Launch in orbit of the space experiment PAMELA and ground data results Roberta Sparvoli on behalf of the PAMELA Collaboration.

Launch in orbit of the Launch in orbit of the

space experimentspace experiment PAMELAPAMELA

and ground data and ground data resultsresults

Roberta SparvoliRoberta Sparvoli on behalf of the PAMELA Collaborationon behalf of the PAMELA Collaboration

R. Sparvoli - 9th ICATPP Conference - Villa Olmo - October 2005R. Sparvoli - 9th ICATPP Conference - Villa Olmo - October 2005

Outline of the talkOutline of the talk

Scientific goalsScientific goals Apparatus overview & satellite Apparatus overview & satellite Ground dataGround data Status of the missionStatus of the mission ConclusionsConclusions


Bari FlorenceFrascati

Italy:Italy:TriesteNaplesRome CNR, Florence

Moscow St. Petersburg

NMSU

GSFC

USA:USA:

Russia:Russia:

India:India:

Mumbai

Germany:Germany:Siegen

Sweden:Sweden:KTH, Stockholm

PAMELA CollaborationPAMELA Collaboration


PAMELA will:PAMELA will: Search for antimatterSearch for antimatter Search for dark matterSearch for dark matter Study cosmic-ray propagationStudy cosmic-ray propagation Study solar physics and solar Study solar physics and solar

modulationmodulation Study the electron spectrum (local Study the electron spectrum (local

sources?)sources?)

PAMELA SciencePAMELA Science


+ Long-term monitoring of the solar modulation of cosmic rays Energetic particles from the Sun (e+) High-energy particles in the Earth magnetosphere

PAMELA CapabilitiesPAMELA CapabilitiesPAMELA will explore:PAMELA will explore: Antiproton flux Antiproton flux 80 MeV - 190 GeV80 MeV - 190 GeV Positron fluxPositron flux 50 MeV – 270 GeV50 MeV – 270 GeV Electron flux Electron flux up to 400 GeVup to 400 GeV Proton flux Proton flux up to 700 GeVup to 700 GeV Electron/positron fluxElectron/positron fluxup to 2 TeVup to 2 TeV Light nuclei (up to Z=6) Light nuclei (up to Z=6) up to 200 GeV/nup to 200 GeV/n Light isotopes (D, Light isotopes (D, 33He) up to 1 GeV/nHe) up to 1 GeV/n Antinuclei search Antinuclei search (sensitivity better than 10 (sensitivity better than 10-7 -7 in in

He/He)He/He)


Cosmic-ray antiparticle Cosmic-ray antiparticle measurements: antiprotonsmeasurements: antiprotons

Secondary production (upper and lower limits)Simon et al.

Primary production from annihilation (m() = 964 GeV)

Secondary production (CAPRICE94-based)Bergström et al.

Unexplored Region

Black Holes

Dark matter

ExtragalacticPrimordial p

Dark matter

Propagation

PAMELA energy range

Charge dependentmodulation effects


Cosmic-ray antiparticle Cosmic-ray antiparticle measurements: positronsmeasurements: positrons

Unexplored Region

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 Propagation

Dark matter

PAMELA energy range


Cosmic-ray Cosmic-ray Antimatter SearchAntimatter Search


The Satellite Resurs-DK1The Satellite Resurs-DK1

Built by the space factory Built by the space factory TsSKB in Samara (Russia)TsSKB in Samara (Russia)

Soyuz-TM launcher from Soyuz-TM launcher from Bajkonur (also from TsSKB)Bajkonur (also from TsSKB)

PAMELA PAMELA mounted inside amounted inside a PPressuriressurizzed Containered Container, , attached to the satelliteattached to the satellite

Lifetime >3 yearsLifetime >3 years


Orbit characteristicsOrbit characteristics

quasi-polar (quasi-polar (70.4°70.4°))elliptical (elliptical (300÷600 km300÷600 km))

SAA


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-MansiiskKhanty-Mansiisk (Siberia, Russia). Not (Siberia, Russia). Not yet officially established.yet officially established.

Scheme of PAMELA control room in NTsOMZ


PAMELA prior delivery to Russia (March 2005)

The PAMELA apparatusThe PAMELA apparatus

AnticoincidenceShield

Shower Tail CatcherScintillator (see nexttalk V. Malvezzi)

TOF (see next talk S. Russo)

Magnetic Spectrometer

Calorimeter

Neutron Detector (see next talk V. Malvezzi)

PAMELA CPU (see next talkA. Basili)


The PAMELA apparatusThe PAMELA apparatus

GFGF ~20.5 cm ~20.5 cm22srsrMass: 470 kgMass: 470 kgSize: 120x40x45 Size: 120x40x45 cmcm33

Power Budget: 360 Power Budget: 360 WW

Calorimeter Performances:• p/e+ selection eff. 90%• p rejection factor 105

• e- rejection factor 104

Spatial Resolution • 2.8 μm bending view• 13.1 μm non-bending view

MDR from test beam data 1 TV

ND p/e separation capabilities >10 above 10 GeV/c, increasing with energy


Ground data sessionsGround data sessions

Number of files downlinked in Rome:Number of files downlinked in Rome:

311311 in aboutin about 480 hours480 hours of data takingof data taking

Number of files downlinked in Samara: Number of files downlinked in Samara:

113113 in aboutin about 140 hours140 hours of data takingof data taking

We had so far two main sessions of cosmic ray We had so far two main sessions of cosmic ray acquisitions on ground:acquisitions on ground:

RomeRome – Tor Vergata University clean – Tor Vergata University clean room: February/March 2005room: February/March 2005

SamaraSamara – Progress clean area: May 2005– Progress clean area: May 2005


Ground data performance Ground data performance analysisanalysis

The main task of the ground data acquisition is The main task of the ground data acquisition is the analysis of the the analysis of the detector performancedetector performance. .

The statistics collected allowed to make an The statistics collected allowed to make an accurate analysis of the performance of the single accurate analysis of the performance of the single PAMELA subdetectors, determining in some cases PAMELA subdetectors, determining in some cases sub-system sub-system resolutionsresolutions and and efficienciesefficiencies..

The comparison between Rome, Samara and The comparison between Rome, Samara and previous beam-test data allowed to study PAMELA previous beam-test data allowed to study PAMELA behavior behavior with timewith time, so to detect possible failures , so to detect possible failures due to ageing of some structures.due to ageing of some structures.


PAMELA EventPAMELA Event

Ground Muon:2.8 GV



Ground Hadron:6.6 GV



GF: 400 cm2

sr

CalorimeterSelf Trigger


Ground muon resultsGround muon results

Preliminary

Preliminary!

Preliminary!

Preliminary!

Final data ready by the end of 2005 !Final data ready by the end of 2005 !


Detectors tested at PS/SPS test facilities as prototypes and in FM configuration

SPS, July 2000

FMSPS, September 2003

Magnet/Tracker,CalorimeterSPS, July 2002

PAMELA StatusPAMELA Status


Detectors tested at PS/SPS test facilities as prototypes and in FM configurationPAMELA Mass&Thermal Model qualified, March-May 2003

PAMELA Mass&Thermal Model inside Pamela Pressurized

Container at TsSKB Samara/Russia



Detectors tested at PS/SPS test facilities as prototypes and in FM configurationPAMELA Mass&Termal Model qualified, March-May 2003

PAMELA Thermal Model passed thermal tests at TsSKB Thermal/Vacuum

Chamber



Detectors tested at PS/SPS test facilities as prototypes and in FM configurationPAMELA Mass&Thermal Model qualified, March-May 2003

PAMELA Technological Model completed and delivered to Russia,December 2003


PAMELA Technological Model inside the Transport

Container before delivery to Samara


PAMELA StatusPAMELA StatusDetectors tested at PS/SPS test facilities as prototypes and in FM configurationPAMELA Mass&Thermal Model qualified, March-May 2003PAMELA Technological Model completed and delivered to Russia,December 2003PAMELA Flight Model assembled in Rome TV clean room, 2004-2005

Assembling phases of PAMELA in Roma Tor Vergata clean

room



PAMELA Flight Model on the shaker in IABG

Full cycle of vibration/shock of the Flight Model passed at IABG/Munich, January 2005

Detectors tested at PS/SPS test facilities as prototypes and in FM configurationPAMELA Mass&Thermal Model qualified, March-May 2003PAMELA Technological Model completed and delivered to Russia,December 2003PAMELA Flight Model assembled in Rome TV clean room, 2004-2005



PAMELA Flight Model delivered to Russia, April 2005


Detectors tested at PS/SPS test facilities as prototypes and in FM configurationPAMELA Mass&Thermal Model qualified, March-May 2003PAMELA Technological Model completed and delivered to Russia,December 2003PAMELA Flight Model assembled in Rome TV clean room, 2004-2005 Antonov 72 in Genoa airportAntonov 72 in Genoa airport

PAMELA onboard during flightPAMELA onboard during flight






Reopening of PAMELA Flight Model in TsSKB


PAMELA StatusPAMELA StatusPAMELA StatusPAMELA Status

PAMELA Pressurized container tested with Resurs-DK1 Satellite, June 2005




Tests of PAMELA Pressurized Container tilting mechanism


PAMELA StatusPAMELA StatusPAMELA StatusPAMELA Status

Ongoing tests on Resurs-DK1 Satellite





Antennas of Resurs_DK1



Ongoing tests on Resurs-DK1 Satellite





Resurs_DK1 on the shaker


Integration in Bajkonur Integration in Bajkonur cosmodrome,cosmodrome,

December 2005December 2005


Conclusions IConclusions I PAMELA is the first space experiment which will PAMELA is the first space experiment which will

measure Antiprotons and Positrons to high energies (measure Antiprotons and Positrons to high energies (≥≥ 200GeV) with an unprecedented statistical precision;200GeV) with an unprecedented statistical precision;

PAMELA will set a new lower limit for finding Antihelium;PAMELA will set a new lower limit for finding Antihelium;

PAMELA will look for Dark Matter candidates;PAMELA will look for Dark Matter candidates;

PAMELA will provide measurements on elemental PAMELA will provide measurements on elemental spectra and low mass isotopes with an unprecedented spectra and low mass isotopes with an unprecedented statistical precision and will help to improve the statistical precision and will help to improve the understanding of particle propagation in the interstellar understanding of particle propagation in the interstellar medium;medium;

PAMELA will be able to measure the high energy tail of PAMELA will be able to measure the high energy tail of solar spectra and for the first time solar positrons.solar spectra and for the first time solar positrons.


Conclusions IIConclusions II Pamela has been delivered to Russia at the end of Pamela has been delivered to Russia at the end of

March 2005;March 2005;

PAMELA has collected ground cosmic-rays for PAMELA has collected ground cosmic-rays for various months at the laboratories of Rome Tor various months at the laboratories of Rome Tor Vergata and at the Samara TsSKB-Progress factory;Vergata and at the Samara TsSKB-Progress factory;

All detectors are performing as designed and All detectors are performing as designed and PAMELA seems able to achieve its scientific goals;PAMELA seems able to achieve its scientific goals;

Right now PAMELA is undergoing the integrations Right now PAMELA is undergoing the integrations tests with the Resurs-DK1 satellite in Samara;tests with the Resurs-DK1 satellite in Samara;

By mid November 2005 PAMELA will be delivered to By mid November 2005 PAMELA will be delivered to Bajkonur for the launch into orbit foreseen for Bajkonur for the launch into orbit foreseen for beginning 2006 !beginning 2006 !

Launch in orbit of the space experiment PAMELA and ground data results Roberta Sparvoli on behalf of the PAMELA Collaboration.

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