Radio properties of three young supernova remnants in the Large Magellanic Cloud

Dickel, John R.; Milne, D. K.

doi:10.1086/117266

Cited by 50 publications

(61 citation statements)

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“…1d).ÈThis young, Balmer-lineÈdominated SNR has a shell structure with an apparent gap to the southeast. The X-ray morphology is similar to that in radio images (Dickel & Milne 1995), although the gap is not as strongly deÐned in radio. This SNR has a shock velocity in the range of 1000È1900 km s~1 (Smith et al 1991), suggesting it is one of the younger LMC remnants.…”

Section: Appendix a Individual Snr Properties And Referencessupporting

confidence: 55%

“…1c).ÈAlthough Mathewson et al (1983) classiÐed N103B as having centrally concentrated X-ray emission, an examination at higher resolution and sensitivity suggests that the remnant is in fact shell-type and that the brighter X-ray region is not central but in fact is located near the limb of the SNR. This o †set is easier to see in the radio images (Dickel & Milne 1995), which show a well-deÐned shell brightened to the west. A study by Hughes et al (1995) suggests that this SNR, although not Balmer-lineÈdominated at optical wavelengths, is nonetheless the result of a Type Ia SN explosion, based on characteristic lines in the X-ray spectra.…”

Section: Appendix a Individual Snr Properties And Referencesmentioning

confidence: 93%

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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

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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.

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Section: Appendix a Individual Snr Properties And Referencessupporting

confidence: 55%

Section: Appendix a Individual Snr Properties And Referencesmentioning

confidence: 93%

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

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“…Outside the fast-moving material is a bright x-ray shell (Long et al 1981;Mathewson et al 1983) that is associated with an optical emission line rim (Hughes 1994;Blair et al 1994) of radius ∼ 1 arcminute (∼ 13 parsecs). Dickel & Milne (1995) observed 6 centimeter radio emission that coincides with the x-ray shell. Blair et al (2000) found that the abundances derived for the ejecta in N132D roughly match models of a star with an initial mass of 35 M ⊙ with the following condition: the O-rich mantle of the progenitor star did not mix with deeper O-burning layers.…”

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confidence: 89%

Cosmic Origins Spectrograph Observations of the Chemical Composition of SNR LMC N132d

France¹,

Beasley²,

Keeney³

et al. 2009

ApJ

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We present new far-ultraviolet spectra of an oxygen-rich knot in the Large Magellanic Cloud supernova remnant N132D, obtained with the Hubble Space T elescope-Cosmic Origins Spectrograph. Moderate resolution (∆v ≈ 200 km s −1 ) spectra in the HST far-ultraviolet bandpass (1150 λ 1750Å) show emission from several ionization states of oxygen as well as trace amounts of other species. We use the improvements in sensitivity and resolving power offered by COS to separate contributions from different velocity components within the remnant, as well as emission from different species within the oxygen-rich knot itself. This is the first time that compositional and velocity structure in the ultraviolet emission lines from N132D has been resolved, and we use this to assess the chemical composition of the remnant. No nitrogen is detected in N132D and multiple carbon species are found at velocities inconsistent with the main oxygen component. We find helium and silicon to be associated with the oxygen-rich knot, and use the reddening-corrected line strengths of O III], O IV], O V, and Si IV to constrain the composition and physical characteristics of this oxygen-rich knot. We find that models with a silicon-to-oxygen abundance ratio of N (Si)/N (O) = 10 −2 can reproduce the observed emission for a shock velocity of ≈ 130 km s −1 , implying a mass of ∼ 50 M ⊙ for the N132D progenitor star.

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“…FIGURE 1. Plot of X-ray image with 2.5 cm ATCA contours [1]. Contours are 1.7, 1.3, 0.9, 0.6, 0.3, and 0.1 mJy/beam.…”

Section: Analysis and Resultsmentioning

confidence: 99%

“…[1] The radio and X-ray morphologies are strikingly similar; the western edge (near the HII region) shows considerable structure and is ∼ 3 times brighter than the eastern edge. [1,2] In both bands, the emission arises from a region 7 pc in diameter (d=50kpc to LMC assumed). Due to its proximity to a star forming region, it was originally suspected that N103B was the result of the core collapse of a massive object.…”

Section: Introductionmentioning

confidence: 94%

Exploring the small scale structure of N103B

Lewis¹

2001

AIP Conference Proceedings

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Abstract. We present the preliminary results of a 40.8 ks Chandra ACIS observation of the young supernova remnant (SNR) N103B located in the Large Magellanic Cloud. The image reveals structure at the sub-arcsecond level, including several bright knots and filamentary structures. The remnant has the characteristic spectrum of a Type Ia SNR, containing strong lines of Fe, He-and H-like Si and S, Ar, and Ca. Narrow band images reveal non-uniformities in the remnant.

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Radio properties of three young supernova remnants in the Large Magellanic Cloud

Cited by 50 publications

References 0 publications

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

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

Cosmic Origins Spectrograph Observations of the Chemical Composition of SNR LMC N132d

Exploring the small scale structure of N103B

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