Calibration of the AGILE Gamma Ray Imaging Detector
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1 Calibration of the AGILE Gamma Ray Imaging Detector Andrew Chen on behalf of the AGILE Team April 11, 2011
2 AGILE Astrorivelatore Gamma ad Immagini LEggero Italian Space Agency (ASI) small mission Participation from INAF, INFN, Italian univerities, industrial partners Launched April 23, 2007 from Sriharikota, India
3 AGILE Gamma-ray Imaging Detector (GRID): 30 MeV - 50 GeV X-ray detector (Super-AGILE): kev Mini-calorimeter (MCAL): 300 kev MeV
4 AGILE-GRID Pair-production telescope Tungsten-Silicon Tracker: 12 planes, 0.8X cm 3
5 On-board Trigger Combination of hardware (Level-1) and software (Level 2) Simulations in GEANT v3.21 Validated with cosmic-ray muons at Tortona and beam tests at INFN-Frascati
6 Event reconstruction - Kalman filter Simplified on-board Kalman filter to reject albedo photons Retains 85-95% On-ground analysis using complete Kalman filter Provides reconstructed energy and photon incidence direction Unreconstructable events are rejected
7 Background rejection filters Detailed analysis of event morphology to distinguish photons from charged particles Events classified as gamma-rays (G), uncertain (L), particles (P) or single-track (S) All analysis except pulsar timing use G exclusively
8 Monte Carlo Simulations Series of runs with events each over a radius of cm Spectral index -1.7, energies ranging from 4 MeV to 50 GeV Each run contains a parallel plane of photons from a different incidence direction Off-axis angle = 1,30,35,40,45,50,60 Roll angle 0, 45
9 Effective area theta = 0 FMG FT3abG F4G Effective Area (cm^2) Energy (MeV) Figure: geometric area fraction of surviving events classified as G
10 Effective area theta = 40 FMG FT3abG F4G Effective Area (cm^2) Energy (MeV) Figure: geometric area fraction of surviving events classified as G
11 Energy Dispersion MeV 0.4 Fraction in energy channel true energy (MeV)
12 Energy Dispersion MeV 0.4 Fraction in energy channel true energy (MeV)
13 Energy Dispersion MeV 0.4 Fraction in energy channel true energy (MeV)
14 Energy Dispersion MeV 0.4 Fraction in energy channel true energy (MeV)
15 Energy Dispersion MeV 0.4 Fraction in energy channel true energy (MeV)
16 Energy Dispersion MeV 0.4 Fraction in energy channel true energy (MeV)
17 Energy Dispersion MeV 0.4 Fraction in energy channel true energy (MeV)
18 Energy Dispersion MeV 0.4 Fraction in energy channel true energy (MeV)
19 Energy Dispersion MeV 0.4 Fraction in energy channel true energy (MeV)
20 Energy Dispersion MeV 0.4 Fraction in energy channel true energy (MeV)
21 Energy Dispersion MeV 0.4 Fraction in energy channel true energy (MeV)
22 Energy Dispersion MeV 0.4 Fraction in energy channel true energy (MeV)
23 Energy Dispersion MeV 0.4 Fraction in energy channel true energy (MeV)
24 Energy Dispersion MeV 0.4 Fraction in energy channel true energy (MeV)
25 Energy Dispersion MeV 0.4 Fraction in energy channel true energy (MeV)
26 Energy Dispersion MeV 0.4 Fraction in energy channel true energy (MeV)
27 Point spread dispersion /Users/andrew/work/testBUILD20/testfit/testfitpsf2_100_30_0 psf Entries χ 2 / ndf / 196 Prob 1 p ± 10.9 p ± p ± rho (deg)
28 Point spread dispersion /Users/andrew/work/testBUILD20/testfit/testfitpsf2_400_30_0 psf Entries 0 χ 2 / ndf / Prob 1 p0 280 ± 26.5 p ± p ± rho (deg)
29 Point spread dispersion /Users/andrew/work/testBUILD20/testfit/testfitpsf2_1000_30_0 psf Entries 0 χ 2 / ndf 13.5 / Prob 1 p ± 38.7 p ± p ± rho (deg)
30 Physical sources - Effective area Physical sources are modeled as a sum of monoenergetic sources P i In principle, A eff = A(E i )w(e i ) Pi w(e i ) where w(e i ) = (E α i+1 E α i ) j EDP(E i, E j ) and all quantitites are a function of incidence angle in instrument coordinates, event type (G) and filter (FM) In practice, this quantity was too sensitive to small changes in the spectral index due to contributions from low energy photons, where the effective area is poorly calibrated. Therefore, we use w(e i ) = f (E i )(E α i+1 E α i ) where f (E i ) is determined post-hoc
31 Physical sources - Point spread dispersion PSD = P i PSD(E i )w(e i ) Pi w(e i ) where w(e i ) = (E α i+1 E α i ) j A eff (E i )EDP(E i, E j ) and all quantitites are a function of incidence angle in instrument coordinates, event type (G) and filter (FM) The current version (I0007/I0010) of the PSD files uses histograms taken directly from the Monte Carlo simulations. New PSD files (I0023/I0024) are in preparation which contain values derived from a fit to the Monte Carlo data using a three parameter King function: f (ρ)dω = N(1 1/γ)(1 + (ρ/δ)2 ) 2γ )dω
32 In-flight Calibration Procedure Long-term integrations of AGILE in-flight data in both pointing (2007/07/ /10/15) and spinning (2009/11/ /10/31) modes of the Vela and anti-center regions, generating counts and exposure maps with a bin size of 0.3 Maximum likelihood analysis taking into account Galactic diffuse emission and isotropic background Point sources: Vela pulsar in the Vela region, Crab and Geminga pulsars and IC443 in the anti-center region Analysis performed with fixed position and fixed, power-law spectra Model counts compared to data to validate point spread function Spectra and fluxes compared to those published in the Fermi Catalog in order to determine the post-hoc scaling factors for the effective area
33 Energy-dependent effective area scaling factors 10-6 theta = df/de (cm^-2 s^-1 MeV^-1) E (MeV) Figure: We introduce energy-dependent scaling factors into the sensitive area response function to correct for the underestimate of the flux and spectra. (I0023 I0024)
34 Energy-dependent effective area scaling factors 10-6 I0024 theta = df/de (cm^-2 s^-1 MeV^-1) E (MeV) Figure: We introduce energy-dependent scaling factors into the sensitive area response function to correct for the underestimate of the flux and spectra. (I0023 I0024)
35 Point spread function, Vela, E > 100 MeV MeV < E < 50 GeV, theta = e l (deg) Figure: A 10 slice centered on Vela. The data are well-fit by the point-spread function assuming a spectral index of -1.66, weighted by effective area, spectrum, and energy dispersion.
36 Point spread function, Vela, E > 100 MeV MeV < E < 50 GeV, theta = e b (deg) Figure: A 10 slice centered on Vela. The data are well-fit by the point-spread function assuming a spectral index of -1.66, weighted by effective area, spectrum, and energy dispersion.
37 Point spread function, Vela, E > 400 MeV MeV < E < 50 GeV, theta = e l (deg) Figure: A 10 slice centered on Vela. The data are well-fit by the point-spread function assuming a spectral index of -1.66, weighted by effective area, spectrum, and energy dispersion.
38 Point spread function, Vela, E > 400 MeV MeV < E < 50 GeV, theta = e b (deg) Figure: A 10 slice centered on Vela. The data are well-fit by the point-spread function assuming a spectral index of -1.66, weighted by effective area, spectrum, and energy dispersion.
39 Single energy vs. composite PSF Energy (MeV) 68% C.R Table: 68% Containment radius, off-axis angle = 30, single energy Energy Range 68% C.R. 100 MeV - 50 GeV MeV - 50 GeV MeV - 50 GeV 0.8 Table: 68% Containment radius, off-axis angle = 30, α = 1.66
40 Work in progress Validate Crab flux and spectra, other sources Understand post-hoc scaling factors Allow AGILE-GRID scientific analysis below 100 MeV Re-evaluate EDP-dependent effective area calculation
41 Cross-calibration with Fermi - in preparation AGILE-GRID sensitivity is highest around 100 MeV, decreases rapidly above 10 GeV Fermi-LAT effective area is highest above 1 GeV, decreases rapidly below 200 MeV Use Fermi-LAT catalog data to determine how source flux below 200 MeV can change AGILE sensitivity for a give Fermi flux and spectrum In collaboration with Fermi, use simultaneous data to determine how energy dispersion, energy dependence of effective area, and off-axis exposure influence Fermi and AGILE sensitivity
42 AGILE & Fermi, 1-day exposure AGILE-GRID AGILE-GRID Fermi-LAT (pointing) (spinning) (front) FOV (sr) Rate of drift 1 /day 1 /sec 4 /min Sky coverage 1/5 70% whole sky Source livetime fraction 1-day exposure (10 7 cm 2 s) 30 off-axis, 100 MeV
43 Fermi vs. AGILE pointing Figure: Top: off-axis angle vs. time; Bottom: histogram of off-axis angle. AGILE = red, Fermi = blue
44 Fermi vs. AGILE spinning Figure: Top: off-axis angle vs. time; Bottom: histogram of off-axis angle. AGILE = red, Fermi = blue
45 Conclusion In-flight data confirm modeling of point spread function Extreme sensitivity to source spectrum due to large energy dispersion Post-hoc scaling factors compensate for lack of energy dispersion term in effective area calculation More pronounced at lower and higher energies Necessary first step in cross-calibration with Fermi-LAT Many avenues to resolve apparent discrepancies
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