XMM-Newton EPIC observation of SMC SNR 0102-72.3

Sasaki, M.; Stadlbauer, T.; Haberl, F.; Filipović, Miroslav; Bennie, P. J.

doi:10.1051/0004-6361:20000015

Cited by 20 publications

(16 citation statements)

References 15 publications

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“…In 10 subregions we found Ne abundances significantly higher than cosmic value, with an average Ne/Ne = 1.7 ± 0.2 over all the subregions. Typically the Ne overabundance is associated with overabundances of O, Mg, Si (Sasaki et al 2001) and Fe and is a clear signature of the ejecta, but this is not the case, since Fe is underabundant and we found solar O abundances. Similar values of the Ne abundance in the Vela SNR were found by Plucinsky et al (2002), who showed that the Vela Bullet D X-ray emission can be described with a non-equilibrium of ionization model (which seems to exclude that Bullet D is a fragment of ejecta) with Ne/Ne ≈ 2.…”

Section: Spectral Analysismentioning

confidence: 62%

Shock-cloud interaction in the Vela SNR observed withXMM-Newton

Miceli¹,

Bocchino

Maggio

et al. 2005

A&A

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We analyzed an XMM-Newton EPIC observation of a bright knot, named FilD, in the northern rim of the Vela SNR, where the shock has encountered a cloud. The good combination of sensitivity, spectral, and spatial resolution allowed us to describe the internal structure of the observed ISM clouds and to obtain estimates of their temperature, density, O, Ne, and Fe abundances, and of their extension along the line of sight. We also examined the interaction of the shock with the FilD knot and estimated that the time elapsed from the shock impact is about one cloud crushing time. Our analysis allowed us to conclude that the observed X-ray emission is best explained by the propagation of transmitted shocks through ISM inhomogeneities with an inward increasing density profile. We found that the interaction with the shock determines the heating of the inner part of the clouds and the evaporation of the outer part.

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Section: Spectral Analysismentioning

confidence: 62%

Shock-cloud interaction in the Vela SNR observed withXMM-Newton

Miceli¹,

Bocchino

Maggio

et al. 2005

A&A

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“…They concluded that abundance inhomogeneities exist in the plasma. The insufficiency of a single T e -plasma to parameterize the global spectrum was confirmed by Sasaki et al (2001) with XMM-Newton EPIC PN data; these authors invoked two plasma components and additionally examined distinct regions of the remnant.…”

Section: Caveat On Global Line Ratiosmentioning

confidence: 93%

“…Since the northern portion of the remnant displays a linear shelf appearance, it is conceivable that the expanding ejecta has encountered a dense region of the circumstellar medium (CSM); the higher density would encourage more rapid ionization. Sasaki et al (2001) examined EPIC PN spectra from a northeastern segment (eastward of the shelf ) and from the bright X-ray arc in the southeast. They found that the northern spectrum had a higher fitted temperature and an order of magnitude higher ionization timescale than the southern region, indicating higher ionization.…”

Section: Caveat On Global Line Ratiosmentioning

confidence: 99%

“…By contrast, Eriksen et al (2001) estimate a free expansion age of 2100 yr. Hughes et al (2000) deduce that a significant fraction of the shock energy has gone into cosmic rays. Composite X-ray spectra of moderate resolution have been obtained for the whole remnant with ASCA (Hayashi et al 1994) and XMM-Newton (Sasaki et al 2001). These observations confirm that a singlecomponent nonequilibrium plasma is inadequate to account for the global SNR spectrum.…”

Section: Introductionmentioning

confidence: 99%

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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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“…It is the brightest SNR in X-rays in the Small Magellanic Cloud (SMC). E0102 has been extensively imaged by Chandra (Gaetz et al 2000;Hughes et al 2000) and XMM-Newton (Sasaki et al 2001). Figures 1 and 2 show images of E0102 with the relevant spectral extraction regions for each of the instruments included in this analysis.…”

Section: The Snr 1e 01022-7219mentioning

confidence: 99%

SNR 1E 0102.2-7219 as an X-ray calibration standard in the 0.5−1.0 keV bandpass and its application to the CCD instruments aboardChandra,Suzaku,SwiftandXMM-Newton

Plucinsky

Beardmore

Foster

et al. 2016

A&A

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Context. The flight calibration of the spectral response of charge-coupled device (CCD) instruments below 1.5 keV is difficult in general because of the lack of strong lines in the on-board calibration sources typically available. This calibration is also a function of time due to the effects of radiation damage on the CCDs and/or the accumulation of a contamination layer on the filters or CCDs. Aims. We desire a simple comparison of the absolute effective areas of the current generation of CCD instruments onboard the following observatories: Chandra ACIS-S3, XMM-Newton (EPIC-MOS and EPIC-pn), Suzaku XIS, and Swift XRT and a straightforward comparison of the time-dependent response of these instruments across their respective mission lifetimes. Methods. We have been using 1E 0102.2-7219, the brightest supernova remnant in the Small Magellanic Cloud, to evaluate and modify the response models of these instruments. 1E 0102.2-7219 has strong lines of O, Ne, and Mg below 1.5 keV and little or no Fe emission to complicate the spectrum. The spectrum of 1E 0102.2-7219 has been well-characterized using the RGS gratings instrument on XMM-Newton and the HETG gratings instrument on Chandra. As part of the activities of the International Astronomical Consortium for High Energy Calibration (IACHEC), we have developed a standard spectral model for 1E 0102.2-7219 and fit this model to the spectra extracted from the CCD instruments. The model is empirical in that it includes Gaussians for the identified lines, an absorption component in the Galaxy, another absorption component in the SMC, and two thermal continuum components with different temperatures. In our fits, the model is highly constrained in that only the normalizations of the four brightest lines/line complexes (the O vii Heα triplet, O viii Lyα line, the Ne ix Heα triplet, and the Ne x Lyα line) and an overall normalization are allowed to vary, while all other components are fixed. We adopted this approach to provide a straightforward comparison of the measured line fluxes at these four energies. We have examined these measured line fluxes as a function of time for each instrument after applying the most recent calibrations that account for the time-dependent response of each instrument. Results. We performed our effective area comparison with representative, early mission data when the radiation damage and contamination layers were at a minimum, except for the XMM-Newton EPIC-pn instrument which is stable in time. We found that the measured fluxes of the O vii Heα r line, the O viii Lyα line, the Ne ix Heα r line, and the Ne x Lyα line generally agree to within ±10% for all instruments, with 38 of our 48 fitted normalizations within ±10% of the IACHEC model value. We then fit all available observations of 1E 0102.2-7219 for the CCD instruments close to the on-axis position to characterize the time dependence in the 0.5−1.0 keV band. We present the measured line normalizations as a function of time for each CCD instrument so that the users may estimate the un...

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XMM-Newton EPIC observation of SMC SNR 0102-72.3

Cited by 20 publications

References 15 publications

Shock-cloud interaction in the Vela SNR observed withXMM-Newton

Shock-cloud interaction in the Vela SNR observed withXMM-Newton

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

SNR 1E 0102.2-7219 as an X-ray calibration standard in the 0.5−1.0 keV bandpass and its application to the CCD instruments aboardChandra,Suzaku,SwiftandXMM-Newton

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