2004
DOI: 10.1086/423302
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Supernova Remnants in the Magellanic Clouds. IV. X‐Ray Emission from the Largest Supernova Remnant in the Large Magellanic Cloud

Abstract: 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… Show more

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Cited by 21 publications
(30 citation statements)
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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%
“…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%
“…For comparison, the luminosity functions for SNRs in the LMC and SMC are also shown in black and green, respectively. For the LMC, we used data from Williams et al (1999Williams et al ( , 2004, Haberl & Pietsch (1999), and Bamba et al (2006); for the SMC, we used Filipović et al (2008) and van der Heyden et al (2004). In all cases, we converted count rates to luminosities assuming simple thermal plasma models with kT of 0.6 keV and an absorbing N(H) of 5 × 10 20 cm −2 .…”
Section: Comparison With the Local Group Remnant Populationmentioning
confidence: 99%
“…The determined dimensions of MCSNR J0527−7104 of ∼5.1 × 4.0 (∼75 pc × 59 pc), make it comparable in size to large SNRs such as XMMU J0541.8−6659 (Grondin et al 2012). However, the MCSNR J0527−7104 is still smaller than the largest confirmed SNRs in the LMC such as SNR 0450−70.9 (Mathewson et al 1985;Williams et al 2004;Cajko et al 2009), LMC SNR J0550−6823 (Davies et al 1976;Filipovic et al 1998;Bozzetto et al 2012) and SNR0506-6542 (Klimek et al 2010). …”
Section: X-raysmentioning
confidence: 93%
“…By determining the physical characteristics of the hot gas in the SNR from X-ray spectral analysis, the age of the SNR could be inferred (see Maggi et al 2012, for example). Alternatively, optical echelle data could provide a measurement of the expansion velocity of the SNR shell, from which an age could be determined (see Williams et al 2004, for example). Given the propensity of high-mass stars to form in clusters, we can assess the likely supernova (SN) mechanism that produced MCSNR J0527−7104 based on the surrounding high-mass stellar population, or lack thereof.…”
Section: X-raysmentioning
confidence: 99%