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MAGIC Telescope

Prospects for D A R K M A T T E R searches with the. MAGIC Telescope. Josep Flix for MAGIC Collaboration Institut de Física d’Altes Energies (IFAE) – Barcelona. The Fact is. >95% if the Composition of the Universe is still unknown. 0.095 < W CDM h 2 < 0.131.

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MAGIC Telescope

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  1. Prospects for DARK MATTER searches with the MAGIC Telescope Josep Flix for MAGIC Collaboration Institut de Física d’Altes Energies (IFAE) – Barcelona

  2. The Fact is... >95% if the Composition of the Universe is still unknown 0.095 < WCDMh2 < 0.131 The major unresolved question in astrophysics and cosmology nowadays ! 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.

  3. Roszkowski hep-ex/0404052 Good candidates for Cold Dark Matter In Standard Cosmological scenario 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 especially neutralino. + more in literature! KK-Particles, ...

  4. Indirect search for Relic Neutralinos Annihilations taking place in celestial bodies where c’s have been accumulated. High density regions( (WIMP density)2 ) cc Search for excess components in cosmic rays (DIFFUSION) keep directionallity cores of DM halos

  5. 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 tR<30 sec Canary Island La Palma (2200 a.s.l) September 2004: Start of regular data-taking MAGIC is a successful pioneering telescope for low energy gamma ray astronomy producing first results ( hints for E < 100 GeV g-ray detections ) [ See D. Mazin, N. Tonello and M. López talks ]

  6. g-rays from Neutralino self-annihilations I ph cm-2 s-1GeV-1  = angle between pointing direction and center of (sub)halo. Cesarini et al, astro-ph/0305075 ph cm3 s-1 GeV-3 sr-1 <sannv> = averaged annihilation cross section over the halo velocity distribution. Spectra: Sum over all final (f) states, with proper BRs  g-yield mχ=200 GeV g-lines are loop suppressed

  7. g-rays from Neutralino self-annihilations II ph cm-2 s-1GeV-1 GeV2 cm-5 sr Given a telescope qPSF, we integrate over the aperture DW: Geometry dependence: l.o.s integration accounts for neutralino distribution within the halo Normally, in literature is found the Averaged l.o.s integral, as: GeV2 cm-5

  8. DM HALO MODELIZATION SUSY CHOOSE a SUSY scenario MSSM, mSUGRA ... Evaluate <sv>, mc, spectras... Apply relic density constrain Wh2 < WMAPMAX Coannihilations may be important! Model allowed by acc.constrains? SUSY and Higgs searches decay bsg Muon anomalous magetic moment gm-2 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 (FCOSMO) Within the detector angular acceptance Evaluation of fluxes from c annihilations

  9. FSUSY - mSUGRA : Example parameter Scan Prada, Klypin, Flix - Phys. Rev. Lett 93 (2004) DarkSUSY+ISAJET WMAP allowed ~107 input Models 18% UNPHYS 6% EXCL. BY ACC. 1.6% with Wh2 < 0.127 0.24% with Wh2 in WMAP range MAGIC 5 orders of magnitude Coannihilations are important! Resonances to Higss Boson A! Includes Focus Point, Bulk region... Higgsinos and Gauginos (No Winos) FSUSY differs by several orders of magnitude Integrated

  10. Galactic Center : Motivations • From distance and DM density criteria, the Galactic Center is ‘a priori’ the • best candidate place for indirect searches for Dark Matter. BUT: • Other g-ray sources in the FOV, • i.e. SNR Sgr A East • g-rays from GC have several plausible • origin scenarios in competition... • From MAGIC site, the Galactic Center • cuminates at 60 degrees. • This affects to the Ethr 700 GeV[conservative]

  11. Halo modelization - The Galactic Center I Baryons role during galaxy formation? Baryonic infall during galaxy formation results in anincrease of the central density of Dark Matter. ADIABATIC COMPRESSION EFFECT 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... STANDARD PRESCRIPTION: 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

  12. 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%). Prada, Klypin, Flix - Phys. Rev. Lett 93 (2004) The standard adiabatic prescription systematically overpredicts the increase of Dark Matter density in the inner part of halos (< 0.05rvir )... • 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... Klypin, Zhao et al, 2002

  13. Baryons density Total Mass compressed NFW DM density compressed Moore Total Mass compressed Moore DM density compressed NFW DM Mass compressed NFW DM density uncompressed NFW Halo modelization - The Galactic Center III Prada, Klypin, Flix - Phys. Rev. Lett 93 (2004) Detailed mass model of our Galaxy: DENSITY MASS NFW Moore

  14. Halo modelization - The Galactic Center IV Evaluation of average l.o.s Integral (FCOSMO): MAGIC qPSF= 0.1º DW = 10-5 sr qPSF (MAGIC) 3 orders of magnitude COMP. NFW UNCOMP. NFW q1-order = 0.12º q2-orders = 0.3º q1-order = 0.47º q2-orders >0.5º

  15. DRACO highest M/L dwarf DRACO dSph : Motivations • The Milky way is surrounded by a number of smallfaint companion galaxies. Northern source • These dSph are believed to be the most dominated Dark Matter objects. • Distances and M/L ratios: 16 kpc to 250 kpc + M/L 30-300 • Interesting places to test present theoretical predictions of DM profiles. • Also they play an important role in theories of structure formation – subhaloes.

  16. Low star sample Halo modelization - Draco dSph I Different Dark Matter modelizations for DRACO: Flix et al., in preparation Ewans et al. (2004) [ Kleyna et al 2002 data ] Tidal effects included in the model Lokas et al. (2005) (NFW+cut-off) [ Wilkinson et al 2004 data ] 2004 Wilkinson 2002 Kleyna

  17. Halo modelization - Draco dSph II Evaluation of average l.o.s Integral (FCOSMO): Flix et al., in preparation qPSF= 0.1º DW = 10-5 sr qPSF (MAGIC) <1 order of magnitude q1-order = 0.18º q2-orders = 0.39º q1-order = 0.20º q2-orders = 0.41º q1-order = 0.24º q2-orders =0.32º q1-order = 0.17º q2-orders =0.47º

  18. Pros and Cons for MAGIC viable targets Ethr(0º) ~ 100 GeV[Very conservative] FLUX * * ** * [ Dominik’s talk ] M87 Canis Major dSph ZA 60º - No modeled (Tidally stripped) Saggitarius dSph ZA 60º - No modeled (Tidally stripped) * VHE Spectra ** VHE Upper Limits ext = extended

  19. GC comp. (Ethr(0)~ 50 GeV) A summary (comparative) plot – NFW models Flix et al., in preparation  Wh2 showed A0 ≠ 0 (still low sampling) stop coannihilations! SUSY naturalness violated ( M12>2 TeV, i.e.  mc ) M87 M31 DRACO 5s limit curves GC uncomp. GC comp. No substructure enhancement Ethr(0º) ~ 100 GeV [Very conservative] Sensitivity from latest MAGIC ‘04 Crab data

  20. Enhancement factors and other scenarios All these putative contributions could enhance significantly the g-flux 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 <sv> allowed (~ 1 to 2-order magnitude) Q-Balls with high lifetime decay after freeze-out of c non-thermal c production higuer <sv> allowed (???) other WIMPs? g-rays SuperHeavy Dark Matter Kaluza-Klein Particles Leptonic WIMPs (LIMPs) ...

  21. MAGIC PRELIMINARY coming soon... Towards Dark Matter Observations with MAGIC Galactic Center: HESS Flux @ 700 GeV  MAGIC 5s in 2h GC observable from La Palma at zenith >60º High energy threshold (Ethr~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 hoursunder test conditions Proposal for more observations between April-August 2005

  22. Towards Dark Matter Observations with MAGIC DRACO dSph: • DRACO is the most DM dominated dwarf (M/L up to 300). • Low Zenith angle observations  Nominal (low) Energy Threshold. • No known VHE emitters in the FOV. • 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. Joint campaigns with GLAST: GLAST may discover sources compatible to Dark Matter + extended. DARK MATTER spectra hardly distinguisablefrom other emission mechanisms. VHE (>50 GeV) observations decissive: as DM cut-offs must be universal Summary - Conservative c predictions are not that optimistic (targets are weak sources). • Window for scenarios that could enhance significantly the g-flux. - Other scenarios which yield g-rays allow higher fluxes. Planned Dark Matter inspired observations with MAGIC for 2005 Near DM clumps – high-latitude  Observations of > 1 source

  24. Where is the sky section?

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