Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, B. Allanach (Cambridge) L. Baudis (Aachen) H.-C. Cheng (UC Davis) S. Y. Choi (Chonbuk) A. Czarnecki (Edmonton) A. Djouadi (Paris) B. Dutta (Texas A&M) J. Ellis (CERN) L. Evans (CERN) D. Hooper (Fermilab) G. Isidori (Frascati) S. Jaeger (Munich) K. Jakob (Freiburg) E. W. Kolb (Chicago) S. Kraml (CERN) M. Mangano (CERN) A. Masiero (Padua) H-P. Nilles (Bonn) K. Olive (Minnesota) S. Raby (Ohio) Q. Shafi (Delaware) M. Spiropulu (CERN) F. Steffen (MPI Munich) J. Wess (Harvard) F. Wilczek (MIT)

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, A SUSY scenario for LHC from Cosmology OUTLINE Determination of the WIMP mass Determination of the WIMP halo Determination of the rotation curve PREDICTIONS for LHC (if SUSY) Ingredients to this analysis gamma spectra for BG + DMA SUSY Particle Physics Cosmology Astrophysics 23%DM, thermal history of WIMPs annihilation cross section Galaxy formation Cosmics Gamma rays Astronomers Rotation curve Doughnut of stars at 14 kpc Doughnut of H 2 at 4 kpc WdB, C. Sander, V. Zhukov, A. Gladyshev, D. Kazakov,EGRET excess of diffuse Galactic Gamma Rays as Tracer of DM, astro-ph/ , A&A, 444 (2005) 51

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, Thermal History of WIMPs Thermal equilibrium abundance Actual abundance T=M/22 Comoving number density x=m/T Jungmann,Kamionkowski, Griest, PR 1995 WMAP ->  h 2 =0.113  > = cm 3 /s DM increases in Galaxies:  1 WIMP/coffee cup  DMA (  ρ 2 ) restarts again.. T>>M: f+f->M+M; M+M->f+f T f+f T=M/22: M decoupled, stable density (when annihilation rate  expansion- rate, i.e.  = n  (x fr )  H(x fr ) !) Annihilation into lighter particles, like quarks and leptons ->  0 ’s -> Gammas! Only assumption in this analysis: WIMP = THERMAL RELIC!

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, Example of DM annihilation (SUSY) Dominant  +   A  b bbar quark pair Sum of diagrams should yield = cm 3 /s to get correct relic density Quark-Fragmentation known! Hence spectra of positrons, gammas and antiprotons known! Relative amount of ,p,e+ known as well.           f f f f f f Z Z W W  00 f ~ AZ ≈37 gammas

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, M  0 =50 GeV M  0 =70 GeV Momentum dependence of contributions to DM annihilation Z-exchange  N 3,4 2 with both s- and p-wave A-exchange  N 1 N 3,4 only s-wave (p-independent) decoupling time (1 ns after BB)

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, Instrumental parameters: Energy range: GeV Energy resolution: ~20% Effective area: 1500 cm 2 Angular resol.: <0.5 0 Data taking: Main results: Catalogue of point sources Excess in diffuse gamma rays EGRET on CGRO (Compton Gamma Ray Observ.) Data publicly available from NASA archive

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, Energy loss times of electrons and nuclei Protons diffuse much faster than energy loss time, so expect SAME shape everywhere. Indeed observed: outer Galaxy can be fitted with same shape as inner Galaxy.  -1 = 1/E dE/dt  univ

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, The EGRET excess of diffuse galactic gamma rays without and with DM annihilation π0π0 π0π0 WIMPS IC Brems IC Brems If normalization free, only relative point-to-point errors of ≤7% important, not absolute normalization error of 15%. Statistical errors negligible. Fit only KNOWN shapes of BG + DMA, i.e. 1 or 2 parameter fit NO GALACTIC models needed. Propagation of gammas straightforward

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, Background + signal describe EGRET data!

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, Analysis of EGRET data in 6 sky directions A: inner Galaxy (l=±30 0, |b|<5 0 ) B: Galactic plane avoiding A C: Outer Galaxy D: low latitude ( ) E: intermediate lat. ( ) F: Galactic poles ( ) A: inner Galaxy B: outer disc C: outer Galaxy D: low latitude E: intermediate lat.F: galactic poles Total  2 for all regions :28/36  Prob.= 0.8 Excess above background > 10σ.

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, Fits for 180 instead of 6 regions 180 regions: 8 0 in longitude  45 bins 4 bins in latitude  0 0 <|b|< <|b|< <|b|< <|b|<90 0  4x45=180 bins  >1400 data points. Reduced  2 ≈1 with 7% errors bulge disk sun R

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, R x y z 2002,Newberg et al. Ibata et al, Crane et al. Yanny et al. 1/r 2 profile and rings determined from inde- pendent directions xy xz Expected Profile v 2  M/r=cons. and  (M/r)/r 2  1/r 2 for const. rotation curve Divergent for r=0? NFW  1/r Isotherm const. Dark Matter distribution Halo profile Observed Profile xy xz Outer Ring Inner Ring bulge totalDM 1/r 2 halo disk Rotation Curve Normalize to solar velocity of 220 km/s

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, N-body simulation from Canis-Major dwarf galaxy prograde retrogradeObserved stars 13 kpc

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, Fig. 2. The calculated HI scaleheight is shown as a function of the galacto- centric radius in the outer region of the Galaxy. Note that neither the oblate nor the prolate-shaped halos are clearly favoured by the data. Gas flaring in the Milky Way used to determine DM halo Kalberla (Univ. Bonn): If one includes ring of DM with mass Msolar flaring perfectly understood

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, Enhancement of inner (outer) ring over 1/r 2 profile 6 (8). Mass in rings 0.3 (3)% of total DM Inner Ring coincides with ring of dust and H 2 -> gravitational potential well! H2H2 4 kpc coincides with ring of neutral hydrogen molecules! H+H->H 2 in presence of dust-> grav. potential well at 4-5 kpc.

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, Physics Questions answered SIMULTANEOUSLY if WIMP = thermal relic Astrophysicists: What is the origin of “GeV excess” of diffuse Galactic Gamma Rays? Astronomers: Why a change of slope in the galactic rotation curve at R 0 ≈ 11 kpc? Why ring of stars at 13 kpc? Why ring of molecular hydrogen at 4 kpc? Cosmologists: How is DM annihilating? A: into quark pairs How is Cold Dark Matter distributed? Particle physicists: Is DM annihilating as expected in Supersymmetry? A: DM substructure A: DM annihilation A: standard profile + substructure A: Cross sections perfectly consistent with mSUGRA for light gauginos, heavy squarks/sleptons

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, Expected SUSY mass spectra in mSUGRA mSUGRA: common masses m 0 and m 1/2 for spin 0 and spin ½ particles

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, Gauge unification perfect with SUSY spectrum from EGRET With SUSY spectrum from EGRET + WMAP data and start values of couplings from final LEP data perfect gauge coupling unification! Update from Amaldi, dB, F ü rstenau, PLB SM SUSY Also b->s  and g-2 agree within 2σ with SUSY spectrum from EGRET NO FREE PARAMETER

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, All SUSY masses allowed by WMAP, if scanned over all tanb and A0 Only large tanb left, if all constraints from Higgs, chargino, g-2 and bsgamma required Parameter scan confirms large tb and large m0 All points have correct relic density EGRET Excl. Chargino Ex:Higgs bsg Excl.: g-2 Excl. EWSB C. Sander, thesis KA

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, Relic density extremely sensitive to tb at large tb. Determining relic density at colliders -> Δtb ≈ 0.1 Sensitivity from fast running of Higgs mass terms: m A 2 =m 1 2 +m 2 2

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23,

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23,

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, Summary Analysis shows intriguing hint that WIMP is thermal relic with expected annihilation into quark pairs 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 FROM GAMMA RAYS. DM becomes visible by gamma rays from fragmentation (30-40 gamma rays of few GeV pro annihilation from π0 decays) Conventional models CANNOT explain above points SIMULTANEOUSLY, especially spectrum of gamma rays in all directions, 1/r 2 profile, shape of rotation curve, ring of stars at 14 kpc and ring of H 2 at 4 kpc, …. Results rather model independent, since only KNOWN spectral shapes of signal and background used, NO model dependent calculations of abs.fluxes. Different models or unknown experimental problems may change boost factor and/or WIMP mass, BUT NOT the distribution in the sky.

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, Summary of summary LHC accelerator ( ): 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 LHC measures WIMP mass GeV, gluino around 500 GeV and squarks and sleptons around or above 1 TeV then PERFECT.

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, Clustering of DM -> boosts annihilation rate Clumps with M min -> dominant contribution -> MANY clumps in given direction -> same boostfactor in all directions Annihilation  SQUARE of DM density Clustersize: ≈ solar system? M min  M סּ ? Steeply falling mass spectrum. Boost factor  / 2  (Berezinski, Dokuchaev,..) From fit: B≈100 for WIMP of 60 GeV

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, 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) More realistic models have anisotropic diffusion. E.g. spiral galaxies have magnetic fields perpendicular to disk-> antiprotons may spiral quickly out of Galaxy. Objections against DMA interpretation 1) Does antiproton rate exclude interpretation of EGRET data? (L.B.)

Wim de Boer, Karlsruhe LHC-D, SUSY/BSM, Bonn, Feb. 23, Antiprotons B/C ratio Preliminary results from GALPROP with isotropic and anisotropic propagation Summary: with anisotropic propagation you can send charged particles whereever you want and still be consistent with B/C and 10 Be/ 9 Be