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class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.16533">arXiv:2310.16533</a> <span> [<a href="https://arxiv.org/pdf/2310.16533">pdf</a>, <a href="https://arxiv.org/format/2310.16533">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad3300">10.1093/mnras/stad3300 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ATCA Study of Small Magellanic Cloud Supernova Remnant 1E 0102.2-7219 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Alsaberi%2C+R+Z+E">Rami Z. E. Alsaberi</a>, <a href="/search/?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/?searchtype=author&query=Dai%2C+S">S. Dai</a>, <a href="/search/?searchtype=author&query=Sano%2C+H">H. Sano</a>, <a href="/search/?searchtype=author&query=Kothes%2C+R">R. Kothes</a>, <a href="/search/?searchtype=author&query=Payne%2C+J+L">J. L. Payne</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/?searchtype=author&query=Collischon%2C+C">C. Collischon</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Hill%2C+T">T. Hill</a>, <a href="/search/?searchtype=author&query=Kavanagh%2C+P+J">P. J. Kavanagh</a>, <a href="/search/?searchtype=author&query=Knies%2C+J">J. Knies</a>, <a href="/search/?searchtype=author&query=Leahy%2C+D">D. Leahy</a>, <a href="/search/?searchtype=author&query=Macgregor%2C+P+J">P. J. Macgregor</a>, <a href="/search/?searchtype=author&query=Maggi%2C+P">P. Maggi</a>, <a href="/search/?searchtype=author&query=Maitra%2C+C">C. Maitra</a>, <a href="/search/?searchtype=author&query=Manojlovi%C4%87%2C+P">P. Manojlovi膰</a>, <a href="/search/?searchtype=author&query=Mart%C3%ADn%2C+S">S. Mart铆n</a>, <a href="/search/?searchtype=author&query=Matthew%2C+C">C. Matthew</a>, <a href="/search/?searchtype=author&query=Ralph%2C+N+O">N. O. Ralph</a>, <a href="/search/?searchtype=author&query=Rowell%2C+G">G. Rowell</a>, <a href="/search/?searchtype=author&query=Ruiter%2C+A+J">A. J. Ruiter</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.16533v1-abstract-short" style="display: inline;"> We present new and archival Australia Telescope Compact Array and Atacama Large Millimeter/submillimeter Array data of the Small Magellanic Cloud supernova remnant 1E 0102.2-7219 at 2100, 5500, 9000, and 108000 MHz; as well as Hi data provided by the Australian Square Kilometre Array Pathfinder. The remnant shows a ring-like morphology with a mean radius of 6.2 pc. The 5500 MHz image reveals a bri… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.16533v1-abstract-full').style.display = 'inline'; document.getElementById('2310.16533v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.16533v1-abstract-full" style="display: none;"> We present new and archival Australia Telescope Compact Array and Atacama Large Millimeter/submillimeter Array data of the Small Magellanic Cloud supernova remnant 1E 0102.2-7219 at 2100, 5500, 9000, and 108000 MHz; as well as Hi data provided by the Australian Square Kilometre Array Pathfinder. The remnant shows a ring-like morphology with a mean radius of 6.2 pc. The 5500 MHz image reveals a bridge-like structure, seen for the first time in a radio image. This structure is also visible in both optical and X-ray images. In the 9000 MHz image we detect a central feature that has a flux density of 4.3 mJy but rule out a pulsar wind nebula origin, due to the lack of significant polarisation towards the central feature with an upper limit of 4 per cent. The mean fractional polarisation for 1E 0102.2-7219 is 7 +- 1 and 12 +- 2 per cent for 5500 and 9000 MHz, respectively. The spectral index for the entire remnant is -0.61 +- 0.01. We estimate the line-of-sight magnetic field strength in the direction of 1E 0102.2-7219 of ~44 microG with an equipartition field of 65 +- 5 microG. This latter model, uses the minimum energy of the sum of the magnetic field and cosmic ray electrons only. We detect an Hi cloud towards this remnant at the velocity range of ~160-180 km s-1 and a cavity-like structure at the velocity of 163.7-167.6 km s-1. We do not detect CO emission towards 1E 0102.2-7219. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.16533v1-abstract-full').style.display = 'none'; document.getElementById('2310.16533v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.05090">arXiv:2210.05090</a> <span> [<a href="https://arxiv.org/pdf/2210.05090">pdf</a>, <a href="https://arxiv.org/format/2210.05090">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac2922">10.1093/mnras/stac2922 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New ASKAP Radio Supernova Remnants and Candidates in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">Luke M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Filipovi%C4%87%2C+M+D">Miroslav D. Filipovi膰</a>, <a href="/search/?searchtype=author&query=Sano%2C+H">H. Sano</a>, <a href="/search/?searchtype=author&query=Alsaberi%2C+R+Z+E">R. Z. E. Alsaberi</a>, <a href="/search/?searchtype=author&query=Barnes%2C+L+A">L. A. Barnes</a>, <a href="/search/?searchtype=author&query=Boji%C4%8Di%C4%87%2C+I+S">I. S. Boji膷i膰</a>, <a href="/search/?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/?searchtype=author&query=Chomiuk%2C+L">L. Chomiuk</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/?searchtype=author&query=Dai%2C+S">S. Dai</a>, <a href="/search/?searchtype=author&query=Ghavam%2C+M">M. Ghavam</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Hill%2C+T">T. Hill</a>, <a href="/search/?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/?searchtype=author&query=Jarrett%2C+T">T. Jarrett</a>, <a href="/search/?searchtype=author&query=Kavanagh%2C+P+J">P. J. Kavanagh</a>, <a href="/search/?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/?searchtype=author&query=Kothes%2C+R">R. Kothes</a>, <a href="/search/?searchtype=author&query=Leahy%2C+D">D. Leahy</a>, <a href="/search/?searchtype=author&query=Lenc%2C+E">E. Lenc</a>, <a href="/search/?searchtype=author&query=Leonidaki%2C+I">I. Leonidaki</a>, <a href="/search/?searchtype=author&query=Maggi%2C+P">P. Maggi</a>, <a href="/search/?searchtype=author&query=Maitra%2C+C">C. Maitra</a>, <a href="/search/?searchtype=author&query=Matthew%2C+C">C. Matthew</a> , et al. (12 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.05090v2-abstract-short" style="display: inline;"> We present a new Australian Square Kilometre Array Pathfinder (ASKAP) sample of 14 radio Supernova Remnant (SNR) candidates in the Large Magellanic Cloud (LMC). This new sample is a significant increase to the known number of older, larger and low surface brightness LMC SNRs. We employ a multi-frequency search for each object and found possible traces of optical and occasionally X-ray emission in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.05090v2-abstract-full').style.display = 'inline'; document.getElementById('2210.05090v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.05090v2-abstract-full" style="display: none;"> We present a new Australian Square Kilometre Array Pathfinder (ASKAP) sample of 14 radio Supernova Remnant (SNR) candidates in the Large Magellanic Cloud (LMC). This new sample is a significant increase to the known number of older, larger and low surface brightness LMC SNRs. We employ a multi-frequency search for each object and found possible traces of optical and occasionally X-ray emission in several of these 14 SNR candidates. One of these 14 SNR candidates (MCSNR J0522-6543) has multi-frequency properties that strongly indicate a bona fide SNR. We also investigate a sample of 20 previously suggested LMC SNR candidates and confirm the SNR nature of MCSNR J0506-6815. We detect lower surface brightness SNR candidates which were likely formed by a combination of shock waves and strong stellar winds from massive progenitors (and possibly surrounding OB stars). Some of our new SNR candidates are also found in a lower density environments in which SNe type Ia explode inside a previously excavated interstellar medium (ISM). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.05090v2-abstract-full').style.display = 'none'; document.getElementById('2210.05090v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for publication in MNRAS, this version corrects arXiv metadata only</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.10026">arXiv:2201.10026</a> <span> [<a href="https://arxiv.org/pdf/2201.10026">pdf</a>, <a href="https://arxiv.org/format/2201.10026">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac210">10.1093/mnras/stac210 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Mysterious Odd Radio Circle near the Large Magellanic Cloud -- An Intergalactic Supernova Remnant? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Filipovi%C4%87%2C+M+D">Miroslav D. Filipovi膰</a>, <a href="/search/?searchtype=author&query=Payne%2C+J+L">J. L. Payne</a>, <a href="/search/?searchtype=author&query=Alsaberi%2C+R+Z+E">R. Z. E. Alsaberi</a>, <a href="/search/?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/?searchtype=author&query=Macgregor%2C+P+J">P. J. Macgregor</a>, <a href="/search/?searchtype=author&query=Rudnick%2C+L">L. Rudnick</a>, <a href="/search/?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/?searchtype=author&query=Leahy%2C+D">D. Leahy</a>, <a href="/search/?searchtype=author&query=Ducci%2C+L">L. Ducci</a>, <a href="/search/?searchtype=author&query=Kothes%2C+R">R. Kothes</a>, <a href="/search/?searchtype=author&query=Andernach%2C+H">H. Andernach</a>, <a href="/search/?searchtype=author&query=Barnes%2C+L">L. Barnes</a>, <a href="/search/?searchtype=author&query=Boji%C4%8Di%C4%87%2C+I+S">I. S. Boji膷i膰</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/?searchtype=author&query=Collier%2C+J+D">J. D. Collier</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/?searchtype=author&query=Crocker%2C+R+M">R. M. Crocker</a>, <a href="/search/?searchtype=author&query=Dai%2C+S">S. Dai</a>, <a href="/search/?searchtype=author&query=Galvin%2C+T+J">T. J. Galvin</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Heber%2C+U">U. Heber</a>, <a href="/search/?searchtype=author&query=Hill%2C+T">T. Hill</a>, <a href="/search/?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/?searchtype=author&query=Hurley-Walker%2C+N">N. Hurley-Walker</a> , et al. (26 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.10026v1-abstract-short" style="display: inline;"> We report the discovery of J0624-6948, a low-surface brightness radio ring, lying between the Galactic Plane and the Large Magellanic Cloud (LMC). It was first detected at 888 MHz with the Australian Square Kilometre Array Pathfinder (ASKAP), and with a diameter of ~196 arcsec. This source has phenomenological similarities to Odd Radio Circles (ORCs). Significant differences to the known ORCs - a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.10026v1-abstract-full').style.display = 'inline'; document.getElementById('2201.10026v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.10026v1-abstract-full" style="display: none;"> We report the discovery of J0624-6948, a low-surface brightness radio ring, lying between the Galactic Plane and the Large Magellanic Cloud (LMC). It was first detected at 888 MHz with the Australian Square Kilometre Array Pathfinder (ASKAP), and with a diameter of ~196 arcsec. This source has phenomenological similarities to Odd Radio Circles (ORCs). Significant differences to the known ORCs - a flatter radio spectral index, the lack of a prominent central galaxy as a possible host, and larger apparent size - suggest that J0624-6948 may be a different type of object. We argue that the most plausible explanation for J0624-6948 is an intergalactic supernova remnant due to a star that resided in the LMC outskirts that had undergone a single-degenerate type Ia supernova, and we are seeing its remnant expand into a rarefied, intergalactic environment. We also examine if a massive star or a white dwarf binary ejected from either galaxy could be the supernova progenitor. Finally, we consider several other hypotheses for the nature of the object, including the jets of an active galactic nucleus (AGN) or the remnant of a nearby stellar super-flare. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.10026v1-abstract-full').style.display = 'none'; document.getElementById('2201.10026v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages accepted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.00446">arXiv:2111.00446</a> <span> [<a href="https://arxiv.org/pdf/2111.00446">pdf</a>, <a href="https://arxiv.org/format/2111.00446">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac813">10.1093/mnras/stac813 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New XMM-Newton observations of faint, evolved supernova remnants in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kavanagh%2C+P+J">P. J. Kavanagh</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Filipovic%2C+M+D">M. D. Filipovic</a>, <a href="/search/?searchtype=author&query=Points%2C+S+D">S. D. Points</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Maggi%2C+P">P. Maggi</a>, <a href="/search/?searchtype=author&query=Maitra%2C+C">C. Maitra</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.00446v3-abstract-short" style="display: inline;"> The Large Magellanic Cloud (LMC) hosts a rich population of supernova remnants (SNRs), our knowledge of which is the most complete of any galaxy. However, there remain many candidate SNRs, identified through optical and radio observations where additional X-ray data can confirm their SNR nature and provide details on their physical properties. In this paper we present XMM-Newton observations that… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.00446v3-abstract-full').style.display = 'inline'; document.getElementById('2111.00446v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.00446v3-abstract-full" style="display: none;"> The Large Magellanic Cloud (LMC) hosts a rich population of supernova remnants (SNRs), our knowledge of which is the most complete of any galaxy. However, there remain many candidate SNRs, identified through optical and radio observations where additional X-ray data can confirm their SNR nature and provide details on their physical properties. In this paper we present XMM-Newton observations that provide the first deep X-ray coverage of ten objects, comprising eight candidates and two previously confirmed SNRs. We perform multi-frequency studies using additional data from the Magellanic Cloud Emission Line Survey (MCELS) to investigate their broadband emission and used Spitzer data to understand the environment in which the objects are evolving. We confirm seven of the eight candidates as bona-fide SNRs. We used a multi-frequency morphological study to determine the position and size of the remnants. We identify two new members of the class of evolved Fe-rich remnants in the Magellanic Clouds (MCs), several SNRs well into their Sedov-phase, one SNR likely projected towards a HII region, and a faint, evolved SNR with a hard X-ray core which could indicate a pulsar wind nebula. Overall, the seven newly confirmed SNRs represent a ~10% increase in the number of LMC remnants, bringing the total number to 71, and provide further insight into the fainter population of X-ray SNRs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.00446v3-abstract-full').style.display = 'none'; document.getElementById('2111.00446v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">31 pages, 23 figures, accepted for publication in MNRAS. (Version 3: accepted)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.14698">arXiv:2010.14698</a> <span> [<a href="https://arxiv.org/pdf/2010.14698">pdf</a>, <a href="https://arxiv.org/format/2010.14698">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/staa3382">10.1093/mnras/staa3382 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New Optically Identified Supernova Remnants in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Yew%2C+M">Miranda Yew</a>, <a href="/search/?searchtype=author&query=Filipovi%C4%87%2C+M+D">Miroslav D. Filipovi膰</a>, <a href="/search/?searchtype=author&query=Stupar%2C+M">Milorad Stupar</a>, <a href="/search/?searchtype=author&query=Points%2C+S+D">Sean D. Points</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">Manami Sasaki</a>, <a href="/search/?searchtype=author&query=Maggi%2C+P">Pierre Maggi</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">Frank Haberl</a>, <a href="/search/?searchtype=author&query=Kavanagh%2C+P+J">Patrick J. Kavanagh</a>, <a href="/search/?searchtype=author&query=Parker%2C+Q+A">Quentin A. Parker</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">Evan J. Crawford</a>, <a href="/search/?searchtype=author&query=Vukoti%C4%87%2C+B">Branislav Vukoti膰</a>, <a href="/search/?searchtype=author&query=Uro%C5%A1evi%C4%87%2C+D">Dejan Uro拧evi膰</a>, <a href="/search/?searchtype=author&query=Sano%2C+H">Hidetoshi Sano</a>, <a href="/search/?searchtype=author&query=Seitenzahl%2C+I+R">Ivo R. Seitenzahl</a>, <a href="/search/?searchtype=author&query=Rowell%2C+G">Gavin Rowell</a>, <a href="/search/?searchtype=author&query=Leahy%2C+D">Denis Leahy</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">Luke M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Maitra%2C+C">Chandreyee Maitra</a>, <a href="/search/?searchtype=author&query=Leverenz%2C+H">Howard Leverenz</a>, <a href="/search/?searchtype=author&query=Payne%2C+J+L">Jeffrey L. Payne</a>, <a href="/search/?searchtype=author&query=Park%2C+L+A+F">Laurence A. F. Park</a>, <a href="/search/?searchtype=author&query=Alsaberi%2C+R+Z+E">Rami Z. E. Alsaberi</a>, <a href="/search/?searchtype=author&query=Pannuti%2C+T+G">Thomas G. Pannuti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2010.14698v1-abstract-short" style="display: inline;"> We present a new optical sample of three Supernova Remnants and 16 Supernova Remnant (SNR) candidates in the Large Magellanic Cloud(LMC). These objects were originally selected using deep H$伪$, [SII] and [OIII] narrow-band imaging. Most of the newly found objects are located in less dense regions, near or around the edges of the LMC's main body. Together with previously suggested MCSNR J0541-6659,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.14698v1-abstract-full').style.display = 'inline'; document.getElementById('2010.14698v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.14698v1-abstract-full" style="display: none;"> We present a new optical sample of three Supernova Remnants and 16 Supernova Remnant (SNR) candidates in the Large Magellanic Cloud(LMC). These objects were originally selected using deep H$伪$, [SII] and [OIII] narrow-band imaging. Most of the newly found objects are located in less dense regions, near or around the edges of the LMC's main body. Together with previously suggested MCSNR J0541-6659, we confirm the SNR nature for two additional new objects: MCSNR J0522-6740 and MCSNRJ0542-7104. Spectroscopic follow-up observations for 12 of the LMC objects confirm high [SII]/H$伪$ a emission-line ratios ranging from 0.5 to 1.1. We consider the candidate J0509-6402 to be a special example of the remnant of a possible Type Ia Supernova which is situated some 2$^\circ$ ($\sim 1.75$kpc) north from the main body of the LMC. We also find that the SNR candidates in our sample are significantly larger in size than the currently known LMC SNRs by a factor of $\sim 2$. This could potentially imply that we are discovering a previously unknown but predicted, older class of large LMC SNRs that are only visible optically. Finally, we suggest that most of these LMC SNRs are residing in a very rarefied environment towards the end of their evolutionary span where they become less visible to radio and X-ray telescopes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.14698v1-abstract-full').style.display = 'none'; document.getElementById('2010.14698v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 25 figures, to appear in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1911.04051">arXiv:1911.04051</a> <span> [<a href="https://arxiv.org/pdf/1911.04051">pdf</a>, <a href="https://arxiv.org/format/1911.04051">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s10509-019-3696-8">10.1007/s10509-019-3696-8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radio Emission from Interstellar Shocks: Young Type Ia Supernova Remnants and the Case of N 103B in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Alsaberi%2C+R+Z+E">R. Z. E. Alsaberi</a>, <a href="/search/?searchtype=author&query=Barnes%2C+L+A">L. A. Barnes</a>, <a href="/search/?searchtype=author&query=Filipovic%2C+M+D">M. D. Filipovic</a>, <a href="/search/?searchtype=author&query=Maxted%2C+N+I">N. I. Maxted</a>, <a href="/search/?searchtype=author&query=Sano%2C+H">H. Sano</a>, <a href="/search/?searchtype=author&query=Rowell%2C+G">G. Rowell</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Gurovich%2C+S">S. Gurovich</a>, <a href="/search/?searchtype=author&query=Urovsevic%2C+D">D. Urovsevic</a>, <a href="/search/?searchtype=author&query=Onic%2C+D">D. Onic</a>, <a href="/search/?searchtype=author&query=For%2C+B+Q">B. Q. For</a>, <a href="/search/?searchtype=author&query=Manojlovic%2C+P">P. Manojlovic</a>, <a href="/search/?searchtype=author&query=Wong%2C+G">G. Wong</a>, <a href="/search/?searchtype=author&query=Galvin%2C+T">T. Galvin</a>, <a href="/search/?searchtype=author&query=Kavanagh%2C+P">P. Kavanagh</a>, <a href="/search/?searchtype=author&query=Ralph%2C+N">N. Ralph</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Maggi%2C+P">P. Maggi</a>, <a href="/search/?searchtype=author&query=Tothil%2C+N+F+H">N. F. H. Tothil</a>, <a href="/search/?searchtype=author&query=Fukui%2C+Y">Y. Fukui</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1911.04051v1-abstract-short" style="display: inline;"> Here we present a radio continuum study based on new and archival data from the Australia Telescope Compact Array towards N 103B, a young (<=1000 yrs) spectroscopically confirmed type Ia SNR in the Large Magellanic Cloud (LMC) and proposed to have originated from a single degenerate progenitor. The radio morphology of this SNR is asymmetrical with two bright regions towards the north-west and sout… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.04051v1-abstract-full').style.display = 'inline'; document.getElementById('1911.04051v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1911.04051v1-abstract-full" style="display: none;"> Here we present a radio continuum study based on new and archival data from the Australia Telescope Compact Array towards N 103B, a young (<=1000 yrs) spectroscopically confirmed type Ia SNR in the Large Magellanic Cloud (LMC) and proposed to have originated from a single degenerate progenitor. The radio morphology of this SNR is asymmetrical with two bright regions towards the north-west and south-west of the central location as defined by radio emission. N 103B identified features include: a radio spectral index of -0.75+-0.01 (consistent with other young type Ia SNRs in the Galaxy); a bulk SNR expansion rate as in X-rays; morphology and polarised electrical field vector measurements where we note radial polarisation peak towards the north-west of the remnant at both 5500 and 9000 MHz. The spectrum is concave-up and the most likely reason is the non-linear diffusive shock acceleration effects or presence of two different populations of ultra-relativistic electrons. We also note unpolarized clumps near the south-west region which is in agreement with this above scenario. We derive a typical magnetic field strength for N 103B, of 16.4 microG for an average rotation measurement of 200 rad m^-2. However, we estimate the equipartition field to be of the order of ~235 microG with an estimated minimum energy of Emin=6.3*10^48 erg. The close (~0.5 degree) proximity of N 103B to the LMC mid-plane indicates that an early encounter with dense interstellar medium may have set an important constrain on SNR evolution. Finally, we compare features of N 103B, to six other young type Ia SNRs in the LMC and Galaxy, with a range of proposed degeneracy scenarios to highlight potential differences due to a different models. We suggest that the single degenerate scenario might point to morphologically asymmetric type Ia supernova explosions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1911.04051v1-abstract-full').style.display = 'none'; document.getElementById('1911.04051v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2019. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.10425">arXiv:1909.10425</a> <span> [<a href="https://arxiv.org/pdf/1909.10425">pdf</a>, <a href="https://arxiv.org/format/1909.10425">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stz2650">10.1093/mnras/stz2650 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The ASKAP-EMU Early Science Project:Radio Continuum Survey of the Small Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Joseph%2C+T+D">T. D. Joseph</a>, <a href="/search/?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/?searchtype=author&query=Boji%C4%8Di%C4%87%2C+I">I. Boji膷i膰</a>, <a href="/search/?searchtype=author&query=Alexander%2C+E+L">E. L. Alexander</a>, <a href="/search/?searchtype=author&query=Wong%2C+G+F">G. F. Wong</a>, <a href="/search/?searchtype=author&query=Andernach%2C+H">H. Andernach</a>, <a href="/search/?searchtype=author&query=Leverenz%2C+H">H. Leverenz</a>, <a href="/search/?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/?searchtype=author&query=Alsaberi%2C+R+Z+E">R. Z. E. Alsaberi</a>, <a href="/search/?searchtype=author&query=Anderson%2C+C">C. Anderson</a>, <a href="/search/?searchtype=author&query=Barnes%2C+L+A">L. A. Barnes</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/?searchtype=author&query=Bunton%2C+J+D">J. D. Bunton</a>, <a href="/search/?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/?searchtype=author&query=Collier%2C+J+D">J. D. Collier</a>, <a href="/search/?searchtype=author&query=D%C3%A9nes%2C+H">H. D茅nes</a>, <a href="/search/?searchtype=author&query=Fukui%2C+Y">Y. Fukui</a>, <a href="/search/?searchtype=author&query=Galvin%2C+T">T. Galvin</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/?searchtype=author&query=Kapinska%2C+A+D">A. D. Kapinska</a>, <a href="/search/?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/?searchtype=author&query=Kothes%2C+R">R. Kothes</a> , et al. (31 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1909.10425v1-abstract-short" style="display: inline;"> We present two new radio continuum images from the Australian Square Kilometre Array Pathfinder (ASKAP) survey in the direction of the Small Magellanic Cloud (SMC). These images are part of the Evolutionary Map of the Universe (EMU) Early Science Project (ESP) survey of the Small and Large Magellanic Clouds. The two new source lists produced from these images contain radio continuum sources observ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.10425v1-abstract-full').style.display = 'inline'; document.getElementById('1909.10425v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.10425v1-abstract-full" style="display: none;"> We present two new radio continuum images from the Australian Square Kilometre Array Pathfinder (ASKAP) survey in the direction of the Small Magellanic Cloud (SMC). These images are part of the Evolutionary Map of the Universe (EMU) Early Science Project (ESP) survey of the Small and Large Magellanic Clouds. The two new source lists produced from these images contain radio continuum sources observed at 960 MHz (4489 sources) and 1320 MHz (5954 sources) with a bandwidth of 192 MHz and beam sizes of 30.0"x30.0" and 16.3"x15.1", respectively. The median Root Mean Squared (RMS) noise values are 186$渭$Jy beam$^{-1}$ (960 MHz) and 165$渭$Jy beam$^{-1}$ (1320 MHz). To create point source catalogues, we use these two source lists, together with the previously published Molonglo Observatory Synthesis Telescope (MOST) and the Australia Telescope Compact Array (ATCA) point source catalogues to estimate spectral indices for the whole population of radio point sources found in the survey region. Combining our ASKAP catalogues with these radio continuum surveys, we found 7736 point-like sources in common over an area of 30 deg$^2$. In addition, we report the detection of two new, low surface brightness supernova remnant candidates in the SMC. The high sensitivity of the new ASKAP ESP survey also enabled us to detect the bright end of the SMC planetary nebula sample, with 22 out of 102 optically known planetary nebulae showing point-like radio continuum emission. Lastly, we present several morphologically interesting background radio galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.10425v1-abstract-full').style.display = 'none'; document.getElementById('1909.10425v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 23 figues, 9 tables, Accepted for publication in the Monthly Notices of the Royal Astronomical Society</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1903.03226">arXiv:1903.03226</a> <span> [<a href="https://arxiv.org/pdf/1903.03226">pdf</a>, <a href="https://arxiv.org/format/1903.03226">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stz971">10.1093/mnras/stz971 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of a Pulsar-powered Bow Shock Nebula in the Small Magellanic Cloud Supernova Remnant DEMS5 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Alsaberi%2C+R+Z+E">Rami Z. E. Alsaberi</a>, <a href="/search/?searchtype=author&query=Maitra%2C+C">C. Maitra</a>, <a href="/search/?searchtype=author&query=Filipovi%27c%2C+M+D">M. D. Filipovi'c</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Maggi%2C+P">P. Maggi</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Manjolovi%27c%2C+P">P. Manjolovi'c</a>, <a href="/search/?searchtype=author&query=Velovi%27c%2C+V">V. Velovi'c</a>, <a href="/search/?searchtype=author&query=Kavanagh%2C+P">P. Kavanagh</a>, <a href="/search/?searchtype=author&query=Maxted%2C+N+I">N. I. Maxted</a>, <a href="/search/?searchtype=author&query=Urovsevi%27c%2C+D">D. Urovsevi'c</a>, <a href="/search/?searchtype=author&query=Rowell%2C+G+P">G. P. Rowell</a>, <a href="/search/?searchtype=author&query=Wong%2C+G+F">G. F. Wong</a>, <a href="/search/?searchtype=author&query=For%2C+B+-">B. -Q. For</a>, <a href="/search/?searchtype=author&query=O%27Brien%2C+A+N">A. N. O'Brien</a>, <a href="/search/?searchtype=author&query=Galvin%2C+T+J">T. J. Galvin</a>, <a href="/search/?searchtype=author&query=Staveley-Smith%2C+L">L. Staveley-Smith</a>, <a href="/search/?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/?searchtype=author&query=Jarrett%2C+T">T. Jarrett</a>, <a href="/search/?searchtype=author&query=Kothes%2C+R">R. Kothes</a>, <a href="/search/?searchtype=author&query=Luken%2C+K+J">K. J. Luken</a>, <a href="/search/?searchtype=author&query=Hurley-Walker%2C+N">N. Hurley-Walker</a>, <a href="/search/?searchtype=author&query=Sano%2C+H">H. Sano</a>, <a href="/search/?searchtype=author&query=Oni%27c%2C+D">D. Oni'c</a> , et al. (10 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1903.03226v2-abstract-short" style="display: inline;"> We report the discovery of a new Small Magellanic Cloud Pulsar Wind Nebula (PWN) at the edge of the Supernova Remnant (SNR)-DEM S5. The pulsar powered object has a cometary morphology similar to the Galactic PWN analogs PSR B1951+32 and 'the mouse'. It is travelling supersonically through the interstellar medium. We estimate the Pulsar kick velocity to be in the range of 700-2000 km/s for an age b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.03226v2-abstract-full').style.display = 'inline'; document.getElementById('1903.03226v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.03226v2-abstract-full" style="display: none;"> We report the discovery of a new Small Magellanic Cloud Pulsar Wind Nebula (PWN) at the edge of the Supernova Remnant (SNR)-DEM S5. The pulsar powered object has a cometary morphology similar to the Galactic PWN analogs PSR B1951+32 and 'the mouse'. It is travelling supersonically through the interstellar medium. We estimate the Pulsar kick velocity to be in the range of 700-2000 km/s for an age between 28-10 kyr. The radio spectral index for this SNR PWN pulsar system is flat (-0.29 $\pm$ 0.01) consistent with other similar objects. We infer that the putative pulsar has a radio spectral index of -1.8, which is typical for Galactic pulsars. We searched for dispersion measures (DMs) up to 1000 cm/pc^3 but found no convincing candidates with a S/N greater than 8. We produce a polarisation map for this PWN at 5500 MHz and find a mean fractional polarisation of P $\sim 23$ percent. The X-ray power-law spectrum (Gamma $\sim 2$) is indicative of non-thermal synchrotron emission as is expected from PWN-pulsar system. Finally, we detect DEM S5 in Infrared (IR) bands. Our IR photometric measurements strongly indicate the presence of shocked gas which is expected for SNRs. However, it is unusual to detect such IR emission in a SNR with a supersonic bow-shock PWN. We also find a low-velocity HI cloud of $\sim 107$ km/s which is possibly interacting with DEM S5. SNR DEM S5 is the first confirmed detection of a pulsar-powered bow shock nebula found outside the Galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.03226v2-abstract-full').style.display = 'none'; document.getElementById('1903.03226v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 15 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1703.02676">arXiv:1703.02676</a> <span> [<a href="https://arxiv.org/pdf/1703.02676">pdf</a>, <a href="https://arxiv.org/ps/1703.02676">ps</a>, <a href="https://arxiv.org/format/1703.02676">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/aa653c">10.3847/1538-4365/aa653c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Statistical Analysis of Supernova Remnants in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">Luke M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Filipovi%C4%87%2C+M+D">Miroslav D. Filipovi膰</a>, <a href="/search/?searchtype=author&query=Vukoti%C4%87%2C+B">Branislav Vukoti膰</a>, <a href="/search/?searchtype=author&query=Pavlovi%C4%87%2C+M+Z">Marko Z. Pavlovi膰</a>, <a href="/search/?searchtype=author&query=Urosevi%C4%87%2C+D">Dejan Urosevi膰</a>, <a href="/search/?searchtype=author&query=Kavanagh%2C+P+J">Patrick J. Kavanagh</a>, <a href="/search/?searchtype=author&query=Arbutina%2C+B">Bojan Arbutina</a>, <a href="/search/?searchtype=author&query=Maggi%2C+P">Pierre Maggi</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">Manami Sasaki</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">Frank Haberl</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">Evan J. Crawford</a>, <a href="/search/?searchtype=author&query=Roper%2C+Q">Quentin Roper</a>, <a href="/search/?searchtype=author&query=Grieve%2C+K">Kevin Grieve</a>, <a href="/search/?searchtype=author&query=Points%2C+S+D">S. D. Points</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1703.02676v2-abstract-short" style="display: inline;"> We construct the most complete sample of supernova remnants (SNRs) in any galaxy - the Large Magellanic Cloud (LMC) SNR sample. We study their various properties such as spectral index ($伪$), size and surface-brightness. We suggest an association between the spatial distribution, environment density of LMC SNRs and their tendency to be located around supergiant shells. We find evidence that the 16… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.02676v2-abstract-full').style.display = 'inline'; document.getElementById('1703.02676v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.02676v2-abstract-full" style="display: none;"> We construct the most complete sample of supernova remnants (SNRs) in any galaxy - the Large Magellanic Cloud (LMC) SNR sample. We study their various properties such as spectral index ($伪$), size and surface-brightness. We suggest an association between the spatial distribution, environment density of LMC SNRs and their tendency to be located around supergiant shells. We find evidence that the 16 known type Ia LMC SNRs are expanding in a lower density environment compared to the Core-Collapse (CC) type. The mean diameter of our entire population (74) is 41 pc, which is comparable to nearby galaxies. We didn't find any correlation between the type of SN explosion, ovality or age. The $N(<D)$ relationship of $a={0.96}$ implies that the randomised diameters are readily mimicking such an exponent. The rate of SNe occurring in the LMC is estimated to be $\sim$1 per 200 yr. The mean $伪$ of the entire LMC SNR population is $伪=-0.52$, which is typical of most SNRs. However, our estimates show a clear flattening of the synchrotron $伪$ as the remnants age. As predicted, our CC SNRs sample are significantly brighter radio emitters than the type Ia remnants. We also estimate the $危- D$ relation for the LMC to have a slope $\sim3.8$ which is comparable with other nearby galaxies. We also find the residency time of electrons in the galaxy ($4.0-14.3$ Myr), implying that SNRs should be the dominant mechanism for the production and acceleration of CRs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.02676v2-abstract-full').style.display = 'none'; document.getElementById('1703.02676v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 March, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 March, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in APJSS, updated to fix a few typos and references</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1604.01458">arXiv:1604.01458</a> <span> [<a href="https://arxiv.org/pdf/1604.01458">pdf</a>, <a href="https://arxiv.org/format/1604.01458">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Supernova Remnants In The Magellanic Clouds </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Filipovi%C4%87%2C+M+D">Miroslav D. Filipovi膰</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">Luke M. Bozzetto</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1604.01458v1-abstract-short" style="display: inline;"> We present initial results of an ongoing study of the supernova remnants (SNRs) and candidates in the Magellanic Clouds. Some 108 objects in both Clouds are considered to be either an SNR or a reliable candidate. This represents the most complete sample of known SNRs in any galaxy. therefore, this study allows us to study SNR population properties such as the size and spectral index distribution.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.01458v1-abstract-full').style.display = 'inline'; document.getElementById('1604.01458v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1604.01458v1-abstract-full" style="display: none;"> We present initial results of an ongoing study of the supernova remnants (SNRs) and candidates in the Magellanic Clouds. Some 108 objects in both Clouds are considered to be either an SNR or a reliable candidate. This represents the most complete sample of known SNRs in any galaxy. therefore, this study allows us to study SNR population properties such as the size and spectral index distribution. Here, we also show 12 known Large Magellanic Cloud SNRs from type Ia SN explosions and briefly comment on their importance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.01458v1-abstract-full').style.display = 'none'; document.getElementById('1604.01458v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Publ. Astron. Obs. Belgrade</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1510.08922">arXiv:1510.08922</a> <span> [<a href="https://arxiv.org/pdf/1510.08922">pdf</a>, <a href="https://arxiv.org/format/1510.08922">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201527414">10.1051/0004-6361/201527414 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Two evolved supernova remnants with newly identified Fe-rich cores in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kavanagh%2C+P+J">Patrick J. Kavanagh</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">Manami Sasaki</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">Luke M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Points%2C+S+D">Sean D. Points</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">Evan J. Crawford</a>, <a href="/search/?searchtype=author&query=Dickel%2C+J">John Dickel</a>, <a href="/search/?searchtype=author&query=Filipovic%2C+M+D">Miroslav D. Filipovic</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">Frank Haberl</a>, <a href="/search/?searchtype=author&query=Maggi%2C+P">Pierre Maggi</a>, <a href="/search/?searchtype=author&query=Whelan%2C+E+T">Emma T. Whelan</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1510.08922v1-abstract-short" style="display: inline;"> Aims. We present a multi-wavelength analysis of the evolved supernova remnants MCSNR J0506-7025 and MCSNR J0527-7104 in the Large Magellanic Cloud. Methods. We used data from XMM-Newton, the Australian Telescope Compact Array, and the Magellanic Cloud Emission Line Survey to study their broadband emission and used Spitzer and HI data to gain a picture of their environments. We performed a multi-wa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.08922v1-abstract-full').style.display = 'inline'; document.getElementById('1510.08922v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1510.08922v1-abstract-full" style="display: none;"> Aims. We present a multi-wavelength analysis of the evolved supernova remnants MCSNR J0506-7025 and MCSNR J0527-7104 in the Large Magellanic Cloud. Methods. We used data from XMM-Newton, the Australian Telescope Compact Array, and the Magellanic Cloud Emission Line Survey to study their broadband emission and used Spitzer and HI data to gain a picture of their environments. We performed a multi-wavelength morphological study and detailed radio and X-ray spectral analyses to determine their physical characteristics. Results. Both remnants were found to have bright X-ray cores, dominated by Fe L-shell emission, consistent with reverse shock heated ejecta with determined Fe masses in agreement with Type Ia explosion yields. A soft X-ray shell, consistent with swept-up interstellar medium, was observed in MCSNR J0506-7025, suggestive of a remnant in the Sedov phase. Using the spectral fit results and the Sedov self-similar solution, we estimated the age of MCSNR J0506-7025 to be ~16-28 kyr, with an initial explosion energy of (0.07-0.84)x10^51 erg. A soft shell was absent in MCSNR J0527-7104, with only ejecta emission visible in an extremely elongated morphology extending beyond the optical shell. We suggest that the blast wave has broken out into a low density cavity, allowing the shock heated ejecta to escape. We found that the radio spectral index of MCSNR J0506-7025 is consistent with the standard ~0.5 for SNRs. Radio polarisation at 6 cm indicates a higher degree of polarisation along the western front and at the eastern knot, with a mean fractional polarisation across the remnant of P~(20 \pm 6)%. Conclusions. The detection of Fe-rich ejecta in the remnants suggests that both resulted from Type Ia explosions. The newly identified Fe-rich cores in MCSNR J0506-7025 and MCSNR J0527-7104 makes them members of the expanding class of evolved Fe-rich remnants in the Magellanic Clouds. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.08922v1-abstract-full').style.display = 'none'; document.getElementById('1510.08922v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 October, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 13 figures, accepted for publication in A&A. arXiv admin note: text overlap with arXiv:1509.06475</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 586, A4 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1509.09223">arXiv:1509.09223</a> <span> [<a href="https://arxiv.org/pdf/1509.09223">pdf</a>, <a href="https://arxiv.org/format/1509.09223">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201526932">10.1051/0004-6361/201526932 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The population of X-ray supernova remnants in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Maggi%2C+P">P. Maggi</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Kavanagh%2C+P+J">P. J. Kavanagh</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/?searchtype=author&query=Vasilopoulos%2C+G">G. Vasilopoulos</a>, <a href="/search/?searchtype=author&query=Pietsch%2C+W">W. Pietsch</a>, <a href="/search/?searchtype=author&query=Points%2C+S+D">S. D. Points</a>, <a href="/search/?searchtype=author&query=Chu%2C+Y+-">Y. -H. Chu</a>, <a href="/search/?searchtype=author&query=Dickel%2C+J">J. Dickel</a>, <a href="/search/?searchtype=author&query=Ehle%2C+M">M. Ehle</a>, <a href="/search/?searchtype=author&query=Williams%2C+R">R. Williams</a>, <a href="/search/?searchtype=author&query=Greiner%2C+J">J. Greiner</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1509.09223v3-abstract-short" style="display: inline;"> We present a comprehensive X-ray study of the population of supernova remnants (SNRs) in the LMC. Using primarily XMM-Newton, we conduct a systematic spectral analysis of LMC SNRs to gain new insights on their evolution and the interplay with their host galaxy. We combined all the archival XMM observations of the LMC with those of our Very Large Programme survey. We produced X-ray images and spect… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.09223v3-abstract-full').style.display = 'inline'; document.getElementById('1509.09223v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1509.09223v3-abstract-full" style="display: none;"> We present a comprehensive X-ray study of the population of supernova remnants (SNRs) in the LMC. Using primarily XMM-Newton, we conduct a systematic spectral analysis of LMC SNRs to gain new insights on their evolution and the interplay with their host galaxy. We combined all the archival XMM observations of the LMC with those of our Very Large Programme survey. We produced X-ray images and spectra of 51 SNRs, out of a list of 59. Using a careful modelling of the background, we consistently analysed all the X-ray spectra and measure temperatures, luminosities, and chemical compositions. We investigated the spatial distribution of SNRs in the LMC and the connection with their environment, characterised by various SFHs. We tentatively typed all LMC SNRs to constrain the ratio of core-collapse to type Ia SN rates in the LMC. We compared the X-ray-derived column densities to HI maps to probe the three-dimensional structure of the LMC. This work provides the first homogeneous catalogue of X-ray spectral properties of LMC SNRs. It offers a complete census of LMC SNRs exhibiting Fe K lines (13% of the sample), or revealing contribution from hot SN ejecta (39%). Abundances in the LMC ISM are found to be 0.2-0.5 solar, with a lower [$伪$/Fe] than in the Milky Way. The ratio of CC/type Ia SN in the LMC is $N_{\mathrm{CC}}/N_{\mathrm{Ia}} = 1.35(_{-0.24}^{+0.11})$, lower than in local SN surveys and galaxy clusters. Comparison of X-ray luminosity functions of SNRs in Local Group galaxies reveals an intriguing excess of bright objects in the LMC. 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. (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.09223v3-abstract-full').style.display = 'none'; document.getElementById('1509.09223v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 October, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy and Astrophysics. 54 pages, 18 figures, 12 tables. The resolution of the figures has been reduced compared to the journal version; v2: New title, minor text edits; v3: Correct version 2</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 585, A162 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1509.06475">arXiv:1509.06475</a> <span> [<a href="https://arxiv.org/pdf/1509.06475">pdf</a>, <a href="https://arxiv.org/format/1509.06475">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201526987">10.1051/0004-6361/201526987 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multi-frequency study of the newly confirmed supernova remnant MCSNR J0512-6707 in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kavanagh%2C+P+J">P. J. Kavanagh</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Points%2C+S+D">S. D. Points</a>, <a href="/search/?searchtype=author&query=Filipovic%2C+M+D">M. D. Filipovic</a>, <a href="/search/?searchtype=author&query=Maggi%2C+P">P. Maggi</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1509.06475v1-abstract-short" style="display: inline;"> We present a study of the supernova remnant MCSNR J0512-6707 in the Large Magellanic Cloud. We used new data from XMM-Newton to characterise the X-ray emission and data from the Australian Telescope Compact Array, the Magellanic Cloud Emission Line Survey, and Spitzer to gain a picture of the environment into which the remnant is expanding. We performed a morphological study, determined radio pola… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.06475v1-abstract-full').style.display = 'inline'; document.getElementById('1509.06475v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1509.06475v1-abstract-full" style="display: none;"> We present a study of the supernova remnant MCSNR J0512-6707 in the Large Magellanic Cloud. We used new data from XMM-Newton to characterise the X-ray emission and data from the Australian Telescope Compact Array, the Magellanic Cloud Emission Line Survey, and Spitzer to gain a picture of the environment into which the remnant is expanding. We performed a morphological study, determined radio polarisation and magnetic field orientation, and performed an X-ray spectral analysis. We estimated the its size to be 24.9 (\pm1.5) x 21.9 (\pm1.5) pc, with the major axis rotated ~29 deg east of north. Radio polarisation at 3 cm and 6 cm indicate a higher degree of polarisation in the NW and SE tangentially oriented to the SNR shock front, indicative of an SNR compressing the magnetic field threading the interstellar medium. The X-ray spectrum is unusual as it requires a soft (~0.2 keV) CIE thermal plasma of interstellar medium abundance, in addition to a harder component. Using our results and the Sedov dynamical model, we showed that this emission is not consistent with a Sedov remnant. We suggested that the thermal X-rays can be explained by MCSNR J0512-6707 having initially evolved into a wind-blown cavity and is now interacting with the surrounding dense shell. The origin of the hard component remains unclear. We could not determine the supernova type from the X-ray spectrum. Indirect evidence was found in the study of the local stellar population and star formation history in the literature, which suggests a core-collapse origin. MCSNR J0512-6707 likely resulted from the core-collapse of high mass progenitor which carved a low density cavity into its surrounding medium, with the soft X-rays resulting from the impact of the blast wave with the surrounding shell. The unusual hard X-ray component requires deeper and higher spatial resolution radio and X-ray observations to confirm its origin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.06475v1-abstract-full').style.display = 'none'; document.getElementById('1509.06475v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 7 figures, accepted for publication in Astronomy and Astrophysics. arXiv admin note: text overlap with arXiv:1505.06458</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 583, A121 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1508.06323">arXiv:1508.06323</a> <span> [<a href="https://arxiv.org/pdf/1508.06323">pdf</a>, <a href="https://arxiv.org/format/1508.06323">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stv1992">10.1093/mnras/stv1992 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Optical discovery and multiwavelength investigation of supernova remnant MCSNR J0512-6707 in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Reid%2C+W+A">Warren A. Reid</a>, <a href="/search/?searchtype=author&query=Stupar%2C+M">Milorad Stupar</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">Luke M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Parker%2C+Q+A">Quentin A. Parker</a>, <a href="/search/?searchtype=author&query=Filipovic%2C+M+D">Miroslav D. Filipovic</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1508.06323v2-abstract-short" style="display: inline;"> We present optical, radio and X-ray data that confirm a new supernova remnant (SNR) in the Large Magellanic Cloud (LMC) discovered using our deep H-alpha imagery. Optically, the new SNR has a somewhat filamentary morphology and a diameter of 56 x 64 arcsec (13.5 x 15.5 pc at the 49.9 kpc distance of the LMC). Spectroscopic follow-up of multiple regions show high [SII]/H-alpha emission-line ratios… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.06323v2-abstract-full').style.display = 'inline'; document.getElementById('1508.06323v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1508.06323v2-abstract-full" style="display: none;"> We present optical, radio and X-ray data that confirm a new supernova remnant (SNR) in the Large Magellanic Cloud (LMC) discovered using our deep H-alpha imagery. Optically, the new SNR has a somewhat filamentary morphology and a diameter of 56 x 64 arcsec (13.5 x 15.5 pc at the 49.9 kpc distance of the LMC). Spectroscopic follow-up of multiple regions show high [SII]/H-alpha emission-line ratios ranging from 0.66+/-0.02 to 0.93+/-0.01, all of which are typical of an SNR. We found radio counterparts for this object using our new Australia Telescope Compact Array (ATCA) 6cm pointed observations as well as a number of available radio surveys at 8 640 MHz, 4 850 MHz, 1 377 MHz and 843 MHz. With these combined data we provide a spectral index (alpha) = -0.5 between 843 and 8640 MHz. Both spectral line analysis and the magnetic field strength, ranging from 124 - 184 mG, suggest a dynamical age between 2,200 and 4,700 yrs. The SNR has a previously catalogued X-ray counterpart listed as HP 483 in the ROSAT Position Sensitive Proportional Counter (PSPC) catalogue. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.06323v2-abstract-full').style.display = 'none'; document.getElementById('1508.06323v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 March, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 August, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 11 figures. Published MNRAS. New version in order to update acknowledgements</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Warren Reid et al. 2015, MNRAS 454, 991 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1505.06458">arXiv:1505.06458</a> <span> [<a href="https://arxiv.org/pdf/1505.06458">pdf</a>, <a href="https://arxiv.org/format/1505.06458">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201526143">10.1051/0004-6361/201526143 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> XMM-Newton observation of SNR J0533-7202 in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kavanagh%2C+P+J">P. J. Kavanagh</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Whelan%2C+E+T">E. T. Whelan</a>, <a href="/search/?searchtype=author&query=Maggi%2C+P">P. Maggi</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Filipovic%2C+M+D">M. D. Filipovic</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1505.06458v1-abstract-short" style="display: inline;"> 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 (flare-filtered exposure times of 18 ks EPIC-pn and 31 ks EPIC-MOS1/MOS2). We produced X-ray images of the SNR, performed an X-ray spectral analysis, and compared the r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1505.06458v1-abstract-full').style.display = 'inline'; document.getElementById('1505.06458v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1505.06458v1-abstract-full" style="display: none;"> 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 (flare-filtered exposure times of 18 ks EPIC-pn and 31 ks EPIC-MOS1/MOS2). We produced X-ray images of the SNR, 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 brighter than the north-east. The X-ray emission is correlated with the radio emission from the remnant. We determine that this morphology is likely due to the SNR expanding into a non-uniform ambient medium and not an absorption effect. We estimate the size to be 53.9 (\pm 3.4) x 43.6 (\pm 3.4) pc, with the major axis rotated ~64 degrees east of north. We find no spectral signatures of ejecta 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 an age of ~17-27 kyr, with an initial explosion energy of (0.09-0.83) x 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 find 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. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1505.06458v1-abstract-full').style.display = 'none'; document.getElementById('1505.06458v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 May, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 4 figures, accepted for publication in Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 579, A63 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1409.6547">arXiv:1409.6547</a> <span> [<a href="https://arxiv.org/pdf/1409.6547">pdf</a>, <a href="https://arxiv.org/format/1409.6547">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201424354">10.1051/0004-6361/201424354 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> XMM-Newton study of 30 Dor C and a newly identified MCSNR J0536-6913 in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kavanagh%2C+P+J">P. J. Kavanagh</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Filipovic%2C+M+D">M. D. Filipovic</a>, <a href="/search/?searchtype=author&query=Points%2C+S+D">S. D. Points</a>, <a href="/search/?searchtype=author&query=Maggi%2C+P">P. Maggi</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1409.6547v1-abstract-short" style="display: inline;"> Aims: We present a study of the superbubble (SB) 30 Dor C and the newly identified MCSNR J0536-6913 in the LMC. Methods: All available XMM-Newton data (exposure times of 420 ks EPIC-pn, 556 ks EPIC-MOS1, 614 ks EPIC-MOS2) were used to characterise the thermal X-ray emission in the region. An analysis of the non-thermal X-rays is also presented and discussed in the context of emission mechanisms pr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.6547v1-abstract-full').style.display = 'inline'; document.getElementById('1409.6547v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1409.6547v1-abstract-full" style="display: none;"> Aims: We present a study of the superbubble (SB) 30 Dor C and the newly identified MCSNR J0536-6913 in the LMC. Methods: All available XMM-Newton data (exposure times of 420 ks EPIC-pn, 556 ks EPIC-MOS1, 614 ks EPIC-MOS2) were used to characterise the thermal X-ray emission in the region. An analysis of the non-thermal X-rays is also presented and discussed in the context of emission mechanisms previously suggested in the literature. These data are supplemented by X-ray data from Chandra, optical data from the MCELS, and radio data from ATCA and MOST. Results: The brightest thermal emission was found to be associated with a new supernova remnant, MCSNR J0536-6913. X-ray spectral analysis of MCSNR J0536-6913 suggested an ejecta-dominated remnant with lines of O, Ne, Mg, and Si, and a total 0.3-10 keV luminosity of ~8E+34 erg/s. Based on derived ejecta abundance ratios, we determined the mass of the stellar progenitor to be either ~18 M_sun or as high as >40 M_sun, though the spectral fits were subject to assumptions (e.g., uniform temperature and well-mixed ejecta). The thermal emission from the SB exhibited enrichment by alpha-process elements, evidence for a recent core-collapse SNR interaction with the SB shell. We detected non-thermal X-ray emission throughout 30 Dor C, with the brightest regions being highly correlated with the H-alpha and radio shells. We created a non-thermal spectral energy distribution for the north-eastern shell of 30 Dor C which was best-fit with an exponentially cut-off synchrotron model. Conclusions: Thermal X-ray emission from 30 Dor C is very complex, consisting of a large scale SB emission at the eastern shell wall with the brightest emission due to MCSNR J0536-6913. The fact that the non-thermal spectral energy distribution of the SB shell was observed to roll-off is further evidence that the non-thermal X-rays from 30 Dor C are synchrotron in origin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.6547v1-abstract-full').style.display = 'none'; document.getElementById('1409.6547v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 September, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 21 figures, accepted for publication in Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 573, A73 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1408.1850">arXiv:1408.1850</a> <span> [<a href="https://arxiv.org/pdf/1408.1850">pdf</a>, <a href="https://arxiv.org/format/1408.1850">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201423575">10.1051/0004-6361/201423575 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multi-frequency study of DEM L299 in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Warth%2C+G">Gabriele Warth</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">Manami Sasaki</a>, <a href="/search/?searchtype=author&query=Kavanagh%2C+P+J">Patrick J. Kavanagh</a>, <a href="/search/?searchtype=author&query=Filipovi%C4%87%2C+M+D">Miroslav D. Filipovi膰</a>, <a href="/search/?searchtype=author&query=Points%2C+S+D">Sean D. Points</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">Luke M. Bozzetto</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1408.1850v1-abstract-short" style="display: inline;"> We have studied the HII region DEM L299 in the Large Magellanic Cloud to understand its physical characteristics and morphology in different wavelengths. 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 H alpha, [SII], and [OIII] data from the Magellanic Cloud Emission Line Survey and radio 21… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.1850v1-abstract-full').style.display = 'inline'; document.getElementById('1408.1850v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1408.1850v1-abstract-full" style="display: none;"> We have studied the HII region DEM L299 in the Large Magellanic Cloud to understand its physical characteristics and morphology in different wavelengths. 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 H alpha, [SII], and [OIII] data from the Magellanic Cloud Emission Line Survey and radio 21 cm line data from the Australia Telescope Compact Array (ATCA) and the Parkes telescope, and radio continuum data from ATCA and the Molonglo Synthesis Telescope. 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 [SII]/H alpha 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 HII region N 164 that lies south-west of it. We determined the spectral index of SNR B0543-68.9 to be alpha=-0.34, which indicates the dominance of thermal emission and therefore a rather mature SNR. 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 (3.5-18.1) kyr for the SNR and a temperature of 0.64 (0.44-1.37) keV for the hot gas inside the SNR, and a temperature of the hot gas inside the superbubble of 0.74 (0.44-1.1) keV. We conclude that DEM L299 consists of a superposition of SNR B0543-68.9 and a superbubble, which we identified based on optical data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.1850v1-abstract-full').style.display = 'none'; document.getElementById('1408.1850v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy and Astrophysics. 17 pages, 16 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 567, A136 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1404.3823">arXiv:1404.3823</a> <span> [<a href="https://arxiv.org/pdf/1404.3823">pdf</a>, <a href="https://arxiv.org/ps/1404.3823">ps</a>, <a href="https://arxiv.org/format/1404.3823">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-6256/147/6/162">10.1088/0004-6256/147/6/162 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multi-frequency observations of a superbubble in the LMC: The case of LHA 120-N 70 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=De+Horta%2C+A+Y">A. Y. De Horta</a>, <a href="/search/?searchtype=author&query=Sommer%2C+E+R">E. R. Sommer</a>, <a href="/search/?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/?searchtype=author&query=O%27Brien%2C+A">A. O'Brien</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Collier%2C+J+D">J. D. Collier</a>, <a href="/search/?searchtype=author&query=Wong%2C+G+F">G. F. Wong</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/?searchtype=author&query=Tothill%2C+N+F+H">N. F. H. Tothill</a>, <a href="/search/?searchtype=author&query=Maggi%2C+P">P. Maggi</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1404.3823v1-abstract-short" style="display: inline;"> We present a detailed study of new Australia Telescope Compact Array (ATCA) and XMM-Newton observations of LHA 120-N 70 (hereafter N 70), a spherically shaped object in the Large Magellanic Cloud (LMC) classified as a superbubble (SB). Both archival and new observations were used to produce high quality radio-continuum, X-ray and optical images. The radio spectral index of N 70 is estimated to be… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1404.3823v1-abstract-full').style.display = 'inline'; document.getElementById('1404.3823v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1404.3823v1-abstract-full" style="display: none;"> We present a detailed study of new Australia Telescope Compact Array (ATCA) and XMM-Newton observations of LHA 120-N 70 (hereafter N 70), a spherically shaped object in the Large Magellanic Cloud (LMC) classified as a superbubble (SB). Both archival and new observations were used to produce high quality radio-continuum, X-ray and optical images. The radio spectral index of N 70 is estimated to be $伪=-0.12\pm 0.06$ indicating that while a supernova or supernovae have occurred in the region at some time in the distant past, N70 is not the remnant of a single specific supernova. N70 exhibits limited polarisation with a maximum fractional polarisation of 9% in a small area of the north west limb. We estimate the size of N 70 to have a diameter of 104 pc ($\pm 1$ pc). The morphology of N 70 in X-rays closely follows that in radio and optical, with most X-ray emission confined within the bright shell seen at longer wavelengths. Purely thermal models adequately fit the soft X-ray spectrum which lacks harder emission (above 1 keV). We also examine the pressure output of N 70 where the values for the hot (PX) and warm (PHii) phase are consistent with other studied Hii regions. However, the dust-processed radiation pressure (PIR) is significantly smaller than in any other object studied in Lopez et al. (2013). N70 is a very complex region that is likely to have had multiple factors contributing to both the origin and evolution of the entire region. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1404.3823v1-abstract-full').style.display = 'none'; document.getElementById('1404.3823v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 April, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages 8 figures accepted for publication in AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1401.8025">arXiv:1401.8025</a> <span> [<a href="https://arxiv.org/pdf/1401.8025">pdf</a>, <a href="https://arxiv.org/ps/1401.8025">ps</a>, <a href="https://arxiv.org/format/1401.8025">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s10509-014-1825-y">10.1007/s10509-014-1825-y <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radio-continuum study of MCSNR J0536-7038 (DEM L249) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Filipovic%2C+M+D">M. D. Filipovic</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1401.8025v1-abstract-short" style="display: inline;"> We present a detailed radio-continuum study on Australia Telescope Compact Array (ATCA) observations of Large Magellanic Cloud (LMC) supernova remnant (SNR), MCSNR J0536-7038. This Type Ia SNR follows a horseshoe morphology, with a size 32 pc $\times$ 32 pc (1-pc uncertainty in each direction). It exhibits a radio spectrum $伪=-0.52\pm0.07$ between $位= 73$ and 6 cm. We report detections of regions… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.8025v1-abstract-full').style.display = 'inline'; document.getElementById('1401.8025v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1401.8025v1-abstract-full" style="display: none;"> We present a detailed radio-continuum study on Australia Telescope Compact Array (ATCA) observations of Large Magellanic Cloud (LMC) supernova remnant (SNR), MCSNR J0536-7038. This Type Ia SNR follows a horseshoe morphology, with a size 32 pc $\times$ 32 pc (1-pc uncertainty in each direction). It exhibits a radio spectrum $伪=-0.52\pm0.07$ between $位= 73$ and 6 cm. We report detections of regions showing moderately high fractional polarisation at 6 cm, with a peak value of 71$\pm$25% and a mean fractional polarisation of 35$\pm$8%. We also estimate an average rotation measure across the remnant of -237 rad m$^{-2}$. The intrinsic magnetic field appears to be uniformly distributed, extending in the direction of the two brightened limbs of the remnant. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.8025v1-abstract-full').style.display = 'none'; document.getElementById('1401.8025v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 January, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astrophysics and Space Science</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1401.1868">arXiv:1401.1868</a> <span> [<a href="https://arxiv.org/pdf/1401.1868">pdf</a>, <a href="https://arxiv.org/ps/1401.1868">ps</a>, <a href="https://arxiv.org/format/1401.1868">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stu051">10.1093/mnras/stu051 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multi-frequency study of a new Fe-rich supernova remnant in the Large Magellanic Cloud, MCSNR J0508-6902 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Kavanagh%2C+P+J">P. J. Kavanagh</a>, <a href="/search/?searchtype=author&query=Maggi%2C+P">P. Maggi</a>, <a href="/search/?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/?searchtype=author&query=Stupar%2C+M">M. Stupar</a>, <a href="/search/?searchtype=author&query=Parker%2C+Q+A">Q. A. Parker</a>, <a href="/search/?searchtype=author&query=Reid%2C+W+A">W. A. Reid</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Uro%C5%A1evi%C4%87%2C+D">D. Uro拧evi膰</a>, <a href="/search/?searchtype=author&query=Dickel%2C+J">J. Dickel</a>, <a href="/search/?searchtype=author&query=Sturm%2C+R">R. Sturm</a>, <a href="/search/?searchtype=author&query=Williams%2C+R">R. Williams</a>, <a href="/search/?searchtype=author&query=Ehle%2C+M">M. Ehle</a>, <a href="/search/?searchtype=author&query=Gruendl%2C+R">R. Gruendl</a>, <a href="/search/?searchtype=author&query=Chu%2C+Y+-">Y. -H. Chu</a>, <a href="/search/?searchtype=author&query=Points%2C+S">S. Points</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1401.1868v1-abstract-short" style="display: inline;"> We present a detailed radio, X-ray and optical study of a newly discovered Large Magellanic Cloud (LMC) supernova remnant (SNR) which we denote MCSNR J0508-6902. Observations from the Australian Telescope Compact Array (ATCA) and the $\textit{XMM-Newton}$ X-ray observatory are complemented by deep H$伪$ images and Anglo Australian Telescope AAOmega spectroscopic data to study the SNR shell and its… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.1868v1-abstract-full').style.display = 'inline'; document.getElementById('1401.1868v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1401.1868v1-abstract-full" style="display: none;"> We present a detailed radio, X-ray and optical study of a newly discovered Large Magellanic Cloud (LMC) supernova remnant (SNR) which we denote MCSNR J0508-6902. Observations from the Australian Telescope Compact Array (ATCA) and the $\textit{XMM-Newton}$ X-ray observatory are complemented by deep H$伪$ images and Anglo Australian Telescope AAOmega spectroscopic data to study the SNR shell and its shock-ionisation. Archival data at other wavelengths are also examined. The remnant follows a filled-in shell type morphology in the radio-continuum and has a size of $\sim$74 pc $\times$ 57 pc at the LMC distance. The X-ray emission exhibits a faint soft shell morphology with Fe-rich gas in its interior $-$ indicative of a Type Ia origin. The remnant appears to be mostly dissipated at higher radio-continuum frequencies leaving only the south-eastern limb fully detectable while in the optical it is the western side of the SNR shell that is clearly detected. The best-fit temperature to the shell X-ray emission ($kT = 0.41^{+0.05}_{-0.06}$ keV) is consistent with other large LMC SNRs. We determined an O/Fe ratio of $<21$ and an Fe mass of 0.5-1.8$~M_{\odot}$ in the interior of the remnant, both of which are consistent with the Type Ia scenario. We find an equipartition magnetic field for the remnant of $\sim$28 $渭$G, a value typical of older SNRs and consistent with other analyses which also infer an older remnant. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.1868v1-abstract-full').style.display = 'none'; document.getElementById('1401.1868v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 January, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2014. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1312.4790">arXiv:1312.4790</a> <span> [<a href="https://arxiv.org/pdf/1312.4790">pdf</a>, <a href="https://arxiv.org/format/1312.4790">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-637X/780/1/50">10.1088/0004-637X/780/1/50 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A multi-wavelength look at the young plerionic supernova remnant 0540-69.3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Brantseg%2C+T">Thomas Brantseg</a>, <a href="/search/?searchtype=author&query=McEntaffer%2C+R+L">Randall L. McEntaffer</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">Luke M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Filipovic%2C+M">Miroslav Filipovic</a>, <a href="/search/?searchtype=author&query=Grieves%2C+N">Nolan Grieves</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1312.4790v1-abstract-short" style="display: inline;"> We present a study of the plerionic supernova remnant 0540-69.3 in the LMC in X-ray, radio, optical, and infrared. We find that the shell of 0540-69.3 is characterized in the X-ray by thermal nonequilibrium plasma with depleted Mg and Si abundances and a temperature of kT ~ 0.7 keV. This thermal emission is superimposed with synchrotron emission in several regions. Based on X-ray spectra and on mo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1312.4790v1-abstract-full').style.display = 'inline'; document.getElementById('1312.4790v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1312.4790v1-abstract-full" style="display: none;"> We present a study of the plerionic supernova remnant 0540-69.3 in the LMC in X-ray, radio, optical, and infrared. We find that the shell of 0540-69.3 is characterized in the X-ray by thermal nonequilibrium plasma with depleted Mg and Si abundances and a temperature of kT ~ 0.7 keV. This thermal emission is superimposed with synchrotron emission in several regions. Based on X-ray spectra and on morphological considerations in all surveyed wavebands, we conclude that the shell is expanding into a clumpy and highly inhomogeneous medium. In one region of the shell we find an overabundance of Ne, suggesting the presence of ejecta near the edge of the remnant. We also see evidence for reheating of material via a reverse shock originating from the interaction of the supernova blast wave with a particularly dense cloud in the surrounding medium. Finally, we perform the first detailed study of the "halo" region extending 1.2-2.2 pc from the central pulsar. We detect the presence of thermal and nonthermal spectral components but do not find evidence for mixing or ejecta. We conclude that the thermal component is not a counterpart to similar optical and infrared halos and that it is most likely due to the projection of shell material along the line of sight. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1312.4790v1-abstract-full').style.display = 'none'; document.getElementById('1312.4790v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 December, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">35 pages, 17 figures, accepted by ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 780, 50-72, 2014 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1312.3706">arXiv:1312.3706</a> <span> [<a href="https://arxiv.org/pdf/1312.3706">pdf</a>, <a href="https://arxiv.org/ps/1312.3706">ps</a>, <a href="https://arxiv.org/format/1312.3706">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stu499">10.1093/mnras/stu499 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radio-continuum study of Large Magellanic Cloud Supernova Remnant J0509-6731 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Filipovic%2C+M+D">M. D. Filipovic</a>, <a href="/search/?searchtype=author&query=Urosevic%2C+D">D. Urosevic</a>, <a href="/search/?searchtype=author&query=Kothes%2C+R">R. Kothes</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1312.3706v2-abstract-short" style="display: inline;"> We present a detailed study of Australia Telescope Compact Array (ATCA) observations ($位$ = 20, 13, 6 & 3~cm) of supernova remnant (SNR) J0509--6731 in the Large Magellanic Cloud (LMC). The remnant has a ring morphology with brightened regions towards the south-western limb. We also find a second brightened inner ring which is only seen in the radio-continuum. The SNR is almost circular, with a di… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1312.3706v2-abstract-full').style.display = 'inline'; document.getElementById('1312.3706v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1312.3706v2-abstract-full" style="display: none;"> We present a detailed study of Australia Telescope Compact Array (ATCA) observations ($位$ = 20, 13, 6 & 3~cm) of supernova remnant (SNR) J0509--6731 in the Large Magellanic Cloud (LMC). The remnant has a ring morphology with brightened regions towards the south-western limb. We also find a second brightened inner ring which is only seen in the radio-continuum. The SNR is almost circular, with a diameter ranging from 7 to 8~pc, and a steep radio spectral index between 36 and 3~cm of $伪=-0.73\pm0.02$, which is characteristic of younger SNRs. We also report detection of radially orientated polarisation across the remnant at 6~cm, with a mean fractional polarisation level of $P\cong$~(26~$\pm$~13)%. We find the magnetic field ($\sim$168~$渭$G) and $危- D$ ($危= $ $1.1\times 10^{-19}$~W m$^{-2}$~Hz$^{-1}$~sr$^{-1}$ , $D=$ 7.35~pc) to be consistent with other young remnants. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1312.3706v2-abstract-full').style.display = 'none'; document.getElementById('1312.3706v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 March, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 December, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2013. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1310.2569">arXiv:1310.2569</a> <span> [<a href="https://arxiv.org/pdf/1310.2569">pdf</a>, <a href="https://arxiv.org/format/1310.2569">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201322820">10.1051/0004-6361/201322820 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Four new X-ray-selected supernova remnants in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Maggi%2C+P">P. Maggi</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Kavanagh%2C+P+J">P. J. Kavanagh</a>, <a href="/search/?searchtype=author&query=Points%2C+S+D">S. D. Points</a>, <a href="/search/?searchtype=author&query=Dickel%2C+J">J. Dickel</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Chu%2C+Y+-">Y. -H. Chu</a>, <a href="/search/?searchtype=author&query=Gruendl%2C+R+A">R. A. Gruendl</a>, <a href="/search/?searchtype=author&query=Filipovic%2C+M+D">M. D. Filipovic</a>, <a href="/search/?searchtype=author&query=Pietsch%2C+W">W. Pietsch</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1310.2569v1-abstract-short" style="display: inline;"> Aims: We present a detailed multi-wavelength study of four new supernova remnants (SNRs) in the Large Magellanic Cloud (LMC). The objects were identified as SNR candidates in X-ray observations performed during the survey of the LMC with XMM-Newton. Methods: Data obained with XMM-Newton are used to investigate the morphological and spectral features of the remnants in X-rays. We measure the plas… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1310.2569v1-abstract-full').style.display = 'inline'; document.getElementById('1310.2569v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1310.2569v1-abstract-full" style="display: none;"> Aims: We present a detailed multi-wavelength study of four new supernova remnants (SNRs) in the Large Magellanic Cloud (LMC). The objects were identified as SNR candidates in X-ray observations performed during the survey of the LMC with XMM-Newton. Methods: Data obained with XMM-Newton are used to investigate the morphological and spectral features of the remnants in X-rays. We measure the plasma conditions, look for supernova (SN) ejecta emission, and constrain some of the SNR properties (e.g. age and ambient density). We supplement the X-ray data with optical, infrared, and radio-continuum archival observations, which allow us to understand the conditions resulting in the current appearance of the remnants. Based on the spatially-resolved star formation history (SFH) of the LMC together with the X-ray spectra, we attempt to type the supernovae that created the remnants. Results: We confirm all four objects as SNRs, to which we assign the names MCSNR J0508-6830, MCSNR J0511-6759, MCSNR J0514-6840, and MCSNR J0517-6759. In the first two remnants, an X-ray bright plasma is surrounded by very faint [S II] emission. The emission from the central plasma is dominated by Fe L-shell lines, and the derived iron abundance is greatly in excess of solar. This establishes their type Ia (i.e. thermonuclear) SN origin. They appear to be more evolved versions of other Magellanic Cloud iron-rich SNRs which are centrally-peaked in X-rays. From the two other remnants (MCSNR J0514-6840 and MCSNR J0517-6759), we do not see ejecta emission. At all wavelengths at which they are detected, the local environment plays a key role in their observational appearance. We present evidence that MCSNR J0517-6759 is close to and interacting with a molecular cloud, suggesting a massive progenitor. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1310.2569v1-abstract-full').style.display = 'none'; document.getElementById('1310.2569v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 October, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 10 colour Figures, 3 Tables; submitted to Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 561, A76, January 2014 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1304.0495">arXiv:1304.0495</a> <span> [<a href="https://arxiv.org/pdf/1304.0495">pdf</a>, <a href="https://arxiv.org/ps/1304.0495">ps</a>, <a href="https://arxiv.org/format/1304.0495">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stt568">10.1093/mnras/stt568 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multifrequency study of SNR J0533-7202, a new supernova remnant in the LMC </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Maggi%2C+P">P. Maggi</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Uro%C5%A1evi%C4%87%2C+D">D. Uro拧evi膰</a>, <a href="/search/?searchtype=author&query=Payne%2C+J+L">J. L. Payne</a>, <a href="/search/?searchtype=author&query=De+Horta%2C+A+Y">A. Y. De Horta</a>, <a href="/search/?searchtype=author&query=Stupar%2C+M">M. Stupar</a>, <a href="/search/?searchtype=author&query=Gruendl%2C+R">R. Gruendl</a>, <a href="/search/?searchtype=author&query=Dickel%2C+J">J. Dickel</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1304.0495v1-abstract-short" style="display: inline;"> We present a detailed study of Australia Telescope Compact Array (ATCA) observations of a newly discovered Large Magellanic Cloud (LMC) supernova remnant (SNR), SNR J0533-7202. This object follows a horseshoe morphology, with a size 37 pc x 28 pc (1-pc uncertainty in each direction). It exhibits a radio spectrum with the intrinsic synchrotron spectral index of alpha= -0.47+-0.06 between 73 and 6 c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1304.0495v1-abstract-full').style.display = 'inline'; document.getElementById('1304.0495v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1304.0495v1-abstract-full" style="display: none;"> We present a detailed study of Australia Telescope Compact Array (ATCA) observations of a newly discovered Large Magellanic Cloud (LMC) supernova remnant (SNR), SNR J0533-7202. This object follows a horseshoe morphology, with a size 37 pc x 28 pc (1-pc uncertainty in each direction). It exhibits a radio spectrum with the intrinsic synchrotron spectral index of alpha= -0.47+-0.06 between 73 and 6 cm. We report detections of regions showing moderately high fractional polarisation at 6 cm, with a peak value of 36+-6% and a mean fractional polarisation of 12+-7%. We also estimate an average rotation measure across the remnant of -591 rad m^-2. The current lack of deep X-ray observation precludes any conclusion about high-energy emission from the remnant. The association with an old stellar population favours a thermonuclear supernova origin of the remnant. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1304.0495v1-abstract-full').style.display = 'none'; document.getElementById('1304.0495v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 April, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 5 figures accepted to Monthly Notices of the Royal Astronomical Society</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1211.4746">arXiv:1211.4746</a> <span> [<a href="https://arxiv.org/pdf/1211.4746">pdf</a>, <a href="https://arxiv.org/format/1211.4746">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201220431">10.1051/0004-6361/201220431 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multiwavelength study of the newly confirmed supernova remnant MCSNR J0527-7104 in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kavanagh%2C+P+J">Patrick J. Kavanagh</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">Manami Sasaki</a>, <a href="/search/?searchtype=author&query=Points%2C+S+D">Sean D. Points</a>, <a href="/search/?searchtype=author&query=Filipovi%C4%87%2C+M+D">Miroslav D. Filipovi膰</a>, <a href="/search/?searchtype=author&query=Maggi%2C+P">Pierre Maggi</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">Luke M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">Evan J. Crawford</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">Frank Haberl</a>, <a href="/search/?searchtype=author&query=Pietsch%2C+W">Wolfgang Pietsch</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1211.4746v1-abstract-short" style="display: inline;"> The Large Magellanic Cloud (LMC) hosts a rich and varied population of supernova remnants (SNRs). Optical, X-ray, and radio observations are required to identify these SNRs, as well as to ascertain the various processes responsible for the large array of physical characteristics observed. In this paper we attempted to confirm the candidate SNR [HP99] 1234, identified in X-rays with ROSAT, as a tru… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1211.4746v1-abstract-full').style.display = 'inline'; document.getElementById('1211.4746v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1211.4746v1-abstract-full" style="display: none;"> The Large Magellanic Cloud (LMC) hosts a rich and varied population of supernova remnants (SNRs). Optical, X-ray, and radio observations are required to identify these SNRs, as well as to ascertain the various processes responsible for the large array of physical characteristics observed. In this paper we attempted to confirm the candidate SNR [HP99] 1234, identified in X-rays with ROSAT, as a true SNR by supplementing these X-ray data with optical and radio observations. Optical data from the Magellanic Cloud Emission Line Survey (MCELS) and new radio data from the Molonglo Observatory Synthesis Telescope (MOST), in addition to the ROSAT X-ray data, were used to perform a morphological analysis of this candidate SNR. An approximately ellipsoidal shell of enhanced [SII], typical of an SNR ([SII]/Halpha > 0.4), was detected in the optical. This enhancement is coincident with faint radio emission at 36 cm. Using the available data we estimated the size of the remnant to be ~5.1' x 4.0' (~75 pc x 59 pc). However, the measurement along the major-axis was somewhat uncertain due to a lack of optical and radio emission at its extremities and the poor resolution of the X-ray data. Assuming this SNR is in the Sedov phase and adopting the ambient mass density of 1.2x10^-25 g cm^-3 measured in a nearby HII region, an age estimate of ~25 kyr was calculated for a canonical initial explosion energy of 10^51 erg. However, this age estimate should be treated cautiously due to uncertainties on the adopted parameters. Analysis of the local stellar population suggested a type Ia event as a precursor to this SNR, however, a core-collapse mechanism could not be ruled out due to the possibility of the progenitor being a runaway massive star. With the detection of X-ray, radio and optical line emission with enhanced [SII], this object was confirmed as an SNR and we assign the identifier MCSNR J0527-7104. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1211.4746v1-abstract-full').style.display = 'none'; document.getElementById('1211.4746v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 November, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 6 figures. Accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1211.1744">arXiv:1211.1744</a> <span> [<a href="https://arxiv.org/pdf/1211.1744">pdf</a>, <a href="https://arxiv.org/ps/1211.1744">ps</a>, <a href="https://arxiv.org/format/1211.1744">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.2298/SAJ1285025B">10.2298/SAJ1285025B <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radio-Continuum Observations Of Small, Radially Polarised Supernova Remnant J0519-6902 In The Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/?searchtype=author&query=Uro%C5%A1evi%C4%87%2C+D">D. Uro拧evi膰</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1211.1744v1-abstract-short" style="display: inline;"> We report on new Australian Telescope Compact Array (ATCA) observations of SNR J0519-6902. The Supernova Remnant (SNR) is small in size (~8 pc) and exhibits a typical SNR spectrum of alpha = -0.53 +- 0.07, with steeper spectral indices found towards the northern limb of the remnant. SNR J0519-6902 contains a low level of radially orientated polarisation at wavelengths of 3 & 6 cm, which is charact… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1211.1744v1-abstract-full').style.display = 'inline'; document.getElementById('1211.1744v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1211.1744v1-abstract-full" style="display: none;"> We report on new Australian Telescope Compact Array (ATCA) observations of SNR J0519-6902. The Supernova Remnant (SNR) is small in size (~8 pc) and exhibits a typical SNR spectrum of alpha = -0.53 +- 0.07, with steeper spectral indices found towards the northern limb of the remnant. SNR J0519-6902 contains a low level of radially orientated polarisation at wavelengths of 3 & 6 cm, which is characteristic of younger SNRs. A fairly strong magnetic field was estimated of ~171 microG. The remnant appears to be the result of a typical Type Ia supernovae, sharing many properties as another small and young Type Ia LMC SNR, J0509-6731. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1211.1744v1-abstract-full').style.display = 'none'; document.getElementById('1211.1744v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 November, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages 7 figures, submitted to Serbian Astronomical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1208.0182">arXiv:1208.0182</a> <span> [<a href="https://arxiv.org/pdf/1208.0182">pdf</a>, <a href="https://arxiv.org/ps/1208.0182">ps</a>, <a href="https://arxiv.org/format/1208.0182">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201219708">10.1051/0004-6361/201219708 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multi-frequency study of supernova remnants in the Large Magellanic Cloud. Confirmation of the supernova remnant status of DEM L205 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Maggi%2C+P">P. Maggi</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/?searchtype=author&query=Points%2C+S+D">S. D. Points</a>, <a href="/search/?searchtype=author&query=Chu%2C+Y+-">Y. -H. Chu</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Pietsch%2C+W">W. Pietsch</a>, <a href="/search/?searchtype=author&query=Gruendl%2C+R+A">R. A. Gruendl</a>, <a href="/search/?searchtype=author&query=Dickel%2C+J">J. Dickel</a>, <a href="/search/?searchtype=author&query=Smith%2C+R+C">R. C. Smith</a>, <a href="/search/?searchtype=author&query=Sturm%2C+R">R. Sturm</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/?searchtype=author&query=De+Horta%2C+A+Y">A. Y. De Horta</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1208.0182v1-abstract-short" style="display: inline;"> We present new X-ray and radio data of the LMC SNR candidate DEM L205, obtained by XMM-Newton and ATCA, along with archival optical and infrared observations. We use data at various wavelengths to study this object and its complex neighbourhood, in particular in the context of the star formation activity, past and present, around the source. We analyse the X-ray spectrum to derive some remnant's p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1208.0182v1-abstract-full').style.display = 'inline'; document.getElementById('1208.0182v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1208.0182v1-abstract-full" style="display: none;"> We present new X-ray and radio data of the LMC SNR candidate DEM L205, obtained by XMM-Newton and ATCA, along with archival optical and infrared observations. We use data at various wavelengths to study this object and its complex neighbourhood, in particular in the context of the star formation activity, past and present, around the source. We analyse the X-ray spectrum to derive some remnant's properties, such as age and explosion energy. Supernova remnant features are detected at all observed wavelengths: soft and extended X-ray emission is observed, arising from a thermal plasma with a temperature kT between 0.2 keV and 0.3 keV. Optical line emission is characterised by an enhanced [SII]/Halpha ratio and a shell-like morphology, correlating with the X-ray emission. The source is not or only tentatively detected at near-infrared wavelengths (< 10 microns), but there is a detection of arc-like emission at mid and far-infrared wavelengths (24 and 70 micron) that can be unambiguously associated with the remnant. We suggest that thermal emission from dust heated by stellar radiation and shock waves is the main contributor to the infrared emission. Finally, an extended and faint non-thermal radio emission correlates with the remnant at other wavelengths and we find a radio spectral index between -0.7 and -0.9, within the range for SNRs. The size of the remnant is ~79x64 pc and we estimate a dynamical age of about 35000 years. We definitely confirm DEM L205 as a new SNR. This object ranks amongst the largest remnants known in the LMC. The numerous massive stars and the recent outburst in star formation around the source strongly suggest that a core-collapse supernova is the progenitor of this remnant. (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1208.0182v1-abstract-full').style.display = 'none'; document.getElementById('1208.0182v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 August, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 6 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astronomy and Astrophysics, Volume 546, A109, October 2012 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1206.5679">arXiv:1206.5679</a> <span> [<a href="https://arxiv.org/pdf/1206.5679">pdf</a>, <a href="https://arxiv.org/ps/1206.5679">ps</a>, <a href="https://arxiv.org/format/1206.5679">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201218971">10.1051/0004-6361/201218971 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multi-frequency observations of SNR J0453-6829 in the LMC; A composite supernova remnant with a pulsar wind nebula </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Filipovic%2C+M+D">M. D. Filipovic</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/?searchtype=author&query=Points%2C+S+D">S. D. Points</a>, <a href="/search/?searchtype=author&query=Pietsch%2C+W">W. Pietsch</a>, <a href="/search/?searchtype=author&query=De+Horta%2C+A+Y">A. Y. De Horta</a>, <a href="/search/?searchtype=author&query=Tothill%2C+N">N. Tothill</a>, <a href="/search/?searchtype=author&query=Payne%2C+J+L">J. L. Payne</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1206.5679v1-abstract-short" style="display: inline;"> The Large Magellanic Cloud (LMC) is rich in supernova remnants (SNRs) which can be investigated in detail with radio, optical and X-ray observations. SNR J0453-6829 is an X-ray and radio-bright remnant in the LMC, within which previous studies revealed the presence of a pulsar wind nebula (PWN), making it one of the most interesting SNRs in the Local Group of galaxies. We study the emission of SNR… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1206.5679v1-abstract-full').style.display = 'inline'; document.getElementById('1206.5679v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1206.5679v1-abstract-full" style="display: none;"> The Large Magellanic Cloud (LMC) is rich in supernova remnants (SNRs) which can be investigated in detail with radio, optical and X-ray observations. SNR J0453-6829 is an X-ray and radio-bright remnant in the LMC, within which previous studies revealed the presence of a pulsar wind nebula (PWN), making it one of the most interesting SNRs in the Local Group of galaxies. We study the emission of SNR J0453-6829 to improve our understanding of its morphology, spectrum, and thus the emission mechanisms in the shell and the PWN of the remnant. We obtained new radio data with the Australia Telescope Compact Array and analysed archival XMM-Newton observations of SNR J0453-6829. We studied the morphology of SNR J0453-6829 from radio, optical and X-ray images and investigated the energy spectra in the different parts of the remnant. Our radio results confirm that this LMC SNR hosts a typical PWN. The prominent central core of the PWN exhibits a radio spectral index alpha_Core of -0.04+/-0.04, while in the rest of the SNR shell the spectral slope is somewhat steeper with alpha_Shell = -0.43+/-0.01. We detect regions with a mean polarisation of P ~ (12+/-4)% at 6 cm and (9+/-2)% at 3 cm. The full remnant is of roughly circular shape with dimensions of (31+/-1) pc x (29+/-1) pc. The spectral analysis of the XMM-Newton EPIC and RGS spectra allowed us to derive physical parameters for the SNR. Somewhat depending on the spectral model, we obtain for the remnant a shock temperature of around 0.2 keV and estimate the dynamical age to 12000-15000 years. Using a Sedov model we further derive an electron density in the X-ray emitting material of 1.56 cm^-3, typical for LMC remnants, a large swept-up mass of 830 solar masses, and an explosion energy of 7.6 x 10^50 erg. These parameters indicate a well evolved SNR with an X-ray spectrum dominated by emission from the swept-up material. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1206.5679v1-abstract-full').style.display = 'none'; document.getElementById('1206.5679v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 June, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A, 7 pages, 8 figures, figure 5 with lower resolution</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1205.1259">arXiv:1205.1259</a> <span> [<a href="https://arxiv.org/pdf/1205.1259">pdf</a>, <a href="https://arxiv.org/ps/1205.1259">ps</a>, <a href="https://arxiv.org/format/1205.1259">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.2298/SAJ1284069B">10.2298/SAJ1284069B <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multifrequency radio observations of SNR J0536-6735 (N 59B) with associated pulsar </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/?searchtype=author&query=De+Horta%2C+A+Y">A. Y. De Horta</a>, <a href="/search/?searchtype=author&query=Stupar%2C+M">M. Stupar</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1205.1259v1-abstract-short" style="display: inline;"> We present a study of new Australian Telescope Compact Array (ATCA) observations of supernova remnant, SNR J0536-6735. This remnant appears to follow a shell morphology with a diameter of D=36x29 pc (with 1 pc uncertainty in each direction). There is an embedded Hii region on the northern limb of the remnant which made various analysis and measurements (such as flux density, spectral index and pol… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1205.1259v1-abstract-full').style.display = 'inline'; document.getElementById('1205.1259v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1205.1259v1-abstract-full" style="display: none;"> We present a study of new Australian Telescope Compact Array (ATCA) observations of supernova remnant, SNR J0536-6735. This remnant appears to follow a shell morphology with a diameter of D=36x29 pc (with 1 pc uncertainty in each direction). There is an embedded Hii region on the northern limb of the remnant which made various analysis and measurements (such as flux density, spectral index and polarisation) difficult. The radio-continuum emission followed the same structure as the optical emission, allowing for extent and flux density estimates at 20 cm. We estimate a surface brightness for the SNR at 1 GHz of 2.55x10^-21 W m^-2 Hz^-1 sr^-1. Also, we detect a distinctive radio-continuum point source which confirms the previous suggestion of this remnant being associated with a pulsar wind nebulae (PWN). The tail of this remnant isn't seen in the radio-continuum images and is only seen in the optical and X-ray images. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1205.1259v1-abstract-full').style.display = 'none'; document.getElementById('1205.1259v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 May, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages 4 figures, accepted for publication in SAJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1202.2618">arXiv:1202.2618</a> <span> [<a href="https://arxiv.org/pdf/1202.2618">pdf</a>, <a href="https://arxiv.org/format/1202.2618">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201118694">10.1051/0004-6361/201118694 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multi-Frequency Study of Supernova Remnants in the Large Magellanic Cloud. The case of LMC SNR J0530-7007 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=De+Horta%2C+A+Y">A. Y. De Horta</a>, <a href="/search/?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Maggi%2C+P">P. Maggi</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Urosevi%C4%87%2C+D">D. Urosevi膰</a>, <a href="/search/?searchtype=author&query=Pietsch%2C+W">W. Pietsch</a>, <a href="/search/?searchtype=author&query=Gruendl%2C+R">R. Gruendl</a>, <a href="/search/?searchtype=author&query=Dickel%2C+J">J. Dickel</a>, <a href="/search/?searchtype=author&query=Tothill%2C+N+F+H">N. F. H. Tothill</a>, <a href="/search/?searchtype=author&query=Chu%2C+Y+-">Y. -H. Chu</a>, <a href="/search/?searchtype=author&query=Payne%2C+J+L">J. L. Payne</a>, <a href="/search/?searchtype=author&query=Collier%2C+J+D">J. D. Collier</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1202.2618v1-abstract-short" style="display: inline;"> Context: The Supernova Remnants (SNRs) known in the Large Magellanic Cloud (LMC) show a variety of morphological structures in the different wavelength bands. This variety is the product of the conditions in the surrounding medium with which the remnant interacts and the inherent circumstances of the supernova event itself. Aims: This paper performs a multi-frequency study of the LMC SNR J0530-7… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1202.2618v1-abstract-full').style.display = 'inline'; document.getElementById('1202.2618v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1202.2618v1-abstract-full" style="display: none;"> Context: The Supernova Remnants (SNRs) known in the Large Magellanic Cloud (LMC) show a variety of morphological structures in the different wavelength bands. This variety is the product of the conditions in the surrounding medium with which the remnant interacts and the inherent circumstances of the supernova event itself. Aims: This paper performs a multi-frequency study of the LMC SNR J0530-7007 by combining Australia Telescope Compact Array (ATCA), Molonglo Observatory Synthesis Telescope (MOST), R枚ntgensatellit (ROSAT) and Magellanic Clouds Emission Line Survey (MCELS) observations. Methods: We analysed radio-continuum, X-ray and optical data and present a multi-wavelength morphological study of LMC SNR J0530-7007. Results We find that this object has a shell-type morphology with a size of 215"x180" (52 pc x 44 pc); a radio spectral index (alpha=-0.85+-0.13); with [Sii]/Halpha > 0.4 in the optical; and the presence of non-thermal radio and X-ray emission. Conclusions: We confirmed this object as a bona-fide shell-type SNR which is probably a result of a Type Ia supernova. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1202.2618v1-abstract-full').style.display = 'none'; document.getElementById('1202.2618v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 February, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 8 figures accepted by A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1201.1082">arXiv:1201.1082</a> <span> [<a href="https://arxiv.org/pdf/1201.1082">pdf</a>, <a href="https://arxiv.org/ps/1201.1082">ps</a>, <a href="https://arxiv.org/format/1201.1082">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201117881">10.1051/0004-6361/201117881 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> XMMU J0541.8-6659, a new supernova remnant in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Grondin%2C+M+-">M. -H. Grondin</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Pietsch%2C+W">W. Pietsch</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/?searchtype=author&query=Filipovic%2C+M+D">M. D. Filipovic</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Points%2C+S">S. Points</a>, <a href="/search/?searchtype=author&query=Smith%2C+R+C">R. C. Smith</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1201.1082v1-abstract-short" style="display: inline;"> The high sensitivity of the XMM-Newton instrumentation offers the opportunity to study faint and extended sources in the Milky Way and nearby galaxies such as the Large Magellanic Cloud (LMC) in detail. The ROSAT PSPC survey of the LMC has revealed more than 700 X-ray sources, among which there are 46 supernova remnants (SNRs) and candidates. We have observed the field around one of the most promi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.1082v1-abstract-full').style.display = 'inline'; document.getElementById('1201.1082v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1201.1082v1-abstract-full" style="display: none;"> The high sensitivity of the XMM-Newton instrumentation offers the opportunity to study faint and extended sources in the Milky Way and nearby galaxies such as the Large Magellanic Cloud (LMC) in detail. The ROSAT PSPC survey of the LMC has revealed more than 700 X-ray sources, among which there are 46 supernova remnants (SNRs) and candidates. We have observed the field around one of the most promising SNR candidates in the ROSAT PSPC catalogue, labelled [HP99] 456 with XMM-Newton, to determine its nature. We investigated the XMM-Newton data along with new radio-continuum, near infrared and optical data. In particular, spectral and morphological studies of the X-ray and radio data were performed. The X-ray images obtained in different energy bands reveal two different structures. Below 1.0 keV the X-ray emission shows the shell-like morphology of an SNR with a diameter of ~73 pc, one of the largest known in the LMC. For its thermal spectrum we estimate an electron temperature of (0.49 +/- 0.12)keV assuming non-equilibrium ionisation. The X-ray images above 1.0 keV reveal a less extended source within the SNR emission, located ~1' west of the centre of the SNR and coincident with bright point sources detected in radio-continuum. This hard component has an extent of 0.9' (i.e. ~13 pc at a distance of ~50 kpc) and a non-thermal spectrum. The hard source coincides in position with the ROSAT source [HP99] 456 and shows an indication for substructure. We firmly identify a new SNR in the LMC with a shell-like morphology and a thermal spectrum. Assuming the SNR to be in the Sedov phase yields an age of ~23 kyr. We explore possible associations of the hard non-thermal emitting component with a pulsar wind nebula (PWN) or background active galactic nuclei (AGN). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.1082v1-abstract-full').style.display = 'none'; document.getElementById('1201.1082v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 January, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 7 figures, accepted for publication in Astronomy and Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1111.6649">arXiv:1111.6649</a> <span> [<a href="https://arxiv.org/pdf/1111.6649">pdf</a>, <a href="https://arxiv.org/format/1111.6649">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1111/j.1365-2966.2011.20231.x">10.1111/j.1365-2966.2011.20231.x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multi-frequency study of the Large Magellanic Cloud Supernova Remnant J0529-6653 near Pulsar B0529-66 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Urosevi%C4%87%2C+D">D. Urosevi膰</a>, <a href="/search/?searchtype=author&query=Pietsch%2C+W">W. Pietsch</a>, <a href="/search/?searchtype=author&query=Payne%2C+J+L">J. L. Payne</a>, <a href="/search/?searchtype=author&query=De+Horta%2C+A+Y">A. Y. De Horta</a>, <a href="/search/?searchtype=author&query=Stupar%2C+M">M. Stupar</a>, <a href="/search/?searchtype=author&query=Tothill%2C+N">N. Tothill</a>, <a href="/search/?searchtype=author&query=Dickel%2C+J">J. Dickel</a>, <a href="/search/?searchtype=author&query=Chu%2C+Y+-">Y. -H. Chu</a>, <a href="/search/?searchtype=author&query=Gruendl%2C+R">R. Gruendl</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1111.6649v1-abstract-short" style="display: inline;"> We report the ATCA and ROSAT detection of Supernova Remnant (SNR) J0529--6653 in the Large Magellanic Cloud (LMC) which is positioned in the projected vicinity of the known radio pulsar PSR B0529-66. In the radio-continuum frequencies, this LMC object follows a typical SNR structure of a shell morphology with brightened regions in the south-west. It exhibits an almost circular shape of D=33 x 31 p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.6649v1-abstract-full').style.display = 'inline'; document.getElementById('1111.6649v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1111.6649v1-abstract-full" style="display: none;"> We report the ATCA and ROSAT detection of Supernova Remnant (SNR) J0529--6653 in the Large Magellanic Cloud (LMC) which is positioned in the projected vicinity of the known radio pulsar PSR B0529-66. In the radio-continuum frequencies, this LMC object follows a typical SNR structure of a shell morphology with brightened regions in the south-west. It exhibits an almost circular shape of D=33 x 31 pc (1 pc uncertainty in each direction) and radio spectral index of alpha=-0.68$+-$0.03 - typical for mid-age SNRs. We also report detection of polarised regions with a peak value of 17+-7% at 6 cm. An investigation of ROSAT images produced from merged PSPC data reveals the presence of extended X-ray emission coincident with the radio emission of the SNR. In X-rays, the brightest part is in the north-east. We discuss various scenarios in regards to the SNR-PSR association with emphasis on the large age difference, lack of a pulsar trail and no prominent point-like radio or X-ray source. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.6649v1-abstract-full').style.display = 'none'; document.getElementById('1111.6649v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 November, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 9 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1109.3945">arXiv:1109.3945</a> <span> [<a href="https://arxiv.org/pdf/1109.3945">pdf</a>, <a href="https://arxiv.org/ps/1109.3945">ps</a>, <a href="https://arxiv.org/format/1109.3945">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Radio continuum observations of LMC SNR J0550-6823 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/?searchtype=author&query=Payne%2C+J+L">J. L. Payne</a>, <a href="/search/?searchtype=author&query=De+Horta%2C+A+Y">A. Y. De Horta</a>, <a href="/search/?searchtype=author&query=Stupar%2C+M">M. Stupar</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1109.3945v1-abstract-short" style="display: inline;"> We report on new Australia Telescope Compact Array (ATCA) observations of the Large Magellanic Cloud (LMC) supernova remnant (SNR) J0550-6823 (DEM L328). This object is a typical horseshoe SNR with a diameter of 373" x 282" +- 4" (90 x 68 +- 1), making it one of the largest known SNRs in the Local Group. We estimate a relatively steep radio spectral index of alpha = -0.79 +- 0.27. However, its str… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1109.3945v1-abstract-full').style.display = 'inline'; document.getElementById('1109.3945v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1109.3945v1-abstract-full" style="display: none;"> We report on new Australia Telescope Compact Array (ATCA) observations of the Large Magellanic Cloud (LMC) supernova remnant (SNR) J0550-6823 (DEM L328). This object is a typical horseshoe SNR with a diameter of 373" x 282" +- 4" (90 x 68 +- 1), making it one of the largest known SNRs in the Local Group. We estimate a relatively steep radio spectral index of alpha = -0.79 +- 0.27. However, its stronger than expected polarisation of 50% +- 10% is atypical for older and more evolved SNRs. We also note a strong correlation between [Oiii] and radio images, classifying this SNR as oxygen dominant. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1109.3945v1-abstract-full').style.display = 'none'; document.getElementById('1109.3945v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 September, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 5 figures, submitted to Revista Mexicana de Astronomia y Astrofisica</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1009.2816">arXiv:1009.2816</a> <span> [<a href="https://arxiv.org/pdf/1009.2816">pdf</a>, <a href="https://arxiv.org/ps/1009.2816">ps</a>, <a href="https://arxiv.org/format/1009.2816">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.2298/SAJ1081043B">10.2298/SAJ1081043B <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multifrequency Radio Observations of a SNR in the LMC. The Case of SNR J0527-6549 (DEM l204) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/?searchtype=author&query=Bojici%C4%87%2C+I+S">I. S. Bojici膰</a>, <a href="/search/?searchtype=author&query=Mendik%2C+A">A. Mendik</a>, <a href="/search/?searchtype=author&query=Wardlaw%2C+B">B. Wardlaw</a>, <a href="/search/?searchtype=author&query=Payne%2C+J+L">J. L. Payne</a>, <a href="/search/?searchtype=author&query=De+Horta%2C+A+Y">A. Y. De Horta</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1009.2816v1-abstract-short" style="display: inline;"> We present a detailed study and results of new Australia Telescope Compact Array (ATCA) observations of supernova remnant, SNR J0527-6549. This Large Magellanic Cloud (LMC) ob ject follows a typical supernova remnant (SNR) horseshoe morphology with a diameter of D=(66x58)+-1 pc which is among the largest SNRs in the LMC. Its relatively large size indicates older age while a steeper than expected r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1009.2816v1-abstract-full').style.display = 'inline'; document.getElementById('1009.2816v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1009.2816v1-abstract-full" style="display: none;"> We present a detailed study and results of new Australia Telescope Compact Array (ATCA) observations of supernova remnant, SNR J0527-6549. This Large Magellanic Cloud (LMC) ob ject follows a typical supernova remnant (SNR) horseshoe morphology with a diameter of D=(66x58)+-1 pc which is among the largest SNRs in the LMC. Its relatively large size indicates older age while a steeper than expected radio spectral index of aplha=-0.92+-0.11 is more typical for younger and energetic SNRs. Also, we report detections of regions with a high order of polarization at a peak value of ~54+-17% at 6 cm. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1009.2816v1-abstract-full').style.display = 'none'; document.getElementById('1009.2816v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 September, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 Pages, 6 figures, accepted for publication in SAJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0806.3605">arXiv:0806.3605</a> <span> [<a href="https://arxiv.org/pdf/0806.3605">pdf</a>, <a href="https://arxiv.org/ps/0806.3605">ps</a>, <a href="https://arxiv.org/format/0806.3605">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.2298/SAJ140605001H">10.2298/SAJ140605001H <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radio-Continuum Emission From The Young Galactic Supernova Remnant G1.9+0.3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=De+Horta%2C+A+Y">A. Y. De Horta</a>, <a href="/search/?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/?searchtype=author&query=Stootman%2C+F+H">F. H. Stootman</a>, <a href="/search/?searchtype=author&query=Pannuti%2C+T+G">T. G. Pannuti</a>, <a href="/search/?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/?searchtype=author&query=Collier%2C+J+D">J. D. Collier</a>, <a href="/search/?searchtype=author&query=Sommer%2C+E+R">E. R. Sommer</a>, <a href="/search/?searchtype=author&query=Kosakowski%2C+A+R">A. R. Kosakowski</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0806.3605v3-abstract-short" style="display: inline;"> We present an analysis of a new Australia Telescope Compact Array (ATCA) radio-continuum observation of supernova remnant (SNR) G1.9+0.3, which at an age of $\sim$181$\pm$25 years is the youngest known in the Galaxy. We analysed all available radio-continuum observations at 6-cm from the ATCA and the Very Large Array. Using this data we estimate an expansion rate for G1.9+0.3 of 0.563%$\pm$0.078%… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0806.3605v3-abstract-full').style.display = 'inline'; document.getElementById('0806.3605v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0806.3605v3-abstract-full" style="display: none;"> We present an analysis of a new Australia Telescope Compact Array (ATCA) radio-continuum observation of supernova remnant (SNR) G1.9+0.3, which at an age of $\sim$181$\pm$25 years is the youngest known in the Galaxy. We analysed all available radio-continuum observations at 6-cm from the ATCA and the Very Large Array. Using this data we estimate an expansion rate for G1.9+0.3 of 0.563%$\pm$0.078% per year between 1984 and 2009. We note that in the 1980's G1.9+0.3 expanded somewhat slower (0.484% per year) than more recently (0.641% per year). We estimate that the average spectral index between 20-cm and 6-cm, across the entire SNR is $伪=-0.72\pm 0.26$ which is typical for younger SNRs. At 6-cm, we detect an average of 6% fractionally polarised radio emission with a peak of 17%$\pm$3%. The polarised emission follows the contours of the strongest of X-ray emission. Using the new equipartition formula we estimate a magnetic field strength of B$\approx 273渭$G, which to date, is one of the highest magnetic field strength found for any SNR and consistent with G1.9+0.3 being a very young remnant. This magnetic field strength implies a minimum total energy of the synchrotron radiation of E$_{\textrm{min}} \approx$ 1.8$\times$10$^{48}$ ergs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0806.3605v3-abstract-full').style.display = 'none'; document.getElementById('0806.3605v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 June, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2008. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">As accepted by Serbian Astronomical Journal</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a 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