Probing the cosmic X-ray laboratory with the Chandra HETGS

Flanagan, Kathryn A.; Canizares, C. R.; Dewey, Daniel; Fredericks, A. C.; Houck, J. C.; Lee, J. C.; Marshall, Herman L.; Schattenburg, Mark L.

doi:10.1117/12.461738

Cited by 4 publications

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“…This is indicative of a less decelerated expansion in that direction. Chandra observations have shown that there is evidence for a spatially varying distribution of the ionization stages and the existence of a reverse shock in the ejecta (Gaetz et al 2000;Flanagan et al 2001). The results obtained from the spectral analysis of the XMM-Newton EPIC-PN data show that there are differences in the plasma states between various parts of the SNR with spatial temperature and ionization stage variations, contributing to its complicated structure.…”

Section: Discussionmentioning

confidence: 99%

XMM-Newton EPIC observation of SMC SNR 0102-72.3

Sasaki

Stadlbauer

Haberl

et al. 2001

A&A

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Abstract.Results from observations of the young oxygen-rich supernova remnant SNR 0102−72.3 in the Small Magellanic Cloud during the calibration phase of the XMM-Newton Observatory are presented. Both EPIC-PN and MOS observations show a ringlike structure with a radius of ∼15 already known from Einstein, ROSAT and Chandra observations. Spectra of the entire SNR as well as parts in the eastern half were analyzed confirming shocked hot plasma in non-uniform ionization stages as the origin of the X-ray emission. The spectra differ in the northeastern and the southeastern part of the X-ray ring, showing emission line features of different strength. The temperature in the northeastern part is significantly higher than in the southeast, reflected by the lines of higher ionization stages and the harder continuum. Comparison to radio data shows the forward shock of the blast wave dominating in the northern part of the SNR, while the southern emission is most likely produced by the recently formed reverse shock in the ejecta. In the case of the overall spectrum of SNR 0102−72.3, the two-temperature non-equilibrium ionization model is more consistent with the data in comparison to the single plane-parallel shock model. The structure of SNR 0102−72.3 is complex due to variations in shock propagation leading to spatially differing X-ray spectra.

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Section: Discussionmentioning

confidence: 99%

XMM-Newton EPIC observation of SMC SNR 0102-72.3

Sasaki

Stadlbauer

Haberl

et al. 2001

A&A

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Probing X-ray Emitting Plasma with High Resolution Chandra and XMM-Newton Spectra

Lee¹

2005

Highlights astron.

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Abstract. Highlights of interesting astrophysical discoveries are reviewed in the context of high resolution X-ray spectroscopy made possible with Chandra and XMM-Newton , and its relevance to atomic physics calculations and measurements is discussed. These spectra have shown that the overlap between astrophysics and atomic physics is stronger than ever, as discoveries of new X-ray lines and edge structure is matching the need for increasingly detailed theoretical calculations and experimental measurements of atomic data. X-ray spectral probes of astrophysical systems at high resolutionHigh resolution X-ray spectroscopy provides a powerful new tool for advancing our understanding of the physical environments of energetic astrophysical systems. As demonstrated with Chandra and XMM spectral studies, the scientific impact is far reaching, encompassing studies of stars, supernova remnants (SNR), X-ray binaries (XRBs), active galactic nuclei (AGN), clusters, and the interstellar and intergalactic medium (respectively ISM and IGM). To give a flavor for some of the newly X-ray discovered spectral features and their relevance to spectral modeling and calculations, I will draw mostly on examples from observations of AGN and XRBs with which I have been involved. See for a complete review of Chandra and XMM results.

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ChandraHigh‐Resolution X‐Ray Spectrum of Supernova Remnant 1E 0102.2−7219

Flanagan

Canizares

Dewey

et al. 2004

ApJ

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Chandra High Energy Transmission Grating Spectrometer observations of the supernova remnant (SNR) 1E 0102.2À7219 in the Small Magellanic Cloud reveal a spectrum dominated by X-ray emission lines from hydrogen-like and helium-like ions of oxygen, neon, magnesium, and silicon, with little iron. The dispersed spectrum shows a series of monochromatic images of the source in the light of individual spectral lines. Detailed examination of these dispersed images reveals Doppler shifts within the SNR, indicating bulk matter velocities on the order of 1000 km s À1 . These bulk velocities suggest an expanding ringlike structure with additional substructure, inclined to the line of sight. A two-dimensional spatial/velocity map of the SNR shows a striking spatial separation of redshifted and blueshifted regions and indicates a need for further investigation before an adequate three-dimensional model can be found. The radii of the ringlike images of the dispersed spectrum vary with ionization stage, supporting an interpretation of progressive ionization due to passage of the reverse shock through the ejecta. Plasma diagnostics with individual emission lines of oxygen are consistent with an ionizing plasma in the low-density limit and provide temperature and ionization constraints on the plasma. Assuming a pure metal plasma, the mass of oxygen is estimated at $6 M , consistent with a massive progenitor.

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Probing the cosmic X-ray laboratory with the Chandra HETGS

Cited by 4 publications

References 0 publications

XMM-Newton EPIC observation of SMC SNR 0102-72.3

XMM-Newton EPIC observation of SMC SNR 0102-72.3

Probing X-ray Emitting Plasma with High Resolution Chandra and XMM-Newton Spectra

ChandraHigh‐Resolution X‐Ray Spectrum of Supernova Remnant 1E 0102.2−7219

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