simulations of thermal grbs as observed by glast gbm+lat
DESCRIPTION
Simulations of Thermal GRBs as observed by GLAST GBM+LAT. Milan Battelino Stockholm Observatory DC2 Closeout Meeting 31 May - 2 June 2006. Outline. Background The Hybrid Model Simulation flow Results. a. b. GRB Standard Model. Band, D. et al.:1993 ApJ 413 , 281. - PowerPoint PPT PresentationTRANSCRIPT
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Simulations of Thermal GRBs as observed by
GLAST GBM+LAT
Milan BattelinoStockholm Observatory
DC2 Closeout Meeting 31 May - 2 June 2006
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Outline
•Background•The Hybrid Model•Simulation flow•Results
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GRB Standard Model
Excellent fit for majority of GRB spectra in BATSE energy window
Band, D. et al.:1993 ApJ 413, 281
, , Ec , Aband
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Optically Thin Synchrotron Spectrum
Low energiesSelf absorption
÷2
High energiesCut off
Observed region
FC: s = -1.5
SC: s = -1.6s = -2.1s = -2/3
BATSE
Fermi-shock-accelerated
e– distribution: p ~ 2.2
-pNe
log
Characteristic synchrotron frequency Cooling frequency
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Line of Death
Hard to explain with optically thin synchrotronmodel!
Crider et al: 1997, ApJ 479, L39+Preece et al: 1998, ApJ 506, L23
Time-resolved spectra from 57 bright BATSE burstsA substantial fraction of the time-resolved spectrafrom bright BATSE burstsshow hard sub-peakspectra!
-2/3
This has to be considered when implementing a model.
Also high energy componentsin the MeV – GeV band...
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Other Models...Review paper by GRB Group, 2006
• Synchrotron and Inverse Compton– Electron IC Scattering– Synchrotron Self-Compton– Proton Synchrotron Emission– Thermal Components + Synchrotron
• Pion production and cascades – Hadronic Cascades– Neutron-proton decoupling
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Hybrid ModelRyde, F: 2004, ApJ 614, 827
Wien spectrum : = 2 Planck spectrum : = 1
Blackbody + Powerlaw kT, AkT, s, Apow
GRB 911016
Bose-Einstein function+ Powerlaw(s)
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LOD not a problem with
-2/3
LOD not a problem in Hybrid Model
-1.6
...also: a peak at s = -1.6, close to s = -1.5
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How to simulate Hybrid Model?
• Model independent simulator software (C++) producing photon histogram files
• Extend gtobssim software (C++):– New celestialSource class:
GRBtemplateManager (by Nicola Omodei) that reads photon histogram files
• Extend GBM Tools package (IDL):– Read photon histogram files
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Simple Burst Modeler
Model
N(E,t)
ComponentList
1
ParameterList
1
Parameter
P(t)
1..n
PlotDevice1
Hybrid
Blackbody Powerlaw
Lightcurve Breakpoint
Component
C(E,t)
1..n1
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Hybrid Model Parameters
Blackbody Component• Lightcurve (Flux)• Temperature (kT)• Normalization
Powerlaw Component• Lightcurve (Flux) • Spectral index/indices• Breakpoints• Normalization
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Hybrid Model Simulation
Blackbody component
Broken power-law : synchrotron emission spectrum
GRB 911016
BATSE window
~ 3 GeV based on results byde Jager et al, 1996, ApJ 457, 253
High energy cut-off
Competition between the acceleration (heating) of the electrons and the radiativecooling leads to a maximal energy that the electrons can be accelerated to.
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File Header
GRBtemplateManagerNicola Omodei
• Photon Histogram:
• Number of energy bins (columns):
• Min Energy:
• Max Energy:
• Number of time bins (rows):
• Timebinwidth:
• Energy binning:
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GBM Tools extensions
• GRBtemplate photon histogram file – populate energy bins from LAT photon
histogram file with internal energy binning defined by energy grid
• Energy grid photon histogram file1. GBM Simulator reads definition file,
determines energy grids for NaI and BGO detectors and saves energy grids as files
2. SBM reads energy grid files and produces histogram files
3. GBM Simulator reads SBM histogram files to produce, apportion photons and create TTE files.
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Model Parameter Values + guesses
LAT lightcurve histogram file
GLAST Definition file
XSPEC
BATSE Trigger Data
1
LAT FITS and response files
gtobssimgtselectgtrspgen
3
SBM2
gtbin4
GBM Simulator
NaI/BGO Energy Grid
5
Separate NaI and BGO lightcurve histogram files
6
GBM Simulator 7
NaI/BGO TTE, background and response files
8
XSPEC 9
Simulation Flow
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NaI #2 + NaI #9 + BGO #1 + LAT
= 27.1o, = 95.3o
s1 = -1.30 +/- 0.04
s2 = -1.71 +/- 0.02
2= 0.9
Resolution : 1 x 5.0 s
Joint Spectral AnalysisGRB 911016
s2 = -1.7
s1 = -1.3
SBM input XSPEC Model
Blackbody+
(Broken Powerlawx
High Energy Cutoff)
XSPEC Result
s1 = -1.33 +/- 0.02
s2 = -1.81 +/- 0.08
Resolution : 5 x 1.0 s
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GRB 941026Time integrated: 0.0 - 5.0 s
S1 = -1.6
S2 = -2.1
SBM Input
S1 = -1.7 +/- 0.03
S2 = -2.1 +/- 0.2
XSPEC Result
ÿ2÷= 0.78
= 27.1o, = 95.3o
NaI #2 + NaI #9 + BGO #1 + LAT
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Conclusion
• Hard to determine high energy cutoff in time-resolved spectra above 3 GeV
• Blackbody component easily detected if it is the cause of spectral hardness
• Position of powerlaw breakpoint hard to determine when strong blackbody component
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The End
Thanks to: Nicola Omodei, Valerie Connaughton and Felix Ryde