Suzaku Observation of 30 Dor C: A Supernova Remnant with the Largest Non-Thermal Shell

Yamaguchi, Hiroya; Bamba, Aya; Koyama, K.

doi:10.1093/pasj/61.sp1.s175

Cited by 20 publications

(34 citation statements)

References 34 publications

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“…The superbubble 30 Dor C stands out in X-rays as it contains, in the western part, an X-ray synchrotron-emitting shell with a radius of 47 pc, which makes it the largest known X-ray synchrotron shell (24)(25)(26). X-ray synchrotron emission, which indicates the presence of VHE electrons, is usually associated with 100 − 2000 yearold SNRs with radii smaller than 25 pc.…”

Section: Dor Cmentioning

confidence: 99%

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The exceptionally powerful TeV γ-ray emitters in the Large Magellanic Cloud

Abramowski

Aharonian

Benkhali

et al. 2015

Science

132

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The Large Magellanic Cloud, a satellite galaxy of the Milky Way, has been observed with the High Energy Stereoscopic System (H.E.S.S.) above an energy of 100 billion electron volts for a deep exposure of 210 hours. Three sources of different types were detected: the pulsar wind nebula of the most energetic pulsar known, N 157B; the radio-loud supernova remnant N 132D; and the largest nonthermal x-ray shell, the superbubble 30 Dor C. The unique object SN 1987A is, unexpectedly, not detected, which constrains the theoretical framework of particle acceleration in very young supernova remnants. These detections reveal the most energetic tip of a γ-ray source population in an external galaxy and provide via 30 Dor C the unambiguous detection of γ-ray emission from a superbubble.

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Section: Dor Cmentioning

confidence: 99%

“…If the radiation fields are known, the magnetic field can be inferred from the combination of X-ray and γ-ray measurements. N 157B is likely associated with (26). For N 132D, radio data is from (33), and X-ray limits are from (34) and from re-analysed Chandra data.…”

Section: N 157bmentioning

confidence: 99%

The exceptionally powerful TeV γ-ray emitters in the Large Magellanic Cloud

Abramowski

Aharonian

Benkhali

et al. 2015

Science

132

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“…In recent years, non-thermal X-ray emission has been detected from a number of Galactic (RCW 38, Wolk et al 2002;Westerlund 1, Muno et al 2006), and extragalactic SBs. These include N 11 (Maddox et al 2009), N 51D (Cooper et al 2004), 30 Dor C (Bamba et al 2004;Smith & Wang 2004;Yamaguchi et al 2009) in the Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA.…”

Section: Introductionmentioning

confidence: 99%

XMM-Newtonstudy of 30 Doradus C and a newly identified MCSNR J0536−6913 in the Large Magellanic Cloud

Kavanagh

Sasaki

Bozzetto

et al. 2014

A&A

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Aims. We present a detailed study of the superbubble 30 Dor C and the newly identified supernova remnant MCSNR J0536-6913 in the Large Magellanic Cloud. Methods. All available XMM-Newton data (flare-filtered exposure times of 420 ks EPIC-pn, 556 ks EPIC-MOS1, 614 ks EPIC-MOS2) were used to characterise the thermal X-ray emission in the region. An analysis of the non-thermal X-ray emission is also presented and discussed in the context of emission mechanisms previously suggested in the literature. These data are supplemented by X-ray data from Chandra, optical data from the Magellanic Cloud Emission Line Survey, and radio data from the Australia Telescope Compact Array and the Molonglo Observatory Synthesis Telescope. Results. The brightest thermal emission towards 30 Dor C was found to be associated with a new supernova remnant, MCSNR J0536−6913. X-ray spectral analysis of MCSNR J0536−6913 suggested an ejecta-dominated remnant with lines of O, Ne, Mg, and Si, and a total 0.3−10 keV X-ray luminosity of ∼8 × 10 34 erg s −1 . Based on derived ejecta abundance ratios, we determined the mass of the stellar progenitor to be either ∼18 M or as high as > ∼ 40 M , though the spectral fits were subject to simplifying assumptions (e.g., uniform temperature and well-mixed ejecta). The thermal emission from the superbubble exhibited enrichment by α-process elements, evidence for a recent core-collapse SNR interaction with the superbubble shell. We detected non-thermal X-ray emission throughout 30 Dor C, with the brightest regions being highly correlated with the Hα and radio shells. We created a non-thermal spectral energy distribution for the north-eastern shell of 30 Dor C which was best-fit with an exponentially cut-off synchrotron model. Conclusions. Thermal X-ray emission from 30 Dor C is very complex, consisting of a large scale superbubble emission at the eastern shell wall with the brightest emission due to MCSNR J0536−6913. The fact that the non-thermal spectral energy distribution of the superbubble shell was observed to roll-off is further evidence that the non-thermal X-ray emission from 30 Dor C is synchrotron in origin.

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“…A standard picture of thermal plasmas associated with supernova remnants (SNRs) is that the state of the gas appears to be either an ionizing plasma (IP) for young or intermediate aged SNRs (e.g., Kepler's SNR, Kinugasa & Tsunemi 1999), or plasma in collisional ionization equilibrium (CIE) for old SNRs (e.g., 30 Dor C, Yamaguchi et al 2009a). However, recent X-ray observations have revealed several SNRs that are in the recombination-dominated phase (IC 443, Yamaguchi et al 2009b;W 49 B, Ozawa et al 2009; G359.1−0.5, Ohnishi et al 2011;W 28, Sawada & Koyama 2012;W 44, Uchida et al 2012;G346.6−0.2, Yamauchi et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Discovery of recombining plasma in the supernova remnant 3C 391

Satô

Koyama

Takahashi

et al. 2014

Publications of the Astronomical Society of Japan

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Recent X-ray study of middle-aged supernova remnants (SNRs) reveals strong radiative recombination continua (RRCs) associated with overionized plasmas, which origin still remains uncertain. We report a discovery of an RRC in the middle-aged SNR 3C 391. If the X-ray spectrum is fitted with a two-temperature plasma model in collisional ionization equilibrium (CIE), residuals of a Si XIV Lyα line at 2.006 keV, a S XVI Lyα line at 2.623 keV and the edge of a RRC of Si XIII at 2.666 keV are found. In fact, the X-ray spectrum is well described by the composite model consisting of the CIE plasma and a recombining plasma (RP). The abundance pattern suggests that the RP is due to ejecta from core-collapse supernova of the progenitor mass of about 15 M . There is no significant difference of the recombining parameters between the south-east region and the north-west region surrounded by dense molecular clouds. We also find a hint of a Fe I Kα line at 6.4 keV (2.4 σ detection) from the south-east region of the SNR.

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Suzaku Observation of 30 Dor C: A Supernova Remnant with the Largest Non-Thermal Shell

Cited by 20 publications

References 34 publications

The exceptionally powerful TeV γ-ray emitters in the Large Magellanic Cloud

The exceptionally powerful TeV γ-ray emitters in the Large Magellanic Cloud

XMM-Newtonstudy of 30 Doradus C and a newly identified MCSNR J0536−6913 in the Large Magellanic Cloud

Discovery of recombining plasma in the supernova remnant 3C 391

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