<i>XMM-Newton</i>study of 30 Doradus C and a newly identified MCSNR J0536−6913 in the Large Magellanic Cloud

Kavanagh, Patrick; Sasaki, M.; Bozzetto, L. M.; Filipović, Miroslav; Points, Sean; Maggi, Pierre; Haberl, F.

doi:10.1051/0004-6361/201424354

Cited by 35 publications

(55 citation statements)

References 66 publications

(134 reference 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: 94%

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

Maggi

Haberl

Kavanagh

et al. 2016

A&A

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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: 94%

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

Maggi

Haberl

Kavanagh

et al. 2016

A&A

Self Cite

156

205

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“…Detailed study of 30 Dor C superbubble with XMM-Newton was performed recently by Kavanagh et al (2014). Apart from the hard X-ray shell which is highly correlated with the H α and radio shells the non-thermal X-ray emission was detected from all regions of 30 Dor C as well.…”

Section: Non-thermal Emission From Globular Clusters and Superbubblesmentioning

confidence: 99%

“…The authors found that the non-thermal X-ray emission may be fitted with a power-law model but an exponential cut-off synchrotron model may fit the spectrum better. The maximal energy of electrons max which is required to justify the X-ray synchrotron model was estimated by Kavanagh et al (2014) as max ≈ 80 TeV (B/10µG) −1/2 . The synchrotron losses time of the electrons is below 1.5 kyrs and therefore efficient particle acceleration is required.…”

Section: Non-thermal Emission From Globular Clusters and Superbubblesmentioning

confidence: 99%

“…The synchrotron losses time of the electrons is below 1.5 kyrs and therefore efficient particle acceleration is required. Kavanagh et al (2014) argued that 30 Dor C is currently undergoing a phase of high energy particle acceleration by massive star winds and perhaps supernova remnants expanding in the hot superbubble. The maximal energy of the electrons might be somewhat lower than that derived by Kavanagh et al (2014) if one account for the effect of turbulent magnetic fields in the superbubble on the spectra of the synchrotron radiation .…”

Section: Non-thermal Emission From Globular Clusters and Superbubblesmentioning

confidence: 99%

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Nonthermal particles and photons in starburst regions and superbubbles

Bykov

2014

Astron Astrophys Rev

118

102

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Starforming factories in galaxies produce compact clusters and loose associations of young massive stars. Fast radiation-driven winds and supernovae input their huge kinetic power into the interstellar medium in the form of highly supersonic and superalfvenic outflows. Apart from gas heating, collisionless relaxation of fast plasma outflows results in fluctuating magnetic fields and energetic particles. The energetic particles comprise a long-lived component which may contain a sizeable fraction of the kinetic energy released by the winds and supernova ejecta and thus modify the magnetohydrodynamic flows in the systems. We present a concise review of observational data and models of nonthermal emission from starburst galaxies, superbubbles, and compact clusters of massive stars. Efficient mechanisms of particle acceleration and amplification of fluctuating magnetic fields with a wide dynamical range in starburst regions are discussed. Sources of cosmic rays, neutrinos and multi-wavelength nonthermal emission associated with starburst regions including potential galactic "PeVatrons" are reviewed in the global galactic ecology context.

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“…However, this number has been steadily increasing in recent years because of improved observation sensitivity and/or multi-wavelength confirmation of candidates. Recent additions include Kavanagh et al (2013Kavanagh et al ( , 2015, Bozzetto et al (2014), and Maggi et al (2014). Bozzetto et al (2013, hereafter BF13) used radio observations by the Australia Telescope Compact Array (ATCA) A&A 579, A63 (2015) The image is overlaid with 6 cm (5500 MHz) contours with levels corresponding to 3, 6, 9, 12, and 15σ (from BF13, Fig.…”

Section: Introductionmentioning

confidence: 99%

XMM-Newtonobservation of SNR J0533–7202 in the Large Magellanic Cloud

Kavanagh

Sasaki

Whelan

et al. 2015

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Aims. We present an X-ray study of the supernova remnant SNR J0533−7202 in the Large Magellanic Cloud (LMC) and determine its physical characteristics based on its X-ray emission. Methods. We observed SNR J0533−7202 with XMM-Newton (background flare-filtered exposure times of 18 ks EPIC-pn and 31 ks EPIC-MOS1, EPIC-MOS2). We produced X-ray images of the supernova remnant, performed an X-ray spectral analysis, and compared the results to multi-wavelength studies.Results. The distribution of X-ray emission is highly non-uniform, with the south-west region much brighter than the north-east. The detected X-ray emission is correlated with the radio emission from the remnant. We determine that this morphology is most likely due to the supernova remnant expanding into a non-uniform ambient medium and not an absorption effect. We estimate the remnant size to be 53.9 (±3.4) × 43.6 (±3.4) pc, with the major axis rotated ∼64• east of north. We find no spectral signatures of ejecta emission and infer that the X-ray plasma is dominated by swept up interstellar medium. Using the spectral fit results and the Sedov self-similar solution, we estimate the age of SNR J0533−7202 to be ∼17−27 kyr, with an initial explosion energy of (0.09−0.83) × 10 51 erg. We detected an X-ray source located near the centre of the remnant, namely XMMU J053348.2−720233. The source type could not be conclusively determined due to the lack of a multi-wavelength counterpart and low X-ray counts. We found that it is likely either a background active galactic nucleus or a low-mass X-ray binary in the LMC. Conclusions. We detected bright thermal X-ray emission from SNR J0533−7202 and determined that the remnant is in the Sedov phase of its evolution. The lack of ejecta emission prohibits us from typing the remnant with the X-ray data. Therefore, the likely Type Ia classification based on the local stellar population and star formation history reported in the literature cannot be improved upon.

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XMM-Newtonstudy of 30 Doradus C and a newly identified MCSNR J0536−6913 in the Large Magellanic Cloud

Cited by 35 publications

References 66 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

Nonthermal particles and photons in starburst regions and superbubbles

XMM-Newtonobservation of SNR J0533–7202 in the Large Magellanic Cloud

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