Attività sperimentali e prospettive future su raggi cosmici nello spazio D. Martello Univ & INFN Lecce Pisa 6 Aprile 2009.

Presentazione sul tema: "Attività sperimentali e prospettive future su raggi cosmici nello spazio D. Martello Univ & INFN Lecce Pisa 6 Aprile 2009."— Transcript della presentazione:

1 Attività sperimentali e prospettive future su raggi cosmici nello spazio D. Martello Univ & INFN Lecce Pisa 6 Aprile 2009

2 D. Martello CSNII - 6 Aprile 2009 2 Sigle attive Satelliti:Satelliti: PAMELA : RC carichi ad energie 0.1 GeV » TeV PAMELA : RC carichi ad energie 0.1 GeV » TeV AGILE : fotoni tra 18-60 KeV / 30 MeV-30 GeV AGILE : fotoni tra 18-60 KeV / 30 MeV-30 GeV FERMI : fotoni 10 KeV – 25 MeV / 20 MeV – 300 GeV FERMI : fotoni 10 KeV – 25 MeV / 20 MeV – 300 GeV Stazione Spaziale:Stazione Spaziale: AMS: RC carichi ad energie GeV-TeV fotoni ad energie GeV-100 GeV fotoni ad energie GeV-100 GeV Palloni stratosferici : Palloni stratosferici : CREAM RC carichi ad energie 1-500 TeV CREAM RC carichi ad energie 1-500 TeV Sigle chiuse

3 D. Martello CSNII - 6 Aprile 2009 3 La radiazione cosmica nello spazio in CSNII: FTE – 2006-2009 2006200720082009 AGILE13.513.913.59.1 AMS-0242.542.143.147.4 CREAM6.88.75.23.2 FERMI39.340.940.951.2 PAMELA29.928.12835.9 CR tot 132133.7130.7146.8 CSNII582.4602.9611.0600.7 % CSNII 22.722.121.424.4

4 D. Martello CSNII - 6 Aprile 2009 4 La radiazione cosmica nello spazio in CSNII: Risorse 2006 – 2009 2006200720082009 AGILE118.399.57966.5 AMS-02765.11048712554 CREAM118.812233 FERMI732.8644762650 PAMELA646.4731.5598.5616.5 CR tot 2381.425352174.51890 CSNII17544166471582314059 % EXP CSNII 13.615.213.713.4

5 D. Martello CSNII - 6 Aprile 2009 5 The AGILE Mission Sriharikota launch base (India) PSLV-C8 launch, April 23, 2007 INAF-IASF Milano INAF-IASF Bologna INAF-IASF Roma INFN- Sez. Trieste INFN- Sez. Roma I INFN- Sez. Roma II INFN- Sez. Pavia Università di Trieste Università di Roma “Tor Vergata” Università “La Sapienza” CIFS - Consorzio Interuniversitario per la Fisica Spaziale (Torino)

6 D. Martello CSNII - 6 Aprile 2009 6 AGILE: inside the cube… ANTICOINCIDENCE INAF-IASF-Mi (F.Perotti) HARD X-RAY IMAGER (SUPER-AGILE) INAF-IASF-Rm (E.Costa, M. Feroci) GAMMA-RAY IMAGER SILICON TRACKER INFN-Trieste (G.Barbiellini, M. Prest) (MINI) CALORIMETER INAF-IASF-Bo, Thales- Alenia Space (LABEN) (G. Di Cocco, C. Labanti)

7 D. Martello CSNII - 6 Aprile 2009 7 AGILE orbital parameters Equatorial Orbit: 2.48° @ 540 km a.s.l. Low particle background ! Measured particle background in orbit confirms expectations: better by a factor of ~2-3. SIMU

8 D. Martello CSNII - 6 Aprile 2009 8 The gamma-ray sky in Galactic coordinates above 100 MeV detected by AGILE during its first 9 months of operations (July 2007-March 2008). 9 months of data AGILE Gamma-Ray Sky Submitted to Il Saggiatore

9 D. Martello CSNII - 6 Aprile 2009 9 First AGILE-GRID Catalog of high-confidence gamma-ray sources detected during Cycle-1. The sources were obtained by integrating all data during the period July 2007 – June 2008. The color code refers to the average gamma-ray intensity 12 months of data AGILE Gamma-Ray Catalog

10 D. Martello CSNII - 6 Aprile 2009 10 Multiwave analysis of Markarian 421 june 2008 flare Spectral energy distribution showing two different states of emission. Multifrequency detection of Mrk 421 by AGILE and by MAGIC-VERITAS, BAT, ASM, and WEBT during the period 9-15 June, 2008 Hard X-ray lightcurve (top panel) and gammaray/TeV lightcurve (middle panel), and X-ray hardness ratio (bottom panel) Astrophys.J.Lett.691:L13-L19,2009

11 D. Martello CSNII - 6 Aprile 2009 11 Gamma Ray Burst GRB 080514B Several tens of GRBs were detected during Cycle- 1 by Super-AGILE and MCAL, but only one so far was clearly detected in the energy range above 100 MeV, a clear indication of the rarity of strong GRB gamma-ray emission. This gamma ray burst showed an afterglow counterpart at X- rays and in the optical, and a measured distance (from the photometric redshift) of z=1.8. Giuliani, A., et al., A&A, 491, 25L (2008) GRB 080721

12 D. Martello CSNII - 6 Aprile 2009 12 AGILE-GRID lightcurve above 100 MeV of the gamma-ray transient source AGL J2022-3622 that reached its peak on November 24, 2007. Time sequence of AGILE-GRID gamma-ray counts maps above100 MeV centered on the Eta Carinae region during the period 10-17 October, 2008. The time sequence starts at the upper left corner and each map corresponds to a 2-day integration. The color bar scale is in units of counts cm-2 s-1 pixel-1. Gamma Ray Transient in the Galactic Plane

13 CSNII - 6 Aprile 2009 Science Highlights from the first six months of operations of the Fermi observatory Riunione Commissione Scientifica Nazionale II Cascina - Pisa Cascina - Pisa 6-8 Aprile 2009 Ronaldo Bellazzini (INFN-Pisa) ronaldo.bellazzini@pi.infn.it Fermi INFN Team coordinator

14 D. Martello CSNII - 6 Aprile 2009 14 … and then … Launch from Cape Canaveral Air Station 11 June 2008 at 12:05PM EDT

15 D. Martello CSNII - 6 Aprile 2009 15 GLAST renamed Fermi by NASA on August 26, 2008 http://fermi.gsfc.nasa.gov/ “ Enrico Fermi (1901-1954) … was the first to suggest a viable mechanism for astrophysical particle acceleration. This work is the foundation for our understanding of many types of sources to be studied by the Fermi Gamma-ray Space Telescope, formerly known as GLAST. ” “ Questo nuovo nome e' stato selezionato con un sondaggio pubblico realizzato dalla NASA e che ha ricevuto piu' di 12 mila risposte. Oltre ad avere un legame diretto con la scienza dei raggi-gamma della nostra nuova missione, Fermi ha un significato speciale per il DoE, l'ASI e l'INFN, tre agenzie che hanno maggiormente contribuito alla missione" DoE – NASA – international partnership

16 D. Martello CSNII - 6 Aprile 2009 16 FERMI – The Key Facts Instruments on board –Large Area Telescope (LAT) –20MeV – >300GeV –Gamma Burst Monitor –10KeV – 30MeV Observing strategy –Survey + Pointing (Autonomous Repoint Request, Target of Opportunities) FERMI at NASA-KSFC for final preparation for launch on may 16 2008 International multi-agency mission

17 D. Martello CSNII - 6 Aprile 2009 17 Modular design of LAT p 4x4 array of identical towers each one including a Tracker a Calorimeter and an Electronics Module. p Surrounded by an Anti-Coincidence shield (not shown in the picture).  e+e+ e-e-

18 D. Martello CSNII - 6 Aprile 2009 18  e+e+ e-e- Tracker/Converter (TKR): Silicon strip detectors (single sided, each layer is rotated by 90 degrees with respect to the previous one) W conversion foils ~80 m 2 of silicon ~10 6 electronics chans fully digital electronics High precision tracking, small dead time Calorimeter (CAL): 1536 CsI crystals Analog 4 range readout 8.5 X0 Hodoscopic Shower profile reconstruction (leakage correction) Modular design of LAT

19 D. Martello CSNII - 6 Aprile 2009 19 Operating modes Primary observing mode is Sky Survey –Full sky every 2 orbits (3 hours) –Uniform exposure, with each region viewed for ~30 minutes every 2 orbits –Best serves majority of science, facilitates multiwavelength observation planning –Exposure intervals commensurate with typical instrument integration times for sources –EGRET sensitivity reached in days Pointed observations when appropriate (selected by peer review in later years) with automatic earth avoidance selectable. Target of Opportunity pointing. Autonomous repoints for onboard GRB detections in any mode.

20 D. Martello CSNII - 6 Aprile 2009 20 Year 1 Science Operations Timeline Overview L AUNCH L +60 days week week week week month 12 m o n t h s spacecraft turn-on checkout LAT, GBM turn-on check out “first light” whole sky initial tuning/calibrations pointed + sky survey tuning Start Year 1 Science Ops Start Year 2 Science Ops in-depth instrument studies sky survey + ~weekly GRB re-points + extraordinary TOOs Release Flaring and Monitored Source Info GBM and LAT GRB Alerts continuous release of new photon data Observatoryrenaming GI Cycle 1 Funds Release Fellows Year 1 Start LAT 6-month high-confidence source release, GSSC science tools advance release GI Cycle 2 Proposals LAT Year 1 photon data release PLUS LAT Year 1 Catalog and Diffuse Model 2ndSymposium June 11, 2008 August 12, 2009

21 D. Martello CSNII - 6 Aprile 2009 21 Instrument performance and calibration   No evidence of a reduction in hit efficiency (well above 99% on average)   No significant change in the alignment constants (intra and inter-tower) after the launch (the LAT underwent up to 4 g acceleration + vibration)   No evidence of any increase in the overall noise level (~1 noise hit per event for the full LAT)   remarkable stability of CAL and ACD ACD veto @ 0.4MIPs 1% drift over 4 months CAL average 0-suppression 1% drift over 4 months

22 FERMI Gamma-Ray Sky Front > 200 MeV, Back > 400 MeV PRELIMINARY Submitted to ApJS - also on arXiv:0902.1340 3 months of data

23 D. Martello CSNII - 6 Aprile 2009 23 205 sources arXiv:0902.1340v1 [astro-ph.HE] 8 Feb 2009 3 months of data

24 D. Martello CSNII - 6 Aprile 2009 24 The Pulsing Sky 3 months of data

25 D. Martello CSNII - 6 Aprile 2009 25 GRB080916C: the bright one [GCN 8246 – Tajima, H., Bregeon J. et al., GCN 8245, 8278 – Goldstein, A. et al.] GRB 080916C GRB080825C GRB081024B GRB090217: the recent one [GCN 8903 – Masanori Ohno et al.] 5

26 D. Martello CSNII - 6 Aprile 2009 26 8 keV – 260 keV 260 keV – 5 MeV LAT raw LAT > 100 MeV LAT > 1 GeV T0T0 The first low-energy peak is not observed at LAT energies 14 events above 1 GeV The bulk of the emission of the 2 nd peak is moving toward later times as the energy increases Clear signature of spectral evolution new era of GeV GRB lightcurves! GRB080916C

27 D. Martello CSNII - 6 Aprile 2009 27 GRB080916C GROND optical follow up [GCN 8257, 8272] Faint (21.7 mag at T 0 +32h) and fading (T 0 +3.3d) source RA = 119.8472˚, Dec = −56.6383˚ (±0.5” at 68% C.L.)‏ Photometric redshift of z=4.2 +/- 0.3 (12B light years from us!) Large fluence (2.4×10 -4 erg/cm 2 ) & redshift (z = 4.35 ± 0.15)  record breaking apparent isotropic energy release E γ,iso ≈ 8.8×10 54 erg ≈ 4.9 M  c 2  suggests strong beaming (jet)  record breaking highest lower limit on Γ from opacity constraints (w/o considering EBL) Γ min ≈ 890 ± 20 (bin ‘b’, for  t = 2 s) & Γ min ≈ 600 (bin ‘d’)

28 D. Martello CSNII - 6 Aprile 2009 28 Not only  -rays in the LAT - high energy CR electrons The LAT can operate as “high energy electron telescope” –Photon reconstruction works perfectly for electrons –All events above ~20 GeV are downlinked Advantages: –Large collecting area –Continuous (high duty cycle) and long observation –No atmospheric correction Disadvantages –can not separate electrons from positrons

29 D. Martello CSNII - 6 Aprile 2009 29 What we can see Simulation of less than 30 days of on orbit operations The solid line is the primary electron model used in the simulation –Spectral index -3.3 above the geomagnetic cutoff Unprecedented high statistics data sample –Several millions of electrons above 20GeV after selection cuts in 6 months –>2.5k events above 500 GeV –Compared with few thousands from balloon experiments in the whole energy range SIMULATION

30 D. Martello CSNII - 6 Aprile 2009 30 The result Embargoed at the present stage! –Final spectrum is beautiful with extraordinary accuracy –will set the stage for modelling CR generation and propagation –Submission of paper to PRL in march –APS / TANGO-Paris May 2009 first public announcement –A comment to the paper draft (not from the authors ….) –It is anyway evident that Fermi data is providing unprecedented accuracy in the determination of the electron-positron spectrum in the 20-1000 GeV energy range, with a potential profound impact on our understanding of galactic cosmic ray physics.

31 D. Martello CSNII - 6 Aprile 2009 31 The Fermi voice Post-launch Papers 2 published by Science 4 accepted by ApJ –Already available on astro-ph 10 submitted 5 hot or close to submission Fermi observations of high-energy gamma-ray emission from GRB 080916C A.A. Abdo, et al.

32 D. Martello CSNII - 6 Aprile 2009 32 PAMELA Payload for Antimatter Matter Exploration and Light Nuclei Astrophysics

33 D. Martello CSNII - 6 Aprile 2009 33    km  km SAA Low-earth elliptical orbit Low-earth elliptical orbit 350 – 610 km 350 – 610 km Quasi-polar (70 o inclination) Quasi-polar (70 o inclination) Lifetime >3 years (assisted) Lifetime >3 years (assisted) Le caratteristiche dell’orbita

34 D. Martello CSNII - 6 Aprile 2009 34 Bari Florence Frascati Italy: Trieste Naples Rome CNR, Florence Moscow St. Petersburg Russia: Germany: Siegen Sweden: KTH, Stockholm La collaborazione Internazionale

35 D. Martello CSNII - 6 Aprile 2009 35

36 D. Martello CSNII - 6 Aprile 2009 36 Design Performance Energy range Antiprotons 80 MeV - 150 GeV Positrons 50 MeV – 300 GeV Electrons up to 500 GeV Protons up to 700 GeV Electrons+positrons up to 2 TeV (from calorimeter) Light Nuclei (He/Be/C) up to 200 GeV/n AntiNuclei search sensitivity of 3x10 -8 in He/He   Simultaneous measurement of many cosmic-ray species   New energy range   Unprecedented statistics

37 D. Martello CSNII - 6 Aprile 2009 37 PAMELA Launch 15/06/06 16 Gigabytes trasmitted daily to Ground NTsOMZ Moscow

38 D. Martello CSNII - 6 Aprile 2009 38 The Physics of PAMELA Study of solar physics and solar modulation Study of terrestrial magnetosphere Study of high energy electron spectrum (local sources?) Search for dark matter annihilation Search for antihelium (primordial antimatter)‏ Search for new Matter in the Universe (Strangelets?) Study of cosmic-ray propagation

39 D. Martello CSNII - 6 Aprile 2009 39 Antiproton to proton ratio PRL 102, 051101 (2009)

40 D. Martello CSNII - 6 Aprile 2009 40 Antiproton Flux Preliminary statistical errors only energy in the spectrometer

41 D. Martello CSNII - 6 Aprile 2009 41 Positron to Electron Ratio astro-ph 0810.4995

42 D. Martello CSNII - 6 Aprile 2009 42 0808.3725 DM 0808.3867 DM 0809.2409 DM 0810.2784 Pulsar 0810.4846 DM / pulsar 0810.5292 DM 0810.5344 DM 0810.5167 DM 0810.5304 DM 0810.5397 DM 0810.5557 DM 0810.4147 DM 0811.0250 DM 0811.0477 DM During first week after PAMELA results posted on arXiv )

43 D. Martello CSNII - 6 Aprile 2009 43 25 GeV 35 GeV PAMELA data analysis Calorimeter energy fraction, F. The fraction of calorimeter energy deposited inside a cylinder of radius 0.3 Moliere radii, as a function of deflection.

44 D. Martello CSNII - 6 Aprile 2009 44 A DM with: -mass MD M = 1TeV -annihilation DM DM μ + μ− Which DM spectra can fit the data ? Nima Arkani-HamedNima Arkani-Hamed et al. Phys.Rev.D79:015014,2009 A. Cirelli

45 D. Martello CSNII - 6 Aprile 2009 45 We have argued that dark matter physics is far richer than usually thought, involving a multiplet of states and a new sector of dark forces. We have been led to propose this picture not by a flight of fancy but rather directly from experimental data. Even so, one can justifiably ask whether such extravagances are warranted. After all, experimental anomalies come and go, and it is entirely possible that the suite of hints that motivate our proposal are incorrect, or that they have more conventional explanations. However, we are very encouraged by the fact that the theory we have presented fits into a very reasonable picture of particle physics, is supported by overlapping pieces of experimental evidence, and that features of the theory motivated by one set of experimental anomalies automatically provide the ingredients to explain the others… Nima Arkani-HamedNima Arkani-Hamed et al. Phys.Rev.D79:015014,2009

46 D. Martello CSNII - 6 Aprile 2009 46 Secondary production Moskalenko & Strong 98 Pulsar Component Atoyan et al. 95 Pulsar Component Zhang & Cheng 01 Pulsar Component Yüksel et al. 08 KKDM (mass 300 GeV) Hooper & Profumo 07 PAMELA Positron Fraction

47 D. Martello CSNII - 6 Aprile 2009 47 PAMELA Proton Spectrum

48 D. Martello CSNII - 6 Aprile 2009 48 Solar modulation Interstellar spectrum July 2006 August 2007 February 2008 Decreasing solar activity Increasing GCR flux sun-spot number Ground neutron monitor PAMELA (statistical errors only)

49 D. Martello CSNII - 6 Aprile 2009 49 December 13th 2006 event Solar Flare Preliminary!

50 D. Martello CSNII - 6 Aprile 2009 50 Preliminary! December 13th 2006 He differential spectrum December 13th 2006 He differential spectrum

51 D. Martello CSNII - 6 Aprile 2009 51 Grigorov, Sov. Phys. Dokl. 22, 305 1977 NINA ApJ Supp.132 365, 2001 AMS Phys. Lett. B 472 2000.215, Phys. Lett. B 484 2000.10–22 Lipari, Astrop. Ph. 14, 171, 2000 Huang et al, Pys Rev. D 68, 053008 2003 Sanuki et al, Phys Rev D75 043005 2007 Honda et al, Phys Rev D75 043006 2007  Atmospheric neutrino contribution  Astronaut dose on board International Space Station   Indirect measurement of cross section in the atmosphere   Agile e Fermi background cross-check --- M. Honda, 2008 Proton flux at various cutoffs

52 D. Martello CSNII - 6 Aprile 2009 52 Secondary nuclei B nuclei of secondary origin: CNO + ISM  B + … Local secondary/primary ratio sensitive to average amount of traversed matter (l esc ) from the source to the solar system Local secondary abundance:   study of galactic CR propagation (B/C used for tuning of propagation models) Preliminary

53 D. Martello CSNII - 6 Aprile 2009 53 GR2 - 27/6/07 Cosmic Ray Energetics And Mass Il gruppo collegato di Siena alla sezione INFN-Pisa ha partecipato ai primi due voli antartici di CREAM nel 2004 (42 giorni di volo) e 2005 (28 giorni). Attualmente il gruppo sta concludendo l’analisi dati.

54 D. Martello CSNII - 6 Aprile 2009 54 Command and Data Module (CDM) CREAM can measure individual energy spectra and elemental composition (1 ≤ Z ≤ 26 and above) of cosmic rays up to hundreds of TeV   3 independent charge measurements : Timing-based Charge Detector (TCD) Pixelated Silicon Detector (SCD) Scintillating fiber Hodoscopes   2 independent energy measurements : Transition Radiation Detector (Z > 3) Tungsten Sci-Fi calorimeter (Z ≥ 1)   Tracking provided by TRD and CAL   Collecting power ~ 0.3 m 2 sr for Z=1, 2 ~ 1.3 m 2 sr for Z>3   S2 hodoscope (INFN) CREAM-I instrument

55 D. Martello CSNII - 6 Aprile 2009 55   Timing Charge Detector (TCD) (Penn State Univ.) 5 mm thick fast (< 3 ns) plastic scintillator paddles charge measurement from H to Fe (  ~ 0.2-0.35 e) backscatter rejection by fast pulse shaping   Silicon Charge Detector (SCD) (Ewha Womans University) ● ● 2 planes, 2916 Si pixels each Active area ~ 0.65 m 2 ● ● charge measurement from Z=1 to Z~33 (  ~ 0.1-0.2 e)   Cerenkov counter (University of Chicago, GSFC) 1 cm thick plastic radiator with blue wavelength shifter low energy particles veto CREAM-2 Instrument Tungsten-SciFi Calorimeter (INFN)   50 × 50 cm 2   3.5 mm W (1 X 0 )   0.5 mm Sci-Fibers   1 cm granularity   20 layers 20 X 0, ~ 0.7     2560 channels (40 HPDs)

56 D. Martello CSNII - 6 Aprile 2009 56 Black circles CREAM-I Red stars HEAO-3-C2 Boron to carbon abundance ratio    The lines in the plot represent leaky- box propagation model calculations for various values of the magnetic- rigidity dependence parameter, , in escape from the Galaxy. CREAM-I measured the B/C ratio up to an energy of 1.5 TeV/ n [Ahn et al., Astroparticle Physics 30 (2008) 133] The results indicate that the interstellar propagation pathlength decreases fairly rapidly with energy, with an energy dependence (E -  ) in the range  0.5 - 0.6

57 D. Martello CSNII - 6 Aprile 2009 57 Black circles CREAM-I Red stars HEAO-3-C2 Ahn et al., Astroparticle Physics 30 (2008) 133 N/O = 10% N/O = 15% N/O = 5% The lines in the plot represent model calculations of N/O ratio with the escape parameter  = 0.6. The different curves correspond to different assumptions on the amount of nitrogen in the source material. CREAM-I measurement of N/O up to 1.5 TeV/n suggests a N/O source abundance close to 10%, larger than some previous estimates based on lower-energy isotope measurements. Nitrogen to oxygen abundance ratio

58 D. Martello CSNII - 6 Aprile 2009 58 Energy spectra of cosmic-ray nuclei Presented at the XV ISVHECRI Conference in Paris, Sept. 2008 In press in Nucl. Phys. B (Proc. Suppl.) CREAM-II measured the absolute intensities of C, O, Ne, Mg, Si, Fe in the particle energy range 800 GeV - 100 TeV. Energy spectra of more abundant heavy nuclei in cosmic rays are well fitted to power-laws with very similar spectral indexes. The average spectral index is: 2.66 ± 0.04

59 D. Martello CSNII - 6 Aprile 2009 59 ISS febbraio 2009

60 D. Martello CSNII - 6 Aprile 2009 60 AMS A LPHA M AGNETIC S PECTROMETER  Ricerca di anti-materia di origine primordiale   Ricerca indiretta di materia oscura   Misura di precisione dello spettro energetico e della composizione dei raggi cosmici dal GeV al TeV AMS-01: 1995-1998 VOLO PRECURSORE SULLO SHUTTLE AMS-02: 1999-2010 CONFIGURAZIONE COMPLETA PER 3 ANNI DI PRESA DATI SULLA BASE SPAZIALE

61 D. Martello CSNII - 6 Aprile 2009 61 AMS-02 : il rivelatore Accettanza: » 0.5 m 2 sr (» 200 volte PAMELA) Bending power » 0.8 Tm 2 TOF : trigger, , dE/dx (Z) Tracker: § Q, R, dE/dx (Z<26) RICH : , Z ECAL : E, e/p TRD: e/p

62 D. Martello CSNII - 6 Aprile 2009 62 Time of Flight F. Palmonari, Bologna TRD B. Borgia, Rome Silicon Tracker R. Battistion, Perugia Calorimeter F. Cervelli, Pisa Magnet RICH G. Laurenti, Bologna Requires ¼ of a shuttle to ISS AMS on ISS Italian participation

63 D. Martello CSNII - 6 Aprile 2009 63 Test statici ABG

64 D. Martello CSNII - 6 Aprile 2009 64 Test statici ABG

65 D. Martello CSNII - 6 Aprile 2009 65 Tracciatore al silicio

66 D. Martello CSNII - 6 Aprile 2009 66 Lower ToF

67 D. Martello CSNII - 6 Aprile 2009 67 RICH

68 D. Martello CSNII - 6 Aprile 2009 68 ECAL

69 D. Martello CSNII - 6 Aprile 2009 69 Magnete FM

70 D. Martello CSNII - 6 Aprile 2009 70 I. AMS Preintegrazione 2008

71 D. Martello CSNII - 6 Aprile 2009 71 November 12, 2008

72 D. Martello CSNII - 6 Aprile 2009 72 November 12, 2008 …..

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76 D. Martello CSNII - 6 Aprile 2009 76 Conclusioni AGILE, FERMI, PAMELA in presa dati. Grande quantita’ di risultati in molti campi che stanno monopolizzando l’interesse della comunita’.AGILE, FERMI, PAMELA in presa dati. Grande quantita’ di risultati in molti campi che stanno monopolizzando l’interesse della comunita’. AMS-02 in avanzata fase di integrazione ormai si prepara al lancio.AMS-02 in avanzata fase di integrazione ormai si prepara al lancio. Il contributo della CSN2 e’ sicuramente di grandissima rilevanza internazionale.Il contributo della CSN2 e’ sicuramente di grandissima rilevanza internazionale.