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

D. Martello CSNII - 6 Aprile 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 KeV / 30 MeV-30 GeV AGILE : fotoni tra 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 TeV CREAM RC carichi ad energie TeV Sigle chiuse

D. Martello CSNII - 6 Aprile La radiazione cosmica nello spazio in CSNII: FTE – AGILE AMS CREAM FERMI PAMELA CR tot CSNII % CSNII

D. Martello CSNII - 6 Aprile La radiazione cosmica nello spazio in CSNII: Risorse 2006 – AGILE AMS CREAM FERMI PAMELA CR tot CSNII % EXP CSNII

D. Martello CSNII - 6 Aprile 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)

D. Martello CSNII - 6 Aprile 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)

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

D. Martello CSNII - 6 Aprile 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

D. Martello CSNII - 6 Aprile 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 The color code refers to the average gamma-ray intensity 12 months of data AGILE Gamma-Ray Catalog

D. Martello CSNII - 6 Aprile 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

D. Martello CSNII - 6 Aprile Gamma Ray Burst GRB B 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

D. Martello CSNII - 6 Aprile AGILE-GRID lightcurve above 100 MeV of the gamma-ray transient source AGL J that reached its peak on November 24, Time sequence of AGILE-GRID gamma-ray counts maps above100 MeV centered on the Eta Carinae region during the period October, 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

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) Fermi INFN Team coordinator

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

D. Martello CSNII - 6 Aprile GLAST renamed Fermi by NASA on August 26, “ Enrico Fermi ( ) … 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

D. Martello CSNII - 6 Aprile 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 International multi-agency mission

D. Martello CSNII - 6 Aprile 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-

D. Martello CSNII - 6 Aprile  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

D. Martello CSNII - 6 Aprile 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.

D. Martello CSNII - 6 Aprile 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

D. Martello CSNII - 6 Aprile 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 0.4MIPs 1% drift over 4 months CAL average 0-suppression 1% drift over 4 months

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

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

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

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

D. Martello CSNII - 6 Aprile 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

D. Martello CSNII - 6 Aprile GRB080916C GROND optical follow up [GCN 8257, 8272] Faint (21.7 mag at T 0 +32h) and fading (T d) source RA = ˚, Dec = − ˚ (±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’)

D. Martello CSNII - 6 Aprile 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

D. Martello CSNII - 6 Aprile 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

D. Martello CSNII - 6 Aprile 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 GeV energy range, with a potential profound impact on our understanding of galactic cosmic ray physics.

D. Martello CSNII - 6 Aprile 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 C A.A. Abdo, et al.

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

D. Martello CSNII - 6 Aprile    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

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

D. Martello CSNII - 6 Aprile

D. Martello CSNII - 6 Aprile Design Performance Energy range Antiprotons 80 MeV 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

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

D. Martello CSNII - 6 Aprile 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

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

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

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

D. Martello CSNII - 6 Aprile DM DM DM Pulsar DM / pulsar DM DM DM DM DM DM DM DM DM During first week after PAMELA results posted on arXiv )

D. Martello CSNII - 6 Aprile 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.

D. Martello CSNII - 6 Aprile 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

D. Martello CSNII - 6 Aprile 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

D. Martello CSNII - 6 Aprile 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

D. Martello CSNII - 6 Aprile PAMELA Proton Spectrum

D. Martello CSNII - 6 Aprile 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)

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

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

D. Martello CSNII - 6 Aprile Grigorov, Sov. Phys. Dokl. 22, NINA ApJ Supp , 2001 AMS Phys. Lett. B , Phys. Lett. B –22 Lipari, Astrop. Ph. 14, 171, 2000 Huang et al, Pys Rev. D 68, Sanuki et al, Phys Rev D Honda et al, Phys Rev D  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

D. Martello CSNII - 6 Aprile 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

D. Martello CSNII - 6 Aprile 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.

D. Martello CSNII - 6 Aprile 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

D. Martello CSNII - 6 Aprile   Timing Charge Detector (TCD) (Penn State Univ.) 5 mm thick fast (< 3 ns) plastic scintillator paddles charge measurement from H to Fe (  ~ 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 (  ~ 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)

D. Martello CSNII - 6 Aprile 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 

D. Martello CSNII - 6 Aprile 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

D. Martello CSNII - 6 Aprile Energy spectra of cosmic-ray nuclei Presented at the XV ISVHECRI Conference in Paris, Sept 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 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

D. Martello CSNII - 6 Aprile ISS febbraio 2009

D. Martello CSNII - 6 Aprile 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: VOLO PRECURSORE SULLO SHUTTLE AMS-02: CONFIGURAZIONE COMPLETA PER 3 ANNI DI PRESA DATI SULLA BASE SPAZIALE

D. Martello CSNII - 6 Aprile 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

D. Martello CSNII - 6 Aprile 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

D. Martello CSNII - 6 Aprile Test statici ABG

D. Martello CSNII - 6 Aprile Test statici ABG

D. Martello CSNII - 6 Aprile Tracciatore al silicio

D. Martello CSNII - 6 Aprile Lower ToF

D. Martello CSNII - 6 Aprile RICH

D. Martello CSNII - 6 Aprile ECAL

D. Martello CSNII - 6 Aprile Magnete FM

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

D. Martello CSNII - 6 Aprile November 12, 2008

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D. Martello CSNII - 6 Aprile 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.