ricci pamela taup11 short - infnmain antenna in ntsomz launch from baikonur → june 15th 2006, 0800...
TRANSCRIPT
The image cannot be displayed. Your computer may not have enough memory to open the image, or the image may have been corrupted. Restart your computer, and then open the file again. If the red x still appears, you may have to delete the image and then insert it again.
Marco Ricci INFN, Laboratori Nazionali di Frascati, Frascati (Roma) , Italy
On behalf of the PAMELA Collaboration
TAUP 2011 Munich, September 5-9, 2011
Moscow St. Petersburg
Russia:
Sweden: KTH, Stockholm
Germany: Siegen
Italy: Bari Florence Frascati Trieste Naples Rome CNR, Florence
The PAMELA Instrument
Main antenna in NTsOMZ
Launch from Baikonur → June 15th 2006, 0800 UTC.
‘First light’ → June 21st 2006, 0300 UTC.
• Detectors operated nominally as expected after launch • Different trigger and hardware configurations evaluated
→ PAMELA in continuous data-taking mode since commissioning phase ended on July 11th 2006
Till ~now: ~1910 days of data taking ~25 TByte of raw data downlinked >2x109 triggers recorded and analyzed
PAMELA milestones
70ο
610 km
350 km
SAA
• Low-earth elliptical orbit
• 350 – 610 km
• Quasi-polar (70o inclination)
• SAA crossed
ApJ 457, L 103 1996 ApJ 532, 653, 2000
arXiv:0810.4994, PRL, NJP11,105023
arXiv:0810.4995, Nature, Astrop. Phys
Science 2011 arXiv:1103.4055
arXiv:0708.2587 2008AdSpR..41..168C 2008AdSpR..41.2037D 2008AdSpR..41.2043C
Pamela data
High precision charged
cosmic ray measurement in Low Earth
Orbit
Prl in press
Scientific achievements
Cosmic Ray Spectra
Cosmic-Ray Acceleration and Propagation in the Galaxy
p & He absolute fluxes
• First high-statistics and high-precision measurement over three decades in energy
• Dominated by systematics (~4% below 300 GV)
• Low energy minimum solar activity (φ = 450÷550 GV)
• High-energy a complex structure of the spectra emerges…
Adriani et al. , Science 332 (2011) 6025
Proton
Helium
p & He absolute fluxes @ high energy
Deviations from single power law (SPL):
Spectra gradually soften in the range 30÷230GV
Abrupt spectral hardening @ ~235GV
Sola
r m
odul
atio
n
Sola
r m
odul
atio
n
2.85 2.67
232 GV
Spectral index
2.77 2.48
243 GV
Standard scenario of SN blast waves expanding in the ISM needs additional features
p/He ratio vs R
Instrumental p.o.v.
Systematic uncertainties partly cancel out (livetime, spectrometer reconstruction, …)
Theoretical p.o.v.
Solar modulation negligible information about IS spectra down to GV region
Propagation effects (diffusion and fragmentation) negligible above ~100GV information about source spectra
(Putze et al. 2010)
p/He ratio vs R
First clear evidence of different H and He slopes above ~10GV
Ratio described by a single power law (in spite of the evident structures in the individual spectra)
αHe-αp = 0.078 ±0.008 χ2~1.3
Various hypoteses • Additional Source Wolfendale 2011
• Spallation Blasi & Amato 2011 • Weak local component (+ others) Vladimirov,
Johanesson, Moskalenko 2011
Electrons
Phys. Rev. Lett. 106, 201101 (2011)
PAMELA Electron flux measured up to 625 GeV
Spectrometric measurement
Adriani et al. , PRL 106, 201101 (2011) e+ +e-
Calorimetric measurements
e- Electron absolute flux
Largest energy range covered in any experiment hitherto with no atmospheric overburden
Low energy
• minimum solar activity (φ = 450÷550 GV)
High energy
No significant disagreement with recent ATIC and Fermi data
Softer spectrum consistent with both systematics and growing positron component
All electrons
ANTIPARTICLES
Positron fraction
Low energy charge-dependent solar modulation (see later)
High energy (quite robust) evidence of positron excess above 10GeV
Adriani et al. , Nature 458 (2009) 607 Adriani et al., AP 34 (2010) 1 (new results)
(Moskalenko & Strong 1998) GALPROP code • Plain diffusion model • Interstellar spectra
FERMI positron/electron ratio The Fermi-LAT has measured the cosmic-ray positron and electron spectra separately, between 20 – 130 GeV, using the Earth's magnetic field as a charge discriminator
The two independent methods of background subtraction,Fit-Based and MC-Based, produce consistent results
The observed positron fraction is consistent with the one measured by PAMELA
W. Mitthumsiri et al. @ Fermi Symposium (May 2011) and J.Vandenbroucke ICRC 2011
Antiproton flux
• Largest energy range covered hiterto (0.6 -180 GeV)
• Overall agreement with pure secondary calculation
• Experimental uncertainty (stat⊕sys) smaller than spread in theoretical curves constraints on propagation parameters
(Ptuskin et al. 2006) GALPROP code • Plain diffusion model • Solar modulation: spherical model ( φ=550MV )
(Donato et al. 2001) • Diffusion model with convection and reacceleration • Uncertainties on propagation param . and cross sec. • Solar modulation: spherical model ( φ=500MV ) A
drian
i et al. - PR
L 10
5 (2010
) 121101
Antiproton-to-proton ratio
Adriani et al. - PRL 105 (2010) 121101
• Overall agreement with pure secondary calculation
Antiprotons Consistent with pure secondary production
Positrons Evidence for an excess
A challenging puzzle for CR physicists
Positron-excess interpretations
Dark matter
boost factor required
lepton vs hadron yield must be consistent with p-bar observation
Astrophysical processes
• known processes
• large uncertainties on environmental parameters
(Blasi 2009) e+ (and e-) produced as secondaries in the CR acceleration sites (e.g. SNR)
(Hooper, Blasi and Serpico, 2009) contribution from diffuse mature & nearby young pulsars.
(Cholis et al. 2009) Contribution from DM annihilation.
26
A NEUTRON STAR WITH A STRONG MAGNETIC FIELD:
FAST ROTATING PULSAR (P = 33 msec)
L(spindown) = 5 1038 erg/s
O. Adriani et al., Ap.J.Lett. 737 L29 (2011); arXiv:1107.4882
29
• Antiprotons trapped in Earth’s inner radiation belt have been observed for the first time by the PAMELA experiment, confirming the existence of a significant antiproton flux in the SAA below ~1 GeV in kinetic energy.
• The flux exceeds the galactic CR antiproton flux by three orders of magnitude at the current solar minimum, thereby constituting the most abundant antiproton source near the Earth.
• A measurement of the sub-cutoff antiproton spectrum outside the SAA region is also under study.
• PAMELA results allow CR transport models to be tested in the terrestrial atmosphere and significantly constrain predictions from trapped antiproton models, reducing uncertainties concerning the antiproton production spectrum in Earth’s magnetosphere.
Solar Modulation of galactic cosmic rays
BESS
Caprice / Mass /TS93 AMS-01
Pamela • Study of charge sign
dependent effects Asaoka Y. et al. 2002, Phys. Rev.
Lett. 88, 051101), Bieber, J.W., et al. Physi-cal
Review Letters, 84, 674, 1999. J. Clem et al. 30th ICRC 2007 U.W. Langner, M.S. Potgieter,
Advances in Space Research 34 (2004)
Decreasing solar activity
Increasing GCR flux
Comparison of the proton flux measured between 1.5 and 1.57GV by PAMELA and ULYSSES as a function of time
Dec 13th largest CME since 2003, anomalous at sol min
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
p! n!
AMS courtesy
• PAMELA has been in orbit and studying cosmic rays for 5 years.
• >109 triggers registered and > 25 TB of data have been down-linked.
• The proton and helium nuclei spectra have been measured up to 1.2 TV. The observations challenge the current paradigm of cosmic ray acceleration and propagation.
• The e- spectrum up to 600 GeV shows no evident deviations from standard scenario, but is not inconsistent with an additional electron component.
• Antiproton-to-proton flux ratio and antiproton energy spectrum (~100 MeV - ~200 GeV) show no significant deviations from secondary production expectations.
• High energy positron fraction (>10 GeV) increases significantly (and unexpectedly!) with energy. Primary source?
• Discovery of geomagnetically trapped cosmic-ray antiprotons.
• Analysis ongoing to finalize the antiparticle measurements (positron flux, positron fraction), continuous study of solar modulation effects at low energy; primary and secondary nuclei abundance (up to Oxygen); isotopes; upper limit to anti-He.
• Extension of the mission to 2012? Agreements INFN-RSA in progress.
ApJ 457, L 103 1996 ApJ 532, 653, 2000
arXiv:0810.4994, PRL, NJP11,105023
arXiv:0810.4995, Nature, Astrop. Phys
Science 2011 arXiv:1103.4055
arXiv:0708.2587 2008AdSpR..41..168C 2008AdSpR..41.2037D 2008AdSpR..41.2043C
Pamela data
High precision charged
cosmic ray measurement in Low Earth
Orbit
Prl in press