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PAMELA SPACE MISSIONPAMELA SPACE MISSION
ICHEP 2006 MOSCOW
Piergiorgio Picozza Pamela collaboration
INFN & University of Roma “Tor Vergata”
PAMELAPAMELA PPayload for ayload for AAntimatter ntimatter MMatter atter EExploration and xploration and LLight Nucleiight Nuclei
AAstrophysicsstrophysics
In orbit on June 15, 2006, on board of the In orbit on June 15, 2006, on board of the DK1 satellite by a Soyuz rocket from the DK1 satellite by a Soyuz rocket from the Bajkonour launch site.Bajkonour launch site.
From July 11 Pamela is in continuous data From July 11 Pamela is in continuous data taking modetaking mode
Bari Florence Frascati
Italy:TriesteNaples Rome CNR, Florence
Moscow St. Petersburg
Russia:
India:
Mumbay
Germany:Siegen
Sweden:KTH, Stockholm
PAMELA CollaborationPAMELA Collaboration
WiZardWiZard Russian Italian Missions Russian Italian Missions
PAMELA
Pamela Flight ModelPamela Flight Model
AnticoincidenceShield
TOF
First level trigger
Particle identification(up to 1GeV/c)
dE/dx
MAGNETIC SPECTROMETER
B=0.48T6 planes double sided Si strips 300 m thickSpatial resolution ~3m
MDR ~ 1400GV/c
Shower Tail CatcherScintillator
NEUTRON DETECTOR
36 3He counters in polyetilenmoderators to discriminate between very high energy electron and proton components
GF: 21.5 cm2 sr Mass: 470 kgSize: 130x70x70 cm3
Power Budget: 360W
IMAGING CALORIMETER :
44 Si layers intervealed with 22 W planes 16.3 X0 / 0.6 l0
e+/p and at level of 10-4 ~ 10-5
ep
On-ground muon resultsOn-ground muon results2005 acquisition of atmospheric particles during PAMELA test before delivering Check of spectrometer systematics with positive and negative muons
Preliminary results:- no efficiency correction- first-order alignment- no ETA p.f.a.
Preliminary!
Preliminary!
ParticleParticle Number (3 yrs)Number (3 yrs) Energy RangeEnergy Range
ProtonsProtons 3.103.1088 80 MeV – 700 GeV80 MeV – 700 GeV
AntiprotonsAntiprotons >3.10>3.1044 80 MeV – 190 GeV80 MeV – 190 GeV
ElectronsElectrons 6.106.1066 50 MeV – 2 TeV50 MeV – 2 TeV
PositronsPositrons >3.10>3.1055 50 MeV – 270 GeV50 MeV – 270 GeV
HeHe 4.104.1077 80 MeV/n – 700 GeV/n80 MeV/n – 700 GeV/n
BeBe 4.104.1044 80 MeV/n – 700 GeV/n80 MeV/n – 700 GeV/n
CC 4.104.1055 80 MeV/n – 700 GeV/n80 MeV/n – 700 GeV/n
Antihelium LimitAntihelium Limit 5.105.10-8-8 80 MeV/n – 30 GeV/n80 MeV/n – 30 GeV/n
PAMELA capabilities in 3 y. of operationPAMELA capabilities in 3 y. of operation
Resurs-DK1 Spacecraft TsSKB-Progress
Ground Station(s)Ground Station(s) Main Station:Main Station: Research Centre for Earth Operative Research Centre for Earth Operative
Monitoring Monitoring “NtsOMZ”“NtsOMZ” (Moscow, Russia); (Moscow, Russia);
Main antenna in NTsOMZ
Additional Station:Additional Station: Khanty-MansiskyKhanty-Mansisky (Siberia, Russia). Not (Siberia, Russia). Not yet officially established.yet officially established.
Scheme of PAMELA control room in NTsOMZ
Flight data: 2.8 GV electron
PAMELA eventPAMELA event
Flight data: 4.2 GV electron
PAMELA eventPAMELA event
Flight data: 9.7 GV non-interactingHelium Nucleus
PAMELA eventPAMELA event
Flight data: 13 GV Interacting
Helium Nucleus
PAMELA eventPAMELA event
Flight data: 14.4 GV non-interacting proton
PAMELA eventPAMELA event
Flight data: 36 GV interacting proton
Flight data: ~500 GV/c electron
e- e+
p
Topological development of the shower variable versus rigidity [GV]
ee--
ee++
pppp
e- e+ p
He
dE/dx in the calorimeter versus rigidity [GV]
RR
dE/dx
Orbit characteristicsOrbit characteristics
quasi-polar (quasi-polar (70°70°))elliptical (elliptical (300÷600 km300÷600 km))3-years-long mission3-years-long mission
SAA
Passage in South Atlantic Anomaly
Neutron counts
Trigger RateTrigger Rate
Example: Trigger rate with 3 different trigger configurations
The Science of PamelaThe Science of Pamela
Cosmic-ray Cosmic-ray Antimatter Antimatter
SearchSearch
PAMELA 2006-2009
Antiproton MeasurementsAntiproton Measurements
Distortion on the secondary antiproton flux induced by an Extragalactic Distortion on the secondary antiproton flux induced by an Extragalactic Antimatter and Black Hole evaporation componentsAntimatter and Black Hole evaporation components
•Background from normal secondary production
•Mass91 data from XXVI ICRC, OG.1.1.21 , 1999
•Caprice94 data from ApJ , 487, 415, 1997
•Caprice98 data from ApJ Letters 534, L177, 2000
Extragalactic Antimatter
Black Hole evaporation
Dark MatterDark Matter
What do we espect from What do we espect from Pamela?Pamela?
a) CDM neutralinos annihilation in the Galactic halo in minimal SUSY
b) In R-parity- violating SUSY
NEUTRALINO ANNIHILATIONNEUTRALINO ANNIHILATION
Search of structures in antiproton spectrumSearch of structures in antiproton spectrum
Secondary production (upper and lower limits)Simon et al.
Secondary production (CAPRICE94-based)Bergström et al.
Primary production from annihilation (m() = ~ 1 TeV)
( astro-ph 9904086)
PAMELA:PAMELA:
Cosmic-Ray Antiparticle Cosmic-Ray Antiparticle Measurements: Measurements:
AntiprotonsAntiprotons
fd: Clumpiness factors needed to disentangle a neutralino induced component in the antiproton flux
MSSM
A.Lionetto, A.Morselli, V.Zdravkovic
JCAP09(2005)010 [astro-ph/0502406]
cMSSM
see Aldo Morselli talk
cMSSM A0 = 0, > 0, mt =174 GeV
see Aldo Morselli talk
Distortion of the secondary positron fraction induced by a signal from a Distortion of the secondary positron fraction induced by a signal from a heavy neutralino.heavy neutralino.
Baltz & EdsjöPhys.Rev. D59 (1999)astro-ph 9808243
Positron with HEATPositron with HEAT
Cosmic-ray antiparticle measurements:Cosmic-ray antiparticle measurements:positronspositrons
Secondary production ‘Leaky box model’ (Protheroe 1982)
Primary production from
annihilation (m() = 336 GeV)
Secondary production ‘Moskalenko + Strong model’ (1998) without reacceleration
Charge dependentmodulation effects
PAMELA energy range
Primary and Secondary Primary and Secondary SpectraSpectra
Unambiguous interpretation of exotic matter Unambiguous interpretation of exotic matter signature requires a clear understanding of signature requires a clear understanding of the secondary spectra and their sources.the secondary spectra and their sources.
Primary cosmic ray spectra as a powerful tool Primary cosmic ray spectra as a powerful tool for quantify the source of atmospheric for quantify the source of atmospheric neutrino anomaly.neutrino anomaly.
Secondary to Primary ratiosSecondary to Primary ratios
Helium and Hydrogen IsotopesHelium and Hydrogen Isotopes
Protons Protons Helium Helium
Concomitant GoalsConcomitant Goals
Near electrons sourcesNear electrons sources
Solar Flare Particle SpectraSolar Flare Particle Spectra
Charge-Sign Dependent Solar Charge-Sign Dependent Solar Modulation Modulation
New Radiation BeltsNew Radiation Belts
High Energy electronsHigh Energy electrons
The study of primary electrons is especially important because they give information on the nearest sources of cosmic rays
Electrons with energy above 100 MeV rapidly loss their energy due to synchrotron radiation and inverse Compton processes
The discovery of primary electrons with energy above 1012 eV will evidence the existence of cosmic ray sources in the nearby interstellar space (r300 pc)
Charge-Sign Dependent Solar Charge-Sign Dependent Solar ModulationModulation
Osservational evidence that the negative Osservational evidence that the negative charge component of galactic cosmic rays is charge component of galactic cosmic rays is modulated in the heliosphere differently than modulated in the heliosphere differently than the positive onethe positive one
.. Modification and modulation of Galactic Modification and modulation of Galactic
Cosmic Ray spectra in the heliosphere Cosmic Ray spectra in the heliosphere complicate the interpretation of the exotic complicate the interpretation of the exotic matter results at low energy.matter results at low energy.
Measurements of the abundances of species Measurements of the abundances of species with the same mass but different charge sign with the same mass but different charge sign in Ain A++ and A and A-- of the solar cycle. of the solar cycle.
– – High energy from ~ 1 GeV to ~ 10 GeVHigh energy from ~ 1 GeV to ~ 10 GeV
– Content of e+, e-, p, 3He– Content of e+, e-, p, 3He
– e+ over e- dominance– e+ over e- dominance
– Low L- shell – Low L- shell low altitudelow altitude
– Life time O(seconds)– Life time O(seconds)
Secondary production from CR Secondary production from CR interactioninteraction
with atmospherewith atmosphere
High Energy Radiation Belts
≈
PAMELA will be able to measure electrons at very high energy to discover sources near the solar system
Earliest example of the interplay between Earliest example of the interplay between particles physics and cosmologyparticles physics and cosmology
““We must regard it rather an accident that the We must regard it rather an accident that the Earth and presumably the whole Solar System Earth and presumably the whole Solar System contains a preponderance of negative electrons contains a preponderance of negative electrons and positive protons. It is quite possible that for and positive protons. It is quite possible that for some of the stars it is the other way about”some of the stars it is the other way about”
Dirac Nobel Speech (1933)Dirac Nobel Speech (1933)
wizard.roma2.infn.it/pamelawizard.roma2.infn.it/pamela