Supernova Remnants in the Magellanic Clouds. I. The Colliding Remnants DEM L316

Williams, R. M.; Chu, You‐Hua; Dickel, John R.; Beyer, R. A.; Petre, Robert; Smith, R. C.; Milne, D. K.

doi:10.1086/303990

Cited by 39 publications

(49 citation statements)

References 23 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…On the other hand it is difficult to understand the minimum X-ray emission in the overlapping region of both SNRs. We note in that context that Williams et al (1997), who studied the colliding SNRs DEM L316 in the Large Magellanic Cloud, did not find X-ray emission in the region of overlap of both SNRs. We conclude that details of the conditions in the interacting regions are not well constrained and need a more detailed investigation According to the interaction scenario the SNR in the north exploded first and created a complete circular, shelltype SNR.…”

Section: Optical X-ray and Infrared Datamentioning

confidence: 82%

Is the Cygnus Loop two supernova remnants?

Uyanıker

Reich

Yar

et al. 2002

A&A

View full text Add to dashboard Cite

Abstract. The Cygnus Loop is classified as a middle-aged supernova remnant (SNR) located below the Galactic equator ( = 74• , b = −8.• 6) and 770 pc away from us. Its large size and little confusion with Galactic emission makes it an ideal test ground for evolutionary and structural theories of SNRs. New radio continuum mapping of the Cygnus Loop at 2695 MHz with the Effelsberg 100-m telescope provides indications that the Cygnus Loop consists of two separate SNRs. Combining this result with data from the literature we argue that a secondary SNR exists in the south with a recently detected neutron star close to its center. Two interacting SNRs seem to be the best explanation to account for the Cygnus Loop observations at all wavelengths.

show abstract

Section: Optical X-ray and Infrared Datamentioning

confidence: 82%

Is the Cygnus Loop two supernova remnants?

Uyanıker

Reich

Yar

et al. 2002

A&A

View full text Add to dashboard Cite

show abstract

“…The angular resolution of the CTIO images was about 1B5; the half-power beamwidth of the radio images was 12 00 . Other details of these observations are given in Williams et al (1997).…”

Section: Observationsmentioning

confidence: 99%

“…Three-color images comparing the Chandra morphology to emission in H, [O iii], and 7 cm radio (Williams et al 1997) are shown in Figures 2a-2c. In general, the brightest regions of X-ray emission appear to correspond to areas that are fainter at radio wavelengths.…”

Section: X-ray Morphologiesmentioning

confidence: 99%

Supernova Remnants in the Magellanic Clouds. VI. The DEM L316 Supernova Remnants

Williams

Chu

2005

ApJ

View full text Add to dashboard Cite

The DEM L316 system contains two shells, both with the characteristic signatures of supernova remnants (SNRs). We analyze Chandra and XMM-Newton data for DEM L316, investigating its spatial and spectral X-ray features. Our Chandra observations resolve the structure of the northeastern SNR (shell A) as a bright inner ring and a set of ''arcs'' surrounded by fainter diffuse emission. The spectrum is well fit by a thermal plasma model with a temperature of $1.4 keV; we do not find significant spectral differences for different regions of this SNR. The southwestern SNR (shell B) exhibits an irregular X-ray outline, with a brighter interior ring of emission including a bright knot of emission. Overall, the emission of the SNR is well described by a thermal plasma of temperature $0.6 keV. The bright knot, however, is spectrally distinct from the rest of the SNR, requiring the addition of a high-energy spectral component consistent with a power-law spectrum of photon index 1.6-1.8. We confirm the findings of Nishiuchi and coworkers that the spectra of these shells are notably different, with shell A requiring a high iron abundance for a good spectral fit, implying a Type Ia origin. We further explicitly compare abundance ratios to model predictions for Type Ia and Type II supernovae. The low ratios for shell A (O/ Fe of 1.5 and Ne/ Fe of 0.2) and the high ratios for shell B (O/ Fe of 30-130 and Ne/ Fe of 8-16) are consistent with Type Ia and Type II origins, respectively. The difference between the SNR progenitor types casts some doubt on the suggestion that these SNRs are interacting with one another. Subject headingg s: ISM: individual ( DEM L316) -supernova remnants -X-rays: ISM

show abstract

“…Taking advantage of these properties of the LMC, we have begun a systematic study of SNRs in the Magellanic Clouds. In previous work, we have made multiwavelength studies of the colliding remnants DEM L 316 (Williams et al 1997, hereafter Paper I) and for two SNRs, N11L and N86, which show breakout structures (Williams et al 1999, hereafter Paper II).…”

Section: Introductionmentioning

confidence: 99%

Supernova Remnants in the Magellanic Clouds. III. An X‐Ray Atlas of Large Magellanic Cloud Supernova Remnants

Williams

Chu

Dickel

et al. 1999

ASTROPHYS J SUPPL S

Self Cite

View full text Add to dashboard Cite

We have used archival ROSAT data to present X-ray images of 31 supernova remnants (SNRs) in the Large Magellanic Cloud (LMC). We have classiÐed these remnants according to their X-ray morphologies, into the categories of shell-type, di †use face, centrally brightened, point-sourceÈdominated, and irregular. We suggest possible causes of the X-ray emission for each category and for individual features of some of the SNRs.

show abstract

Supernova Remnants in the Magellanic Clouds. I. The Colliding Remnants DEM L316

Cited by 39 publications

References 23 publications

Is the Cygnus Loop two supernova remnants?

Is the Cygnus Loop two supernova remnants?

Supernova Remnants in the Magellanic Clouds. VI. The DEM L316 Supernova Remnants

Supernova Remnants in the Magellanic Clouds. III. An X‐Ray Atlas of Large Magellanic Cloud Supernova Remnants

Contact Info

Product

Resources

About