A detailed observation of a LMC supernova remnant DEM L241 with<i>XMM-Newton</i>

Bamba, Aya; Ueno, Masaru; Nakajima, Hiroshi; Mori, Koji; Koyama, K.

doi:10.1051/0004-6361:20054096

Cited by 27 publications

(42 citation statements)

References 42 publications

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“…Given a lack of plerionic remnants in the SMC we can use the LMC for comparison. PWN containing remnants in the LMC typically have a lower index: α = 1.0 ± 0.2 in SNR 0453-68. for DEM L241 (Bamba et al 2006); and α ∼ 1.2 − 1.6 over several regions from N 157B (Chen et al 2006). At SMC distance the calculated luminosity would be consistent with that expected expected from a PWN.…”

Section: X-raysupporting

confidence: 79%

HFPK 334: An Unusual Supernova Remnant in the Small Magellanic Cloud

Crawford

Filipović

McEntaffer

et al. 2014

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We present new Australia Telescope Compact Array (ATCA) radio-continuum and XMM-Newton/Chandra X-ray Observatory (CXO) observations of the unusual supernova remnant HFPK 334 in the Small Magellanic Cloud (SMC). The remnant follows a shell type morphology in the radio-continuum and has a size of ∼20 pc at the SMC distance. The X-ray morphology is similar, however, we detect a prominent point source close to the center of the SNR exhibiting a spectrum with a best fit powerlaw with a photon index of Γ = 2.7 ± 0.5. This central point source is most likely a background object and cannot be directly associated with the remnant. The high temperature, nonequilibrium conditions in the diffuse region suggest that this gas has been recently shocked and point toward a younger SNR with an age of 1800 years. With an average radio spectral index of α = −0.59 ± 0.09 we find that an equipartition magnetic field for the remnant is ∼90 µG, a value typical of younger SNRs in lowdensity environments. Also, we report detection of scattered radio polarisation across the remnant at 20 cm, with a peak fractional polarisation level of 25±5%.

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Section: X-raysupporting

confidence: 79%

HFPK 334: An Unusual Supernova Remnant in the Small Magellanic Cloud

Crawford

Filipović

McEntaffer

et al. 2014

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“…Considering its large extent and low surface brightness, it is most likely an older remnant. The low temperature is similar to 3 SMC SNRs (van der Heyden et al 2004;Filipović et al 2008), and cooler than any known bright LMC SNR (Williams et al 2004;Williams & Chu 2005;Borkowski et al 2006;Bamba et al 2006). …”

Section: X-raymentioning

confidence: 56%

Multi-frequency study of Local Group supernova remnants

Crawford

Filipović

Haberl

et al. 2010

A&A

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Context. The SNRs known in the Local Group show a variety of morphological structures that are relatively uncorrelated in the different wavelength bands. This variety is probably caused by the different conditions in the surrounding medium with which the remnant interacts. Aims. Recent ATCA, XMM-Newton and MCELS observations of the Magellanic Clouds (MCs) cover a number of new and known SNRs which are poorly studied, such as SNR J0528-6714. This particular SNR exhibits luminous radio-continuum emission, but is one of the unusual and rare cases without detectable optical and very faint X-ray emission (initially detected by ROSAT and listed as object [HP99] 498). We used new multi-frequency radio-continuum surveys and new optical observations at Hα, [S ii] and [O iii]wavelengths, in combination with XMM-Newton X-ray data, to investigate the SNR properties and to search for a physical explanation for the unusual appearance of this SNR. Methods. We analysed the X-ray and Radio-Continuum spectra and present multi-wavelength morphological studies of this SNR. Results. We present the results of new moderate resolution ATCA observations of SNR J0528-6714. We found that this object is a typical older SNR with a radio spectral index of α = −0.36 ± 0.09 and a diameter of D = 52.4 ± 1.0 pc. Regions of moderate and somewhat irregular polarisation were detected which are also indicative of an older SNR. Using a non-equilibrium ionisation collisional plasma model to describe the X-ray spectrum, we find temperatures kT of 0.26 keV for the remnant. The low temperature, low surface brightness, and large extent of the remnant all indicate a relatively advanced age. The near circular morphology indicates a type Ia event. Conclusions. Our study revealed one of the most unusual cases of SNRs in the Local Group of galaxies -a luminous radio SNR without optical counterpart and, at the same time, very faint X-ray emission. While it is not unusual to not detect an SNR in the optical, the combination of faint X-ray and no optical detection makes this SNR very unique.

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“…The observation times correspond to phases of ∼0.17 and ∼0.26 and the flux increase is thus consistent with the behavior we observe at these phases with the Swift XRT. However, the XMM observation of Bamba et al (2006) was obtained at a phase of ∼0.6 which corresponds to orbital maximum but did not show a particularly high flux. This could be indicative of cycleto-cycle variability if confirmed by additional observa- …”

Section: Comparison With Previous X-ray Observationsmentioning

confidence: 93%

A Luminous Gamma-Ray Binary in the Large Magellanic Cloud

Corbet

Chomiuk

Coe

et al. 2016

ApJ

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Gamma-ray binaries consist of a neutron star or a black hole interacting with a normal star to produce gamma-ray emission that dominates the radiative output of the system. Only a handful of such systems have been previously discovered, all within our Galaxy. Here we report the discovery with the Fermi Large Area Telescope (LAT) of a luminous gamma-ray binary in the Large Magellanic Cloud from a search for periodic modulation in all sources in the third Fermi LAT catalog. This is the first such system to be found outside the Milky Way. The system has an orbital period of 10.3 days and is associated with a massive O5III star located in the supernova remnant DEM L241, previously identified as the candidate high-mass X-ray binary (HMXB) CXOU J053600.0-673507. X-ray and radio emission are also modulated on the 10.3 day period, but are in anti-phase with the gamma-ray modulation. Optical radial velocity measurements suggest that the system contains a neutron star. The source is significantly more luminous than similar sources in the Milky Way at radio, optical, X-ray and gamma-ray wavelengths. The detection of this extra-galactic system, but no new Galactic systems raises the possibility that the predicted number of gamma-ray binaries in our Galaxy have been overestimated, and that HMXBs may be born containing relatively slowly rotating neutron stars.

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A detailed observation of a LMC supernova remnant DEM L241 withXMM-Newton

Cited by 27 publications

References 42 publications

HFPK 334: An Unusual Supernova Remnant in the Small Magellanic Cloud

HFPK 334: An Unusual Supernova Remnant in the Small Magellanic Cloud

Multi-frequency study of Local Group supernova remnants

A Luminous Gamma-Ray Binary in the Large Magellanic Cloud

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