Particle Physics with Space Detectors

Transcription

1 Particle Physics with Space Detectors Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 1

2 Basic problem: To study gamma ray and cosmic ray in the MeV- GeV range you need to go outside the atmosphere Why you want to study these items if you are a particle physicist? Nature of Dark Matter (possible connection with supersymmetry) Quantum gravity limits Cosmic accelerators Matter antimatter asymmetry Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 2

3 Cosmic Accelerators Man-made Accelerators Cosmic Accelerators GRB? Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 3

4 What is the Universe made of? Bright stars: 0.5% Baryons (total): 4.4% ± 0.4% Matter: 27% ± 4% Cold Dark Matter: 22.6% ± 4% Neutrinos: < 0.15% Dark Energy: 73% ± 6% h= astro-ph W m ~0.3 W l ~0.7 WMAP+SN+HST astro-ph/ Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 4

5 Candidates for Galactic Dark Matter Massive Compact Halo Objects (MACHOs) Low (sub- solar) mass stars. Standard baryonic composition. Use gravity microlensing to study. Could possibly account for 25% to 50% of Galactic Dark Matter. Neutrinos Small contribution if atmospheric neutrino results are correct, since m n < 1eV. Large scale galactic structure hard to reconcile with neutrino dominated dark matter Weakly Interacting Massive Particles ( WIMPs) Non- Standard Model particles, ie: supersymmetric neutralinos Heavy (> 10GeV) neutrinos from extended gauge theories. Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 5

6 Neutralino WIMPs Assume c present in the galactic halo c is its own antiparticle => can annihilate in galactic halo producing gamma-rays, antiprotons, positrons. Antimatter not produced in large quantities through standard processes (secondary production through p + p --> p + X) So, any extra contribution from exotic sources (c c annihilation) is an interesting signature ie: c c --> p + X Produced from (e. g.) c c --> q / g / gauge boson / Higgs boson and subsequent decay and/ or hadronisation. Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 6

7 Supersymmetry introduces free parameters: In the MSSM, with Grand Unification assumptions the masses and couplings of the SUSY particles as well as their production cross sections, are entirely described once five parameters are fixed: M 1/2 the mass parameter of supersymmetric partners of gauge fields (gauginos) the higgs mixing parameters m that appears in the neutralino and chargino mass matrices m 0, the common mass for scalar fermions at the GUT scale A, the trilinear coupling in the Higgs sector the ratio between the two vacuum expectation values of the Higgs fields defined as: tang b = v 2 / v 1 = <H 2 > / <H 1 > (3 S ) Experimental lower limit on the mass of the lightest neutralino assuming MSSM (Minimal Standard Supersymmetric Model) M c > 50 GeV ( Lep, s = 189 GeV ) hep-ph/ Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 7

8 EGRET data & Susy models A.Morselli, A.Lionetto, A.Cesarini, F.Fucito, P.Ullio, 2002 EGRET data Annihilation channel b-bbar Mc =50 GeV background model(galprop) WIMP annihilation (DarkSusy) Total Contribution ~2 degrees around the galactic center Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 8

9 Main Diagrams for Neutralino Annihilation gauge bosons Light fermion pairs suppressed due to Pauli Principle (neutralinos are Majorana particles and fermions fi Pauli Principle at zero momentum fi p wave fi µ fermion mass!) Low values of tan b (<3.8 excluded by electroweak data (g2, LEP Higgs Limit and BR(bôsg) At larger values of tan b, bbar dominant final state ( orders of magnitudes for tan b >5 ) fermions Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 9

10 Differential yield for each annihilation channel total yields yields not due to p 0 decay WIMP mass=200gev Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 10

11 Differential yield for b bar neutralino mass Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 11

12 Total photon spectrum from the galactic center from cc ann. (6 S ) Two-year scanning mode Infinite energy resolution g lines With finite energy resolution 50 GeV 300 GeV Bergstrom et al. Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 12

13 HALO SUBSTRUCTURE Milky Way A.Font and J.Navarro, astro- ph/ kpc Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 13

14 GLAST Expectation & Susy models A.Morselli, A.Lionetto, A.Cesarini, F.Fucito, P.Ullio, 2003 ~2 degrees around the galactic center, 2 years data Annihilation channel W + W - m x =80.3 GeV (Galprop) (one example from DarkSusy) Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 14

15 Positron with HEAT Positron fraction e + / ( e + + e - ) Energy(GeV) ICRC 01 p.1867 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 15

16 Positron with HEAT ICRC 01 p.1867 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 16

17 Positron Ratio Background from normal secondary production Background from normal secondary production (ApJ 493, 694, 1998) Signal from ~ 300 GeV neutralino annihilations (Phys.Rev. D59 (1999) astro-ph ) Caprice98 data from XXVI ICRC, OG , 1999 Total Caprice94 data from ApJ, 532, 653, 2000 Signal from neutralino annihilations Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 17

18 PAMELA POSITRONS expectation for 3 years of operation Secondary production Secondary production Leaky box model Secondary production Moskalenko + Strong model without reacceleration Primary production from c c annihilation (m(c) = 336 GeV) Total Primary production Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 18

19 Distortion of the secondary antiproton flux induced by a signal from a heavy Higgsino-like neutralino. Particles and photons are sensitive to different neutralinos. Gaugino-like particles are more likely to produce an observable flux of antiprotons whereas Higgsino-like annihilations are more likely to produce an observable gamma-ray signature Background from normal secondary production Signal from 964 GeV neutralino annihilations ( astro-ph ) Caprice94 data from ApJ, 487, 415, 1997 Mass91 data from XXVI ICRC, OG , 1999 AMS98 Caprice98 data from ApJ, 561, (2001), 787. astro-ph/ BESS data from Phys.Rev.Lett, 2000, 84, 1078 BESS 00 AMS data : preliminary Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 19

20 PAMELA ANTIPROTONS expectation Secondary production (upper and lower limits) Simon et al. Primary production from c c annihilation (m(c) = 964 GeV) Secondary production Primary production Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 20

21 Distortion on the secondary antiproton flux induced by an Extragalactic Antimatter component Background from normal secondary production Mass91 data from XXVI ICRC, OG , 1999 CAPRICE94 data from ApJ, 487, 415, 1997 Antiproton/proton Ratio Extragalactic Antimatter Primordial Black Hole evaporation CAPRICE98 data from ApJ Letters 534, L177, 2000 HEAT 00 data from Phys.Rev.Lett. 87 (2001) astro-ph/ BESS 00 BESS data from Phys.Rev.Lett. 88 (2002) astro-ph/ Kinetic Energy (GeV) Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 21

22 ANTIMATTER LIMITS 2003 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 22

23 MASS Matter Antimatter Space Spectrometer Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 23

24 The CAPRICE 94 flight Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 24

25 CAPRICE 94 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 25

26 Proton energy spectrum at the top of atmosphere CAPRICE98 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 26

27 The helium energy spectrum at the top of atmosphere CAPRICE98 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 27

28 SilEye on MIR Space Station wizard.roma2.infn.it Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 28

29 The NINA instrument a silicon wafer 6x6 cm 2, 380 mm thick with 16 strips, 3.6 mm wide in two orthogonal views X -Y NINA2-MITA Launch The basic silicon detector NINA 2 on MITA The complete detector Launch of NINA 1 : 10/8/1998 Launch of NINA 2 : 15/7/2000 More info: Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 29

30 PAMELA Physics Objectives AntiProton spectrum : 80 MeV GeV Positron spectrum : 50 MeV GeV Search for Antinuclei e + + e - up to 1 TeV Multi TeV electrons Solar and Trapped Cosmic Rays Solar Energetic Particles Long Term Solar Modulation Radiation Belts Transient Phenomena Bare Mass: 450 Kg Total Mass: ~750 Kg Power: 350 W GF: 21 cm 2 sr MDR: 740 GV/c RESURS-DK1 Satellite Mass: Kg Elliptical Orbit 70.4 incl Km altitude Launch: December 2003 Mission Life > 3 Yr. Launcher : Soyuz-TM Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 30

31 Pamela TOF Protons 80 MeV 700 GeV Antiprotons 80 MeV 190 GeV Electrons 50 MeV 2 TeV Positrons 50 MeV GeV Nuclei < 700 GeV/n Limits for Antinuclei ~10-8 ANTI TRD TRK Total Mass 440 Kg Power 355 W MDR 770 GV CALO ND Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 31

32 The Wizard Group O. Adriani 1, M. Ambriola 2,, G. Barbiellini 3,L.M. Barbier 4,S. Bartalucci 5, G. Bazilevskaja 6, R. Bellotti 2, D. Bergstrom 7, 5. Bertazzoni 8, V. Bidoli 9, M. Boezio 3, E. Bogomolov 10, V. Bonvicini 3, M. Boscherini 1, U. Bravar 14, F. Cafagna 2, P. Carlson 7, M. Casolino 8, M. Castellano 2, G. Castellini 15, E.R. Christian 4, F. Ciacio 2, M. Circella 2, R. D Alessandro 1, G. De Cataldo 2, C.N. De Marzo 2, M.P. De Pascale 9, N.Finetti 1, T. Francke 7, G. Furano 9, A. Gabbanini 15, A.M. Galper 11, N. Giglietto 2, M. Grandi 1, A. Grigorjeva 6, M. Hof 12, S.V. Koldashov 11, M.G. Korotkov 11, J.F. Krizmanic 4, S. Krutkov 10, B. Marangelli 2, L. Marino 5, W. Menn 12, V.V. Mikhailov 11, N. Mirizzi 2, J.W. Mitchell 4, A.A. Moiseev 11, A. Morselli 9, R. Mukhametshin 6, J.F. Ormes 4, J.V. Ozerov 11, P. Papini 1, A. Perego 1, S. Piccardi 1, P. Picozza 9, M. Ricci 5, A. Salsano 8, P. Schiavon 3, M. Simon 12, R. Sparvoli 9, B. Spataro 5, P. Spillantini 1, P. Spinelli 2, S.A. Stephens 13, S.J. Stochaj 14, Y. Stozhkov 6, R.E. Streitmatter 4, F. Taccetti 15, M. Tesi 15, A. Vacchi 3, E. Vannuccini 1, G. Vasiljev 10, V. Vignoli 15, S.A. Voronov 11, N. Weber 7, Y. Yurkin 11, N. Zampa 3 1 University and INFN, Firenze (Italy) 9 University of Roma Tor Vergata and INFN Roma2, Roma, (ltaly) 2 University and INFN, Bari (Italy) 10 Ioffe Physical Technical Institute (Russia) 3 University and INFN, Trieste (Italy) 11 Moscow Engineering and Physics Institute, Moscow (Russia) 4 NASA Goddard Space Flight Center Greenbelt (USA) 12 Siegen University, Physics Department, Siegen (Germany) 5 Laboratori Nazionali INFN, Frascati (Italy) 13 Tata Institute of Fundamental Research, Bombay (India) 6 Lebedev Physical Institute (Russia) 14 Particle Astrophysics Laboratory, NMSU, Las Cruces (USA) 7 Royal Institute of Technology, Stockholm (Sweden) 15 Istituto di Ricerca Onde Elettromagnetiche CNR, Firenze (Italy) 8 Electronic Engineering Department, II University, Roma-Tor Vergata (Italy) Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 32

33 Past, Present and Future Projects MASS-89, 91, TS-93, CAPRICE PAMELA GLAST WiZard Program NINA-2 NINA-1 M 89 M 91 TS 93 C 94 C 97 C 98 AGILE PAMELA GLAST SILEYE-1 NINA-1 NINA-2 SILEYE-3 SILEYE-2 SILEYE-4 SILEYE-2 ALTEINO: SILEYE-3 SILEYE-1 ALTEA: SILEYE-4 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 33

34 field of view PAMELA Launch Presurized container with PAMELA in operating position Expected Date of launch : end of 2003 PAMELA in launching position The Resurs-DK1 satellite Carrier rocket: SOYUZ Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 34

35 More information on PAMELA : please visit us: Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 35

36 AMS Lancio: Durata: 3 anni Protoni fino ad alcuni TeV Antiprotoni fino a 200 GeV Elettroni fino al TeV Positroni fino a 200 GeV Nuclei fino ad alcuni TeV AntiNuclei fino al TeV g fino a 100 GeV Isotopi leggeri fino a 20 GeV Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 36

37 AMS Altezza: Km Inclinazione 51.7 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 37

38 AGILE Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 38

39 Super Agile Mask AGILE Super Agile Silicon plane AntiCoincidence Photomultipliers Top: 0.5cm plastic scintillator Lateral: 12 panels 0.6 cm Tracker, 14 X/Y planes W 0.07 X0 X/Y plane, 121 mm pitch distance between planes 1.6cm Calorimeter 1.5 X0 CsI Calorimeter 1.4*2*40 cm 3 bars Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 39

40 More information on AGILE : please visit us: Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 40

41 GLAST Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 41

42 Silicon Tracker tower 18 planes of X Y silicon detectors + converters Gamma-Ray Large Area Space Telescope 12 trays with 2.5% R.L. of Pb, 4 trays with 25%, 2 trays without converters Tracker 1.68 m 84 cm Grid DAQ Electronics DAQ Electronics ACD Anticoincidence Shield Calorimeter Thermal Blanket ( 8.5 Rad.Length) Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 42

43 GLAST Instrument Description lgeneral Characteristics: imaging, wide fieldof-view, pair-conversion telescope, backed by EM calorimetry using modern HEP technology: *energy range: *energy Geminga resolution: 10% *effective area: *field-of-view: EGRET GLAST simulation 10 MeV to 300 GeV Geminga > 8,000 cm 2 (above 1 GeV) ~2p sr IC 443 *point source sensitivity: Crab 2 x 10-9 ph cm -2 s -1 (@ 100 MeV) Crab ph cm -2 s -1 ( > 1 GeV) *source location determination: 30 arcsec - 5 arcmin *cosmic ray/g rejection > 10 5 to 1 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 43

44 GLAST Performance Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 44

45 GLAST LAT Strength - New EGRET Catalog Every 2 days - All 3EG sources + ~ 80 new in 2 days fi periodicity searches (pulsars, X-ray binaries) In scanning mode, the LAT will achieve after one day sensitivity sufficient to detect (5s) the weakest EGRET sources fi pulsar beam, emission vs. luminosity, age, B Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 45

46 One year All-Sky Survey Simulation, Eg > 100 MeV All-sky intensity map based on five years EGRET data. EGRET GLAST Integral Flux (E>100 MeV) cm -2 s -1 All-sky intensity map from a GLAST one year survey, based on the extrapolation of the number of sources versus sensitivity of EGRET Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 46

47 GRB studies with GLAST EGRET observed delayed GeV emission from the GRB of February 17, 1994, including a 20 GeV photon that arrived 80 minutes after the burst began. GLAST will make the definitive measurements of the high-energy behaviour of GRBs and GRB afterglows. Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 47

48 GRB studies with GLAST (2) Study of the initial impulsive phase: Dt< 1 ms Expected detection rate (above 50 MeV): yr -1 Broad band spectral information: ~ 200 kev - 30 GeV Rapid (few seconds) communication of GRB quicklook results Single g angular resolution ~10 arcmin at high energies for good source localization. Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 48

49 Gamma Gamma -ray ray missions deadtime Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 49

50 Test of Quantum Gravity (1 q ) Candidate effect: E=photon energy c 2 P 2 = E 2 ( 1+ f(e/e QG )) E QG =effective quantum gravity energy scale Deformed dispersion relation with function f model dependent function of E/E QG if E<< E QG series expansion is applicable c 2 P 2 = E 2 ( 1+ a(e/e QG )+ O(E/E QG ) 2 ) v = de/dp ~ c ( 1+ a(e/e QG )) vacuum as quantum-gravitational medium which respond differently to the propagation of particle of different energies. (analogous to propagation through an electromagnetic plasma) Medium fluctuation at a scale of the order of L p ~10-33 cm Dt = ~ a E/E QG D/c Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 50

51 Test of Quantum Gravity (2) Dt = ~ a E/E QG D/c E 1 E 1 E 2 E 2 t=t i E1 Dt i =0 Dt f =0 t=t f E1 E 2 E 2 D ~ cm E QG ~10 19 GeV c~ cm Dt(ms) ~ 60 DE(GeV) even at pulsars distance: D ~ cm Dt(ms) ~ 100 E QG ~10 14 GeV Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 51

52 another quantum gravity test Flux absorption due to the interaction with the infrared and microwave background g ray source if the center of mass energy is: Microwave and infrared background g E=w 1 e + Earth photons interactions produce electron positron pairs g J E=w 2 e - Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 52

53 Flux absorption due to the interaction with the infrared and microwave background (2) The cross section of the process gg -> e + e - is: where r e is the classical radius of the electron and: w 1 and w 1 are respectively the energies of the low and the high energies gamma ray and J is their angle of incidence. g g E=w 1 J e + e - E=w 2 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 53

54 Flux absorption due to the interaction with the infrared and microwave background (3) the ratio between the flux I(L) at a distance L from the source and the initial flux I can be written as: where k g is the absorption coefficient: I(L)/I o =exp(-k g L) that contains the cross section and the low energy photon distribution. For the microwave spectrum: g g J E=w 1 E=w 2 e + e - Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 54

55 Transparency of the Universe Super Cluster Virgo Cluster 60mly, 18mpc Andromeda (700 kpc, 2.9Mly) LMC (50 kpc, 179kly) Our galaxy Distance (mpc) IR 2.7 k p g e + e - p g p + p - Z~1 ~ cm Z~0.53, 2C279 radio g g e + e - Z~0.03 ~ cm (Mrk521) Z~10-6 cm GeV 10 TeV E(eV) Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 55

56 another quantum gravity test: the higher threshold condition introduced by quantum-gravity can be of the for From the only hypothesis that we have seen some level of absorption G. Amelino-Camelia, gr-qc/ Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 56

57 Flux absorption due to the interaction with the infrared background in H HEGRA Coll. astro/ph Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 57

58 Acceleration of Cosmic Rays If cosmic rays are accelerated in supernova remnants, then the high-energy gamma-ray spectral index in supernova remnants will be equal to the cosmic-ray spectral index at the source. GLAST will have enough angular resolution to resolve the remnant IC443 and enough sensitivity to measure its spectral index. Galactic anticenter at Eg > 100 MeV. EGRET data and GLAST one-year all-sky survey EGRET GLAST simulation Geminga Geminga IC 443 Crab Crab Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 58

59 Expected number of isotropic extragalactic photons detected by LAT after 5 years. Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 59

60 Summary of AGILE and GLAST physic items Cosmic Diffuse Background Origin is still a mystery for gamma rays Is there a truly diffuse cosmological component? Supermassive BHs and AGN Remarkable objects that shine most brightly in gamma rays Gamma rays probe central engine Gamma rays probe jets GRBs High-energy prompt and delayed emission not understood EGRET provided only a glimpse Quantum gravity effects possible Unidentified Sources Mystery has been with us for > 20 years Third EGRET Catalog includes 170 unidentified sources A new class of Galactic sources? SNRs Site of CR acceleration E < ev (still unproven for nuclei!) Should see extended sources in gammas (from p o decay) to answer the question definitively Pulsars Gemingas only shine in gamma regime Uncover acceleration mechanisms Understand beaming Cosmology - AGNs Spectral roll-offs due to EBL are in GLAST range GLAST can see to z > 4 Cosmology - Dark Matter PBHs, cosmic strings, WIMP annihilation all predicted to shine in gamma rays From here GLAST Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 60

61 The GLAST Participating Institutions Italian Team Institutions INFN - Instituto Nazionale di Fisica Nucleare: Units of Bari, Perugia, Pisa, Padova, Rome 2, Trieste Universities of Bari, Perugia, Padova, Pisa, Rome 2, Trieste, Udine ASI - Italian Space Agency IFC/CNR- Istituto di Fisica, Cosmica, CNR American Team Institutions SU - Stanford University, Physics Department and EGRET group, Hanson Experimental Physics Laboratory SU-SLACStanford Linear Accelerator Center, SLAC, Particle Astrophysics group GSFC-NASA Goddard Space Flight Center, Laboratory for High Energy Astrophysics NRL - U. S. Naval Research Laboratory, E. O. Hulburt Center for Space Research, X-ray and gamma-ray branches UCSC- University of California at Santa Cruz, Physics Department SSU- Sonoma State University, Department of Physics & Astronomy UW- University of Washington, TAMUK- Texas A&M University-Kingsville Japanese Team Institutions University of Tokyo ICRR - Institute for Cosmic-Ray Research ISAS- Institute for Space and Astronautical Science Hiroshima University French Team Institutions CEA/DAPNIA Commissariat à l'energie Atomique, Département d'astrophysique, de physique des Particules, de physique Nucliaire et de l'instrumentation Associée, CEA, Saclay IN2P3 Institut National de Physique Nucléaire et de Physique des Particules, IN2P3 IN2P3/LPNHE-X Laboratoire de Physique Nucléaire des Hautes Energies de l'école Polytechnique IN2P3/PCC Laboratoire de Physique Corpusculaire et Cosmologie, Collège de France IN2P3/CENBG Centre d'études nucléaires de Bordeaux Gradignan Swedish Team Institutions KTHRoyal Institute of Technology Stockholms Universitet Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 61

62 Sensitivity of g-ray detectors All sensitivities are at 5s. Cerenkov telescopes sensitivities (Veritas, MAGIC, Whipple, Hess, Celeste, Stacee, Hegra) are for 50 hours of observations. Large field of view detectors sensitivities (AGILE, GLAST, Milagro, ARGO, AMS) are for 1 year of observation. Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 62

63 Energy versus time for X and Gamma ray detectors AMS GLAST AGILE MEGA SuperAGILE Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 63

64 Conclusion: AGILE will provide transient quicklook alert for all the Cerenkov telescope that will operate from 2002: MAGIC, Whipple, Hess, Celeste, Stacee, Hegra... AGILE will make simultaneous observations together with the ground all-sky monitors like MILAGRO and ARGO. for the first time there will be the possibility to fill the gap between space and ground! Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 64

65 2 nd Conclusions Neutralinos are a promising candidate for WIMP dark matter Neutralinos can annihilate in the galactic halo... this could give rise to high energy (> 10GeV) antiproton signature and/or gamma-ray signature. Pamela experiment is designed to measure antiproton spectrum from 80MeV to 190GeV. >3 year mission large event samples Combination of TRD + Si tracker + imaging Si- W calo + TOF (trigger) and anticoincidence can isolate a pure sample of antiprotons. Engineering model currently under construction. Flight model due ~ June Launch: end From March 2006 GLAST will search for gamma-ray signature Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 65

66 3 rd Conclusions GLAST will explore a good portion of the supersymmetric parameter space GLAST will explore the Cold and Hot Dark Matter contribution through the IR absorption of g-ray from extragalactic sources and these are only additional items for GLAST! Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 66

67 4 th Conclusions Í GLAST will be an important step in gamma ray astronomy ( ~ sources compared to ~ 200 of EGRET) Í A partnership between High Energy Physics and g Astrophysics Í Beam test and software development well on the way Í Wide range of possible answers/discoveries Í Gold era for multiwavelenght studies Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 67

68 Gamma-Ray Astronomy Long Term Plan Ultimate Objective: To image the particle accelerator near the event cm -2 s -1 Sensitivity cm -2 s arc sec Angular resolution cm -2 s -1 GLAST 10 arc sec 1%? Energy resolution 5 arc min 5 % Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 68

69 Source creation acceleration injection Cosmic rays: about 10 Myears in the Galaxy (6-7 g/cm2) g n further acceleration? Cosmic Rays Propagation Modulation Atmosphere 40 km 23 Xo High Montain Detectors Cherencov Detectors Space experiments ~ 400 km Direct detection Balloons ~ 40 km ~3 g/cm 2 residual atmosphere Extensive Air Shower Detectors Particle Astrophysics Experiments Underground, Under-ice, Underwater Particle Aldo Accelerators Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 69