Supernova remnants in the Magellanic Clouds. III

Mathewson, D. S.; Ford, V. L.; Tuohy, I.; Mills, B. Y.; Turtle, A. J.; Helfand, D. J.

doi:10.1086/191037

Cited by 89 publications

(125 citation statements)

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“…Its nature as a superbubble rather than a standard SNR was already recognised by Mathewson et al (1985). It was however listed as an SNR in Blair et al (2006, Kavanagh et al 2015a), but it was revealed only later and is most likely distinct from the non-thermal shell.…”

Section: Cleaning the Sample: Objects Not Includedmentioning

confidence: 95%

“…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. In the 1990s, several new SNRs were discovered with ROSAT pointed observations (Chu et al 1993(Chu et al , 2000Smith et al 1994), sometimes aided by optical spectroscopy (Chu et al 1995(Chu et al , 1997.…”

Section: Literature Surveymentioning

confidence: 99%

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

Maggi

Haberl

Kavanagh

et al. 2016

A&A

149

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: Cleaning the Sample: Objects Not Includedmentioning

confidence: 95%

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

149

205

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“…In the field of RX J0536.0-6735 (CAL 60) note the faint ring of nebulosity almost filling the image and nearly centered on the X-ray position. This is part of the SNR DEM 241 (Mathewson et al 1985). Since the source is variable, some stars have also been observed in this field.…”

Section: Spectroscopy and Optical Identificationsmentioning

confidence: 97%

“…Mathewson et al (1985) concluded that CAL 60 was associated with the supernova remnant DEM 241. There is a faint ring of emission visible on our finding chart.…”

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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“…Theoretical models of hot gas in SNRs of ages 10 5 -10 6 yr (e.g., Slavin & Cox 1992, 1993Shelton 1999) cannot be compared easily with observations because few evolved SNRs are known and they are expected to be faint and difficult to observe. SNR 0450À70.9 ( Mathewson et al 1985) is the largest known remnant in the Large Magellanic Cloud ( LMC). Its optical extent of 6A5 ; 4A7 corresponds to 98 ; 70 pc at the LMC distance of 50 kpc ( Feast 1999).…”

Section: Introductionmentioning

confidence: 99%

Supernova Remnants in the Magellanic Clouds. IV. X‐Ray Emission from the Largest Supernova Remnant in the Large Magellanic Cloud

Williams¹,

Chu²,

Dickel³

et al. 2004

ApJ

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We present the first X-ray detection of SNR 0450À70.9, the largest known supernova remnant (SNR) in the Large Magellanic Cloud. To study the physical conditions of this SNR, we have obtained XMM-Newton X-ray observations, optical images and high-dispersion spectra, and radio continuum maps. Optical images of SNR 0450À70.9 show a large, irregular elliptical shell with bright filaments along the eastern and western rims and within the shell interior. The interior filaments have higher [S ii]/H ratios and form an apparent inner shell morphology. The X-ray emission region is smaller than the full extent of the optical shell, with the brightest X-ray emission found within the small interior shell and on the western rim of the large shell. The expansion velocity of the small shell is $220 km s À1 , while that of the large shell is $120 km s À1 . The radio image shows central brightening and a fairly flat radio spectral index over the SNR. However, no point X-ray or radio source corresponding to a pulsar is detected, and the X-ray emission is predominantly thermal. Therefore, these phenomena can be most reasonably explained in terms of the advanced age of the large SNR. Using hydrodynamic models combined with a nonequilibrium ionization model for thermal X-ray emission, we derived a lower limit on the SNR age of~45,000 yr, well into the later stages of SNR evolution. Despite this, the temperature and density derived from spectral fits to the X-ray emission indicate that the remnant is still overpressured and thus that the development is largely driven by hot gas in the SNR interior. Subject headingg s: ISM: individual (SNR 0450À70.9) -Magellanic Clouds -supernova remnants -X-rays: ISM

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Supernova remnants in the Magellanic Clouds. III

Cited by 89 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

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

Supernova Remnants in the Magellanic Clouds. IV. X‐Ray Emission from the Largest Supernova Remnant in the Large Magellanic Cloud

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