Galactic Diffuse Gamma-Ray Emission GLAST Japan Workshop November 24-25, 2006 Tuneyoshi KAMAE (SLAC/KIPAC, Stanford University) 1. Introduction: • Status of EGRET g -ray diffuse emission mdeling • What Integral see in hard X-ray band • Diffuse emission seen in the X-ray band 2. New anaysis technologies for GLAST era we are working on • Correct p-p int. modeling for secondary particles (pub and to be pub) • Correct analysis of low-energy EGRET diffuse emission (to be pub) • 3D ISM distr. by Nakanishi and Sofue for H2 and HI (pub and to be pub) • Modeling of non-Fermi acceleration senario (in progress) 3. Preliminary results • Possible new interpretation of EGRET g -ray diffuse emission (in progress) • Clarification of “unidentified sources”: Suzaku, Nanten, GLAST, NuStar
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Galactic Diffuse Gamma-Ray EmissionGLAST Japan Workshop
November 24-25, 2006
Tuneyoshi KAMAE (SLAC/KIPAC, Stanford University)
1. Introduction:• Status of EGRET γ-ray diffuse emission mdeling• What Integral see in hard X-ray band• Diffuse emission seen in the X-ray band
2. New anaysis technologies for GLAST era we are working on• Correct p-p int. modeling for secondary particles (pub and to be pub)• Correct analysis of low-energy EGRET diffuse emission (to be pub) • 3D ISM distr. by Nakanishi and Sofue for H2 and HI (pub and to be pub)• Modeling of non-Fermi acceleration senario (in progress)
3. Preliminary results• Possible new interpretation of EGRET γ-ray diffuse emission (in progress)• Clarification of “unidentified sources”: Suzaku, Nanten, GLAST, NuStar
Cosmic Ray Propagation and Interaction- Interplay among sources(SNRs), propagation, targets(H2,HI, ISRF) -
From Strong and Moskalenko
GALPROP: γ-Ray Spectrum- A parameter set to explain EGRET γ-ray spectrum -
IC: uncertainty in •e−/e+
•ISRF
e−/e+: •2-3 time the local flux•spectral shape adjusted
π0: proton flux•~2 times higher than LIS
GALPROP: Longitude Distribution- Optimized to explain EGRET γ-ray map -
30-50MeV 50-70MeV 70-100MeV
100-150MeV 150-300MeV 500-1000MeV
Glon distribution for |Glat|<5.5 deg Look all similar: tracer for H2 and HI?
GALPROP: Latitude Distribution- Optimized to explain EGRET γ-ray map -
30-50MeV 50-70MeV 70-100MeV
100-150MeV 150-300MeV 500-1000MeV
Glat distribution for |Glon|<30.5 deg Look all similar: tracer for H2 and HI?
Observation in Hard X-ray Band- Ginga, ASCA, Integral, Suzaku -
Exposure map of Integral Has not survey the entire ridge
Observation in Hard X-ray Band- Integral -
Enhancement in |Glon|<10 deg
Deconvolution of EGRET’s PSF- Why essential -
True directionof γ-ray
Reconstructed direction of γ-ray
Angular dependence of “exposure” (~FOV)
True exposure
Assumed exposure
EGRET PSF for E<150MeV
EGRET FOV
High latitude flux is systematically over estimated by up to 20-30%
Need sharper image for detailed analyses
Kamae, in prep
Deconvolution of EGRET PSF- PSF Representation on Glon-Glat Map is Glat-dependent -
Index2.2 at Glat=0.0
Index2.2 at Glat=+/-22.0 Index2.2 at Glat=+/-26.0
Angular Response Matrix Based on EgretPsf- Building 3600x3600 Matrix for E0-E9-
Deconvolution of EGRET’s PSF- Ideal and Poisson noise dominated cases -
True Latitude Distribution in Low Energy- PSF deconvolved maps –