Cosmic Rays II. CR observation Air and space based experiments Underground. experiments. experiments. Ground based. Astroparticle Course 1

Size: px

Start display at page:

Download "Cosmic Rays II. CR observation Air and space based experiments Underground. experiments. experiments. Ground based. Astroparticle Course 1"

Corey Jenkins
5 years ago
Views:

1 Cosmic Rays II CR observation Air and space based experiments Underground experiments Ground based experiments Astroparticle Course 1

2 Cosmic Ray Observation The figure shows that several quite different kinds of detectors are necessary to study cosmic rays over their whole energy range. Direct observations are only possible up to few hundreds of TeV for charged CR. For γ-rays, whose flux is lower by several orders of magnitudes, this limit occurs around 100 GeV. At higher energies primary CR induce in the atmosphere Air Showers detectable at ground. Astroparticle Course 2

3 CR experiments In the knee region: Tibet, HEGRA, CASA-MIA, EAS- TOP, Dice, KASCADE - KASCADE GRANDE, At higher energies: Volcano Ranch, Akeno, Yakutsk, Fly s High, Sugar, AGASA, HiRes, Havera Park, Auger, Ultra high energy cosmic rays Astroparticle Course 3

4 Aperture and acceptance The number of events detected by a given experiment depends, on one side, on the flux of the incoming particles and, on the other side, on the probability of interaction of such particles. This probability has a component depending on the physics of the microscopic event and another one connected to the geometry of the experimental apparatus. It is contained in a function, called the aperture: dn dt dφ = D de A(E) ds dω dt de D = Duty cycle The aperture of a cosmic ray experiment, A, represents the product of the solid angle times the area viewed from the incoming particles and is measured in km 2 sr. The acceptance is obtained from the aperture taking into account the efficiency of detection and the duty cycle during the period of observation. A c ( E) = D dt ε ( E, t) A( E, t) ε = efficiency Astroparticle Course 4

5 Balloon or spacecraft experiments In the interval around 1 GeV, about 10 particles per second cross a telescope of the kind in figure (the aperture is small). A small detector flown at the top of the atmosphere in a balloon or satellite is therefore sufficient for measuring charge, energy and direction of the particles. Astroparticle Course 5

6 Balloon or spacecraft experiments In the interval around 1 GeV, about 10 particles per second cross a telescope of the kind in figure (the aperture is small). A small detector flown at the top of the atmosphere in a balloon or satellite is therefore sufficient for measuring charge, energy and direction of the particles. Advanced Composition Explorer (ACE) Astroparticle Course 6

Balloon or spacecraft experiments In the interval around 1 GeV, about 10 particles per second cross a telescope of the kind in figure (the aperture is small).

7 Balloon or spacecraft experiments In the interval around 1 GeV, about 10 particles per second cross a telescope of the kind in figure (the aperture is small). A small detector flown at the top of the atmosphere in a balloon or satellite is therefore sufficient for measuring charge, energy and direction of the particles. Measurement of the charge is based on the ionization energy loss in emulsions. de dx 2 Z 2 β Advanced Composition Explorer (ACE) Energy and mass are measured with calorimeters (emulsion chambers: lead foil and emulsions), scintillators, transition radiation detectors, and Čerenkov radiation detectors. University of Chicago Astroparticle Course Cosmic Ray Experiment 7 on Spacelab

JACEE-10 (1990) and JACEE-11/12 (1993) in Antarctica have pushed the exposure time to more than one week per flight, JACEE-13 was

8 JACEE JACEE (Japanese-American Collaborative Emulsion Experiment) is a series of balloon-borne lead-emulsion chambers designed to directly measure the primary composition and spectra of cosmic rays at energies in the region of 1 TeV TeV. JACEE-10 (1990) and JACEE-11/12 (1993) in Antarctica have pushed the exposure time to more than one week per flight, JACEE-13 was completed in Antarctica, January 1995, JACEE-14 flew in December January JACEE-14 flight Launch of JACEE-11 Astroparticle Course 8

ASCA ASCA, Advanced Satellite for Cosmology

9 ASCA ASCA, Advanced Satellite for Cosmology and Astrophysics, (formerly named Astro-D) is Japan's fourth cosmic X-ray astronomy mission, successfully launched on February 20, 1993 and observed till First direct evidence that supenovae can Astroparticle Course accelerate CR 9

EGRET is 10 to 20 times larger and more sensitive than previous detectors operating at these high energies and has made detailed

10 EGRET The Energetic Gamma Ray Experiment Telescope (EGRET), onboard the Compton Gamma Ray Observatory (CGRO), provides a very high energy gamma-ray window. Its energy range is from 30 MeV to 30 GeV. EGRET is 10 to 20 times larger and more sensitive than previous detectors operating at these high energies and has made detailed observations of high energy processes associated with diffuse gamma-ray emission, gamma-ray bursts, cosmic rays, pulsars, and active galaxies known as gamma-ray blazars. Astroparticle Course 10

11 Muon detection Detection of muons important for discriminating between different primaries: more muons are produced in air showers induced by heavy nuclei, because they develop relatively high in the atmosphere, where density is lower, and it is easier for charged pions to decay to muons. Only muons (and neutrinos) can penetrate to large depths underground, till depths of tens of km of water equivalent. Measurements from GRAPES collaboration Astroparticle Course 11

12 Muon detection From PDG 2007 Detection of muons important for discriminating between different primaries: more muons are produced in air showers induced by heavy nuclei, because they develop relatively high in the atmosphere, where density is lower, and it is easier for charged pions to decay to muons. Only muons (and neutrinos) can penetrate to large depths underground, till depths of tens of km of water equivalent. Measurements from GRAPES collboration Astroparticle Course 12

13 Muon detection From PDG 2007 Detection of muons important for discriminating between different primaries: more muons are produced in air showers induced by heavy nuclei, because they develop relatively high in the atmosphere, where density is lower, and it is easier for charged pions to decay to muons. 1 km w. e. l Only muons (and neutrinos) kmρw = can penetrate to large depths underground, till depths of tens of km of water equivalent = 10 cm 1g cm = g cm 1 10 Measurements from GRAPES collaboration Astroparticle Course 13

14 Underground experiments Muons of a few hundred GeV and above have penetration depth of the order of a km even in rock and can be detected underground. Moreover, upgoing neutrinos can interact with nucleons in rock, water or ice. The EAS-TOP experiment at Gran Sasso (Campo Imperatore, 2000 m a.s.l.) has been in operation between 1989 and 2000, for CR physics in the energy range ev. It operated in coincidence with the underground experiment MACRO, which made interesting measures in various fields, among which measurements of the vertical muons coming from downgoing cosmic rays and of the upgoing muons coming from the interactions of neutrinos with the earth rock. Astroparticle Course 14

Underground experiments Muons of a few hundred GeV and above have penetration depth of the order of a km even in rock and can be detected underground.

15 Underground experiments Muons of a few hundred GeV and above have penetration depth of the order of a km even in rock and can be detected underground. Moreover, upgoing neutrinos can interact with nucleons in rock, water or ice. The EAS-TOP experiment at Gran Sasso (Campo Imperatore, 2000 m a.s.l.) has been in operation between 1989 and 2000, for CR physics in the energy range ev. It operated in coincidence with the underground experiment MACRO, which made interesting measures in various fields, among which measurements of the vertical muons coming from downgoing cosmic rays and of the upgoing muons coming from the interactions of neutrinos with the earth rock. EAS-TOP muonhadron Astroparticle Course detector 15

Neutrino telescopes Neutrino astronomy offers the possibility of observing sources which correspond to the central engines of the most energetic astrophysical phenomena.

16 Neutrino telescopes Neutrino astronomy offers the possibility of observing sources which correspond to the central engines of the most energetic astrophysical phenomena. The drawback, of course, is that the weak interactions of neutrinos imply that a very massive detector with extremely good background rejection is required to observe a measurable flux. Since the Earth acts as a shield against all particles except neutrinos, a neutrino telescope uses the detection of upwardgoing muons as a signature of muon neutrino interactions in the matter below the detector. The muon detection medium may be a natural body of water or ice through which the muon emits Čerenkov light. Its detection allows the determination of the muon trajectory. Astroparticle Course 16

Mediterranean telescopes, like Nemo, Antares near the French coast, and Nestor in the Greek sea, are complementary to other projects pointing to

17 Nemo, Antares,, Nestor, Km3-Net Nemo (Neutrino Mediterranean Observatory), located in the sea near Sicily (Capo Passero), is a project aiming to realize an underwater neutrino telescope with a volume of 1 km 3. Mediterranean telescopes, like Nemo, Antares near the French coast, and Nestor in the Greek sea, are complementary to other projects pointing to the southern emisphere (like Amanda-ICECUBE). After a first phase of prototype s study, the three Mediterranean project will start a common effort for the realization of a unique km 3 project. Nemo Antares Astroparticle Course Nestor 17

18 ICECUBE After the completion, in the same location, of the successful experiment Amanda-II, the extension to a km 3, IceCube, will be installed at the South Pole during Austral summers over approximately six years. The IceCube In-Ice detector will consist of a minimum of 4200 optical modules deployed on 70 vertical strings buried 1450 to 2450 meters under the surface of the ice, and an IceTop surface air-shower detector array of a minimum of 280 optical modules. Astroparticle Course 18

19 ICECUBE After the completion, in the same location, of the successful experiment Amanda-II, the extension to a km 3, IceCube, will be installed at the South Pole during Austral summers over approximately six years. The IceCube In-Ice detector will consist of a minimum of 4200 optical modules deployed on 70 vertical strings buried 1450 to 2450 meters under the surface of the ice, and an IceTop Left: surface South Pole air-shower station detector array of a minimum of 280 optical modules. Right: IceCube Astroparticle Course 19

20 ICECUBE After the completion, in the same location, of the successful experiment Amanda-II, the extension to a km 3, IceCube, will be installed at the South Pole during Austral summers over approximately six years. The IceCube In-Ice detector will consist of a minimum of 4200 optical modules deployed on 70 vertical strings buried 1450 to 2450 meters under the surface of the ice, and an IceTop Left: surface South Pole air-shower station detector array of a minimum of 280 optical modules. Right: IceCube Astroparticle Course 20

21 ICECUBE After the completion, in the same location, of the successful experiment Amanda-II, the extension to a km 3, IceCube, will be installed at the South Pole during Austral summers over approximately six years. The IceCube In-Ice detector will consist of a minimum of 4200 optical modules deployed on 70 vertical strings buried 1450 to 2450 meters under the surface of the ice, and an IceTop Left: surface South Pole air-shower station detector array of a minimum of 280 optical modules. Right: IceCube Hits temporal order: red, orange, yellow, green, Astroparticle Course 21

ICECUBE After the completion, in the same location, of the successful experiment Amanda-II, the extension to a km 3, IceCube, will be installed at the South Pole during Austral summers over

22 ICECUBE After the completion, in the same location, of the successful experiment Amanda-II, the extension to a km 3, IceCube, will be installed at the South Pole during Austral summers over approximately six years. The IceCube In-Ice detector will consist of a minimum of 4200 optical modules deployed on 70 vertical strings buried 1450 to 2450 meters under the surface of the ice, and an IceTop Left: surface South Pole air-shower station detector array of a minimum of 280 optical modules. Right: IceCube ICE-TOP Hits temporal order: red, orange, yellow, green, Astroparticle Course 22

23 Molière radius The Molière radius is a characteristic constant of a material which describes its electromagnetic interaction properties. It is related to the radiation length, X 0, by R M = X ( Z + 1.2) 0 where Z is the atomic number. R M is the reference scale in the lateral distribution of a shower. In fact, the average energy loss in a plastic scintillator of electrons, photons, and muons (in unit of the energy loss of vertically penetrating muons, VEM), is something like (Yakutsk and AGASA) S( r) = N e C e R α (1 + R) ( η α ) f ( r) where R = r/r M. Astroparticle Course 23

Ground experiments For primaries with energy > 10 15 ev, enough particles reach ground to be detected.

24 Ground experiments For primaries with energy > ev, enough particles reach ground to be detected. A primary of ev will have about particles in the resulting cascade, and Coulomb scattering of the shower particles (mainly electrons) and the transverse momentum in the hadronic interactions will spread them over a wide area (over 10 km 2 for ev primary), since the Molière radius in air at sea level is about 79 m. A ground based experiment is made by a number of particle detectors in a regular array (about 1 km spaced for ev). The particle detector used at the surface are scintillators and water- Čerenkov detectors. Radiation detectors are Čerenkov telescopes and fluorescence detectors. Astroparticle Course 24

Density sampling and fast timing Density sampling: the shower particle density is measured only at some locations at ground, that is in the array of detectors.

25 Density sampling and fast timing Density sampling: the shower particle density is measured only at some locations at ground, that is in the array of detectors. The energy is proportional to the total number of particles. Quantitatively, one identifies the shower core and measures the signal at 600 m from it, S(600), which is found to be quite insensitive to the primary composition and the interaction model used to simulate air showers. Fast timing: the arrival time of signals in different detectors allow reconstruction of the direction to better than 3. Astroparticle Course 25

The plastic material, excited by the charged particle, emits light

26 Scintillators The most diffused are the plastic scintillators (inorganic salt or organic plastic). The plastic material, excited by the charged particle, emits light photons which are detected by a photomultiplier (PMT) and transformed in an amplified electric signal. Astroparticle Course 26

27 Water Čerenkov When a charged particle cross the water faster than light, it produces a cone of Čerenkov light around its direction. This light can be reflected by the wall s tank and conveyed to the PMT in the upper part of the detector. The lateral density distribution of the water Čerenkov signal, ρ(r), in units of vertical equivalent muons (VEM) per m 2 is given by ρ ( r) = k r ( η + r / 4000) where r is the distance from the shower core in meters, k a normalization parameter and η a function of the zenith angle and shower energy. Astroparticle Course 27

28 Water Čerenkov When a charged particle cross the water faster than light, it produces a cone of Čerenkov light around its direction. This light can be reflected by the wall s tank and conveyed to the PMT in the upper part of the detector. PAO water Čerenkov The lateral density distribution of the water Čerenkov signal, ρ(r), in units of vertical equivalent muons (VEM) per m 2 is given by ρ ( r) = k r ( η + r / 4000) where r is the distance from the shower core in meters, k a normalization parameter and η a function of the zenith angle and shower energy. Astroparticle Course 28

Fluorescence detectors Fly s Eye fluorescence detectors The excitation of 2 + band of air nitrogen by the charged particles of an air shower of energy larger than ~ 3 10 17 ev produces fluorescence

29 Fluorescence detectors Fly s Eye fluorescence detectors The excitation of 2 + band of air nitrogen by the charged particles of an air shower of energy larger than ~ ev produces fluorescence light in the UV band ( nm), which can be detected from very large distances. A cosmic primary of ev gives a fluorescence track of km, depending on the mass of the primary and the inclination, which allows the reconstruction of the longitudinal profile and the depth of its maximum to within ±50 g/cm 2. This light, coming from a restricted field of view, is very weak, like a light bulb of a few watts, and requires to be detected dark nights (no moon or city lights) and clear time (no clouds or fog). This means that the duty cycle for this method of detection is less than 100%, usually 10%. PAO Los Leones Astroparticle Course fluorescence station 29

30 Čerenkov detectors The majority of air shower particles travel very close to the speed of light, in fact faster than the speed of light in the atmosphere. The resultant polarization of local atoms causes the emission of a faint, bluish light known as Čerenkov radiation. Depending on the energy of the initial primary, there may be thousands of electrons/positrons in the resulting cascade which are capable of emitting Čerenkov radiation. As a result, a large "pool" of Čerenkov light accompanies the particles in the air shower. This pool of light is pancakelike in appearance, about 200 meters in diameter but only a meter or so in thickness. Air Čerenkov detectors focuses this light to to a focal plane where it is detected by photomultipliers. Astroparticle Course 30

Čerenkov detectors The majority of air shower particles travel very close to the speed of light, in fact faster than the speed of light in the atmosphere.

31 Čerenkov detectors The majority of air shower particles travel very close to the speed of light, in fact faster than the speed of light in the atmosphere. The resultant polarization of local atoms causes the emission of a faint, bluish light known as Čerenkov radiation. Depending on the energy of the initial primary, there may be thousands of electrons/positrons in the resulting cascade which are capable of emitting Čerenkov radiation. As a result, a large "pool" of Čerenkov light accompanies the particles in the air shower. This pool of light is pancakelike in appearance, about 200 meters in diameter but only a meter or so in thickness. Air Čerenkov detectors focuses this light to to a focal plane where it is detected by photomultipliers. Astroparticle Course 31

and muon detectors. The energies explored are in the knee region.

32 KASCADE and KASCADE-Grande KASCADE (KArlsruhe Shower Core and Array DEtector) is a ground detector, located in Karlsruhe (Germany), made by scintillators and muon detectors. The energies explored are in the knee region. KASCADE-Grande is an extension of KASCADE toward higher energies. Astroparticle Course 32

33 Ultra high energy CR experiments The first pioneeristic experiments used small configurations of ground arrays of Geiger-Müller or plastic scintillators: Pamir (1946), Agassiz (1956). Area km VR FY HP OWL EUSO AUGER Hires AGASA Yak Year Astroparticle Course 33

Ultra high energy CR experiments The first pioneeristic experiments used small configurations of ground arrays of Geiger-Müller or plastic scintillators: Pamir (1946), Agassiz (1956).

34 Ultra high energy CR experiments The first pioneeristic experiments used small configurations of ground arrays of Geiger-Müller or plastic scintillators: Pamir (1946), Agassiz (1956). Linsley & Scarsi (1957), 19 plastic scintillators coupled to photomultipliers and oscilloscopes, largest event with ev Area km VR FY HP OWL EUSO AUGER Hires AGASA Yak Year Astroparticle Course 34

35 Ultra high energy CR experiments The first pioneeristic experiments used small configurations of ground arrays of Geiger-Müller or plastic scintillators: Pamir (1946), Agassiz (1956). Watson & al. (1967), 200 water Čerenkov coupled to photomultipliers over 12 km 2, 4 events with > ev Area km VR FY HP OWL EUSO AUGER Hires AGASA Yak Year Astroparticle Course 35

36 Ultra high energy CR experiments The first pioneeristic experiments used small configurations of ground arrays of Geiger-Müller or plastic scintillators: Pamir (1946), Agassiz (1956). Krasilnikov & al. (1970), up to 86 scintillators and 43 Čerenkov detectors over 25 km 2, largest event ev Area km VR FY HP OWL EUSO AUGER Hires AGASA Yak Year Astroparticle Course 36

37 AGASA The Akeno Giant Air Shower Array was the first giant apparatus: 111 plastic scintillators on the ground, 1 km spaced, and 27 shielded muon detectors, spread over an area of ~100 km 2. Also calorimeters (small) and water Čerenkov detectors. Astroparticle Course 37

AGASA The Akeno Giant Air Shower Array was the first giant apparatus: 111 plastic scintillators on the ground, 1 km spaced, and 27 shielded muon detectors,

38 AGASA The Akeno Giant Air Shower Array was the first giant apparatus: 111 plastic scintillators on the ground, 1 km spaced, and 27 shielded muon detectors, spread over an area of ~100 km 2. Also calorimeters (small) and water Čerenkov detectors. Box with scintillator and electronics in AGASA Astroparticle Course 38

39 AGASA The Akeno Giant Air Shower Array was the first giant apparatus: 111 plastic scintillators on the ground, 1 km spaced, and 27 shielded muon detectors, spread over an area of ~100 km 2. Also calorimeters (small) and water Čerenkov detectors. AGASA muon detectors Astroparticle Course 39

40 AGASA The Akeno Giant Air Shower Array was the first giant apparatus: 111 plastic scintillators on the ground, 1 km spaced, and 27 shielded muon detectors, spread over an area of ~100 km 2. Also calorimeters (small) and water Čerenkov detectors. AGASA water Čerenkov Astroparticle Course 40

41 AGASA AGASA detected 6 events with energy above ev. The most energetic event was observed on December, 3 rd AGASA closed in Highest energy event in AGASA: ev Astroparticle Course 41

42 AGASA AGASA detected 6 events with energy above ev. The most energetic event was observed on December, 3 rd AGASA closed in Highest energy event in AGASA: ev Astroparticle Course 42

43 Fly s s Eye In 1981, the cosmic ray group of the University of Utah started the construction, in the Dugway desert, of the first experiment using the air fluorescence technique, following a successful trial at Volcano Ranch. The two eyes, 3.3 km apart, were made up of 67 and 36 modules, respectively, with 12 photomultiplier tubes per module. The most energetic event was one with energy ev. Astroparticle Course 43

44 HiRes HiRes (High Resolution Fly s Eye) is the successor to the Fly s Eye experiment, which was operated at the same site over the period It consisted of two detector stations (HiRes-I and HiRes-II) located 12.6 km apart. HiRes-I (HiRes-II) had 21 (42) modules pointing to 3-17 (3-31 ) in elevation. 256 PMT were placed at the focal plane of each mirror. The data analysis was carried out in monocular mode, with best statistical power and wider energy range, or stereo mode, with best resolution but less statistic. Astroparticle Course 44

45 HiRes HiRes (High Resolution Fly s Eye) is the successor to the Fly s Eye experiment, which was operated at the same site over the period It consisted of two detector stations (HiRes-I and HiRes-II) located 12.6 km apart. HiRes-I (HiRes-II) had 21 (42) modules pointing to 3-17 (3-31 ) in elevation. 256 PMT were placed at the focal plane of each mirror. The data analysis was carried out in monocular mode, with best statistical power and wider energy range, or stereo mode, with best resolution but less statistic. Energy calibration in HiRes Astroparticle Course 45

46 HiRes HiRes (High Resolution Fly s Eye) is the successor to the Fly s Eye experiment, which was operated at the same site over the period It consisted of two detector stations (HiRes-I and HiRes-II) located 12.6 km apart. HiRes-I (HiRes-II) had 21 (42) modules pointing to 3-17 (3-31 ) in elevation. 256 PMT were placed at the focal plane of each mirror. The data analysis was carried out in monocular mode, with best statistical power and wider energy range, or stereo mode, with best resolution but less statistic. ICRC 2007 CR spectrum from HiRes 13 events with E>10 Astroparticle Course 20 ev 46

47 Pierre Auger Observatory PAO is a hybrid detector, employing the two methods of ground array and fluorescence technique for the detection of EAS. Comparing results from the different types of detectors helps to reconcile the two sets of data and produce the most accurate results about the energy of primary cosmic rays. It started operation in 2004 and a northern site is planned in Colorado. Astroparticle Course 47

Pierre Auger Observatory PAO is a hybrid detector, employing the two methods of ground array and fluorescence technique for the detection of EAS.

48 Pierre Auger Observatory PAO is a hybrid detector, employing the two methods of ground array and fluorescence technique for the detection of EAS. Comparing results from the different types of detectors helps to reconcile the two sets of data and produce the most accurate results about the energy of primary cosmic rays. It started operation in 2004 and a northern site is planned in Colorado. Located at Pampa Amarilla in Argentina Size: 50x60 km2=3000 km water Čerenkov 24 fluorescence telescopes in 4 stations 17 nations involved 300 physicists and 100 technicians 38 Italian physicists from 8 Italian groups Astroparticle Course 48

49 Pierre Auger Observatory Recent physical results of PAO were communicated at the ICRC 2007 and on November, 9 th Exp Obs > / > / km 2 sr yr ~ 0.8 full Auger year Astroparticle Course 49

50 Pierre Auger Observatory Recent physical results of PAO were communicated at the ICRC 2007 and on November, 9 th Centaurus A Exp Obs > / > / km 2 sr yr ~ 0.8 full Auger year Astroparticle Course 50

51 Pierre Auger Observatory Recent physical results of PAO were communicated at the ICRC 2007 and on November, 9 th Centaurus A More details later Exp Obs > / > / km 2 sr yr ~ 0.8 full Auger year Astroparticle Course 51

air-fluorescence techniques, like PAO. It is being deployed in the high desert in Millard County, Utah, USA.

52 Telescope Array The Telescope Array project is a collaboration between universities and institutes in Japan, Taiwan, China and the USA. The experiment is designed to observe cosmic-ray-induced air showers at extremely high energies using a combination of ground array and air-fluorescence techniques, like PAO. It is being deployed in the high desert in Millard County, Utah, USA. SD full operation started on the beginning of First data are expected in Fluorescence site construction Ground array Astroparticle Course deployment 52

JEM-EUSO EUSO EUSO is a space mission devoted to the investigations of cosmic rays and neutrinos at very high energy (> 10 20 ev) by looking downward from space, under a 60 angle, at the

The phase-b study, however, has been postponed for a long time because of financial problems in ESA

53 JEM-EUSO EUSO EUSO is a space mission devoted to the investigations of cosmic rays and neutrinos at very high energy (> ev) by looking downward from space, under a 60 angle, at the fluorescence light produced when cosmic rays hit the air molecules. Phase-A study of EUSO under the ESA has successfully finished in July The phase-b study, however, has been postponed for a long time because of financial problems in ESA and Italy. Then, Japanese and U.S. teams re-defined EUSO as a mission attached to the Japanese Experiment Module/Exposure Facility of the International Space Station. They renamed it as JEM-EUSO and started the preparation targeting the launch in 2012 in the framework of second phase of JEM/EF utilization. Astroparticle Course 53

OWL OWL (Orbiting Wide angle Light collectors) is a satellite project aiming at the observation of the air shower s development from the space in mono and stereo mode.

through the earth. In the second one, they will separate to 600 km for ~ 2.

54 OWL OWL (Orbiting Wide angle Light collectors) is a satellite project aiming at the observation of the air shower s development from the space in mono and stereo mode. Three phases are planned: in the first one, two satellites will fly in formation with a separation of 10 to 20 km for about 3 months to search for upward-going showers from ν τ s propagating through the earth. In the second one, they will separate to 600 km for ~ 2.5 years to measure the high energy end of the CR spectrum and in the third one the altitude will be reduced to 600 km and the separation to 500 km to study the CR flux near ev. Claimed energy resolution is 14% at ev, angular resolution less than 1, stereo aperture = km 2 sr, duty cycle ~ 10%. Astroparticle Course 54

Status and results from the Pierre Auger Observatory

April 15-19, 2007 Aspen, Colorado Status and results from the Pierre Auger Observatory Lorenzo Perrone for the Auger Collaboration Università del Salento and INFN Lecce Italy The Physics Case: highest