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PAMELA. P ayload for A ntimatter M atter E xploration and L ight Nuclei A strophysics. Italy:. CNR, Florence. Bari. Florence. Frascati. Naples. Rome. Trieste. Russia:. Moscow St. Petersburg. Germany:. Sweden:. Siegen. KTH, Stockholm. PAMELA Collaboration.

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pamela
PAMELA

Payload for Antimatter Matter Exploration and Light NucleiAstrophysics

pamela collaboration

Italy:

CNR, Florence

Bari

Florence

Frascati

Naples

Rome

Trieste

Russia:

Moscow

St. Petersburg

Germany:

Sweden:

Siegen

KTH, Stockholm

PAMELA Collaboration
resurs dk1 satellite orbit
Resurs-DK1 satellite + orbit
  • Resurs-DK1: multi-spectral imaging of earth’s surface
  • PAMELA mounted inside a pressurized container
  • Lifetime >3 years (assisted, first time last February). Expected till end 2011.
  • Data transmitted to NTsOMZ, Moscow via high-speed radio downlink. ~16 GB per day
  • Quasi-polar and elliptical orbit (70.0°, 350 km - 600 km)
  • Traverses the South Atlantic Anomaly
  • Crosses the outer (electron) Van Allen belt at south pole

PAMELA

Resurs-DK1

Mass: 6.7 tonnes

Height: 7.4 m

Solar array area: 36 m2

350 km

70o

SAA

610 km

~90 mins

slide4

Electron (e-) flux, energy measurement

Two independent energy measurements:

Rigidity from Tracker

  • bremsstrahlungabove tracker
  • decreasing energy resolution

Energy from Calorimeter

  • sampling calorimeter
  • increasing energy resolution
  • possibility to cross-check the energy measurement

Mirko Boezio, HEAD 2010, 2010/03/03

electron identification
Electron identification

S1

CARD

CAT

S2

TOF

SPE

CAS

S3

CALO

S4

ND

  • Analyzed data July 2006 – December 2008 (~850 days)
  • Collected triggers >109
  • Identified ~ 5.5 105 electrons between 1 and 200 GeV
  • Electron/positron identification:
  • rigidity (R)  SPE
  • |Z|=1 (dE/dx=MIP) SPE&ToF
  • b=1 ToF
  • e-/e+ separation (charge sign)  SPE
  • (e-/p-bar separation  CALO)
  • ~ no background, issues:
    • - spillover protons at high energy
    • - spectrometer resolution
    • - selection efficiencies

Mirko Boezio, HEAD 2010, 2010/03/03

pamela electron e spectrum
PAMELA Electron (e-) Spectrum

Mirko Boezio, HEAD 2010, 2010/03/03

pamela electron e spectrum1
PAMELA Electron (e-) Spectrum

Mirko Boezio, HEAD 2010, 2010/03/03

pamela electron e spectrum3
PAMELA Electron (e-) Spectrum

Preliminary

Mirko Boezio, HEAD 2010, 2010/03/03

pamela electron e spectrum4
PAMELA Electron (e-) Spectrum

Preliminary

Mirko Boezio, HEAD 2010, 2010/03/03

pamela electron e e spectrum
PAMELA Electron (e- + e+) Spectrum

Mirko Boezio, HEAD 2010, 2010/03/03

positron to electron fraction
Positron to Electron Fraction

In Nature article published data acquired till February 2008

New data reduction: data till end of 2008. With same approach of Nature paper ~30% increase in statistics better understanding of systematics.

Secondary productionMoskalenko & Strong 98

Adriani et al, arXiv:1001.3522 [astro-ph.HE]

proton and alpha spectrum
Proton and Alpha Spectrum

Preliminary

Mirko Boezio, HEAD 2010, 2010/03/03

antiprotons
Antiprotons

Preliminary

Errors might be

underestimated, possible residual spillover-proton

contamination

Preliminary

Antiprotons in CRs are in agreement with secondary production

Mirko Boezio, HEAD 2010, 2010/03/03

summary
Summary
  • PAMELA has been in orbit and studying cosmic rays for ~42 months. >109 triggers registered and >18 TB of data has been down-linked.
  • e- spectrum up to ~200 GeV shows spectral features that may point to additional components. Analysis is ongoing to increase the statistics and expand the measurement of the e- spectrum up to ~500 GeV and e+ spectrum up to ~300 GeV (all electrum (e- + e+) spectrum up to ~1 TV).
  • High energy positron fraction (>10 GeV) increases significantly (and unexpectedly!) with energy. Primary source?
  • Data at higher energies might help to resolve origin of rise (spillover limit ~300 GeV).
  • Antiproton-to-proton flux ratio and antiproton energy spectrum (~100 MeV - ~200 GeV) show no significant deviations from secondary production expectations.

http://pamela.roma2.infn.it

slide16

Thanks!

Mirko Boezio, HEAD 2010, 2010/03/03