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Villa Mondragone, 30 Settembre 2008

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Presentation on theme: "Villa Mondragone, 30 Settembre 2008"— Presentation transcript:

1 Villa Mondragone, 30 Settembre 2008
WiZard PAMELA Commissione INFN II Piergiorgio Picozza Villa Mondragone, 30 Settembre 2008

2 Stato del Satellite Approvato il prolungamento fino al 31 Dicembre 2009 Iniziate le procedure per un prolungamento per un ulteriore triennio

3 Pamela as a Space Observatory at 1AU
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 solar physics and solar modulation Study of terrestrial magnetosphere Study of high energy electron spectrum (local sources?)

4 PAMELA Status ~630 giorni di presa dati (~73% live-time)
~10 TByte of raw data trasmessi >109 triggers ottenuti e sotto analisi Gravi ritardi nell’analisi dovuti ad una situazione di mezzi di calcolo ancora troppo deficitaria

5 Antiprotoni

6 Alignment Incoherent misalignment Correction with protons
2 steps: column alignment + inter-column alignment Coherent misalignment Correction with electrons (or electrons + positrons) and comparison with simulation

7 PAMELA Protons Spillover

8 Antiproton-Proton Ratio
PAMELA Preliminary

9 Antiproton to proton ratio
Preliminary

10 Antiproton to proton ratio
Preliminary

11 Positroni

12 Flight data: 42 GeV/c electron
Mirko Boezio, IDM2008, 2008/08/20

13 Flight data: 92 GeV/c positron

14 Flight data: 36 GeV/c interacting proton
Mirko Boezio, IDM2008, 2008/08/20 Mirko Boezio, IDM2008, 2008/08/20

15 Positron selection with calorimeter
Rigidity: GV e- p (non-int) p (int) Total negative  3067 Total positive  Selected electrons  2032 Selected positrons  322 p (non-int) e+ p (int) Preliminary Fraction of charge released along the calorimeter track (left, hit, right) Mirko Boezio, IDM2008, 2008/08/20 Mirko Boezio, IDM2008, 2008/08/20 15

16 Positron selection with calorimeter
Rigidity: GV e- e+ Total negative  3067 Total positive  Selected electrons  2032 Selected positrons  322 p Preliminary Fraction of charge released along the calorimeter track (left, hit, right) + Energy-momentum match Starting point of shower Mirko Boezio, IDM2008, 2008/08/20 Mirko Boezio, IDM2008, 2008/08/20 16

17 Positron selection with calorimeter
Rigidity: GV e- e+ Total negative  3067 Total positive  Selected electrons  2032 Selected positrons  322 p Preliminary Fraction of charge released along the calorimeter track (left, hit, right) + Energy-momentum match Starting point of shower Longitudinal profile Mirko Boezio, IDM2008, 2008/08/20 Mirko Boezio, IDM2008, 2008/08/20 17

18 Positron selection with calorimeter
Fraction of charge released along the calorimeter track (left, hit, right) Flight data: rigidity: GV Test beam data Momentum: 50GeV/c e- e- e- p e+ e+ p Mirko Boezio, IDM2008, 2008/08/20 Energy-momentum match Starting point of shower

19 Positron selection e- e+ p e- p e+ Rigidity: 20-30 GV
Fraction of charge released along the calorimeter track (left, hit, right) Neutrons detected by ND e- e- p e+ e+ p Energy-momentum match Starting point of shower Mirko Boezio, IDM2008, 2008/08/20

20 Positron selection e- e- e+ e+ p p p p Rigidity: 10-15 GV
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 p e- p e- p e+ p e+ Rigidity: GV Rigidity: GV Mirko Boezio, IDM2008, 2008/08/20 Mirko Boezio, IDM2008, 2008/08/20

21 e+ background estimation from data
Rigidity: GV Preliminary e- p e+ ‘presampler’ p Fraction of charge released along the calorimeter track (left, hit, right) + Energy-momentum match Starting point of shower Mirko Boezio, IDM2008, 2008/08/20 Mirko Boezio, IDM2008, 2008/08/20

22 e+ background estimation from data
Rigidity: 6-8 GV Preliminary e- p e+ ‘presampler’ p Fraction of charge released along the calorimeter track (left, hit, right) + Energy-momentum match Starting point of shower Mirko Boezio, IDM2008, 2008/08/20 Mirko Boezio, IDM2008, 2008/08/20

23

24 Positron to Electron Fraction
Preliminary!!! Charge sign dependent solar modulation End 2007: ~ positrons total Mirko Boezio, IDM2008, 2008/08/20 Mirko Boezio, IDM2008, 2008/08/20

25 Positrons with HEAT

26

27 Challenges Background calculation Solar Modulation at low energies
Charge-sign dependence of solar modulation

28

29 Flux (p/cm^2 sr s) Kinetic Energy (GeV) Proton flux July 2006

30 Galactic H and He spectra
Preliminary !!!

31 Solar Modulation of galactic cosmic rays
BESS Caprice / Mass /TS93 AMS-01 Pamela Continuous monitoring of solar activity Study of charge sign dependent effects Asaoka Y. et al. 2002, Phys. Rev. Lett. 88, ), Bieber, J.W., et al. Physi-cal Review Letters, 84, 674, 1999. J. Clem et al. 30th ICRC 2007

32 Solar modulation Preliminary!! Increasing GCR flux solar activity
Interstellar spectrum Preliminary!! (statistical errors only) Increasing GCR flux July 2006 August 2007 February 2008 solar activity Decreasing sun-spot number Ground neutron monitor PAMELA 35

33 Charge dependent solar modulation
Preliminary!! + +

34 Positron Fraction Preliminary
Mirko Boezio, INFN Trieste - Fermilab, 2008/05/02

35

36 A > 0 Positive particles A < 0

37 Charge sign dependence of cosmic ray modulation.
Two systematic deviations from reflection symmetry of the interplanetary magnetic field: 1) The Parker field has opposite magnetic polarity above and below the equator, but the spiral field lines themselves are mirror images of each other. This antisymmetry produces drift velocity fields that for positive particles converge on the heliospheric equator in the A+ state or diverge from it in A- state. Negatively charged particles behave in the opposite manner and the drift patterns interchange when the solar polarity diverge. 2) Systematic ordering of turbulent helicity can cause diffusion coefficients to depend directly on charge sign and polarity state. Bieber, J.W., et al. Phys. Rev. Letters, 84, 674, 1999.

38 Radiation Belts South Atlantic Anomaly Secondary production from CR interaction with atmosphere

39 Pamela maps at various altitudes
PRELIMINARY !!!! Altitude scanning

40 Primary and Albedo (sub-cutoff measurements)‏

41 Sub-cutoff

42 Size of SAA for altitudes between 350-600km
B<0.21Gs, L-shell <1.2 Latitude Altitudes changes from 350 to 600km Longitude

43 Proton spectrum in SAA, polar and equatorial regions

44 e+/e- ratio in the equatorial region (L<1.2, B>0.25)

45 Differential energy spectra of secondary electron and positron fluxes at the geomagnetic equator (L<1.2, B>0.25) Flux (a.u.) Fluxx

46

47 December 2006 Solar particle events
Dec 13th largest CME since 2003, anomalous at sol min

48 December 13th event Preliminary!

49 December 14th 2006 event Preliminary!
Magnetic Field Neutron Monitor X-ray P,e- December 14th event Magnetic Field Neutron Monitor X-ray P,e- Arrival of event of Dec 14th End of event of Dec 14th Decrease of primary spectrum Arrival of magnetic cloud from CME of Dec 13th Shock 1774km/s (gopalswamy, 2007) Decrease of Neutron Monitor Flux Low energy tail of Dec 13th event Solar Quiet spectrum Below galactic spectrum: Start of Forbush decrease Preliminary!

50 December 13th 2006 He differential spectrum
Preliminary!

51 Conferenze da Ottobre 2007 Presentazioni fatte dalla collaborazione internazionale
IEEE UCLA Dark Matter La Thuile Waseda Giappone Rencontre de Blois Vulcano COSPAR 2008 ICHEP SLAC Summer School IDM ISVHEC Parigi SIF CRIS TeV Texas Conf. (Dic.) + Conferenze Russe

52 Seminari Internazionali
Harvard FermiLab Nikhef Aachen Parigi (APC, Univ. 7) Entro Novembre Penn State Maryland Karlsrhue Kiel Corneil Stanford Michigan Durham CERN

53 Riunioni generali di analisi
Siegen Germania Firenze Bari Roma S. Pietroburgo Napoli Ottobre

54 Costi fissi ricorrenti
4 Gigabyte downlink aggiuntivo 60 Messi nel contratto INFN-RSA. Finanziamento annuale Commissione Turni tecnici russi a NTsOMZ Assistenza NTsOMZ Internet NtsOMZ MEPhI Consumi presso NTsOMZ Supporto GRID MEPhI Totale 238

55 Calcolo Potenziamento delle stazioni di calcolo locali.
137 k€ inventariabile

56 Costi ricorrenti Presenza a Mosca 21 .5 mesi 142.5 k€
Coordinamento estero Picozza k€ Coordinamento estero Boezio k€

57 Test GSI Missioni Estere 32 k€ Trasporto 6 k€ Materiale 5 k€
Totale k€

58 Riunioni di analisi riunioni di collaborazione: 3 in Italia 57.5
3 estere Riunione gruppi analisi: Coordinamento Picozza interno Boezio interno

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