Search for supersymmetric dark matter with space experiments

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Legacy of LEP and the SLC Siena, 8-11 October 2001 Thursday 11 October

1 Search for supersymmetric dark matter with space experiments Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata The Legacy of LEP and the SLC Siena, 8-11 October 2001 Thursday 11 October 2001 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 1

2 Gamma ray attenuation ~400Km ~40Km ~10Km ~4Km 0 Km 1µeV 1meV 1eV 1KeV 1MeV 1GeV Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 2

3 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 3

4 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 4

EGRET Principle of gamma ray detection A γ_ray which enters the top of the EGRET instrument will pass undetected through the large anticoincidence scintillator surrounding the spark chamber and has a

5 EGRET Principle of gamma ray detection A γ_ray which enters the top of the EGRET instrument will pass undetected through the large anticoincidence scintillator surrounding the spark chamber and has a probability 33% of converting into an electron_positron pair in one of the thin tantalum (Ta) sheets interleaved between the 28 closely spaced spark chambers in the upper portion of the instrument. Below the conversion stack are two 4 x 4 arrays of plastic scintillation detector tiles spaced 60 cm apart which register the passage of charged particles. If the time_of_flight delay indicates a downward moving particle which passed through a valid combination of upper and lower scintillator tiles, and the anticoincidence system has not been triggered by a charged particle, the track information is recorded digitally. In this manner, a three dimensional picture of the path of the electron_positron pair is measured. The energy deposition in the NaI(Tl) Total absorption Shower Counter (TASC) located directly below the lower array of plastic scintillators is used to estimate the photon energy. Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 5

6 Search for the Nature of Dark Matter Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 6

Search for the Nature of Dark Matter The EGRET team (Mayer-Hasselwander et al, 1998) have seen a convincing signal for a strong excess of emission from the galactic center, with I(E) x E 2 peaking at

7 Search for the Nature of Dark Matter The EGRET team (Mayer-Hasselwander et al, 1998) have seen a convincing signal for a strong excess of emission from the galactic center, with I(E) x E 2 peaking at ~ 2 GeV, and in an error circle of 0.2 degree radius including the position l = 0 o and b = 0 o. In their paper it was speculated that among other possible causes, this excess could be due to the continuum γ-ray spectrum from Wimp annihilation. With the dramatically improved angular resolution and effective area of GLAST, this effect should become both more localized and pronounced if it is a Galactic Center phenomenon. EGRET Map of Galactic Center Region Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 7

8 Cosmic Ray Interaction with Inter Stellar Matter (1) Inner Galaxy ( l <60 o, b <10 o ) by EGRET. ID=Elect. Brems., IC=Inv. Compton, Isotr. Diff., and NN : 0 production and decay Galactic Background Model Strong et al. astro- ph/ Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 8

9 Distortion of the secondary positron fraction induced by a signal from a heavy neutralino. 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 Caprice94 data from ApJ, 532, 653, 2000 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 9

10 Positron with HEAT ICRC 01 p.1867 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 10

What is the Universe made of? We know that there is dark matter, which is needed to explain the dynamics of stars in Galaxies and of galaxies in clusters.

11 What is the Universe made of? We know that there is dark matter, which is needed to explain the dynamics of stars in Galaxies and of galaxies in clusters. This dark matter does not interact with light, and we do not know wich particles is made of. The peripheral stars of the galaxy M63 rotate around the center so fast that they would fly away in space without the presence of additional mass inside the galaxy. This is indirect evidence for the presence of dark matter Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 11

12 Dark matter problem The LSP can be a good candidate also for the solution of the Dark Matter Problem. Experimentally in spiral galaxies the ratio between the matter density and the Critical density Ω=ρ/ρ crit is : (ρ crit ~1.5 g cm -2 ) lum 0.01 but from rotation curves must exist a galactic dark halo of mass at least: halo 0.1 from gravitational behavior of the galaxies in clusters the Universal mass density is : halo from structure formation theories and analyses of the CMB: halo 0. 3 but from big bang nucleosinthesis and analyses of the CMB the Barionic matter cannot be more then: B (astro-ph/ ) So the best candidate seems to be a Weakly Interacting Massive Particles (WIMP), but neutrinos with mass less then 30 ev do not reproduce well the observed structure of the Universe, so the LSP is a good candidate to solve the Dark matter problem. Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 12

13 Observational constraints on Ω m and Ω λ. Ω m ~0.3 Ω λ ~0.7 A.H. Jaffe et al., Astro-ph Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 13

14 Supernova constraints to cosmological model A.Riess, astro- ph/ Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 14

15 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 ν < 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 15

16 Why Supersymmetry? (1 S ) The standard electroweak model is very successful but nevertheless has some problems: the unitarity of electroweak interaction breaks down at energy Scales < 1 TeV in the absence of a mechanism to account for electroweak symmetry breaking it leaves many fundamental parameters unexplained (like sin 2 ϑ W ) moreover the gauge structure in the standard model suggest the existence of a Grand Unified theory of electroweak and strong interaction at an energy around GeV and at energies around the Plank mass GeV there is the need of a theory that includes the Gravitational force because the quantum gravitational effects cannot be neglected. The Supersymmetry seems to be the most promising field of research to solve these problems. If Supersymmetry is true there is the prediction of the existence of a whole class of new particles that are the supersymmetric partners of the known particles. In particular the Lightest Supersymmetric Particle (LSP) must be stable by R-parity conservation and can escape detection due to its weakly interacting nature. Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 16

17 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, Sezione di Roma 2 & Università di Roma Tor Vergata 17

18 Termal relics Freeze out at h 2 = m n ρ c cm 3 sec -1 σ a v Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 18

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

19 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, Sezione di Roma 2 & Università di Roma Tor Vergata 19

20 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: M2 the mass parameter of supersymmetric partners of gauge fields (gauginos) the higgs mixing parameters µ that appears in the neutralino and chargino mass matrices m0, 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 β = 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 GeV ( Lep, s = 189 GeV) UHM : universal soft supersymmetry-breaking scalar masses for Higgs nuhm: non-universal 1999 : available LEP data 2000 : assessment of the likely sensitivity of data to be taken in ( the µ<0 plot is similar) hep-ph/ Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 20

21 SuperSymmetric Dark Matter (4 S ) Possible signature: Gamma Ray from Neutralino Annihilation Annihilation at rest: bump around Neutralino mass φ γ Diffuse background 10 GeV 100 GeV A=pseudoscalar χ ± =chargino χ 0 =neutralino H=Higgs boson Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 21

22 (5 S ) Signal rate from Supersymmetry The signal rate is : where: is the local halo neutralino density in units of 0.4 GeV/cm 3 f halo is a factor that can vary between 0.3 and 2 due to the uncertainty in modeling the galactic halo. Sensitivity of GLAST up to 300 GeV ~ cm -2 s -1 with f halo ~1, ρ 0.4 χ ~ 3, b = ( 100 MeV / E(MeV) ) -1.1 photon cm -2 s -1 sr -1 In two years, full eff. E/E ~5% min ph cm -2 s -1 sr -1 E/E ~10% min ph cm -2 s -1 sr -1 GLAST has the possibility to explore a good portion of the possible values of this parameters space Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 22

23 (5b S ) Signal rate from Supersymmetry (2) But in more general form we have: where: is the angle between the line of sight and the Galactic center, r( ) is the distance along that line of sight I( ) is the angular dependence of the gamma-ray flux. The galactic dark matter density distribution can have the form ρ(r) ~ r α with α ~ 1.8 and the predicted photon flux can be 10 4 brighter from certain directions! (the sources can appear nearly point-like) R ~ 8.5 kpc Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 23

24 HALO SUBSTRUCTURE Milky Way A.Font and J.Navarro, astro- ph/ kpc Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 24

25 Gamma ray fluxes from substructures as seen in the N-body simulations L. Bergstrom, J. Edsjo and C. Gunnarssonz, astro- ph/ Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 25

26 Total photon spectrum from the galactic center from ann. (6 S ) Two-year scanning mode Infinite energy resolution γ lines With finite energy resolution 50 GeV 300 GeV Bergstrom et al. Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 26

27 GLAST Performance : Energy resolution for lateral photons σ E /E =1.5% θ > 56 0 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 27

Number of photons expected in GLAST for cc -> gg from a 1-sr cone near the galactic center (7 S ) higgsino-like neutralino higgsino-like neutralino gaugino-like

28 Number of photons expected in GLAST for cc -> gg from a 1-sr cone near the galactic center (7 S ) higgsino-like neutralino higgsino-like neutralino gaugino-like gaugino-like Two-year scanning mode exposure. Each point is a different set of Minimal SuperSymmetric Standard Model parameters The galaxy dark matter halo profile giving the maximal flux has been assumed. The solid line shows the number of events needed to obtain a five-sigma detection over the galactic diffuse gamma-ray background as estimated from EGRET data. Bergstrom et al. astro-ph/ χ γ χ γ or Ζ Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 28

Sensitivity of γ-ray detectors MSSM A 0 = 0 µ > 0 m t =174 GeV tan β = 50 m 0 =1000 m 1/2 =300 Ω d.m. h 2 ~0.15 AMS Aldo Morselli 01/01 http://www.roma2.infn.

29 Sensitivity of γ-ray detectors MSSM A 0 = 0 µ > 0 m t =174 GeV tan β = 50 m 0 =1000 m 1/2 =300 Ω d.m. h 2 ~0.15 AMS Aldo Morselli 01/01 All sensitivities are at 5σ. 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 are for 1 year of observation. MAGIC sensitivity based on the availability of high efficiency PMT s Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 29

30 Diffuse gamma ray flux from cosmological ann. In this case broader line due to redshift. EGRET extragalactic diffuse data m = 86 GeV m = 166 GeV Bergstrom et. al. astro-ph/ Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 30

31 In the minimal supersymmetric extension of the Standard Model four neutral spin-1/2 Majorana particles are introduced: the partners of the neutral gauge bosons B, W the neutral CP-even higgsinos H 0 1, H0 2. Diagonalizing the corresponding mass matrix, four mass eigenstates are obtained. The lightest of these, is commonly referred as the neutralino. It is useful to introduce the gaugino fraction Z g defined as: Z g = N N 2 2 and classify the neutralino as higgsino-like when Z g <0.01, mixed when 0.01 < Z g < 0.99 and gaugino like if Z g >0.99. Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 31

32 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 Caprice94 data from ApJ, 487, 415, 1997 Background from normal secondary production Signal from 964 GeV neutralino annihilations ( astro-ph ) BESS data from Phys.Rev.Lett, 2000, 84, 1078 HEAT data from Phys.Rev.Lett, 1996, 76, 3057 Mass91 data from XXVI ICRC, OG , 1999 Caprice98 data sub.to ApJ, astro-ph/ (prelim.on ApJ Letters 534, L177, 2000, May 10) Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 32

33 Distortion of the secondary positron fraction induced by a signal from a heavy neutralino. 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 Caprice94 data from ApJ, 532, 653, 2000 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 33

34 Distortion of the secondary positron fraction induced by a signal from a heavy neutralino. M K s =11.7 GeV M K s = GeV BR(e + e - ) M K s =19 GeV M K s =54 GeV Baltz & Edsjö Phys.Rev. D59 (1999) astro-ph Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 34

35 Distortion of the secondary positron fraction induced by a signal from a heavy neutralino. Distortion of the secondary antiproton flux induced by a signal from a heavy Higgsino-like neutralino. Expected data from Pamela for one year of operation are shown in red. P.Picozza and A.Morselli,astro-ph/ Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 35

Excluded by LSP to be Neutral Estimated reaches before LHC 0.025 < Ω d.m. h 2 < 1 0.1 < Ω d.m. h 2 < 0.

36 Excluded by LSP to be Neutral Estimated reaches before LHC < Ω d.m. h 2 < < Ω d.m. h 2 < 0.3 GLAST MSSM A 0 = 0 µ > 0 m t =174 GeV tan β = 10 Direct search Pamela, AMS Km 3 Fixed Halo profile, indirect limits better if halo is clumpy See astro-ph Excluded by chargino mass limit > 95 GeV Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 36

Estimated reaches before LHC 2 Excluded by LSP to be Neutral 0.025 < Ω d.m. h 2 < 1 0.1 < Ω d.m. h 2 < 0.

37 Estimated reaches before LHC 2 Excluded by LSP to be Neutral < Ω d.m. h 2 < < Ω d.m. h 2 < 0.3 GLAST All the plane Direct search MSSM A 0 = 0 µ > 0 m t =174 GeV tan β = 50 Km 3 Pamela, AMS Fixed Halo profile, indirect limits better if halo is clumpy See astro-ph Excluded by chargino mass limit > 95 GeV Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 37

Excluded by LEP Estimated reaches before LHC 3 0.025 < Ω d.m. h 2 < 1 0.1 < Ω d.m. h 2 < 0.

38 Excluded by LEP Estimated reaches before LHC < Ω d.m. h 2 < < Ω d.m. h 2 < 0.3 MSSM A 0 = 0 µ > 0 m t =174 GeV M 1/2 = 400 GeV Fixed Halo profile, indirect limits better if halo is clumpy Direct search GLAST Km 3 See astro-ph Pamela, AMS Excluded by LEP Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 38

PAMELA Physics Objectives AntiProton spectrum : 80 MeV - 180 GeV Positron spectrum : 50 MeV - 200 GeV Search for Antinuclei e + + e - up to 1 TeV

Mass: 450 Kg Total Mass: ~750 Kg Power: 350 W GF: 21 cm 2 sr MDR: 740 GV/c RESURS-DK1 Satellite Mass: 10500 Kg Elliptical Orbit 70.4 incl.

39 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 2002 Mission Life > 3 Yr. Launcher : Soyuz-TM Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 39

40 An overview of PAMELA TOF : Time of Flight System TRD : Transition Radiation Detector 1.2m Magnetic Spectrometer TRK : Silicon Tracker CAL : Electromagnetic Si/W Calorimeter ANTI :Anticoincidence System Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 40

Pamela Separating p from e - For more information: http:/wizard.roma2.infn.

41 Pamela Separating p from e - For more information: Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 41

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.

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.

42 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 42

43 New Detector Technology (for space) Silicon strip detector Strip-shaped PN diode micron thick micron wide VLSI amplifier Stable particle tracker that allows micron-level tracking of gamma-rays Well known technology in Particle Physics experiments. Used by our collaboration in balloon experiments (MASS, TS93, CAPRICE), on MIR Space Station ( SilEye) and on satellite (NINA) Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 43

44 MASS Matter Antimatter Space Spectrometer GAS CHERENKOV TOF MAGNET TRACKING SYSTEM 1 m TOF CALORIMETER Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 44

45 The CAPRICE 94 flight Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 45

46 CAPRICE94 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 46

The NINA instrument a silicon wafer 6x6 cm

6 mm wide in two orthogonal views X -Y The

Launch of NINA 1 : 10/8/1998 Launch of NINA

47 The NINA instrument a silicon wafer 6x6 cm 2, 380 µm thick with 16 strips, 3.6 mm wide in two orthogonal views X -Y The basic silicon detector NINA 2 on MITA Launch of NINA 1 : 10/8/1998 Launch of NINA 2 : 15/7/2000 The complete detector More info: Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 47

48 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 48

49 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 49

50 GLAST Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 50

51 Gamma-Ray GLAST Large Area Space Telescope Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 51

52 Gamma-Ray Large Area Space Telescope 4*4 array of towers 1.68 m 84 cm Anticoincidence Shield Imaging calorimeter tower ( 8.5 Rad.Length) Silicon Tracker tower 18 planes of X Y silicon detectors + converters 12 trays with 2.5% R.L. of Pb, 4 trays with 25%, 2 trays without converters Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 52

53 GLAST Instrument Description General 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) ~2π 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/γ rejection > 10 5 to 1 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 53

planes (x,y): 0.45 X o reduce multiple scattering 4 back tracking planes (x,y): 1.

54 Instrument GLAST Large Area Telescope (LAT) Design Pair-conversion telescope 16 towers modularity height/width = 0.4 large field-of-view Tracker Modules Si-strip detectors: fine pitch: 236 µm, high efficiency 12 front tracking planes (x,y): 0.45 X o reduce multiple scattering 4 back tracking planes (x,y): 1.0 X o increase sensitivity > 1 GeV One of 18 Tracker trays (detectors top & bottom) Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 54

5 rl depth PIN photodiode readout from both ends: 2 ch/xtal x 80 xtals/mod = 2,560 ch segmentation allows pattern recognition (

55 GLAST Large Area Telescope (LAT) Design Instrument Pair-conversion telescope 16 towers modularity height/width = 0.4 large field-of-view Calorimeter Modules Hodoscopic Imaging Array of CsI crystals: ~ 8.5 rl depth PIN photodiode readout from both ends: 2 ch/xtal x 80 xtals/mod = 2,560 ch segmentation allows pattern recognition ( imaging ) and leakage correction Mechanical Prototype of Carbon Cell Design 8.5 rl Compression Cell Design Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 55

4 large field-of-view Anticoincidence Shield Segmented, plastic scintillator tile array: high efficiency,

56 Instrument GLAST Large Area Telescope (LAT) Design Pair-conversion telescope 16 towers modularity height/width = 0.4 large field-of-view Anticoincidence Shield Segmented, plastic scintillator tile array: high efficiency, low-noise, hermetic; segment ACD sufficiently and only veto event if a track points to hit tile ACD tile readout with Wavelength Shifting Fiber Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 56

57 GLAST Performance Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 57

GLAST LAT Strength - New EGRET Catalog Every 2 days - All 3EG sources + ~ 80 new in 2 days In scanning mode, the LAT will achieve after one day sensitivity sufficient to detect (5 ) the

58 GLAST LAT Strength - New EGRET Catalog Every 2 days - All 3EG sources + ~ 80 new in 2 days In scanning mode, the LAT will achieve after one day sensitivity sufficient to detect (5 ) the weakest EGRET sources periodicity searches (pulsars, X-ray binaries) pulsar beam, emission vs. luminosity, age, B Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 58

59 Summary of 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 π 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 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 59

60 The GLAST Participating Institutions Italian Team Institutions INFN - Instituto Nazionale di Fisica Nucleare: Units of Bari, Perugia, Pisa, Rome 2, Trieste 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 60

61 Energy versus time for X and Gamma ray detectors Energy 1 TeV 100 GeV 10 GeV 1 GeV 100 MeV WHIPPLE CAT HEGRA CANGAROO EGRET GRANITE MILAGRO ARGO HESS CELESTE, STACEE, Solar Two MAGIC Super Cangaroo AMS AGILE VERITAS G L A S T 10 MeV 1 MeV COMPTEL HESSI INTEGRAL MEGA 100 KeV 10 KeV BATSE OSSE SIGMA RXTE ASCA BeppoSAX HETE 2 Super AGILE Constellation-X 1 KeV ROSAT Chandra XMM Swift XEUS Year Aldo Morselli 15/02/01 Aldo Morselli 7/01 Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 61

62 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: beginning In 2005 GLAST will search for gamma-ray signature Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 62

63 2 nd 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 γ-ray from extragalactic sources and these are only additional items for GLAST! Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 63

Search for exotic process with space experiments

Search for exotic process with space experiments Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata Rencontres de Moriond, Very High Energy Phenomena in the Universe Les Arc, 20-27