hep-ph/0603180
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Indirect Detection With Neutrinos

• Neutralinos elastically scatter with nuclei in
  the Sun, becoming gravitationally bound
• As neutralinos accumulate in the Suns core, they
  annihilate at an increasing rate
• After Gyr, annihilation rate typically reaches
  equilibrium with capture rate, generating a
  potentially observable flux of high-energy
  neutrinos

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Indirect Detection With Neutrinos

• Muon neutrinos from the Sun interacting via
  charged current produce energetic muons
• Kilometer-scale neutrino telescope IceCube
  currently under construction at South Pole

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Indirect Detection With Neutrinos

• Rate observed at IceCube depends primarily on the
  neutralino capture rate in the Sun (the elastic
  scattering cross section)
• The reach of neutrino telescopes is, therefore,
  expected to be tied to that of direct detection
  experiments

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Indirect Detection With Neutrinos

• Important Caveat WIMPs scatter with nuclei in
  the Sun through both spin-independent and
  spin-dependent scattering
• Sensitivity of direct detection to spin-dependent
  scattering is currently very weak

Spin-Dependent
Spin-Independent
F. Halzen and Hooper, PRD, hep-ph/0510048
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Indirect Detection With Neutrinos
What kind of neutralino has large spin-dependent
couplings?
?
Z
q
q
q
q
Always Small
? fH12 - fH22 2
Substantial Higgsino Component Needed
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Indirect Detection With Neutrinos
What kind of neutralino has large spin-dependent
couplings?


High Neutrino Rates
Hooper and A. Taylor, hep-ph/0607086
F. Halzen and Hooper, PRD,
hep-ph/0510048
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Indirect Detection With Neutrinos
Rates complicated by competing scalar and
axial-vector scattering processes
Current CDMS Constraint




Hooper and A. Taylor, hep-ph/0607086
F. Halzen and Hooper, PRD,
hep-ph/0510048
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Indirect Detection With Neutrinos
Rates complicated by competing scalar and
axial-vector scattering processes but becomes
simple with future bounds
Current CDMS Constraint
100 Times Stronger Constraint


High Neutrino Rates


Hooper and A. Taylor, hep-ph/0607086
F. Halzen and Hooper, PRD,
hep-ph/0510048
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Indirect Detection With Gamma-Rays

• Advantages of 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)

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Indirect Detection With 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 rate may be
  roughly extracted

Hooper and A. Taylor, hep-ph/0607086
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Indirect Detection With 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

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Indirect Detection With 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

Hooper and A. Taylor, hep-ph/0607086
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Information From Anti-Matter

• Gamma-ray observations can tell us the fraction
  of neutralino annihilation to various modes (??,
  ?Z), but cannot measure the total cross section
• 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
• Cosmic positron measurements can roughly
  measure the neutralinos total annihilation
  cross section

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Putting It All Together
Direct Detection
Neutrino Telescopes

?-Rays e
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Putting It All Together
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Studying SUSY with the LHC and Astrophysics
Benchmark model IM3 SUSY Inputs M2673 GeV,
?619 GeV, mA397 GeV, tan?51, 2130 GeV
squarks Measured by the LHC m? 236 10,
msquark2130 30, tan?51 15,
mA397 1 (no sleptons, charginos, or
heavy neutralinos) Measured by astrophysical
experiments ??N9.6 10-9 pb x/? 2, R? lt 10
yr-1, ????Z / ?tot lt 10-5

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Studying SUSY with the LHC and Astrophysics
Benchmark model IM3

Actual Value
LHCRelic Density
Astro
Hooper and A. Taylor, hep-ph/0607086
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Studying SUSY with the LHC and Astrophysics
Benchmark model IM1 SUSY Inputs M2551 GeV,
?1318 GeV, mA580 GeV, tan?6.8, 2240 GeV
squarks Measured by the LHC m? 276 10,
msquark2240 30, (no sleptons,
charginos, heavy neutralinos, heavy Higgs
bosons or tan?) Measured by astrophysical
experiments ??N lt 10-10 pb, R? lt 10 yr-1,
????Z / ?tot lt 10-4 to 10-6

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Studying SUSY with the LHC and Astrophysics
Benchmark model IM1

Actual Value
LHCRelic Density
Hooper and A. Taylor, hep-ph/0607086
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Studying SUSY with the LHC and Astrophysics
Benchmark model IM1

Actual Value
LHCRelic Density
Astro
Hooper and A. Taylor, hep-ph/0607086
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Studying SUSY with the LHC and Astrophysics
Benchmark model IM1

Actual Value
LHCRelic Density
Astro
Hooper and A. Taylor, hep-ph/0607086
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Is It SUSY?

• Thus far, we have assumed that the new particles
  seen at the Tevatron/LHC and in dark matter
  experiments are superpartners of SM particles
• Several alternatives to supersymmetry have been
  proposed which may effectively mimic the
  signatures of supersymmetry at the LHC

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Is It SUSY?

• Universal Extra Dimensions (UED)
• All SM particles allowed to travel around extra
  dimension(s) with size TeV-1
• Particles moving around extra dimensions appear
  as heavy versions of SM particles (Kaluza-Klein
  modes)
• The lightest Kaluza-Klein particle can be stable,
  weakly interacting and a suitable candidate for
  dark matter
• Can we distinguish Kaluza-Klein modes from
  superpartners?

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Is It SUSY?

• Discriminating Supersymmetry and UED at the LHC
• Squarks and gluinos or KK quarks and KK
  gluons cascade to combinations of jets,
  leptons and missing energy mass measurements
  possible, but are they sparticles or KK
  states? ? Spin-determination
  crucial

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Is It SUSY?

• Discriminating Supersymmetry and UED at the LHC
• Recent literature on SUSY/UED discrimination
  (see Cheng, Matchev, Schmaltz Datta, Kong,
  Matchev Datta, Kane, Toharia Alves, Eboli,
  Plehn Athanasiou, Lester, Smilie, Webber)
  
• In the case of somewhat heavy masses or
  quasi-degenerate spectra, spin determination
  becomes very challenging/impossible
• The observation of 2nd level KK modes
  would bolster case for UED, but could be
  confused with a Z prime, for example
  

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Is It SUSY?

• Discriminating Supersymmetry and UED with Dark
  Matter
• Kalzua-Klein dark matter (KK photon, B(1))
  annihilates primarily to charged leptons pairs
  (20-25 to each of ee-, ??- and ??-)
• Neutarlino annihilations to light fermions,
  in contrast, are chirality suppressed
  (?v ? mf/m?2)
• This difference can lead to very distinctive
  signatures in indirect dark matter
  experiments

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Is It SUSY?
The Gamma-Ray Annihilation Spectrum
Neutralino annihilations to gauge/Higgs bosons
and heavy quarks produce rather soft gamma-ray
spectrum
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Is It SUSY?
The Gamma-Ray Annihilation Spectrum
Kaluza-Klein dark matter particles produce harder
spectrum due to 20-25 annihilation to tau
pairs, and final state radiation
Total, including ?s and FSR
Quark fragmentation alone (SUSY-like)
Including ?s
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Is It SUSY?
The Cosmic Positron Spectrum
Annihilations to ee- ( and ??-, ??-) generate

distinctive hard spectrum with edge
UED Case
Gauge Bosons, Heavy Quarks
background
(mDM300 GeV, BF5, moderate propagation)
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Is It SUSY?
Pamela
The Cosmic Positron Spectrum Clearly
identifiable by future experiments (Pamela,
AMS-02) for light/moderate masses
UED Case
Gauge Bosons, Heavy Quarks
background
(mDM300 GeV, BF5, moderate propagation)
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Supersymmetry in the ILC Era

• Combined with LHC data, likely able to measure
  much/most/all of the sparticle and Higgs masses
• With such knowledge of the particle spectrum, it
  may become possible to accurately calculate the
  expected relic abundance of neutralinos, and
  compare this to the observed dark matter density

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Supersymmetry in the ILC Era

• Combined with LHC data, likely able to measure
  much/most/all of the sparticle and Higgs masses
• With such knowledge of the particle spectrum, it
  may become possible to accurately calculate the
  expected relic abundance of neutralinos, and
  compare this to the observed dark matter density

? Confirmation that neutralinos make up the dark
matter of our universe!
But what if they dont match?
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Supersymmetry in the ILC Era
What if the calculated abundance doesnt match
astrophysical observations?

• SuperWIMP Scenario neutralinos freeze-out, and
  later decay to gravitinos
• Non-WIMP dark matter generated through
  WIMP-like freeze-out process
• No signal for direct or indirect detection

?
g

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Supersymmetry in the ILC Era
What if the calculated abundance doesnt match
astrophysical observations?

• Relic abundance calculation assumes standard
  cosmological picture
• Non-standard cosmology/expansion history can lead
  to very different relic abundance (see
  Lykken and Barenboim, last week)

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Current Observations
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The ILC Is A Window Into The Early Universe!




Terascale Observations
Current Observations
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Summary

• If (low-scale) supersymmetry exists in nature,
  then the LHC is exceedingly likely to discover
  superpartners
• The sparticle spectrum measured by the LHC will
  be very incomplete unless most of the sparticles
  are very light
• To learn more about the SUSY spectrum with
  colliders, we may have to wait for the ILC

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Summary

• If (low-scale) supersymmetry exists in nature,
  then the LHC is exceedingly likely to discover
  superpartners
• The sparticle spectrum measured by the LHC will
  be very incomplete unless most of the sparticles
  are very light
• To learn more about the SUSY spectrum with
  colliders, we may have to wait for the ILC

(but Im not that patient!)
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Summary

• Direct and indirect detection of dark matter can
  provide additional information on the
  couplings/composition of the lightest neutralino
  and masses of exchanged particles
• In many cases, dark matter measurements can break
  degeneracies between bulk/funnel/coannihilation
  regions of parameter space
• For models in the A-funnel region of
  parameter space, mA can often be determined
  by astrophysical measurements
• Astrophysical probes of neutralino dark
  matter can fill in some of the gaps in our
  post-LHC/pre-ILC understanding of supersymmetry

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DZERO
CMS
ANTA
ZEPLIN
A T L S
RES
H E S
I C E C U B E
CDF
D M S
VERITAS
M A G I C
GLAST
I C E
A
M E L A
P
M S
Lets use all of the tools we have to solve the
puzzles of the terascale!
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