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![Page 1: The PAMELA experiment: looking for antiparticles in Cosmic Rays Oscar Adriani University of Florence and INFN Florence Waseda, 14 January 2009.](https://reader035.fdocuments.net/reader035/viewer/2022062309/5697bfda1a28abf838cafdee/html5/thumbnails/1.jpg)
The PAMELA experiment:looking for
antiparticles in Cosmic Rays
Oscar AdrianiUniversity of Florence
and INFN Florence
Waseda, 14 January 2009
![Page 2: The PAMELA experiment: looking for antiparticles in Cosmic Rays Oscar Adriani University of Florence and INFN Florence Waseda, 14 January 2009.](https://reader035.fdocuments.net/reader035/viewer/2022062309/5697bfda1a28abf838cafdee/html5/thumbnails/2.jpg)
Oscar Adriani Waseda, January 14th, 2009
Outline
• The PAMELA experiment: short review• Results on cosmic-ray antimatter abundance:– Antiprotons– Positrons
• Other results:– Cosmic-ray galactic light nuclei (primaries & secondaries)
– Solar physics– Terrestrial physics
• Conclusions
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Oscar Adriani Waseda, January 14th, 2009
Moscow St. Petersburg
Russia
SwedenKTH, Stockholm
GermanySiegen
ItalyBari Florence Frascati TriesteNaples Rome CNR, Florence
Tha PAMELA collaboration
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Oscar Adriani Waseda, January 14th, 2009
PAMELAPayload for Antimatter/Matter Exploration and
Light-nuclei Astrophysics
Direct detection of CRs in space Main focus on antimatter component
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Oscar Adriani Waseda, January 14th, 2009
First historical measurements of p-bar/p ratio
Anti-nucleosyntesis
WIMP dark-matter
annihilation in the galactic
halo
Background:CR interaction with ISMCR + ISM p-bar + …
Evaporation of primordial black holes
Why CR antimatter?
![Page 6: The PAMELA experiment: looking for antiparticles in Cosmic Rays Oscar Adriani University of Florence and INFN Florence Waseda, 14 January 2009.](https://reader035.fdocuments.net/reader035/viewer/2022062309/5697bfda1a28abf838cafdee/html5/thumbnails/6.jpg)
Oscar Adriani Waseda, January 14th, 2009
Cosmic-ray Antimatter from Dark Matter annihilationAnnihilation of relic Weakly Interacting Massive Particles (WIMPs) gravitationally
confined in the galactic halo
Distortion of antiproton and positron spectra from purely secondary production
• A plausible dark matter candidate isneutralino (), the lightest SUSYParticle (LSP).Most likely processes:• qq hadrons anti-p, e+,… • W+W-,Z0Z0,… e+,…
positron peak Ee+~M/2 positron continuum Ee+~M/20
• Another possible candidate is the lightest Kalusa-Klein Particle (LKP): B(1)
Fermionic final states no longer suppressed:
• B(1)B(1) e+e-
direct dicay positron peak Ee+ ~ MB(1)
p-bar, e+
You are here Milky Way
Halo
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Oscar Adriani Waseda, January 14th, 2009
CR antimatter
Antiprotons Positrons
CR + ISM ± + x ± + x e± + x CR + ISM 0 + x e±
• Propagation dominated by energy losses (inverse Compton & synchrotron radiation)• Local origin (@100GeV 90% from <2kpc)
___ Moskalenko & Strong 1998 Positron excess?
Charge-dependent solar modulation
Solar polarity reversal 1999/2000
Asaoka Y. Et al. 2002
¯
+
CR + ISM p-bar + …•Propagation dominated by nuclear interactions•Kinematical threshold: Eth~5.6 for the reaction
pppppp
Experimental scenario before PAMELA
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Oscar Adriani Waseda, January 14th, 2009
CR antimatter: available data
Antiprotons Positrons___ Moskalenko & Strong 1998
BESS-polar(long-duration)
“Standard” balloon-borne experiments• low exposure (~20h)
large statistical errors• atmospheric secondaries (~5g/cm2) additional systematic uncertainty @low-energy
Why in space?
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Oscar Adriani Waseda, January 14th, 2009
PAMELA detectors
GF: 21.5 cm2 sr Mass: 470 kgSize: 130x70x70 cm3
Power Budget: 360W Spectrometer microstrip silicon tracking system + permanent magnetIt provides:
- Magnetic rigidity R = pc/Ze- Charge sign- Charge value from dE/dx
Time-Of-Flightplastic scintillators + PMT:- Trigger- Albedo rejection;- Mass identification up to 1 GeV;- Charge identification from dE/dX.
Electromagnetic calorimeterW/Si sampling (16.3 X0, 0.6 λI) - Discrimination e+ / p, anti-p / e- (shower topology)- Direct E measurement for e-
Neutron detectorplastic scintillators + PMT:- High-energy e/h discrimination
Main requirements high-sensitivity antiparticle identification and precise momentum measure+ -
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Oscar Adriani Waseda, January 14th, 2009
Principle of operation
•Measured @ground with protons of known momentum
MDR~1TV•Cross-check in flight with protons (alignment) and electrons (energy from calorimeter)
Iterative 2 minimization as a function of track state-vector components
Magnetic deflection|η| = 1/R R = pc/Ze magnetic rigidity
R/R =
Maximum Detectable Rigidity (MDR)def: @ R=MDR R/R=1
MDR = 1/
Track reconstruction
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Oscar Adriani Waseda, January 14th, 2009
Principle of operationZ measurement
Bethe Bloch ionization energy-loss of heavy (M>>me) charged particles
1st plane
pd
3He
4He
Li
Be
B,C
track average
e±
(saturation)
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Oscar Adriani Waseda, January 14th, 2009
Principle of operation
• Particle identification @ low energy• Identify albedo (up-ward going particles < 0 ) NB! They mimic antimatter!
Velocity measurement
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Oscar Adriani Waseda, January 14th, 2009
Principle of operation
• Interaction topologye/h separation
• Energy measurement of electrons and positrons (~full shower containment)
electron (17GV)hadron (19GV)
Electron/hadron separation
5%aE
ba
E
σE
+ NEUTRONS!!
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Oscar Adriani Waseda, January 14th, 2009
The Resurs DK-1 spacecraft• Multi-spectral remote sensing of earth’s surface
-near-real-time high-quality images• Built by the Space factory TsSKB Progress in Samara (Russia)• Operational orbit parameters:
-inclination ~70o
-altitude ~ 360-600 km (elliptical)• Active life >3 years • Data transmitted via Very high-speed Radio Link (VRL)
• PAMELA mounted inside a pressurized container • moved from parking to data-taking position few times/year
Mass: 6.7 tonsHeight: 7.4 mSolar array area: 36 m2
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Oscar Adriani Waseda, January 14th, 2009
PAMELA design performance
energy range particles in 3 years
Antiprotons 80 MeV ÷190 GeV O(104)
Positrons 50 MeV ÷ 270 GeV O(105)
Electrons up to 400 GeV O(106)Protons up to 700 GeV O(108)Electrons+positrons up to 2 TeV (from calorimeter)Light Nuclei up to 200 GeV/n He/Be/C: O(107/4/5)Anti-Nuclei search sensitivity of 3x10-8 in anti-He/He
Unprecedented statistics and new energy range for cosmic ray physics (e.g. contemporary antiproton and positron maximum energy ~ 40 GeV) Simultaneous measurements of many species
Magnetic curvature & trigger spillover showercontainment
Maximum detectable rigidity (MDR)
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Oscar Adriani Waseda, January 14th, 2009
PAMELA milestones
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 since
commissioning 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 December 2008:~800 days of data taking~16 TByte of raw data downlinked~16•108 triggers recorded and analysed(Data from May till now under analysis)
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Antiprotons
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Oscar Adriani Waseda, January 14th, 2009
High-energy antiproton analysis• Analyzed data July 2006 – February 2008 (~500 days) • Collected triggers ~108
• Identified ~ 10 106 protons and ~ 1 103 antiprotons between 1.5 and 100 GeV ( 100 p-bar above 20GeV )
• Antiproton/proton identification:• rigidity (R) SPE• |Z|=1 (dE/dx vs R) SPE&ToF• vs R consistent with Mp ToF• p-bar/p separation (charge sign) SPE• p-bar/e- (and p/e+ ) separation CALO
• Dominant background spillover protons:• finite deflection resolution of the SPE wrong assignment of charge-sign @ high energy • proton spectrum harder than positron p/p-bar increase for increasing energy (103 @1GV 104 @100GV)
Required strong SPE selection
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Oscar Adriani Waseda, January 14th, 2009
Antiproton identification
e- (+ p-bar)
p-bar
p
-1 Z +1
“spillover” p
p (+ e+)
proton-consistency cuts(dE/dx vs R and vs R)
electron-rejection cuts based on calorimeter-pattern topology
1 GV5 GV
( For |Z|=1, deflection=1/p )
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Oscar Adriani Waseda, January 14th, 2009
MDR > 850 GV
Minimal track requirements
Strong track requirements:•strict constraints on 2 (~75% efficiency)•rejected tracks with low-resolution clusters along the trajectory
- faulty strips (high noise)- -rays (high signal and multiplicity)
Proton-spillover background
MDR = 1/(evaluated event-by-event by the fitting
routine)
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Oscar Adriani Waseda, January 14th, 2009
p-bar p“spillover” p
10 GV 50 GV
Proton-spillover backgroundMDR = 1/
(evaluated event-by-event by the fitting
routine)
R < MDR/10
MDR depends on:• number and distribution of fitted points along the trajectory• spatial resolution of the single position measurements• magnetic field intensity along the trajectory
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Oscar Adriani Waseda, January 14th, 2009
Antiproton-to-proton ratio
astro-ph 0810.4994 In press by PRL*preliminary*(Petter Hofverberg’s PhD Thesis)
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Positrons
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Oscar Adriani Waseda, January 14th, 2009
High-energy positron analysis• Analyzed data July 2006 – February 2008 (~500 days) • Collected triggers ~108
• Identified ~ 150 103 electrons and ~ 9 103 positrons between 1.5 and 100 GeV (180 positrons above 20GeV )
• Electron/positron identification:• rigidity (R) SPE •|Z|=1 (dE/dx=MIP) SPE&ToF• =1 ToF• e-/e+ separation (charge sign) SPE• e+/p (and e-/p-bar) separation CALO
• Dominant background interacting protons:• fluctuations in hadronic shower development might mimic pure em showers• proton spectrum harder than positron p/e+ increase for increasing energy (103 @1GV 104 @100GV)
Required strong CALO selection
S1
S2
CALO
S4
CA
RD
CA
S
CAT
TOFSPE
S3
ND
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Oscar Adriani Waseda, January 14th, 2009
Positron identification with CALO• Identification based on:
– Shower topology (lateral and longitudinal profile, shower starting point)
– Total detected energy (energy-rigidity match)
• Analysis key points:– Tuning/check of selection criteria with:
• test-beam data• simulation• flight data dE/dx from SPE & neutron yield from ND
– Selection of pure proton sample from flight data (“pre-sampler” method):• Background-suppression method• Background-estimation methodFinal results make NON USE of test-beam and/or simulation
calibrations.The measurement is based only on flight data
with the background-estimation method
51 GV positron
80 GV proton
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Oscar Adriani Waseda, January 14th, 2009
Positron identificationFraction of charge released along the calorimeter track
(e+)
p (non-int)
p (int)
NB!
p-bar (int)
e-
p-bar (non-int)
Z=-1
Z=+1
Rigidity: 20-30 GV
LEFT HIT RIGHT
strips
plan
es
0.6 RM
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Oscar Adriani Waseda, January 14th, 2009
e- ( e+ )
pp-bar
e
h
Positron identification
Energy-momentum match
En
erg
y m
easu
red
in
Calo
/D
efl
ecti
on
in
Tra
cker
(MIP
/GV
)
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Oscar Adriani Waseda, January 14th, 2009
Positron identificationFraction of charge released along the calorimeter track
(e+)
p (non-int)
p (int)
NB!
p-bar (int)
e-
p-bar (non-int)
Z=-1
Z=+1
Rigidity: 20-30 GV
+Constraints on:
Energy-momentum match
e+
p
p-bar
e-
Z=-1
Z=+1
Rigidity: 20-30 GV
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Oscar Adriani Waseda, January 14th, 2009
Positron identification51 GV positron
80 GV proton
Shower starting-point Longitudinal profile
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Oscar Adriani Waseda, January 14th, 2009
e+
p
p-bar
e-
Z=-1
Z=+1
Rigidity: 20-30 GV
Positron identificationFraction of charge released along the calorimeter track
+Constraints on:
Energy-momentum match
Shower starting-point
Longitudinal profile
e+
p
e-Rigidity: 20-30 GV
Z=-1
Z=+1
Lateral profile
BK-suppression
method
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Oscar Adriani Waseda, January 14th, 2009
Check of calorimeter selection
pppp
Flight dataRigidity: 20-30
GV
Test beam dataMomentum: 50GeV/c
ee--
Fraction of charge released along the calorimeter track
+Constraints on:
Energy-momentum match
Shower starting-point
ee--
ee++
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Oscar Adriani Waseda, January 14th, 2009
Check of calorimeter selection
pp
Flight dataRigidity: 20-30
GV
ee--
ee++
Fraction of charge released along the calorimeter track
+Constraints on:
Energy-momentum match
Shower starting-point
ee--
ee++
pp
Flight dataNeutron yield in ND
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Oscar Adriani Waseda, January 14th, 2009
Check of calorimeter selection
Rigidity: 10-15 GV Rigidity: 15-20 GV
neg (e-)
e+e+p
pos (p)
p
Energy loss in silicon tracker detectors:
• Top: positive (mostly p) and negative events (mostly e-)• Bottom: positive events identified as p and e+ by trasversal profile method
neg (e-)pos (p)
Relativistic rise
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Oscar Adriani Waseda, January 14th, 2009
2 W planes: ≈1.5 X0
20 W planes: ≈15 X0
CALORIMETER: 22 W planes: 16.3 X0
The “pre-sampler” method
Selection of a pure sample of protons from flight data
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Oscar Adriani Waseda, January 14th, 2009
Rigidity: 20-28 GV
Proton background evaluation
Fraction of charge released along the
calorimeter track (left, hit, right)
+Constraints on:
Energy-momentum match
Shower starting-point
e+
p (pre-sampler)
e-
p
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Oscar Adriani Waseda, January 14th, 2009
Rigidity: 28-42 GV
Proton background evaluation
Fraction of charge released along the
calorimeter track (left, hit, right)
+Constraints on:
Energy-momentum match
Shower starting-point
e+
p (pre-sampler)
e-
p
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Oscar Adriani Waseda, January 14th, 2009
Positron fraction
astro-ph 0810.4995
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Oscar Adriani Waseda, January 14th, 2009
(( Do we have any antimatter excess in CRs? ))
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Oscar Adriani Waseda, January 14th, 2009
Antiproton-to-proton ratioSecondary Production Models
(Donato et al. 2001)• Diffusion model with convection and reacceleration• Solar modulation: spherical model (f=500MV ) Uncertainty band related to propagation parameters (~10% @10GeV) Additional uncertainty of ~25% due to production cs should be considered !!
(Ptuskin et al. 2006) GALPROP code • Plain diffusion model • Solar modulation: spherical model ( f=550MV )
(Moskalenko et al. 2006) GALPROP code • Plain diffusion model • Solar modulation: drift model ( A<0, =15o )
CR + ISM p-bar + …
No evidence for any antiproton excess
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Oscar Adriani Waseda, January 14th, 2009
(Moskalenko & Strong 1998) GALPROP code • Plain diffusion model • Interstellar spectra
Positron fractionSecondary Production Models CR + ISM ± + … ± + … e± +
… CR + ISM 0 + … e±
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Oscar Adriani Waseda, January 14th, 2009
Positron fractionSecondary Production Models
(Moskalenko & Strong 1998) GALPROP code • Plain diffusion model • Interstellar spectra
(Delahaye et al. 2008)• Plain diffusion model• Solar modulation: spherical model (=600MV)
Uncertainty band related to e- spectral index (e= 3.44±0.1 (3) MIN÷MAX) Additional uncertainty due to propagation parameters should be considered (factor ~6 @1GeV ~4 @high-energy)
Soft ( ‘big’)
Hard ( ‘small’)
CR + ISM ± + … ± + … e± + … CR + ISM 0 + … e±
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Oscar Adriani Waseda, January 14th, 2009
Electron spectrum
~ E- 3.24±0.04
F1AEF
~φ3.24
e
e+ ~ E-3.5 expected from pure
secondary
models
NB!!• Flux in the spectrometer• No solar demodulation
Geom.cutoffHard, small!
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Oscar Adriani Waseda, January 14th, 2009
Positron fractionSecondary Production Models
soft
hard
Quite robust evidence for a positron excess
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Oscar Adriani Waseda, January 14th, 2009
Primary positron sources
Dark Matter• e+ yield depend on the dominant decay channel LSPs seem disfavored due to suppression of e+e- final states low yield (relative to p-bar) soft spectrum from cascade decays
LKPs seem favored because can annihilate directly in e+e- high yield (relative to p-bar) hard spectrum with pronounced cutoff @ MLKP (>300 GeV)
• Boost factor required to have a sizable e+ signalNB: constraints from p-bar data!!
LKP -- M= 300 GeV (Hooper & Profumo 2007)
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Oscar Adriani Waseda, January 14th, 2009
Primary positron sourcesAstrophysical processes
• Local pulsars are well-known sites of e+e- pair production: they can individually and/or coherently contribute to the e+e- galactic flux and explain the PAMELA e+ excess (both spectral feature and intensity) No fine tuning required
if one or few nearby pulsars dominate, anisotropy could be detected in the angular distribution possibility to discriminate between pulsar and DM origin of e+ excess
All pulsars (rate = 3.3 / 100 years)(Hooper, Blasi, Seprico 2008)
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Oscar Adriani Waseda, January 14th, 2009
(Chang et al 2008)
PAMELA positron excess might be connected with ATIC electron+positron structures?
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Oscar Adriani Waseda, January 14th, 2009
Primary positron sourcesPAMELA positron fraction
alone insufficient to understand the origin of
positron excess
Additional experimental data will be provided by PAMELA:– e+ fraction @ higher energy (up to 300 GeV)
– individual e- e+ spectra – anisotropy (…maybe)– high energy e++e- spectrum (up to 2 TV)
Complementary information from:– gamma rays– neutrinos