PRESENT AND FUTURE DARK MATTER SEARCHES WITH - PowerPoint Presentation

1. PRESENT AND FUTUREDARK MATTER SEARCHES WITHIMAGING ATMOSPHERIC CHERENKOV TELESCOPESJ-F. GlicensteinIRFU, CEA-Saclay

2. OutlineImaging Atmospheric Cherenkov TelescopesIndirect dark matter searches with IACTResults on the Galactic Halo (H.E.S.S)Dwarf Galaxies: Segue (MAGIC, VERITAS)Galaxy clusters: Fornax (H.E.S.S)Dark matter searches with CTA

3. 3Major Active IACTsH.E.S.S. MAGIC VERITAS

4. High Energy Stereoscopic Systemlocated in Namibia, latitude=-23o, altitude=1800 m4 telescopes, 107 m2 eachcameras 960 PMTFOV= 5otrigger threshold=100GeVinstalled: january 2004installation of 5th telescope in 2011, first light expected 2012mirror: 600m2, 2048 PMT, FOV=3.5o, trigger threshold=20 GeV

5. Major Atmospheric Gamma-ray Imaging Cherenkovlocated in La Palma (Canaries Islands),latitude=+29o, altitude=2225 mmirror: 234 m2camera 534 PMTFOV=3.5otrigger threshold=60 GeVinstalled late 2004installation 2nd telescope in 2009mirror 234m2, 1099 PMT

6. Very Energetic Radiation Imaging Telescope Array Systemorigin: Whipple collaboration (10 m, late 80s)located in Arizona,latitude=+32o, altitude=1275 m4 telescopes, 106 m2 eachcameras 499 PMTFOV=3.5otrigger threshold=100 GeVinstalled in april 2007

7. Gamma- ray~ 10 kmParticleshower~ 1oCherenkov light~ 120 m12 34 brief flash ~3 ns steroscopy: cosmic ray background rejection improved gamma ray reconstructionImaging atmospheric Cherenkov telescopes

8. VHE gamma-ray astronomy: catalog of sourcesMoriond Cosmology 2012Present and future DM searches with IACT 8The VHE gamma-ray sky (November 2011)http://www.mppmu.mpg.de/~rwagner/sources/ ~100 sources (60 galactic)

9. Indirect DM searches with IACTsMoriond Cosmology 2012Present and future DM searches with IACT 9WIMP annihilation flux into g rays observed by an IACT:particle modelfAP: dark halo model Most current particle models: neutralinos (MSSM) U Extra Dimensions (Servant, Tait 2003) boson B leptophilic models (PAMELA excess) decaying dark matter Astrophysical factor:  dense targets Galactic Center nearby dwarf galaxies, globular clusters galaxy clusters (Fornax) dark matter clumps

10. Signal boosts: particle physicsMoriond Cosmology 2012Present and future DM searches with IACT 10FSRIBrelative velocity b Sommerfeld effect:effective low velocity dispersions resonances at:Internal Brehmstrahlungannihilation to W+W-,ff (c heavy higgsino-like)

11. Signal boosts: astrophysicsMoriond Cosmology 2012Present and future DM searches with IACT 11 Boost effect B from unresolved DM clumps estimated with Aquarius simulation (Springel et al 2008) B sensitive the assumed value of Mlim ( Mlim-0.226) B ~ (a few) for point-like searches towards dwarf galaxies B up to 2 order of mag. for extended searches (galaxy clusters)Mlim = 10-6 M ⊙Mlim = 5 10-3 M ⊙Fornax galaxy cluster

12. HESS searches towards the Galactic haloMoriond Cosmology 2012Present and future DM searches with IACT 12 112 hours collected (2004-2008) 1 degree around GC galactic plane (|b| < 0.3o) excluded background estimated by reflected bakground technique

13. H.E.S.S. limits on WIMP annihilation in the Galactic haloMoriond Cosmology 201213Present and future DM searches with IACT Excluded 95% C.L.mSUGRA modelsA.Abramovski et al. (HESS), Phys.Rev.Lett 106, 161301 (2011)

14. Searches towards globular clusters: M15Moriond Cosmology 2012Present and future DM searches with IACT 14UMiDracoM15 (adiabatic compression)MSSM + WMAP constraintsSame (Woods et al) DM halo modellingExcluded (95% CL)HESS limit very small 0.04 pc core low metalicity(“primordial”) not dominated by DMWHIPPLE Woods et al (Whipple) 2008: constraints at the 10-23 level (1.2 hour!) A.Abramovski et al (HESS) ApJ 735 11 (2011): also at 10-23 level (15.2 h) takes into account heating of DM by stars in GC core

15. Dwarf spheroidal galaxiesMoriond Cosmology 2012Present and future DM searches with IACT 15 dark matter dominated mass range: 107-109 M ⊙ observed by IACTs: Sagittarius, Carina, Sculptor, Draco,Willman1, Segue1, Umin, Canis Major, Boötes 1 data on surface brightness,velocity dispersion, globular clusters,colors  galactic structure wellmodeledWalker et al 2007 Belokurov et al 2006

16. Segue 1 dwarf galaxyMoriond Cosmology 201216Present and future DM searches with IACT discovered 2006 in the SEGUE (Sloan) catalog by Belokurov et al. located 23±2 kpc from the Sun located at the intersection of Saggitarius and Orphan stellar streams unclear whether dwarf galaxy or globular cluster only 71 stars resolved. velocity dispersion s=3.7±1.5 km/s M = 5.8 106 M⊙seems dominated by DM, but error on mass ~ 100% log (core radius)MVGCdwarfgalaxies

17. MAGIC observations of Segue1 dwarfMoriond Cosmology 201217Present and future DM searches with IACT single telescope observations (MAGIC1), taken in 2008-2009 ~ 29.5 h good data no evidence for signal Segue 1 dwarf model was modelled as an Einasto profile (Essig et al 2010) analysis in a slightly extended region |a|< 0.14o (DW = 10-5 sr) J(DW) = 1.78 1019 GeV5/cm2 sr Emin = 100 GeV

18. MAGIC searches towards Segue1: MSUGRA exclusionMoriond Cosmology 201218Present and future DM searches with IACT Excluded 95% C.L. 2 s errors on J(DW)(uncertainty on M)J.Aleksic et al. (MAGIC), JCAP 06 035(2011)<sv>min ~ 10-23 cm3s-1( cc t+t-)

19. VERITAS observations of Segue 1 dwarfMoriond Cosmology 201219Present and future DM searches with IACT 48.7 hours obtained in 2010 and 2011 no evidence for signal same Einasto profile than the MAGIC paper analysis in region q < 0.12o J(DW) = 7.7 1018 GeV5/cm2 sr-Emin = 300 GeV-Significance of signal inside q<0.12o: 1.4 s -”contamination” by bright star(h-Leonis) -removed from background evaluationtarget

20. VERITAS searches towards Segue 1: exclusion limitsMoriond Cosmology 201220Present and future DM searches with IACT <sv> min ~ 2 10-24 cm3 s-1(cct+t-) <sv> from thermal modelsExcluded 95% C.L.E.Aliu et al (VERITAS), PRD 85, 062001 (2012)

21. VERITAS searches towards Segue 1: boosts Moriond Cosmology 201221Present and future DM searches with IACT Wino-like neutralino self-annihilation self-annihilation to a 250 GeV particle pair E.Aliu et al (VERITAS), PRD 85, 062001 (2012)Excluded 95% C.L.<sv> from thermal models

22. Searches towards Segue 1: leptophilic modelsMoriond Cosmology 201222Present and future DM searches with IACT A fraction of parameter space excluded by MAGIC @ low energyand VERITAS @ high energyMAGICVERITAS

23. Sagittarius dwarf galaxyMoriond Cosmology 201223Present and future DM searches with IACT old limits recent observations of Sgr stream allows better modellingof Sgr Dwarf (closest dwarf)update on former HESS limitsby Viana et al (AstroparticlePhysics 2012) should be detectable with CTA (Mwimp a few TeV,200 h observation)However, expected signal from msecond pulsars in M54 (background)also detectable at 4-60 s HESSCTA

24. The Fornax galaxy clusterMoriond Cosmology 2012Present and future DM searches with IACT 24distance d=19 Mpccentral galaxy NGC1399 with a passive SMBH (109 M ⊙) total mass ~ 1014 M ⊙ , extends over 1 Mpc (6o) dark matter distribution well studied with X-rays, globular clusters, stars etc 2 approaches in modelling: assume NFW profile with concentration param. from virial mass (RB02) use directly measured profilesSchuberth et al (2009)X raysGC

25. H.E.S.S. observations of the Fornax galaxy clusterMoriond Cosmology 201225Present and future DM searches with IACT 14.5 hours of data obtained in 2005 “minimal energy” of observations: Emin = 260 GeV boost effect expected from substructure  signal in extended regions signal region: q < 0.1o, significance S = 2.3 sq < 0.5o, significance S=1.2sq< 1o, significance S=0.6s

26. HESS limits on Fornax: effect of source extension Moriond Cosmology 2012Present and future DM searches with IACT 26

27. H.E.S.S. results on Fornax: WIMPs exclusionMoriond Cosmology 201227Present and future DM searches with IACT A. Abramovski et al., arXiv1202.5494 (2012), accepted in ApJ.

28. H.E.S.S limits on Fornax: KK modelsMoriond Cosmology 201228Present and future DM searches with IACT

29. HESS results on Fornax: boost factorsMoriond Cosmology 201229Present and future DM searches with IACT Excluded 95% CL

30. The next generation of IACTs: CTA (2015)Moriond Cosmology 201230Present and future DM searches with IACT low energy sectionEthresh ~ 10 GeV4 ø=23 m telescopescore array100 GeV-10 TeV23 ø=12 m telescopeshigh energy section32 ø=5-6 m tel.on 10 km2 area2 arrays: north+south all-sky coverage

31. Sensitivity of CTAMoriond Cosmology 2012Present and future DM searches with IACT 31x 10 flux sensitivity gainenergy range increaseFlux sensitivity for a 50 h observation

32. Dwarf galaxy searches with CTAMoriond Cosmology 201232Present and future DM searches with IACT Low energyHigh energySeveral arrays layout studiedSculptorSegue 1Courtesy A. VianaD.Nieto

33. dwarf galaxies with CTA (2)Moriond Cosmology 201233Present and future DM searches with IACT Boost factorA signal from Willman 1 or Segue 1 may be observable with CTAdepending on boost factor.

34. Galactic plane flux sensitivity (CTA)Moriond Cosmology 2012Present and future DM searches with IACT 34 assume Emin = 50 GeV 500 GeV WIMP annihilating to bb x10 gain in effective area, x2 gain in hadron rejection reaches 10-13 cm-2 s-1 sensitivity, except on new sources ~400 hours total10 hours each bin

35. Searches for clumpsMoriond Cosmology 2012Present and future DM searches with IACT 35HESS sensitivity clumps from ViaLacteaII (Diemand, Kuhlen, Madau, 2008)~104 resolved halos in MW (M>105Msol) 103 random realizations (rotate the observer position @8.5 kpc) 168±44 clumps inside HESS galactic survey

36. Expected <sv> limits with clumps (galactic plane)Moriond Cosmology 2012Present and future DM searches with IACT 36 Missing one order of mag. to reach thermal <sv>P.Brun, E.Moulin,J.Diemand, J-F.G, PRD 83, 015003 (2011)

37. Expected <sv> limits with clumps (1/4 sky)Moriond Cosmology 2012Present and future DM searches with IACT 37P.Brun, E.Moulin,J.Diemand, J-F.G, PRD 83, 015003 (2011) 1/4 survey in ~6 years assume 5 10-13 cm-2s-1 sensitivity (5 hour/bin) number of subhalos: 3907±324 thermal WIMPs region reachable

38. Conclusion Best constraints on <sv> from observation by H.E.S.S of galactic halo Many observations of dwarf galaxies. Most stringent constraints from observation of Segue 1 (Magic & Veritas) The limits have important astrophysical systematics (GC vs dwarf galaxies, modelling) Constraints on DM annihilation in the Fornax cluster (H.E.S.S) competitive with those from dwarf.With planned array CTA, observations of Segue1, Willman1 reach the thermal annihilation region with proper boost Searches for clump with CTA may give detections or provide stringent constraints. Moriond Cosmology 2012Present and future DM searches with IACT 38

39. Back-up slidesMoriond Cosmology 201239Present and future DM searches with IACT

40. Moriond Cosmology 201240Present and future DM searches with IACT

41. Moriond Cosmology 201241Present and future DM searches with IACT

42. Moriond Cosmology 201242Present and future DM searches with IACT

43. HESS searches towards the Galactic haloMoriond Cosmology 201243Present and future DM searches with IACT

44. 44CTA: array designtarget performancesMoriond Cosmology 2012Present and future DM searches with IACT

45. 45Present and future DM searches with IACT Moriond Cosmology 2012Expectations for Galactic plane survey assumes x 2 improvement in hadron rejectionx 2 gain in angular resolution x 10 gain in effective area  overall increase in sensitivity of ~ 9 expect ~ 300 sources in -30 deg≤ l ≤ 30 deg.Funk,Hinton,Hermann,Digel, arXiV0901.1885HESS map of the Gal.plane, total exp ~500 hourssimulated CTA map, flat exposure ~ 5 hours/field