Implications of cosmological gamma-ray absorption - II. Modification of gamma-ray spectra

By Tanja M. Kneiske, T. Bretz, K. Mannheim, D. Hartmann. 2003

347 citations recorded by the source corpus.

Bearing on the model for the time-dependent metagalactic radiation field developed in the first paper of this series, we compute the gamma-ray attenuation due to pair production in photon-photon scattering. Emphasis is on the effects of varying the star formation rate and the fraction of UV radiation assumed to escape from the star forming regions, the latter being important mainly for high-redshift sources. Conversely, we investigate how the metagalactic radiation field can be measured from the gamma-ray pair creation cutoff as a function of redshift, the Fazio-Stecker relation. For three observed TeV-blazars (Mkn501, Mkn421, H1426+428) we study the effects of gamma-ray attenuation on their spectra in detail.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/215f21c17a978196c8de7d30b8b18e199f73d393

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Citations in the corpus

BLAZARS AS ULTRA-HIGH-ENERGY COSMIC-RAY SOURCES: IMPLICATIONS FOR TeV GAMMA-RAY OBSERVATIONS (2011, methodology): “…“E20, low IR" and “E19, low IR" are the cascade spectra initiated bythe E−2 injection with Emaxp = 10 20 eV and 1019 eV protons, respectively, using the low-IR EBL model (Kneiske et al. 2004), whereas the curve labeled “E19, best fit" is the spectrum withEmaxp = 10 19 eV for the best-fit EBL model.”
Electron-positron pairs in physics and astrophysics: from heavy nuclei to black holes (2009, methodology): “This calculation was applied to further study of the optical depth of the Universe to high-energy γ-rays [291, 292, 293].”
Intergalactic Photon Spectra from the Far-IR to the UV Lyman Limit for 0 < z < 6 and the Optical Depth of the Universe to High-Energy Gamma Rays (2005, methodology): “The favored “best-fit” model of Kneiske et al. (2004) gives an optical depth τ = 1 at Eγ ≃ 5 TeV for z = 0.03, the redshift of the blazars Mrk 421 and Mrk 501.”
THE LARGE AREA TELESCOPE ON THE FERMI GAMMA-RAY SPACE TELESCOPE MISSION (2009, methodology): “According to current EBL models (e.g., Primack et al. 1999; Stecker et al. 2006; Kneiske et al. 2004), absorption breaks in the LAT energy range are expected for sources located atz ≥ 0.5.”
Cosmogenic neutrinos: parameter space and detectabilty from PeV to ZeV (2010, background): “One can notice that Kneiske et al. (2004) find higher photon densities in the far infrared bump at large redshift compared to Stecker et al. (2006), and lower densities in the optical and UV range.”
The Astrophysics of Ultrahigh-Energy Cosmic Rays (2011, background): “…medium, cosmic rays primarily interact with the Cosmic Microwave Background (CMB) photons at the highest energies, and with infrared, optical, and ultraviolet background (IR-UV) photons at slightly lower energy (see, e.g., Kneiske et al. 2004; Stecker et al. 2006 for detailed background models).”
Extreme TeV blazars and the intergalactic magnetic field (2010, methodology): “We adopt the LowSFRmodel of Kneiske et al. (2004) which provides an optical depth similar to that of all the other updated models up to energies of 4–5 TeV.”
Semi-analytic modelling of the extragalactic background light and consequences for extragalactic gamma-ray spectra: Modelling of the EBL and gamma-ray spectra (2012, methodology): “A follow-up paper, Kneiske et al. (2004), expanded this earlier model into six realizations, varying in gas temperature contribution, SFR and UV escape fraction.”
Variable Very High Energy γ-Ray Emission from Markarian 501 (2007, methodology): “4.2), EBL-de-absorbed using the ’Low’ model of Kneiske et al (2004).”
CONTRIBUTION OF GAMMA-RAY-LOUD RADIO GALAXIES’ CORE EMISSIONS TO THE COSMIC MeV AND GeV GAMMA-RAY BACKGROUND RADIATION (2011, background): “Here ω(Fγ [Lγ , z]) is the detection efficiency of Fermi at the photon flux Fγ , which corresponds to the flux from a source with a gamma-ray luminosity Lγ at redshift z. High-energy γ -rays ( 20 GeV) propagating through the universe are absorbed by the interaction with the extragalactic background ”
MODELING THE EXTRAGALACTIC BACKGROUND LIGHT FROM STARS AND DUST (2009, methodology): “In such models, one integrates over star formation rates and stellar properties (e.g. Salamon & Stecker 1998; Dwek et al. 1998; Kneiske et al. 2002, 2004).”
New limits on the density of the extragalactic background light in the optical to the far-infrared from the spectra of all known TeV blazars (2007, methodology): “Using the H 1426+428 spectrum, together with the spectra of previously detected TeV blazars, limits on the EBL were derived (Costamante et al. 2003; Kneiske et al. 2004).”