Ground- and Space-Based Gamma-Ray Astronomy

Funk, S.

doi:10.1146/annurev-nucl-102014-022036

Cited by 94 publications

(76 citation statements)

References 207 publications

(158 reference statements)

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“…7. e-ASTROGAM sensitivity for 1-year exposure (thick purple line) compared to typical γ-ray energy spectra for several SNRs; young SNRs (<1000 years) are shown in green. High-energy data (E > 100 MeV) are taken from [60]; lowenergy data (related to RX J1713.7-3946) from [131].…”

Section: What Are the Cr Energy Distributions Produced Insidementioning

confidence: 99%

The e-ASTROGAM mission

et al. 2017

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e-ASTROGAM ('enhanced ASTROGAM') is a breakthrough Observatory space mission, with a detector composed by a Silicon tracker, a calorimeter, and an anticoincidence system, dedicated to the study of the non-thermal Universe in the photon energy range from 0.3 MeV to 3 GeV -the lower energy limit can be pushed to energies as low as 150 keV, albeit with rapidly degrading angular resolution, for the tracker, and to 30 keV for calorimetric detection. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with polarimetric capability. Thanks to its performance in the MeV-GeV domain, substantially improving its predecessors, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on the surroundings. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous generation instruments, e-ASTROGAM will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LIGO-Virgo-GEO600-KAGRA, SKA, ALMA, E-ELT, TMT, LSST, JWST, Athena, CTA, IceCube, KM3NeT, and the promise of eLISA.

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Section: What Are the Cr Energy Distributions Produced Insidementioning

confidence: 99%

The e-ASTROGAM mission

et al. 2017

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“…As indicated, the black dots are from the MAGIC telescopes while the blue squares were measured by the Fermi spacecraft. The cutoff at low energies is an indication of the kinematic threshold for pion production, while the break at high energies, if this emission is from pion-decay, indicates a break in the energy spectrum of hadrons produced by the SNR blast wave (see Funk 2015).…”

Section: Cosmic Ray Escape In Fermi Accelerationmentioning

confidence: 99%

“…The evidence for PeV CRs is less certain. All of the SNRs identified so far show breaks in their γ-ray spectra well below 100 TeV (e.g., Funk 2015). These remnants have been observed with the currently operating ground-based Cherenkov telescopes H.E.S.S, MAGIC and VERITAS.…”

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confidence: 92%

Cosmic Ray Production in Supernovae

et al. 2018

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We give a brief review of the origin and acceleration of cosmic rays (CRs), emphasizing the production of CRs at different stages of supernova evolution by the first-order Fermi shock acceleration mechanism. We suggest that supernovae with trans-relativistic outflows, despite being rather rare, may accelerate CRs to energies above 10 18 eV over the first year of their evolution. Supernovae in young compact clusters of massive stars, and interaction powered superluminous supernovae, may accelerate CRs well above the PeV regime. We discuss the acceleration of the bulk of the galactic CRs in isolated supernova remnants and re-acceleration of escaped CRs by the multiple shocks present in superbubbles produced by associations of OB stars. The effects of magnetic field amplification by CR driven instabilities, as well as superdiffusive CR transport, are discussed for nonthermal radiation produced by nonlinear shocks of all speeds including trans-relativistic ones.

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“…fig. 6 in Funk (2015) -for the case of our type II SNR. In this figure, we re-normalized arbitrarily the different spectra at different ages to roughly peak at the same value for visual purposes.…”

Section: Gamma-ray Spectra and Evolutionmentioning

confidence: 81%

Time evolution of gamma rays from supernova remnants

Gaggero

Zandanel

Cristofari

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present a systematic phenomenological study focused on the time evolution of the non-thermal radiation -from radio waves to gamma rays -emitted by typical supernova remnants via hadronic and leptonic mechanisms, for two classes of progenitors: thermonuclear and core-collapse.To this aim, we develop a numerical tool designed to model the evolution of the cosmic-ray spectrum inside a supernova remnant, and compute the associated multiwavelength emission. We demonstrate the potential of this tool in the context of future population studies based on large collection of high-energy gamma-ray data.We discuss and explore the relevant parameter space involved in the problem, and focus in particular on their impact on the maximum energy of accelerated particles, in order to study the effectiveness and duration of the PeVatron phase.We outline the crucial role of the ambient medium through which the shock propagates during the remnant evolution. In particular, we point out the role of dense clumps in creating a significant hardening in the hadronic gamma-ray spectrum.

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Ground- and Space-Based Gamma-Ray Astronomy

Cited by 94 publications

References 207 publications

The e-ASTROGAM mission

The e-ASTROGAM mission

Cosmic Ray Production in Supernovae

Time evolution of gamma rays from supernova remnants

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