The Pierre Auger Observatory
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1 The Pierre Auger Observatory Hunting the Highest Energy Cosmic Rays II EAS Detection at the Pierre Auger Observatory March 07 E.Menichetti - Villa Gualino, March
2 EAS The Movie March 07 E.Menichetti - Villa Gualino, March
3 EAS Early History March 07 E.Menichetti - Villa Gualino, March
4 The Hybrid Concept SD: Sampling Lateral Profile at ground FD: Measuring E tot & Longitudinal Profile March 07 E.Menichetti - Villa Gualino, March
5 Geography - I Very flat region Pampa Amarilla Malargüe (Argentina) 35 o S latitude 69 o W longitude 1400 m height 875 g/cm 2 Very low population density (< 0.1 /km 2 ) Good atmospheric conditions (clouds, aerosol, light ) March 07 E.Menichetti - Villa Gualino, March
6 Geography - II March 07 E.Menichetti - Villa Gualino, March
7 The South Site Total area ~3000 km Surface detectors ( water tanks ) 24 fluorescence telescopes 6 in each of 4 buildings 50 km March 07 E.Menichetti - Villa Gualino, March
8 Advertisement - I March 07 E.Menichetti - Villa Gualino, March
9 Topography 1500 m March 07 E.Menichetti - Villa Gualino, March
10 Ground Array EAS sampled at ground by a number of detector stations Shower front EM shower Shower core hard muons March 07 E.Menichetti - Villa Gualino, March
11 EAS Direction from Timing B.Rossi, 1953 March 07 E.Menichetti - Villa Gualino, March
12 Light Emission by Muons muon 41 Water n N ph ph 2 500sin photomultiplier 250 photons/cm Vertical Equivalent Muon Light Collection < 1% C Retro-diffusing Walls When a particle travels faster than the velocity of light in water, light is emitted March 07 E.Menichetti - Villa Gualino, March
13 Tank Details March 07 E.Menichetti - Villa Gualino, March
14 From Design to Reality March 07 E.Menichetti - Villa Gualino, March
15 PM and HV Voltage Divider 9 PM from Photonis HV made on board March 07 E.Menichetti - Villa Gualino, March
16 Mechatronics, Pedestals March 07 E.Menichetti - Villa Gualino, March
17 Solar Panels, Antennas March 07 E.Menichetti - Villa Gualino, March
18 SD Pulse Height from Muons Signal unit ~ 1 VEM ~ 94 ph.e. March 07 E.Menichetti - Villa Gualino, March
19 SD P.H. Spectrum for Calibration Most frequent signals ~ atmospheric muons.. We measure muon lifetime A/D ratio - sliding average over 3 min of signals > 512 March 07 E.Menichetti - Villa Gualino, March
20 SD Muon Calibration March 07 E.Menichetti - Villa Gualino, March
21 SD Linearity (Low Signals) March 07 E.Menichetti - Villa Gualino, March
22 SD: Signal Components Simulation March 07 E.Menichetti - Villa Gualino, March
23 SD FADC Traces µ ± e ± γ 1GeV 10MeV 10MeV 1.2m Water 240MeV 10MeV 10MeV ~track ~ energy Time (ns) March 07 E.Menichetti - Villa Gualino, March
24 SD - Hunting the Shower I Concept: Energy from Lateral Distribution! 1) EAS direction from tank timing, position March 07 E.Menichetti - Villa Gualino, March
25 SD Twin Tanks Good to check timing resolution March 07 E.Menichetti - Villa Gualino, March
26 SD - Hunting the Shower II 2) Reconstruct LDF Fit to empirical formula 3) Get S(1000) Detector signal at ground, 1 km off the core 4) Correct for slant depth S 38 (1000) Constant Intensity Cut Take 38 0 Zenith as a Reference Previous experiments, MCarlo: E = k S 38 (1000) AUGER Unique Capability: Get k constant from FD March 07 E.Menichetti - Villa Gualino, March
27 Communications Network March 07 E.Menichetti - Villa Gualino, March
28 SD Aperture Relative aperture (trigger included) vs. Energy Full efficiency above 3 EeV March 07 E.Menichetti - Villa Gualino, March
29 SD Resolution S(1000) Zenith Several sources of systematic uncertainty 1. VEM calibration 2. Timing 3. S(1000) slant depth effects (CIC) Core Position S(1000)>30VEM March 07 E.Menichetti - Villa Gualino, March
30 FD Fluorescence Yield Atmosphere working as a large scale calorimeter March 07 E.Menichetti - Villa Gualino, March
31 FD The Fly s Eye Concept Fluorescence Light EAS Path Sensor Array March 07 E.Menichetti - Villa Gualino, March
32 Advertisement - II March 07 E.Menichetti - Villa Gualino, March
33 FD Telescope Four FD Eyes 6x4=24 Telescopes Shutter Corrector Ring Optical UV Filter Mirror Pixel Camera Light Collectors,440 PM Electronics Analog Chain, FADC 12 bit, 10 MSPS March 07 E.Menichetti - Villa Gualino, March
34 FD Telescope Aperture, UV Filter, Corrector Ring, Pixel Camera, Mirror March 07 E.Menichetti - Villa Gualino, March
35 FD Electronics Signal Formation Front-End Electronics March 07 E.Menichetti - Villa Gualino, March
36 FD Calibration Drum Diffuse, uniform camera illumination Central Laser Facility AUGER Test Beam 355 nm Steerable laser SD tank optical fiber March 07 E.Menichetti - Villa Gualino, March
37 FD Corrections Atmospheric Monitoring: Density, Transparency, Aerosols Several Gadgets: Horizontal Attenuation Monitor Balloon Radiosondes CLF LIDAR Phase Function Monitor Cerenkov subtraction Based on track geometry, iterative Unseen Energy Neutrinos, MCarlo: ~ EeV March 07 E.Menichetti - Villa Gualino, March
38 FD From Shower to Data FADC Traces Pixel signals CLF ~Uniform amplitude Pixel Signal EAS Longitudinal profile March 07 E.Menichetti - Villa Gualino, March E.Menichetti SIF 2006
39 FD Geometry, Energy, Profile SDP: Time fit..and its problems for 1-eye evts Abs. Calib. ~ 5 γ/adc count FY ~ 4.2 γ/m Electron Track But: New results expected soon AIRFLY (LNF, Argonne,..) FLASH (SLAC) σ Xmax ~ 30 g cm -2 March 07 E.Menichetti - Villa Gualino, March
40 Hybrid Reconstruction Typical SD SD+ FD FD Top Hybrid Not included in the sample March 07 E.Menichetti - Villa Gualino, March
41 Hybrid Performance From Laser Shots Effective Aperture March 07 E.Menichetti - Villa Gualino, March
42 Energy Calibration with Hybrids log 10 E FD (EeV) E Systematics Budget (projected) FD Fluorescence Yield 15% ( 8%) Abs/Rel Calibration 12% Atmosphere 11 % ( 6%) Other 12 % Total 25 % ( 17%) SD Detector calibration 10% S 38 (1000) 8 % Other 7 % log 10 S 38 (1000) Total 16 % Overall Energy Scale (Includes Hybrid Statistics) E dependent % Expected to to % March 07 E.Menichetti - Villa Gualino, March
43 Spectrum This Statistics: ~ ½ Year of Full Observatory (~7000 km 2 sr yr) (NB: AGASA pre-vulcano) Still investigating systematics (e.g.energy scale still uncertain) Preliminary: Data difficult to reconcile with AGASA (pre/post-vulcano) But: Wait for statistics, reduced systematics Energy: Systematics ~ ±30-50 %; Statistical Error ~15-10% Efficiency =100% above 3 EeV A few high energy events March 07 E.Menichetti - Villa Gualino, March
44 Anisotropies: Exposure, Rates Galactic Coordinates; E=1 5 EeV March 07 E.Menichetti - Villa Gualino, March
45 Anisotropies: AGASA, SUGAR AGASA Angular range: 20 Energy interval ( EeV) 2116 / ratio = 0.98 ± 0.02 ±0.0 (22% excess projection: 2634 evts, 10-σ effect) SUGAR Angular range 5 Energy interval ( EeV) 286 / ratio = 0.98 ± 0.06 ± 0. (85% excess projection: 536 evts, 14.5-σ effect) March 07 E.Menichetti - Villa Gualino, March
46 Next Step: The North Site March 07 E.Menichetti - Villa Gualino, March
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