1 Pierre Auger Observatory Vitor de Souza

2 Credit & Copyright: Alex Cherney (Terrastro)

3 Instruments Moons of Jupiter

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

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

Via Láctea: Infravermelho Dirbe Team, COBE, NASA

Via Láctea: Vísivel por Axel Melinger

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

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

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

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

Fontes Pontuais Raios Gama > eV Telescópios Cerenkov, por Jim Hinton

TeV = eV PeV= eV EeV= eV ZeV= eV KASCADE E ~ eV

TeV = eV PeV= eV EeV= eV ZeV= eV AGASA E > eV

Auger E > 5.7 x eV TeV = eV PeV= eV EeV= eV ZeV= eV

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

HOW DO WE DO ASTROPARTICLE PHYSICS ?

Astroparticle Physics ? ? ?

SOURCE S SKYMAP ENERGY SPECTRUM COMPOSITIO N

WHAT CAN WE LEARN FROM NATURE BY UNSCRAMBLING THIS PUZZLE ?

Source Skymap Source type identification

Energy Spectrum

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

25 Move the racket V Vr

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

34 Keep the particle inside the acceleration region RSRS rLrL

35 Movie about aceleration Credits: Raboud University Nijmegen the Netherlands

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

37 Composition e-e-  e-e-

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

WHAT QUESTIONS THE PIERRE AUGER OBSERVATORY INTENDS TO ANSWER ?

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

M. Hillas 1 pc = 3 x m

Interesting points: – There are only a few sources able to – acelerate particles beyond eV

Propagation J. Cronin 1 pc = 3 x m

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

Universe is not empty

Energy loss E = eV E = eV E = 5x eV E = eV E = 8x eV E = 5x eV E = 8x eV E = 6x eV E = 5x eV

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

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

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

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

Slide: Silvia Mollerach 1 pc = 3 x m

Slide: Silvia Mollerach 1 pc = 3 x m

Interesting points: – There are only a few sources able to – acelerate particles beyond 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

Science Case: – There are only a few sources able to – acelerate particles beyond 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

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

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

Energy Spectrum Composition Source Skymap ?

Energy Spectrum Measurement flux Energy

Shower Development Measure Components Composition

Energy Arrival Direction Source Skymap

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

Know Detector Techniques Ground ArraysFluorescence Telescopes

Measurement flux Energy Arrival Direction Shower Development Measure Components

Measurement flux Energy Arrival Direction Shower Development Measure Components

Measurement flux Energy Arrival Direction Shower Development Measure Components

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

Movie about Auger

71 Extensive Air Shower

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

73 Extensive Air Shower E0E0 DsDs

74 Counting Showers

75 Counting Showers

76 Counting Showers

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

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

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

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

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

Spectrum Measurement flux Energy GZK-Like Suppression Ankl e

Energy Arrival Direction Source Skymap

km

86 Arrival time

87 Arrival time

88 Arrival time

Arrival Direction

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

91 Hybrid Angular Resolution

Energy Arrival Direction Source Skymap

Energy Arrival Direction Source Skymap

AGN Correlation

Energy Shower Development Measure Components Composition

Energy Shower Development Measure Components Composition

Energy Shower Development Measure Components Composition

No photons detected

No neutrinos detected

Astroparticle Physics Puzzle SOURC E SKYMAP ENERGY SPECTRUM COMPOSITIO N

106 Auger Observatory Puzzle

107 Auger Observatory Puzzle LightHeavier ?

108 Auger Observatory Puzzle Isotropic AGN Correlation LightHeavier ?

109 Questions Is the suppression above 5x 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 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 > eV ~ E c. m. > 5x eV ?

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

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

years ago... Astroparticle Physicist Astroparticle Physics Puzzle

114 Today Astroparticle Physicist Astroparticle Physics Puzzle

115 Today Astroparticle Physicist Astroparticle Physics Puzzle

116 Pierre Auger Observatory Vitor de Souza