Supernova remnants in the Magellanic Clouds

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

doi:10.1086/190952

Cited by 65 publications

(85 citation statements)

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“…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

156

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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%

“…SNR B0538−69.3: the first classification as an SNR dates back to Mathewson et al (1984), based on radio and weak optical evidence. BMD10 included that source with the wrong J2000 coordinates.…”

Section: Cleaning the Sample: Objects Not Includedmentioning

confidence: 99%

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

Maggi

Haberl

Kavanagh

et al. 2016

A&A

156

205

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“…The complex nebulae SNR B0050−72.8 was identified as a SNR by Mathewson et al (1984) and Mills et al (1982) based on optical and radio-continuum (MOST) detections. They suggest this remnant has a steep (non-thermal) radio-continuum spectrum and is most likely an older SNR since it has a diameter of ∼57 pc.…”

Section: The Smc Snr B0050−728 (Dem S68; Hfpk 285; J005240-723820)mentioning

confidence: 99%

“…SNRs and SNR candidates in the SMC. The radio spectral index (α) is taken from Filipović et al (2005) Payne et al 2007;van der Heyden et al 2004;Dickel et al 2001;Mathewson et al 1984;Mills et al 1982;Hughes & Smith 1994;Nazé et al 2004, and references therein). Thirteen of the remnants were covered by early XMM-Newton observations and a comprehensive study was presented by van der Heyden et al (2004).…”

Section: Introductionmentioning

confidence: 99%

New XMM-Newton observations of supernova remnants in the Small Magellanic Cloud

Filipović

Haberl

Winkler³

et al. 2008

A&A

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Context. A complete overview of the supernova remnant (SNR) population is required to investigate their evolution and interaction with the surrounding interstellar medium in the Small Magellanic Cloud (SMC). Aims. Recent XMM-Newton observations of the SMC cover three known SNRs (DEM S5, SNR B0050−72.8, and SNR B0058−71.8), which are poorly studied and are X-ray faint. We used new multi-frequency radio-continuum surveys and new optical observations at H α , [S ii], and [O iii] wavelengths, in combination with the X-ray data, to investigate their properties and to search for new SNRs in the SMC. Methods. We used X-ray source selection criteria and found one SMC object with typical SNR characteristics (HFPK 334), that was initially detected by ROSAT. We analysed the X-ray spectra and present multi-wavelength morphological studies of the three SNRs and the new candidate. Results. Using a non-equilibrium ionisation collisional plasma model, we find temperatures kT around 0.18 keV for the three known remnants and 0.69 keV for the candidate. The low temperature, low surface brightness, and large extent of the three remnants indicates relatively large ages. The emission from the new candidate (HFPK 334) is more centrally peaked and the higher temperature suggests a younger remnant. Our new radio images indicate that a pulsar wind nebulae (PWN) is possibly associated with this object. Conclusions. The SNRs known in the SMC show a variety of morphological structures that are relatively uncorrelated in the different wavelength bands, probably caused by the different conditions in the surrounding medium with which the remnant interacts.

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“…These studies found that the majority of SMC SNRs are likely in the Sedov-adiabatic phase of evolution. IKT 16 was discovered as a candidate supernova remnant in the SMC by Inoue et al (1983) using Einstein, and its identity as a shell-type SNR was confirmed through radio and Hα analysis (Mathewson et al 1984). VDH04 included this remnant as part of their study of SMC SNRs.…”

Section: Introductionmentioning

confidence: 99%

IKT 16: a composite supernova remnant in the Small Magellanic Cloud

Owen

Filipović

Ballet

et al. 2011

A&A

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Aims. IKT 16 is an X-ray and radio-faint supernova remnant (SNR) in the Small Magellanic Cloud (SMC). A previous X-ray study of this SNR found a hard X-ray source near its centre. Using all available archival and proprietary XMM-Newton data, alongside new multi-frequency radio-continuum surveys and optical observations at Hα and forbidden [SII] and [OIII] lines, we aim to constrain the properties of the SNR and discover the nature of the hard source within. Methods. We combine XMM-Newton datasets to produce the highest quality X-ray image of IKT 16 to date. We use this, in combination with radio and optical images, to conduct a multi-wavelength morphological analysis of the remnant. We extract separate spectra from the SNR and the bright source near its centre, and conduct spectral fitting of both regions. Results. We find IKT 16 to have a radius of 37 ± 3 pc, with the bright source located 8 ± 2 pc from the centre. This is the largest known SNR in the SMC. The large size of the remnant suggests it is likely in the Sedov-adiabatic phase of evolution. Using a Sedov model to fit the SNR spectrum, we find an electron temperature kT of 1.03 ± 0.12 keV and an age of ≈14700 yr. The absorption found requires the remnant to be located deep within the SMC. The bright source is fit with a power law with index Γ = 1.58 ± 0.07, and is associated with diffuse radio emission extending towards the centre of the SNR. We argue that this source is likely to be the neutron star remnant of the supernova explosion, and infer its transverse kick velocity to be 580 ± 100 km s −1 . The X-ray and radio properties of this source strongly favour a pulsar wind nebula (PWN) origin.

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Supernova remnants in the Magellanic Clouds

Cited by 65 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

New XMM-Newton observations of supernova remnants in the Small Magellanic Cloud

IKT 16: a composite supernova remnant in the Small Magellanic Cloud

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