Summary of indirect detection
of neutralino dark matter
Joakim Edsjö
Stockholm University
[email protected]
Outline
Outline
Will focus on these
in the MSSM!
••
••
WIMPs
WIMPs as
as Dark
Dark Matter
Matter –– Neutralinos
Neutralinos
Indirect
Indirect detection
detection techniques
techniques
•• Current
Current direct
direct detection
detection limits
limits and
and their
their
implications
implications for
for neutrino
neutrino telescopes
telescopes
•• Conclusions
Conclusions
The
The MSSM
MSSM –– general
general
The Lightest Supersymmetric
Particle (LSP)
Usually the neutralino. If
R-parity is conserved, it is stable.
The Neutralino –
˜ 10 = N11 B˜ + N12 W˜ 3 + N13 H˜ 10 + N14 H˜ 20
Gaugino fraction
2
Zg = N11 + N12
2
1. Select MSSM parameters
2. Calculate masses, etc
3. Check accelerator
constraints
4. Calculate relic density
5. 0.05 < Ωχh2 < 0.2 ?
6. Calculate fluxes, rates,...
Calculation done with
www.physto.se/~edsjo/darksusy/
Relic
Relic density
density vs
vs mass
mass and
and composition
composition
The
Theneutralino
neutralinoisiscosmologically
cosmologicallyinteresting
interestingfor
foraawide
wide
range
rangeof
ofmasses
massesand
andcompositions!
compositions!
The
The m
m -Z
-Zgg parameter
parameter space
space
Gauginos
Ωh 2
>1
Ωh 2
<0
.02
5
LE
P
Mixed
Higgsinos
Low sampling
WIMP
WIMP search
search strategies
strategies
••
••
Direct
Directdetection
detection
Indirect
Indirectdetection:
detection:
–– neutrinos
neutrinosfrom
fromthe
theEarth/Sun
Earth/Sun
–– antiprotons
antiprotonsfrom
fromthe
thegalactic
galactichalo
halo
–– positrons
positronsfrom
fromthe
thegalactic
galactichalo
halo
–– antideutrons
antideutronsfrom
fromthe
thegalactic
galactichalo
halo
–– gamma
gammarays
raysfrom
fromthe
thegalactic
galactichalo
halo
–– gamma
gammarays
raysfrom
fromexternal
externalgalaxies/halos
galaxies/halos
–– synchrotron
synchrotronradiation
radiationfrom
fromthe
thegalactic
galacticcenter
center//
galaxy
galaxyclusters
clusters
–– gammas
gammasfrom
fromaround
aroundthe
thesun
sun
–– ......
Pa
on mel
th a &
eir
A
w MS
ay
!
Positrons
Positrons –– example
example spectra
spectra
The HEAT feature at ~7 GeV can be fit better with neutralinos than
without, but...
...the signal strength needs to be boosted, e.g. by clumps,
...and the fit is not perfect
Antiproton
Antiproton signal
signal
Easy to get high fluxes, but...
Pa
on mel
th a &
eir
A
w MS
ay
!
Background + signal
Antiprotons
Antiprotons –– fits
fits to
to Bess
Bess data
data
Background only
No need for, but room for a signal.
Gamma
Gamma lines
lines –– rates
rates in
in GLAST
GLAST
NFW halo profile, ∆Ω ≈ 1 sr
Bergström, Ullio & Buckley, ’97
Gamma
Gamma fluxes
fluxes from
from simulated
simulated halo
halo
Continuous gammas
Gamma lines
N-body simulations from Calcáneo-Roldan and Moore, Phys. Rev. D62 (2000) 23005.
Cosmological
Cosmological gamma
gamma rays
rays
Thermal production
Non-thermal production
Ullio, Bergström, Edsjö & Lacey, astro-ph/0207125
Edelweiss
Edelweiss
June
June 2002
2002
Direct
Direct detection
detection –– current
current limits
limits
Spin-independent scattering
Spin-dependent scattering
Edelweiss
excluded
Direct detection experiments have started exploring the MSSM parameter space!
Limits:
Limits: flux
flux from
from the
the Earth/Sun
Earth/Sun
Edelweiss
excluded
Earth
Edelweiss
excluded
Sun
• Super-K limit from Shantanu Desai’s talk yesterday, converted to full flux with 1 GeV threshold
• Macro limit from Ivan de Mitri’s talk yesterday, converted to a Φµ limit (hard spectrum, 1 GeV threshold)
• Antares expected 3 yrs limits from Susan Cartwright’s talk yesterday (hard, conv. to 1 GeV threshold)
Flux
Flux from
from Earth/Sun
Earth/Sun and
and future
future
direct
direct detection
detection limits
limits
Earth
Future direct
detection exps.
Sun
Future direct
detection exps.
Comparing
Comparing different
different searches
searches
• Take all future searches with expected sensitivities
within the coming 5–10 years.
• Determine which areas in the mχ-Zg parameter
space they can explore.
• Compare!
The
The m
m -Z
-Zgg parameter
parameter space
space
Gauginos
Ωh 2
>1
Ωh 2
<0
.02
5
LE
P
Mixed
Higgsinos
Low sampling
MSSM
MSSM parameter
parameter space
space
Future
Future probed
probed regions
regions II
Direct detection
Earth, km3
Sun, km3
MSSM
MSSM parameter
parameter space
space
Future
Future probed
probed regions
regions IIII
Antiprotons
Z
MSSM
MSSM parameter
parameter space
space
All
All dark
dark matter
matter searches
searches combined
combined
Large
Largeparts
partsof
ofthe
the
parameter
parameterspace
space
can
canbe
beprobed
probedby
by
future
futuresearches.
searches.
Conclusions
Conclusions
•• Many
Manyindirect
indirectsearches
searcheson
onthe
theway,
way,some
somehave
havestarted
startedexploring
exploringthe
the
MSSM
MSSMparameter
parameterspace.
space.
•• Antiprotons:
Antiprotons:easy
easyto
toget
gethigh
highrates
ratesand
andfit
fitthe
thespectrum,
spectrum,but
butno
no
special
specialfeatures
featuresunless
unlessfor
forheavy
heavyWIMPs
WIMPsand
andlarge
largeboost
boostfactors.
factors.
•• Antideutrons:
Antideutrons:The
Thesignal
signalisislow,
low,but
butthere
thereseems
seemsto
tobe
beaawindow
window<<11
GeV
GeVwhere
wherethe
thebackground
backgroundisislow.
low.
•• Positrons:
Positrons:intriguing
intriguingpositron
positronexcess
excessin
inHEAT,
HEAT,Caprice
Capriceand
andMASS
MASS
91
91data.
data.Fits
Fitsare
arebetter
betterwith
withneutralinos
neutralinoswith
withaaboosted
boostedsignal,
signal,but
butthe
the
fits
fitsare
arenot
notperfect.
perfect.
•• Neutrino
Neutrino telescopes:
telescopes:Complementarity
Complementaritywith
withdirect
directsearches
searchesfor
forthe
the
Sun.
Sun.
•• Gamma
Gammalines:
lines:very
verynice
nicefeature,
feature,but
butsignal
signalmodel
modeldependent.
dependent.
Cosmological
Cosmologicalgammas
gammasmay
maybe
bedetectable
detectableby
byGLAST.
GLAST.
•• Spike
Spikeat
atGC:
GC:Signal
Signalcan
canbe
behigh,
high,ififthe
thecusp
cuspisissteep
steepenough
enoughand
andthe
the
black
blackhole
holeformation
formationhistory
historyisisfavourable.
favourable.