Aldo Morselli, INFN & Università di Roma Tor Vergata, 1
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1 Aldo Morselli, INFN & Università di Roma Tor Vergata, 1
2 Why study γ s? γ rays offer a direct view into Nature s largest accelerators. the Universe is mainly transparent to γ rays with < 20 GeV that can probe cosmological volumes. Any opacity is energy-dependent for higher energy. Most particle relics of the early universe produce γ rays when they annihilate or decay. Two GLAST instruments: LAT: 20 MeV 300 GeV GBM: 10 kev 30 MeV Launch: December year mission (10-year goal) 550km, ~26 o Large Area Telescope (LAT) GLAST Burst Monitor (GBM) Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 2
3 Precision Si-strip Tracker (TKR) ~80 m 2 Si, 18 XY tracking planes. Single-sided silicon strip detectors (228 µm pitch) Measure the photon direction; gamma ID. Hodoscopic CsI Calorimeter(CAL) Array of 1536 CsI(Tl) crystals in 8 layers. Measure the photon energy; image the shower. Segmented Anticoincidence Detector (ACD) 89 plastic scintillator tiles and 8 ribbons. Reject background of charged cosmic rays; segmentation removes self-veto effects at high energy. Electronics System Includes flexible, robust hardware trigger and software filters in flight software. Overview of LAT 16 towers-tkr+cal+daq γ Tracker ACD e + e Grid Calorimeter Systems work together to identify and measure the flux of cosmic gamma rays with energy 20 MeV - >300 GeV. Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 3
4 Gamma-Ray Large Area Space Telescope GLAST Scheme Aldo Morselli, INFN & Università di Roma Tor Vergata, 4
5 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 Japanese Institutions French Institutions Swedish 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 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 IN2P3/LPTA Laboratoire de Physique Theorique et Astroparticules, Montpellier 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 5
6 SLAC 12/16 Towers in the GRID on 7/10/05 Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 6
7 SLAC 16/16 Aldo Morselli, Towers INFN & in Università the di Roma GRID Tor Vergata, on 20/10/05 aldo.morselli@roma2.infn.it 7
8 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 8
9 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, 9
10 LAT MC Derived Performance Aldo Morselli, INFN & Università di Roma Tor Vergata, 10
11 Energy versus time for X and Gamma ray detectors Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 11
12 Sensitivity of γ-ray detectors AMS trk AMS Cal High galactic latitudes(φ b = γ cm -2 s -1 sr -1 (100 MeV/E) 1.1 ). 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 & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 12
13 GLAST LAT High Energy Capabilities EGRET on CGRO firmly established the field of high-energy gamma-ray astrophysics and demonstrated the importance and potential of this energy band. GLAST is the next great step beyond EGRET, providing a leap in capabilities: Very large Field of View (FOV) (~20% of sky), factor 4 greater than EGRET Broadband (4 decades in energy, including the essentially unexplored region E > 10 GeV) Unprecedented Point Spread function (PSF) for gamma rays (factor > 3 better than EGRET for E>1 GeV). On axis >10 GeV, 68% containment < 0.12 degrees (7.2 arc-minutes) Large effective area (factor > 5 better than EGRET) Results in factor > 30 improvement in sensitivity below < 10 GeV, and >100 at higher energies. Much smaller deadtime per event (27 µsec, factor ~4,000 better than EGRET s) No expendables long mission without degradation (5 year requirement, 10 year goal). Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 13
14 GLAST addresses a broad science menu of interest to both the High Energy Particle Physics and High Energy Astrophysics communities. Systems with (super-massive) black holes & relativistic jets Gamma-ray bursts (GRBs) Pulsars Origin of Cosmic Rays Probing the era of galaxy formation Discovery! Particle Dark Matter? Other relics from the Big Bang? Extra dimensions? New source classes? Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 14
15 Where should we look for WIMPs with GLAST? Galactic center Galactic satellites Galactic halo Extra-galactic Aldo Morselli, INFN & Università di Roma Tor Vergata, 15
16 Aldo Morselli, INFN & Università di Roma Tor Vergata, 16
17 Aldo Morselli, INFN & Università di Roma Tor Vergata, 17
18 EGRET data & Susy models Annihilation channel W + W - Mχ =80.3 GeV background model(galprop) WIMP annihilation (DarkSusy) Total Contribution ~2 degrees around the galactic center EGRET data N b = N χ = Typical Nχ values: NFW: Nχ = 10 4 Moore: Nχ = Isotermal: Nχ = 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 18
19 Signal rate from Supersymmetry gamma-ray flux from neutralino annihilation governed by supersymmetric parameters J(ϕ): governed by halo distribution Aldo Morselli, INFN & Università di Roma Tor Vergata, 19
20 GLAST Aldo Morselli, INFN & Università di Roma Tor Vergata, 20
21 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/ ] 21
22 EGRET, E > 1GeV Mayer-Hasselwander et al, 1998 Integral data 2 0 x 2 0 field IBIS/ISGRI kev Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 22
23 Point source location for GLAST~ 5 arcmin 1 pixel ~ 5 arcmin 2 0 x 2 0 field IBIS/ISGRI kev Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 23
24 2 0 x 2 0 field EGRET, E > 1GeV Point source location for GLAST~ 5 arcmin 1 pixel ~ 5 arcminaldo Morselli, INFN & Università di Roma Tor Vergata, 2 0 x 2 0 aldo.morselli@roma2.infn.it field IBIS/ISGRI kev24
25 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 25
26 cmssm Signal and Background are separated? tg(β)=55, sign(µ)=+1 Signal Background no electroweak symmetry breaking Aldo Morselli, INFN & Università di Roma Tor Vergata, 26
27 cmssm Signal and Background are separated? tg(β)=55, sign(µ)=+1 Signal Background no elecroweak symmetry breaking Aldo Morselli, INFN & Università di Roma Tor Vergata, 27
28 msugra Sensitivity plot for 5 years observation of msugra for GLAST for tg(b)=55. 3σ Sensitivity plot for for GLAST for a truncated (NFW) halo profile WMAP 3 3σ allowed region tg(β)=55, sign(µ)=+1 GLAST 3σ sensitivity is shown at the blue line and below for truncated NFW halo profile GLAST limits no electroweak symmetry breaking Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 28
29 msugra 3σ Sensitivity plot for for GLAST for a truncated (NFW) halo profile tg(β)=55, sign(µ)=+1 Sensitivity plot for 5 years observation of msugra for GLAST for tg(b)=55. WMAP 3 3σ allowed region mχ=300 GeV mχ=400 GeV GLAST 3σ sensitivity is shown at the blue line and below for truncated NFW halo profile GLAST limits mχ=200 GeV equi neutralino mass curves no electroweak symmetry breaking Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 29
30 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 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 30
31 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 31
32 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 32
33 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 33
34 Model independent results for the GC 1 deg radius, 4 years of operations, truncated NFW ( J(ψ)= 1200, E>1GeV) Aldo Morselli, INFN & Università di Roma Tor Vergata, aldo.morselli@roma2.infn.it 34
35 Model independent results for the GC Aldo Morselli, INFN & Università di Roma Tor Vergata, 35
36 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 31 Jan 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 36
37 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 37
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