PAMELAPAMELA SpaceSpace MissionMission FirstFirst ResultsResults inin CosmicCosmic RaysRays
Piergiorgio Picozza INFN & University of Rome “ Tor Vergata” , Italy
Virtual Institute of Astroparticle Physics
June 20, 2008 Robert L. Golden ANTIMATTERANTIMATTER
Antimatter Lumps Trapped in our Galaxy antiparticles Antimatter and Dark Matter Research
Wizard Collaboration -- BESS (93, 95, 97, 98, 2000) - MASS – 1,2 (89,91) - - Heat (94, 95, 2000)
--TrampSI (93) - IMAX (96)
-CAPRICE (94, 97, 98) - BESS LDF (2004, 2007)
- ATIC (2001, 2003, 2005)
- AMS-01 (98)
AntimatterAntimatter
“We must regard it rather an accident that the Earth and presumably the whole Solar System contains a preponderance of negative electrons and positive protons. It is quite possible that for some of the stars it is the other way about”
P. Dirac, Nobel lecture (1933) 4% 23% 73%
Signal (supersymmetry)…
… and background (GLAST AMS-02) + ISMCR +→ + + pppppp + + + CR pp ISM μπ→→→+ e 0 γγπ→→→ ee −+ Another possible scenario: KK Dark Matter Lightest Kaluza-Klein Particle (LKP): B(1) Bosonic Dark Matter: fermionic final states no longer helicity suppressed. e+e- final states directly produced.
As in the neutralino case there are 1-loop processes that produces monoenergetic γγin the final state. P
Secondary production (upper and lower limits) Simon et al. ApJ 499 (1998) 250.
from χχ Secondary annihilation production (Primary Bergström et production al. ApJ 526 m(c) = 964 (1999) 215 GeV) Ullio : astro- ph/9904086 AntiprotonAntiproton--ProtonProton RatioRatio
Potgieter at al. arXiv:0804.0220v1 [astro-ph]
WhatWhat dodo wewe needneed??
MeasurementsMeasurements atat higherhigher energiesenergies
BetterBetter knowledgeknowledge ofof backgroundbackground
HighHigh statisticsstatistics
ContinuousContinuous monitoringmonitoring ofof solarsolar modulationmodulation
LongLong DurationDuration FlightsFlights AntimatterAntimatter DarkDark MatterMatter
SpaceSpace MissionsMissions PAMELA BESS 15-06-2006 2007
AMS-02 2009
PEBS-DbarSUSY 2011-2013 GAPS 2013 GammaGamma SpaceSpace ExperimentsExperiments
AGILE 11-06-2008 23-04-2007 PAMELAPAMELA Payload for Antimatter Matter Exploration and Light Nuclei Astrophysics PAMELAPAMELA CollaborationCollaboration
Italy: Bari Florence Frascati Naples Rome Trieste CNR, Florence Russia:
Moscow St. Petersburg
Germany: Sweden: Siegen KTH, Stockholm Pamela as a Space Observatory at 1AU
Search for dark matter annihilation
Search for antihelium (primordial antimatter)
Search for new Matter in the Universe (Strangelets?) Study of cosmic-ray propagation
Study of solar physics and solar modulation
Study of terrestrial magnetosphere
Study of high energy electron spectrum (local sources?) - + e- p e p (He,...)
Trigger, ToF, dE/dx
- + Sign of charge, rigidity, dE/dx
Electron energy, dE/dx, lepton-hadron separation GF ~21.5 cm2sr Mass: 470 kg Size: 130x70x70 cm3 DesignDesign performanceperformance Energy range Antiproton flux 80 MeV - 190 GeV Positron flux 50 MeV – 270 GeV Electron/positron flux up to 2 TeV (from calorimeter)
Electron flux up to 400 GeV Proton flux up to 700 GeV Light nuclei (up to Z=6) up to 200 GeV/n He/Be/C: -8 Antinuclei search Sensitivity of O(10 ) in He-bar/He
• Unprecedented statistics and new energy range for cosmic ray physics • Simultaneous measurements of many species
ResursResurs--DK1DK1 satellitesatellite
Main task: multi-spectral remote sensing of earth’s surface Built by TsSKB Progress in Samara, Russia
Lifetime >3 years (assisted) Data transmitted to ground via high-speed radio downlink
PAMELA mounted inside a pressurized container
Mass: 6.7 tonnes Height: 7.4 m Solar array area: 36 m2 PAMELAPAMELA
LaunchLaunch 15/06/15/06/0606
16 Gigabytes trasmitted daily to Ground NTsOMZ Moscow OrbitOrbit CharacteristicsCharacteristics
350 km SAA
70ο
610 km • Low-earth elliptical orbit • 350 – 610 km • Quasi-polar (70o inclination) • Lifetime >3 years (assisted) PAMELA Orbit
Outer radiation belt Download @orbit 3754 – 15/02/2007 07:35:00 MWT
NP SP S1
S2 S3 95 min
Inner EQ EQ radiation belt (SSA)
orbit 3751 orbit 3752 orbit 3753 Flight data: 0.171 GV positron
Flight data: 0.169 GV electron Flight data: 0.632 GeV/c antiproton annihilation Flight data: 84 GeV/c interacting antiproton Flight data: 92 GeV/c positron Flight data: 14.7 GV Interacting nucleus (Z = 8) PAMELAPAMELA StatusStatus
TillTill 2nd2nd ofof MarchMarch 20082008 PAMELAPAMELA hashas collectedcollected ~~ 8.8TB8.8TB ofof data,data, correspondingcorresponding toto ~~ 10109 triggerstriggers AntiprotonAntiproton--ProtonProton RatioRatio
preliminary AntiprotonAntiproton--ProtonProton RatioRatio
preliminary Cirelli, Franceschini, Strumia
arXiv:0802.3378v2 [hep-ph] PamelaPamela PositronsPositrons
th TillTill AugustAugust 3030th aboutabout 2000020000 positronspositrons fromfrom 200200 MeVMeV upup toto 200200 GeVGeV havehave beenbeen analyzedanalyzed
MoreMore thanthan 1500015000 positronspositrons overover 11 GeVGeV
OtherOther eighteight monthsmonths datadata toto bebe analyzedanalyzed PositronPositron -- ElectronElectron ratioratio Pre lim in ary PAMELA PositronPositron -- ElectronElectron ratioratio
PositronPositron -- ElectronElectron ratioratio
Pre lim in ary PositronsPositrons withwith HEATHEAT PositronsPositrons withwith HEATHEAT && PAMELAPAMELA
Pre lim in ary ProblemsProblems
9 BackgroundBackground calculationcalculation
9 SolarSolar ModulationModulation atat lowlow energiesenergies
9 ChargeCharge--signsign dependencedependence ofof solarsolar modulationmodulation DiffusionDiffusion HaloHalo ModelModel
SecondariesSecondaries // primariesprimaries i.e. Boron/ Carbon to constrain propagation parameters D. Maurin, F. Donato R. Taillet and P.Salati F. Donato et.al, ApJ, 563, 172, ApJ, 555, 585, 2001 [astro-ph/0101231] 2001 [astro-ph/0103150] B/C Ratio Antiproton flux
Astrophysic B/C constraints
Nuclear cross sections!! PreliminaryPreliminary ResultsResults B/CB/C Pre lim in ary HeliumHelium andand HydrogenHydrogen IsotopesIsotopes
SecondarySecondary toto PrimaryPrimary ratiosratios
Fluxsr s) (p/cm^2
Kinetic Energy (GeV) Proton flux July 2006
Pre GalacticGalactic HH andand HeHe spectraspectra lim in ary
!!! SolarSolar PhysicsPhysics withwith PAMELAPAMELA
SolarSolar ModulationModulation ofof galacticgalactic cosmiccosmic raysrays
Continuous monitoring Pamela AMS-01 of solar activity Caprice / Mass /TS93 BESS
Study of charge sign dependent effects Asaoka Y. et al. 2002, Phys. Rev. Lett. 88, 051101), Bieber, J.W., et al. Physi- cal Review Letters, 84, 674, 1999. J. Clem et al. 30th ICRC
2007 AntiprotonAntiproton fluxesfluxes
A range of minimal (R-parity conserving) SUSY predictions of Galactic antiprotons spectrum, with neutralino masses 45-700 GeV Proton fluxes at TOA Annual Variation of P spectrum ) -1 GeV -1 s -1 sr -2 P flux (m
Kinetic Energy (GeV) p/p ratio
Time variation of p/p ratio at solar maximum Observed data by BESS Charge dependent model prediction(Bieber et al.) Bieber, J.W., et al. Phys. Rev. Letters, 84, 674, 1999. AntiprotonAntiproton--ProtonProton RatioRatio
preliminary Pre lim ProtonProton SpectraSpectra in ary !!! P/(cm^2 sr GeV s)
RED: JULY 2006 BLUE: AUGUST 2007 22 2 2 Primary spectrum =F Fis ( − )[(E+/ME φ) − M ]
July 2006 497±2 January 2007 481±2 Φ = August 2007 441±2
PositronPositron FractionFraction
Pre lim in ary
Mirko Boezio, INFN Trieste - Fermilab, 2008/05/02 Pamela
Clem at al. 30th ICRC 2007 ChargeCharge signsign dependencedependence ofof cosmiccosmic rayray modulationmodulation..
Two systematic deviations from reflection symmetry of the interplanetary magnetic field:
1) The Parker field has opposite magnetic polarity above and below the equator, but the spiral field lines themselves are mirror images of each other. This antisymmetry produces drift velocity fields that for positive particles converge on the heliospheric equator in the A+ state or diverge from it in A- state. Negatively charged particles behave in the opposite manner and the drift patterns interchange when the solar polarity diverge.
2) Systematic ordering of turbulent helicity can cause diffusion coefficients to depend directly on charge sign and polarity state. Bieber, J.W., et al. Phys. Rev. Letters, 84, 674, 1999. DecemberDecember 20062006 SolarSolar particleparticle eventsevents
Dec 13th largest CME since 2003, anomalous at sol min December 13th 2006 event
Preliminary! December 13th 2006 He differential spectrum
Preliminary! December 14th 2006 event X-rayX-ray
P,e-P,e-
Low energy tail of Dec 13th event
Arrival of event of Dec 14th MagneticMagneticFieldField
NeutronNeutronMonitorMonitor
Solar Quiet spectrum
BelowEndgalactic of eventspectrum: of Dec 14th Start of Forbush decrease
Decrease of primary spectrum
Arrival of magnetic cloud from CME of Dec 13th Shock 1774km/s (gopalswamy, 2007) Decrease of Neutron Monitor Flux
Preliminary! RadiationRadiation BeltsBelts
SouthSouth AtlanticAtlantic AnomalyAnomaly
SecondarySecondary productionproduction fromfrom CRCR interactioninteraction withwith atmosphereatmosphere PamelaPamela WorldWorld MapsMaps:: 350350 –– 650650 kmkm altalt
36 MeV p, 3.5 MeV e- PamelaPamela mapsmaps atat variousvarious altitudesaltitudes !!!! INARY PRELIM
Altitude scanning PrimaryPrimary andand AlbedoAlbedo (sub(sub--cutoffcutoff measurements)measurements) OtherOther ObjectivesObjectives
SearchSearch forfor thethe existenceexistence ofof AntimatterAntimatter inin thethe UniverseUniverse
PAMELA AMS AMS in Space
S ea e rc rs h ve fo ni r t U he he e f t xi o st in en g ce ori o e f Accelerators th an r ti fo Un h iv arc er e se S
The Big Bang origin of the Universe requires matter and antimatter to be equally abundant at the very hot beginning WhatWhat aboutabout heavyheavy antinuclei?antinuclei?
The discovery of one nucleus of antimatter (Z≥2) in the cosmic rays would have profound implications for both particle physics and astrophysics.
• For a Baryon Symmetric Universe Gamma rays limits put any domain of antimatter more than 100 Mpc away
(Steigman (1976) Ann Rev. Astr. Astrophys., 14, 339; Dudarerwicz and Wolfendale (1994) M.N.R.A. 268, 609, A.G. Cohen, A. De Rujula and S.L. Glashow, Astrophys. J. 495, 539, 1998) AntimatterAntimatter DirectDirect researchresearch
AntimatterAntimatter whichwhich hashas escapedescaped asas aa cosmiccosmic rayray fromfrom aa distantdistant antigalaxyantigalaxy Streitmatter, R. E., Nuovo Cimento, 19, 835 (1996)
AntimatterAntimatter fromfrom globularglobular clustersclusters ofof antistarsantistars inin ourour GalaxyGalaxy asas antistellarantistellar windwind oror antianti--supernovaesupernovae explosionexplosion K. M. Belotsky et al., Phys. Atom. Nucl. 63, 233 (2000), astro-ph/9807027 CosmicCosmic--rayray antimatterantimatter searchsearch
“We must regard it rather an accident that the Earth and presumably the whole Solar BESS combined (new) System contains a preponderance of negative electrons and positive protons. It is quite possible that for some of the stars expected it is the other way about”
P. Dirac, Nobel lecture (1933) HighHigh EnergyEnergy electronselectrons
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 (r≤300 pc) CALO SELF TRIGGER EVENT: 167*103 MIP RELEASED 279 MIP in S4 26 Neutrons in ND Search for New Matter in the Universe: An example is the search for “strangelets”.
There are six types of Quarks found in accelerators. All matter on Earth is made out of only two types of quarks. “Strangelets” are new types of matter composed of three types of quarks which should exist in the cosmos.
Carbon Nucleus Strangelet i. A stable, single “super nucleon” d n d u p u d s s u d d s with three types of d u d u s d u u u s quarks u u u s u s d d d uu u d d d d u d s ii. “Neutron” stars may u u d d u d u d u d d s u d d d d d be one big d u u d s u uu us u u strangelet d uu d d
AMS courtesy ConclusionConclusion
PAMELA is the first space experiment which is measuring the Antiprotons and Positrons to the high energies (> 150GeV) with an unprecedented statistical precision
PAMELA is setting a new lower limit for finding Antihelium
PAMELA is looking for Dark Matter candidates
PAMELA is providing measurements on elemental spectra and low mass isotopes with an unprecedented statistical precision and is helping to improve the understanding of particle propagation in the interstellar medium
PAMELA is able to measure the high energy tail of solar particles. THANKSTHANKS
http://http:// pamela.roma2.infn.itpamela.roma2.infn.it