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