Multifrequency observations of one of the largest supernova remnants in the local group of galaxies, LMC - SNR J0450-709

Čajko, Kristina O.; Crawford, E. J.; Filipović, Miroslav

doi:10.2298/saj0979055c

Cited by 27 publications

(26 citation statements)

References 20 publications

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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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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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“…While this is the largest confirmed SNR in the SMC there are several larger cousins in the Large Magellanic Cloud (LMC) (Cajko et al 2009;Klimek et al 2010). The radio emission from the SNR is also found to be faint (32 mJy at 1400 MHz; Table 2).…”

Section: Properties Of the Snrmentioning

confidence: 90%

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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“…Using the flux density measurements shown in Table 2, we estimated a radio spectral index for DEM L299 of α = −0.34 ± 0.03. More information on the observing procedure and other sources observed in this session/project can be found in Bojičić et al (2007), Crawford et al (2008aCrawford et al ( ,b, 2010, Cajko et al (2009), de Horta et al (2012, Grondin et al (2012), Haberl et al (2012), Maggi et al (2012), Kavanagh et al (2013), and Bozzetto et al (2010Bozzetto et al ( , 2012aBozzetto et al ( ,b,c,d, 2013.…”

Section: Radio-continuum Datamentioning

confidence: 99%

Multi-frequency study of DEM L299 in the Large Magellanic Cloud

Warth

Sasaki

Kavanagh

et al. 2014

A&A

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Aims. We have studied the H ii region DEM L299 in the Large Magellanic Cloud (LMC) to understand its physical characteristics and morphology in different wavelengths. Methods. We performed a spectral analysis of archived XMM-Newton EPIC data and studied the morphology of DEM L299 in X-ray, optical, and radio wavelengths. We used Hα, [S ii], and [O iii] data from the Magellanic Cloud Emission Line Survey (MCELS) and radio 21 cm line data from the Australia Telescope Compact Array (ATCA) and the Parkes Telescope as well as radio continuum data (3 cm, 6 cm, 20 cm, 36 cm) from ATCA and from the Molonglo Synthesis Telescope (MOST). Results. Our morphological studies imply that, in addition to the supernova remnant SNR B0543-68.9 reported in previous studies, a superbubble also overlaps the SNR in projection. The position of the SNR is clearly defined through the [S ii]/Hα flux ratio image.Moreover, the optical images show a shell-like structure that is located farther to the north and is filled with diffuse X-ray emission, which again indicates the superbubble. Radio 21 cm line data show a shell around both objects. Radio continuum data show diffuse emission at the position of DEM L299, which appears clearly distinguished from the H ii region LHA 120-N 164 that lies south-west of it. We determined the spectral index of SNR B0543-68.9 to be α = −0.34, which indicates the dominance of thermal emission and therefore a rather mature remnant. We determined the basic properties of the diffuse X-ray emission for the SNR, the superbubble, and a possible blowout region of the bubble, as suggested by the optical and X-ray data. We obtained an age of (8.9 +9.2 −5.4 ) kyr for the SNR and a temperature of (0.64 +0.73 −0.20 ) keV for the hot gas inside the SNR, as well as a thermal energy content and temperature of the hot gas inside the superbubble of (4.3 +8.1 −2.6 ) × 10 50 φ 0.5 erg and (0.74 +0.36 −0.30 ) keV, with φ being the gas-filling factor. Conclusions. We conclude that DEM L299 consists of a superposition of SNR B0543-68.9 and a superbubble, which we identified based on optical data.

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Multifrequency observations of one of the largest supernova remnants in the local group of galaxies, LMC - SNR J0450-709

Cited by 27 publications

References 20 publications

Multi-frequency study of Local Group supernova remnants

Multi-frequency study of Local Group supernova remnants

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

Multi-frequency study of DEM L299 in the Large Magellanic Cloud

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