Thermal and Nonthermal X‐Ray Emission in Supernova Remnant RCW 86

Borkowski, Kazimierz J.; Rho, Jeonghee; Reynolds, Stephen P.; Dyer, K. K.

doi:10.1086/319716

Cited by 83 publications

(69 citation statements)

References 28 publications

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“…As a significant non-thermal X-ray component (whose potential origin in discussed in Section 5) has also been detected in our analysis, another possibility is that the synchrotron continuum is dominating the observed Xray spectrum. Borkowski et al (2001) determined that a strong synchrotron continuum can cause X-ray lines to appear to be much weaker than that of a solar abundance plasma.…”

Section: Nature Of the Thermal X-ray Emissionmentioning

confidence: 99%

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: Nature Of the Thermal X-ray Emissionmentioning

confidence: 99%

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

Auchettl

Wong

et al. 2017

ApJ

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“…G266.2-1.2: Slane et al 2001). Spatially resolved data show that SNR spectra are spatially complex (e.g., RCW 86: Borkowski et al 2001b;Bocchino et al 2000; for a review see Hwang 2001). 13 A catalog, based on Chandra data and complete down to L 0.125−8.0 keV ∼ 10 36 erg s −1 , of 110 sources located in a large central region of the nearby face-on spiral M 101 -a system that is considered to be in many ways similar to the Galaxy -contains 9 SNRs (Pence et al 2001).…”

Section: Supernova Remnantsmentioning

confidence: 99%

X-ray spectral components of starburst galaxies

Peršić

Rephaeli

2002

A&A

124

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Abstract. X-ray emission processes in starburst galaxies (SBGs) are assessed, with the aim of identifying and characterizing the main spectral components. Our survey of spectral properties, complemented with a model for the evolution of galactic stellar populations, leads to the prediction of a complex spectrum. Comparing the predicted spectral properties with current X-ray measurements of the nearby SBGs M 82 and N253, we draw the following tentative conclusions: 1) X-ray binaries with accreting neutron stars are the main contributors in the 2-15 keV band, and could be responsible for the yet uninterpreted hard component required to fit the observed 0.5-10 keV spectra of SBGs; 2) diffuse thermal plasma contributes at energies < ∼ 1 keV; 3) nonthermal emission, from Compton scattering of FIR and CMB radiation fields photons off supernova-accelerated relativistic electrons, and AGN-like emission, are likely be the dominant emission at energies > ∼ 30 keV; 4) supernova remnants make a relatively minor contribution to the X-ray continuum but may contribute appreciably to the Fe-K emission at 6.7 keV.

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“…Koyama et al (1995) discovered synchrotron X-rays from shells of SN 1006, which is the first observational result indicating that SNRs accelerate electrons up to $TeV. By now, several SNRs have been identified as synchrotron X-ray emitters (e.g., RX J1713.7À3946, Koyama et al 1997;Slane et al 1999;RCW 86, Bamba et al 2000;Borkowski et al 2001;Rho et al 2002;Cas A, Vink & Laming 2003; see also Bamba et al 2005;Bamba 2004). …”

Section: Introductionmentioning

confidence: 97%

ChandraObservations of Galactic Supernova Remnant Vela Jr.: A New Sample of Thin Filaments Emitting Synchrotron X‐Rays

Bamba

Yamazaki

Hiraga

2005

ApJ

100

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The Galactic supernova remnant (SNR) Vela Jr. (RX J0852.0À4622, G266.6-1.2) shows sharp filamentary structures on its northwestern edge in the hard X-ray band. The filaments are very smooth and located on the extreme outside edge of the remnant. We measured the averaged scale width of the filaments (w u and w d ) with excellent spatial resolution with Chandra, and they are on the order of the size of the point-spread function of Chandra on the upstream side and 49B5 (36B0-88B8) on the downstream side. The spectra of the filaments are very hard and have no linelike structure; they were well reproduced with an absorbed power-law model with À ¼ 2:67 (2.55-2.77) or a SRCUT model with roll ¼ 4:3 (3:4 5:3) ; 10 16 Hz under the assumption of p ¼ 0:3. These results imply that the hard X-rays are synchrotron radiation emitted by accelerated electrons, as mentioned previously. Using a correlation between the function B roll /w 2 d and the SNR age, we estimated the distance and the age of Vela Jr.: the estimated distance and age are 0.33 (0.26-0.50) kpc and 660 (420-1400) yr, respectively. These results are consistent with previous reports, implying that the B-age relation may be a useful tool for estimating the distance and the age of synchrotron X-ray-emitting SNRs. Subject headingg s: acceleration of particles -ISM: individual (G266.6-1.2, RX J0852.0À4622) -supernova remnants -X-rays: ISM

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Thermal and Nonthermal X‐Ray Emission in Supernova Remnant RCW 86

Cited by 83 publications

References 28 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

X-ray spectral components of starburst galaxies

ChandraObservations of Galactic Supernova Remnant Vela Jr.: A New Sample of Thin Filaments Emitting Synchrotron X‐Rays

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