pamela space mission first results in cosmic rays
DESCRIPTION
PAMELA Space Mission First Results in Cosmic Rays. Piergiorgio Picozza INFN & University of Rome “ Tor Vergata” , Italy Pamela Collaboration Rencontres de Blois 2008 Challenges in Particle Astrophysics Blois, May 22, 2008. PAMELA. - PowerPoint PPT PresentationTRANSCRIPT
PAMELA Space MissionPAMELA Space Mission
First Results in Cosmic Rays First Results in Cosmic Rays
Piergiorgio Picozza INFN & University of Rome “ Tor Vergata” , Italy
Pamela CollaborationPamela Collaboration
Rencontres de Blois 2008Rencontres de Blois 2008Challenges in Particle AstrophysicsChallenges in Particle Astrophysics
Blois, May 22, 2008
PAMELAPAMELAPPayload for ayload for AAntimatter ntimatter MMatter atter EExploration xploration
and and LLight Nucleiight Nuclei AAstrophysicsstrophysics
PAMELA CollaborationPAMELA Collaboration
Moscow St. Petersburg
Russia:
Sweden:KTH, Stockholm
Germany:Siegen
Italy:Bari Florence Frascati TriesteNaples Rome CNR, Florence
Pamela as a Space Observatory at 1AU
Study of solar physics and solar modulation
Study of terrestrial magnetosphere
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 high energy electron spectrum (local sources?)
Sign of charge, rigidity, dE/dx
Electron energy, dE/dx, lepton-hadron
separation
e- p -
e+ p (He,...)
Trigger, ToF, dE/dx
- +
GF ~21.5 cmGF ~21.5 cm2sr sr Mass: 470 kg Mass: 470 kg Size: 130x70x70 cmSize: 130x70x70 cm3
Energy range
Antiproton flux 80 MeV - 190 GeV Positron flux 50 MeV – 270 GeVElectron/positron flux up to 2 TeV (from calorimeter)
Electron flux up to 400 GeVProton flux up to 700 GeVLight nuclei (up to Z=6) up to 200 GeV/n He/Be/C:Antinuclei search Sensitivity of O(10
-8) in He-bar/He
Design performanceDesign performance
• Unprecedented statistics and new energy range for cosmic ray physics
• Simultaneous measurements of many species
Resurs-DK1 satelliteResurs-DK1 satellite
Mass: 6.7 tonnesHeight: 7.4 mSolar array area: 36 m2
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
PAMELAPAMELA
LaunchLaunch15/06/0615/06/06
16 Gigabytes trasmitted 16 Gigabytes trasmitted daily to Grounddaily to Ground
NTsOMZ MoscowNTsOMZ Moscow
OrbitOrbit Characteristics Characteristics
km
km
SAA
• Low-earth elliptical orbit
• 350 – 610 km
• Quasi-polar (70o inclination)
• Lifetime >3 years (assisted)
Download @orbit 3754 – 15/02/2007 07:35:00 MWT
S1 S2 S3
Inner radiation belt
(SSA)
orbit 3752 orbit 3753orbit 3751
NP SP
EQ EQ
Outer radiation belt
95 min
PAMELA Orbit
Flight data: 0.169 GV electron
Flight data: 0.171 GV positron
Flight data: 0.632 GeV/cantiproton annihilation
Flight data: 84 GeV/c interacting antiproton
Flight data: 92 GeV/cpositron
Flight data: 14.7 GVInteracting nucleus
(Z = 8)
PAMELA StatusPAMELA Status
Till 2nd of March 2008 PAMELA has Till 2nd of March 2008 PAMELA has collected ~ 8.8TB of data, collected ~ 8.8TB of data, corresponding to corresponding to ~~ 10 109 9 triggerstriggers
4% 23% 73%
(GLAST AMS-02)
Signal (supersymmetry)…
… and background
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-loopprocesses that produces monoenergeticγ γ in the final state.
Secondary production Bergström et al. ApJ 526 (1999) 215
Secondary production (upper and lower limits)Simon et al. ApJ 499 (1998) 250.
from χχ annihilation (Primary production m(c) = 964 GeV)
Ullio : astro-ph/9904086
P
Antiproton-Proton RatioAntiproton-Proton Ratio
Antiproton-Proton RatioAntiproton-Proton Ratio
preliminary
Antiproton-Proton RatioAntiproton-Proton Ratio
preliminary
Cirelli, Franceschini, Strumia
arXiv:0802.3378v2 [hep-ph]
Positron - Electron ratioPositron - Electron ratio
Potgieter at al. arXiv:0804.0220v1 [astro-ph]
Pamela PositronsPamela Positrons
Till August 30Till August 30thth about 20000 positrons about 20000 positrons from 200 MeV up to 200 GeV have been from 200 MeV up to 200 GeV have been analyzedanalyzed
More than 15000 positrons over 1 GeVMore than 15000 positrons over 1 GeV
Other eight months data to be analyzedOther eight months data to be analyzed
Positron - Electron ratioPositron - Electron ratio
PAMELA
Preliminary
Positron - Electron ratioPositron - Electron ratio
Positron - Electron ratioPositron - Electron ratioPrelim
inary
Positrons with HEAT Positrons with HEAT
Positrons with HEAT & PAMELA Positrons with HEAT & PAMELA Prelim
inary
ProblemsProblems
Background calculationBackground calculation
Solar Modulation at low energiesSolar Modulation at low energies
Charge-sign dependence of solar Charge-sign dependence of solar modulationmodulation
Diffusion Halo ModelDiffusion Halo Model
Secondaries / primaries Secondaries / primaries i.e. Boron/ Carbon to constrain propagation parametersi.e. Boron/ Carbon to constrain propagation parameters
D. Maurin, F. Donato R. Taillet and P.Salati ApJ, 555, 585, 2001 [astro-ph/0101231]
F. Donato et.al, ApJ, 563, 172, 2001 [astro-ph/0103150]
AstrophysicAstrophysicB/CB/C
constraintsconstraints
Nuclear Nuclear cross cross
sections!!sections!!
B/C Ratio Antiproton flux
Preliminary Results B/CPreliminary Results B/CPreliminary
Helium and Hydrogen IsotopesHelium and Hydrogen Isotopes
Secondary to Primary ratiosSecondary to Primary ratios
Kinetic Energy (GeV)
Flu
x (p
/cm
^2 s
r s)
Proton flux July 2006
Galactic H and He spectraGalactic H and He spectraPrelim
inar
y !!!
Solar Physics with PAMELASolar Physics with PAMELA
Solar Modulation of galactic cosmic raysSolar Modulation of galactic cosmic rays
BESS
Caprice / Mass /TS93AMS-01
Pamela
Continuous Continuous monitoring monitoring of solar activityof solar activity
Study of charge sign Study of charge sign
dependent effectsdependent effects Asaoka Y. et al. 2002, Phys. Asaoka Y. et al. 2002, Phys.
Rev. Lett. 88, 051101), Rev. Lett. 88, 051101), Bieber, J.W., et al. Physi-cal Bieber, J.W., et al. Physi-cal
Review Letters, 84, 674, Review Letters, 84, 674, 1999. 1999.
J. Clem et al. J. Clem et al. 30th ICRC 30th ICRC
20072007
Antiproton-Proton RatioAntiproton-Proton Ratio
preliminary
Proton SpectraProton SpectraPrelim
inar
y !!!
RED: JULY 2006BLUE: AUGUST 2007
P/(
cm^2
sr
GeV
s)
Primary spectrum 2222is MφE+/ME F =F
July 2006 497±2January 2007 481±2August 2007 441±2
BESS Coll. 30th ICRC 2007
Positron FractionPositron Fraction
Mirko Boezio, INFN Trieste - Fermilab, 2008/05/02Mirko Boezio, INFN Trieste - Fermilab, 2008/05/02
Preliminary
Clem at al. 30th ICRC 2007
Pamela Pamela
Charge sign dependence of cosmic ray Charge sign dependence of cosmic ray modulation.modulation.
Two systematic deviations from reflection symmetry of the Two systematic deviations from reflection symmetry of the interplanetary magnetic field:interplanetary magnetic field:
1) The Parker field has opposite magnetic polarity above and 1) The Parker field has opposite magnetic polarity above and below the equator, but the spiral field lines themselves are below the equator, but the spiral field lines themselves are mirror images of each other. This antisymmetry produces mirror images of each other. This antisymmetry produces drift velocity fields that for positive particles converge on the drift velocity fields that for positive particles converge on the heliospheric equator in the Aheliospheric equator in the A++ state or diverge from it in A state or diverge from it in A- -
state.state. Negatively charged particles behave in the opposite manner Negatively charged particles behave in the opposite manner
and the drift patterns interchange when the solar polarity and the drift patterns interchange when the solar polarity diverge.diverge.
2) Systematic ordering of turbulent helicity can cause 2) Systematic ordering of turbulent helicity can cause diffusion coefficients to depend directly on charge sign and diffusion coefficients to depend directly on charge sign and polarity state. polarity state. Bieber, J.W., et al. Phys. Rev. Letters, 84, 674, Bieber, J.W., et al. Phys. Rev. Letters, 84, 674, 1999. 1999.
December 2006 Solar particle eventsDecember 2006 Solar particle events
Dec 13th largest CME since 2003, anomalous at sol min
December 13th 2006 event
Preliminary!
Preliminary!
December 13th 2006 He differential spectrum
December 14th 2006 event
Preliminary!
Solar Quiet spectrum
Low energy tail of Dec 13th event
Below galactic spectrum: Start of Forbush decrease
Magnetic Field
Neutron Monitor
X-ray
P,e-
Decrease of primary spectrum
Arrival of magnetic cloud from CME of Dec 13th
Shock 1774km/s (gopalswamy, 2007)
Decrease of Neutron Monitor Flux
Magnetic Field
Neutron Monitor
X-ray
P,e-
Arrival of event of Dec 14th
End of event of Dec 14th
Radiation BeltsRadiation Belts
South Atlantic AnomalySouth Atlantic Anomaly
Secondary production from CR Secondary production from CR interaction with atmosphereinteraction with atmosphere
Pamela World Maps: 350 – 650 km altPamela World Maps: 350 – 650 km alt
36 MeV p, 3.5 MeV e-
Pamela maps at various altitudesPamela maps at various altitudesPRELIMINARY !!!!
Altitude scanning
Primary and Albedo (sub-cutoff Primary and Albedo (sub-cutoff measurements)measurements)
Other ObjectivesOther Objectives
AMSPAMELA AMS PAMELA AMS in Spacein Space
AcceleratorsAccelerators
The Big Bang origin of the Universe requires matter and antimatter
to be equally abundant at the very hot beginning
Search for the existence of anti Universe Search for th
e origin of th
e Universe
Search for the existence of Antimatter in the Search for the existence of Antimatter in the UniverseUniverse
What about heavy antinuclei?What about heavy antinuclei? The discovery of one nucleus of antimatter The discovery of one nucleus of antimatter
(Z≥2) in the cosmic rays would have profound (Z≥2) in the cosmic rays would have profound implications for both particle physics and implications for both particle physics and astrophysics.astrophysics.
• For a Baryon Symmetric Universe Gamma For a Baryon Symmetric Universe Gamma
rays limits put any domain of antimatter rays limits put any domain of antimatter
more than 100 Mpc away more than 100 Mpc away
(Steigman (1976) Ann Rev. Astr. Astrophys., (Steigman (1976) Ann Rev. Astr. Astrophys., 1414, 339; Dudarerwicz , 339; Dudarerwicz
and Wolfendale (1994) M.N.R.A. and Wolfendale (1994) M.N.R.A. 268268, 609, A.G. Cohen, A. De Rujula , 609, A.G. Cohen, A. De Rujula
and S.L. Glashow, Astrophys. J. 495, 539, 1998)and S.L. Glashow, Astrophys. J. 495, 539, 1998)
Antimatter Direct researchAntimatter Direct research
AntimatterAntimatter which has escaped as a which has escaped as a cosmic ray from a distant antigalaxy cosmic ray from a distant antigalaxy
Streitmatter, R. E., Nuovo Cimento, 19, 835 (1996)Streitmatter, R. E., Nuovo Cimento, 19, 835 (1996)
AntimatterAntimatter from globular clusters of from globular clusters of antistars in our Galaxy as antistellar wind antistars in our Galaxy as antistellar wind or anti-supernovae explosionor anti-supernovae explosion
K. M. Belotsky et al., Phys. Atom. Nucl. 63, 233 (2000), K. M. Belotsky et al., Phys. Atom. Nucl. 63, 233 (2000), astro-ph/9807027astro-ph/9807027
Cosmic-ray antimatter searchCosmic-ray antimatter search
“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)
BESS combined (new)
expected
High Energy electronsHigh Energy electrons
The study of primary electrons is especially The study of primary electrons is especially important because they give information on the important because they give information on the nearest sources of cosmic rays nearest sources of cosmic rays
Electrons with energy above 100 MeV rapidly Electrons with energy above 100 MeV rapidly loss their energy due to synchrotron radiation loss their energy due to synchrotron radiation and inverse Compton processes and inverse Compton processes
The discovery of primary electrons with energy The discovery of primary electrons with energy above 10above 1012 12 eV will evidence the existence of eV will evidence the existence of cosmic ray sources in the nearby interstellar cosmic ray sources in the nearby interstellar space (rspace (r300 pc) 300 pc)
CALO SELF TRIGGER EVENT: 167*103 MIP RELEASED279 MIP in S4 26 Neutrons in ND
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.
i. A stable, single “super nucleon” with three types of quarks
ii. “Neutron” stars may be one big strangelet
Carbon Nucleus Strangelet
uuddss
ssdd
ddss
ssuudd
uudduuuudddd
ssuussuuuudd
dd dd dddd dd
uuuu
uuuu
ssuu ss
ssss
dddd uu
uuuudd
uuuudd
dddd uu
uuuudd
dddd uu dddd uu dddd uudddd uu
uuuudd uuuudd
uuuudd
p n
AMS courtesy
Search for New Matter in the Universe:
ConclusionConclusion
PAMELA is the first space experiment which is measuring PAMELA is the first space experiment which is measuring
the Antiprotons and Positrons to the high energies (> the Antiprotons and Positrons to the high energies (>
150GeV) with an unprecedented statistical precision150GeV) with an unprecedented statistical precision PAMELA is setting a new lower limit for finding AntiheliumPAMELA is setting a new lower limit for finding Antihelium PAMELA is looking for Dark Matter candidatesPAMELA is looking for Dark Matter candidates PAMELA is providing measurements on elemental spectra PAMELA is providing measurements on elemental spectra
and low mass isotopes with an unprecedented statistical and low mass isotopes with an unprecedented statistical
precision and is helping to improve the understanding of precision and is helping to improve the understanding of
particle propagation in the interstellar mediumparticle propagation in the interstellar medium PAMELA is able to measure the high energy tail of solar PAMELA is able to measure the high energy tail of solar
particles.particles.
THANKSTHANKS
http:// pamela.roma2.infn.ithttp:// pamela.roma2.infn.it