Ingredients to this analysis

Transcription

1 The dark connection between Canis Major, Monoceros Stream, gas flaring, the rotation curve and the EGRET excess From EGRET excess of diffuse Galactic gamma rays Determination of WIMP mass Determination of WIMP halo (= standard halo + DM ring) Ingredients to this analysis Astronomers Rotation curve Tidal streams Gas flaring Confirmation: Rotation curve Canis Major/Monoceros stream Gas flaring PREDICTIONS for LHC (if SUSY) for direct searches for solar neutrinos Astrophysics Cosmology Particle Physics Cosmics Gamma rays 23%DM, thermal history of WIMPs Annihilation cross section Tidal disruption of dwarf Gamma ray spectra for BG + DMA Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

2 How do streams of DM form from tidal disruption of dwarf galaxies? Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

3 The local group of galaxies Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

4 The Milky Way and its 13 satellite galaxies Canis Major Tidal force F G 1/r 3 Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

5 Tidal streams of dark matter from CM and Sgt CM Sun Sgt From David Law, Caltech Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

6 Artistic view of Canis Major Dwarf just below Galactic disc Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

7 N-body simulation from Canis-Major dwarf galaxy Observed stars R=13 kpc,φ=-20 0,ε=0.8 Canis Major (b=-15 0 ) prograde retrograde Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

8 Gas flaring in the Milky Way P M W Kalberla, L Dedes, J Kerp and U Haud, no ring with ring Gas flaring needs EGRET ring with mass of M! Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

9 Do antiproton data exclude interpretation of EGRET data? Bergstrom et al. astro-ph/ , Abstract: we investigate the viability of the model using the DarkSUSY package to compute the gamma-ray and antiproton fluxes. We are able to show that their (=WdB et al) model is excluded by a wide margin from the measured flux of antiprotons. Problem with DarkSUSY (DS): 1) Flux of antiprotons/gamma in DarkSUSY: O(1) from DMA. However, O(10-2 ) from LEP data Reason: DS has diffusion box with isotropic diffusion -> DMA fills up box with high density of antiprotons 2) Priors of DARKSUSY.(and other propagation models as well): a) static galactic magnetic fields are negligible b) gas is smoothly distributed c) propagation in halo and disk are the same ALL priors likely wrong and can change predictions for DM seaches by ORDER OF MAGNITUDE (and still ok with all observations!) Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

10 One propagation model of our Galaxy GALAXY IS BIG STORAGE TANK FOR ANTIPROTONS IN DARKSUSY and GALPROP Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

11 Simple observations of CR in Galaxy B/C=secondary/primary ratio determine grammage, i.e. the amount of material a CR sees along its trajectory.-> Average density needed of 0.2 particles/cm 3. This is factor 5 lower than the disk density. Simple interpretation: particles propagate mainly in halo! Escape time of CR particle about 10 7 years from radioactive clocks (e.g. 10Be has lifetime f Simple interpretation: halo is several kpc thick, else escape to fast Priors: no static magnetic fields diffusion coeff. same in halo and disk gas of disk smoothly distributed, i.e. no gas clouds Priors all wrong and they change propagation drastically. Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

12 Another propagation model including static magnetic fields and gas clouds and anisotropic diffusion it is shown that Galactic cosmic rays can be effectively confined through magnetic reflection by molecular clouds, Integral excess of positrons in bulge because positrons are trapped in magnetic mirrors between gas clouds? Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

13 The van Allen belts are trapped cosmic rays in magnetic mirrors of earth Radiation in inner belt: 25 Sv/yr inside space ship Lethal dose for human: 3 Sv/h Satellites switch of electronics, wenn entering dense radiation areas. Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

14 Comparing radioactive isotopes with positron distribution (Knödlseder et al.) 1809 kev ( 26 Al) 511 kev Problem: expect most low energy positrons to originate from radioactive nuclei with β+ decay. But these are distributed in bulge AND disk. Positrons mostly in bulge. Why??? Unknown positron source only in bulge?? Light DM? Or simply: relativistic positrons escape in disk and annihilate in bulge? Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

15 astro-ph/ NO annihilation in molecular clouds (MC), although 75% of mass in MC. Why? Either volume of MC too small OR MC are magnetic mirrors as postulated by Chandran! Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

16 How to check Chandran model? Following modifications to GALPROP model from Moskalenko & Strong made: 1) Implement DM as source distribution 2) Modify diffusion equation to allow for anisotropic diffusion (Diffusion coeff. is matrix instead of const.) 3) Implement non-equidistant grid for the solution of the diffusion equation to allow finer sampling of disk region (see talk by Iris Gebauer on Thursday) Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

17 Preliminary results from GALPROP with isotropic and anisotropic propagation CHANDRAN model GALPROP model Summary: with anisotropic propagation you can send charged particles whereever you want and still be consistent with B/C and 10 Be/ 9 Be Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

18 Escape time of cosmic rays and grammage (distance x density) B/C determines grammage 10 Be/ 9 Be determines escape time B/C=secondary/prim.determines grammage. In GALPROP by large halo In Chandran: by reflecting magnetic mirrors. 10 Be (t 1/2 = 1.51 Myr) is cosmic Clock: lifetime of cosmics 10 7 yrs. In GALPROP by large halo In CHANDRAN: by long trapping. Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

19 Summary >>10σ EGRET excess shows intriguing hint that: WIMP is thermal relic with expected annihilation into quark pairs DM becomes visible by gamma rays from fragmentation (30-40 gamma rays of few GeV pro annihilation from π 0 decays) Results rather model independent, since only KNOWN spectral shapes of signal and background used, NO model dependent calculations of abs.fluxes. Different shapes or unknown experimental problems may change the gamma ray flux and/or WIMP mass, BUT NOT the distribution in the sky. SPATIAL DISTRIBUTION of annihilation signal is signature for DMA which clearly shows that EGRET excess is tracer of DM by fact that one can construct rotation curve and tidal streams from gamma rays. DM interpretation strongly supported independently by gas flaring Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

20 What about Supersymmetry? Assume msugra 5 parameters: m 0, m 1/2, tanb, A, sign μ Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

21 10-27 Annihilation cross sections in m 0 -m 1/2 plane (μ > 0, A 0 =0) tan=5 tan=50 bb t t bb t t EGRET WMAP neutralinos squarks ττ WW ττ WW For WMAP x-section of <σv> cm 3 /s one needs large tanβ Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

22 EGRET excess interpreted as DM consistent with WMAP, Supergravity and electroweak constraints Stau coannihilation m A resonance Stau LSP Too large boostfactor for EGRET data Charginos, neutralinos and gluinos light h<114 Bulk EGRET WMAP LSP largely Bino DM may be supersymmetric partner of CMB Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

23 Coannihilations vs selfannihilation of DM If it happens that other SUSY particles are around at the freeze-out time, they may coannihilate with DM. E.g. Stau + Neutralino -> tau Chargino + Neutralino -> W Thermal relic σ coanni + σ selfanni = cm 3 /s. If coannihilation dominates, selfannihilation 0 In present universe only selfannihilation, since other SUSY particles decayed, so no coannihilation. If selfannihilation x-section 0, no indirect detection. CONCLUSION: EGRET data strongly prefers regions without strong coannihilation. Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

24 Gauge unification perfect with SUSY spectrum from EGRET SM SUSY Update from Amaldi, db, Fürstenau, PLB NO FREE parameter With SUSY spectrum from EGRET + WMAP data and start values of couplings from final LEP data perfect gauge coupling unification! Also b->sγ and g-2 in agreement with SUSY spectrum from EGRET Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

25 Grand Unified Theories Possible evolution of Universe Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

26 Indirect DM detection from solar neutrinos SUN Celestial bodies collect DM in their cores by their high density. Annihilation can result in flux of HIGH energy neutrinos from sun (from b-decays or from Z-decays). EGRET Neutrinos can be detected by large detectors,like Super-Kamiokande, Amanda, Ice-Cube, Baksan by the charged current interactions with nuclei,which yields muons in the detectors. Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

27 Direct Detection of WIMPs WIMPs elastically scatter off nuclei => nuclear recoils Measure recoil energy spectrum in target χ 0 H,Z χ 0 If SUSY particle spectrum known, elastic scattering X-section can be calculated EGRET? CDMS XENON10 Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,

28 Summary on WIMP searches Indirect detection: (SPACE EXPERIMENTS) intriguing hint for signals from DMA for 60 GeV WIMP from gamma rays Direct detection: (UNDERGROUND OBSERVATORIES) expected to observe signal in near future IF we are not in VOID of clumpy DM halo Direct production:(accelerators (LHC )): cannot produce WIMPs directly (too small cross section), BUT IF WIMPs are Lightest Supersymmetric Particle (LSP) THEN WIMPs observable in DECAY of SUSY particles IF EVERY METHOD measures SAME WIMP mass, then PERFECT. In this case Dark Matter is the supersymmetric partner of the CMB! Wim de Boer, Karlsruhe Pre-SUSY07 Summerschool, Karlsruhe, July 23-25,