Supernova remnants in the Magellanic Clouds

Mathewson, D. S.; Ford, V. L.; Dopita, Michael A.; Tuohy, I. R.; Long, Knox S.; Helfand, D. J.

doi:10.1086/190854

Cited by 197 publications

(191 citation statements)

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“…The survey with Einstein allowed Long et al (1981) to list 26 SNRs detected in X-rays, confirming many previously suggested candidates (based on optical or radio data). Mathewson et al (1983) provided a catalogue of 25 SNRs with radio, optical, and X-ray results. With more observations, Mills et al (1984) and Mathewson et al (1984Mathewson et al ( , 1985 increased the size of the sample to 32.…”

Section: Literature Surveymentioning

confidence: 99%

The population of X-ray supernova remnants in the Large Magellanic Cloud

Maggi

Haberl

Kavanagh

et al. 2016

A&A

146

205

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Aims. We present a comprehensive X-ray study of the population of supernova remnants (SNRs) in the Large Magellanic Cloud (LMC). Using primarily XMM-Newton observations, we conduct a systematic spectral analysis of LMC SNRs to gain new insight into their evolution and the interplay with their host galaxy. Methods. We combined all the archival XMM-Newton observations of the LMC with those of our Very Large Programme LMC survey. We produced X-ray images and spectra of 51 SNRs, out of a list of 59 objects compiled from the literature and augmented with newly found objects. Using a careful modelling of the background, we consistently analysed all the X-ray spectra and measure temperatures, luminosities, and chemical compositions. The locations of SNRs are compared to the distributions of stars, cold gas, and warm gas in the LMC, and we investigated the connection between the SNRs and their local environment, characterised by various star formation histories. We tentatively typed all LMC SNRs, in order to constrain the ratio of core-collapse to type Ia SN rates in the LMC. We also compared the column densities derived from X-ray spectra to H i maps, thus probing the three-dimensional structure of the LMC. Results. This work provides the first homogeneous catalogue of the X-ray spectral properties of SNRs in the LMC. It offers a complete census of LMC remnants whose X-ray emission exhibits Fe K lines (13% of the sample), or reveals the contribution from hot supernova ejecta (39%), which both give clues to the progenitor types. The abundances of O, Ne, Mg, Si, and Fe in the hot phase of the LMC interstellar medium are found to be between 0.2 and 0.5 times the solar values with a lower abundance ratio [α/Fe] than in the Milky Way. The current ratio of core-collapse to type Ia SN rates in the LMC is constrained to N CC /N Ia = 1.35( +0.11 −0.24 ), which is lower than in local SN surveys and galaxy clusters. Our comparison of the X-ray luminosity functions of SNRs in Local Group galaxies (LMC, SMC, M31, and M33) reveals an intriguing excess of bright objects in the LMC. Finally, we confirm that 30 Doradus and the LMC Bar are offset from the main disc of the LMC to the far and near sides, respectively.

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Section: Literature Surveymentioning

confidence: 99%

The population of X-ray supernova remnants in the Large Magellanic Cloud

Maggi

Haberl

Kavanagh

et al. 2016

A&A

146

205

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“…The main source of uncertainty in the measured flux densities is the definition of the area best representing the SNR, which dominates the statistical error. Based on different trials, we estimate that the combined flux density errors from all radio images used in this study (apart from 73 cm where the error is in order of 20%; Mathewson et al 1983;Clarke et al 1976), are ∼10% at each given frequency. Using the flux densities from Table 1, we estimated spectral indices for the PWN (α Core = −0.04 ± 0.04), the outer SNR shell excluding the core (α Shell = −0.43 ± 0.01), and the whole SNR (α Total = −0.39 ± 0.03); see Fig.…”

Section: Radio-continuummentioning

confidence: 99%

“…SNR J0453-6829 was initially classified as an SNR based on the Einstein X-Ray survey by Long et al (1981, source 1 in their catalogue) and Wang et al (1991, their source 2). Mathewson et al (1983) catalogued this object based on studies of optical and MOlonglo Synthesis Telescope (MOST) survey data, and reported an optical size of 140 × 131 . SNR J0453-6829 is also listed in the 408 MHz MC4 catalogue of Clarke et al (1976) as a distinctive pointlike radio source, for which Mathewson et al (1983) later remeasured a flux density of 350 mJy.…”

Section: Introductionmentioning

confidence: 99%

“…Mathewson et al (1983) catalogued this object based on studies of optical and MOlonglo Synthesis Telescope (MOST) survey data, and reported an optical size of 140 × 131 . SNR J0453-6829 is also listed in the 408 MHz MC4 catalogue of Clarke et al (1976) as a distinctive pointlike radio source, for which Mathewson et al (1983) later remeasured a flux density of 350 mJy. Mills et al (1984) detected this source with specific MOST pointings and reported a rather flat spectral index of α = −0.38.…”

Section: Introductionmentioning

confidence: 99%

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Multi-frequency observations of SNR J0453–6829 in the LMC

Haberl

Filipović

Bozzetto

et al. 2012

A&A

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Context. The Large Magellanic Cloud (LMC) is rich in supernova remnants (SNRs), which can be investigated in detail with radio, optical, and X-ray observations. SNR J0453-6829 is an X-ray and radio-bright remnant in the LMC, within which previous studies revealed the presence of a pulsar wind nebula (PWN), making it one of the most interesting SNRs in the Local Group of galaxies. Aims. We study the emission of SNR J0453-6829 to improve our understanding of its morphology, spectrum, and thus the emission mechanisms in the shell and the PWN of the remnant. Methods. We obtained new radio data with the Australia Telescope Compact Array and analysed archival XMM-Newton observations of SNR J0453-6829. We studied the morphology of SNR J0453-6829 from radio, optical, and X-ray images and investigated the energy spectra in the different parts of the remnant. Results. Our radio results confirm that this LMC SNR hosts a typical PWN. The prominent central core of the PWN exhibits a radio spectral index α Core of −0.04 ± 0.04, while in the rest of the SNR shell the spectral slope is somewhat steeper with α Shell = −0.43 ± 0.01. We detect regions with a mean polarisation of P (12 ± 4)% at 6 cm and (9 ± 2)% at 3 cm. The full remnant is of roughly circular shape with dimensions of (31 ± 1) pc × (29 ± 1) pc. The spectral analysis of the XMM-Newton EPIC and RGS spectra allowed us to derive physical parameters for the SNR. Somewhat depending on the spectral model, we obtain for the remnant a shock temperature of around 0.2 keV and estimate the dynamical age to 12 000-15 000 years. Using a Sedov model we further derive an electron density in the X-ray emitting material of 1.56 cm −3 , typical for LMC remnants, a large swept-up mass of 830 M , and an explosion energy of 7.6 × 10 50 erg. These parameters indicate a well evolved SNR with an X-ray spectrum dominated by emission from the swept-up material.

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“…It is listed by Wang et al (1991) as a SNR. Mathewson et al (1983) designate it SNR 0520-69.4 and show an optical and X-ray image. Because of its identification with a nonstellar object, a finding chart is not given in this paper.…”

Section: Spectroscopy and Optical Identificationsmentioning

confidence: 99%

LMC stellar X-ray sources observed with ROSAT. 1: X-ray data and search for optical counterparts

Schmidtke

Cowley

Frattare

et al. 1994

PASP

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ABSTRACT. Observations of Einstein LMC X-ray point sources have been made with ROS AT s High-Resolution Imager to obtain accurate positions from which to search for optical counterparts. This paper is the first in a series reporting results of the ROS AT observations and subsequent optical observations. It includes the X-ray positions and fluxes, information about variability, optical finding charts for each source, a list of identified counterparts, and information about candidates which have been observed spectroscopically in each of the fields. Sixteen point sources were measured at a >3cr level, while 15 other sources were either extended or less significant detections. About 50% of the sources are serendipitous detections (not found in previous surveys). More than half of the X-ray sources are variable. Sixteen of the sources have been optically identified or confirmed: six with foreground cool stars, four with Seyfert galaxies, two with SNR in the LMC, and four with peculiar hot LMC stars. Presumably the latter are all binaries, although only one (CAL 83) has been previously studied in detail.

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Supernova remnants in the Magellanic Clouds

Cited by 197 publications

References 0 publications

The population of X-ray supernova remnants in the Large Magellanic Cloud

The population of X-ray supernova remnants in the Large Magellanic Cloud

Multi-frequency observations of SNR J0453–6829 in the LMC

LMC stellar X-ray sources observed with ROSAT. 1: X-ray data and search for optical counterparts

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