This presentation was created based on the slides by Vitor de Souza from his talk at the 4th
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1 This presentation was created based on the slides by Vitor de Souza from his talk at the 4th School on Cosmic Rays and Astrophysics UFABC - Santo André - São Paulo - Brazil August 25 to September
2 The multimessenger approach to astroparticle physics Célio A. Moura Universidade Federal do ABC UFABC Seminario Facultad de Ciencias Físico Matemáticas BUAP October 27, 2010
3 Energy Spectrum
4 Via Láctea: Rádio (408 MHz) C. Haslam et al., MPIfR, SkyView
5 Via Láctea: Rádio (1420 MHz) Dickey et.al. UMn. NRAO SkyView
6 Via Láctea: Infravermelho Dirbe Team, COBE, NASA
7 Via Láctea: Vísivel por Axel Melinger
8 Via Láctea: Ultravioleta J. Bonnell et.al.(gsfc, NASA)
9 Via Láctea: Ráios X Digel et. al. GSFC, ROSAT, NASA
10 Via Láctea: Ráios Gama > 100 MeV (CGRO, NASA)
11 Point Sources Gamma Rays > 1012 ev Cerenkov Telescopes, by Jim Hinton
12 Other messengers
13 KASCADE E ~ ev TeV = 1012 ev PeV= 1015 ev EeV= 1018 ev ZeV= 1021 ev
14 AGASA 1 8 E > 10 ev TeV = 1012 ev PeV= 1015 ev EeV= 1018 ev ZeV= 1021 ev
15 Auger E > 5.7 x ev TeV = 1012 ev PeV= 1015 ev EeV= 1018 ev ZeV= 1021 ev
16 Astroparticle Physics Second ASPERA* Astroparticle physics is a new multidisciplinary field of research that deals with the study of particles coming from the Universe. *It is an European network of national government agencies responsible for coordinating and funding national research efforts in Astroparticle Physics.
17 Astroparticle Physics The study of the physics phenomena occurring in astronomical objects by measuring the high energy particles they produce. Astrophysics Particle Physics Cosmology
18 HOW DO WE DO ASTROPARTICLE PHYSICS?
19 Astroparticle Physics S E C R P U O S YMA SK ENERGY SPECTRUM COM POS IT IO N
20 WHAT CAN WE LEARN FROM NATURE BY UNSCRAMBLING THIS PUZZLE?
21 Source Skymap Source type identification
22 Energy Spectrum
23 Acceleration (Original) Fermi acceleration mechanism (second ordem). First order acceleration Fermi mechanism.
24 Keep the particle inside the acceleration region E GeV 10 r L, pc Z B G 6 RS rl 15 E ev 10 Z B G R S, pc 24
25 Energy spectrum Magnetic field Intensity Structure Shock wave speed Size of the region Particle charge Injection speed Scape probability 25
26 Composition e- e- E GeV 10 r L, pc Z B G 6 15 E ev 10 Z B G R S, pc 26
27 A s t r o p h y s i c a l Spectrum M o d e l s Composition Source Directions M e a s u r e d C o s m i c R a y D a t a 27
28 20 years ago... Pierre Auger Observatory Science Case E > 1019 ev Interesting! 28
29 15 E ev 10 Z B G R S, pc M. Hillas
30 Interesting points: There are only a few sources able to accelerate particles beyond 1019 ev
31 Propagation J. Cronin
32 Interesting points: There are only a few sources able to accelerate particles beyond 1019 ev - Particle propagate straight from the source to Earth
33 Universe is not empty
34 p + 2, 7 K p + o GZK Effect 1 pc = 3 x m J. Cronin
35 Interesting points: There are only a few sources able to accelerate particles beyond ev - Particle propagate straight from the source to the Earth Sources are not far away (D < 100 Mpc)
36 1 pc = 3 x m Slide: Silvia Mollerach
37 Slide: Silvia Mollerach 1 pc = 3 x m
38 Interesting points: There are only a few sources able to accelerate particles beyond 1019 ev - Particle propagate straight from the source to the Earth Sources are not far away (D < 100 Mpc) The Universe is anisotropic and has voids inside 100 Mpc
39 Characteristics Large Collection Area Pierre Auger = 3000 km2 Observatory 1 particle per km2 per century
40 Energy Spectrum Composition Source Skymap?
41 Energy Spectrum Measurement flux Energy
42 Energy Composition Shower Development Measure Components
43 Energy Arrival Direction Source Skymap
44 Energy Spectrum Measurement flux Energy Composition Arrival Direction Shower Development Source Skymap Measure Components
45 UHECR Detector Techniques Ground Arrays Fluorescence Telescopes
46 Measurement flux Energy Arrival Direction Shower Development Measure Components
47 Measurement flux Energy Arrival Direction Shower Development Measure Components
48 Measurement flux Energy Arrival Direction Shower Development Measure Components
49 Extensive Air Shower 49
50 Energy Spectrum Measurement flux Energy Composition Arrival Direction Shower Development Source Skymap Measure Components
51 Telescope view Telescopes measure the intensity and arrival time of the fluorescence light 51
52 Camera view Telescopes measure the intensity and arrival time of the fluorescence light 52
53 Longitudinal Profile The intensity as a function of elevation can be transformed into the energy deposited in the atmosphere as a function of depth53
54 Fitting the Longitudinal Profile Xmax The total calorimetric energy of the shower is proportional to the integral of the energy deposited 54
55 Energy Spectrum Measurement flux Energy Composition Arrival Direction Shower Development Source Skymap Measure Components
56 Measurement flux Spectrum Energy GZK-Like Suppression Ankle
57 Energy Arrival Direction Source Skymap
58 Arrival Direction
59 Camera view Telescopes measure the intensity and arrival time of the fluorescence light 59
60 Hybrid Angular Resolution 60
61 Energy Arrival Direction Source Skymap
62 Energy Source Skymap Arrival Direction
63 AGN Correlation
64 Energy Composition Shower Development Measure Components
65 Energy Composition Shower Development Measure Components
66
67
68
69
70 Energy Composition Shower Development Measure Components
71 No photons detected
72 No neutrinos detected
73 Double Bangs in the Atmosphere M. M. Guzzo and C. A. Moura, Astropart. Phys. 25, 277 (2006) [arxiv:hep-ph/ ].
74 Composition
75 UHECR Puzzle 75
76 UHECR Puzzle Light Heavier Isotropic? AGN Correlation 76
77 Questions Is the suppression above 5x101 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? 77
78 Questions Are AGNs the sources or are they only tracers? Is the composition change astrophysical or do we need new particle physics for El a b > ev ~ Ec. m. > 5x101 4 ev? 78
79 Questions Is there something we do not understand in the shower development? 79
80 Questions Is there any relation of all this with DM and DE? 80
81 Answers may come from Auger, Auger North, JEM-EUSO: nuclei, gammas, neutrinos; IceCube, KM3Net (ANTARES, NEMO, NESTOR): neutrinos; Fermi, HESS, Magic: gammas. Pamela, Fermi, CDMS, Xenon, DAMA, etc. DM WMAP and similars-> DE
82 20 years ago... Astroparticle Physicist Astroparticle Physics Puzzle 82
83 Today Astroparticle Physicist Astroparticle Physics Puzzle 83
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