1. 1 Pierre Auger Observatory Vitor de Souza vitor@ifsc.usp.br

2. 2 Credit & Copyright: Alex Cherney (Terrastro)

3. 3 Instruments Moons of Jupiter

5. Via Láctea: Rádio (408 MHz) C. Haslam et al., MPIfR, SkyView

6. Via Láctea: Rádio (1420 MHz) Dickey et.al. UMn. NRAO SkyView

7. Via Láctea: Infravermelho Dirbe Team, COBE, NASA

8. Via Láctea: Vísivel por Axel Melinger

9. Via Láctea: Ultravioleta J. Bonnell et.al.(GSFC, NASA)

10. Via Láctea: Ráios X Digel et. al. GSFC, ROSAT, NASA

11. Via Láctea: Ráios Gama > 100 MeV (CGRO, NASA)

12. E f = m e c 2 + m e c 2 = 1 MeV E  > 1 MeV -> ~ 10 2 1 Hz

13. Fontes Pontuais Raios Gama > 10 1 2 eV Telescópios Cerenkov, por Jim Hinton

14. TeV = 10 12 eV PeV= 10 15 eV EeV= 10 18 eV ZeV= 10 21 eV KASCADE E ~ 10 1 6 eV

15. TeV = 10 12 eV PeV= 10 15 eV EeV= 10 18 eV ZeV= 10 21 eV AGASA E > 10 1 8 eV

16. Auger E > 5.7 x 10 1 9 eV TeV = 10 12 eV PeV= 10 15 eV EeV= 10 18 eV ZeV= 10 21 eV

17. Astroparticle Physics The study of the physics fenomena occuring in astronomical objetcs by measuring the high energy particles they produce. AstrophysicsParticle Physics

18. HOW DO WE DO ASTROPARTICLE PHYSICS ?

19. Astroparticle Physics ? ? ?

20. SOURCE S SKYMAP ENERGY SPECTRUM COMPOSITIO N

21. WHAT CAN WE LEARN FROM NATURE BY UNSCRAMBLING THIS PUZZLE ?

22. Source Skymap Source type identification

23. Energy Spectrum

24. 24 Accelerating a ball V - V Ball against a wallBall against a racket V - V

25. 25 Move the racket V Vr

26. 26 vBGvBG VRGVRG GrandStand Reference Frame (G) Racket Reference Frame (R) V B R = V B G + V R G VBRVBR B = Ball R = Racket G = GrandStand

27. 27 B = Ball R = Racket G = GrandStand vBRivBRi V B R f V B R i = V B G i + V R G V B R f = - V B R i Racket Reference Frame (R)

28. 28 V B R i = V B G i + V R G V B R f = V B G f + V R G V B G f = V B R f - V R G Grandstand Reference Frame (G)

29. 29 V B R i = V B G i + V R G V B R f = V B G f + V R G V B G f = V B R f - V R G V B G f = - V B R i - V R G Grandstand Reference Frame (G) Using from previus slide: V B R f = - V B R i

30. 30 V B R i = V B G i + V R G V B R f = V B G f + V R G V B G f = V B R f - V R G V B G f = - V B R i - V R G Grandstand Reference Frame (G) Using from previus slide: V B R f = - V B R i But: V B R i = V B G i + V R G

31. 31 V B R i = V B G i + V R G V B R f = V B G f + V R G V B G f = V B R f - V R G V B G f = - V B R i - V R G V B G f = - V B G i - V R G - V R G V B G f = - V B G i - 2V R G Grandstand Reference Frame (G) Using from previus slide: V B R f = - V B R i But: V B R i = V B G i + V R G

32. 32 Accelerating a particle Ball = Particle Racket = Magnetic Fields If the racket does not move V p f = V p i B B = 0 VPiVPi VPfVPf

33. 33 Accelerating a particle Move the racket ! The particle gains energy B B = 0 VRVR VRVR VPiVPi VPfVPf

34. 34 Keep the particle inside the acceleration region RSRS rLrL

35. 35 Movie about aceleration Credits: Raboud University Nijmegen the Netherlands

36. 36 Energy spectrum ● Magnetic field ● Intensity ● Structure ● Shock wave speed ● Size of the region ● Particle charge ● Injection speed ● Scape probability

37. 37 Composition e-e-  e-e-

38. 38 Ray DataRay Data AstrophysicalAstrophysical M e a s u r e d C o s m i c ModelsModels Spectrum Composition Source Directions

39. WHAT QUESTIONS THE PIERRE AUGER OBSERVATORY INTENDS TO ANSWER ?

40. 40 20 years ago... Interesting ! Pierre Auger Observatory Science Case E > 10 1 9 eV

41. M. Hillas 1 pc = 3 x 10 1 6 m

42. Interesting points: – There are only a few sources able to – acelerate particles beyond 10 1 9 eV

43. Propagation J. Cronin 1 pc = 3 x 10 1 6 m

44. Interesting points: – There are only a few sources able to – acelerate particles beyond 10 1 9 eV - Particle propate straight from the source to Earth

45. Universe is not empty

47. Energy loss E = 10 2 1 eV E = 10 2 0 eV E = 5x10 1 9 eV E = 10 2 0 eV E = 8x10 1 9 eV E = 5x10 1 9 eV E = 8x10 1 9 eV E = 6x10 1 9 eV E = 5x10 1 9 eV

48. p +  2, 7 K  p +  o J. Cronin GZK Effect 1 pc = 3 x 10 1 6 m

49. J. Cronin GZK Effect 1 pc = 3 x 10 1 6 m p +  2, 7 K  p +  o

50. J. Cronin GZK Effect 1 pc = 3 x 10 1 6 m p +  2, 7 K  p +  o

51. Interesting points: – There are only a few sources able to – acelerate particles beyond 10 1 9 eV - Particle propate straight from the source to Earth – Sources are not far away (D < 100 Mpc)

52. Slide: Silvia Mollerach 1 pc = 3 x 10 1 6 m

53. Slide: Silvia Mollerach 1 pc = 3 x 10 1 6 m

54. Interesting points: – There are only a few sources able to – acelerate particles beyond 10 1 9 eV - Particle propate straight from the source to Earth – Sources are not far away (D < 100 Mpc) – The Universe is anisotropic and has voids – inside 100 Mpc

55. Science Case: – There are only a few sources able to – acelerate particles beyond 10 19 eV - Particle propate straight from the source to Earth – Sources are not far away (D < 100 Mpc) – The Universe is anisotropic and has voids – inside 100 Mpc

56. WHAT ARE THE CHARACTERISTICS OF THE OBSERVATORY NEEDED TO STUDY THIS PHENOMENA ?

57. Characteristics 1 particle per km 2 per century Large Collection Area Pierre Auger Observatory = 3000 km 2

58. Energy Spectrum Composition Source Skymap ?

59. Energy Spectrum Measurement flux Energy

60. Shower Development Measure Components Composition

61. Energy Arrival Direction Source Skymap

62. Energy Spectrum Measurement flux Energy Arrival Direction Shower Development Measure Components Composition Source Skymap

63. Know Detector Techniques Ground ArraysFluorescence Telescopes

64. Measurement flux Energy Arrival Direction Shower Development Measure Components

65. Measurement flux Energy Arrival Direction Shower Development Measure Components

66. Measurement flux Energy Arrival Direction Shower Development Measure Components

69. Auger Collaboration: ArgentinaMexico Australia Netherlands Bolivia * Poland Brazil Slovenia Czech Republic Spain France United Kingdom Germany USA Italy Vietnam * Portugal * Associated countries

70. Movie about Auger

71. 71 Extensive Air Shower

72. 72 Movie about shower development Credits: H. Drescher, University of Frankfurt

73. 73 Extensive Air Shower E0E0 DsDs

74. 74 Counting Showers

75. 75 Counting Showers

76. 76 Counting Showers

77. Energy Spectrum Measurement flux Energy Arrival Direction Shower Development Measure Components Composition Source Skymap

78. 78 Telescope view Telescopes measure the intensity and arrival time of the fluorescence light

79. 79 Camera view Telescopes measure the intensity and arrival time of the fluorescence light

80. 80 Longitudinal Profile The intensity as a function of elevation can be transformed into the energy deposited in the atmosphere as a function of depth

81. 81 Fitting the Longitudinal Profile The total calorimetric energy of the shower is proportional to the integral of the energy deposited Xmax

82. Energy Spectrum Measurement flux Energy Arrival Direction Shower Development Measure Components Composition Source Skymap

83. Spectrum Measurement flux Energy GZK-Like Suppression Ankl e

84. Energy Arrival Direction Source Skymap

85. 85 1.5 km

86. 86 Arrival time

87. 87 Arrival time

88. 88 Arrival time

89. Arrival Direction

90. 90 Camera view Telescopes measure the intensity and arrival time of the fluorescence light

91. 91 Hybrid Angular Resolution

92. Energy Arrival Direction Source Skymap

93. Energy Arrival Direction Source Skymap

94. AGN Correlation

95. Energy Shower Development Measure Components Composition

96. Energy Shower Development Measure Components Composition

101. Energy Shower Development Measure Components Composition

102. No photons detected

103. No neutrinos detected

105. Astroparticle Physics Puzzle SOURC E SKYMAP ENERGY SPECTRUM COMPOSITIO N

106. 106 Auger Observatory Puzzle

107. 107 Auger Observatory Puzzle LightHeavier ?

108. 108 Auger Observatory Puzzle Isotropic AGN Correlation LightHeavier ?

109. 109 Questions Is the suppression above 5x10 1 9 eV due to interaction with the CMB or is it due to the source limit ? How to reconcile the AGN correlation with A > 1 ? ● Very low magnetic fields ? ● Nearby source with enhanced flux and power ?

110. 110 Questions Are AGNs the sources or are they only tracers ? Is the composition change astrophysical or do we need new particle physics for E l a b > 10 1 8 eV ~ E c. m. > 5x10 1 4 eV ?

111. 111 Questions Is there something we do not understand in the shower development ?

112. 112 Answers should come from: ● Auger South continuous operations and enhancements ● Auger South innovative data analysis ● Auger North ~ 20000 km 2 ~ 7 x Auger South ● Composition above 10 1 9. 5 eV ● Multi-messenger approach: Neutrinos, TeV- Gamma

113. 113 20 years ago... Astroparticle Physicist Astroparticle Physics Puzzle

114. 114 Today Astroparticle Physicist Astroparticle Physics Puzzle

115. 115 Today Astroparticle Physicist Astroparticle Physics Puzzle

116. 116 Pierre Auger Observatory Vitor de Souza vitor@ifsc.usp.br