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Indirect detection of Dark Matter with gamma-rays - status & outlook

Indirect detection of Dark Matter with gamma-rays - status & outlook. Jan Conrad Oskar Klein Centre Stockholm University conrad@fysik.su.se. Intro. g. g. W - /Z/q. c. p 0. g. g. c. g. W + /Z / q. Indirect detection rate = (particle physics part) × (astrophysical part)

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Indirect detection of Dark Matter with gamma-rays - status & outlook

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  1. Indirect detection of Dark Matter with gamma-rays - status & outlook Jan Conrad Oskar Klein Centre Stockholm University conrad@fysik.su.se

  2. Jan Conrad, Stockholm Universitet Intro g g W-/Z/q c p0 g g c g W+/Z /q Indirect detection rate = (particle physics part) × (astrophysical part) PPP APP Will consider generic WIMP, no specific models (except otherwise stated), no axions, for example

  3. Jan Conrad, Stockholm Universitet Signatures I Ullio et al. Phys.Rev.D66:123502,2002 cc ...  p0  gg cc  Z,gg Birkedal et al., Bringmann et al. JHEP 0801:049,2008.

  4. Jan Conrad, Stockholm Universitet What happened since the last IDM? From Johann Cohen-Tanugi IDM 2008 GLAST -talk ”A wealth of exciting science from GLAST very soon!” … not true …. Fermi did allright though ……

  5. Jan Conrad, Stockholm Universitet ... what else happened ? see Lavalle’s talk yesterday + Fermi-LAT, Phys.Rev.Lett.102:181101,2009 PAMELA, Nature 458:607-609,2009 ” leptophilic models” = + PAMELA, Phys.Rev.Lett.102:051101,2009 Bergström et al.,Phys.Rev.Lett.103:031103,2009

  6. Jan Conrad, Stockholm Universitet Signatures II: the come-back kid: IC • Motivated by PAMELA/Fermi light lepton results. • Interaction/backreaction of light lepons on surrounding radiation gives rise to broad-band spectrum – in particular IC  gamma-rays. No time to talk about spatial signatures: see J. Siegal-Gaskins talk Colafrancesco et al, Astron.Astroph.455:21,2006 Profumo & Jeltema, JCAP 0907:020,2009

  7. Jan Conrad, Stockholm Universitet Census of relevant gamma-ray experiments MILAGRO VERITAS AGILE AGIS MAGIC AMS HAWC Fermi CTA HESS future exp. CANGAROO

  8. Gamma-rays: sensitvitiy overview Large FOV Fermi: ACTs: Water Cherenkov ACT/Fermi: angular resolution (0.10) at high energies (WC: ~0.5) CTA/CTA-US 2018 AGIS Jan Conrad, Stockholm Universitet

  9. Jan Conrad, Stockholm Universitet Targets + Fermi publications Fermi-LAT: TeVPA 2009, arXiv:0912.3828  Goodenough & Hooper, arXiv:0910.2998 Dobler et al., arXiv:0910.4583 Fermi-LAT: Astrophys.J.712:147-158,2010 Fermi-LAT: JCAP 1005:025,2010Scott et al.: JCAP 1001:031,2010 Buckley & Hooper, arXiv:1004.1644 Cirelli et. al. arXIv: 0912.0663 Fermi-LAT: JCAP 1004:014,2010 Akorvazian et. al. arXiv:1002.3820 Huetsi et. al. arXiv:1004.2036 Fermi-LAT: Phys.Rev.Lett.104:091302,2010

  10. Jan Conrad, Stockholm Universitet The Galactic Center

  11. Jan Conrad, Stockholm Universitet The GC in >GeV gamma-rays ~ 0.4 deg • H.E.S.S: updated position, energy spectrum and DM constraints (see Daniil Nekrassov’s talk). • Fermi: • LAT 1 FGL J1745.6-2900 consistent with H.E.S.S. source (i.e. Sgr A* and PWN 359.9) • (does not exclude SNR Sgr A east). e.g. J. Cohen-Tanugi (Fermi-LAT), Fermi Symposium 2009

  12. Jan Conrad, Stockholm Universitet Fermi Galactic Centre • Analysis: • Unbinned likelihood • 11 month (front converting) • 7x7 deg ROI • Model • Gal. Diffuse (GALPROP) • Isotropic • Point sources (1 FGL) Residuals under investigation - Galactic diffuse emission? - effective area systematics? - NB: DM seems unlikely e.g. V. Vitale (Fermi-LAT), RICAP 2009

  13. Jan Conrad, Stockholm Universitet Dwarfs, Dark Matter satellites and Galaxy Clusters.

  14. Jan Conrad, Stockholm Universitet Fermi-LAT: Search for Dark Matter satellites See also D. Hoopers talk • Search for DM clumps • Steady • Extended • Non-power-law (DM) • No counterparts. • Fermi –Search • b > 10o • No counterpart • Spatially extended • Spectrum consistent with DM spectrum • Constant emission • Threshold 5σ e.g. P. Wang, TeVPA 2009 No detection in 10 month of data (consistent with expectations)

  15. Jan Conrad, Stockholm Universitet Dwarfs probed in gamma-rays Veritas Fermi H.E.S.S. MAGIC H.E.S.S. in prep.

  16. Analysis details see Viana’s talk. see Wagner’s talk Jan Conrad, Stockholm Universitet

  17. Jan Conrad, Stockholm Universitet Dwarfs MAGIC Draco, Willman HESS Canis M VERITAS Willman HESS Sag (cusped) 10-26 Stacked Fermi dwarf (more robust!) (Doesn’t include Segue See M. Llena -Gardes talk (Friday).

  18. Jan Conrad, Stockholm Universitet Also dwarfs can be used to say something about Leptophilics 10-24 10-25 10-25 Fermi-LAT: Astrophys.J.712:147-158,2010

  19. Jan Conrad, Stockholm Universitet

  20. Jan Conrad, Stockholm Universitet Galactic diffuse emission To some: To us: Diffusion reacceleration convection energy loss spallation decay IC synch Radiation field brems B-field B-field CNO Gas e p p-bar,  π± e± Gas  π0  γγ  π0  γγ DM  Li, B   π± e±

  21. Jan Conrad, Stockholm Universitet Fermi halo emission • Use spatial and spectral features in an multicomponent likelihood fit  work in progress See Andersson, Cuoco, Zaharijas talks 10-24 conservative (no background) caveat.: no e+/e- diffusion Decaying DM exlcuded for all but muonic decays Cirelli et. al. arXIv: 0912.0663

  22. Jan Conrad, Stockholm Universitet Halo: H.E.S.S. • Approach 1: Slightly off- GC center observation (b~2o), with an off source (b ~8o) away from GC. • Approach 2: Drift scan mode • Would be the most sensitive analysis if systematics can be controlled. see Nekrassovs talk uses Aquarius boost factor

  23. Jan Conrad, Stockholm Universitet

  24. Jan Conrad, Stockholm Universitet The Fermi isotropic gamma-ray background • Infer the isotropic gamma-ray emission by multi-component fit. • Consistent with powerlaw (-2.41) • Estimates: • EGB • Cosmic rays • Quasi-isotropic galactic contributions. Fermi-LAT: Phys.Rev.Lett.104:101101,2010

  25. Jan Conrad, Stockholm Universitet Cosmological WIMPs Fermi-LAT: JCAP 1004:014,2010 N.B. Considerable quasi-isotropic contribution from halo substructure is possible. see Zaharijas talk

  26. Jan Conrad, Stockholm Universitet Fermi-LAT: constraints for cosmological WIMPs Only resolved Extrapolated to 1e-6 sol. M

  27. Jan Conrad, Stockholm Universitet Spectral features

  28. Jan Conrad, Stockholm Universitet Fermi line analysis Fermi-LAT: Phys.Rev.Lett.104:091302,2010 • Unbinned profile likelihood with background model from data, signal model is energy dispersion of the LAT. • ROI: b>10 and 20x20 around GC • Sources removed for b > 10. 10-27 T. Ylinen, PhD thesis, Stockholm Non public energy reco

  29. Jan Conrad, Stockholm Universitet Summary of line emission constraints UX1 lines Mambrini, JCAP 0912:005,2009 Gustafsson et al, PRL,99:041301,2007 IDM lines Fermi HESS GC (binned) 100 h MSSM EGRET GC (binned) EGRET: Pullen at al, Phys.Rev.D76:063006,2007 H.E.S.S: Ripken, PhD thesis, Hamburg U.

  30. Jan Conrad, Stockholm Universitet

  31. Jan Conrad, Stockholm Universitet What does it look like next-to-next IDM? Fermi 5 yr combined dwarfs Fermi 5 yr halo, no substructure Grey: indicating diffuse bg range. Fermi 1 yr dwarfs H.E.S.S. 50 h halo, (Aquarius substructure) or Dwarf stacking? 10-27 …. with some work and ideas …. + energy range, event selection (Fermi) + news from othe exps. AMS,LHC(?)

  32. Cherenkov Telescope Array (CTA) 2018 22-24 m 10-12 m ~7m Jan Conrad, Stockholm Universitet

  33. Jan Conrad, Stockholm Universitet What can CTA do - conservatively CTA Sag, NFW, 20 h (based on CTA Design study simulations). NB: 5 σ PRELIMINARY! CTA halo (~100h) (if halo sensitivity improvment comparable to Sag dwarf improvement) Aquarius

  34. Jan Conrad, Stockholm Universitet Lines CTA preliminary (based on HESS type analysis of CTA simulation of the GC)

  35. Jan Conrad, Stockholm Universitet Conclusions & Final remarks. • Who ordered the Galactic Centre? • Strongest constraints to be expected from the halo if systematics can be controlled. Dwarf stacking might be preferable: similar constraints, less systematics? • Keep an eye on Fermi UNIDs. • Fermi is going strong and there are some interesting results in the pipeline. • MAGIC II operational, H.E.S.S II coming up, too. • Pamela/Fermi CR excess: DM origin essentially ruled out by gamma-rays. • For next-to-next IDM: going to cut ”deep” into annihilation cross-section space. • Further down the road: CTA

  36. Jan Conrad, Stockholm Universitet ….. or ….

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