Overview of the GLAST Observatory Current status of two instruments (GBM and LAT)

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1 GLAST LAT Project SSI Jul 29, 2005 Gamma Ray Large Area Space Telescope Eduardo do Couto e Silva SLAC SLAC Summer Institute Jul 29, 2005 E. do Couto e Silva 1

2 Outline Overview of the GLAST Observatory Current status of two instruments (GBM and LAT) GLAST Science Highlights of Instrument Capabilities Selected Physics Topics Particle Acceleration» Active Galactic Nuclei» Supernova Remnants Diffuse γ Ray Emission Dark Matter Searches and New Physics Timeline E. do Couto e Silva 2

3 GLAST Observatory : Overview GLAST will measure the direction, energy and arrival time of celestial γ rays Will follow on the measurements by its predecessor (EGRET) with unprecedented capabilities Orbit 565 km, circular Inclination 28.5 o LAT will record gamma-rays in the energy range ~ 20 MeV to >300 GeV Observing modes All sky survey Pointed observations Lifetime 5 years (min) Launch Date Aug 2007 Launch Vehicle Delta 2920H-10 Launch Site Kennedy Space Center Re-pointing Capabilities Autonomous Rapid slew speed (75 in < 10 minutes) GBM will provide correlative observations of transient events in the energy range ~10 kev 25 MeV E. do Couto e Silva 3

4 GLAST Burst Monitor: Overview LAT FoV NaI and BGO counters exposed to the entire sky Principal Investigator: Charles Meegan GBM FoV NaI crystals (12) ~10 kev to ~1 MeV low-energy spectral coverage in the typical GRB energy regime over a wide FoV rough burst locations over a wide FoV BGO crystals (2) ~150 kev to ~30MeV high-energy spectral coverage to overlap LAT range over a wide FoV GBM 10 kev to ~ 25 MeV Correlative observations of transient phenomena Spectral Measurements measures spectra for bursts and connects with LAT measurements Afterglows in Gamma Ray Bursts Wide Sky Coverage (8 sr) autonomous repoint for exceptionally bright bursts that occur outside LAT field of view (an important question from EGRET) Connections to the Ground Network of Telescopes burst alerts to the LAT and ground telescopes within seconds E. do Couto e Silva 4

5 Current Status of GBM Assembly 12 NaI modules 2 BGO modules Environmental Tests E. do Couto e Silva at Max Planck Institute 5

6 Principal Investigator: Peter Michelson Silicon Microstrip Tracker ~ 80 m 2 of silicon readout channels Strip pitch = 228 µm xy layers interleaved with W converters Total Rad length ~1.5 X 0 Large Area Telescope: Overview The LAT is a pair-conversion telescope of 16 towers surrounded by plastic scintillators γ Silicon Microstrip Tracker Measures γ direction γ identification Calorimeter Hodoscopic array Array of 1536 CsI(Tl) crystals in 8 layers Total Rad length ~8.5 X 0 e + e Calorimeter Measures γ energy Shower imaging Anti-Coincidence Detector 89 scintillator tiles Segmented design LAT 3000 kg, 650 W (allocation) 1.8 m 1.8 m 1.0 m 20 MeV 300 GeV Currently there is no other telescope covering this energy range E. do Couto e Silva 6 Anti-Coincidence Detector Rejects background of charged cosmic rays segmentation removes self-veto effects at high energy

7 Current Status of LAT Assembly 18 CAL modules completed 16 CAL SLAC ~80m 2 of silicon in hand. 8 TKR SLAC. Six Towers in the flight grid ACD completed and being tested at GSFC. Delivery to SLAC scheduled for mid August E. do Couto e Silva 7

8 LAT Data from Tests at SLAC From A. Borgland Photon Candidates 10-20% of cosmic ray showers are not muons Muon candidates Most of the 120Hz of triggers recorded with 6 towers are muons E. do Couto e Silva 8

9 Science with GLAST High Energy Sky Survey : Unidentified EGRET sources and GLAST Source Catalog Are these unresolved point sources? Population Studies To avoid peculiarities of individual sources (AGN, Pulsars, SNR ) Diffuse Gamma ray emission Galactic and Extragalactic Physics of particle acceleration formation of AGN jets, extraction of rotational energy from spinning neutron stars, dynamics of shocks in SNRs. role of hadrons in radiation processes in AGN and SNR High-energy behaviour of transients : Gamma Ray Burst Solar Flares Discovery Potential: New astrophysical objects Origin of Extragalactic Background Searches for Dark Matter and Extra Dimensions Tests of Lorentz Invariance LAT strengths: All-sky monitoring Broad range of time scales Energy range E. do Couto e Silva 9

10 LAT will Rediscover the γ Ray Sky GLAST 1 year E. do Couto e Silva 10

11 All Sky Monitoring with Improved Sensitivity 100 sec 1 orbit* EGRET Fluxes - GRB (100sec) - PKS flare - 3C279 flare - Vela Pulsar During the all-sky survey, GLAST will have sufficient sensitivity after O(1) day to detect (5σ) the weakest EGRET sources!!! - Crab Pulsar - 3EG (SNR γ Cygni?) 1 day^ - 3EG C279 lowest 5σ detection - 3EG (AGN) - Mrk Weakest 5σ EGRET source *zenith-pointed E. do Couto e Silva 11 ^ rocking all-sky scan: alternating orbits point above/below the orbit plane

12 Gamma Ray Bursts: GBM and LAT GBM Huge field of view (8sr) Measure spectra for bursts from 10 kev to 30 MeV LAT Wide field of view (>2sr) Extends spectral coverage to higher energies GLAST Can be re-pointed to catch exceptionally bright bursts that occur outside the LAT field of view GLAST all-sky monitoring will be follow transient phenomena to a wide range of time scales from ~ 100 µs (GRB, solar flares) to hours or longer (AGN) Simulated GBM and LAT response to time-integrated flux from bright GRB Spectral model parameters from CGRO wide-band fit 1 NaI (14 º) and 1 BGO (30 º) E. do Couto e Silva 12

13 AGN (Blazar): Emission Mechanisms (Buckley, Science, 1998) Adapted from P. Coppi Most of the AGN s found by EGRET were blazars Variability implies jets are relativistic Jets point towards us! Radiation is produced by the following processes (1 or more): Synchrotron Self Compton External Compton Proton Induced Cascades Proton Synchrotron Key issues to be addressed: Energetics of the source mechanism for jet formation mechanism for jet collimation nature of the plasma particle acceleration E. do Couto e Silva 13

14 Multiwavelenght Observations Contemporaneous observations with other wavelengths will help disentangle effects from state changes within individual sources GLAST will provide continuous baseline in GeV for ground based γ ray telescopes Below is an illustration from Aharonian et al. (astro-ph/ ) Blazar PKS rd EGRET catalog High γ-ray state (Verstrand et al. 1995) ~30 km Atmosphere: γ ~10 3 g cm -2 For E g > ~ O(100) GeV, must measure light emitted at the atmosphere (Cerenkov) GeV-TeV campaigns will be key to GLAST science! Multiwavelength planning in progress: ttp://glast.gsfc.nasa.gov/scienc e/multi/ E. do Couto e Silva 14

15 Adapted from P. Coppi Leptonic models Direct acceleration by electric fields e.g. pulsar Stochastic shock/wave acceleration e.g. 1 st and 2 nd order Fermi processes Hadronic models Particles are created at desired energies Do not need to be ultra relativistic but need large target densities (e.g. SNR) Easier to accelerate But harder to extract energy from Particle Acceleration E. do Couto e Silva 15

16 Time lags: hadronic or leptonic model in AGNs? Time correlation between AGN flares Favors hadronic processes γ rays leptonic processes are preferred by some theorists Hadronic models have not yet been excluded! X rays Credit: EGRET Team Changes in Luminosity in a fraction of a day! Variability constrains the size of the emitting source E. do Couto e Silva 16

17 SNR: Sites of Hadronic Acceleration? Supernova Remnants are considered sites of galactic cosmic ray acceleration Non-thermal emission has been seen in X-rays Signs of γ-ray activity EGRET measured GeV activity near SNR (3EG J ) Recent detection of TeV γ-rays by HESS does not agree with leptonic models Question: Do γ rays originate from hadronic or leptonic processes? GLAST will make measurements in the range of 100MeV-100GeV essential ingredient to resolve the origin (p vs e+/-) Supernova remnant RX J HESS 04 (color) + ASCA (contours) Uchiyama (2003) Adapted from Aharonian s talk at the Texas Symposium 2004 HESS data π 0 model e +/- model GLAST E. do Couto e Silva 17

18 AGN: Extragalactic Background Light High energy photons (GeV or TeV) from AGNs interact with intergalactic photons (IR or UV) leading to pair production the absorption is strongly dependent on the distance from the source (inferred from redshift) GLAST will see thousands of blazars instead of peculiarities of individual sources, look for systematic effects vs redshift key energy range for cosmological distances TeV-IR attenuation is more local due to opacity effect is model-dependent (this is good): No EBL A dominant factor in EBL models is the era of galaxy formation AGN roll-offs may help distinguish models of galaxy formation Salamon & Stecker Primack & Bullock How many blazars have intrinsic rolloffs in this energy range ( GeV)? An important question by itself for GLAST! Power of statistics is the key Must measure the redshifts for a large sample of these blazars! Chen, Reyes, and Ritz, ApJ 2004 E. do Couto e Silva 18

19 Gamma Ray Background Radiation About 90% of the γ ray emission is concentrated in the Galactic plane, these are thought to be high energy cosmic Rays that interact with the Interstellar medium (ISM) EGRET Gamma Ray Emissions > 100 MeV π 0 cosmic p e- rays ISM γ γ γ Extragalactic Background b > 10 deg Galactic Background falls rapidly at higher latitudes, away from the plane less gas, E. do Couto e Silva 19

20 Origin of Extragalactic Diffuse γ Radiation GLAST can shed light in one of the long-standing problems in high energy astrophysics The origin of the extragalactic radiation Original EGRET spectrum Galactic Diffuse γ ray is subtracted Reanalysis using slightly modified e- spectrum with respect to the local injected spectrum Strong, Moskalenko, Reimer (2004) What is it made of? Blazars we know New physics we can probe Primordial diffuse If else fails LAT E. do Couto e Silva 20

21 Galactic Diffuse Gamma Ray Emission The γ ray sky is dominated by diffuse emission Accurate modelling is essential EGRET GLAST Many more point sources Background determination for energy above 10 GeV Sharper definition of the diffuse background (smaller bins in the sky) E. do Couto e Silva 21

22 Complex Modeling of Particle Transport Sources of CR: SNRs, Shocks, Superbubbles Particle acceleration Photon emission Halo disk escape Courtesy of I. Moskalenko P He CNO X,γ e + - diffusion energy losses reacceleration convection etc. π + - _ P p ISM gas e + - B solar modulation synchrotron ISRF gas π 0 LiBeB He CNO IC bremss ACE Chandra GLAST Need to model Number density of primary nuclei Production cross section Gas distribution and composition BESS AMS Charged particle measurements will provide consistency checks for γ ray models E. do Couto e Silva 22

23 EGRET DATA: γ excess is controversial After diffuse background subtraction there was an excess of γ seen in the EGRET Data Revisited pp cross section accounts for a fraction of the GeV excess EGRET DATA New Model Old pp interaction models Constant inelastic cross-section Feynman scaling No diffraction dissociation Old Model New pp interaction model Rising cross-sections Scaling violation Diffraction dissociation E. do Couto e Silva 23 Kamae et al. 05, Kamae, Karlsson, Mizuno et al. 05, Kamae, Karlsson, Cohen-Tanugi Mizuno et al.05

24 Can WIMPs be the source of Dark Matter? Direct searches: scattering of WIMPS with nucleons in the detector DAMA, CDMS, EDELWEISS, etc. Indirect Searches: WIMP annihilations into other particles GLAST, ICECUBE, ANTARES, GENIUS, HEAT, AMS, etc Galactic Extragalactic Earth Sun Galactic Halo Galactic Center photons neutrinos neutrinos antideuterons positrons antiprotons photons positrons photons E. do Couto e Silva 24

25 Neutralino Annihilations Good particle physics candidate for galactic halo dark matter is the LSP in R- parity conserving SUSY χ 0 1 = ~ ~ ~ 3 0 a 11B + a12w + a13h ~ H If true, there may well be observable halo annihilations a 0 2 χ χ q q γγ or Zγ lines Example: χ 0 from Standard SUSY, annihilations to jets, producing an extra component of multi-gev γ flux that follows halo density (not isotropic) peaking at ~ 0.1 M χ 0 or lines at M χ 0. Background is galactic γ ray diffuse. Although calculation for γ-rays is less uncertain than for other signals (multi-gev antiprotons, positrons) a null result will not likely constrain SUSY parameter space. If SUSY uncovered at accelerators, GLAST may be able to determine its cosmological significance quickly. E. do Couto e Silva 25

26 DM from SUSY: γ line and continuum ˆ) F σj (n Clumpy halo increase rates! 1 J ( l) dl( nˆ ) 2 ( nˆ) = ρ 2 Rρ χ line of sight γ from π 0 decays Large uncertainties in the Particle spectrum Halo model Background estimation γ lines Clumpy halo increase rate! E. do Couto e Silva 26 N-body simulations from Calcáneo-Roldan and Moore, Phys. Rev. D62 (2000)

27 Halo Dark Matter Searches with GLAST Wimp Annihilations in halo Clumps (b > 10 deg): gamma continuum from ~100 MeV lines (2 γ, γζ) Depends on models of clumps» see previous slides IC from secondary electrons (Baltz & Wai 04) >GeV IC from e + starlight near galactic plane < 30 deg (trapping by B field) KK DM Scenario electron line (20% Br) smeared into a sharp edge via mainly IC >500 GeV: ~ 100e±/year edge height (Baltz & Hooper 05) all-sky signature! E. do Couto e Silva 27

28 SUSY or Extra Dimensions? Neutralinos (SUSY) are not the only viable solution for Dark Matter Extra Dimension Theories can also provide candidates with signatures in GLAST E. do Couto e Silva 28

29 Extra Dimensions: Possible GLAST Signatures? Large Extra Dimensions Thermal graviton emission (how much energy went into the bulk without affecting cosmological evolution?) (Perez- Lorenzana 2005) BBN (Hannestad 2004) For n=2 there would be many KK Modes which would release too much energy into gravitons Gravitons emitted by stellar objects take away energy SN (Hannestad 2003) NS shines because gravitons are gravitationally trapped Massive Graviton decays into γγ continuously emitted by the Universe (less robust) Excess in diffuse gamma ray emission around 30 MeV Gamma ray emission from NS in the galactic bulge Problem: heavy KK can decay into more lighter KK modes not on SM particles only Universal Extra Dimensions B 1 B 1 annihilation in Galactic Center Two photons via loop diagrams B 1 B 1 annihilation in Galactic Center Charged lepton production is not helicity suppressed 59% charged leptons 35% quarks 4% neutrinos 1% charged gauge bosons 0.5 % neutral gauge bosons 0.5 % Higgs bosons Primary gamma rays Bremstrahlung of charged leptons Secondary gamma rays Photons from qq and synchroton High Energy Signal (hundreds of GeV) Limited statistics and maybe E/E Low Energy Signal ( < 100 MeV) Uncertainties in the background Can theorists give us a signal between 10 and 100 GeV? LZP (Agashe and Servant hep-ph ) E. do Couto e Silva 29

30 GLAST MISSION GLAST MISSION OPERATIONS ELEMENTS ELEMENTS GPS µsec Large Area Telescope & GBM GLAST Spacecraft Telemetry 1 kbps - DELTA 7920H - GN - S TDRSS SN S & Ku LAT Instrument Science Operations Center White Sands Mission Operations Center (MOC) GLAST Science Support Center Archive HEASARC GSFC GRB Coordinates Network Alerts Schedules GBM Instrument Operations Center Data, Command Loads E. do Couto e Silva 30

31 Operation Phases First year of science operations initial on-orbit checkout, verification, and calibrations, followed by an allsky survey detailed instrument characterization refinement of the alignment key projects needed by the community source catalog, diffuse background models, etc. Transients data on transients will be released, with caveats. repoints for bright bursts and burst alerts enabled. First Year Guest Observer Program limited first-year guest observer program extraordinary Targets of Opportunities supported. workshops for guest observers on science tools and mission characteristics for proposal preparation Observing plan in subsequent years driven by guest observer proposal selections by peer review. All data released through the GLAST Science Support Center (GSSC). E. do Couto e Silva 31

32 The Look Ahead The GLAST mission is completing the fabrication phase and is well into integration. LAT, GBM, and spacecraft assembly complete by early Delivery of the LAT and GBM instruments for observatory integration in spring Observatory integration and test spring 2006 through summer CY07. Major scientific conference, the First GLAST Symposium, being planned for early Fabrication Instrument & Spacecraft I&T Observatory I&T Launch E. do Couto e Silva 32

33 GLAST LAT Project GLAST E. do Couto e Silva SSI Jul 29, 2005 August 2007 launch 33

34 Back up slides E. do Couto e Silva 34

35 Burst Handling Upon detection of a GRB, GLAST can take two DIFFERENT kinds of actions: alerts to the ground GBM and LAT issue alerts independently autonomous repoint to follow burst both GBM and LAT can generate a repoint request GBM will probably detect more bursts than LAT. However, if LAT detects a burst, it will probably provide a better localization of the burst position; therefore, GBM repoint request routed through LAT, which either passes on the GBM request or sends LAT s position. alerts will happen more frequently than repoint requests E. do Couto e Silva 35

36 LAT Performance (1) From LAT Science Requirements Document (SRD) Energy Resolution on-axis 100 MeV SRD: < 10%, current: 9% 10 GeV SRD: < 10%, current: 8% GeV SRD: < 20%, current: <15% Energy Resolution off-axis GeV SRD: < 6%, current: <5% Point Spread Function on-axis 68% 100 MeV SRD: < 3.5 0, current: (F), (T) 68% 10 GeV SRD: < , current: (F), (T) Point Spread Function ratios 95% to 68% containment SRD: < 3, current: 2.1(F), 2.6(B) 55 0 to normal incidence SRD: < 1.7, current: 1.6 GRB localization SRD: < 10 arcmin, 5 arcmin (ignoring BACK information) Peak Effective Area ( 1 GeV < E < 10 GeV) SRD: > 8000 cm 2, current: cm 10GeV Background Rejection (E > 100 MeV) SRD: < 10% diffuse, current: 6% diffuse (adjustable) E. do Couto e Silva 36

37 LAT Performance (2) Source Location Determination SRD: < 0.5 arcmin, <0.4 arcmin (ignoring BACK information) Field of View SRD: > 2 sr, current: 2.4 sr Rosat or Einstein X-ray source EGRET 95% 5σ LAT source r = 7 3EG r = 0.3 LAT 95% E. do Couto e Silva 37

38 LAT Performance (3) Point Source Sensitivity SRD: < cm -2 s -1, current: cm -2 s -1 Assumptions 5σ high latitude source, 1 yr (livetime) all sky survey Φ(>100MeV) = cm -2 s -1 sr -1, Energy spectrum ~ 1/E 2.1 Sensitivity for E > E 0 Assumptions 5σ, 1/E 2 spectrum at high latitude E. do Couto e Silva 38 Nucl. Phys. B85(2000)

39 LAT Performance (4) LAT has 5 times better angular resolution than 2 GeV and it improves at higher energies E. do Couto e Silva 39

40 Beam Test Results Data from beam tests on Engineering Models were used to Validate MC technology choices Develop and validate MC tools Correlation method Raw Beam Test Data 20 GeV e+ on-axis Profile fitting Containment Space Angle (deg) 10 1 Monte Carlo Beam Test Data GLAST Photons on Data axis 68% Containment 95% Containment (errors are 2σ) 0.1 E. do Couto e Silva Energy (MeV)

41 The Central Engine is a Messy Place! Radiative processes contribute in different ways to the spectral energy density Adapted from P. Coppi Small angle It is also a function of viewing angle Large angle What is happening here? E. do Couto e Silva 41

42 Dark Matter Detection with GLAST Not too many photons GLAST sensitivity curve There is no obvious choice for the model! Each point corresponds to one possible model All models assume the same Dark Matter distribution in the halo E. do Couto e Silva 42 With 2 years of data is harder for GLAST to detect neutralinos if the model is below the curve Bergström, Ullio & Buckley, 97

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