1. DARK MATTER: direct and indirect detection
Fiorenza Donato
Dip. Fisica Teorica, Un. Torino & INFN
IFAE, Perugia

2. Neutralino as the CDM candidate
Stable (if R-parity is conserved)
Mass: m~ GeV
Non-relativistic at decoupling  CDM
Neutral & colourless
Weakly interacting (WIMP)
Good relic density h2
mh2=0.1120± bh2= ± (WMAP07-Komatsu et al. ApJS2011) m ~  ~ (WMAP07&BAO&SNIa)

3. Which Supersymmetric Model?
Theoretical and experimental constraints are too faint to outline a model
Minimal Supersymmetric extension of the Standard Model (MSSM) depends on the SYMMETRY BREAKING mechanism:
Gravity mediated  neutralino DM
Gauge mediated  gravitino DM
Anomaly mediated  neutralino, stau sneutrino
The nature and phenomenology of LSP depends on susy breaking and regions of the susy parameter space

4. Effective MSSM scheme (effMSSM)
(Model parameters defined at the EW scale)
Independent parameters:
M1 U(1) gaugino soft breaking term
M2 SU(2) gaugino soft breaking term
μ Higgs mixing mass parameter
tan β ratio of two Higgs v.e.v.’s
mA mass of CP odd neutral Higgs boson
mq soft mass common to all squarks
ml soft mass common to all sleptons
A trilinear parameter
R ≡ M1/M2 (=0.5 in GUT)
Experimental Bounds
- Accelerator (LEP & Tevatron) data on Higgs and supersymmetric particle (negative) searches
b s
- BSμ+ μ-
- am≡(gm-2)/2
Requirements that neutralino is the LSP
No a priori on the relic density h2
Subdominant neutralinos, if detectable, could be very interesting for particle physics (new physics) and cosmology (mixture of candidates)

5. SIGNALS from RELIC WIMPs
Direct searches: elastic scattering of a WIMP off detector nuclei
Measure of the recoil energy
Indirect searches: in CRs
signals due to annihilation of accumulated in the centre of celestial bodies (Earth and Sun)
 neutrino flux
signals due to annihilation in the galactic halo
 neutrinos
 gamma-rays
 antiprotons, positrons, antideuterons
N.B. New particles are searched at colliders
But we cannot say anything about DM candidates!

6. Direct detection rate NT, A, mN: nucleus properties
m: nucleus-neutralino reduced mass
1. r0,c: local (solar neighborhood) CDM density ASTROPHYSICS
f(w): WIMP velocity distribution in the MW halo
2. s elastic cross-section
= min(1, Wch2/(WCDMh2) PARTICLE PHYSICS
3. F(ER) NUCLEAR form factor
(scalar)
nucleon
N. B. Neutrons behave as WIMPS – most insidious background

7. The very DM signature: the annual modulation
Residual rate for single hit events
December
June
0.82 ton year total exposure
@ LN Gran Sasso (INFN)
DAMA/NaI & DAMA/Libra
exp. Reported a positive
evidence for
a modulated signal 8.2s C.L.
Bernabei et al. Eur. Phys. J. C 2010

8. Interpretation of direct detection results with the Torino code in effMSSM
No-channeling
Channeling
Red region: DAMA annual modulation (with astroph. uncert.)
Scatter plot: reference effMSSM (red: WMAP ok)
Shaded blue: effMSSM with hadronic uncertainties

9. CDMS Experiment (Ge) Ahmed at el. PRL 2009; PRL 2011
PRL 2009: 2 and 15.5 keV
(23% bkgd):
Bottino, FD, Fornengo, Scopel PRD 2010
DAMA & CDMS 2 events & theory
compatible GeV neutralino
BUT in PRL 2011: reanalysis
Lower energy threshold
 NO candiate events

10. CoGent Experiment (Ge)
Aalseth et al. PRL 2011
WIMP contribution
incompatible with 90%CL
Null WIMP Hypothesis
________________________________________________________
CRESST Experiment (CaWO4) W. Seidel, IDM 2010
32 events on Oxigen:
“Background estimate of 8.7 ± 1.4 events
not enough to explain 32 signals”

11. Liquid Xenon Set stringent limits Light-yield function: crucial
Xenon100(Aprile et al 2011)
Set stringent limits
Xenon10 (Angle et al. 2011)
Light-yield function: crucial
Near energy threshold

12. Experiments and Models Bottino, Fornengo, Scopel PRD 2011
1 strong effect (Dama)
+ other hints:
A1, A2: DAMA
(B: CDMS 2 events)
C: CoGent D: Cresst
Red (WMAP ok)
& Blue dots: MSSM
Light neutralinos agrees well with Dama & with all other hints
& cosmology & accelerator data

13. The actual situation is of great interest and new results
The direct detection experiments have exciting results
It is difficult to reconcile (strong or weak) WIMP evidences with exclusions from other experiments.
Uncertainties in the halo shape, velcoity distribution function and escape velocities are not sufficient.
(see T. Schwetz arxiv: , Kopp et al.)
Several experimental points need further study and checks.
The actual situation is of great interest and
new results
are expected in the near future:
stay tuned!

14. NEUTRALINO INDIRECT SIGNALS
Annihilation inside celestial bodies:
 at n telescopes as up-going m’s
Annihilation in the galactic halo:
 -rays
- diffuse, monochromatic line, radio 
and g keep directionality
can be detected only if emitted from high c density regions
Charged particles diffuse in the galactic halo
antimatter searched as rare components in cosmic rays (CRs)
ASTROPHYSICS OF COSMIC RAYS!

15. 2-zone Semi-analytic Diffusive Model
Maurin, Donato, Taillet, Salati ApJ 2001; Maurin, Taillet, Donato A&A 2002
Strong & Moskalenko ApJ 1998; Strong, Moskalenko, Ptuskin astro-ph/ (Galprop)
+All the effects included (VA0 & VC0)
+2D semi-analytic
+ Local Bubble for radioactives
- ISM constant
VC constant througout the halo
VA in the disk
Diffusion coefficient K(R)=K0bRd
Convective velocity Vc
Alfven velocity VA
Diffusive halo thickness L
Acceleration spectrum Q(E)=pa
K0, d, Vc, VA, L, (a)
Systematic scan
of parameter space
Evaluation of uncertainties

16. ANTIPROTONS IN COSMIC RAYS Donato, Maurin, Salati, Barrau, Boudoul, Taillet, et al, ApJ 2002 ; ApJ (2001);
BergstrÖm, EdsjÖ, Ullio, ApJ (1999);
Bieber et al. PRL (1999); Moskalenko et al., ApJ (2002); Donato, Maurin, Brun, Delahaye, Salati PRL2009
PCR + HISM
PCR + HeISM p- + X
aCR + HISM
aCR + HeISM
Diffusion
Measured
fluxes
Nuclear cross sections
Diffusion model tested on B/C
Maurin, Taillet, Donato A&A 2002
Putze, Derome, Maurin A&A 2010

17. Antiproton/proton: data, models, exotic tips
Theoretical calculations with the semi-analytical DM,
compatible with stable and radioactive nuclei
Donato, Maurin, Brun, Delahaye, Salati PRL 2009
PROTON flux:
Φ=Aβ-P1R-P2
T<20 GeV: Bess
(Shikaze et al. Astropart. Phys. 2007)
T>20 GeV, our fit (Bess98, BessTeV&AMS):
{24132; 0; 2.84}
NO need for new phenomena (astrophysical / particle physics)

18. Antideuteron Signal-to-Background
Antideuterons in Cosmic Rays
FD, Fornengo, Salati PRD 2000; FD, Fornengo, Maurin PRD 2008
Antideuterons may form by the fusion of an antiproton and an antineutron
Antideuteron Signal-to-Background
MAX
MED
MIN
m=50 GeV
Dashed: MED
m=10
m=100
m=500
Low energy antideuterons have a high discrimination power

19. ANTIDEUTERONS & future experiments
effMSSM neutralino dark matter can be detected by means of next generation space instruments measuring antideuterons in CRs

20. MSSM Inspections with Antideuterons
GAPS ULDB reach
Median propagation
Parameters
Red: dominant neutralinos
Blue: sub-dominant neutralinos

21. Constraints on Dark Matter contribution from positron/electron data
Donato et al. PRL 2009
Example: m=1 TeV, WW
fit improves, but highest points
in E not explained
High boost factor required 
ONLY Secondary positrons
Best fit propagation parameters

22. Effect on antiprotons
The same example: 1 TeV DM
candidate
B=400 largely excluded by
Pamela!
B=40 marginally allowed
Antiprotons are strong constraints to exotic contributions!

23. Conclusions
Direct DM detection experiments have exciting results – some tension
Positive DM results may nicely be interpreted in terms of relic light neutralinos in effMSSM
Indirect DM detection lives as well an intense phase – more standard astrophysics is needed