P A M E L A Payload for Antimatter / Matter Exploration ...
Transcript of P A M E L A Payload for Antimatter / Matter Exploration ...
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P A M E L A
Payload for Antimatter /
Matter Exploration and
Light-nuclei Astrophysics
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Anticoincidence reduces out of
acceptance background
Sign of charge,
rigidity, dE/dx
Electron energy, dE/dx,
lepton-hadron
separation
e- p -
e+ p (He,...)
Trigger, ToF, dE/dx
- +
~470 kg
~360 W
~1.3
m
21.5 cm2sr
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Resurs-DK1 satellite
Mass: 6.7 tonnes
Height: 7.4 m
Solar 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
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Launch: 15th June 2006, 0800 UTC
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• Quasi-polar (70.0°) • Elliptical (350 km - 600 km) • PAMELA traverses the South Atlantic Anomaly • At the South Pole PAMELA crosses the outer (electron) Van Allen belt
70.0o
610 km
350 km
SAA
Orbit characteristics
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6.5 GV
interacting proton
candidate
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PAMELA event
13 GV
Interacting helium nucleus
candidate
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5.7 GV
non-interacting carbon nucleus
candidate
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18 GV
non-interacting anti-proton
candidate
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84 GV
interacting antiproton
candidate
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92 GV positron
candidate
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Antiprotons
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Bending in spectrometer: sign of charge
Ionisation energy loss (dE/dx): magnitude of charge
Interaction pattern in calorimeter: electron-like or proton-like, electron energy
Time-of-flight: trigger, albedo rejection, mass determination (up to 1 GeV)
Positron (NB: p/e+ ~103-4)
Antiproton (NB: e-/p ~ 102)
Antiproton / positron identification
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Antiproton Results
O. Adriani et al., PRL 102, 051101 (2009); PRL 105, 121101 (2010)
Donato et al. (PRL 102 (2009) 071301)
Simon et al. (ApJ 499 (1998) 250) Ptuskin et al. (ApJ 642 (2006) 902)
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Cosmic-Ray Antiprotons and DM limits
D. G. Cerdeno, T. Delahaye & J. Lavalle, arXiv: 1108:1128 Antiproton flux predictions for a 12 GeV WIMP annihilating into different mass combinations of an intermediate two-boson state which further decays into quarks.
See also: •M. Asano, T. Bringmann & C. Weniger, arXiv:1112.5158. • M. Garny, A. Ibarra & S. Vogl, arXiv:1112.5155 • R. Kappl & M. W. Winkler, arXiv:1140.4376
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PAMELA trapped antiprotons
Adriani et al., APJL 737 L29 (2011); arXiv:1107.4882
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Positrons
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Positron to Electron Fraction
Secondary production Moskalenko & Strong 98
Adriani et al, Astropart. Phys. 34 (2010) 1 arXiv:1001.3522 [astro-ph.HE]
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But antiprotons in CRs are in agreement with secondary production
CR Positron spectrum significantly harder than expectations from secondary production
A Challenging Puzzle for CR Physics
Preliminary
Donato et al. (PRL 102 (2009) 071301)
Ptuskin et al. (ApJ 642 (2006) 902)
Simon et al. (ApJ 499 (1998) 250)
Preliminary
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Astrophysical Explanation: SNR
P.Blasi et al., PRL 103 (2009) 051104 arXiv:0903.2794 [astro-ph]
Positrons (and electrons) produced as secondaries in the sources (e.g. SNR) where CRs are accelerated. But also other secondaries are produced: significant increase expected in the p/p and B/C ratios.
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Positrons detection Where do positrons come from?
Mostly locally within 1 Kpc, due to the energy losses by Synchrotron Radiation and Inverse Compton
Typical lifetime
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Astrophysical Explanation: Pulsars
Are there “standard” astrophysical explanations of the high energy positron data?
Young, nearby pulsars
Not a new idea: Boulares, ApJ 342 (1989), Atoyan et al (1995)
Geminga pulsar
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Mechanism: the spinning B of the pulsar strips e- that accelerated at the polar cap or at the outer gap emit γ that make production of e±
that are trapped in the cloud, further accelerated and later released at τ ~ 105 years.
Young (T < 105 years) and nearby (< 1kpc) If not: too much diffusion, low energy, too low flux. Geminga: 157 parsecs from Earth and 370,000 years old B0656+14: 290 parsecs from Earth and 110,000 years old. Diffuse mature pulsars
Astrophysical Explanation: Pulsars
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Astrophysical Explanation: Pulsars
H. Yüksak et al., arXiv:0810.2784v2 Contributions of e- & e+ from Geminga assuming different distance, age and energetic of the pulsar diffuse mature &nearby young pulsars
Hooper, Blasi, and Serpico arXiv:0810.1527
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M. Cirelli et al., Nucl. Phys. B 813 (2009) 1; arXiv: 0809.2409v3
Interpretation: DM Which DM spectra can fit the data?
DM with and dominant annihilation channel (possible candidate: Wino)
positrons antiprotons
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Interpretation: DM Which DM spectra can fit the data? DM with and dominant annihilation channel (no “natural” SUSY candidate)
positrons antiprotons But B≈104
M. Cirelli et al., Nucl. Phys. B 813 (2009) 1; arXiv: 0809.2409v3
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Interpretation: DM
DM with and dominant annihilation channel
positrons antiprotons
M. Cirelli et al., Nucl. Phys. B 813 (2009) 1; arXiv: 0809.2409v3
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Interpretation: DM I. Cholis et al. Phys. Rev. D 80 (2009)
123518; arXiv:0811.3641v1
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Electrons
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Results from three ATIC flights
ATIC-4 with 10 BGO layers has improved e , p separation. (~4x lower background)
“Bump” is seen in all three flights.
ATIC 1+2
“Source on/source off” significance of bump for ATIC1+2 is about 3.8 sigma J Chang et al. Nature 456, 362 (2008)
Significance for ATIC1+2+4 is 5.1 sigma
ATIC 1+2+4 ATIC 1 ATIC 2 ATIC 4
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FERMI All Electron Spectrum
A. Abdo et al., Phys.Rev.Lett. 102 (2009) 181101 M. Ackermann et al., Phys. Rev. D 82, 092004 (2010)
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Electrons measured with H.E.S.S.
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PAMELA electron (e-) spectrum
e+ + e-
e-
Flux=A • E-
= 3.18 ±0.05
O. Adriani et al., PRL 106 (2011) 201101.
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Theoretical uncertainties on “standard” positron fraction
D. Grasso et al., arXiv:0905.0636
Does not fit at all the
PAMELA ratio:
Modify the injection indices of
GALPROP?
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The Completed AMS Detector on ISS
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The Completed AMS Detector on ISS
S. Schael, UCLA Dark Matter Conference 2012,