The Diffuse Gamma‐Ray Background from Supernovae

Watanabe, K.; Hartmann, D. H.; Leising, M. D.

doi:10.1086/307110

Cited by 64 publications

(85 citation statements)

References 62 publications

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“…Our results are comparable to those of previous studies. Although early studies showed large contributions from SNe Ia (Clayton & Silk 1969;Clayton & Ward 1975;The et al 1993;Zdziarski 1996;Watanabe et al 1999;Ruiz-Lapuente et al 2001), later studies report contributions to be ∼10 (Strigari et al 2005) and 10 ) less than the measured intensity. If the dominant fraction of the CGB could be subtracted by future detectors, the SN Ia contribution could be detected.…”

Section: Contribution To the Cosmic Gamma-ray Backgroundmentioning

confidence: 82%

REVEALING TYPE Ia SUPERNOVA PHYSICS WITH COSMIC RATES AND NUCLEAR GAMMA RAYS

Horiuchi¹,

Beacom²

2010

ApJ

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Type Ia supernovae (SNe Ia) remain mysterious despite their central importance in cosmology and their rapidly increasing discovery rate. The progenitors of SNe Ia can be probed by the delay time between progenitor birth and explosion as SNe Ia. The explosions and progenitors of SNe Ia can be probed by MeV nuclear gamma rays emitted in the decays of radioactive nickel and cobalt into iron. We compare the cosmic star formation and SN Ia rates, finding that their different redshift evolution requires a large fraction of SNe Ia to have large delay times. A delay-time distribution of the form t −α with α = 1.0 ± 0.3 provides a good fit, implying that 50% of SNe Ia explode more than ∼1 Gyr after progenitor birth. The extrapolation of the cosmic SN Ia rate to z = 0 agrees with the rate we deduce from catalogs of local SNe Ia. We investigate prospects for gamma-ray telescopes to exploit the facts that escaping gamma rays directly reveal the power source of SNe Ia and uniquely provide tomography of the expanding ejecta. We find large improvements relative to earlier studies by Gehrels et al. in 1987 andWoosley in 1997 due to larger and more certain SN Ia rates and advances in gamma-ray detectors. The proposed Advanced Compton Telescope, with a narrow-line sensitivity ∼60 times better than that of current satellites, would, on an annual basis, detect up to ∼100 SNe Ia (3σ ) and provide revolutionary model discrimination for SNe Ia within 20 Mpc, with gamma-ray light curves measured with ∼10σ significance daily for ∼100 days. Even more modest improvements in detector sensitivity would open a new and invaluable astronomy with frequent SN Ia gamma-ray detections.

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Section: Contribution To the Cosmic Gamma-ray Backgroundmentioning

confidence: 82%

REVEALING TYPE Ia SUPERNOVA PHYSICS WITH COSMIC RATES AND NUCLEAR GAMMA RAYS

Horiuchi¹,

Beacom²

2010

ApJ

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“…1). As discussed by several authors [5,6,7], type Ia supernovae could make a significant contribution in this energy range, which we shall evaluate in Section 2.…”

Section: Introductionmentioning

confidence: 93%

Soft gamma-ray background and light dark matter annihilation

et al. 2006

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The bulk of the extragalactic background between 10 keV and 10 GeV is likely to be explained by the emission of Seyfert galaxies, type Ia supernovae, and blazars. However, as revealed by the INTEGRAL satellite, the bulge of our galaxy is an intense source of a 511 keV gamma-ray line, indicating the production of a large number of positrons that annihilate. The origin of the latter is debated, and they could be produced, in particular, by the (S-or P -wave) annihilation of light Dark Matter particles into e + e − . In any case, the cumulated effect of similar sources at all redshifts could lead to a new background of hard X-ray and soft gamma-ray photons. On the basis of the hierarchical model of galaxy formation, we compute analytically the SNIa contribution to the background, and add it to Seyfert and blazars emission models. Confronting these expected contributions to observation, we find that any extra contribution to this unresolved background around 511 keV should be lower than about 4 keV cm −2 s −1 sr −1 . We also estimate analytically the extragalactic background due to Dark Matter annihilation, increasing the accuracy of the earlier computations. Indeed, we take into account the large positron escape fraction from low mass dark matter halos, unable to confine a dense and magnetized interstellar medium. Our new background estimate turns out to be one order of magnitude lower so that the hypothesis of a light Dark Matter candidate remains compatible with the observed extragalactic background for a wider range of particle masses and cross-sections.PACS numbers: 95.35.+d, 95.85.Nv, 95.85.Pw, 97.60.Bw

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“…In the GeV regime the MRF seems to originate from unresolved blazars and galaxies. Gamma rays emitted by novae, supernovae, and γ-ray bursts contribute the bulk of the observed background in the window around 1 MeV (e.g., Watanabe et al 1999;Weidenspointner 1999;Ruiz-Lapuente et al 2000). In principle, the evolution of the MRF should be predictable with structure formation models (e.g., Sommerville & Primack 1999), so that the observed MRF could be used to infer either the role of AGNs, low surface brightness objects, decays of relic particles, or to single out cosmological parameters.…”

Section: Introductionmentioning

confidence: 99%

Implications of cosmological gamma-ray absorption

Kneiske

Mannheim

Hartmann

2002

A&A

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154

222

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Abstract. Gamma-ray absorption due to γγ-pair creation on cosmological scales depends on the line-of-sight integral of the evolving density of low-energy photons in the Universe, i.e. on the history of the diffuse, isotropic radiation field. Here we present and discuss a semi-empirical model for this metagalactic radiation field based on stellar light produced and reprocessed in evolving galaxies. With a minimum of parameters and assumptions, the present-day background intensity is obtained from the far-IR to the ultraviolet band. Predicted model intensities are independent of cosmological parameters, since we require that the comoving emissivity, as a function of redshift, agrees with observed values obtained from deep galaxy surveys. The far-infrared background at present predicted from optical galaxy surveys falls short in explaining the observed one, and we show that this deficit can be removed by taking into account (ultra)luminous infrared galaxies with a seperate star formation rate. The accuracy and reliability of the model, out to redshifts of z ∼ 5, allow a realistic estimate of the attenuation length of GeV-to-TeV gamma-rays and its uncertainty, which will be the focus of a subsequent paper.

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The Diffuse Gamma‐Ray Background from Supernovae

Cited by 64 publications

References 62 publications

REVEALING TYPE Ia SUPERNOVA PHYSICS WITH COSMIC RATES AND NUCLEAR GAMMA RAYS

REVEALING TYPE Ia SUPERNOVA PHYSICS WITH COSMIC RATES AND NUCLEAR GAMMA RAYS

Soft gamma-ray background and light dark matter annihilation

Implications of cosmological gamma-ray absorption

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