A High‐Resolution Study of Nonthermal Radio and X‐Ray Emission from Supernova Remnant G347.3−0.5

Lazendić, J. S.; Slane, Patrick; Gaensler, B. M.; Reynolds, Stephen P.; Plucinsky, Paul P.; Hughes, John P.

doi:10.1086/380956

Cited by 138 publications

(195 citation statements)

References 43 publications

(89 reference statements)

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“…Only part of the remnant shell could be detected in radio synchrotron emission up to now, with a poorly known spectral form (Lazendic et al 2004). For the spatially integrated radio flux, Aharonian et al (2006) estimate about twice the value found by Lazendic et al (2004). Most recently, Acero et al (2009) have derived a total flux value of 22 Jy < S < 26 Jy at 1.4 GHz, still about two times higher than estimated by Aharonian et al (2006).…”

Section: Introductionmentioning

confidence: 83%

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: Introductionmentioning

confidence: 83%

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

Berezhko¹,

Völk²

2010

A&A

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“…In their discussion, these authors argued that an enhanced value of the CO (J ¼ 2 1)/(J ¼ 1 0) line ratio in cloud A indicates the physical interaction with the SNR shock (see also Butt et al 2001). This estimate, $6 kpc, was often used in subsequent studies of the physical properties of G347.3À0.5 (e.g., Lazendic et al 2004;Pannuti et al 2003;Cassam-Chenai et al 2004b).…”

Section: Introductionmentioning

confidence: 99%

A Detailed Study of Molecular Clouds toward the TeV Gamma‐Ray Supernova Remnant G347.3−0.5

Moriguchi

Tamura

Tawara

et al. 2005

ApJ

108

134

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The supernova remnant G347.3À0.5 (J1713.7À3946) is known as one of the unique SNRs that emit TeV -rays, as well as nonthermal X-rays. We present a detailed study of molecular gas toward this SNR obtained with the 4 m millimeter and submillimeter telescope NANTEN at an angular resolution of 2A6. This study has revealed that several intensity peaks and the overall distribution of the molecular gas with radial velocities from À12 to À3 km s À1 show a remarkably good correlation with the X-ray features, strongly supporting the recently derived kinematic distance around 1 kpc, as opposed to the 6 kpc previously claimed. In addition, we show that absorption of X-rays is caused by local molecular gas at softer X-ray bands. Subsequent measurements of the submillimeter J ¼ 3 2 transition of CO made with the ASTE 10 m and CSO 10.4 m submillimeter telescopes toward three of the molecular intensity peaks have revealed higher excitation conditions, most likely higher temperatures above $30 K , in contrast to the typical gas temperature, 10 K, in low-mass dark clouds. This temperature rise is most likely caused by enhanced heating by the high-energy events in the SNR, where possible mechanisms include heating by X-rays, -rays, and/or cosmic-ray protons, although we admit that additional radiative heating by young protostars embedded may be working as well. In one of the CO peaks, we have confirmed the presence of broad molecular wings of $20 km s À1 velocity extent in the CO J ¼ 3 2 transition. Two alternative interpretations for the wings are presented; one is shock acceleration by the blast wave, and the other is molecular outflow driven by an embedded protostar. The SNR evolution is well explained as the free expansion phase based on the distance of 1 kpc. The molecular data set should be valuable for making a further detailed comparison with the -ray and X-ray distributions in order to examine the cosmic-ray acceleration quantitatively. Subject headingg s: cosmic rays -ISM: individual (SNR J1713.37À3946) -ISM: kinematics and dynamicssupernova remnants

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“…The leptonic scenario fits the broadband spectrum of an SNR assuming a pool of accelerated electrons scattered off the cosmic microwave background (CMB) producing VHE g-rays, while the magnetic field and electron spectrum cutoff are tuned to fit the radio and X-ray data (e.g., Lazendic et al 2004). The hadronic model fits the VHE g-ray spectrum assuming a beam of accelerated protons hits a target, such as a nearby molecular cloud (Aharonian 2002 based on a simplified "one-zone" model, which typically includes CMB photons only.…”

Section: Introductionmentioning

confidence: 99%

Inverse Compton Emission from Galactic Supernova Remnants: Effect of the Interstellar Radiation Field

Porter¹,

V²,

Strong³

2006

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The evidence for particle acceleration in supernova shells comes from electrons whose synchrotron emission is observed in radio and X-rays. Recent observations by the HESS instrument reveal that supernova remnants also emit TeV g-rays, long-awaited experimental evidence that supernova remnants can accelerate cosmic rays up to the "knee" energies. Still, uncertainty exists whether these g-rays are produced by electrons via inverse Compton scattering or by protons via -decay. The multiwavelength spectra of supernova remnants can be fitted 0 p with both mechanisms, although a preference is often given to -decay due to the spectral shape at very high 0 p energies. A recent study of the interstellar radiation field indicates that its energy density, especially in the inner Galaxy, is higher than previously thought. In this Letter we evaluate the effect of the interstellar radiation field on the inverse Compton emission of electrons accelerated in a supernova remnant located at different distances from the Galactic center. We show that contribution of optical and infrared photons to the inverse Compton emission may exceed the contribution of cosmic microwave background and in some cases broaden the resulting g-ray spectrum. In addition, we show that if a supernova remnant is located close to the Galactic center, its gray spectrum will exhibit a "universal" cutoff at very high energies due to the Klein-Nishina effect and not due to the cutoff of the electron spectrum. As an example, we apply our calculations to the supernova remnants RX J1713.7Ϫ3946 and G0.9ϩ0.1, recently observed by HESS.

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A High‐Resolution Study of Nonthermal Radio and X‐Ray Emission from Supernova Remnant G347.3−0.5

Cited by 138 publications

References 43 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

A Detailed Study of Molecular Clouds toward the TeV Gamma‐Ray Supernova Remnant G347.3−0.5

Inverse Compton Emission from Galactic Supernova Remnants: Effect of the Interstellar Radiation Field

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