Results from PAMELA Mirko Boezio INFN Trieste, Italy On behalf of the PAMELA collaboration Indirect...
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![Page 1: Results from PAMELA Mirko Boezio INFN Trieste, Italy On behalf of the PAMELA collaboration Indirect and Direct Detection of Dark Matter February 7 th 2011.](https://reader033.fdocuments.net/reader033/viewer/2022042821/56649d635503460f94a45ad3/html5/thumbnails/1.jpg)
Results from PAMELA
Mirko BoezioINFN Trieste, Italy
On behalf of the PAMELA collaborationIndirect and Direct Detection of Dark Matter
February 7th 2011
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Isotopic composition
[ACE]Solar Modulation
[PAMELA,ULYSSES
] AntimatterAntimatter
Dark MatterDark Matter[BESS, PAMELA, AMS]
Elemental Composition
[CREAM, ATIC, TRACER, NUCLEON,CALET, GAMMA-400?]
Extreme Energy CR[AUGER, EUSO, TUS/KLYPVE, OWL??]
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PAMELAPAMELAPPayload for ayload for AAntimatter ntimatter MMatter atter EExploration xploration
and and LLight Nucleiight Nuclei AAstrophysicsstrophysics
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PAMELA CollaborationPAMELA Collaboration
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PAMELA InstrumentPAMELA Instrument
GF ~21.5 cmGF ~21.5 cm2srsr Mass: 470 kg Mass: 470 kg
Size: 130x70x70 cmSize: 130x70x70 cm3
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Mirko Boezio, IDDDM, Aspen, 2011/02/07
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Design Performance Energy range
• Antiprotons 80 MeV - 190 GeV
• Positrons 50 MeV – 300 GeV
• Electrons up to 800 GeV• Protons up to 1 TeV
• Helium up to 400 GeV/n
• Electrons+positrons up to 2 TeV ( by calorimeter)
• Light Nuclei (Li/Be/B/C) up to 200 GeV/n • AntiNuclei search sensitivity of 3x10-8 in He/He
Mirko Boezio, IDDDM, Aspen, 2011/02/07
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PAMELA
Launch15/06/06
16 Gigabytes trasmitted daily to GroundNTsOMZ Moscow
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OrbitOrbit Characteristics Characteristics
km
km
SAA
• Low-earth elliptical orbit
• 350 – 610 km
• Quasi-polar (70o inclination)
• SAA crossed
Mirko Boezio, IDDDM, Aspen, 2011/02/07
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Download @orbit 3754 – 15/02/2007 07:35:00 MWT
S1 S2 S3
orbit 3752 orbit 3753orbit 3751
NP SP
EQ EQ
95 min
Outer radiation belt
Inner radiation belt
(SSA)
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Subcutoff particlesSubcutoff particles
Mirko Boezio, IDDDM, Aspen, 2011/02/07
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Main antenna in NTsOMZ
Launch from Baikonur June 15th 2006, 0800 UTC.
‘First light’ June 21st 2006, 0300 UTC.
• Detectors operated as expected after launch• Different trigger and hardware configurations evaluated
PAMELA in continuous data-taking mode sincecommissioning phase ended on July 11th 2006
Trigger rate* ~25HzFraction of live time* ~ 75%Event size (compressed mode) ~5kB 25 Hz x 5 kB/ev ~ 10 GB/day(*outside radiation belts)
Till ~now:~1400 days of data taking~20 TByte of raw data downlinked>2x109 triggers recorded and analyzed
PAMELA milestones
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Scientific goalsScientific goalsScientific goalsScientific goals• Search for dark matter annihilation
• Search for antihelium (primordial antimatter)• Search for new Matter in the Universe
(Strangelets?)
• Study of cosmic-ray propagation (light nuclei and isotopes)
• Study of electron spectrum (local sources?)
• Study solar physics and solar modulation• Study terrestrial magnetosphere
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Dark MatterDark Matter
Mirko Boezio, IDDDM, Aspen, 2011/02/07
Indirect Detection
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DM annihilationsDM particles are stable. They can annihilate in pairs.
Primary annihilation channels Decay Final states
σσa= <= <σσv>v>
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Particle ID with PAMELAParticle ID with PAMELA
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Flight data: 0.169 GV electron
Flight data: 0.171 GV positron
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Flight data: 0.763 GeV/cantiproton annihilation
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Bending in spectrometer: sign of chargeIonisation energy loss (dE/dx): magnitude of charge
Interaction pattern in calorimeter: electron-like or proton-like, electron energy
Time-of-flight: trigger, albedo rejection, mass determination (up to 1 GeV)
Positron(NB: p/e+ ~103-
4)
Antiproton (NB: e-/p ~ 102)
Antiproton / Positron Antiproton / Positron Identification Identification
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Flight data: 14.7 GVInteracting nucleus
(Z = 8)
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Antiproton to proton ratio Antiproton to proton ratio (0.06 GeV - 180 GeV)(0.06 GeV - 180 GeV)
Donato et al. (PRL 102 (2009) 071301)
Simon et al. (ApJ 499 (1998) 250) Ptuskin et al. (ApJ 642 (2006) 902)
PRL 102, 051101 (2009) and PRL. 105, 121101 (2010)
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Antiproton FluxAntiproton Flux (0.06 GeV - 180 GeV)(0.06 GeV - 180 GeV)
Donato et al. (ApJ 563 (2001) 172)
Ptuskin et al. (ApJ 642 (2006) 902)
PRL. 105, 121101 (2010)
Systematics errors included
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Antiprotons inside SAAGalactic AntiprotonsAntiprotons below cutoff at equator
Galactic antiprotons
PAMELA trapped PAMELA trapped antiprotonsantiprotons
Preliminary
Mirko Boezio, IDDDM, Aspen, 2011/02/07
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Positron to Electron Positron to Electron FractionFraction
Secondary production Moskalenko & Strong 98
Adriani et al, Astropart. Phys. 34 (2010) 1 arXiv:1001.3522 [astro-ph.HE]
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But antiprotons in CRs are in agreement with secondary production
Uncertainties on:• Secondary production (primary fluxes, cross section)• Propagation models• Electron spectrum
A Challenging Puzzle for CR PhysicsA Challenging Puzzle for CR Physics
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A Challenging Puzzle for CR PhysicsA Challenging Puzzle for CR Physics
P.Blasi, PRL 103 (2009) 051104; arXiv:0903.2794Positrons (and electrons) produced as secondaries in the sources (e.g. SNR) where CRs are accelerated.
I. Cholis et al., Phys. Rev. D 80 (2009) 123518; arXiv:0811.3641v1
Contribution from DM annihilation.
D. Hooper, P. Blasi, and P. Serpico, JCAP 0901:025,2009; arXiv:0810.1527 Contribution from diffuse mature &nearby young pulsars.
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G. Kane, R. Lu, and S. Watson, Phys.Lett.B681, 151 (2009); arXiv:0906.4765v3
A Challenging Puzzle for CR PhysicsA Challenging Puzzle for CR Physics
T. Delahaye et al., A&A 501, 821(2009); arXiv: 0809.5268v3
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Cosmic Ray SpectraCosmic Ray Spectra
Cosmic-Ray Acceleration and Propagation in the Galaxy
Mirko Boezio, IDDDM, Aspen, 2011/02/07
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Diffusion Halo ModelDiffusion Halo Model
Mirko Boezio, IDDDM, Aspen, 2011/02/07
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PAMELA
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Proton and Helium Nuclei Proton and Helium Nuclei SpectraSpectra
Mirko Boezio, IDDDM, Aspen, 2011/02/07
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Proton and Helium Nuclei Proton and Helium Nuclei SpectraSpectra
GALPROP
Mirko Boezio, IDDDM, Aspen, 2011/02/07
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Proton and Helium Nuclei Proton and Helium Nuclei SpectraSpectra
Mirko Boezio, IDDDM, Aspen, 2011/02/07
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Boron and Carbon nuclei Boron and Carbon nuclei SpectraSpectraCarbon Boron
Mirko Boezio, IDDDM, Aspen, 2011/02/07
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0.9 GV < R < 1 GV
p
d
H isotopes separationH isotopes separation
Mirko Boezio, IDDDM, Aspen, 2011/02/07
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Positrons detectionWhere do positrons come from?
Mostly locally within 1 Kpc, due to the energy losses by Synchrotron Radiation and Inverse Compton
Typical lifetime
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PAMELA electron (ePAMELA electron (e--) ) spectrumspectrum
e+ + e-
e-
Mirko Boezio, IDDDM, Aspen, 2011/02/07
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PAMELA electron (ePAMELA electron (e--) ) spectrumspectrum
Preliminary
Tracker based
Calorimeter based
Mirko Boezio, IDDDM, Aspen, 2011/02/07
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Theoretical uncertainties on Theoretical uncertainties on “standard” positron fraction“standard” positron fraction
T. Delahaye et al., arXiv: 0809.5268v3
γ = 3.54 γ = 3.34
Flux=A • E-
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PAMELA electron (ePAMELA electron (e--) ) spectrumspectrum
Flux=A • E-
= 3.18 ±0.05GALPROP
prediction from e- flux
Mirko Boezio, IDDDM, Aspen, 2011/02/07
“New Primary Contribution”
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Independently to the fit of the electron spectra, we also perform a χ2
comparison between the expected positron fraction from GALPROP simulation and PAMELA measurement of the positron fraction.
Confidence level, in parameter space (2;ϕ0) obtained from a fit of the electron spectra (red) and of the positron fraction (green). Cruces show the best-fit combination.
Interestingly, the best fit value for the two independent fit are very similar.
Preliminary
positron fraction
electron spectrum
Fit of electron spectrumFit of electron spectrum
90%
95%
99%
Mirko Boezio, IDDDM, Aspen, 2011/02/07
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Solar ModulationSolar Modulation
Mirko Boezio, IDDDM, Aspen, 2011/02/07
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Positron to Electron Positron to Electron FractionFraction
Secondary production Moskalenko & Strong 98
Adriani et al, Astropart. Phys. 34 (2010) 1 arXiv:1001.3522 [astro-ph.HE]
Solar Modulation?
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Solar Modulation of Galactic Solar Modulation of Galactic Cosmic RaysCosmic Rays
Courtesy of M. Potgieter
PAMELAPAMELA
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Preliminar
y
Time Dependence of PAMELA Proton Time Dependence of PAMELA Proton FluxFlux
Mirko Boezio, IDDDM, Aspen, 2011/02/07
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Preliminar
y
Time Dependence of PAMELA Proton Time Dependence of PAMELA Proton FluxFlux
Mirko Boezio, IDDDM, Aspen, 2011/02/07
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Preliminar
y
Time Dependence of PAMELA Electron Time Dependence of PAMELA Electron (e(e--) Flux) Flux
Mirko Boezio, IDDDM, Aspen, 2011/02/07
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Preliminar
y
Time Dependence of PAMELA Electron Time Dependence of PAMELA Electron (e(e--) Flux) Flux
Mirko Boezio, IDDDM, Aspen, 2011/02/07
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Flux variation as a function of time for rigidities between 0.72 and 1.04 GV
Time DependenceTime Dependence
Preliminar
y
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Increase of the flux measured by PAMELA from July 2006 to December 2008
Time DependenceTime Dependence
Preliminar
y
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U.W. Langner, M.S. Potgieter, Advances in Space Research 34 (2004).
PAMELA Electron to Positron Ratio and Theoretical PAMELA Electron to Positron Ratio and Theoretical ModelsModels
Preliminary
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Summary PAMELA ResultsSummary PAMELA Results
Mirko Boezio, IDDDM, Aspen, 2011/02/07
PAMELA Data
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SummarySummary• PAMELA has been in orbit and studying cosmic rays for ~4.5 years. >109 triggers registered and >19 TB of data has been down-linked.
• Antiproton-to-proton flux ratio and antiproton energy spectrum (~100 MeV - ~200 GeV) show no significant deviations from secondary production expectations. • High energy positron fraction (>10 GeV) increases significantly (and unexpectedly!) with energy. Primary source?
•The proton and helium nuclei spectra have been measured up to 1.2 TV. The observations challenge the current paradigm of cosmic ray acceleration and propagation.
• The e- spectrum up to 600 GeV shows spectral features that may point to additional components.
• Analysis ongoing to finalize the antiparticle measurements (positron flux, positron fraction), continuous study of solar modulation effects at low energy.
• Waiting for AMS to compare contemporary measurements.Mirko Boezio, IDDDM, Aspen, 2011/02/07
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Taiwan
CSISTNCUAcademia SinicaNSPO
KoreaIHEP
HelsinkiTurku
Aarhus
Ciemat-Madrid
LIP-Lisbon
MITYaleJohns HopkinsMarylandFlorida
A&MMexico
BolognaMilanoPerugiaPisaRomaSiena
AnnecyGrenobleMontpellier
IEE, IHEP
Jiao Tong UniversitySoutheast University
ESANIKHEF
NLR, Amsterdam
ETH-ZurichGeneva Univ.
Kurchatov Inst.Inst. of Theor. & Experimental Physics
Moscow State Univercity
Achen I & IIIKarlsruheMunich
Bucharest
AMS-02 on ISSIn Orbit April 2011
TRD
RICH
VacuumCase
Tracker
MA
GN
ET
He V
essel
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The Completed AMS Detector on ISSTransition Radiation
Detector (TRD)
Silicon Tracker
Electromagnetic Calorimeter (ECAL)
Magnet
Ring Image Cerenkov Counter (RICH)
Time of Flight Detector (TOF)
Size: 3m x 3m x 3mWeight: 7 tons
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AMS-02 new AMS-02 new configurationconfiguration
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AMS S.C. Magnet:MDR 2.18 TV
AMS Perm. Magnet:MDR 2.14 TV
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AMS Capability Space Part AMS Capability Space Part 20062006
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Mirko Boezio, IDDDM, Aspen, 2011/02/07