First results of the PAMELA Space Experiment. F.S. Cafagna, INFN Bari on behalf of the PAMELA Collaboration
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1 First results of the PAMELA Space Experiment F.S. Cafagna, INFN Bari on behalf of the PAMELA Collaboration
2 PAMELA Collaboration Italy: Bari Florence Frascati Naples Rome Trieste CNR, Florence Russia: Moscow St. Petersburg Germany: Sweden: F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb Siegen KTH, Stockholm
3 PAMELA Science PAMELA as a Space 1AU F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
4 PAMELA Science F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
5 PAMELA Science F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
6 PAMELA Science F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
7 Why Anti(particle)matter matters? Earth F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
8 Why Anti(particle)matter matters? Earth F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
9 Why Anti(particle)matter matters? Earth F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
10 Why Anti(particle)matter matters? Earth F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
11 Why Anti(particle)matter matters? F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
12 PAMELA detectors Main requirements high-sensitivity antiparticle identification and precise momentum measure GF: 21.5 cm 2 sr Mass: 470 kg Size: 130x70x70 cm 3 Power Budget: 360W F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
13 PAMELA detectors Main requirements high-sensitivity antiparticle identification and precise momentum measure Time-Of-Flight plastic scintillators + PMT -Trigger; -Albedo rejection; -Mass identification up to 1 GeV; -Charge identification from de/dx. + - Electromagnetic calorimeter W/Si sampling (16.3 X 0, 0.6λ I ) Discrimination e + / p, pbar/e - (shower topology) Direct E measurement for e - GF: 21.5 cm 2 sr Mass: 470 kg Size: 130x70x70 cm 3 Power Budget: 360W Neutron detector plastic scintillators + PMT: -High-energy e/h discrimination Spectrometer microstrip silicon tracking system + permanent magnet Magnetic rigidity (R = pc/ze) Charge sign Charge value from de/dx F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
14 Design Performance Antiprotons Positrons Electrons Protons Electrons+positrons Light Nuclei (He/Be/C) 80 MeV GeV 50 MeV 270 GeV up to 400 GeV up to 700 GeV up to 2 TeV (calorimeter alone) up to 200 GeV/n AntiNuclei search sensitivity of 3x10-8 in He/He Simultaneous measurement of many cosmic-ray species New energy range Unprecedented statistics F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
15 PAMELA: the integration F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
16 The Resurs DK-1 spacecraft Mass: 6.7 tons Height: 7.4 m Solar array area: 36 m 2 PAMELA inside a pressurized container Moved from parking to data-taking position few times/year Multi-spectral remote sensing of earth s surface near-real-time high-quality images Built by the Space factory TsSKB Progress in Samara (Russia) Operational orbit parameters: inclination ~70 o altitude ~ km (elliptical) Active life >3 years Data transmitted via Very highspeed Radio Link (VRL) F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
17 PAMELA: in the satellite & launch Launch from Baikonur: June 15th 2006, 0800 UTC. Power On: June 21 st 2006, 0300 UTC. Detectors operated as expected after launch PAMELA in continuous data-taking mode since commissioning phase ended on July 11 th 2006 ~600 days of data taking (~73% livetime) ~10 TByte of raw data downlinked >10 9 triggers recorded and under analysis F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
18 Antiproton:spillover -1 Z +1 p (+ e + ) p Preliminary e - (+ p-bar) spillover p p-bar Deflection: = 1/R 5 GV 1 GV The main difficulty for the antiproton measurement is the spillover proton bk. At high energy due to the finite deflection resolution of the spectrometer F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
19 High-energy antiproton selection Preliminary R < MDR/10 p-bar spillover p p MDR = 1/s h (evaluated event-by-event by the fitting routine) 10 GV 50 GV MDR depends on: number and distribution of fitted points along the trajectory spatial resolution of the single position measurements magnetic field intensity along the trajectory F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
20 Antiproton Selection e - e + p α p GV -1 e - e + p p GV -1 p p F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb GV -1
21 Antiproton to Proton Ratio Astro-ph F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
22 Antiproton to Proton Ratio Astro-ph F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
23 Positron selection with calorimeter Z=-1 e - Fraction of charge released along the calorimeter track p-bar (non-int) p-bar (int) Z=+1 plan es LEFT HIT RIGHT p (non-int) strips p (int) (e + ) 0.6 R M Rigidity: GV F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
24 Positron selection with calorimeter Z=-1 e - Fraction of charge released along the calorimeter track Z=+1 p-bar Constrains on: Energy momentum match Shower startingpoint Longitudinal profile e + p Rigidity: GV F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
25 Positron selection with calorimeter Fraction of charge released along the calorimeter track e - e + Constrains on: Energy momentum match Shower starting-point Longitudinal profile p p, d Rigidity: GV F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
26 Positron selection with calorimeter Z=-1 e - Fraction of charge released along the calorimeter track Z=+1 p e + Constrains on: Energy momentum match Shower starting-point Longitudinal profile Cross check: Simulation Tracker de/dx Neutron Detector Preliminary Rigidity: GV F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
27 The pre-sampler method The electromagnetic calorimeter Characteristics: 44 Si layers (X/Y) +22 W planes 16.3 X o / 0.6 l channels Dynamic range 1400 mip Self-trigger mode (> 300 GeV GF~600 cm 2 sr) PROTON SELECTION 2 W planes: 1.5 X 0 20 W planes: 15 X 0 F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
28 The pre-sampler method The electromagnetic calorimeter Characteristics: 44 Si layers (X/Y) +22 W planes 16.3 X o / 0.6 l channels Dynamic range 1400 mip Self-trigger mode (> 300 GeV GF~600 cm 2 sr) POSITRON SELECTION 20 W planes: 15 X 0 2 W planes: 1.5 X 0 F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
29 e + background estimation from data Fraction of charge released along the calorimeter track Constrains on: Energy momentum match Shower starting-point presampler p e - p e + Rigidity: GV F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
30 Positron to Electron Fraction Astro-ph End 2007: ~ e + >1.5GV ~2 000 e+> 5 GeV F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
31 Positron to Electron Fraction Pulsar Component Yüksel et al. 08 Pulsar Component Atoyan et al. 95 KKDM (mass 300 GeV) Hooper & Profumo 07 Pulsar Component Zhang & Cheng 01 Secondary production F.S. Cafagna, XLIV Recontres Moskalenko De & Moriond, Strong 98 La Thuille 7th Feb
32 DM? PAMELA ability of measuring both proton and electron charge ration, make it possible to put several constrains to the models M. Cirelli, M. Kadastik, M. Raidal, A. Strumia arxiv: v3 F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
33 See you at PAMELA Physics Workshop PAMELA Physics Workshop Villa Mondragone, Monte Porzio Catone (Rome) May THANKS!!!! F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
34 Conclusions PAMELA is a permanent cosmic ray space laboratory. PAMELA is the first space experiment which is measuring the antiproton and positron cosmic-ray components to the high energies (10 2 GeV) with an unprecedented statistical precision. More exciting results will come in the next future! Stay tuned for fluxes... THANKS!!!! F.S. Cafagna, XLIV Recontres De Moriond, La Thuille 7th Feb
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