Study of Nonthermal Emission from SNR RX J1713.7−3946 with<i>Suzaku</i>

Tanaka, Takaaki; Uchiyama, Y.; Aharonian, F.; Takahashi, Tadayuki; Bamba, Aya; Hiraga, Junko S.; Kataoka, J.; Kishishita, Tetsuichi; Kokubun, M.; Mori, Koji; Nakazawa, K.; Petre, Robert; Tajima, H.; Watanabe, Shin

doi:10.1086/591020

Cited by 156 publications

(195 citation statements)

References 46 publications

(62 reference statements)

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“…It has been argued that correlated density and magnetic field strength variations lead rather naturally to a spatial correlation of the hadronic VHE emission with the synchrotron emission. Similar arguments have been brought forward by Tanaka et al (2008). Also, the recent broad-band X-ray synchrotron measurements (Uchiyama et al 2007;Takahashi et al 2008) with the Suzaku instrument were compared to the theoretical synchrotron spectra and were found to be quite consistent with a hadronic model.…”

Section: Introductionsupporting

confidence: 61%

Nonthermal and thermal emission from the supernova remnant RX J1713.7-3946

Berezhko¹,

Völk²

2010

A&A

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Aims.A nonlinear kinetic theory of cosmic ray (CR) acceleration in supernova remnants (SNRs) is employed to investigate the properties of SNR RX J1713.7-3946. Methods. Observations of the nonthermal radio and X-ray emission spectra, as well as the HESS measurements of the very high energy γ-ray emission, are used to constrain the astronomical and CR acceleration parameters of the system. It is argued that RX J1713.7-3946 is a core collapse supernova (SN) of type II/Ib with a massive progenitor, and it has an age of ≈1600 yr and is at a distance of ≈1 kpc. It is also assumed that the CR injection/acceleration takes place uniformly across the shock surface for this kind of core collapse SNR. Results. The theory gives a consistent description for all the existing observational data, including the nondetection of thermal X-rays and the spatial correlation of the X-ray and γ-ray emission in the remnant. Specifically, it is shown that an efficient production of nuclear CRs, leading to strong shock modification and a strong downstream magnetic field B d ≈ 140 μG can reproduce in detail the observed synchrotron emission from radio to X-ray frequencies, together with the γ-ray spectral characteristics as observed by the HESS telescopes. Conclusions. The calculations are consistent with RX J1713.7-3946 being an efficient source of nuclear CRs.

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Section: Introductionsupporting

confidence: 61%

Nonthermal and thermal emission from the supernova remnant RX J1713.7-3946

Berezhko¹,

Völk²

2010

A&A

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“…Therefore the different photon indices can be more naturally interpreted as the presence of spectral cutoffs associated with the unavoidable cutoff in the acceleration spectrum of parent electrons. A solid evidence of such cutoff energy has been reported in a young SNR RX J1713.7-3946 (on the order of 1000 yr) with the Suzaku broadband spectrum of more than two decades in the energy band, i.e., ∼40 keV (Tanaka et al 2008). Although the FoV of the Suzaku HXD is not small enough to allow detailed imaging spectroscopy, Tanaka et al (2008)'s study suggests that a spectral cutoff is a common feature for the synchrotron spectrum, which shows a typical photon index of 2-3 below 10 keV of shell-type SNRs.…”

Section: Interpretation Of Variation In Spectral Shapementioning

confidence: 83%

Nonthermal emission properties of the northwestern rim of supernova remnant RX J0852.0-4622

Kishishita

Hiraga

Uchiyama

2013

A&A

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The supernova remnant (SNR) RX J0852.0-4622 (Vela Jr., G266.6-1.2) is one of the most important SNRs for investigating the acceleration of multi-TeV particles and the origin of Galactic cosmic rays because of its strong synchrotron X-ray and TeV γ-ray emission, which show a shell-like morphology similar to each other. Using the XMM-Newton archival data consisting of multiple pointing observations of the northwestern rim of the remnant, we investigate the spatial properties of the nonthermal X-ray emission as a function of distance from an outer shock wave. All X-ray spectra are well reproduced by an absorbed power-law model above 2 keV. It is found that the spectra show gradual softening from a photon index Γ = 2.56 in the rim region to Γ = 2.96 in the interior region. We show that this radial profile can be interpreted as a gradual decrease of the cutoff energy of the electron spectrum due to synchrotron cooling. By using a simple spectral evolution model that includes continuous synchrotron losses, the spectral softening can be reproduced with the magnetic field strength in the post-shock flow to less than several tens of μG. If this is a typical magnetic field in the SNR shell, γ-ray emission would be accounted for by inverse Compton scattering of high-energy electrons that also produce the synchrotron X-ray emission. Future hard X-ray imaging observations with Nustar and ASTRO-H and TeV γ-ray observations with the Cherenkov Telescope Array (CTA) will allow us to explore other possible explanations of the systematic softening of the X-ray spectra.

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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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Study of Nonthermal Emission from SNR RX J1713.7−3946 withSuzaku

Cited by 156 publications

References 46 publications

Nonthermal and thermal emission from the supernova remnant RX J1713.7-3946

Nonthermal and thermal emission from the supernova remnant RX J1713.7-3946

Nonthermal emission properties of the northwestern rim of supernova remnant RX J0852.0-4622

The e-ASTROGAM mission

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