1. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 1 JOSEP FLIX [IFAE] MAGIC Telescope Prospects for D A R K M A T T E R searches with the Josep Flix for MAGIC Collaboration Institut de Física d’Altes Energies (IFAE) – Barcelona

2. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 2 JOSEP FLIX [IFAE] The Fact is... Embarrassing: baryons (i.e. stars, planets, ourselves...) only account for 5%... Determination of DM nature is one of the biggest challenges by far in present-day fundamental science. The major unresolved question in astrophysics and cosmology nowadays ! >95% if the Composition of the Universe is still unknown 0.095 <  CDM h 2 < 0.131

3. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 3 JOSEP FLIX [IFAE] Good candidates for Cold Dark Matter In Standard Cosmological scenario Cold Dark Matter Cold Dark Matter is favoured (Structure formation) CDM in form of Weakly Interacting Massive Particles WIMPs Neutral Weak interaction Stable Massive NON-BARYONIC! Various proposed particle candidates  for non-baryonic CDM  Theoretically most appealing candidate: SUSY-WIMPs neutralino especially neutralino. Roszkowski hep-ex/0404052 + more in literature! KK-Particles,...

4. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 4 JOSEP FLIX [IFAE] Annihilations taking place in celestial bodies where  ’s have been accumulated. High density regions (  (WIMP density) 2 ) Indirect search for Relic Neutralinos cores of DM halos keep directionallity Search for excess components in cosmic rays (DIFFUSION) 

5. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 5 JOSEP FLIX [IFAE] The MAGIC Telescope I Up-to-date largest Imaging Air Cherenkov Telescope for  -ray astronomy. (17 m mirror dish) - low design energy threshold E  = 30 GeV - fast repositioning t R <30 sec Canary Island La Palma (2200 a.s.l) MAGIC is a successful pioneering telescope for low energy gamma ray astronomy producing first results ( hints for E < 100 GeV  -ray detections ) [ See D. Mazin, N. Tonello and M. López talks ] September 2004: September 2004: Start of regular data-taking

6. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 6 JOSEP FLIX [IFAE]  -rays from Neutralino self-annihilations I = averaged annihilation cross section over the halo velocity distribution.  = angle between pointing direction and center of (sub)halo. Spectra: Sum over all final (f) states, with proper BRs   -yield ph cm -2 s -1 GeV -1 ph cm 3 s -1 GeV -3 sr -1  -lines are loop suppressed Cesarini et al, astro-ph/0305075 m χ =200 GeV

7. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 7 JOSEP FLIX [IFAE]  -rays from Neutralino self-annihilations II Geometry dependence: Geometry dependence: l.o.s integration accounts for neutralino distribution within the halo Given a telescope  PSF, we integrate over the aperture  : ph cm -2 s -1 GeV -1 GeV 2 cm -5 sr GeV 2 cm -5 Normally, in literature is found the Averaged l.o.s integral, as:

8. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 8 JOSEP FLIX [IFAE] Evaluation of fluxes from  annihilations CHOOSE a SUSY scenario MSSM, mSUGRA... Evaluate, m , spectras... Apply relic density constrain  h 2 < WMAP MAX Coannihilations may be important! Model allowed by acc.constrains? SUSY and Higgs searches decay b  s  Muon anomalous magetic moment g  -2 SUSY DM HALO MODELIZATION CHOOSE a TARGET Galactic Center, dSph (i.e. DRACO), Nearby galaxies, Clusters... Model the Dark Matter density Profiles from N-Body simulations or suggested by Obs. Constrains Use observational DATA: DM do not follow light! (e.g. JEANS Formalism) Evaluate the l.o.s Integral (  COSMO ) Within the detector angular acceptance

9. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 9 JOSEP FLIX [IFAE]  SUSY - mSUGRA : Example parameter Scan DarkSUSY+ISAJET WMAP allowed Coannihilations are important! Resonances to Higss Boson A!  SUSY differs by several orders of magnitude MAGIC 5 orders of magnitude Prada, Klypin, Flix - Phys. Rev. Lett 93 (2004) Includes Focus Point, Bulk region... Higgsinos and Gauginos (No Winos) ~10 7 input Models 18% UNPHYS 6% EXCL. BY ACC. 1.6% with  h 2 < 0.127 0.24% with  h 2 in WMAP range Integrated

10. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 10 JOSEP FLIX [IFAE] Galactic Center : Motivations ‘a priori’ - From distance and DM density criteria, the Galactic Center is ‘a priori’ the best candidate place best candidate place for indirect searches for Dark Matter. - Other  -ray sources in the FOV, i.e. SNR Sgr A East -  -rays from GC have several plausible origin scenarios in competition... BUT: - From MAGIC site, the Galactic Center cuminates at 60 degrees. This affects to the E thr  700 GeV [conservative]

11. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 11 JOSEP FLIX [IFAE] Halo modelization - The Galactic Center I Baryonic infall during galaxy formation results in an increase of the central density of Dark Matter. ADIABATIC COMPRESSION EFFECT STANDARD PRESCRIPTION: spherical symmetry haloscircular orbits of infalling particles... Response of Dark Matter to the condensation of baryons was usually calculated using the model of adiabatic contraction, which assumes spherical symmetry halos and circular orbits of infalling particles... Blumenthal et al, 1986 Indeed, we know that halos in hierarchical structure formation scenarios grow via multiple violent mergers and accretion along filaments... and particle orbits in halos are highly eccentric... Baryons role during galaxy formation?

12. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 12 JOSEP FLIX [IFAE] Halo modelization - The Galactic Center II We used detailed models of our Milky Way galaxy and applied modified Adiabatic contraction to model the GC DM distribution. * This prescription gives reasonable accuracy compared to Gnedin et al 2004 analytical approx. from high-resolution simulation (~10%). Detailed mass model of our Galaxy: - extensive data on the solar neighborhood. - motion of stars and HII regions in the outer MW part. - Motion of satellites and globular clusters in our halo... Prada, Klypin, Flix - Phys. Rev. Lett 93 (2004) Klypin, Zhao et al, 2002 The standard adiabatic prescription systematically overpredicts the increase of Dark Matter density in the inner part of halos (  < 0.05r vir )...

13. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 13 JOSEP FLIX [IFAE] Halo modelization - The Galactic Center III Detailed mass model of our Galaxy: Total Mass compressed NFW Total Mass compressed Moore DM Mass compressed NFW DENSITYMASS DM density compressed NFW Baryons density DM density compressed Moore DM density uncompressed NFW Prada, Klypin, Flix - Phys. Rev. Lett 93 (2004) NFW Moore

14. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 14 JOSEP FLIX [IFAE] Halo modelization - The Galactic Center IV Evaluation of average l.o.s Integral (  COSMO ): COMP. NFW UNCOMP. NFW  PSF (MAGIC) 3 orders of magnitude MAGIC  PSF  = 0.1º  = 10 -5 sr  1-order = 0.12º  2-orders = 0.3º  1-order = 0.47º  2-orders >0.5º

15. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 15 JOSEP FLIX [IFAE] DRACO dSph : Motivations - The Milky way is surrounded by a number of small faint companion galaxies. - These dSph are believed to be the most dominated Dark Matter objects. - Interesting places to test present theoretical predictions of DM profiles. - Also they play an important role in theories of structure formation – subhaloes. - Distances and M/L ratios: 16 kpc to 250 kpc + M/L 30-300 DRACO highest M/L dwarf Northern source

16. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 16 JOSEP FLIX [IFAE] Halo modelization - Draco dSph I Different Dark Matter modelizations for DRACO: Tidal effects included in the model Lokas et al. (2005) (NFW+cut-off) [ Wilkinson et al 2004 data ] Ewans et al. (2004) [ Kleyna et al 2002 data ] Low star sample Flix et al., in preparation 2004 Wilkinson 2002 Kleyna

17. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 17 JOSEP FLIX [IFAE] Halo modelization - Draco dSph II Evaluation of average l.o.s Integral (  COSMO ): <1 order of magnitude  PSF  = 0.1º  = 10 -5 sr  1-order = 0.18º  2-orders = 0.39º  1-order = 0.20º  2-orders = 0.41º  1-order = 0.24º  2-orders =0.32º  1-order = 0.17º  2-orders =0.47º Flix et al., in preparation  PSF (MAGIC)

18. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 18 JOSEP FLIX [IFAE] Pros and Cons for MAGIC viable targets ObjectD kpc ZA deg E thr GeV  GeV 2 cm -5  1-order deg Contami- nation? GC(comp)8.560~ 6504.4·10 28.12Yes GC(uncom p) 8.560~ 6501.5·10 25.47 (ext) Yes DRACO8029~ 1507.3·10 23.18 (~ext) No M3177013~ 1102.7·10 23.27 (ext) Yes FLU X Canis Major dSph ZA 60º - No modeled (Tidally stripped) Saggitarius dSph ZA 60º - No modeled (Tidally stripped) ** * * * * VHE Spectra ** VHE Upper Limits ext = extended E thr (0º) ~ 100 GeV [Very conservative] M87 [ Dominik’s talk ]

19. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 19 JOSEP FLIX [IFAE] A summary (comparative) plot – NFW models M87 M 31 DRACO GC uncomp. GC comp. No substructure enhancement  h 2 showed A 0 ≠ 0 (still low sampling) stop coannihilations! SUSY naturalness violated ( M 12 >2 TeV, i.e.  m  ) Flix et al., in preparation E thr (0º) ~ 100 GeV [Very conservative] Sensitivity from latest MAGIC ‘04 Crab data 5  limit curves GC comp. (E thr (0)~ 50 GeV)

20. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 20 JOSEP FLIX [IFAE] Enhancement factors and other scenarios Adiabatic contraction effects (not for dSph) non-constrained SUSY models Wino-like-Neutralinos (1-order mag.) Substructure contribution (>1 & <2-order mag.) Quintassence: Kination regime modify expansion rate  Relic Density higuer allowed (~ 1 to 2-order magnitude) Q-Balls with high lifetime decay after freeze-out of  non-thermal  production higuer allowed (???) other WIMPs? SuperHeavy Dark Matter Kaluza-Klein Particles Leptonic WIMPs (LIMPs)...  -rays All these putative contributions could enhance significantly the  -flux

21. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 21 JOSEP FLIX [IFAE] Towards Dark Matter Observations with MAGIC GC observable from La Palma at zenith >60º High energy threshold (E thr ~O(650 GeV), conservative). Large effective collection area (cut-off determination!) Contamination from other VHE emitters MAGIC observed the GC in September 2004 for ~3 hours under test conditions Galactic Center: Proposal for more observations between April-August 2005 HESS Flux @ 700 GeV  MAGIC 5  in 2h coming soon... MAGIC PRELIMINA RY

22. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 22 JOSEP FLIX [IFAE] Towards Dark Matter Observations with MAGIC DRACO dSph: - DRACO is the most DM dominated dwarf (M/L up to 300). low - Low Zenith angle observations  Nominal (low) Energy Threshold. - No known VHE emitters in the FOV. Clean target - Clean target for Dark Matter observations. - DM modelling of the dwarf + SUSY models  Very Small fluxes compared to GC. - Scenarios with enhancement factors are needed and/or other DM particles ≠ . Proposal for observations between May-June 2005

23. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 23 JOSEP FLIX [IFAE] Summary enhance significantly - Window for scenarios that could enhance significantly the  -flux. weak sources - Conservative  predictions are not that optimistic (targets are weak sources). - Other scenarios which yield  -rays allow higher fluxes. Planned Dark Matter inspired observations with MAGIC for 2005 Near DM clumps – high- latitude GLAST may discover sources compatible to Dark Matter + extended. DARK MATTER spectra hardly distinguisable from other emission mechanisms. VHE (>50 GeV) observations decissive: universal as DM cut-offs must be universal Joint campaigns with GLAST:  Observations of > 1 source

24. XXXXth RENCONTRES de MORIOND – Very High Energy Phenomena in the Universe 24 JOSEP FLIX [IFAE] Where is the sky section?