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Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 1 Novel Searches for Dark Matter with Neutrino Telescopes.

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Presentation on theme: "Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 1 Novel Searches for Dark Matter with Neutrino Telescopes."— Presentation transcript:

1 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 1 Novel Searches for Dark Matter with Neutrino Telescopes Center for Cosmology and Astroparticle Physics Nov 17-18 th, 2008 Prospects for the Search for Dark Matter with Fermi Brian L. Winer The Ohio State University Fermi LAT Dark Matter and New Physics Working Group

2 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 2

3 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 3 WIMP annihilation: gamma-ray yield 200GeV mass WIMP WIMP pair annihilation gamma spectrum

4 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 4 Dark Matter in the gamma ray sky Milky Way Halo simulated by Taylor & Babul (2005) All-sky map of DM gamma ray emission (Baltz 2006) Only dm annihilation radiation shown…. Galactic center Milky Way halo Milky Way satellites Extragalactic sub haloes/clumps

5 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 5 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

6 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 6 Total GCR protons GCR He GCR electrons albedo protons,pbar albedo positrons albedo electrons albedo gammas. Background to all photons: Charged Particles -Rejection power: ~10 5-6 -γ efficiency: ~0.8

7 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 7 Galactic Center l Advantage: Largest Source of DM Photons l Problems:  Astrophysical Sources  CR Accelarators  High Energy Gamma Sources  Behavior at Fermi Energies?? l Initial Sensitivity Estimation  ROI = 0.5 deg of GC, E > 1 GeV  Truncated NFW Profile.  Simulate Particle-yield (DarkSUSY)  Background:  Astrophysical Sources Subtracted  GALPROP Represents Diffuse Background  Simulate Detector Response. Consider Annihilations: (Done Individually)

8 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 8 Dark Matter From the Galactic Center Simple for Test Statistic. (More sophisticated TS under study) - similar - WW less sensitivity - more sensitive. Current Efforts:  Optimize ROI (Plot)  Understand Source Removal  Need data.  Optimize TS. 5 Years of Sky-Survey

9 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 9 Galactic Halo Analysis l Advantage:  Use the large statistics of the full sky. l Challenge:  Critically Dependent on Diffuse Background l Measure the sensitivity to observing a signal.  ROI = R>10 o or |b|>10 o  NFW Profile.  Diffuse Background:  GALPROP (Conv., Opt.)  Simultaneous Fit to both spatial and energy distributions  Mass vs  1 year of running

10 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 10 Galactic diffuse: conventional and optimized GALPROP model l ’conventional’ GALPROP:  calibrated with locally measured electron and proton,helium spectra, as well as synchrotron emission l Optimized GALPROP: Strong, Moskalenko, Reimer, ApJ 537, 736, 2000 Strong, Moskalenko, Reimer, ApJ 613, 962-976, 2004 ConventionalOptimized

11 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 11 Galactic Diffuse Background: Brem l b

12 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 12 Galactic Diffuse Background: Neutral Pion Decay l b

13 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 13 Galactic Diffuse Background: Inverse Compton l b

14 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 14 Galactic Diffuse Background: Total l b

15 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 15 Galactic Halo Analysis l Advantage:  Use the large statistics of the full sky. l Challenge:  Critically Dependent on Diffuse Background l Measure the sensitivity to observing a signal.  ROI = R>10 o or |b|>10 o  NFW Profile.  Diffuse Background:  GALPROP (Conv., Opt.)  Simultaneous Fit to both spatial and energy distributions  Mass vs  1 year of running

16 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 16 Sensitivity for Galactic Halo Analysis Conventional Diffuse Optimized Diffuse Typical DM Photon Yields (1 year) : 1.5 x 10 4 (100 GeV/c 2 ) 3 x 10 3 (250 GeV/c 2 ) 50 250

17 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 17 Halo Analysis: Mass Resolution Warning: Statistical Uncertainty ONLY…think of this as a “best case/Lower Limit” 250 100 0 Current Efforts:  Work on understanding Diffuse Background.  Optimize ROI  Understand Source Removal  Optimize Fitting.  SYSTEMATICS! SYSTEMATICS ! For cases where we observer a signal at 5, we can determine our mass resolution. Error bars represent the 68% CI

18 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 18 Search for Sub-halos l In CDM Paradigm, expect MW to contain potentially large number of sub-halos. l Sensitivity:  Assumes Taylor&Babul (05) Distribution  Sub-halo with Truncated NFW Profile  M WIMP =100 GeV   Annihilation  Background: Extragalactic, Galactic Diffuse (GALPROP)  Search for M sub >10 6 M O  Test Statistic:.

19 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 19 Significance [ σ] No. of satellites Sub-halos Fermi 1-yr Fermi 5-yrs WIMP mass [GeV] * Astrophy Unc. Green: GALPOP optimized Red: GALPROP conventional Most Sub-Halos are found a high (|b|) galactic latitude. Once found an attempt can be made to extract the DM parameters. Below are the error ellipses for the case on the previous page. 99% CL 90% CL 68% CL

20 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 20 Dwarf Spheroidal Galaxies Sagittarius Dwarf Assumes 5 years of observations. Likelihood TS: Sensitivity Improves by 2-4x l Advantage:  Could be DM Dominated l Disadvantage:  DM Profile? l Initial Sensitivity  GALPROP used for Diffuse  Test Statistic:  Simple:  Recent: Likelihood l If NFW Profile, sens a factor of 10 less. l Other dSph (e.g. Draco) will also be studied.

21 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 21 Line Search Simulated detector response to δ function in energy l Advantage: ”Smoking Gun”  Backgrounds from data l Challenges:  Small BR <10 -3  Energy Resolution. l Initial Sensitivity Estimation  ROI = Broken Annulus  20 o 15 o  DM Den High but reduced background  Scan through energy range  Fit Background to exponential  Signal Fit Double Gaussian  Test Statistic: Example MC Sim. Proposed by Stoehr, et al Some recent models predict enhancements.

22 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 22 Line 5σ sensitivity 5 Years of Fermi Data Current Efforts:  Improved event selection and energy reconstruction.  Optimized ROI  Need data  Measure Diffuse Bkg.  Optimize TS. Trials factor included for unknown source.

23 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 23 Summary l Fermi has many targets for the indirect DM search.  Some are statistics limited.  Some are sys. limited  Other Modes:  Cosmological WIMPS  Extra Dim: KK  HE Electrons l Efforts are on-going to optimize these searches.  Real Data Helps! l The DM Working Group plans an intense effort in the first year of operation.  We are happy finally to be in orbit !

24 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 24 WIMP annihilation: gamma-ray flux

25 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 25 Acknowledgements l E Baltz, B. Berenji, E. Bloom, J. Chiang, Y. Edmonds, G. Godfrey, 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, P. Smith, B. Winer (Ohio State) l L. Bergström, T. Bringmann, J. Conrad, J. Edsjö, A. Sellerholm (Stockholm) l A. Moiseev (Goddard) l G. Bertone (Paris) l R. Johnson(Santa Cruz) l J. Ormes (Denver) l R. Rando (Padova) l A. Strong (Max-Planck) Pre-launch Estimates for GLAST Sensitivity to Dark Matter Annihilation Signals E. A. Baltz, et al JCAP, 07 (2008) 013, arXiv: 0806.2911v2

26 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 26 Parameter Space

27 Brian L. Winer, Ohio State University Fermi Gamma-Ray Space Telescope CCAPP DM Workshop Page 27 Cosmological WIMPS

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