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Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 1 DARK2007 Sydney, Sept 24 th -28 th, 2007 The Prospects for the Search.

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Presentation on theme: "Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 1 DARK2007 Sydney, Sept 24 th -28 th, 2007 The Prospects for the Search."— Presentation transcript:

1 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 1 DARK2007 Sydney, Sept 24 th -28 th, 2007 The Prospects for the Search for Dark Matter with GLAST Brian L. Winer The Ohio State University LAT Dark Matter and New Physics Working Group

2 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 2 GLAST LAT Collaboration United States l California State University at Sonoma l University of California at Santa Cruz - Santa Cruz Institute of Particle Physics l Goddard Space Flight Center – Laboratory for High Energy Astrophysics l Naval Research Laboratory l The Ohio State University l Stanford University (SLAC and HEPL/Physics) l University of Washington l Washington University, St. Louis France l IN2P3, CEA/Saclay Italy l INFN, ASI Japanese GLAST Collaboration l Hiroshima University l ISAS, RIKEN Swedish GLAST Collaboration l Royal Institute of Technology (KTH) l Stockholm University PI: Peter Michelson PI: Peter Michelson (Stanford & SLAC) ~225 Members (including ~80 Affiliated Scientists, plus 23 Postdocs, and 32 Graduate Students) Cooperation between NASA and DOE, with key international contributions from France, Italy, Japan and Sweden. Managed at Stanford Linear Accelerator Center (SLAC).

3 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 3 GLAST Burst Monitor (GBM) 5 keV - 25 MeV Large Area Telescope (LAT) 20 MeV - 300 GeV GLAST is a NASA/DOE Mission  Launch: Feb-April 2008  Lifetime: 5-years (10-years goal)  Orbit: 565 km, circular  Inclination: 28.5 o  GLAST is the next generation after EGRET… factor > 30 improvement in sensitivity Large effective area, factor > 5 better than EGRET Field of View ~20% of sky, factor 4 greater than EGRET Point Spread function factor > 3 better than EGRET for E>1 GeV. On axis >10 GeV, 68% containment < 0.12 degrees Smaller deadtime.  Minimize rejection of E>10GeV gamma rays due to backscatter into cosmic ray shield  No expendables (EGRET had spark chamber gas) - long mission without degradation (5-10 years)

4 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 4 e+e+ e–e– Calorimeter Particle tracking detectors Conversion foils Anticoincidence shield Basics of a pair conversion telescopes l Basic structure of a pair conversion telescope l Tracker/converter (detection planes + high Z foils): photon conversion and reconstruction of the electron/positron tracks. l Calorimeter: energy measurement. l Anti-coincidence shield (ACD): backgound rejection (cosmic rays flux ~10 4 higher than the gamma flux). l Signature of a gamma event: l No ACD signal l 2 tracks (1 Vertex)* l Calorimeter signal (~Energy)

5 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 5 GLAST Large Area Telescope (LAT) e+e+ e–e–  Tracking detector  16 tungsten foils (12x3%R.L.,4x18%R.L.)  18 pairs of silicon strip arrays  884736 strips (228 micron pitch) Anti-Coincidence Detector  4% R.L.  89 scintillating tiles  efficiency (>0.9997) for MIPs Calorimeter  8.5 radiation lengths  8 layers cesium iodide logs  1536 logs total (1200kg) 1.8 m 1.0 m One of the biggest Silicon Tracking systems ever constructed.

6 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 6

7 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 7 GEANT4 detector simulation High-energy  interacts in LAT Black: Charged particles White: Photons Red: Deposited energy Blue: Reconstructed tracks Yellow: Inferred γ direction Geometry Detail Over 45,000 volumes, and growing! Interaction Physics QED: derived from GEANT3 with extensions to higher and lower energies (alternate models available) Hadronic: based on GEISHA (alternate models available) Propagation Full treatment of multiple scattering Medium-dependent range cut-off Surface-to-surface ray tracing. Includes information from actual LAT tests detailed instrument response dead channels noise etc. Overall Deadtime Effects F. Longo

8 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 8 Expected GLAST-LAT Performance l Angular resolution of better than 1 degree at energies > 1 GeV l Angular resolution of better than 0.2 degree at energies > 10 GeV l Better than 10% energy resolution for 100 MeV through 100 GeV l About 5% around 1 GeV

9 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 9 GLAST Science 0.01 GeV 0.1 GeV 1 GeV 10 GeV 100 GeV 1 TeV Gamma Ray Bursts Unidentified sources Cosmic ray acceleration Active Galactic Nuclei Dark matter Solar flares Pulsars Quantum Gravity ? thanks: N. Omodei

10 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 10

11 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 11 Gammas from lines  For  Line, energy = WIMP mass  For WIMP masses > M Z /2 can also have Z 0 line  Measurement of line branching fractions would constrain particle theory   γ γ time   γ Z0Z0 Branching fractions are in the range 10 -2 - 10 -4

12 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 12 T. A. Porter et al. 30th ICRC, Merida, Mexico - Final rejection power: 1/10 6 - γ efficiency: 0.8 Sreekumar et al. Astrophys.J.494:523-534,1998 Strong et al. Astrophys.J.613:956-961,2004 Black, total; light green, GCR protons; lavender, GCR He; red, GCR electrons; blue, albedo protons; light blue, albedo positrons; green, albedo electrons; and yellow albedo gammas. Background to all photons: charged particles

13 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 13 Galactic diffuse: conventional and optimized GALPROP model l ’conventional’ GALPROP: l calibrated with locally measured electron and proton,helium spectra, as well as synchroton emission l Optimized GALPROP: Strong, Moskalenko, Reimer, ApJ 537, 736, 2000 Strong, Moskalenko, Reimer, ApJ 613, 962-976, 2004 ConventionalOptimized

14 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 14 Dark Matter in the gamma ray sky Galactic center Milky Way halo Milky Way satellites Extragalactic Milky Way Halo simulated by Taylor & Babul (2005) All-sky map of DM gamma ray emission (Baltz 2006) Only dm annihilation radiation shown….

15 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 15 Several Different Search Modes Search Techniqueadvantageschallenges Galactic center Good Statistics Source confusion/Diffuse background Satellites, subhalos Point sources Low background, Good source id Low statistics Milky Way halo Large statistics Galactic diffuse background Extra- galactic Large Statistics Astrophysics, galactic diffuse background Spectral linesNo astrophysical uncertainties, good source id Low statistics

16 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 16 WIMP annihilation: gamma-ray flux

17 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 17 WIMP annihilation: gamma-ray yield 200GeV mass WIMP WIMP pair annihilation gamma spectrum M WIMP Total#  >100MeV>1GeV>10GeV 10 GeV17.312.61.00 100GeV24.522.512.41.0 1TeV31.029.322.412.3 Gamma ray yield per final state bb

18 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 18 Galactic Center l ROI: 1.0 degree GC, E > 1 GeV l 4 years of operation l Simulate Particle-yield (DarkSUSY) l Simulate GLAST response (ObsSim) l Assume background given by conventional/optimized galprop model Check if WIMP + background can be distinguished from background only (using χ2 for simplicity). 1 GeV 10 Gev

19 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 19 Dark Matter From the Galactic Center E. Nuss, A. Lionetto, A. Morselli

20 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 20 Senstivity to lines: where to look

21 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 21 Line 5σ sensitivity Simulated detector response to δ function in energy Average χ (bootstrapped) > 25 10 -9 10 -8 Y. Edmonds, E. Bloom, J. Cohen-Tanugi 5 Years Worth of data

22 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 22 Example: Dark Matter Satellites Optimistic case: 70 counts signal, 43 counts background within 1.5 deg of clump center 55-days GLAST in-orbit counts map (E>1GeV) Galactic Center 30-deg latitude

23 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 23 l Semi-analytic models of halo substructure 1) l Signal, background flux inside the tidal radius l WIMP mass = 100GeV Significance [ σ] No. of satellites Satellites/Subhalos GLAST 1-yr GLAST 5-yrs How many sources at which signficiance ? WIMP mass [GeV] 100 GeV WIMP, 10 σ detection [2.3e.-26 cm -3 s -1 ] P. Wang, L. Wai, E. Bloom Green: optimized Red: conventional 1)Taylor & Babul, MNRAS, 364, 535 (2004) - MNRAS, 364, 515 (2005) -MNRAS, 348, 811 (2004)

24 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 24 Galactic Halo Analysis l Use the large statistics of the full sky. l Remove the Galactic Center (<10 o ) from consideration l Consider a range of Neutralino Masses l Perform a simulaneous fit to both the energy and spatial distribution. l Measure the sensitivity to observing a signal. Mass vs l 1 year of running A. Sander, R. Hughes, B. Winer

25 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 25 Sensitivity for Galactic Halo Analysis cm 3 -s -1 A. Sander, R. Hughes, B. Winer

26 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 26 Acknowledgements l E. Bloom, Y. Edmonds, P. Wang, L. Wai, J. Cohen-Tanugi(SLAC/KIPAC) l I. Moskalenko (Stanford) l A. Morselli, A. Lionetto (INFN Roma/Tor Vergata) l E. Nuss (Montpellier) l R. Hughes, A. Sander, B. Winer (Ohio State) l L. Bergström, J. Edsjö, A. Sellerholm (Stockholm) l A. Moiseev (Goddard)

27 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 27 Summary Launch Early 2008! l GLAST will shed light on the multi-GeV EGRET data. l The GLAST LAT team is pursing complementary searches for signatures of particle dark matter. l These analyses will continue to be optimized over the next 4-6 months prior to launch. l We are looking forward to launch and adding a new piece to the puzzle of dark matter.

28 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 28 l 1st International GLAST symposium, Stanford, USA (Feb 2007) l L. Bergström, J.C., J. Edsjö, A. Sellerholm: Cosmological WIMPs l G. Bertone, T. Bringmann, R. Rando, A. Morselli : Point sources l A. Lionetto: mSUGRA and ED from the Galactic Centre l A. Morselli, A. Lionetto, E. Nuss: Galactic Centre l Y. Edmonds, E. Bloom, J. C., J. Scargle, L. Wai: Line sensitivity l A. Sander, B. Winer, R. Hughes, L. Wai: Halo sensitivity l L. Wai : Overview l P. Wang, E. Bloom, L. Wai: Galactic Satellites l Summary Paper in preparation More Information... http://glast.gsfc.nasa.gov/science/symposium/2007/program.html

29 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 29 BACKUP SLIDES

30 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 30 l Extra Higgs-Doublet, additional symmetry,Z 2 (H o ) (Inert Doublet Model, Barbieri et. al. PRD 74 (2006) ) l one could think the model was designed for GLAST... It wasn’t. Inert Higgs Dark Matter Gustaffson et. al. astro- ph/0703512

31 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 31 Generic WIMP flux γ yield per annihilation l Flux from given source linecontinuum Dark Matter structure Annihilation cross setcion. Constraint by cosmology to ~ 10 -26 cm 2 ISASUGRA

32 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 32 l ”Optimized model”: allow average CR spectrum to deviate from local spectrum l Modify antiprotons and electrons Background to WIMP signal: galactic diffuse (slide from Igor Moskalenko)

33 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 33 Jan Conrad (KTH, Sthlm) La Thuile March 2007 33 Identification of Dark Matter subhalos Molecular cloud Pulsar 30 GeV WIMP 200 GeV WIMP Baltz, Taylor, Wai, astro-ph/0610731 5 yr GLAST, single clump, 1 degree rejected allowed rejected

34 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 34 Jan Conrad (KTH, Sthlm) Scineghe07 June 2007 34 mSUGRA exclusion (Galactic Center) A.Morselli, E. Nuss, A. Lionetto. First Glast Symposium, 2007 Similar ”analysis” as in generic WIMP case 5yr, 3σ discovery trunc. NFW A 0 = 0 Acc. Limits: Baer et al. hep-ph/0405210

35 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 35 tang  = 60 A 0 = 0

36 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 36 Sagittarius

37 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 37 EGRET excess: Disk surface mass density within 0.8 kpc - Allowed density within 0.8 kpc of the disk 57 – 66 M (Sun) /pcsqr from observations -Stars ~ 40 M(Sun)/pc^2 - ISM ~ 13 M(Sun)/pc^2 - DM ~ 4- 16 M(Sun)/pc^2 - de Boer: 29 M(Sun)/pc^2 Bergström et. Al. JCAP05(2006)006

38 Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 38 EGRET excess: anti-protons Bergström et. Al. JCAP05(2006)006 Anti protons from a SUSY model yelding good fit to EGRET data Spread due to uncertainty in propagation

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