Astroparticle Physics with gamma-rays and cosmic rays experiments in space

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1 Astroparticle Physics with gamma-rays and cosmic rays experiments in space Sixth Meeting on New Worlds in Astroparticle Physics, University of the Algarve, Faro, Portugal, 6-8 September 2007 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 1

2 ( Aldo Morselli, INFN & Università di Roma Tor Vergata, 2

3 Aldo Morselli, INFN & Università di Roma Tor Vergata, 3

4 23 April 12 Aldo o clock Morselli, INFN Roma & Università time di Roma : Tor Launch Vergata, aldo.morselli@roma2.infn.it 4

5 17 April 2007 closing the payload AGILE mounted on the PSLV rocket, inside the Vehicle Assembly Building of Sriharikota Aldo Morselli, INFN & Università di Roma Tor Vergata, 5

6 22 April The rocket PSLV ready for the launch Aldo Morselli, INFN & Università di Roma Tor Vergata, 6

7 23 April 12 o clock Roma time : Launch Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 7

8 Aldo Morselli, INFN & Università di Roma Tor Vergata, 8

9 8 May 2007 first photon received from AGILE in orbit X Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 9 Y

AGILE first news from the sky www.roma2.infn.

10 AGILE first news from the sky Aldo Morselli, INFN & Università di Roma Tor Vergata, 10

11 AGILE first detection of a cosmic June 1, 2007 source: the Vela Pulsar Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 11

July 26, 2007: First Gamma-Ray Burst detected by SuperAGILE On July 24 approximately at 23:25:09 UT SuperAGILE detected and imaged GRB 070724b.

12 July 26, 2007: First Gamma-Ray Burst detected by SuperAGILE On July 24 approximately at 23:25:09 UT SuperAGILE detected and imaged GRB b. The experiment is not yet in its optimal configuration and in particular, the onboard triggering and imaging is not active yet and the absolute position reconstruction is being calibrated by using celestial X-ray sources. Ground analysis results showed that the event was observed at 21 degrees off-axis and the observed duration in the kev energy range is about 55 seconds, with a multi-peak time structure (see figures). The burst position was reconstructed as (RA, Dec) ( deg, deg), which is: RA(J2000) = 01h 10m 31.0s Dec(J2000) = +57d 40' 23" Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 12

13 Aldo Morselli, INFN & Università di Roma Tor Vergata, 13

14 Aldo Morselli, INFN & Università di Roma Tor Vergata, 14

15 ) Aldo Morselli, INFN & Università di Roma Tor Vergata, 15

16 Dark Matter really exist? Concordance model Ω = Ω M + Ω Λ = 1.02±0.02 Ω Λ ~ 0.73 Ω M ~ 0.27 { ΩHDM,ν Ω CDM ~ 0.23 Ω b ~ 0.04 < 0.01 Ω CDM ~ 6 Ω b Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 16

17 Aldo Morselli, INFN & Università di Roma Tor Vergata, 17

18 Particle Physics after Big Bang Aldo Morselli, INFN & Università di Roma Tor Vergata, 18

19 Supersymmetry Particle Sparticle For unbroken supersymmetry they shoul be degenerate in mass Sparticle have not be found at accelerators so far Supersymmetry is broken Supersymmetry breaking schemes: 1) gravity-mediated scenarios 2) Gauge mediated scenarios 3) Anomaly mediated scenarios Aldo Morselli, INFN & Università di Roma Tor Vergata, 19

20 Andamento delle Costanti di Accoppiamento Andamento delle costanti di accoppiamento in funzione dell'energia per il modello Standard delle particelle elementari e per il Minimo Modello Supersimmetrico Minimale Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 20

Neutralino WIMPs Assume χ present in the galactic halo χ is its own antiparticle => can annihilate in galactic halo producing gamma-rays, antiprotons, positrons.

21 Neutralino WIMPs Assume χ present in the galactic halo χ 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 (χ χ annihilation) is an interesting signature ie: χ χ --> p + X Produced from (e. g.) χ χ --> q / g / gauge boson / Higgs boson and subsequent decay and/ or hadronisation. Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 21

22 Propagation Equation for Cosmic Rays in the Milky Way convection velocity field that corresponds to galactic wind and it has a cylindrical symmetry, as the geometry of the galaxy. It s z-component is the only one different from zero and increases linearly with the distance from the galactic plane loss term: fragmentation diffusion coefficient in the impulse space, quasi-linear MHD: diffusion coefficient is function of rigidity loss term: radioactive decay primary spectra injection index semi-analitical solution: Maurin et al, astro-ph/ implemented in Galprop ( Strong & Moskalenko, available on the Web) Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 22

23 B/C ratio Enveloping curves of all the good fits of the experimental B/C data Dashed line: Best fit DR: diffusion+ reacceleration DC: diffusion+convection In DC model problem with the ACE data at low energy A.Lionetto, A.Morselli, V.Zdravkovic Aldo Morselli, INFN & Università di Roma Tor Vergata, JCAP09(2005)010 astro-ph/

propagation parameters for DC propagation halo size diff constant diff index V c gradient

24 Allowed values for the propagation parameters for DR propagation prim spec halo size diffusion constant diff index injection index Alfven velocity Allowed values for the propagation parameters for DC propagation halo size diff constant diff index V c gradient injection indexes Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 24

25 Proton spectra: Upper and lower bounds of due to the uncertainties of propagation parameters Aldo Morselli, INFN & Università di Roma Tor Vergata, 25

26 Helium spectra: Upper and lower bounds of due to the uncertainties of propagation parameters Aldo Morselli, INFN & Università di Roma Tor Vergata, 26

27 Prim/Sec consistency check DR uncertanty band DC uncertanty band (Sc+Ti+V)/Fe Ratio that corresponds to the best fit of B/C; Aldo Morselli, INFN & Università di Roma Tor Vergata, 27

28 CAPRICE98 Galprop 4.1 Aldo Morselli, INFN & Università di Roma Tor Vergata, 28

29 Electron spectra DR DRB Local interstellar spectra DC DRB A.Lionetto, A.Morselli, V.Zdravkovic JCAP09(2005)010 [astro-ph/ ] DR DC Top of the atmosphere spectra Aldo Morselli, INFN & Università di Roma Tor Vergata, 29

30 Positron spectra A.Lionetto, A.Morselli, V.Zdravkovic JCAP09(2005)010 [astro-ph/ ] Aldo Morselli, INFN & Università di Roma Tor Vergata, 30

31 Antiproton spectra: Upper and lower bounds of due to the uncertainties of propagation parameters Aldo Morselli, INFN & Università di Roma Tor Vergata, 31

32 MASS Matter Antimatter Space Spectrometer ( 89&91 ) Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 32

33 Aldo Morselli, INFN & Università di Roma Tor Vergata, 33

34 MASS 89 flight Aldo Morselli, INFN & Università di Roma Tor Vergata, 34

35 MASS 89 flight Aldo Morselli, INFN & Università di Roma Tor Vergata, 35

36 MASS 89 Aldo Morselli, INFN & Università di Roma Tor Vergata, 36

37 PAMELA Payload for Antimatter Matter Exploration and Light Nuclei Astrophysics In orbit on June 15, 2006, on board of the DK1 satellite by a Soyuz rocket from the Bajkonour launch site. First switch-on on June From July 11 Pamela is in continuous data taking mode Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 37

38 PAMELA Aldo Morselli, INFN & Università di Roma Tor Vergata, 38

39 Flight data: GV positron Flight data: GV electron Aldo Morselli, INFN & Università di Roma Tor Vergata, 39

40 PAMELA scientific program PAMELA is a magnetic spectrometer which will fly on a Russian satellite by Fall Its scientific scope is the measurement of the antiproton and positron spectra up to few hundred GeV, of the proton and electron spectra up to 700 GeV and that of light nuclei. energy range particles/3 years Antiproton flux 80 MeV GeV > Positron flux 50 MeV 270 GeV > Electron flux up to 400 GeV Proton flux up to 700 GeV Electron/positron flux up to 2 TeV Light Nuclei (up to Z=6) up to 200 GeV/n He/Be/C: /4/5 AntiNuclei search (sensitivity of in He/He) Unprecedented Statistics and new Energy Range in Cosmic Rays Actual limits: antip&positrons 40 GeV Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 40

41 Pamela in Samara, Russia 4/09/05 Aldo Morselli, INFN & Università di Roma Tor Vergata, 41

Transport from Progress building to Launch Pad 13-6-2006 Aldo

42 Transport from Progress building to Launch Pad Aldo Morselli, INFN & Università di Roma Tor Vergata, 42

PAMELA @ Baikonur 14/06/06 Aldo Morselli, INFN &

43 Baikonur 14/06/06 Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 43

44 PAMELA Launch 15/06/06 Aldo Morselli, INFN & Università di Roma Tor Vergata, 44

45 PAMELA Launch 15/06/06 Aldo Morselli, INFN & Università di Roma Tor Vergata, 45

46 Flight data: 18 GV antiproton Aldo Morselli, INFN & Università di Roma Tor Vergata, 46

47 Flight data: 2.8 GV electron Aldo Morselli, INFN & Università di Roma Tor Vergata, 47

48 Flight data: ~500 GV electron? Aldo Morselli, INFN & Università di Roma Tor Vergata, 48

49 PAMELA event Flight data: 36 GV interacting proton Aldo Morselli, INFN & Università di Roma Tor Vergata, 49

50 Flight data: calorimeter self-trigger (m.p. proton) Aldo Morselli, INFN & Università di Roma Tor Vergata, 50

51 Aldo Morselli, INFN & Università di Roma Tor Vergata, 51

52 Galactic H and He spectra Flight Data Preliminary Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 52

53 Flight Data Preliminary Aldo Morselli, INFN & Università di Roma Tor Vergata, 53

54 PAMELA April 2007 We have collected data for about 20 million seconds in full PAMELA configuration corresponding to ~220 days of continuous data taking. a first milestone: SIX MONTHS OF DATA The amount of data collected is ~4TB, corresponding to more than 480 milion events. more news on PAMELA: Mark Pearce talk this afternoon Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 54

55 Positron spectra: PAMELA expectation for DC model DRB DC A.Lionetto, A.Morselli, V.Zdravkovic JCAP09(2005)010 [astro-ph/ ] Aldo Morselli, INFN & Università di Roma Tor Vergata, 55

56 HEAT Data and positron excess astro-ph/ Aldo Morselli, INFN & Università di Roma Tor Vergata, 56

57 CAPRICE 98 CAPRICE 94 Measurements of Cosmic-Ray Electrons and Positrons by the WiZard/CAPRICE Collaboration M.Boezio et al. [CAPRICE98 Collaboration] Advances in Space Research 27: (4) XXVI International Cosmic Ray Conference, OG , Salt Lake City, 1999 Aldo Morselli, INFN & Università di Roma Tor Vergata, 57

58 Aldo Morselli, INFN & Università di Roma Tor Vergata, 58

59 Aldo Morselli, INFN & Università di Roma Tor Vergata, 59

60 The cosmic ray electron and positron spectra measured at 1 AU during solar minimum activity M.Boezio et al. [ Caprice94 Coll ] The Astrophysical Journal, 532, 653, 2000 Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 60

61 AMS01 brems. events AMS 01 PhysLett B [astro-ph/ ] Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 61

62 Positron ratio: Experimental situation and PAMELA expectation for DC model Moskalenko IV, Strong AW. Astrophys. J. 493:694 (1998) DC HEAT e, HEAT pbar comb. AMS01 brems events AMS01 single tracks DC model A.Lionetto, A.Morselli, V.Zdravkovic JCAP09 (2005) 010 [astro-ph/ ] Aldo Morselli, INFN & Università di Roma Tor Vergata, 62

63 Positron ratio: Experimental situation and PAMELA expectation for DC model Moskalenko IV, Strong AW. Astrophys. J. 493:694 (1998) model with reacceleration model with no reacceleration DC HEAT e, HEAT pbar comb. AMS01 brems events AMS01 single tracks DC model A.Lionetto, A.Morselli, V.Zdravkovic JCAP09 (2005) 010 [astro-ph/ ] Aldo Morselli, INFN & Università di Roma Tor Vergata, 63

64 Positron ratio: Experimental situation and PAMELA expectation for DC model Moskalenko IV, Strong AW. Astrophys. J. 493:694 (1998) model with reacceleration model with no reacceleration and with Protheroe electron spectrum model with no reacceleration nucleon spectrum model DC HEAT e, HEAT pbar comb. AMS01 brems events AMS01 single tracks DC model A.Lionetto, A.Morselli, V.Zdravkovic JCAP09 (2005) 010 [astro-ph/ ] Aldo Morselli, INFN & Università di Roma Tor Vergata, 64

65 Positron ratio: Experimental situation and PAMELA expectation for DC model Moskalenko IV, Strong AW. Astrophys. J. 493:694 (1998) DC model with reacceleration model with no reacceleration and with Protheroe electron spectrum model with no reacceleration flat injection spectrum model Neutralino annihilation pulsar HEAT e, HEAT pbar comb. AMS01 brems events AMS01 single tracks DC model A.Lionetto, A.Morselli, V.Zdravkovic JCAP09 (2005) 010 [astro-ph/ ] Moskalenko IV, Strong Ptuskin, astro/ph Aldo Morselli, INFN & Università di Roma Tor Vergata, 65

66 Antiproton spectra: PAMELA expectation for DC model Antiproton spectra: Pamela expectation for Diffuse and Convection model in 3 yr A.Lionetto, A.Morselli, V.Zdravkovic, JCAP09(2005)010 Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 66

67 PAMELA: Cosmic-Ray Antiparticle Measurements: Antiprotons an example in msugra fd: Clumpiness factors needed to disentangle a neutralino induced component in the antiproton flux f = the dark matter fraction concentrated in clumps d = the overdensity due to a clump with respect to the local halo density A.Lionetto, A.Morselli, V.Zdravkovic JCAP09(2005)010 [astro-ph/ ] Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 67

68 PAMELA: Cosmic-Ray Antiparticle Measurements: Antiprotons MSSM fd: Clumpiness factors needed to disentangle a neutralino induced component in the antiproton flux total background χ contribution A.Lionetto, A.Morselli, V.Zdravkovic JCAP09(2005)010 [astro-ph/ ] Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 68

69 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 5 parameters are fixed: M 1/2 the common mass of supersymmetric partners of gauge fields (gauginos) m 0 µ A the common mass for scalar fermions at the GUT scale the higgs mixing parameters that appears in the neutralino and chargino mass matrices is the proportionality factor between the supersymmetry breaking trilinear couplings and theyukawa couplings tang β = v 2 / v 1 = <H 2 > / <H 1 > the ratio between the two vacuum expectation values of the Higgs fields Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 69

70 msugra Signal Signal and Background are separated? YES tg(β)=55, sign(µ)=+1 Background NO Signal Background Aldo Morselli, INFN & Università di Roma Tor Vergata, 70

71 msugra Signal and Background are separated? tg(β)=55, sign(µ)=+1 Signal Background Signal YES YES YES YES YES YES NO NO NO NO NO NO NO NO NO NO NO NO NO YES YES YES YES YES NO YES YES YES Background Aldo Morselli, INFN & Università di Roma Tor Vergata, 71

72 msugra Signal and Background are separated? tg(β)=55, sign(µ)=+1 Signal Background Signal YES YES YES YES YES YES NO NO NO NO NO NO NO NO NO NO NO NO NO YES YES YES YES YES NO YES YES YES Background Aldo Morselli, INFN & Università di Roma Tor Vergata, 72

73 msugra PAMELA WIMP Detection Sensitivity Aldo Morselli, INFN & Università di Roma Tor Vergata, 73

74 Antiproton spectra: PAMELA expectation for DC model Antiproton spectra: Pamela expectation for Diffuse and Convection model in 3 yr A.Lionetto, A.Morselli, V.Zdravkovic, JCAP09(2005)010 Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 74

75 msugra PAMELA WIMP Detection Sensitivity Aldo Morselli, INFN & Università di Roma Tor Vergata, 75

76 msugra Sensitivity plot for 5 years observation of msugra for GLAST for tg(b)=55 and for other experiments. GLAST 3σ sensitivity is shown at the blue line and below for truncated NFW halo profile accelerator 100 fb -1 from H.Baer et al., hep-ph/ GLAST, PAMELA, LHC, LC Sensitivities to Dark Matter Search LCC4 PAMELA Limits boost factor 10 LC500 LHC limits 100 fb -1 LC1000 limits GLAST limits Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 76

77 msugra PAMELA WIMP Detection Sensitivity larger values of tg(b) gives larger signals both in antiprotons and gammas Aldo Morselli, INFN & Università di Roma Tor Vergata, 77

78 msugra Sensitivity plot for 5 years observation of msugra for GLAST for tg(b)=55 and for other experiments. GLAST 3σ sensitivity is shown at the blue line and below for truncated NFW halo profile accelerator 100 fb -1 from H.Baer et al., hep-ph/ GLAST, PAMELA, LHC, LC Sensitivities to Dark Matter Search LCC4 PAMELA Limits boost factor 10 LC500 LHC limits 100 fb -1 LC1000 limits GLAST limits Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 78

79 GLAST Aldo Morselli, INFN & Università di Roma Tor Vergata, 79

80 GLAST During Integration Both the LAT and GBM are now integrated to the Spacecraft at General Dynamics in Phoenix, Arizona. the LAT and the NaI GBM modules mounted onto the spacecraft. Aldo Morselli, INFN & Università di Roma Tor Vergata, 80

81 LAT MC Derived Performance Aldo Morselli, INFN & Università di Roma Tor Vergata, 81

82 Where should we look for WIMPs with GLAST? Galactic center Galactic satellites Galactic halo Extra-galactic Aldo Morselli, INFN & Università di Roma Tor Vergata, 82

83 This talk See E.Nuss talk Aldo Morselli, INFN & Università di Roma Tor Vergata, 83

EGRET data & Susy models Annihilation channel W + W - Mχ =80.3 GeV EGRET data N b =1.82 10 21 N χ =8.

84 EGRET data & Susy models Annihilation channel W + W - Mχ =80.3 GeV EGRET data N b = N χ = Typical Nχ values: NFW: Nχ = 10 4 Moore: Nχ = Isotermal: Nχ = background model(galprop) WIMP annihilation (DarkSusy) Total Contribution ~2 degrees around the galactic center A.Morselli, A. Lionetto, A. Cesarini, F. Fucito, P. Ullio, astro-ph/ Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 84

85 GLAST Expectation & Susy models ~2 degrees around the galactic center, 2 years data Annihilation channel W + W - Mχ =80 GeV N b = N χ = Typical Nχ values: NFW: Nχ = 10 4 Moore: Nχ = Isotermal: Nχ = (Galprop) (one example from DarkSusy) astro-ph/ A.Cesarini, F.Fucito, A.Lionetto, Aldo A.Morselli, INFN P.Ullio, & Università Astroparticle di Roma Physics, Tor Vergata, 21, , aldo.morselli@roma2.infn.it June 2004 [astro-ph/ ] 85

86 msugra Sensitivity plot for 5 years observation of msugra for GLAST for tg(b)=55 and for other experiments. GLAST 3σ sensitivity is shown at the blue line and below for truncated NFW halo profile accelerator 100 fb -1 from H.Baer et al., hep-ph/ GLAST, PAMELA, LHC, LC Sensitivities to Dark Matter Search LCC4 PAMELA Limits boost factor 10 LC500 LHC limits 100 fb -1 LC1000 limits GLAST limits Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 86

msugra LHC limits tg(β)=10, sign(µ)=+1 LC1000 limits WMAP 3 3 σ allowed region GLAST limits LC500 m h0 < 114.

87 msugra LHC limits tg(β)=10, sign(µ)=+1 LC1000 limits WMAP 3 3 σ allowed region GLAST limits LC500 m h0 < GeV no electroweak symmetry breaking Sensitivity plot for observation of msugra for a number of accelerator experiments and GLAST for tg(β)=10. GLAST 3σ sensitivity is shown at the blue line and below a for truncated Navarro Frank and White (NFW) halo profile Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 87

88 msugra Sensitivity plot for GLAST for a truncated NFW halo profile 5 years of data tg(β)=60, sign(µ)=+1 Sensitivity plot for observation of msugra for GLAST for tg(β)=60. GLAST 3σ sensitivity is shown at the blue line and below for truncated NFW halo profile WMAP 3 3 σ allowed region GLAST 3 σ limits no electroweak symmetry breaking Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 88

89 Model independent results for the GC Assume a truncated NFW profile Assume a dominant annihilationchannel (good assumption except for τ + τ - ) Differential yield for each annihilation channel WIMP mass=200gev figure from: A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, Astroparticle Physics, 21, , Aldo Morselli, June 2004 INFN [astro-ph/ ] & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 89

90 SUSY Model independent results for the GC Max background Min background, 3 σ Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 90

91 EGRET, GLAST, HESS it might still be that a DM component could be singled out, e.g. the EGRET source (?): a DM source can fit the EGRET data; GLAST would detect its spectral and angular signatures and identify without ambiguity such DM source! Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 91

92 Model independent results for the GC Excluded by HESS and MAGIC Max background Min background 3 σ Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 92

2008 Kennedy Space Flight Center LAUNCH June 2008 Science operation begins!

93 August 2004 Assembling of first tower completed GLAST Master Schedule Middle of October 2005 Completion of the LAT Environmental testing February 2006 Delivery to NRL 5 Feb Kennedy Space Flight Center LAUNCH June 2008 Science operation begins! more info : Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 93

94 Conclusion from 15 June 2006 PAMELA is in the sky! Will give strong constraints on propagation parameters. Discovery Potential for Supersymmetry End 2007 : GLAST will be launched from Kennedy Space Flight Center Complementary Discovery Potential for Supersymmetry Both searches complementary to LHC and Direct Search Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 94

95 the end Aldo Morselli, INFN & Università di Roma Tor Vergata, 95

96 Model independent results for the GC Aldo Morselli, INFN & Università di Roma Tor Vergata, 96

The GLAST Participating Institutions American Institutions SU-HEPL Stanford University, Hanson Experimental Physics Laboratory,, SU-SLAC Stanford Linear Accelerator Center, Particle Astrophysics

Hulburt Center for Space Research, X-ray and gamma-ray branches UCSC- SCIPP University of California at Santa Cruz, Santa Cruz Institute of Particle Physics SSU- California State University at

Louis UW- University of Washington, TAMUK- Texas A&M University-Kingsville, Italian Institutions Ohio State University INFN - Istituto Nazionale di Fisica Nucleare and Univ.

for Cosmic-Ray Research ISAS- Institute for Space and Astronautical Science Hiroshima University CEA/DAPNIA Commissariat à l'energie Atomique, Département d'astrophysique, de physique des Particules,

97 The GLAST Participating Institutions American Institutions SU-HEPL Stanford University, Hanson Experimental Physics Laboratory,, SU-SLAC Stanford Linear Accelerator Center, Particle Astrophysics group GSFC-NASA-LHEA 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- SCIPP University of California at Santa Cruz, Santa Cruz Institute of Particle Physics SSU- California State University at Sonoma, Department of Physics & Astronomy, WUStL-Washington University, St. Louis UW- University of Washington, TAMUK- Texas A&M University-Kingsville, Italian Institutions Ohio State University INFN - Istituto Nazionale di Fisica Nucleare and Univ. of Bari, Padova, Perugia, Pisa, Roma2, Trieste, Udine ASI - Italian Space Agency IASF- Milano, Roma Japanese Institutions French Institutions Swedish Institutions University of Tokyo ICRR - Institute for Cosmic-Ray Research ISAS- Institute for Space and Astronautical Science Hiroshima University 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 KTHRoyal Institute of Technology Stockholms Universitet Collaboration members: ~225 Members: 77 Affiliated Sci. ~80 Postdocs: 23 Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it Graduate Students 32 97

98 Dark Matter really exist? color image from the Magellan images of the merging cluster 1E astro:ph/ Chandra image of the cluster 200 kpc weak lensing reconstruction Due to the collision of two clusters, the dissipationless stellar component and the fluid-likex-ray emitting plasma are spatially segregated Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 98

99 Antiproton spectra Torsten Bringmann, Pierre Salati, astro/ph Boost factor Aldo Morselli, INFN & Università di Roma Tor Vergata, 99

100 Secondaries / primaries i.e. Boron/ Carbon to constrain propagation parameters D. Maurin, F. Donato R. Taillet and P.Salati ApJ, 555, 585, 2001 [astro-ph/ ] F. Donato et.al, ApJ, 563, 172, 2001 [astro-ph/ ] B/C Ratio Antiproton flux Astrophysic: B/C constraints Nuclear cross sections!! Fiorenza Donato, this afternoon Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 100

101 Antiproton spectra: Upper and lower bounds of due to the uncertainties of propagation parameters Note: uncertainty will be reduced with the new PAMELA and AMS-02 B/C data Torsten Bringmann, Pierre Salati, astro/ph Aldo Morselli, INFN & Università di Roma Tor Vergata, 101

Conclusion GLAST launch is currently scheduled for Jan. 31 2008. Guest Investigator Program Proposals due September 9 http://glast.gsfc.

102 Conclusion GLAST launch is currently scheduled for Jan Guest Investigator Program Proposals due September 9 proposals/gi_program_backgr ound.html Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 102

The LAT Tracker numbers 11500 sensors 360 trays 18 towers ~ 1M

30M strip tested (30 test/strip on average) > 60 physicist and

Padova,, Pisa, Perugia, Roma2, Bari) ) in partnership with ASI Aldo

103 The LAT Tracker numbers sensors 360 trays 18 towers ~ 1M channels 83 m 2 Si surface > 240K functional test recorded in DB ~ 30M strip tested (30 test/strip on average) > 60 physicist and engineers involved in the italian teams from INFN (Trieste, Udine, Padova,, Pisa, Perugia, Roma2, Bari) ) in partnership with ASI Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 103

Uta Bilow, TU Dresden

Uta Bilow, TU Dresden 2 nd WCPE, São Paulo July 14, 2016 Particle Physics / High Energy Physics t 10-43 s t 10-35 s t 10-10 s t 10-4 s t 3 min t 300 000 y 10-34 m 10-32 m 10-18 m 10-16 m 10-12 m 10-10