THE X-RAY PROPERTIES OF FIVE GALACTIC SUPERNOVA REMNANTS DETECTED BY THE<i>SPITZER</i>GLIMPSE SURVEY

Pannuti, T. G.; Rho, Jeonghee; Heinke, C. O.; Moffitt, William P.

doi:10.1088/0004-6256/147/3/55

Cited by 21 publications

(29 citation statements)

References 92 publications

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“…It is highest in regions 1 and 4 in the eastern side of the remnant, and lowest on the western side (region 3). The N H values are comparable to those previously reported (Yamauchi et al 2008;Sezer et al 2011;Yamauchi et al 2013;Pannuti et al 2014).…”

Section: Spectral Analysissupporting

confidence: 91%

“…This is similar to the values derived by Yamauchi et al (2013) and Sezer et al (2011), but is significantly different from the ASCA and Suzaku results (Yamauchi et al 2008;Pannuti et al 2014). The average temperature of the recombining plasma is 0.26 keV, which is slightly lower than the 0.30…”

Section: Spectral Analysissupporting

confidence: 68%

“…Here the best fit APEC temperature derived from the global spectrum is 1.9 +0.6 −0.3 keV, while those for the individual regions are similar, albeit with larger uncertainties (see Table 2). This temperature is much higher than that expected from a SNR, or from the 0.79 keV excess emission seen directly surrounding G346.6-0.2 (Yamauchi et al 2013), while it is lower than that derived by Pannuti et al (2014) using a single APEC model.…”

Section: Spectral Analysiscontrasting

confidence: 54%

“…However, we do not find evidence for underabundance of Fe or over abundance of Ca as claimed by the above two studies. Note that the ASCA data were unable to verify these due to limited photon statistics (Yamauchi et al 2008;Pannuti et al 2014).…”

Section: Spectral Analysismentioning

confidence: 99%

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An XMM-Newton Study of the Mixed-morphology Supernova Remnant G346.6-0.2

Auchettl

Wong

et al. 2017

ApJ

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We present an X-ray imaging and spectroscopic study of the molecular cloud interacting mixedmorphology (MM) supernova remnant (SNR) G346.6-0.2 using XMM-Newton. The X-ray spectrum of the remnant is well described by a recombining plasma that most likely arises from adiabatic cooling, and has sub-solar abundances of Mg, Si, and S. Our fits also suggest the presence of either an additional power-law component with a photon index of ∼2, or an additional thermal component with a temperature of ∼2.0 keV. We investigate the possible origin of this component and suggest that it could arise from either the Galactic ridge X-ray emission, an unidentified pulsar wind nebula or Xray synchrotron emission from high-energy particles accelerated at the shock. However, deeper, high resolution observations of this object are needed to shed light on the presence and origin of this feature. Based on its morphology, its Galactic latitude, the density of the surrounding environment and its association with a dense molecular cloud, G346.6-0.2 most likely arises from a massive progenitor that underwent core-collapse.

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Section: Spectral Analysissupporting

confidence: 91%

Section: Spectral Analysissupporting

confidence: 68%

Section: Spectral Analysiscontrasting

confidence: 54%

Section: Spectral Analysismentioning

confidence: 99%

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An XMM-Newton Study of the Mixed-morphology Supernova Remnant G346.6-0.2

Auchettl

Wong

et al. 2017

ApJ

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“…Nowadays, surveys provide us with observations of Galactic supernova remnants, e.g. in gamma-rays (Abdo et al 2010), X-ray (Pannuti et al 2014), the infrared (Reach et al 2006) or in submillimeter (van Dishoeck et al 1993). Catalogues of remnants visible in the radio waveband in the northern and southern hemisphere are available in Kothes et al (2006) and Whiteoak & Green (1996), respectively.…”

Section: Introductionmentioning

confidence: 99%

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Meyer¹,

Langer²,

Mackey³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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After the death of a runaway massive star, its supernova shock wave interacts with the bow shocks produced by its defunct progenitor, and may lose energy, momentum, and its spherical symmetry before expanding into the local interstellar medium (ISM). We investigate whether the initial mass and space velocity of these progenitors can be associated with asymmetric supernova remnants. We run hydrodynamical models of supernovae exploding in the pre-shaped medium of moving Galactic core-collapse progenitors. We find that bow shocks that accumulate more than about 1.5 M ⊙ generate asymmetric remnants. The shock wave first collides with these bow shocks 160 − 750 yr after the supernova, and the collision lasts until 830 − 4900 yr. The shock wave is then located 1.35 − 5 pc from the center of the explosion, and it expands freely into the ISM, whereas in the opposite direction it is channelled into the region of undisturbed wind material. This applies to an initially 20 M ⊙ progenitor moving with velocity 20 km s −1 and to our initially 40 M ⊙ progenitor. These remnants generate mixing of ISM gas, stellar wind and supernova ejecta that is particularly important upstream from the center of the explosion. Their lightcurves are dominated by emission from optically-thin cooling and by X-ray emission of the shocked ISM gas. We find that these remnants are likely to be observed in the [OIII] λ 5007 spectral line emission or in the soft energy-band of X-rays. Finally, we discuss our results in the context of observed Galactic supernova remnants such as 3C391 and the Cygnus Loop.

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Population study of Galactic supernova remnants at very high γ-ray energies with H.E.S.S.

Abdalla¹,

Abramowski²,

Aharonian³

et al. 2018

A&A

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Shell-type supernova remnants (SNRs) are considered prime candidates for the acceleration of Galactic cosmic rays (CRs) up to the knee of the CR spectrum at E ≈ 3 × 10 15 eV. Our Milky Way galaxy hosts more than 350 SNRs discovered at radio wavelengths and at high energies, of which 220 fall into the H.E.S.S. Galactic Plane Survey (HGPS) region. Of those, only 50 SNRs are coincident with a H.E.S.S source and in 8 cases the very high-energy (VHE) emission is firmly identified as an SNR. The H.E.S.S. GPS provides us with a legacy for SNR population study in VHE γ-rays and we use this rich data set to extract VHE flux upper limits from all undetected SNRs. Overall, the derived flux upper limits are not in contradiction with the canonical CR paradigm. Assuming this paradigm holds true, we can constrain typical ambient density values around shell-type SNRs to n ≤ 7 cm -3 and electron-to-proton energy fractions above 10 TeV to ep ≤ 5 × 10 −3 . Furthermore, comparisons of VHE with radio luminosities in non-interacting SNRs reveal a behaviour that is in agreement with the theory of magnetic field amplification at shell-type SNRs.

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THE X-RAY PROPERTIES OF FIVE GALACTIC SUPERNOVA REMNANTS DETECTED BY THESPITZERGLIMPSE SURVEY

Cited by 21 publications

References 92 publications

An XMM-Newton Study of the Mixed-morphology Supernova Remnant G346.6-0.2

An XMM-Newton Study of the Mixed-morphology Supernova Remnant G346.6-0.2

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Population study of Galactic supernova remnants at very high γ-ray energies with H.E.S.S.

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