Villa Mondragone, 30 Settembre 2008

Slides:

Advertisements

Similar presentations

ELENA VANNUCCINI ON BEHALF OF PAMELA COLLABORATION Measurement of the Hydrogen and Helium absolute fluxes with the PAMELA experiment.

Advertisements

E. Mocchiutti, INFN Trieste - CALOR th June 2006, Chicago E. Mocchiutti 1, M. Albi 1, M. Boezio 1, V. Bonvicini 1, J. Lund 2, J. Lundquist 1, M.

GLAST The GLAST Balloon Flight experiment was performed with the collaboration of NASA Goddard Space Flight Center, Stanford Linear Accelerator Center,

The Results of Alpha Magnetic Spectrometer (AMS01) Experiment in Space Behcet Alpat I.N.F.N. Perugia TAUP 2001 Laboratori Nazionali del Gran Sasso, Italy.

AMS Discoveries Affecting Cosmic-Ray SIG Priorities Eun-Suk Seo Inst. for Phys. Sci. & Tech. and Department of Physics University of Maryland AAS HEAD.

21 ECRS, Kosice, 12/09/2008 Trapped charge particles measurements in the radiation belt by PAMELA instrument Vladimir V. Mikhailov (MEPHI) for PAMELA collaboration.

Roberta Sparvoli, Sif Milano La missione NINA: misure di raggi cosmici di bassa energia in orbita terrestre Roberta Sparvoli per la Collaborazione.

Cosmic-Ray Antiproton Spatial Distributions Simulated in Magnetosphere Michio Fuki Faculty of Education, Kochi University 2-5-1, Akebono-cho, Kochi ,

PAMELA Payload for Antimatter Matter Exploration and Light Nuclei Astrophysics.

March 13thXXXXth RENCONTRES DE MORIOND 1 The Alpha Magnetic Spectrometer on the International Space Station Carmen Palomares CIEMAT (Madrid) On behalf.

Results from PAMELA Mirko Boezio INFN Trieste, Italy On behalf of the PAMELA collaboration Indirect and Direct Detection of Dark Matter February 7 th 2011.

The Time-of-Flight system of the PAMELA experiment: in-flight performances. Rita Carbone INFN and University of Napoli RICAP ’07, Rome,

ICHEP 2010, Paris, July 2010 Antiparticle Detection in Space for Dark Matter Search: the PAMELA Experiment Oscar Adriani University of Florence INFN.

PAMELA – a satellite experiment searching for dark matter with cosmic ray antiparticles Mark Pearce KTH, Department of Physics, Stockholm, Sweden For the.

HEAD 2010 – Mar.3, 2010 :: IVM/Stanford-KIPAC 1IVM/Stanford-KIPAC 1 PAMELA Workshop, Rome/May 12, 2009 Igor V. Moskalenko (stanford/kipac) Leptons in Cosmic.

March 13thXXXXth RENCONTRES DE MORIOND 1 The Alpha Magnetic Spectrometer on the International Space Station Carmen Palomares CIEMAT (Madrid) On behalf.

Aspen 4/28/05Physics at the End of the Galactic Cosmic Ray Spectrum - “Below the Knee” Working Group “Below the Knee” Working Group Report - Day 3 Binns,

Antimatter in Space Antimatter in Space Mirko Boezio INFN Trieste, Italy PPC Torino July 14 th 2010.

The PLANETOCOSMICS Geant4 application L. Desorgher Physikalisches Institut, University of Bern.

R. Sparvoli – MAPS Perugia Outline of the lecture Lecture 2: Sources of background and their rejection Efficiencies & Contaminations Absolute fluxes.

Measurements of Cosmic-Ray Positrons & Electrons An Experimentalist’s Point of View Michael Schubnell University of Michigan February 4 th, 2009 XLIVth.

Roberta Sparvoli University of Rome “Tor Vergata” and INFN Rome, Italy

PAMELA SPACE MISSION ICHEP 2006 MOSCOW Piergiorgio Picozza Pamela collaboration INFN & University of Roma “Tor Vergata”

P. Bobik, G. Boella, M. J. Boschini, M. Gervasi, D. Grandi, K. Kudela, S. Pensotti, P.G. Rancoita 2D Stochastic Monte Carlo to evaluate the modulation.

The PAMELA Experiment: Preliminary Results after Two Years of Data Taking Emiliano Mocchiutti - INFN Trieste on behalf of the PAMELA Collaboration.

Vladimir Mikhailov (NRNU MEPHI, Moscow) On behavior PAMELA collaboration SUB CUTOFF SPECTRA OF ELECTRONS AND POSITRONS measured in the PAMELA experiment.

Aa GLAST Particle Astrophysics Collaboration Instrument Managed and Integrated at SLAC/Stanford University The Gamma-ray Large Area Space Telescope (GLAST)

Trapped positrons and electrons observed by PAMELA Vladimir Mikhailov NRNU MEPHI, Moscow, Russia For PAMELA collaboration ICPPA 2015, PAMELA workshop,

PAMELA Space Mission Antimatter and Dark Matter Research Piergiorgio Picozza INFN & University of Rome “ Tor Vergata”, Italy TeV Particle Astrophysics.

The Science and First Results of the PAMELA Space Mission The Science and First Results of the PAMELA Space Mission Mirko Boezio INFN Trieste, Italy On.

The Alpha Magnetic Spectrometer (AMS) on the International Space Station (ISS) Maria Ionica I.N.F.N. Perugia International School.

Cosmic Ray Study The PAMELA Experiment Piergiorgio Picozza INFN and University of Rome Tor Vergata 23 rd European Cosmic Ray Symposium Moscow, Russia July.

Antimatter and Dark Matter Searches in Space: the PAMELA Space Mission Antimatter and Dark Matter Searches in Space: the PAMELA Space Mission Piergiorgio.

RCCN International Workshop sub-dominant oscillation effects in atmospheric neutrino experiments 9-11 December 2004, Kashiwa Japan Input data to the neutrino.

H, He, Li and Be Isotopes in the PAMELA-Experiment Wolfgang Menn University of Siegen On behalf of the PAMELA collaboration International Conference on.

GLAST The GLAST Balloon Flight experiment was performed with the collaboration of NASA Goddard Space Flight Center, Stanford Linear Accelerator Center,

1. 2 ISS-present status Trent Martin NASA AMS Project Manager.

High-energy Electron Spectrum From PPB-BETS Experiment In Antarctica Kenji Yoshida 1, Shoji Torii 2 on behalf of the PPB-BETS collaboration 1 Shibaura.

Direct measurements of cosmic rays in space ROBERTA SPARVOLI ROME “TOR VERGATA” UNIVERSITY AND INFN, ITALY Vulcano Workshop 2014 Vulcano Island (Italy),

La missione PAMELA: primi risultati scientifici Paolo Papini INFN – Firenze a nome della collaborazione PAMELA XCIV Congresso Nazionale Società Italiana.

Cosmic Ray Positron Fraction Observations during the A- Magnetic Solar Minimum John Clem and Paul Evenson* * Presenter AESOP Departing Esrange, Sweden.

Rita Carbone, RICAP 11, Roma 3 26/05/2011 Stand-alone low energy measurements of light nuclei from PAMELA Time-of-Flight system. Rita Carbone INFN Napoli.

The high-energy antiproton-to-proton flux ratio with the PAMELA experiment Massimo Bongi INFN - Florence Payload for Antimatter/Matter Exploration and.

HIGH ENERGY POSITRON DETECTION VIA SYNCHROTRON RADIATION IN MAGENTOSPHERE “SONYA” project А.М. Гальпер 1, О.Ф. Прилуцкий 2, С.В. Колдашов 1, В.В. Михайлов.

Topicality of this work is caused by the fact that modern detectors aren't effective in searching electrons and positrons with energies higher than 1 TeV.

Antiproton and Electron Measurements and Dark Matter Searches

Roberta Sparvoli University of Rome ”Tor Vergata” and INFN

The PAMELA Experiment: a Cosmic-Ray Experiment Deep Inside the Heliosphere Mirko Boezio INFN Trieste, Italy On behalf of the PAMELA collaboration ICRC.

Solar modulation of cosmic ray positrons in a quiet heliosphere

The Transition Radiation Detector for the PAMELA Experiment

Understanding CRs with Space Experiments

INFN & University of Roma “Tor Vergata”

Search for Cosmic Ray Anisotropy with the Alpha Magnetic Spectrometer on the International Space Station G. LA VACCA University of Milano-Bicocca.

The PAMELA space experiment: results after seven years in orbit Mirko Boezio INFN Trieste, Italy On behalf of the PAMELA collaboration INFN-Space/3,

INFN e Università di Roma Tor Vergata

Imaging Dark Matter with the Pamela Experiment

Solar Modulation Davide Grandi AMS Group-INFN Milano-Bicocca.

Roberta Sparvoli University of Rome ”Tor Vergata” and INFN

Secondary positrons and electrons measured by PAMELA experiment

Cosmic-Ray Lithium and Beryllium Isotopes in the PAMELA-Experiment

Measurements of Cosmic-Ray Lithium and Beryllium Isotopes

Vladimir Mikhailov (MEPhI) on behalf PAMELA collaboration

for the PAMELA collaboration

Results from the PAMELA space experiment

Calorimetry in space with PAMELA

A. Bruno and F. Cafagna on behalf of the PAMELA collaboration

Recent results on antiparticles in cosmic rays from PAMELA experiment

ICRC2003 OG Calculation of Cosmic-Ray Proton and Anti-proton Spatial Distribution in Magnetosphere Michio Fuki, Ayako Kuwahara, Nozomi, Sawada Faculty.

On the variations of the magnetospheric field line resonance frequency

Presentation transcript:

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

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

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?)

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

Antiprotoni

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

PAMELA Protons Spillover

Antiproton-Proton Ratio PAMELA Preliminary

Antiproton to proton ratio Preliminary

Antiproton to proton ratio Preliminary

Positroni

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

Flight data: 92 GeV/c positron

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

Positron selection with calorimeter Rigidity: 20-30 GV e- p (non-int) p (int) Total negative  3067 Total positive  189055 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

Positron selection with calorimeter Rigidity: 20-30 GV e- e+ Total negative  3067 Total positive  189055 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

Positron selection with calorimeter Rigidity: 20-30 GV e- e+ Total negative  3067 Total positive  189055 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

Positron selection with calorimeter Fraction of charge released along the calorimeter track (left, hit, right) Flight data: rigidity: 20-30 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

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

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: 10-15 GV Rigidity: 15-20 GV Mirko Boezio, IDM2008, 2008/08/20 Mirko Boezio, IDM2008, 2008/08/20

e+ background estimation from data Rigidity: 20-30 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

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

Positron to Electron Fraction Preliminary!!! Charge sign dependent solar modulation End 2007: ~20 000 positrons total Mirko Boezio, IDM2008, 2008/08/20 Mirko Boezio, IDM2008, 2008/08/20

Positrons with HEAT

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

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

Galactic H and He spectra Preliminary !!!

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, 051101), Bieber, J.W., et al. Physi-cal Review Letters, 84, 674, 1999. J. Clem et al. 30th ICRC 2007

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

Charge dependent solar modulation Preliminary!! ¯ + ¯ +

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

A > 0 Positive particles A < 0

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.

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

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

Primary and Albedo (sub-cutoff measurements)‏

Sub-cutoff

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

Proton spectrum in SAA, polar and equatorial regions

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

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

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

December 13th 2006 event Preliminary!

December 14th 2006 event Preliminary! Magnetic Field Neutron Monitor X-ray P,e- December 14th 2006 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!

December 13th 2006 He differential spectrum Preliminary!

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 2008 ISVHEC Parigi SIF CRIS TeV 2008 Texas Conf. (Dic.) + Conferenze Russe

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

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

Costi fissi ricorrenti 4 Gigabyte downlink aggiuntivo 60 Messi nel contratto INFN-RSA. Finanziamento annuale Commissione Turni tecnici russi a NTsOMZ 48 Assistenza NTsOMZ 50 Internet NtsOMZ MEPhI 40 Consumi presso NTsOMZ 25 Supporto GRID MEPhI 15 Totale --------------------------------------------- 238

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

Costi ricorrenti Presenza a Mosca 21 .5 mesi 142.5 k€ Coordinamento estero Picozza 25 k€ Coordinamento estero Boezio 10 k€

Test GSI Missioni Estere 32 k€ Trasporto 6 k€ Materiale 5 k€ Totale 43 k€

Riunioni di analisi riunioni di collaborazione: 3 in Italia 57.5 3 estere 112.5 Riunione gruppi analisi: 104 Coordinamento Picozza 12 interno Boezio 3 interno