1. Search for Gamma Rays from LKP Dark Matter in the UED framework with GLAST a E.Nuss b, J.Cohen-Tanugi c and A.Lionetto d on behalf of GLAST DM & Exotic Physics WG eric.nuss@lpta.in2p3.fr Outlook: 1/ GLAST mission - status 2/ KK Dark Matter with the LAT 3/ Conclusions a http://glast.gsfc.nasa.gov b LPTA Montpellier II University c SLAC – Stanford University d Physics Department & INFN Roma Tor Vergata Preliminary Results

2. GBM correlative observations of transient events Orbit 565 km, circular periode ~95 mns Inclination 28.5 o Lifetime 5 years (min) Launch Date Aug 2007 Launch Vehicle Delta 2920H-10 Launch Site Kennedy Space Center LAT sky coverage 20% of the sky (~2.4 sr) deadtime  as low as 25  s Observing modes All sky survey Pointed observations Re-pointing Capabilities Autonomous Rapid slew speed (75° in < 10 minutes) GLAST and the LAT detector I GBM: ~10 keV - 25 MeV LAT: ~20 MeV - 300 GeV

3. modular pair-conversion telescope : 16 towers surrounded by plastic scintillators Large Area Telescope : Overview (PI: P.Michelson) Silicon Microstrip Tracker ~ 80 m 2 of silicon 8.8 x 10 5 readout channels Strip pitch = 228 µm xy layers interleaved with W converters Total Rad length ~1.5 X 0 Calorimeter Hodoscopic array Array of 1536 CsI(Tl) crystals in 8 layers Total Rad length ~8.5 X 0 Anti-Coincidence Detector 89 scintillator tiles Segmented design 3000 kg, 650 W (allocation) 1.8 m x 1.8 m x 1.0 m 20 MeV – 300 GeV Currently there is no other telescope covering this energy range e+e+ e–e– Silicon Microstrip Tracker Measures  direction  identification Calorimeter Measures  energy Shower imaging Anti-Coincidence Detector Rejects background of charged cosmic rays segmentation removes self-veto effects at high energy 

4. LAT cosmic ray run

5. Candidate Gamma-ray Event in First LAT Flight Tower

6. > All elements of the GLAST mission have completed the fabrication phase and are well into integration. > LAT, GBM, and spacecraft assembly complete by mid 2006. > Delivery of the instruments for observatory integration spring/summer 2006. > Observatory integration and test summer 2006 through summer CY07. Short term activities for the collaboration : > Data Challenge 2 : March->May 2006 > Beam tests at CERN in summer/autumn 2006 GLAST mission status October 2005 : 16 Tower on the LAT November 2005 ACD on the LAT

7. SM in D = 5 with 1 compactified extra-dimension (over S 1 / ℤ 2 with S 1 radius R) Every SM field (bulk field) possess a KK tower 1-loop level computation shows that the LKP is well approximated by the first KK mode of the hypercharge gauge boson B(1) a a Reference papers: Servant, Tait Nucl.Phys.B650:391- 419,2003, Bergstrom et al. Phys.Rev.Lett.94:131301,2005 Kaluza-Klein Dark Matter in (minimal) UED II

8. WMAP results  CDM h 2 = 0.12 ± 0.02 ⇩ ~ 0.5 TeV ≤ m B(1) ≤ ~ 1 TeV (depending on the coannihilation channels) One loop  -chanels are avaible in minimal UED models as through but are out of reach for GLAST due to m B(1) ≥ ~0.5 TeV constraint. Limit from Relic Density

9. B(1) main annihilation channels Unlike the supersymmetric case, charged lepton production is not helicity suppressed and it is the dominant annihilation channel for masses ≤ 0.5 TeV. We assume the branching ratios computed in Servant, Tait (agree with Bergstrom et al) Charged fermion production : Dominant annihilation channel

10. We assume a NFW profile with a boost factor b, centered at Galactic Center The differential  -ray flux from the GC is NB:J(  ) = 0.13 · 10 5 b for  = 10 -5 sr and  tot v ~3 · 10 -26 cm 3 s -1 for 800 GeV KK DM Continuum Gamma Ray Flux

11. Total number of photons per B (1) B (1) annihilation where the sum is over all processes that contribute to primary and secondary gamma rays with B f the corresponding branching ratio. In the following analysis we have considered both the primary and secondary  -ray production Gamma Rays from LKP

12. Hadronization and/or fragmentation of q-qbar final states We include semihadronic decays of  leptons (fairly hard spectrum) Fornengo et al Phys.Rev.D70:103529,2004 ⇩ parametrization of dN  q  /dE for a center of mass energy ~ 1 TeV. We neglect gauge and Higgs bosons final states. Secondary Contribution

13. Flux from Secondary Contribution Different approximations - Tasitsiomi, Olinto Phys.Rev.D66:083006,2002 - DarkSUSY - Fornengo et al Phys.Rev.D70:103529,20 Very good agreement between the two approxiamations (for mSUGRA) our results are for m B(1) = 0.5, 0.8, 1 TeV

14. Total flux contribution from LKP of m B(1) = 0.8 TeV and with a boost factor b = 200 Gamma Ray Flux Contributions

15. Comparison between different spectral shapes primary and secondary contribution mSUGRA and E -2 spectra vs LKP Spectral Shapes

16. > Whole sky 'realistic' simulation (DC2 IRF) > One Year observations, 30 deg radius FOV Galactic Center centered GLAST simulations Dark Matter NFW profile, m B(1) ~ 500 GeV Diffuse background based on GALPROP code (Point source substracted)

17. We simulated a 1 year map of the sky with a NFW profile for a LKP with m B(1) = 500 GeV For E thrs = 5 GeV and  = 0.84 sr (30 deg radius FOV) the total integrated flux leads to 5  significance ⇒ for NFW profile and 500 GeV LKP leads to a boost factor of ~20 is needed to reach the 5 sensitivity Preliminary GLAST Sensitivity

18. >Our (preliminary) computation indicates that, in the energy range E  > 5 GeV, GLAST could detect  -rays from GC via LKP annihilations with moderate boost factors >Connection with ground based Cherenkov arrays (continuum and gamma ray lines) is needed to disantangle KK signal from standard astrophysical signal (~ E -2 spectra) >But this result strongly depends on the background model (need of a precise estimate) >Major conference, first GLAST Symposium, being planned for February 2007 at Stanford. International Organizing Committee formed. > GLAST is planned to be launched in 2007 from the Kennedy Space Center… Conclusions II I Delta 2920 vehicle