2. DARK MATTER IN THE MILKY WAY ALEXEY GLADYSHEV (JINR, DUBNA & ITEP, MOSCOW) SMALL TRIANGLE MEETING 2005

3. A Gladyshev (JINR & ITEP) Small Triangle 20053 Outlook  Introduction.  Evidence for Dark Matter. Types of Dark Matter. Direct searches for the Dark Matter.  EGRET data: an excess of the diffuse gamma ray flux  Dark matter distribution in the Milky Way. Halo density profile. Halo substructure. The Milky Way rotation curve.  Positrons and antiprotons in the cosmic rays  WMAP and EGRET constraints in Constrained Minimal Supersymmetric Standard Model  Conclusions

4. A Gladyshev (JINR & ITEP) Small Triangle 20054 Basic cosmological parameters  Density parameters – ratios of contributions of different components (matter, radiation, etc.) to the critical density  Consider the Friedmann equation in the most general form (including the cosmological constant)

5. A Gladyshev (JINR & ITEP) Small Triangle 20055 Basic cosmological parameters  Then we can define density parameters corresponding to the matter, radiation, cosmological constant, and even spatial curvature  The Friedmann equation can be rewritten then in the form

6. A Gladyshev (JINR & ITEP) Small Triangle 20056 Basic cosmological parameters  For today (a= a 0, H = H 0 ) it corresponds to the cosmic sum rule In the context of the Friedmann-Robetrson-Walker metric the total fraction of radiation, matter, curvature and cosmological constant densities must add up to unity

7. A Gladyshev (JINR & ITEP) Small Triangle 20057 Basic cosmological parameters  In the year 2000, two CMBR missions, BOOMERANG and MAXIMA confirmed that the Universe’s geometry should be very close to flat.  The BOOMERANG result in 2001 gave  The WMAP data released in February 2003 were consistent with

8. A Gladyshev (JINR & ITEP) Small Triangle 20058 Basic cosmological parameters  The radiation component  R, corresponding to relativistic particles from the density of the cosmic microwave background radiation is which gives  R = 2.4  10 -5 h -2 = 4.8  10 -5. Three massless neutrinos contribute an even smaller amount. Therefore one can safely neglect the contribution of relativistic particles to the total density of the Universe

9. A Gladyshev (JINR & ITEP) Small Triangle 20059 Matter in the Universe  The matter contribution to the total density of the Universe can be independently estimated in different ways  Estimation from the dynamics of clusters. A cluster mass M cl can be defined by consideration of galaxy motion within the cluster and/or by gravitational lensing by a cluster gravitational potential. An estimate of the mass of matter in the Universe would be then L are luminosities of a cluster and of the Universe as a whole.

10. A Gladyshev (JINR & ITEP) Small Triangle 200510 Matter in the Universe  This gives the estimate  Another estimate comes from the baryon fraction in matter  Yet another estimate comes from consideration of cluster abundances

11. A Gladyshev (JINR & ITEP) Small Triangle 200511 WMAP  WMAP mission has provided the first detailed full-sky map of the microwave background radiation in the Universe

12. A Gladyshev (JINR & ITEP) Small Triangle 200512

13. A Gladyshev (JINR & ITEP) Small Triangle 200513 WMAP  Results of WMAP Combination with other cosmic experiments gives

14. A Gladyshev (JINR & ITEP) Small Triangle 200514 Evidence for the Dark Matter  First evidence for the dark matter – motion of galaxies within clusters (F.Zwicky, 1933)  The most direct evidence for the existence of large amount of the dark matter are the flat rotation curves of spiral galaxies (the dependence of the linear velocity of stars on the distance to the galactic center)  Spiral galaxies consist of a rather thin disc and a spherical bulb in the galactic center

15. A Gladyshev (JINR & ITEP) Small Triangle 200515 Evidence for the Dark Matter  From the equality of forces one gets  Assuming spherical distribution of mass in the core one gets inner part outer part Solar system rotation curve

16. A Gladyshev (JINR & ITEP) Small Triangle 200516 Evidence for the Dark Matter  Observation tell us that for large radii r which means linear distribution of mass This points to the existence of the huge amount of dark matter surrounding the visible part of the galaxy Contribution of the dark matter halo alone Contribution of the disc (visible stars) alone

17. A Gladyshev (JINR & ITEP) Small Triangle 200517 Evidence for the Dark Matter  Nowadays, thousands of galactic rotation curves are known, and they all suggest the existence of about ten times more mass in the halos than in the stars of the disc Elliptic galaxies and cluster of galaxies also contain a large amount of the dark matter

18. A Gladyshev (JINR & ITEP) Small Triangle 200518 Evidence for the Dark Matter  The Milky Way rotation curve has been measured and confirms the usual picture  Measurements of velocities of Magellanic Clouds tells that the Milky Way has very large and massive halo  VIRGOHI21 object – a galaxy, consisting only of dark matter

19. A Gladyshev (JINR & ITEP) Small Triangle 200519 Matter content of the Universe  The matter content of the Universe is determined by the mass density parameter  M. the possible contributions are The luminous baryonic matter (stars in galaxies) The dark baryonic matter (MAssive Compact Halo Objects - MACHOs ? ) The hot dark matter (massive neutrinos ? ) The cold dark matter (Weakly Interacting Massive Particles - WIMPs - neutralinos ? )

20. A Gladyshev (JINR & ITEP) Small Triangle 200520 Matter content of the Universe  All the luminous matter in the Universe from galaxies, clusters of galaxies, etc. is and is very far from the critical density  Deuterium from the primordial nucleosynthesis provides a good test for the matter density (Large density - Fast interactions - Lower abundance) Observation of primordial deuterium abundance gives  Thus, besides luminous matter there exist invisible baryonic matter, with a mass more than ten times larger.

21. A Gladyshev (JINR & ITEP) Small Triangle 200521 Dark Matter candidates  Baryonic Dark Matter (MACHOs – MAssive Compact Halo Objects)  Normal stars No, since they would be luminous  Hot gas No, since it would shine  Burnt-out stellar remnants seems implausible, since they would arise from a population of normal stars of which there is no trace in the halo  Neutron stars No, since they would arise from supernova explosions and thus eject heavy elements into the galaxy

22. A Gladyshev (JINR & ITEP) Small Triangle 200522 Dark Matter candidates  Baryonic Dark Matter (MACHOs – MAssive Compact Halo Objects)  White dwarfs (stars with a mass which is not enough to reach the supernova phase): possible, since white dwarfs are known to exist and to be plentiful. Maybe they could be plentiful enough to explain the Dark Matter if young galaxies that produced white dwarfs cool more rapidly than present theory predicts. But the production of large numbers of white dwarfs implies the production of a large amount of helium, which is not observed

23. A Gladyshev (JINR & ITEP) Small Triangle 200523 Dark Matter candidates  Baryonic Dark Matter (MACHOs – MAssive Compact Halo Objects)  Brown dwarfs (stars ten times lighter than the Sun) possible Astronomers have found some objects that are either brown dwarf stars or very large planets. However, there is no evidence that brown dwarfs are anywhere near as abundant as they would have to be to account for the Dark Matter in our galaxy

24. A Gladyshev (JINR & ITEP) Small Triangle 200524 Dark Matter candidates  Non-baryonic “hot” dark matter  Massive neutrinos Today we have a convincing evidence of neutrino oscillations. This means that neutrinos have a mass. The measurable quantity – mass- squared difference. If neutrino mass is as large as, their contribution to the total density of the Universe is comparable to the contribution of the luminous baryonic matter!

25. A Gladyshev (JINR & ITEP) Small Triangle 200525 Dark Matter candidates  Non-baryonic “cold” dark matter The most reasonable explanation – weakly interacting massive particles (WIMP’s) WIMP’s could have been produced in the Big Bang origin of the Universe in the right amounts and with the right properties to explain the Dark Matter BUT: we do not know WHAT the WIMP IS

26. A Gladyshev (JINR & ITEP) Small Triangle 200526 Direct searches for the Dark Matter  Optical observations from the Earth (EROS, MACHO, … )  Underground searches (DAMA, EDELWEISS, CDMS, … )  Underwater searches (ANTARES, … )  Searches in space (AMS, … )

27. A Gladyshev (JINR & ITEP) Small Triangle 200527 Direct searches for the Dark Matter  MACHO experiment (MAssive Compact Halo Object)  Location - Mount Stromlo Observatory, Canberra, Australia  Main goal - search for objects like brown dwarfs or planets (Massive Compact Halo Objects - MACHOs)  Signature - occasional amplification of the light by the gravitational lens effect

28. A Gladyshev (JINR & ITEP) Small Triangle 200528 Direct searches for the Dark Matter  The effect is large and easily detectable: the amplification could be as large as 0.75m  The phenomenon has a very symmetric light curve, characterized by only 3 parameters (brightness in the maximum, time and duration of the light amplification)  The amplification is the same for all wavelenghts  For the particular star the effect can take place only once

29. A Gladyshev (JINR & ITEP) Small Triangle 200529 Direct searches for the Dark Matter  Different collaborations have seen the signal (1993-1996) OGLE 18 candidates in the direction to the galactic centre MACHO 120 DUO 10 Gravitional lens effect has been detected also in the direction to the Large Magellanic Cloud MACHO 8 EROS 2 The most probable mass of the lens However, MACHOs can only account for less than ~ 50 % of the halo

30. A Gladyshev (JINR & ITEP) Small Triangle 200530 Direct searches for the Dark Matter  DAMA experiment (DArk MAtter)  Location - Gran Sasso National Laboratory of I.N.F.N.  Main goal - search for dark matter particles: WIMPs  Main process – WIMP elastic scattering on the target nuclei  Measured quantity - nuclear recoil energy in the keV range

31. A Gladyshev (JINR & ITEP) Small Triangle 200531 Direct searches for the Dark Matter  Positive evidence for a WIMP signal could arise from the kinematics of the Earth withing non-rotating WIMP halo. The sun is orbiting about the galactic centre with a velocity of ~ 220 km/s. The Earth is orbiting about the Sun with a velocity of ~ 30 km/s.  The resulting relative Earth-halo velocity is modulated, thus the WIMP flux is also modulated which should lead to the modulation of the count rate.

32. A Gladyshev (JINR & ITEP) Small Triangle 200532 Direct searches for the Dark Matter  DAMA group claim they do observe the modulation of their count rate (results of 4 years running - 57986 kg  d)

33. A Gladyshev (JINR & ITEP) Small Triangle 200533 Direct searches for the Dark Matter  This result is compatible with a signal from WIMPs with a mass and a WIMP-nucleon cross section of

34. A Gladyshev (JINR & ITEP) Small Triangle 200534 Direct searches for the Dark Matter  Severe criticism has arisen in the community, ascribing the observed annual modulation rater to systematics than to a WIMP signature. DAMA insists on their model-independent analysis:  presence of annual modulation with the proper features;  neither systematics nor side reactions able to mimic the signature

35. A Gladyshev (JINR & ITEP) Small Triangle 200535 Direct searches for the Dark Matter  1 st data taking: Fall 2000 2 nd data taking: 1 st semester 2002 3 rd data taking :October 2002 - March 2003  EDELWEISS new limits  DAMA best fit exclusion at > 99.8 % C.L confirmed with 3 new detectors and extended exposure  Exclusion limits are astrophysical model independent

36. A Gladyshev (JINR & ITEP) Small Triangle 200536 Direct searches for the Dark Matter  EDELWEISS II  New run started : improved energy threshold  Expect further factor > 2 in exposure with improved sensitivity  September 2003 : EDELWEISS I stops and EDELWEISS II installation begins with 21×320g Ge  Sensitivity will be improved by a factor of 100

37. A Gladyshev (JINR & ITEP) Small Triangle 200537 Searches for the Dark Matter  AMS-02 experiment (AntiMatter in Space)  Location - International Space Station (Hopes it’ll be launched in 2007, scheduled to be launched 15 Oct 2005, planned 4 Sep 2003)  Main Goal - search for dark matter, missing matter & antimatter in space

38. Indirect searches for the Dark Matter

39. A Gladyshev (JINR & ITEP) Small Triangle 200539 EGRET Excess  EGRET Data on diffuse Gamma Rays show excess in all sky directions with the same energy spectrum from monoenergetic quarks  9 yrs of data taken (1991-2000)  Main purpose: sky map of point sources above diffuse background.

40. A Gladyshev (JINR & ITEP) Small Triangle 200540 EGRET Excess A: Inner Galaxy (l=±30 0, |b|<5 0 ) B: Galactic plane avoiding A (30-330 0 ) C: Outer Galaxy (90-270 0 ) D: Low latitude (10-20 0 ) E: Intermediate lat. (20-60 0 ) F: Galactic poles (60-90 0 ) Excess has the same shape implying the same source everywhere in the galaxy

41. A Gladyshev (JINR & ITEP) Small Triangle 200541 EGRET Excess A: Inner Galaxy (l=±30 0, |b|<5 0 ) B: Galactic plane avoiding A (30-330 0 ) C: Outer Galaxy (90-270 0 ) D: Low latitude (10-20 0 ) E: Intermediate lat. (20-60 0 ) F: Galactic poles (60-90 0 ) Excess has the same shape implying the same source everywhere in the galaxy EGRET gamma excess above extrapolated background from data below 0.5 GeV

42. A Gladyshev (JINR & ITEP) Small Triangle 200542 EGRET Excess A: Inner Galaxy (l=±30 0, |b|<5 0 ) B: Galactic plane avoiding A C: Outer Galaxy D: Low latitude (10-20 0 ) E: Intermediate lat. (20-60 0 ) F: Galactic poles (60-90 0 )

43. A Gladyshev (JINR & ITEP) Small Triangle 200543 EGRET Excess vs WIMP annihilation  The excess of diffuse gamma rays is compatible with WIMP mass of 50 -100 GeV  Region A: inner Galaxy (l=±30 0, |b|<5 0 ) Background WIMP contribution

44. A Gladyshev (JINR & ITEP) Small Triangle 200544 EGRET Excess vs WIMP annihilation A: inner Galaxy (l=±30 0, |b|<5 0 ) B: Galactic plane avoiding A C: Outer Galaxy D: low latitude (10-20 0 ) E: intermediate lat. (20-60 0 ) F: Galactic poles (60-90 0 )

45. A Gladyshev (JINR & ITEP) Small Triangle 200545 EGRET Excess vs WIMP annihilation  3 components (galactic background + extragalactic background + DM annihilation) fitted simultaneously with same WIMP mass and DM normalization in all directions.  Blue: uncertainty from WIMP mass WIMP mass 50 - 100 GeV 65 100 WIMPS 00

46. A Gladyshev (JINR & ITEP) Small Triangle 200546 Determination of halo profile  The differential gamma flux in a direction forming an angle ψ with the direction of the galactic center is given by: WIMP annihilation cross section branching ratio into the tree-level annihilation final state f differential photon yield for the final state f Dark matter mass density BoostfactorWIMP mass

47. A Gladyshev (JINR & ITEP) Small Triangle 200547 Determination of halo profile  A survey of the optical rotation curves of 400 galaxies shows that the halo distributions of most of them can be fitted either with the Navarro-Frank-White (NFW) or the pseudo-isothermal profile. The halo profiles can be parametrized as follows: a is a scale radius, define behaviour at r ≈ a, r >> a and r << a

48. A Gladyshev (JINR & ITEP) Small Triangle 200548 Determination of halo profile  Navarro-Frank-White profile (1,3,1)very cuspy  Moore profile (1.5,0,1.5)very cuspy  Isotermal profile (2,2,0) less cuspy β=2 implies flat rotation curve

49. A Gladyshev (JINR & ITEP) Small Triangle 200549 Determination of halo profile  The spherical profile can be flattened in two directions to form a triaxial halo. N-body simulations suggest the ratio of the short (intermediate) axis to the major axis is typically above 0.5-0.7  It is not clear if the dark matter is homogeneously distributed or has a clumpy character. Clumps can enhance the annihilation rate. This enhancement (boostfactor) can be determined from a fit to the data.

51. A Gladyshev (JINR & ITEP) Small Triangle 200551 Determination of halo profile  The possible enhancement of DM density in the disc was parametrized by a set of Gaussian rings in the galactic plane in addition to the expected triaxial profile for the DM halo. At least two rings should be envisaged: one “outer” ring and one “inner” ring. Parameters of the rings can be determined from a fit to the data. =2  1/r 2 2 Gaussian ovals

52. A Gladyshev (JINR & ITEP) Small Triangle 200552 Determination of halo profile  Spiral structure  Caustic rings

53. A Gladyshev (JINR & ITEP) Small Triangle 200553 Determination of halo profile  Parameters in halo profile fitted by requiring minimal difference between boostfactors of various regions.  If clustering is similar in all directions (same boostfactors everywhere), then the excess of diffuse gamma rays is ~ 2 along the line of sight.  is determined by the halo profile, which is normalized to the local dark matter density ρ 0.  ρ 0 can be estimated from the rotation curve to be 0.3 GeV/cm 3 for a spherical profile and R 0 = 8.5 kpc. For a non-spherical one the density has to be rescaled.

54. A Gladyshev (JINR & ITEP) Small Triangle 200554 Determination of halo profile  Energy spectrum of diffuse gamma rays is well described by background + WIMP annihilation  Longitude and lattitude distributions (different sky directions!) of gammas are used for determination of halo and substructure (rings) parameters

55. A Gladyshev (JINR & ITEP) Small Triangle 200555 Gammas below 0.5 GeV (EGRET) Longitude: azimuthal angle Latitude: angle out of the plane

56. A Gladyshev (JINR & ITEP) Small Triangle 200556 Gammas above 0.5 GeV (EGRET) Longitude: azimuthal angle Latitude: angle out of the plane

57. A Gladyshev (JINR & ITEP) Small Triangle 200557 Fits for 1/r 2 profile with/without rings WITHOUT rings DISC 5 0 <b<10 0 10 0 <b<20 0 20 0 <b<90 0 WITH 2 rings DISC 5 0 <b<10 0 20 0 <b<90 0 10 0 <b<20 0

58. A Gladyshev (JINR & ITEP) Small Triangle 200558 Fit results for halo profile Fit results of halo parameters Enhancement of rings over 1/r 2 profile 2 and 7, respectively. Mass in rings 1.6% and 0.3% of total Dark Matter

59. A Gladyshev (JINR & ITEP) Small Triangle 200559 Determination of halo profile H2H2 H R[kpc] 4  14 kpc coincides with ring of stars at 14-18 kpc due to infall of dwarf galaxy (Yanny, Ibata, ….., 2003)  4 kpc coincides with ring of neutral hydrogen molecules!

60. A Gladyshev (JINR & ITEP) Small Triangle 200560 The Milky Way rotation curve  Contributions to the rotation curve of the Milky Way from  Visible bulge  Visible disk  Dark halo  Inner dark ring  Outer dark ring Outer Ring Inner Ring bulge totalDM 1/r 2 halo disk Rotation Curve

61. A Gladyshev (JINR & ITEP) Small Triangle 200561 Halo density at 300 kpc Cored isothermal halo profile. Total mass: 3×10 12 solar masses SideviewTopview

62. A Gladyshev (JINR & ITEP) Small Triangle 200562 Halo density at 30 kpc Ring halo substructure. R ~ 4 and 14 kpc. SideviewTopview

64. A Gladyshev (JINR & ITEP) Small Triangle 200564 Possible origin of rings  In 1994 Cambridge astronomers discovered a highly distorted dwarf galaxy in the Sagittarius constellation. The galaxy falls towards the Milky Way spreading out stars along its pass.  In 2003 Canis Major dwarf galaxy was discovered  In 2003 a giant stellar structure surrounding the Galaxy was discovered (possibly the remnant of a galaxy “eaten” by Milky Way very long ago)

66. A Gladyshev (JINR & ITEP) Small Triangle 200566 Positrons and antiprotons in cosmic rays  SAME halo and WIMP parameters as for gamma rays

67. A Gladyshev (JINR & ITEP) Small Triangle 200567 Supersymmetry FERMIONS (s=1/2)BOSONS (s=0,1) Quarks Electron, Muon, Tau Neutrinos Photon Z-boson W-boson Higgs

68. A Gladyshev (JINR & ITEP) Small Triangle 200568 Supersymmetry FERMIONS (s=1/2)BOSONS (s=0,1) QuarksSquarks Electron, Muon, TauSleptons Neutrinos Sneutrinos PhotinoPhoton ZinoZ-boson WinoCharginosW-boson Neutralnos Higgsino 1Higgs 1 Higgsino 2Higgs 2

69. A Gladyshev (JINR & ITEP) Small Triangle 200569 Neutralino – SUSY dark matter  Still we know nothing about WIMP  Supersymmetry helps again

70. A Gladyshev (JINR & ITEP) Small Triangle 200570 Neutralino – SUSY dark matter  Lagrangian of the Minimal Supersymmetric Standard Model:  Yukawa interactions

71. A Gladyshev (JINR & ITEP) Small Triangle 200571  Supersymmetry is a broken symmetry.  Breaking takes place in a hidden sector. Messengers to the visible sector can be gravitino, gauge bosons, gauginos, …  Breaking must be soft (dimension of soft SUSY breaking operators  3)  In total one has about a hundred parameters Neutralino – SUSY dark matter

72. A Gladyshev (JINR & ITEP) Small Triangle 200572 Neutralino – SUSY dark matter  Main uncertainties come from soft supersymmetry breaking parameters.  Universality hypothesis: soft supersymmetry breaking parameters unify at the scale of Grand Unification  As a result one has only 5 free parameters (4 + one sign)  Common scalar mass m 0  Common gaugino mass m 1/2  Common soft SUSY breaking parameter A 0  tan  = v 2 / v 1

73. A Gladyshev (JINR & ITEP) Small Triangle 200573 Neutralino – SUSY dark matter  Neutralino – a mixture of superpartners of photon, Z-boson and neutral Higgs bosons  Neutral (no electric chaege, no colour)  Weakly interacting (due to supersymmetry)  The lightest supersymmetric particle  Stable (!) if R-parity is conserved  Perfect candidate for dark matter particle (WIMP) photino zino higgsino higgsino

74. A Gladyshev (JINR & ITEP) Small Triangle 200574 Neutralino – SUSY dark matter  Limits on neutralino mass  Heavy enough to account for cold non- baryonic dark matter in the Universe  Annihilation cross sections are known (at least we know how to calculate them)

75. A Gladyshev (JINR & ITEP) Small Triangle 200575 Neutralino – SUSY dark matter  Main diagrams for neutralino annihilation  Dominant diagram for WMAP cross section:

76. A Gladyshev (JINR & ITEP) Small Triangle 200576 Neutralino – SUSY dark matter  B-fragmentation well studied at LEP! Yield and spectra of positrons, gammas and antiprotons well known!  Galaxy = SUPER-B-factory with luminosity some 40 orders of magnitude above man-made B-factories

77. A Gladyshev (JINR & ITEP) Small Triangle 200577 Neutralino – SUSY dark matter  Annihilation cross sections in m 0 -m 1/2 plane (μ > 0, A 0 =0) tanβ=5 tanβ=50  For WMAP cross section of  2×10 -26 cm 3 /s one needs large tanβ bb t

78. A Gladyshev (JINR & ITEP) Small Triangle 200578 Favoured regions of parameter space  Pre-WMAP allowed regions in the parameter space. Fit to all constraints tanβ=50 Fit to Dark matter constraint

79. A Gladyshev (JINR & ITEP) Small Triangle 200579 Favoured regions of parameter space  WMAP data leave only very small allowed region as shown by the thin blue line which give acceptable neutralino relic density  Excluded by LSP  Excluded by Higgs searches at LEP2  Excluded by REWSB

80. A Gladyshev (JINR & ITEP) Small Triangle 200580 Favoured regions of parameter space  The region compatible with all electroweak constraints as well as with WMAP and EGRET constraints are rather small  It corresponds to the best fit values of parameters tanβ = 51 m 0 = 1400 GeV m 1/2 = 180 GeV A 0 = 0.5 m 0

81. A Gladyshev (JINR & ITEP) Small Triangle 200581 Favoured regions of parameter space  Superparticle spectrum for m 0 =1400 GeV, m 1/2 =180 GeV  Squarks/sleptons are in TeV range  Charginos and neutralinos are light  LSP is largely Bino  Dark Matter may be supersymmetric partner of Cosmic Microwave Background

82. A Gladyshev (JINR & ITEP) Small Triangle 200582 Comparison with direct DM searches Spin-independentSpin-dependent Prediction from EGRET data assuming supersymmetry DAMA CDMS ZEPLIN Edelweiss Projections

83. A Gladyshev (JINR & ITEP) Small Triangle 200583 Summary: input  Astronomy  Dark matter in clusters of galaxies and galaxies itself  Rotation curve of the Milky Way  Astrophysics  Gamma ray flux from the sky (EGRET)  Positrons and antiprotons in cosmic rays  Cosmology  Amount of the dark matter (~23%)  Particle physics  Annihilation cross sections  Spectrum of gamma quanta from quarks/antiquarks

84. A Gladyshev (JINR & ITEP) Small Triangle 200584 Summary: physics questions & answers  Astrophysicists: What is the origin of “GeV excess” of diffuse galactic gamma rays? What is the origin of “7 GeV excess” of positrons in cosmic rays? What is the origin of “GeV excess” of antiprotons in cosmic rays? Answer: Dark matter annihilation

85. A Gladyshev (JINR & ITEP) Small Triangle 200585 Summary: physics questions & answers  Astronomers: Why a change of slope in the Milky Way rotation curve at R 0 =8.3 kpc? Answer: Dark matter substructure Why ring of stars at 14 kpc so stable? Why ring of molecular hydrogen at 4 kpc so stable?

86. A Gladyshev (JINR & ITEP) Small Triangle 200586 Summary: physics questions & answers  Cosmologists: How is Cold Dark Matter distributed? Answer: 1/r 2 profile + substructure (two rings)  Particle physicists: Is DM annihilating as expected in Supersymmetry? Answer: Cross sections are perfectly consistent with SUSY

87. THE END