A New Determination of the Extragalactic Diffuse Gamma-Ray Background from EGRET Data

By A. Strong, I. V. Moskalenko, O. Reimer. 2004

279 citations recorded by the source corpus.

We use the GALPROP model for cosmic-ray propagation to obtain a new estimate of the Galactic component of γ-rays and show that away from the Galactic plane it gives an accurate prediction of the observed EGRET intensities in the energy range 30 MeV to 50 GeV. On this basis we reevaluate the extragalactic γ-ray background. We find that for some energies previous work underestimated the Galactic contribution at high latitudes and hence overestimated the background. Our new background spectrum shows a positive curvature similar to that expected for models of the extragalactic emission based on the blazar population.

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/4a838984dec4f04dc320969a3786b90a59d56c13

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In Nuclear and High Energy Physics

1. A. Strong
2. E. Orlando
3. Anna Franckowiak
4. Y. Inoue
5. E. Quataert
6. Troy A. Porter
7. T. Thompson
8. I. Grenier

Citations in the corpus

• The Starburst Contribution to the Extragalactic γ-Ray Background (2006, background): “The magnitude of the extragalactic -ray background is uncertain, primarily due to the presence of foreground contaminants (cf. Keshet et al. 2004; Strong et al. 2004; Sreekumar et al. 1998).”
• CONTRIBUTION OF GAMMA-RAY-LOUD RADIO GALAXIES’ CORE EMISSIONS TO THE COSMIC MeV AND GeV GAMMA-RAY BACKGROUND RADIATION (2011, background): “Energetic Gamma-Ray Experiment Telescope (EGRET) on board the CGRO confirmed the EGRB spectrum at 0.03–50 GeV (Sreekumar et al. 1998; Strong et al. 2004).”
• THE FERMI-LAT HIGH-LATITUDE SURVEY: SOURCE COUNT DISTRIBUTIONS AND THE ORIGIN OF THE EXTRAGALACTIC DIFFUSE BACKGROUND (2010, unknown): “2 mission (Fichtel et al. 1975) and its spectrum was measured with good accuracy by the Energetic Gamma Ray Experiment Telescope (EGRET Sreekumar et al. 1998; Strong et al. 2004) on board the Compton Observatory.”
• THE LARGE AREA TELESCOPE ON THE FERMI GAMMA-RAY SPACE TELESCOPE MISSION (2009, background): “This re-analysis (Strong et al. 2004b) gives a new estimate of the EGRB that is lower in flux and steeper than found by Sreekumar et al. (1998) and is not consistent with a power-law.”
• THE COSMOLOGICAL IMPACT OF LUMINOUS TeV BLAZARS. I. IMPLICATIONS OF PLASMA INSTABILITIES FOR THE INTERGALACTIC MAGNETIC FIELD AND EXTRAGALACTIC GAMMA-RAY BACKGROUND (2011, methodology): “The most recentFermi estimate of the EGRB is a featureless power-law, somewhat softer than that foundby EGRET, and does not exhibit the localized high-energy excess claimed by a reanalysis of the EGRET data (Strong et al. 2004).”
• Constraints on cosmological dark matter annihilation from the Fermi-LAT isotropic diffuse gamma-ray measurement (2010, methodology): “It explores the gamma-ray sky in the 20 MeV to 300 GeV range and has an improved sensitivity by more than an order of magnitude, compared to its predecessor EGRET [6].”
• A Measurement of the Spatial Distribution of Diffuse TeV Gamma-Ray Emission from the Galactic Plane with Milagro (2008, methodology): “The injection spectrum is a broken power law with a spectral index of 1.5 below 20 GeVand a spectral index of 2.42 above 20 GeV, extending to a maximum electron energy of 1000 TeV, with an electron flux of 1:4 ; 10 9 MeV 1 cm 2 s 1 sr 1 at 34.5 GeV (Strong et al. 2004a, 2004b).”
• Inverse Compton Origin of the Hard X-Ray and Soft Gamma-Ray Emission from the Galactic Ridge (2008, methodology): “At higher energies, an extensive study of the diffuse Galactic γ-ray emission in the context of CR propagation models has been carried out by Strong et al. (2000, 2004b).”
• Cosmic X-Ray Background and Earth Albedo Spectra with Swift BAT (2008, methodology): “In addition to the work of Gruber et al. (1999) we show SMM (Solar Maximum Mission) (MeV) data (Watanabe et al. 1997), and COMPTEL andEGRETdata in a recent revision (Weidenspointner et al. 2000; Strong et al. 2004).”
• The Cosmic Infrared Background Resolved by Spitzer. Contributions of Mid-Infrared Galaxies to the Far-Infrared Background. (2006, background): “…EBL will not change this picture, since the contributions to the total EBL brightness of the radio, UV, X-ray (Mushotzky et al., 2000; Hasinger et al., 2001) and γ ray (Strong et al., 2004) extragalactic backgrounds are smaller by one to three orders of magnitude than the COB and CIB (Scott, 2000).”