Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 1
Particle Physics withSpace Detectors
Aldo MorselliINFN, Sezione di Roma 2 &
Università di Roma Tor Vergata
Roma, 18 Marzo 2004
Corso di Astroparticelle Anno 2003-2004
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 2
Cosa si vuole studiare?• Cielo nei raggi gamma• Antimateria nell'Universo• Brillamenti e tempeste solari• …….
Come?
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 3
Gamma ray attenuation
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 4
Gamma rayattenuation (2)
Relation between the temperatureof a black body and the frequencyat which most of the energy isemitted
Transparency of the atmospherefor radiation of differentwavelengths.The solid line show the heightabove sea-level at which theatmosphere becomes tranparent.
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 5
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 6
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 7
EGRET:the detector
Energy range: 20 MeV - 30 GeVWeight: 1820 KgPower: 160 WField of view: 0. 5 srDead Time: 100 msEffective Area (@1GeV) 1200 cm2
Angular resolution 5.8o
(@100MeV)
Sensitivity 0.1 GeV 5x10-8
for point 1 GeV 1x10-8
sources 10 GeV 2x10-8
(ph cm-2 s-1)*
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 8
EGRET – Principle ofgamma ray detection
A γ_ray which enters the top of the EGRETinstrument will pass undetected through the largeanticoincidence scintillator surrounding the sparkchamber and has a probability 33% of convertinginto an electron_positron pair in one of the thintantalum (Ta) sheets interleaved between the 28closely spaced spark chambers in the upper portionof the instrument.Below the conversion stack are two 4 x 4 arrays ofplastic scintillation detector tiles spaced 60 cm apartwhich register the passage of charged particles. If thetime_of_flight delay indicates a downward movingparticle which passed through a valid combination ofupper and lower scintillator tiles, and theanticoincidence system has not been triggered by acharged particle, the track information is recordeddigitally. In this manner, a three dimensional pictureof the path of the electron_positron pair is measured.The energy deposition in the NaI(Tl) Totalabsorption Shower Counter (TASC) locateddirectly below the lower array of plastic scintillatorsis used to estimate the photon energy.
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 9
Elements of a pair-conversion telescope
• photons materialize into matter-antimatter pairs: Eγ --> me+c2 + me-c2
• electron and positron carry information about the direction, energy and polarization of the γ-ray
(energy measurement)
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 10
Energy loss mechanisms:
Fractional energy loss for e+ and e- in leadPhoton total cross sections
Interaction of electrons and photons with matter
Pair
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 11
MultipleScattering
0.01
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0.15Xo(deg)0.07Xo(deg)0.05Xo(deg)
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0.15Xo(deg)0.07Xo(deg)0.05Xo(deg)
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E(GeV)
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 12
the deep sky
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 13
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 14
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 15
EGRET All Sky Map (>100 MeV)CygnusRegion
3C279
Geminga
Vela
CosmicRay
InteractionsWith ISM
LMCPKS0528+13
4PKS 0208-
512
Crab
PSRB1706-
44
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 16
Third EGRET Catalog
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 17
Binary system formed by a black hole and a companion star
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 18a rotating black hole in an accretion disk
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 19Models for High Energy Emission: A cartoon
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 20
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 21
Astroparticelle :Usare la fisica delle particelle per capire la struttura ed evoluzione dell'Universo(e/o viceversa)
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 22
What is the Universe made of ?observed
expectedfromluminous disk
M33 rotation curve
5 10 R(kpc)
v (km/s)
100
50
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 23
What is the Universe made of ?We know that there isdark matter, which isneeded to explain thedynamics of stars inGalaxies and of galaxiesin clusters. This darkmatter does notinteract with light, andwe do not know wichparticles is made of.
• The peripheral stars of the galaxy M63 rotate around the center so fastthat they would fly away in space without the presence of additional massinside the galaxy. This is indirect evidence for the presence of dark matter
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 24
Dark matter problemThe 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 densityΩ=ρ/ρcrit is : (ρcrit~1.5 g cm-2 )
Ω lum ≤ 0.01but from rotation curves must exist a galactic dark halo of mass at least:
Ω halo ≥ 0.1
from gravitational behavior of the galaxies in clusters the Universalmass density is : Ω halo ≅ 0.2 ÷ 0.3from structure formation theories and analyses of the CMB:
Ω halo ≥ 0. 3
but from big bang nucleosinthesis and analyses of the CMB the Barionic matter cannot be more
then: 0. 03 ≤ Ω B ≤ 0. 05 (astro-ph/0106035)
So the best candidate seems to be a Weakly Interacting Massive Particles (WIMP), but neutrinoswith mass less then 30 eV do not reproduce well the observed structure of the Universe, so theLSP is a good candidate to solve the Dark matter problem.
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 25
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=0.71 + 0.04 - 0.03
WMAP+SN+HSTastro-ph/0302209
astro-ph 0007333
Dark Energy
CDM
BaryonsCold Dark Matter
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 26
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 mν< 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.
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SupersymmetryParticle Sparticle
For unbroken supersymmetry they shoul be degenerate in mass
Sparticle have not be found at accelerators so far
Supersymmetry is brokenSupersymmetry breaking schemes:1) gravity-mediated scenarios2) Gauge mediated scenarios3) Anomaly mediated scenarios
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Andamento delle Costanti di Accoppiamento
Andamento delle costanti di accoppiamento in funzione dell'energia per il modello Standard delleparticelle elementari e per il Minimo Modello Supersimmetrico Minimale
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 29
Neutralino WIMPs
Assume χ present in the galactic halo• χ is its own antiparticle => can annihilate in galactic haloproducing 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 aninteresting signature• ie: χ χ --> p + X• Produced from (e. g.) χ χ --> q / g / gauge boson / Higgs boson andsubsequent decay and/ or hadronisation.
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 30
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:
• M1/2 the mass parameter of supersymmetric partners of gauge fields (gauginos)
• µ the higgs mixing parameters 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
• tang β = v2 / v1 = <H2> / <H1> the ratio between the two vacuum expectation values of theHiggs fields
(3S)
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 31
LEPExperimental
lower limit on themass of the
lightest neutralinoassuming MSSM
(Minimal StandardSupersymmetric Model)
Mχ > 50 GeV
Limits on Supersymmetry already established
hep-ph/0004169
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 32
SuperSymmetric Dark MatterPossible signature:Gamma Rayfrom NeutralinoAnnihilation
Annihilation at rest:bump around Neutralino mass
10 GeV 100 GeV
φγ
Diffuse background
(4S)
A=pseudoscalarχ±=charginoχ0 =neutralinoH=Higgs boson
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 33
Total photon spectrum from the galactic center from χχ ann.
γ lines50 GeV
300 GeV
Bergstrom et al.
Infinite energy resolution
With finite energy resolution
• Two-year scanning mode
(6S)
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HALO SUBSTRUCTURE
A.Font and J.Navarro, astro- ph/ 0106268
600 kpc
Milky Way
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Contours of photons intensity in units of 10-5 ph cm-2 sec-1 sr-1 for Eγ>1GeV, after subtraction of “best estimate of Galactic Diffuse model. Data indicates presence of a galactic halo (Dixon et al. 1998).
Search for the Nature of Dark Matter
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 36
Search for the Nature of Dark Matter• The EGRET team (Mayer-Hasselwander et al, 1998) have seen a convincing signal for a strong excess ofemission from the galactic center, with I(E) x E2 peaking at ~ 2 GeV, and in an error circle of 0.2 degreeradius including the position l = 0o and b = 0o. In their paper it was speculated that among other possiblecauses, this excess could be due to the continuum γ-ray spectrum from Wimp annihilation. With thedramatically improved angular resolution and effective area of GLAST, this effect should become both morelocalized and pronounced if it is a Galactic Center phenomenon.
EGRET Map ofGalactic Center
Region
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EGRET data & Susy models
~2 degrees around the galactic center
EGRET dataA.Morselli, A.Lionetto, A.Cesarini, F.Fucito, P.Ullio, 2002
Annihilation channel b-bbarMχ =50 GeV
background model(Galprop)WIMP annihilation (DarkSusy)Total Contribution
Nb=1.82 1021
Nχ=8. 51 104
Typical Nχ values:NFW: Nχ = 104
Moore: Nχ = 9 106
Isotermal: Nχ = 3 101
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 38
~2 degrees aroundthe galactic center,2 years data
(Galprop)(one example from DarkSusy)
GLAST Expectation & Susy models
astro-ph/0305075
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Differential yieldfor each annihilationchannel
WIMP mass=200GeV
total yields
yields not due to π0decay
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Differential yieldfor b bar
neutralino mass
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region where0.13 < ΩCDM.h2 < 1
GLAST sensitivity (5 σ) for aneutralino density Nχ of 104 ina ΔΩ=10-5 sr region around thegalactic center
Minimal Supersymmetric Standard Model with:A0 = 0, µ > 0, mt =174 GeV
Typical Nχ values for ΔΩ=10-5 sr :NFW: Nχ = 104
Moore: Nχ = 9 106
Isotermal: Nχ = 3 101
A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, astro-ph/0305075 v.2
Estimated reaches with GLAST
region where0.09 < ΩCDM.h2 < 0.13
if GLAST do not see Supersymmetrythis region is excluded for a NFW halo mh0 <114.3 GeV GeV
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 42
region where0.13 < ΩCDM.h2 < 1
GLAST sensitivity (5 σ) for aneutralino density Nχ of 104
in a ΔΩ=10-5 sr region aroundthe galactic center
Minimal Supersymmetric Standard Model with:A0 = 0, µ > 0, mt =174 GeV
Typical Nχ values for ΔΩ=10-5 sr :NFW: Nχ = 104
Moore: Nχ = 9 106
Isotermal: Nχ = 3 101
updated from A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, astro-ph/0305075
Estimated reaches with GLAST
region where0.09 < ΩCDM.h2 < 0.13
if GLAST do not see Supersymmetrythis region is excluded for a NFW halo mh0 <114.3 GeV GeV
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 43
Positron Ratio
(Phys.Rev. D59 (1999) astro-ph 98008243)
•Background from normal secondary production
•Signal from ~ 300 GeV neutralino annihilations
Caprice94 data from ApJ , 532, 653, 2000
(ApJ 493, 694, 1998)
• Caprice98 data from XXVI ICRC, OG.1.1.21, 1999
Total
Signal from neutralino annihilations
Background from normal secondary production
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 44
PAMELAPOSITRONSexpectation
Secondary production
‘Leaky box model’Secondary production‘Moskalenko + Strongmodel’ withoutreacceleration
Primary productionfrom χ χannihilation
(m(χ) = 336 GeV)Primary production
for 3 years of operation
Secondary production
Total
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AMS98
Background from normal secondary production
Signal from 964 GeVneutralino annihilations ( astro-ph 9904086)
Mass91 data from XXVI ICRC, OG.1.1.21 , 1999
Caprice94 data from ApJ, 487, 415, 1997
Caprice98 data fromApJ, 561, (2001), 787. astro-ph/0103513
Distortion of the secondary antiproton flux induced by a signal from a heavy Higgsino-like neutralino.
Particles and photons aresensitive todifferent neutralinos.Gaugino-like particles aremore likely to produce anobservable flux of antiprotonswhereas Higgsino-likeannihilations are more likely toproduce an observablegamma-ray signature
∆ BESS data from Phys.Rev.Lett, 2000, 84, 1078
AMS data : preliminary
BESS 00
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PAMELA: Cosmic-Ray AntiparticleMeasurements: Antiprotons
Secondary production(upper and lower limits)Simon et al.
Secondary production(CAPRICE94-based)Bergström et al.
Primary productionfrom χχ annihilation(m(χ) = 964 GeV)
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RaggiCosmici
Come?
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MASS Matter Antimatter Space Spectrometer
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 49
The CAPRICE 94 flight
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48 cm
48 cmThe TS93 and CAPRICE silicon-tungsten imaging calorimeter.
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CAPRICE 94
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CAPRICE98
Proton energyspectrumat the top ofatmosphere
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The heliumenergyspectrum atthe top ofatmosphere
CAPRICE98
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SilEye on MIR Space Stationwizard.roma2.infn.it
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The complete detector
NINA 2 on MITA
Launch of NINA 1 : 10/8/1998Launch of NINA 2 : 15/7/2000More info: http://wizard.roma2.infn.it
The basic silicon detectorThe basic silicon detector
The NINA instrumentNINA2-MITALaunch
a silicon wafer 6x6 cm2 , 380 µm thick with 16 strips, 3.6 mm wide in two orthogonal views X -Y
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 56
Sampex, Imp 8, NINA
GOES 7, 8,
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PAMELA
RESURS-DK1 SatelliteMass: 10500 KgElliptical Orbit 70.4° incl.300-600 Km altitudeLaunch: December 2002Mission Life > 3 Yr.Launcher : Soyuz-TM
Physics Objectives♦ AntiProton spectrum : 80 MeV - 180 GeV♦ Positron spectrum : 50 MeV - 200 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 KgTotal Mass: ~750 KgPower: 350 WGF: 21 cm2srMDR: 740 GV/c
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 58
Separating pfrom e-
TOF : Time of Flight (S1) Pamelaantiproton
TRD : Transition Radiation Detector
TOF : Time of Flight (S2)
Magnetic Spectrometer
TOF : Time of Flight (S2)
Silicon Calorimeter
positron
1 m
S4 and Neutron detectors
Tracker(s)SiliconStripDetectors
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PamelaTRDTRD
TRKTRK
NDND
TOFTOF
ANTIANTI
CALOCALOMassa del rivelatore 440 KgPotenza 355 WMDR – 770 GV
Protoni 80 MeV – 700 GeVAntiprotoni 80 MeV –190 GeVElettroni 50 MeV – 2 TeVPositroni 50 MeV - 270 GeVNuclei < 700 GeV/nLimite per Antinuclei 10-8
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 60
TRDTRD
TRD
• Threshold detector.
• 9 radiator planes (carbon fiber)and straws tubes (4mm diameter)filled with Xe-CO2 mixture.
• e/p separation (E > 1 GeV/c) atlevel of 10-2.
TRKTRKSi Tracker + magnet
• Permanent magnet B=0.4T
• 6 planes double sided Si strips300 µm thick
• Spatial resolution ~3µm
• MDR = 740 GV/c
TOFTOF
Time-of-flight
• Level 1 trigger
•Albedo discrimination
• dE/dx (Z)
• particle identification (up to1GeV/c)
• Plastic scintillators + PMTs
• Time Resolution ~ 110 ps
ANTIANTI
Anticoincidence system
• Defines tracker acceptance
• off-line or on-line veto
• Plastic scintillators + PMTs
S4 S4 NDND
S4 and Neutron detectors
• Extend the energy range forprimary protons and electronsup to 10 TeV
•Plastic Scintillator. Trigger forneutron detector
• 36 3He counters in apolyetilen moderator
PAMELA DETECTOR
CALOCALO
Si-W Calorimeter
• Imaging Calorimeter :reconstructs shower profile.
Si-X / W / Si-Y structure
22 W planes 16.3 X0 / 0.6 l0
• rejection power e+/p and p/e-
at level of 10-4 ~ 10-5
• Energy Resolution for e±
ΔE/Emeasured < 5% ( 20-200 GeV )selftriggeringG.F.~ 470 cm2 srElectrons up to 2 TeV
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New Detector Technology• Silicon strip detector
Strip-shapedPN diode
50-500micron wide
300-500micron thick
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)
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Silicon Strip Detector Principle
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TRD
CALORIMETER
SPECTROMETER
ANTICOINCIDENCE
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MASS THERMAL MODELMASS THERMAL MODELFLIGHT MODEL FLIGHT MODEL (CERN TEST BEAM)(CERN TEST BEAM)
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10 GeV e-
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10 GeV p
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The Resurs-DK1 satelliteCarrier rocket: SOYUZ
PAMELA Launch
Presurizedcontainer withPAMELAin operatingpositionPAMELA in
launchingposition
field of view
Expected Date of launch :end of 2004
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ANTIPROTON
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AMSLancio: 2007Durata: 3 anni
Protoni fino ad alcuni TeVAntiprotoni fino a 200GeVElettroni fino al TeVPositroni fino a 200 GeVNuclei fino ad alcuni TeVAntiNuclei fino al TeVγ fino a 100 GeVIsotopi leggeri fino a 20GeV
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AMS
Altezza: 320-390 KmAltezza: 320-390 KmInclinazione 51.7Inclinazione 51.7°°
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 71AGILE
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 72
AGILE
AntiCoincidence PhotomultipliersTop: 0.5cm plastic scintillatorLateral: 12 panels 0.6 cm
1.5 X0 CsI Calorimeter1.4*2*40 cm3 bars
X/Y plane, 121 mm pitchdistance between planes 1.6cm
W 0.07 X0
Super Agile Mask Super Agile Silicon plane
Tracker , 14 X/Y planes
Calorimeter
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 73
AGILE
AntiCoincidence Top: 0.5cm plastic scintillatorLateral: 12 panels 0.6 cm
1.5 X0 CsI Calorimeter1.4*2*40 cm3 bars
X/Y plane, 121 µm pitchdistance between planes 1.6cm
W 0.07 X0
Super Agile Mask
Super Agile Silicon plane
25 cm
14 cm
Tracker , 14 X/Y planes
40cm
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Cos-B 8/1975-4/1982
SAS-2 11/1972-7/1973
Energy Calorimeter
Spark ChamberTrigger Telescope
Cerenkov Counter
Anti-Coincidence Dome
AGILE2002-
EGRET4/19911999
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AGILE Silicon Tracker prototype ladder
5 8x8 cm**2 CANBERRA silicon detectors with 195um strip pitch. The detectors aremechanical samples. The mechanical assembly and bonding hasbeen done by Mipot SPA. The procedure is as follows:-> the detectors are aligned one at a time and glued head on with non conductive expoxy gluewhich is made to polimerize with an infrared lamp for 20 minutes.
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AGILE Silicon Tracker prototype
TA1Silicon wafer
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AGILE Silicon Tracker beam test prototype
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Three dimensional PSF as a function of photon energy for AGILE and EGRET.
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GRB studies with AGILE
• Expected detection rate (above 50 MeV): 5-10 yr-1• Broad band spectral information: ~ 200 keV - 30 GeV• Rapid communication of GRB quicklook results
GRB 930131 • Study of the initial impulsive phase: Δt< 1 ms• Expected detection rate (above 50 MeV): 5-10 yr -1
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More information on AGILE :
please visit us:
http://www.ifctr.mi.cnr.it/agile/ http://www.roma2.infn.it/infn/agile/
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GLAST
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GLASTScheme
Gamma-RayLarge Area SpaceTelescope
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Gamma-Ray Large Area Space Telescope
AnticoincidenceShield
Imaging calorimeter tower ( 8.5 Rad.Length)
Silicon Tracker tower18 planes of X Y silicon detectors + converters12 trays with 2.5% R.L. of Pb , 4 trays with 25% ,2 trays without converters
1.68 m
84 cm
4*4 array of towers
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GLAST Instrument Description
EGRET GLAST simulation
Geminga
Crab
Geminga
Crab
IC 443
General Characteristics: imaging, wide field-of-view, pair-conversion telescope, backed by EMcalorimetry using modern HEP technology:
energy range: 10 MeV to 300 GeVenergy resolution: 10%effective area: > 8,000 cm2 (above 1 GeV)field-of-view: ~2π sr
point source sensitivity: 2 x 10-9 ph cm-2 s-1 (@ 100 MeV) 10-10 ph cm-2 s-1 ( > 1 GeV)
source location determination: 30 arcsec - 5 arcmincosmic ray/γ rejection > 105 to 1
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EGRET(Spark Chamber) VS. GLAST(Silicon Strip Detector)
EGRET on Compton GRO(1991-2000)
GLAST Large Area Telescope(2006-2015)
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Detector Technology: X-ray vs. Gamma-ray
X-ray (0.5 - 10keV)Focusing possible
Large effective areaExcellent energy resolutionVery low backgroundNarrow view
Gamma-ray(0.1-500GeV)No focusing possible
Wide field of viewLimited effective areaModerate energy resolutionHigh background
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 87
GLAST Large Area Telescope (LAT) DesignInstrument
Pair-conversion telescope
16 towers ⇒ modularity
height/width = 0.4 ⇒ large field-of-view
Tracker ModulesSi-strip detectors: fine pitch: 236 µm, high efficiency
12 front tracking planes (x,y): 0.45 Xo
reduce multiple scattering 4 back tracking planes (x,y): 1.0 Xo increase sensitivity > 1 GeV
One of 18Tracker trays(detectors top &
bottom)
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 88
GLAST Large Area Telescope (LAT) DesignInstrument
Pair-conversion telescope
Calorimeter Modules
16 towers ⇒ modularity
height/width = 0.4 ⇒ large field-of-view
Mechanical Prototype ofCarbon Cell Design
8.5 rl
Compression Cell Design
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
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 89
GLAST Large Area Telescope (LAT) DesignInstrumentPair-conversion telescope
Anticoincidence ShieldSegmented, plastic scintillator tile array: high efficiency, low-noise, hermetic;
segment ACD sufficiently and only veto event if a track points to hit tile
16 towers ⇒ modularity
height/width = 0.4 ⇒ large field-of-view
ACD tile readoutwith Wavelength
Shifting Fiber
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 90
GLAST Performance
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200 γ bursts per year
⇒ prompt emission sampled to > 20 µs
AGN flares > 2 mn
⇒ time profile + ΔE/E
⇒ physics of jets and acceleration
γ bursts delayed emission
GLAST LAT Strength-Large Field of View-
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 92
GLAST LAT Strength- Continuous All-sky Monitoring -
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In scanning mode, the LAT will achieve after one daysensitivity sufficient to detect (5σ) the weakest EGRETsources
All 3EG sources + ~ 80 new in 2days
⇒ periodicity searches
(pulsars, X-ray binaries)
⇒ pulsar beam, emission vs.
luminosity, age, B
GLAST LAT Strength- New EGRET Catalog Every 2 days -
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 94
One year All-Sky Survey Simulation, Eγ > 100 MeV
All-sky intensity map based on five years EGRET data.
All-sky intensity map from a GLAST one year survey, based on the extrapolation of the number of sourcesversus sensitivity of EGRET
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 95
Active Galactic Nuclei (AGN) γ-ray emission:
Unanswered questions• What are the “primary particle in the γ-ray emitting beam?
• How are particles accelerated….. And where ?
• What is the highest energy the particles are accelerated to ?
( TeV- 107 - 108 TeV ?? )
• What causes AGN γ-ray flares?
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 96
Flux absorption due to the interaction with the infrared and microwave background
γ ray source
Microwave and infrared background
Earth
Ε=ω2
γ
γ
e+
e-
Ε=ω1
ϑ
if the center of mass energy is:
photons interactions produce electron positron pairs
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 97
Flux absorption due to the interaction with the infrared and microwave background (2)
Ε=ω1
γ
γ
e+
e-
Ε=ω2
ϑ ω1 and ω1 are respectively the energies of the low and the high energies gamma ray and ϑ is their angle of incidence.
The cross section of the process γγ −> e+e- is:
where re is the classical radius of the electron and:
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 98
Flux absorption due to the interaction with the infrared and microwave background (3)
γ
γ
e+
e-
Ε=ω1
Ε=ω2
ϑ
the ratio between the flux I(L) at a distance L from the sourceand the initial flux I can be written as:
I(L)/Io=exp(-kγ L)
where kγ is the absorption coefficient:
that contains the cross section and the low energy photon distribution.For the microwave spectrum:
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 99
10-4
10-3
10-2
10-1
100
10-2 100 102 104 106 108
Total Absorption ( microwave + infrared)
Atte
nuat
ion
( I /
I 0 )
E(TeV)
Z=1 (high)
Z=0.03 (high)
Z=0.03 (low)
infrared only
Z=0.03 (high)
Ratio between surviving flux and initial flux versus photon energiesfor two different distances due to the sum of the infrared and black-body background
(4)
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 100
Transparency of the Universe
100 GeV
IR
radio
2.7 kOur galaxy
Super Cluster
γ γ e+ e-
p γ e+ e-
p γ π + π -Z~1 ~ 2 1028 cm
Z~0.03 ~2 1026 cm
E(eV)
Dist
ance
(mpc
)
1010 1012 1014 1016 1018 1020 1022 1024
10 TeV
10-3
10-2
10-1
100
101
102
103
104
105
(Mrk521)
Z~0.53, 2C279
Z~10-6 cm
Andromeda(700 kpc, 2.9Mly)LMC(50 kpc, 179kly)
Virgo Cluster 60mly, 18mpc
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 101
Flux absorption due to the interactionwith the infrared and microwave
background
an example on 3C279:• fixed background• different values of the Hubble constant
10-12
10-11
10-10
10-9
10-8
10-7
101 102 103
3C279
F(>E
) cm
-2 s-1
E(GeV)
Fb=1.52 10-3 E-2.55
Ho=100 km s -1 Mpc -1
Ho=75 km s -1 Mpc -1
Ho=50 km s -1 Mpc -1
F(>E
) cm
-2 s-1
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 102
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 103
GRB studies with GLAST (2)
• Broad band spectral information: ~ 200 keV - 30 GeV• Rapid (few seconds) communication of GRB quicklook results• Single γ angular resolution ~10 arcmin at high energies for good source localization.
• Study of the initial impulsive phase: Δt< 1 ms• Expected detection rate (above 50 MeV): 50-100 yr -1
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 104
Gamma ray missions deadtimeGamma -ray mission deadtime
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 105
Test of Quantum Gravity(1q)
Candidate effect:
c2 P2 = E2 ( 1+ f(E/EQG ))E=photon energy EQG =effective quantum gravity energy scale
Deformed dispersion relation with function f model dependent function of E/EQG
if E<< EQG series expansion is applicablec2 P2 = E2 ( 1+ α(E/EQG )+ Ο(E/EQG ) 2)
v = δE/δP ~ c ( 1+ α(E/EQG ))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 Lp~10-33 cm
Δt = ~ α E/EQG D/c
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 106
Test of Quantum Gravity (2) Δt = ~ α E/EQG D/c
D ~ 2 1028 cm EQG ~1019 GeV c~3 1010 cm Δt(ms) ~ 60 ΔE(GeV)
E1
E2
E1
E2
Δti=0 Δtf=0t=ti
E1
E2
t=tfE1
E2
even at pulsars distance: • D ~ 6 1021 cm Δt(µs) ~ 100 EQG ~1014 GeV
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 107
Cerenkov and Extensive air shower (EAS) gamma ray telescope concepts
Cerenkov
shower~8.5km
~ 40.000 m^2 , but no anticoincidence shield !
γ
Optical detector
EAS
Particle detectors
γ
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 108
Development of vertical 1-TeV proton and γ-ray showerProton γ-ray
Positions in the atmosphere of all showerelectrons above the Cerenkov threshold
Resulting Cerenkov images in the focal plane of a 10-m reflecting mirror .
Proton γ-ray
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 109
Whipple
Supernova remnants
MHK501
10 m telescopesE = >350 GeV
Location: Mt.Hopkinsin operation
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“Solar Farm” Cerenkov gamma ray telescope concept
CELESTELocation: Thémis , France
STACEELocation: Albuquerque
~40 m2 mirror areaE =20 GeV - 200 GeV
Schedule: in test
Gamma-ray
heliostats
Secondary reflector
Camera boxWith PMT’s
Solartower
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 111
Hegra Telescope CT2car
220 m2 mirror areaE =10 GeV- 300 GeVLocation: La Palma(Canary Islands)Scheduled June 2004
MAGIC
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 112
7 Whipple like 10 mtelescopesE = 50 GeV -50TeVLocation: southern ArizonaScheduled 2005?
Whipple
Veritas
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 113
HESS Phase 2four 110m2 telescopesField of view 5 degDetection capabilityat E > 40 GeVSpectroscopy at E > 100 GeVLocation: NamibiaScheduled 2004
(artistic composition) (not yet real ! )
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MILAGROArea 5000 m2
Field of view ~ 1 srE = 250 GeV - 50 TeVLocation: New Mexico2600m alt.Started June ‘99
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 115
ARGOArea 5.200 m2 (full coverage)(10.000 m2 with guard ring)Field of view ~ 1 srE = 50 GeV - 50 TeVLocation: Tibet 4300m alt.Scheduled 2002 (final conf.)
17400 Pads 56 by 60 cm2 each of ResistivePlate Chamber (RPC).Each pad subdivided in pick-up strips 6 cmwide for the space pattern inside the pad. The CLUSTER is made of 12 RPCs Pads
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ARGO
Test Carpetin Tibet
High voltage 8 kV
GAS
Resistive electrode plates Pick-up X strips
Pick-up Y stripsGRD
PVC Spacers
2 mm2 mm2 mm
The detector structure
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Longitudinal development of the electron component of photon initiated shower( with electron threshold energy of 5 MeV and fluctuations superimposed )
16 X0 Yanbajiging
Number of electrons in the shower
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Relation between altitude, number of Radiation Length and g/cm2 traversed
16 X0 Yanbajiging
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Sky coverage of “all sky “ and Cerenkov telescopes in 2002
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 120
High galactic latitudes(Φb=2 10-5 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 ofview detectors sensitivities (AGILE, GLAST, Milagro, ARGO, AMS) are for 1 year of observation.
Sensitivity of γ-ray detectors
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 121
X and Gamma-ray detectors INFNgroundbased
INFN-ASISpace borne
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Gamma-Ray Astronomy Long Term PlanUltimate Objective: To image the particle accelerator near the event
2005 2015 2025
Energy resolution
Angular resolution
Sensitivity
5 arc min
10 arc sec
0.03 arc sec
5 %
1%
?
10-10 cm-2 s-1
10-12 cm-2 s-1
10-14 cm-2 s-1
GLAST
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 123
creationaccelerationinjection
Underground, Under-ice, Underwater
Extensive Air ShowerDetectors
Direct detection
ParticleAstrophysicsExperiments
Modulation
furtheracceleration?
PropagationCosmic rays:about 10 Myears in the Galaxy(6-7 g/cm2)
23 Xo
γ
ν
Cosmic Rays
40 km
Atmosphere
Balloons ~ 40 km~3 g/cm2 residual atmosphere
Space experiments ~ 400 km
High MontainDetectors
Source
Cherencov Detectors
Particle Accelerators
il file PDF inhttp://people.roma2.infn.it/~aldo/
Aldo Morselli INFN, Sezione di Roma 2 & Università di Roma Tor Vergata 124
L'immagine seguente è stata usata per studiare i livelli di stress al CNR.Guarda i due delfini che saltano fuori dall'acqua.I due delfini sono identici.I ricercatori che hanno condotto lo studio sono giunti alla conclusione che una persona è ad un livello di stress troppoelevato se trova che i due delfini sono differenti. Il livello di stress è proporzionale alla quantità di differenze trovate,per cui più i due delfini sembrano differenti, più è elevato il livello di stress.Se vedete molte differenze tra i duedelfini, siete consigliati di smettere subito di studiare e fare immediatamente qualcosa di piacevole.