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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Riggi%2C+S&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Riggi%2C+S&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Riggi%2C+S&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.14078">arXiv:2411.14078</a> <span> [<a href="https://arxiv.org/pdf/2411.14078">pdf</a>, <a href="https://arxiv.org/format/2411.14078">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Computer Vision and Pattern Recognition">cs.CV</span> </div> </div> <p class="title is-5 mathjax"> Self-supervised learning for radio-astronomy source classification: a benchmark </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cecconello%2C+T">Thomas Cecconello</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">Simone Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Becciani%2C+U">Ugo Becciani</a>, <a href="/search/astro-ph?searchtype=author&query=Vitello%2C+F">Fabio Vitello</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">Andrew M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Vizzari%2C+G">Giuseppe Vizzari</a>, <a href="/search/astro-ph?searchtype=author&query=Spampinato%2C+C">Concetto Spampinato</a>, <a href="/search/astro-ph?searchtype=author&query=Palazzo%2C+S">Simone Palazzo</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="2411.14078v2-abstract-short" style="display: inline;"> The upcoming Square Kilometer Array (SKA) telescope marks a significant step forward in radio astronomy, presenting new opportunities and challenges for data analysis. Traditional visual models pretrained on optical photography images may not perform optimally on radio interferometry images, which have distinct visual characteristics. Self-Supervised Learning (SSL) offers a promising approach to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.14078v2-abstract-full').style.display = 'inline'; document.getElementById('2411.14078v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.14078v2-abstract-full" style="display: none;"> The upcoming Square Kilometer Array (SKA) telescope marks a significant step forward in radio astronomy, presenting new opportunities and challenges for data analysis. Traditional visual models pretrained on optical photography images may not perform optimally on radio interferometry images, which have distinct visual characteristics. Self-Supervised Learning (SSL) offers a promising approach to address this issue, leveraging the abundant unlabeled data in radio astronomy to train neural networks that learn useful representations from radio images. This study explores the application of SSL to radio astronomy, comparing the performance of SSL-trained models with that of traditional models pretrained on natural images, evaluating the importance of data curation for SSL, and assessing the potential benefits of self-supervision to different domain-specific radio astronomy datasets. Our results indicate that, SSL-trained models achieve significant improvements over the baseline in several downstream tasks, especially in the linear evaluation setting; when the entire backbone is fine-tuned, the benefits of SSL are less evident but still outperform pretraining. These findings suggest that SSL can play a valuable role in efficiently enhancing the analysis of radio astronomical data. The trained models and code is available at: \url{https://github.com/dr4thmos/solo-learn-radio} <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.14078v2-abstract-full').style.display = 'none'; document.getElementById('2411.14078v2-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.08519">arXiv:2411.08519</a> <span> [<a href="https://arxiv.org/pdf/2411.08519">pdf</a>, <a href="https://arxiv.org/ps/2411.08519">ps</a>, <a href="https://arxiv.org/format/2411.08519">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Detection and classification of radio sources with deep learning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Cecconello%2C+T">T. Cecconello</a>, <a href="/search/astro-ph?searchtype=author&query=Becciani%2C+U">U. Becciani</a>, <a href="/search/astro-ph?searchtype=author&query=Vitello%2C+F">F. Vitello</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="2411.08519v1-abstract-short" style="display: inline;"> In this paper we present three different applications, based on deep learning methodologies, that we are developing to support the scientific analysis conducted within the ASKAP-EMU and MeerKAT radio surveys. One employs instance segmentation frameworks to detect compact and extended radio sources and imaging artefacts from radio continuum images. Another application uses gradient boosting decisio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.08519v1-abstract-full').style.display = 'inline'; document.getElementById('2411.08519v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.08519v1-abstract-full" style="display: none;"> In this paper we present three different applications, based on deep learning methodologies, that we are developing to support the scientific analysis conducted within the ASKAP-EMU and MeerKAT radio surveys. One employs instance segmentation frameworks to detect compact and extended radio sources and imaging artefacts from radio continuum images. Another application uses gradient boosting decision trees and convolutional neural networks to classify compact sources into different astronomical classes using combined radio and infrared multi-band images. Finally, we discuss how self-supervised learning can be used to obtain valuable radio data representations for source detection, and classification studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.08519v1-abstract-full').style.display = 'none'; document.getElementById('2411.08519v1-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> 13 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </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">4 pages, 0 figures, proceedings of the XXXIII Astronomical Data Analysis Software & Systems (ADASS) conference, 5-9 November 2023, Tucson, Arizona, USA</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.16607">arXiv:2409.16607</a> <span> [<a href="https://arxiv.org/pdf/2409.16607">pdf</a>, <a href="https://arxiv.org/format/2409.16607">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> <p class="title is-5 mathjax"> Supernova Remnant Candidates Discovered by the SARAO MeerKAT Galactic Plane Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+L+D">L. D. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Faerber%2C+T">Timothy Faerber</a>, <a href="/search/astro-ph?searchtype=author&query=Bietenholz%2C+M">M. Bietenholz</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Chibueze%2C+J+O">J. O. Chibueze</a>, <a href="/search/astro-ph?searchtype=author&query=Cotton%2C+W+D">W. D. Cotton</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Rigby%2C+A">A. Rigby</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+M+A">M. A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+G+M">G. M. Williams</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="2409.16607v1-abstract-short" style="display: inline;"> Context. Sensitive radio continuum data could remove the difference between the number of known supernova remnants (SNRs) in the Galaxy compared to that expected, but due to confusion in the Galactic plane, faint SNRs can be challenging to distinguish from brighter HII regions and filamentary radio emission. Aims. We wish to exploit new SARAO MeerKAT 1.3 GHz Galactic Plane Survey (SMGPS) radio con… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.16607v1-abstract-full').style.display = 'inline'; document.getElementById('2409.16607v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.16607v1-abstract-full" style="display: none;"> Context. Sensitive radio continuum data could remove the difference between the number of known supernova remnants (SNRs) in the Galaxy compared to that expected, but due to confusion in the Galactic plane, faint SNRs can be challenging to distinguish from brighter HII regions and filamentary radio emission. Aims. We wish to exploit new SARAO MeerKAT 1.3 GHz Galactic Plane Survey (SMGPS) radio continuum data, which covers $251掳\le l \le 358掳$ and $2掳\le l \le 61掳$ at $|b|\le 1.5掳$, to search for SNR candidates in the Milky Way disk. Methods. We also use MIR data from the Spitzer GLIMPSE, Spitzer MIPSGAL, and WISE surveys to help identify SNR candidates. The identified SNR candidate are sources of extended radio continuum emission that lack MIR counterparts, are not known as HII regions in the WISE Catalog of Galactic HII Regions, and are not known previously as SNRs Results. We locate 237 new Galactic SNR candidates in the SMGPS data. We also identify and confirm the expected radio morphology for 201 objects listed in the literature as being SNRs and 130 previously-identified SNR candidates. The known and candidate SNRs have similar spatial distributions and angular sizes. Conclusions. The SMGPS data allowed us to identify a large population of SNR candidates that can be confirmed as true SNRs using radio polarization measurements or by deriving radio spectral indices. If the 237 candidates are confirmed as true SNRs, it would approximately double the number of known Galactic SNRs in the survey area, alleviating much of the difference between the known and expected populations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.16607v1-abstract-full').style.display = 'none'; document.getElementById('2409.16607v1-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </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 by A&A. Images and FITS files of each source can be found here: https://doi.org/10.48479/0n8c-5q84</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.06383">arXiv:2409.06383</a> <span> [<a href="https://arxiv.org/pdf/2409.06383">pdf</a>, <a href="https://arxiv.org/format/2409.06383">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</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/10.1051/0004-6361/202451096">10.1051/0004-6361/202451096 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sifting the debris: Patterns in the SNR population with unsupervised ML methods </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Cecconello%2C+T">T. Cecconello</a>, <a href="/search/astro-ph?searchtype=author&query=Munari%2C+M">M. Munari</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A">A. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Sciacca%2C+E">E. Sciacca</a>, <a href="/search/astro-ph?searchtype=author&query=Vizzari%2C+G">G. Vizzari</a>, <a href="/search/astro-ph?searchtype=author&query=De+Marco%2C+A">A. De Marco</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</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="2409.06383v1-abstract-short" style="display: inline;"> Supernova remnants (SNRs) carry vast amounts of mechanical and radiative energy that heavily influence the structural, dynamical, and chemical evolution of galaxies. To this day, more than 300 SNRs have been discovered in the Milky Way, exhibiting a wide variety of observational features. However, existing classification schemes are mainly based on their radio morphology. In this work, we introduc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.06383v1-abstract-full').style.display = 'inline'; document.getElementById('2409.06383v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.06383v1-abstract-full" style="display: none;"> Supernova remnants (SNRs) carry vast amounts of mechanical and radiative energy that heavily influence the structural, dynamical, and chemical evolution of galaxies. To this day, more than 300 SNRs have been discovered in the Milky Way, exhibiting a wide variety of observational features. However, existing classification schemes are mainly based on their radio morphology. In this work, we introduce a novel unsupervised deep learning pipeline to analyse a representative subsample of the Galactic SNR population ($\sim$ 50% of the total) with the aim of finding a connection between their multi-wavelength features and their physical properties. The pipeline involves two stages: (1) a representation learning stage, consisting of a convolutional autoencoder that feeds on imagery from infrared and radio continuum surveys (WISE 22$渭$m, Hi-GAL 70 $渭$m and SMGPS 30 cm) and produces a compact representation in a lower-dimensionality latent space; and (2) a clustering stage that seeks meaningful clusters in the latent space that can be linked to the physical properties of the SNRs and their surroundings. Our results suggest that this approach, when combined with an intermediate uniform manifold approximation and projection (UMAP) reprojection of the autoencoded embeddings into a more clusterable manifold, enables us to find reliable clusters. Despite a large number of sources being classified as outliers, most clusters relate to the presence of distinctive features, such as the distribution of infrared emission, the presence of radio shells and pulsar wind nebulae, and the existence of dust filaments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.06383v1-abstract-full').style.display = 'none'; document.getElementById('2409.06383v1-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </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 in A&A. 17 pages, 11 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.07727">arXiv:2408.07727</a> <span> [<a href="https://arxiv.org/pdf/2408.07727">pdf</a>, <a href="https://arxiv.org/ps/2408.07727">ps</a>, <a href="https://arxiv.org/format/2408.07727">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/10.1051/0004-6361/202450766">10.1051/0004-6361/202450766 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MeerKAT reveals a ghostly thermal radio ring towards the Galactic Centre </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Filipovic%2C+M+D">M. D. Filipovic</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Cotton%2C+W+D">W. D. Cotton</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C">C. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+S">S. Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Jarrett%2C+T">T. Jarrett</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B">B. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Lazarevic%2C+S">S. Lazarevic</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Lundqvist%2C+P">P. Lundqvist</a>, <a href="/search/astro-ph?searchtype=author&query=Mackey%2C+J">J. Mackey</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Payne%2C+J">J. Payne</a>, <a href="/search/astro-ph?searchtype=author&query=Rowell%2C+G">G. Rowell</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Rizzo%2C+J+R">J. R. Rizzo</a>, <a href="/search/astro-ph?searchtype=author&query=Ruggeri%2C+A+C">A. C. Ruggeri</a> , et al. (4 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="2408.07727v1-abstract-short" style="display: inline;"> We present the serendipitous discovery of a new radio-continuum ring-like object nicknamed Kyklos (J1802-3353), with MeerKAT UHF and L-band observations. The radio ring, which resembles the recently discovered odd radio circles (ORCs), has a diameter of 80 arcsec and is located just 6 deg from the Galactic plane. However, Kyklos exhibits an atypical thermal radio-continuum spectrum (伪 = -0.1 +/- 0… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.07727v1-abstract-full').style.display = 'inline'; document.getElementById('2408.07727v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.07727v1-abstract-full" style="display: none;"> We present the serendipitous discovery of a new radio-continuum ring-like object nicknamed Kyklos (J1802-3353), with MeerKAT UHF and L-band observations. The radio ring, which resembles the recently discovered odd radio circles (ORCs), has a diameter of 80 arcsec and is located just 6 deg from the Galactic plane. However, Kyklos exhibits an atypical thermal radio-continuum spectrum (伪 = -0.1 +/- 0.3), which led us to explore different possible formation scenarios. We concluded that a circumstellar shell around an evolved massive star, possibly a Wolf-Rayet, is the most convincing explanation with the present data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.07727v1-abstract-full').style.display = 'none'; document.getElementById('2408.07727v1-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </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, 5 figures, accepted 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/2404.18462">arXiv:2404.18462</a> <span> [<a href="https://arxiv.org/pdf/2404.18462">pdf</a>, <a href="https://arxiv.org/format/2404.18462">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</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/10.1017/pasa.2024.84">10.1017/pasa.2024.84 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Self-supervised contrastive learning of radio data for source detection, classification and peculiar object discovery </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Cecconello%2C+T">T. Cecconello</a>, <a href="/search/astro-ph?searchtype=author&query=Palazzo%2C+S">S. Palazzo</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Gupta%2C+N">N. Gupta</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C">C. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Ruggeri%2C+A+C">A. C. Ruggeri</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Vitello%2C+F">F. Vitello</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="2404.18462v1-abstract-short" style="display: inline;"> New advancements in radio data post-processing are underway within the SKA precursor community, aiming to facilitate the extraction of scientific results from survey images through a semi-automated approach. Several of these developments leverage deep learning (DL) methodologies for diverse tasks, including source detection, object or morphology classification, and anomaly detection. Despite subst… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.18462v1-abstract-full').style.display = 'inline'; document.getElementById('2404.18462v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.18462v1-abstract-full" style="display: none;"> New advancements in radio data post-processing are underway within the SKA precursor community, aiming to facilitate the extraction of scientific results from survey images through a semi-automated approach. Several of these developments leverage deep learning (DL) methodologies for diverse tasks, including source detection, object or morphology classification, and anomaly detection. Despite substantial progress, the full potential of these methods often remains untapped due to challenges associated with training large supervised models, particularly in the presence of small and class-unbalanced labelled datasets. Self-supervised learning has recently established itself as a powerful methodology to deal with some of the aforementioned challenges, by directly learning a lower-dimensional representation from large samples of unlabelled data. The resulting model and data representation can then be used for data inspection and various downstream tasks if a small subset of labelled data is available. In this work, we explored contrastive learning methods to learn suitable radio data representation from unlabelled images taken from the ASKAP EMU and SARAO MeerKAT GPS surveys. We evaluated trained models and the obtained data representation over smaller labelled datasets, also taken from different radio surveys, in selected analysis tasks: source detection and classification, and search for objects with peculiar morphology. For all explored downstream tasks, we reported and discussed the benefits brought by self-supervised foundational models built on radio data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.18462v1-abstract-full').style.display = 'none'; document.getElementById('2404.18462v1-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </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, 16 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Publ. Astron. Soc. Aust. 41 (2024) e085 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.14235">arXiv:2403.14235</a> <span> [<a href="https://arxiv.org/pdf/2403.14235">pdf</a>, <a href="https://arxiv.org/format/2403.14235">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Computer Vision and Pattern Recognition">cs.CV</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Machine Learning">cs.LG</span> </div> </div> <p class="title is-5 mathjax"> RG-CAT: Detection Pipeline and Catalogue of Radio Galaxies in the EMU Pilot Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gupta%2C+N">Nikhel Gupta</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">Ray P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Hayder%2C+Z">Zeeshan Hayder</a>, <a href="/search/astro-ph?searchtype=author&query=Huynh%2C+M">Minh Huynh</a>, <a href="/search/astro-ph?searchtype=author&query=Petersson%2C+L">Lars Petersson</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+X+R">X. Rosalind Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">Andrew M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Andernach%2C+H">Heinz Andernach</a>, <a href="/search/astro-ph?searchtype=author&query=Gordon%2C+Y">Yjan Gordon</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">Simone Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Yew%2C+M">Miranda Yew</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+E+J">Evan J. Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B">B盲rbel Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Filipovi%C4%87%2C+M+D">Miroslav D. Filipovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Kapin%C5%9Bka%2C+A+D">Anna D. Kapin艣ka</a>, <a href="/search/astro-ph?searchtype=author&query=Shabala%2C+S">Stanislav Shabala</a>, <a href="/search/astro-ph?searchtype=author&query=Vernstrom%2C+T">Tessa Vernstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Marvil%2C+J+R">Joshua R. Marvil</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="2403.14235v1-abstract-short" style="display: inline;"> We present source detection and catalogue construction pipelines to build the first catalogue of radio galaxies from the 270 $\rm deg^2$ pilot survey of the Evolutionary Map of the Universe (EMU-PS) conducted with the Australian Square Kilometre Array Pathfinder (ASKAP) telescope. The detection pipeline uses Gal-DINO computer-vision networks (Gupta et al., 2024) to predict the categories of radio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.14235v1-abstract-full').style.display = 'inline'; document.getElementById('2403.14235v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.14235v1-abstract-full" style="display: none;"> We present source detection and catalogue construction pipelines to build the first catalogue of radio galaxies from the 270 $\rm deg^2$ pilot survey of the Evolutionary Map of the Universe (EMU-PS) conducted with the Australian Square Kilometre Array Pathfinder (ASKAP) telescope. The detection pipeline uses Gal-DINO computer-vision networks (Gupta et al., 2024) to predict the categories of radio morphology and bounding boxes for radio sources, as well as their potential infrared host positions. The Gal-DINO network is trained and evaluated on approximately 5,000 visually inspected radio galaxies and their infrared hosts, encompassing both compact and extended radio morphologies. We find that the Intersection over Union (IoU) for the predicted and ground truth bounding boxes is larger than 0.5 for 99% of the radio sources, and 98% of predicted host positions are within $3^{\prime \prime}$ of the ground truth infrared host in the evaluation set. The catalogue construction pipeline uses the predictions of the trained network on the radio and infrared image cutouts based on the catalogue of radio components identified using the Selavy source finder algorithm. Confidence scores of the predictions are then used to prioritize Selavy components with higher scores and incorporate them first into the catalogue. This results in identifications for a total of 211,625 radio sources, with 201,211 classified as compact and unresolved. The remaining 10,414 are categorized as extended radio morphologies, including 582 FR-I, 5,602 FR-II, 1,494 FR-x (uncertain whether FR-I or FR-II), 2,375 R (single-peak resolved) radio galaxies, and 361 with peculiar and other rare morphologies. We cross-match the radio sources in the catalogue with the infrared and optical catalogues, finding infrared cross-matches for 73% and photometric redshifts for 36% of the radio galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.14235v1-abstract-full').style.display = 'none'; document.getElementById('2403.14235v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </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 PASA. The paper has 22 pages, 12 figures and 5 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.04647">arXiv:2403.04647</a> <span> [<a href="https://arxiv.org/pdf/2403.04647">pdf</a>, <a href="https://arxiv.org/format/2403.04647">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The distance to CRL 618 through its radio expansion parallax </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Menten%2C+K+M">K. M. Menten</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</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="2403.04647v1-abstract-short" style="display: inline;"> CRL 618 is a post-AGB star that has started to ionize its ejecta. Its central HII region has been observed over the last 40 years and has steadily increased in flux density at radio wavelengths. In this paper, we present data that we obtained with the Very Large Array in its highest frequency band (43 GHz) in 2011 and compare these with archival data in the same frequency band from 1998. By applyi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.04647v1-abstract-full').style.display = 'inline'; document.getElementById('2403.04647v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.04647v1-abstract-full" style="display: none;"> CRL 618 is a post-AGB star that has started to ionize its ejecta. Its central HII region has been observed over the last 40 years and has steadily increased in flux density at radio wavelengths. In this paper, we present data that we obtained with the Very Large Array in its highest frequency band (43 GHz) in 2011 and compare these with archival data in the same frequency band from 1998. By applying the so-called expansion-parallax method, we are able to estimate an expansion rate of 4.0$\pm$0.4 mas yr$^{-1}$ along the major axis of the nebula and derive a distance of 1.1$\pm$0.2 kpc. Within errors, this distance estimation is in good agreement with the value of ~900 pc derived from the expansion of the optical lobes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.04647v1-abstract-full').style.display = 'none'; document.getElementById('2403.04647v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </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 on 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/2402.15232">arXiv:2402.15232</a> <span> [<a href="https://arxiv.org/pdf/2402.15232">pdf</a>, <a href="https://arxiv.org/format/2402.15232">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Machine Learning">cs.LG</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Machine Learning">stat.ML</span> </div> </div> <p class="title is-5 mathjax"> Classification of compact radio sources in the Galactic plane with supervised machine learning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Gordon%2C+Y">Y. Gordon</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCrkan%2C+G">G. G眉rkan</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C">C. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Cecconello%2C+T">T. Cecconello</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="2402.15232v1-abstract-short" style="display: inline;"> Generation of science-ready data from processed data products is one of the major challenges in next-generation radio continuum surveys with the Square Kilometre Array (SKA) and its precursors, due to the expected data volume and the need to achieve a high degree of automated processing. Source extraction, characterization, and classification are the major stages involved in this process. In this… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.15232v1-abstract-full').style.display = 'inline'; document.getElementById('2402.15232v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.15232v1-abstract-full" style="display: none;"> Generation of science-ready data from processed data products is one of the major challenges in next-generation radio continuum surveys with the Square Kilometre Array (SKA) and its precursors, due to the expected data volume and the need to achieve a high degree of automated processing. Source extraction, characterization, and classification are the major stages involved in this process. In this work we focus on the classification of compact radio sources in the Galactic plane using both radio and infrared images as inputs. To this aim, we produced a curated dataset of ~20,000 images of compact sources of different astronomical classes, obtained from past radio and infrared surveys, and novel radio data from pilot surveys carried out with the Australian SKA Pathfinder (ASKAP). Radio spectral index information was also obtained for a subset of the data. We then trained two different classifiers on the produced dataset. The first model uses gradient-boosted decision trees and is trained on a set of pre-computed features derived from the data, which include radio-infrared colour indices and the radio spectral index. The second model is trained directly on multi-channel images, employing convolutional neural networks. Using a completely supervised procedure, we obtained a high classification accuracy (F1-score>90%) for separating Galactic objects from the extragalactic background. Individual class discrimination performances, ranging from 60% to 75%, increased by 10% when adding far-infrared and spectral index information, with extragalactic objects, PNe and HII regions identified with higher accuracies. The implemented tools and trained models were publicly released, and made available to the radioastronomical community for future application on new radio data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.15232v1-abstract-full').style.display = 'none'; document.getElementById('2402.15232v1-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </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">27 pages, 15 figures, 9 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.07275">arXiv:2312.07275</a> <span> [<a href="https://arxiv.org/pdf/2312.07275">pdf</a>, <a href="https://arxiv.org/format/2312.07275">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> <p class="title is-5 mathjax"> The SARAO MeerKAT 1.3 GHz Galactic Plane Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Goedhart%2C+S">S. Goedhart</a>, <a href="/search/astro-ph?searchtype=author&query=Cotton%2C+W+D">W. D. Cotton</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+M+A">M. A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Bietenholz%2C+M">M. Bietenholz</a>, <a href="/search/astro-ph?searchtype=author&query=Woudt%2C+P+A">P. A. Woudt</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+L+D">L. D. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D+A+H">D. A. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+H">H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chibueze%2C+J+O">J. O. Chibueze</a>, <a href="/search/astro-ph?searchtype=author&query=Egbo%2C+D">D. Egbo</a>, <a href="/search/astro-ph?searchtype=author&query=Frank%2C+B+S">B. S. Frank</a>, <a href="/search/astro-ph?searchtype=author&query=Hoare%2C+M+G">M. G. Hoare</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Irabor%2C+T">T. Irabor</a>, <a href="/search/astro-ph?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/astro-ph?searchtype=author&query=Kurapati%2C+S">S. Kurapati</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Mutale%2C+M">M. Mutale</a> , et al. (105 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="2312.07275v2-abstract-short" style="display: inline;"> We present the SARAO MeerKAT Galactic Plane Survey (SMGPS), a 1.3 GHz continuum survey of almost half of the Galactic Plane (251掳$\le l \le$ 358掳and 2掳$\le l \le$ 61掳at $|b| \le 1.5掳$). SMGPS is the largest, most sensitive and highest angular resolution 1 GHz survey of the Plane yet carried out, with an angular resolution of 8" and a broadband RMS sensitivity of $\sim$10--20 $渭$ Jy/beam. Here we d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.07275v2-abstract-full').style.display = 'inline'; document.getElementById('2312.07275v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.07275v2-abstract-full" style="display: none;"> We present the SARAO MeerKAT Galactic Plane Survey (SMGPS), a 1.3 GHz continuum survey of almost half of the Galactic Plane (251掳$\le l \le$ 358掳and 2掳$\le l \le$ 61掳at $|b| \le 1.5掳$). SMGPS is the largest, most sensitive and highest angular resolution 1 GHz survey of the Plane yet carried out, with an angular resolution of 8" and a broadband RMS sensitivity of $\sim$10--20 $渭$ Jy/beam. Here we describe the first publicly available data release from SMGPS which comprises data cubes of frequency-resolved images over 908--1656 MHz, power law fits to the images, and broadband zeroth moment integrated intensity images. A thorough assessment of the data quality and guidance for future usage of the data products are given. Finally, we discuss the tremendous potential of SMGPS by showcasing highlights of the Galactic and extragalactic science that it permits. These highlights include the discovery of a new population of non-thermal radio filaments; identification of new candidate supernova remnants, pulsar wind nebulae and planetary nebulae; improved radio/mid-IR classification of rare Luminous Blue Variables and discovery of associated extended radio nebulae; new radio stars identified by Bayesian cross-matching techniques; the realisation that many of the largest radio-quiet WISE HII region candidates are not true HII regions; and a large sample of previously undiscovered background HI galaxies in the Zone of Avoidance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.07275v2-abstract-full').style.display = 'none'; document.getElementById('2312.07275v2-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> 2 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </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. The data release is live and links can be found in the Data Availability Statement in the paper</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.08716">arXiv:2308.08716</a> <span> [<a href="https://arxiv.org/pdf/2308.08716">pdf</a>, <a href="https://arxiv.org/format/2308.08716">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> <p class="title is-5 mathjax"> EMU Detection of a Large and Low Surface Brightness Galactic SNR G288.8-6.3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Filipovi%C4%87%2C+M+D">Miroslav D. Filipovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+S">Shi Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Arbutina%2C+B">Bojan Arbutina</a>, <a href="/search/astro-ph?searchtype=author&query=Hurley-Walker%2C+N">Natasha Hurley-Walker</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">Robert Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+W">Werner Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Sano%2C+H">Hidetoshi Sano</a>, <a href="/search/astro-ph?searchtype=author&query=Uro%C5%A1evi%C4%87%2C+D">Dejan Uro拧evi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Jarrett%2C+T+H">T. H. Jarrett</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">Andrew M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Alsaberi%2C+R+Z+E">Rami Z. E. Alsaberi</a>, <a href="/search/astro-ph?searchtype=author&query=Alsulami%2C+R">R. Alsulami</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">Cristobal Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Ball%2C+B">Brianna Ball</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">Filomena Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">Christopher Burger-Scheidlin</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+E">Evan Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=English%2C+J">Jayanne English</a>, <a href="/search/astro-ph?searchtype=author&query=Haberl%2C+F">Frank Haberl</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">Adriano Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Kapinska%2C+A+D">Anna D. Kapinska</a>, <a href="/search/astro-ph?searchtype=author&query=Kavanagh%2C+P+J">Patrick J. Kavanagh</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B+S">B盲rbel S. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Kothes%2C+R">Roland Kothes</a>, <a href="/search/astro-ph?searchtype=author&query=Lazarevi%C4%87%2C+S">Sanja Lazarevi膰</a> , et al. (14 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="2308.08716v1-abstract-short" style="display: inline;"> We present the serendipitous detection of a new Galactic Supernova Remnant (SNR), G288.8-6.3 using data from the Australian Square Kilometre Array Pathfinder (ASKAP)-Evolutionary Map of the Universe (EMU) survey. Using multi-frequency analysis, we confirm this object as an evolved Galactic SNR at high Galactic latitude with low radio surface brightness and typical SNR spectral index of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.08716v1-abstract-full').style.display = 'inline'; document.getElementById('2308.08716v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.08716v1-abstract-full" style="display: none;"> We present the serendipitous detection of a new Galactic Supernova Remnant (SNR), G288.8-6.3 using data from the Australian Square Kilometre Array Pathfinder (ASKAP)-Evolutionary Map of the Universe (EMU) survey. Using multi-frequency analysis, we confirm this object as an evolved Galactic SNR at high Galactic latitude with low radio surface brightness and typical SNR spectral index of $伪= -0.41\pm0.12$. To determine the magnetic field strength in SNR G288.8-6.3, we present the first derivation of the equipartition formulae for SNRs with spectral indices $伪>-0.5$. The angular size is $1.\!^\circ 8\times 1.\!^\circ 6$ $(107.\!^\prime 6 \times 98.\!^\prime 4)$ and we estimate that its intrinsic size is $\sim40$pc which implies a distance of $\sim1.3$kpc and a position of $\sim140$pc above the Galactic plane. This is one of the largest angular size and closest Galactic SNRs. Given its low radio surface brightness, we suggest that it is about 13000 years old. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.08716v1-abstract-full').style.display = 'none'; document.getElementById('2308.08716v1-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </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 The Astrophysical 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/2305.00809">arXiv:2305.00809</a> <span> [<a href="https://arxiv.org/pdf/2305.00809">pdf</a>, <a href="https://arxiv.org/format/2305.00809">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Star-Planet Interaction at radio wavelengths in YZ Ceti: Inferring planetary magnetic field </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">Corrado Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Biswas%2C+A">Ayan Biswas</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">Paolo Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">Grazia Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Busa%2C+I">Innocenza Busa</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">Francesco Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Das%2C+B">Barnali Das</a>, <a href="/search/astro-ph?searchtype=author&query=Chandra%2C+P">Poonam Chandra</a>, <a href="/search/astro-ph?searchtype=author&query=Perez-Torres%2C+M">Miguel Perez-Torres</a>, <a href="/search/astro-ph?searchtype=author&query=Wade%2C+G+A">Gregg A. Wade</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">Cristobal Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">Carla S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">Filomena Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">Adriano Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">Sara Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">Simone Riggi</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="2305.00809v1-abstract-short" style="display: inline;"> In exoplanetary systems, the interaction between the central star and the planet can trigger Auroral Radio Emission (ARE), due to the Electron Cyclotron Maser mechanism. The high brightness temperature of this emission makes it visible at large distances, opening new opportunities to study exoplanets and to search for favourable conditions for the development of extra-terrestrial life, as magnetic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.00809v1-abstract-full').style.display = 'inline'; document.getElementById('2305.00809v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.00809v1-abstract-full" style="display: none;"> In exoplanetary systems, the interaction between the central star and the planet can trigger Auroral Radio Emission (ARE), due to the Electron Cyclotron Maser mechanism. The high brightness temperature of this emission makes it visible at large distances, opening new opportunities to study exoplanets and to search for favourable conditions for the development of extra-terrestrial life, as magnetic fields act as a shield that protects life against external particles and influences the evolution of the planetary atmospheres. In the last few years, we started an observational campaign to observe a sample of nearby M-type stars known to host exoplanets with the aim to detect ARE. We observed YZ Ceti with the upgraded Giant Metrewave Radio Telescope (uGMRT) in band 4 (550-900 MHz) nine times over a period of five months. We detected radio emission four times, two of which with high degree of circular polarization. With statistical considerations we exclude the possibility of flares due to stellar magnetic activity. Instead, when folding the detections to the orbital phase of the closest planet YZ Cet b, they are at positions where we would expect ARE due to star-planet interaction (SPI) in sub-Alfvenic regime. With a degree of confidence higher than 4.37 sigma, YZ Cet is the first extrasolar systems with confirmed SPI at radio wavelengths. Modelling the ARE, we estimate a magnetic field for the star of about 2.4 kG and we find that the planet must have a magnetosphere. The lower limit for the polar magnetic field of the planet is 0.4 G. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.00809v1-abstract-full').style.display = 'none'; document.getElementById('2305.00809v1-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 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </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, submitted to ApJ Letters in March 2023</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.14357">arXiv:2304.14357</a> <span> [<a href="https://arxiv.org/pdf/2304.14357">pdf</a>, <a href="https://arxiv.org/format/2304.14357">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</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/10.1017/pasa.2023.29">10.1017/pasa.2023.29 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hydra II: Characterisation of Aegean, Caesar, ProFound, PyBDSF, and Selavy source finders </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Boyce%2C+M+M">M. M. Boyce</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Rudnick%2C+L">L. Rudnick</a>, <a href="/search/astro-ph?searchtype=author&query=Ramsay%2C+M">M. Ramsay</a>, <a href="/search/astro-ph?searchtype=author&query=Hale%2C+C+L">C. L. Hale</a>, <a href="/search/astro-ph?searchtype=author&query=Marvil%2C+J">J. Marvil</a>, <a href="/search/astro-ph?searchtype=author&query=Whiting%2C+M">M. Whiting</a>, <a href="/search/astro-ph?searchtype=author&query=Venkataraman%2C+P">P. Venkataraman</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Dea%2C+C+P">C. P. O'Dea</a>, <a href="/search/astro-ph?searchtype=author&query=Baum%2C+S+A">S. A. Baum</a>, <a href="/search/astro-ph?searchtype=author&query=Gordon%2C+Y+A">Y. A. Gordon</a>, <a href="/search/astro-ph?searchtype=author&query=Vantyghem%2C+A+N">A. N. Vantyghem</a>, <a href="/search/astro-ph?searchtype=author&query=Dionyssiou%2C+M">M. Dionyssiou</a>, <a href="/search/astro-ph?searchtype=author&query=Andernach%2C+H">H. Andernach</a>, <a href="/search/astro-ph?searchtype=author&query=Collier%2C+J+D">J. D. Collier</a>, <a href="/search/astro-ph?searchtype=author&query=English%2C+J">J. English</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Leahy%2C+D">D. Leahy</a>, <a href="/search/astro-ph?searchtype=author&query=Micha%C5%82owski%2C+M+J">M. J. Micha艂owski</a>, <a href="/search/astro-ph?searchtype=author&query=Safi-Harb%2C+S">S. Safi-Harb</a>, <a href="/search/astro-ph?searchtype=author&query=Vaccari%2C+M">M. Vaccari</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+E">E. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Cowley%2C+M">M. Cowley</a>, <a href="/search/astro-ph?searchtype=author&query=Kapinska%2C+A+D">A. D. Kapinska</a> , et al. (2 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="2304.14357v1-abstract-short" style="display: inline;"> We present a comparison between the performance of a selection of source finders using a new software tool called Hydra. The companion paper, Paper~I, introduced the Hydra tool and demonstrated its performance using simulated data. Here we apply Hydra to assess the performance of different source finders by analysing real observational data taken from the Evolutionary Map of the Universe (EMU) Pil… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.14357v1-abstract-full').style.display = 'inline'; document.getElementById('2304.14357v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.14357v1-abstract-full" style="display: none;"> We present a comparison between the performance of a selection of source finders using a new software tool called Hydra. The companion paper, Paper~I, introduced the Hydra tool and demonstrated its performance using simulated data. Here we apply Hydra to assess the performance of different source finders by analysing real observational data taken from the Evolutionary Map of the Universe (EMU) Pilot Survey. EMU is a wide-field radio continuum survey whose primary goal is to make a deep ($20渭$Jy/beam RMS noise), intermediate angular resolution ($15^{\prime\prime}$), 1\,GHz survey of the entire sky south of $+30^{\circ}$ declination, and expecting to detect and catalogue up to 40 million sources. With the main EMU survey expected to begin in 2022 it is highly desirable to understand the performance of radio image source finder software and to identify an approach that optimises source detection capabilities. Hydra has been developed to refine this process, as well as to deliver a range of metrics and source finding data products from multiple source finders. We present the performance of the five source finders tested here in terms of their completeness and reliability statistics, their flux density and source size measurements, and an exploration of case studies to highlight finder-specific limitations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.14357v1-abstract-full').style.display = 'none'; document.getElementById('2304.14357v1-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 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </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">Paper accepted for publication in PASA</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">ACM Class:</span> D.2.8 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.14355">arXiv:2304.14355</a> <span> [<a href="https://arxiv.org/pdf/2304.14355">pdf</a>, <a href="https://arxiv.org/format/2304.14355">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</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/10.1017/pasa.2023.24">10.1017/pasa.2023.24 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hydra I: An extensible multi-source-finder comparison and cataloguing tool </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Boyce%2C+M+M">M. M. Boyce</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Rudnick%2C+L">L. Rudnick</a>, <a href="/search/astro-ph?searchtype=author&query=Ramsay%2C+M">M. Ramsay</a>, <a href="/search/astro-ph?searchtype=author&query=Hale%2C+C+L">C. L. Hale</a>, <a href="/search/astro-ph?searchtype=author&query=Marvil%2C+J">J. Marvil</a>, <a href="/search/astro-ph?searchtype=author&query=Whiting%2C+M">M. Whiting</a>, <a href="/search/astro-ph?searchtype=author&query=Venkataraman%2C+P">P. Venkataraman</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Dea%2C+C+P">C. P. O'Dea</a>, <a href="/search/astro-ph?searchtype=author&query=Baum%2C+S+A">S. A. Baum</a>, <a href="/search/astro-ph?searchtype=author&query=Gordon%2C+Y+A">Y. A. Gordon</a>, <a href="/search/astro-ph?searchtype=author&query=Vantyghem%2C+A+N">A. N. Vantyghem</a>, <a href="/search/astro-ph?searchtype=author&query=Dionyssiou%2C+M">M. Dionyssiou</a>, <a href="/search/astro-ph?searchtype=author&query=Andernach%2C+H">H. Andernach</a>, <a href="/search/astro-ph?searchtype=author&query=Collier%2C+J+D">J. D. Collier</a>, <a href="/search/astro-ph?searchtype=author&query=English%2C+J">J. English</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Leahy%2C+D">D. Leahy</a>, <a href="/search/astro-ph?searchtype=author&query=Micha%C5%82owski%2C+M+J">M. J. Micha艂owski</a>, <a href="/search/astro-ph?searchtype=author&query=Safi-Harb%2C+S">S. Safi-Harb</a>, <a href="/search/astro-ph?searchtype=author&query=Vaccari%2C+M">M. Vaccari</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+E">E. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Cowley%2C+M">M. Cowley</a>, <a href="/search/astro-ph?searchtype=author&query=Kapinska%2C+A+D">A. D. Kapinska</a> , et al. (2 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="2304.14355v1-abstract-short" style="display: inline;"> The latest generation of radio surveys are now producing sky survey images containing many millions of radio sources. In this context it is highly desirable to understand the performance of radio image source finder (SF) software and to identify an approach that optimises source detection capabilities. We have created Hydra to be an extensible multi-SF and cataloguing tool that can be used to comp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.14355v1-abstract-full').style.display = 'inline'; document.getElementById('2304.14355v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.14355v1-abstract-full" style="display: none;"> The latest generation of radio surveys are now producing sky survey images containing many millions of radio sources. In this context it is highly desirable to understand the performance of radio image source finder (SF) software and to identify an approach that optimises source detection capabilities. We have created Hydra to be an extensible multi-SF and cataloguing tool that can be used to compare and evaluate different SFs. Hydra, which currently includes the SFs Aegean, Caesar, ProFound, PyBDSF, and Selavy, provides for the addition of new SFs through containerisation and configuration files. The SF input RMS noise and island parameters are optimised to a 90\% ''percentage real detections'' threshold (calculated from the difference between detections in the real and inverted images), to enable comparison between SFs. Hydra provides completeness and reliability diagnostics through observed-deep ($\mathcal{D}$) and generated-shallow ($\mathcal{S}$) images, as well as other statistics. In addition, it has a visual inspection tool for comparing residual images through various selection filters, such as S/N bins in completeness or reliability. The tool allows the user to easily compare and evaluate different SFs in order to choose their desired SF, or a combination thereof. This paper is part one of a two part series. In this paper we introduce the Hydra software suite and validate its $\mathcal{D/S}$ metrics using simulated data. The companion paper demonstrates the utility of Hydra by comparing the performance of SFs using both simulated and real images. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.14355v1-abstract-full').style.display = 'none'; document.getElementById('2304.14355v1-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 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </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">Paper accepted for publication in PASA</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">ACM Class:</span> D.2.4; D.2.6; D.2.8; D.2.10; D.2.11; D.2.13 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.02804">arXiv:2301.02804</a> <span> [<a href="https://arxiv.org/pdf/2301.02804">pdf</a>, <a href="https://arxiv.org/ps/2301.02804">ps</a>, <a href="https://arxiv.org/format/2301.02804">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Radio source analysis services for the SKA and precursors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">Simone Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">Cristobal Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Magro%2C+D">Daniel Magro</a>, <a href="/search/astro-ph?searchtype=author&query=Sortino%2C+R">Renato Sortino</a>, <a href="/search/astro-ph?searchtype=author&query=Pino%2C+C">Carmelo Pino</a>, <a href="/search/astro-ph?searchtype=author&query=Sciacca%2C+E">Eva Sciacca</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">Filomena Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Cecconello%2C+T">Thomas Cecconello</a>, <a href="/search/astro-ph?searchtype=author&query=Vizzari%2C+G">Giuseppe Vizzari</a>, <a href="/search/astro-ph?searchtype=author&query=Vitello%2C+F">Fabio Vitello</a>, <a href="/search/astro-ph?searchtype=author&query=Tudisco%2C+G">Giuseppe Tudisco</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="2301.02804v1-abstract-short" style="display: inline;"> New developments in data processing and visualization are being made in preparation for upcoming radioastronomical surveys planned with the Square Kilometre Array (SKA) and its precursors. A major goal is enabling extraction of science information from the data in a mostly automated way, possibly exploiting the capabilities offered by modern computing infrastructures and technologies. In this cont… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.02804v1-abstract-full').style.display = 'inline'; document.getElementById('2301.02804v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.02804v1-abstract-full" style="display: none;"> New developments in data processing and visualization are being made in preparation for upcoming radioastronomical surveys planned with the Square Kilometre Array (SKA) and its precursors. A major goal is enabling extraction of science information from the data in a mostly automated way, possibly exploiting the capabilities offered by modern computing infrastructures and technologies. In this context, the integration of source analysis algorithms into data visualization tools is expected to significantly improve and speed up the cataloguing process of large area surveys. To this aim, the CIRASA (Collaborative and Integrated platform for Radio Astronomical Source Analysis) project was recently started to develop and integrate a set of services for source extraction, classification and analysis into the ViaLactea visual analytic platform and knowledge base archive. In this contribution, we will present the project objectives and tools that have been developed, interfaced and deployed so far on the prototype European Open Science Cloud (EOSC) infrastructure provided by the H2020 NEANIAS project. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.02804v1-abstract-full').style.display = 'none'; document.getElementById('2301.02804v1-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 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </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">4 pages, 3 figures, proceedings of ADASS XXXI conference, to be published in ASP Conference Series</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.02538">arXiv:2212.02538</a> <span> [<a href="https://arxiv.org/pdf/2212.02538">pdf</a>, <a href="https://arxiv.org/format/2212.02538">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Astronomical source detection in radio continuum maps with deep neural networks </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Magro%2C+D">D. Magro</a>, <a href="/search/astro-ph?searchtype=author&query=Sortino%2C+R">R. Sortino</a>, <a href="/search/astro-ph?searchtype=author&query=De+Marco%2C+A">A. De Marco</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Cecconello%2C+T">T. Cecconello</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Marvil%2C+J">J. Marvil</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Sciacca%2C+E">E. Sciacca</a>, <a href="/search/astro-ph?searchtype=author&query=Vitello%2C+F">F. Vitello</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Fiameni%2C+G">G. Fiameni</a>, <a href="/search/astro-ph?searchtype=author&query=Spampinato%2C+C">C. Spampinato</a>, <a href="/search/astro-ph?searchtype=author&query=Adami%2C+K+Z">K. Zarb Adami</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="2212.02538v1-abstract-short" style="display: inline;"> Source finding is one of the most challenging tasks in upcoming radio continuum surveys with SKA precursors, such as the Evolutionary Map of the Universe (EMU) survey of the Australian SKA Pathfinder (ASKAP) telescope. The resolution, sensitivity, and sky coverage of such surveys is unprecedented, requiring new features and improvements to be made in existing source finders. Among them, reducing t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.02538v1-abstract-full').style.display = 'inline'; document.getElementById('2212.02538v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.02538v1-abstract-full" style="display: none;"> Source finding is one of the most challenging tasks in upcoming radio continuum surveys with SKA precursors, such as the Evolutionary Map of the Universe (EMU) survey of the Australian SKA Pathfinder (ASKAP) telescope. The resolution, sensitivity, and sky coverage of such surveys is unprecedented, requiring new features and improvements to be made in existing source finders. Among them, reducing the false detection rate, particularly in the Galactic plane, and the ability to associate multiple disjoint islands into physical objects. To bridge this gap, we developed a new source finder, based on the Mask R-CNN object detection framework, capable of both detecting and classifying compact, extended, spurious, and poorly imaged sources in radio continuum images. The model was trained using ASKAP EMU data, observed during the Early Science and pilot survey phase, and previous radio survey data, taken with the VLA and ATCA telescopes. On the test sample, the final model achieves an overall detection completeness above 85\%, a reliability of $\sim$65\%, and a classification precision/recall above 90\%. Results obtained for all source classes are reported and discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.02538v1-abstract-full').style.display = 'none'; document.getElementById('2212.02538v1-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 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">18 pages, 11 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.09774">arXiv:2210.09774</a> <span> [<a href="https://arxiv.org/pdf/2210.09774">pdf</a>, <a href="https://arxiv.org/format/2210.09774">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/10.3847/2041-8213/ac9b10">10.3847/2041-8213/ac9b10 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First detection of silicon-bearing molecules in $畏$ Car </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Rizzo%2C+J+R">J. R. Rizzo</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Quintana-Lacaci%2C+G">G. Quintana-Lacaci</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C">C. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Sciacca%2C+E">E. Sciacca</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="2210.09774v1-abstract-short" style="display: inline;"> We present ALMA band 6 observations of the luminous blue variable Eta Car, obtained within the ALMAGAL program. We report SiO J=5-4, SiS J=12-11 and SiN N=5-4 emission in the equatorial region of the Homunculus nebula, constituting the first detection of silicon- and sulphur-bearing molecules in the outskirts of a highly evolved, early-type massive star. SiO, SiS and SiN trace a clumpy equatorial… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.09774v1-abstract-full').style.display = 'inline'; document.getElementById('2210.09774v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.09774v1-abstract-full" style="display: none;"> We present ALMA band 6 observations of the luminous blue variable Eta Car, obtained within the ALMAGAL program. We report SiO J=5-4, SiS J=12-11 and SiN N=5-4 emission in the equatorial region of the Homunculus nebula, constituting the first detection of silicon- and sulphur-bearing molecules in the outskirts of a highly evolved, early-type massive star. SiO, SiS and SiN trace a clumpy equatorial ring that surrounds the central binary at a projected distance of 2 arcsec, delineating the inner rims of the butterfly-shaped dusty region. The formation of silicon-bearing compounds is presumably related to the continuous recycling of dust due to the variable wind regime of Eta Car, that destroys grains and releases silicon back to gas phase. We discuss possible formation routes for the observed species, contextualizing them within the current molecular inventory of Eta Car. We find that the SiO and SiS fractional abundances in localised clumps of the ring, $6.7\times10^{-9}$ and $1.2\times10^{-8}$ respectively, are exceptionally lower than those measured in C- and O-rich AGB stars and cool supergiants; while the higher SiN abundance, $3.6\times10^{-8}$, evidences the nitrogen-rich chemistry of the ejecta. These abundances must be regarded as strict upper limits, since the distribution of H2 in the Homunculus is unknown. In any case, these findings shed new light onto the peculiar molecular ecosystem of Eta Car, and establish its surroundings as a new laboratory to investigate the lifecycle of silicate dust in extreme astrophysical conditions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.09774v1-abstract-full').style.display = 'none'; document.getElementById('2210.09774v1-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> 18 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">17 pages, 7 figures. Accepted in ApJL</span> </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/astro-ph?searchtype=author&query=Bozzetto%2C+L+M">Luke M. Bozzetto</a>, <a href="/search/astro-ph?searchtype=author&query=Filipovi%C4%87%2C+M+D">Miroslav D. Filipovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Sano%2C+H">H. Sano</a>, <a href="/search/astro-ph?searchtype=author&query=Alsaberi%2C+R+Z+E">R. Z. E. Alsaberi</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+L+A">L. A. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Boji%C4%8Di%C4%87%2C+I+S">I. S. Boji膷i膰</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Chomiuk%2C+L">L. Chomiuk</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+S">S. Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Ghavam%2C+M">M. Ghavam</a>, <a href="/search/astro-ph?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+T">T. Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Jarrett%2C+T">T. Jarrett</a>, <a href="/search/astro-ph?searchtype=author&query=Kavanagh%2C+P+J">P. J. Kavanagh</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Kothes%2C+R">R. Kothes</a>, <a href="/search/astro-ph?searchtype=author&query=Leahy%2C+D">D. Leahy</a>, <a href="/search/astro-ph?searchtype=author&query=Lenc%2C+E">E. Lenc</a>, <a href="/search/astro-ph?searchtype=author&query=Leonidaki%2C+I">I. Leonidaki</a>, <a href="/search/astro-ph?searchtype=author&query=Maggi%2C+P">P. Maggi</a>, <a href="/search/astro-ph?searchtype=author&query=Maitra%2C+C">C. Maitra</a>, <a href="/search/astro-ph?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/2207.14075">arXiv:2207.14075</a> <span> [<a href="https://arxiv.org/pdf/2207.14075">pdf</a>, <a href="https://arxiv.org/ps/2207.14075">ps</a>, <a href="https://arxiv.org/format/2207.14075">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/stac2163">10.1093/mnras/stac2163 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery and origin of the radio emission from the multiple stellar system KQVel </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Oskinova%2C+L+M">L. M. Oskinova</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Shultz%2C+M+E">M. E. Shultz</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/astro-ph?searchtype=author&query=Pillitteri%2C+I">I. Pillitteri</a>, <a href="/search/astro-ph?searchtype=author&query=Krticka%2C+J">J. Krticka</a>, <a href="/search/astro-ph?searchtype=author&query=Ignace%2C+R">R. Ignace</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Catanzaro%2C+G">G. Catanzaro</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Giarrusso%2C+M">M. Giarrusso</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Owocki%2C+S+P">S. P. Owocki</a>, <a href="/search/astro-ph?searchtype=author&query=Postnov%2C+K+A">K. A. Postnov</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Robrade%2C+J">J. Robrade</a>, <a href="/search/astro-ph?searchtype=author&query=Leone%2C+F">F. Leone</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="2207.14075v1-abstract-short" style="display: inline;"> KQVel is a binary system composed of a slowly rotating magnetic Ap star with a companion of unknown nature. In this paper, we report the detection of its radio emission. We conducted a multi-frequency radio campaign using the ATCA interferometer (band-names: 16cm, 4cm, and 15mm). The target was detected in all bands. The most obvious explanation for the radio emission is that it originates in the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.14075v1-abstract-full').style.display = 'inline'; document.getElementById('2207.14075v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.14075v1-abstract-full" style="display: none;"> KQVel is a binary system composed of a slowly rotating magnetic Ap star with a companion of unknown nature. In this paper, we report the detection of its radio emission. We conducted a multi-frequency radio campaign using the ATCA interferometer (band-names: 16cm, 4cm, and 15mm). The target was detected in all bands. The most obvious explanation for the radio emission is that it originates in the magnetosphere of the Ap star, but this is shown unfeasible. The known stellar parameters of the Ap star enable us to exploit the scaling relationship for non-thermal gyro-synchrotron emission from early-type magnetic stars. This is a general relation demonstrating how radio emission from stars with centrifugal magnetospheres is supported by rotation. Using KQVel's parameters the predicted radio luminosity is more than five orders of magnitudes lower than the measured one. The extremely long rotation period rules out the Ap star as the source of the observed radio emission. Other possible explanations for the radio emission from KQVel, involving its unknown companion, have been explored. A scenario that matches the observed features (i.e. radio luminosity and spectrum, correlation to X-rays) is a hierarchical stellar system, where the possible companion of the magnetic star is a close binary (possibly of RSCVn type) with at least one magnetically active late-type star. To be compatible with the total mass of the system, the last scenario places strong constraints on the orbital inclination of the KQVel stellar system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.14075v1-abstract-full').style.display = 'none'; document.getElementById('2207.14075v1-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 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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 to MNRAS; 16 pages, 9 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.13933">arXiv:2204.13933</a> <span> [<a href="https://arxiv.org/pdf/2204.13933">pdf</a>, <a href="https://arxiv.org/format/2204.13933">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Latent Space Explorer: Unsupervised Data Pattern Discovery on the Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cecconello%2C+T">T. Cecconello</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Puerari%2C+L">L. Puerari</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Schisano%2C+E">E. Schisano</a>, <a href="/search/astro-ph?searchtype=author&query=Sciacca%2C+E">E. Sciacca</a>, <a href="/search/astro-ph?searchtype=author&query=Maruccia%2C+Y">Y. Maruccia</a>, <a href="/search/astro-ph?searchtype=author&query=Vizzari%2C+G">G. Vizzari</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="2204.13933v1-abstract-short" style="display: inline;"> Extracting information from raw data is probably one of the central activities of experimental scientific enterprises. This work is about a pipeline in which a specific model is trained to provide a compact, essential representation of the training data, useful as a starting point for visualization and analyses aimed at detecting patterns, regularities among data. To enable researchers exploiting… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.13933v1-abstract-full').style.display = 'inline'; document.getElementById('2204.13933v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.13933v1-abstract-full" style="display: none;"> Extracting information from raw data is probably one of the central activities of experimental scientific enterprises. This work is about a pipeline in which a specific model is trained to provide a compact, essential representation of the training data, useful as a starting point for visualization and analyses aimed at detecting patterns, regularities among data. To enable researchers exploiting this approach, a cloud-based system is being developed and tested in the NEANIAS project as one of the ML-tools of a thematic service to be offered to the EOSC. Here, we describe the architecture of the system and introduce two example use cases in the astronomical context. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.13933v1-abstract-full').style.display = 'none'; document.getElementById('2204.13933v1-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 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">4 pages, 3 figures, proceedings of ADASS XXXI conference, to be published in ASP Conference Series</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/astro-ph?searchtype=author&query=Filipovi%C4%87%2C+M+D">Miroslav D. Filipovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Payne%2C+J+L">J. L. Payne</a>, <a href="/search/astro-ph?searchtype=author&query=Alsaberi%2C+R+Z+E">R. Z. E. Alsaberi</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Macgregor%2C+P+J">P. J. Macgregor</a>, <a href="/search/astro-ph?searchtype=author&query=Rudnick%2C+L">L. Rudnick</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Leahy%2C+D">D. Leahy</a>, <a href="/search/astro-ph?searchtype=author&query=Ducci%2C+L">L. Ducci</a>, <a href="/search/astro-ph?searchtype=author&query=Kothes%2C+R">R. Kothes</a>, <a href="/search/astro-ph?searchtype=author&query=Andernach%2C+H">H. Andernach</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+L">L. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Boji%C4%8Di%C4%87%2C+I+S">I. S. Boji膷i膰</a>, <a href="/search/astro-ph?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Collier%2C+J+D">J. D. Collier</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=Crocker%2C+R+M">R. M. Crocker</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+S">S. Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Galvin%2C+T+J">T. J. Galvin</a>, <a href="/search/astro-ph?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/astro-ph?searchtype=author&query=Heber%2C+U">U. Heber</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+T">T. Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/astro-ph?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/2110.08211">arXiv:2110.08211</a> <span> [<a href="https://arxiv.org/pdf/2110.08211">pdf</a>, <a href="https://arxiv.org/format/2110.08211">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Computation">stat.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Machine Learning">stat.ML</span> </div> </div> <p class="title is-5 mathjax"> Astronomical source finding services for the CIRASA visual analytic platform </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Vitello%2C+F">F. Vitello</a>, <a href="/search/astro-ph?searchtype=author&query=Tudisco%2C+G">G. Tudisco</a>, <a href="/search/astro-ph?searchtype=author&query=Sciacca%2C+E">E. Sciacca</a>, <a href="/search/astro-ph?searchtype=author&query=Magro%2C+D">D. Magro</a>, <a href="/search/astro-ph?searchtype=author&query=Sortino%2C+R">R. Sortino</a>, <a href="/search/astro-ph?searchtype=author&query=Pino%2C+C">C. Pino</a>, <a href="/search/astro-ph?searchtype=author&query=Molinaro%2C+M">M. Molinaro</a>, <a href="/search/astro-ph?searchtype=author&query=Benedettini%2C+M">M. Benedettini</a>, <a href="/search/astro-ph?searchtype=author&query=Leurini%2C+S">S. Leurini</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Raciti%2C+M">M. Raciti</a>, <a href="/search/astro-ph?searchtype=author&query=Becciani%2C+U">U. Becciani</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="2110.08211v2-abstract-short" style="display: inline;"> Innovative developments in data processing, archiving, analysis, and visualization are nowadays unavoidable to deal with the data deluge expected in next-generation facilities for radio astronomy, such as the Square Kilometre Array (SKA) and its precursors. In this context, the integration of source extraction and analysis algorithms into data visualization tools could significantly improve and sp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.08211v2-abstract-full').style.display = 'inline'; document.getElementById('2110.08211v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.08211v2-abstract-full" style="display: none;"> Innovative developments in data processing, archiving, analysis, and visualization are nowadays unavoidable to deal with the data deluge expected in next-generation facilities for radio astronomy, such as the Square Kilometre Array (SKA) and its precursors. In this context, the integration of source extraction and analysis algorithms into data visualization tools could significantly improve and speed up the cataloguing process of large area surveys, boosting astronomer productivity and shortening publication time. To this aim, we are developing a visual analytic platform (CIRASA) for advanced source finding and classification, integrating state-of-the-art tools, such as the CAESAR source finder, the ViaLactea Visual Analytic (VLVA) and Knowledge Base (VLKB). In this work, we present the project objectives and the platform architecture, focusing on the implemented source finding services. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.08211v2-abstract-full').style.display = 'none'; document.getElementById('2110.08211v2-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> 18 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">16 pages, 6 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.11995">arXiv:2107.11995</a> <span> [<a href="https://arxiv.org/pdf/2107.11995">pdf</a>, <a href="https://arxiv.org/ps/2107.11995">ps</a>, <a href="https://arxiv.org/format/2107.11995">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</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/stab2168">10.1093/mnras/stab2168 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A scaling relationship for non-thermal radio emission from ordered magnetospheres: from the top of the Main Sequence to planets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Krticka%2C+J">J. Krticka</a>, <a href="/search/astro-ph?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/astro-ph?searchtype=author&query=Ignace%2C+R">R. Ignace</a>, <a href="/search/astro-ph?searchtype=author&query=Shultz%2C+M+E">M. E. Shultz</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Pillitteri%2C+I">I. Pillitteri</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Oskinova%2C+L+M">L. M. Oskinova</a>, <a href="/search/astro-ph?searchtype=author&query=Agliozzo%2C+C">C. Agliozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Todt%2C+H">H. Todt</a>, <a href="/search/astro-ph?searchtype=author&query=Giarrusso%2C+M">M. Giarrusso</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+N+M">N. M. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Robrade%2C+J">J. Robrade</a>, <a href="/search/astro-ph?searchtype=author&query=Leone%2C+F">F. Leone</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="2107.11995v1-abstract-short" style="display: inline;"> In this paper, we present the analysis of incoherent non-thermal radio emission from a sample of hot magnetic stars, ranging from early-B to early-A spectral type. Spanning a wide range of stellar parameters and wind properties, these stars display a commonality in their radio emission which presents new challenges to the wind scenario as originally conceived. It was thought that relativistic elec… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.11995v1-abstract-full').style.display = 'inline'; document.getElementById('2107.11995v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.11995v1-abstract-full" style="display: none;"> In this paper, we present the analysis of incoherent non-thermal radio emission from a sample of hot magnetic stars, ranging from early-B to early-A spectral type. Spanning a wide range of stellar parameters and wind properties, these stars display a commonality in their radio emission which presents new challenges to the wind scenario as originally conceived. It was thought that relativistic electrons, responsible for the radio emission, originate in current sheets formed where the wind opens the magnetic field lines. However, the true mass-loss rates from the cooler stars are too small to explain the observed non-thermal broadband radio spectra. Instead, we suggest the existence of a radiation belt located inside the inner-magnetosphere, similar to that of Jupiter. Such a structure explains the overall indifference of the broadband radio emissions on wind mass-loss rates. Further, correlating the radio luminosities from a larger sample of magnetic stars with their stellar parameters, the combined roles of rotation and magnetic properties have been empirically determined. Finally, our sample of early-type magnetic stars suggests a scaling relationship between the non-thermal radio luminosity and the electric voltage induced by the magnetosphere's co-rotation, which appears to hold for a broader range of stellar types with dipole-dominated magnetospheres (like the cases of the planet Jupiter and the ultra-cool dwarf stars and brown dwarfs). We conclude that well-ordered and stable rotating magnetospheres share a common physical mechanism for supporting the generation of non-thermal electrons. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.11995v1-abstract-full').style.display = 'none'; document.getElementById('2107.11995v1-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> 26 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">Accepted to MNRAS; 26 pages, 13 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.10967">arXiv:2107.10967</a> <span> [<a href="https://arxiv.org/pdf/2107.10967">pdf</a>, <a href="https://arxiv.org/format/2107.10967">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/10.1093/mnras/stab2249">10.1093/mnras/stab2249 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radio Continuum Sources behind the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Boji%C4%8Di%C4%87%2C+I+S">I. S. Boji膷i膰</a>, <a href="/search/astro-ph?searchtype=author&query=Grieve%2C+K+R">K. R. Grieve</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Tothill%2C+N+F+H">N. F. H. Tothill</a>, <a href="/search/astro-ph?searchtype=author&query=Shobhana%2C+D">D. Shobhana</a>, <a href="/search/astro-ph?searchtype=author&query=Rudnick%2C+L">L. Rudnick</a>, <a href="/search/astro-ph?searchtype=author&query=Prandoni%2C+I">I. Prandoni</a>, <a href="/search/astro-ph?searchtype=author&query=Andernach%2C+H">H. Andernach</a>, <a href="/search/astro-ph?searchtype=author&query=Hurley-Walker%2C+N">N. Hurley-Walker</a>, <a href="/search/astro-ph?searchtype=author&query=Alsaberi%2C+R+Z+E">R. Z. E. Alsaberi</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+C+S">C. S. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Collier%2C+J+D">J. D. Collier</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=For%2C+B+-">B. -Q. For</a>, <a href="/search/astro-ph?searchtype=author&query=Galvin%2C+T+J">T. J. Galvin</a>, <a href="/search/astro-ph?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Kavanagh%2C+P+J">P. J. Kavanagh</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Kothes%2C+R">R. Kothes</a>, <a href="/search/astro-ph?searchtype=author&query=Leahy%2C+D">D. Leahy</a>, <a href="/search/astro-ph?searchtype=author&query=Leverenz%2C+H">H. Leverenz</a>, <a href="/search/astro-ph?searchtype=author&query=Maggi%2C+P">P. Maggi</a> , et al. (16 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="2107.10967v1-abstract-short" style="display: inline;"> We present a comprehensive multi-frequency catalogue of radio sources behind the Large Magellanic Cloud between 0.2 and 20 GHz, gathered from a combination of new and legacy radio continuum surveys. This catalogue covers an area of $\sim$144~deg$^2$ at angular resolutions from 45 arcsec to $\sim$3 arcmin. We find 6434 discrete radio sources in total, of which 3789 are detected at two or more radio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.10967v1-abstract-full').style.display = 'inline'; document.getElementById('2107.10967v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.10967v1-abstract-full" style="display: none;"> We present a comprehensive multi-frequency catalogue of radio sources behind the Large Magellanic Cloud between 0.2 and 20 GHz, gathered from a combination of new and legacy radio continuum surveys. This catalogue covers an area of $\sim$144~deg$^2$ at angular resolutions from 45 arcsec to $\sim$3 arcmin. We find 6434 discrete radio sources in total, of which 3789 are detected at two or more radio frequencies. We estimate the median spectral index ($伪$; where $S_{v}\sim谓^伪$) of $伪= -0.89 $ and mean of $-0.88 \pm 0.48$ for 3636 sources detected exclusively at two frequencies (0.843 and 1.384 GHz) with similar resolution (FWHM $\sim$40-45 arcsec). The large frequency range of the surveys makes it an effective tool to investigate Gigahertz Peak Spectrum (GPS), Compact Steep Spectrum (CSS) and Infrared Faint Radio sources populations within our sample. We find 10 GPS candidates with peak frequencies near 5 GHz, from which we estimate their linear size. 1866 sources from our catalogue are (CSS) candidates with $伪<-0.8$. We found six candidates for High Frequency Peaker (HFP) sources, whose radio fluxes peak above 5 GHz and no sources with unconstrained peaks and $伪~>0.5$. We found optical counterparts for 343 of the radio continuum sources, of which 128have a redshift measurement. Finally, we investigate the population of 123 Infrared Faint Radio Sources (IFRSs) found in this study. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.10967v1-abstract-full').style.display = 'none'; document.getElementById('2107.10967v1-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 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">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/2106.01754">arXiv:2106.01754</a> <span> [<a href="https://arxiv.org/pdf/2106.01754">pdf</a>, <a href="https://arxiv.org/format/2106.01754">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Image and Video Processing">eess.IV</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/stab1635">10.1093/mnras/stab1635 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Comparative Study of Convolutional Neural Networks for the Detection of Strong Gravitational Lensing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Magro%2C+D">Daniel Magro</a>, <a href="/search/astro-ph?searchtype=author&query=Adami%2C+K+Z">Kristian Zarb Adami</a>, <a href="/search/astro-ph?searchtype=author&query=DeMarco%2C+A">Andrea DeMarco</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">Simone Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Sciacca%2C+E">Eva Sciacca</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="2106.01754v1-abstract-short" style="display: inline;"> As we enter the era of large-scale imaging surveys with the up-coming telescopes such as LSST and SKA, it is envisaged that the number of known strong gravitational lensing systems will increase dramatically. However, these events are still very rare and require the efficient processing of millions of images. In order to tackle this image processing problem, we present Machine Learning techniques… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.01754v1-abstract-full').style.display = 'inline'; document.getElementById('2106.01754v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.01754v1-abstract-full" style="display: none;"> As we enter the era of large-scale imaging surveys with the up-coming telescopes such as LSST and SKA, it is envisaged that the number of known strong gravitational lensing systems will increase dramatically. However, these events are still very rare and require the efficient processing of millions of images. In order to tackle this image processing problem, we present Machine Learning techniques and apply them to the Gravitational Lens Finding Challenge. The Convolutional Neural Networks (CNNs) presented have been re-implemented within a new modular, and extendable framework, LEXACTUM. We report an Area Under the Curve (AUC) of 0.9343 and 0.9870, and an execution time of 0.0061s and 0.0594s per image, for the Space and Ground datasets respectively, showing that the results obtained by CNNs are very competitive with conventional methods (such as visual inspection and arc finders) for detecting gravitational lenses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.01754v1-abstract-full').style.display = 'none'; document.getElementById('2106.01754v1-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> 3 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">12 pages, 13 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.07639">arXiv:2101.07639</a> <span> [<a href="https://arxiv.org/pdf/2101.07639">pdf</a>, <a href="https://arxiv.org/ps/2101.07639">ps</a>, <a href="https://arxiv.org/format/2101.07639">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Novel EOSC Services for Space Challenges: The NEANIAS First Outcomes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sciacca%2C+E">Eva Sciacca</a>, <a href="/search/astro-ph?searchtype=author&query=Krokos%2C+M">Mel Krokos</a>, <a href="/search/astro-ph?searchtype=author&query=Becciani%2C+U">Ugo Becciani</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">Cristobal Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">Filomena Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Costa%2C+A">Alessandro Costa</a>, <a href="/search/astro-ph?searchtype=author&query=Pino%2C+C">Carmelo Pino</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">Simone Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Vitello%2C+F">Fabio Vitello</a>, <a href="/search/astro-ph?searchtype=author&query=Brandt%2C+C">Carlos Brandt</a>, <a href="/search/astro-ph?searchtype=author&query=Rossi%2C+A">Angelo Rossi</a>, <a href="/search/astro-ph?searchtype=author&query=Topa%2C+E">Eugenio Topa</a>, <a href="/search/astro-ph?searchtype=author&query=Mantovani%2C+S">Simone Mantovani</a>, <a href="/search/astro-ph?searchtype=author&query=Vettorello%2C+L">Laura Vettorello</a>, <a href="/search/astro-ph?searchtype=author&query=Cecconello%2C+T">Thomas Cecconello</a>, <a href="/search/astro-ph?searchtype=author&query=Vizzari%2C+G">Giuseppe Vizzari</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="2101.07639v1-abstract-short" style="display: inline;"> The European Open Science Cloud (EOSC) initiative faces the challenge of developing an agile, fit-for-purpose, and sustainable service-oriented platform that can address the evolving needs of scientific communities. The NEANIAS project plays an active role in the materialization of the EOSC ecosystem by actively contributing to the technological, procedural, strategic and business development of E… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.07639v1-abstract-full').style.display = 'inline'; document.getElementById('2101.07639v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.07639v1-abstract-full" style="display: none;"> The European Open Science Cloud (EOSC) initiative faces the challenge of developing an agile, fit-for-purpose, and sustainable service-oriented platform that can address the evolving needs of scientific communities. The NEANIAS project plays an active role in the materialization of the EOSC ecosystem by actively contributing to the technological, procedural, strategic and business development of EOSC. We present the first outcomes of the NEANIAS activities relating to co-design and delivery of new innovative services for space research for data management and visualization (SPACE-VIS), map making and mosaicing (SPACE-MOS) and pattern and structure detection (SPACE-ML). We include a summary of collected user requirements driving our services and methodology for their delivery, together with service access details and pointers to future works. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.07639v1-abstract-full').style.display = 'none'; document.getElementById('2101.07639v1-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.03843">arXiv:2101.03843</a> <span> [<a href="https://arxiv.org/pdf/2101.03843">pdf</a>, <a href="https://arxiv.org/format/2101.03843">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Machine Learning">stat.ML</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/stab028">10.1093/mnras/stab028 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evolutionary Map of the Universe (EMU):Compact radio sources in the SCORPIO field towards the Galactic plane </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Andernach%2C+H">H. Andernach</a>, <a href="/search/astro-ph?searchtype=author&query=van+Loon%2C+J+T">J. Th. van Loon</a>, <a href="/search/astro-ph?searchtype=author&query=Micha%C5%82owski%2C+M+J">M. J. Micha艂owski</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+T">T. An</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C">C. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Carretti%2C+E">E. Carretti</a>, <a href="/search/astro-ph?searchtype=author&query=Collier%2C+J+D">J. D. Collier</a>, <a href="/search/astro-ph?searchtype=author&query=Joseph%2C+T">T. Joseph</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Kothes%2C+R">R. Kothes</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=McConnell%2C+D">D. McConnell</a>, <a href="/search/astro-ph?searchtype=author&query=Pommier%2C+M">M. Pommier</a>, <a href="/search/astro-ph?searchtype=author&query=Sciacca%2C+E">E. Sciacca</a> , et al. (4 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="2101.03843v1-abstract-short" style="display: inline;"> We present observations of a region of the Galactic plane taken during the Early Science Program of the Australian Square Kilometre Array Pathfinder (ASKAP). In this context, we observed the SCORPIO field at 912 MHz with an uncompleted array consisting of 15 commissioned antennas. The resulting map covers a square region of ~40 deg^2, centred on (l, b)=(343.5掳, 0.75掳), with a synthesized beam of 2… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.03843v1-abstract-full').style.display = 'inline'; document.getElementById('2101.03843v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.03843v1-abstract-full" style="display: none;"> We present observations of a region of the Galactic plane taken during the Early Science Program of the Australian Square Kilometre Array Pathfinder (ASKAP). In this context, we observed the SCORPIO field at 912 MHz with an uncompleted array consisting of 15 commissioned antennas. The resulting map covers a square region of ~40 deg^2, centred on (l, b)=(343.5掳, 0.75掳), with a synthesized beam of 24"x21" and a background rms noise of 150-200 渭Jy/beam, increasing to 500-600 渭Jy/beam close to the Galactic plane. A total of 3963 radio sources were detected and characterized in the field using the CAESAR source finder. We obtained differential source counts in agreement with previously published data after correction for source extraction and characterization uncertainties, estimated from simulated data. The ASKAP positional and flux density scale accuracy were also investigated through comparison with previous surveys (MGPS, NVSS) and additional observations of the SCORPIO field, carried out with ATCA at 2.1 GHz and 10" spatial resolution. These allowed us to obtain a measurement of the spectral index for a subset of the catalogued sources and an estimated fraction of (at least) 8% of resolved sources in the reported catalogue. We cross-matched our catalogued sources with different astronomical databases to search for possible counterparts, finding ~150 associations to known Galactic objects. Finally, we explored a multiparametric approach for classifying previously unreported Galactic sources based on their radio-infrared colors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.03843v1-abstract-full').style.display = 'none'; document.getElementById('2101.03843v1-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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, 15 figures, 15 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.07686">arXiv:2012.07686</a> <span> [<a href="https://arxiv.org/pdf/2012.07686">pdf</a>, <a href="https://arxiv.org/ps/2012.07686">ps</a>, <a href="https://arxiv.org/format/2012.07686">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Astronomical research in the next decade: trends, barriers and needs in data access, management, visualization and analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Sciacca%2C+E">E. Sciacca</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Molinaro%2C+M">M. Molinaro</a>, <a href="/search/astro-ph?searchtype=author&query=Vizzari%2C+G">G. Vizzari</a>, <a href="/search/astro-ph?searchtype=author&query=Krokos%2C+M">M. Krokos</a>, <a href="/search/astro-ph?searchtype=author&query=Brandt%2C+C">C. Brandt</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="2012.07686v1-abstract-short" style="display: inline;"> We report the outcomes of a survey that explores the current practices, needs and expectations of the astrophysics community, concerning four research aspects: open science practices, data access and management, data visualization, and data analysis. The survey, involving 329 professionals from several research institutions, pinpoints significant gaps in matters such as results reproducibility, av… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.07686v1-abstract-full').style.display = 'inline'; document.getElementById('2012.07686v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.07686v1-abstract-full" style="display: none;"> We report the outcomes of a survey that explores the current practices, needs and expectations of the astrophysics community, concerning four research aspects: open science practices, data access and management, data visualization, and data analysis. The survey, involving 329 professionals from several research institutions, pinpoints significant gaps in matters such as results reproducibility, availability of visual analytics tools and adoption of Machine Learning techniques for data analysis. This research is conducted in the context of the H2020 NEANIAS project. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.07686v1-abstract-full').style.display = 'none'; document.getElementById('2012.07686v1-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 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">4 pages, no figures, proceedings of ADASS XXX conference, to be published in ASP Conference Series</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.08161">arXiv:2011.08161</a> <span> [<a href="https://arxiv.org/pdf/2011.08161">pdf</a>, <a href="https://arxiv.org/format/2011.08161">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/staa3606">10.1093/mnras/staa3606 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A warm molecular ring in AG Car: composing the mass-loss puzzle </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Rizzo%2C+J+R">J. R. Rizzo</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</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="2011.08161v1-abstract-short" style="display: inline;"> We present APEX observations of CO J=3-2 and ALMA observations of CO J=2-1, 13CO J=2-1 and continuum toward the galactic luminous blue variable AG Car. These new observations reveal the presence of a ring-like molecular structure surrounding the star. Morphology and kinematics of the gas are consistent with a slowly expanding torus located near the equatorial plane of AG Car. Using non-LTE line mo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.08161v1-abstract-full').style.display = 'inline'; document.getElementById('2011.08161v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.08161v1-abstract-full" style="display: none;"> We present APEX observations of CO J=3-2 and ALMA observations of CO J=2-1, 13CO J=2-1 and continuum toward the galactic luminous blue variable AG Car. These new observations reveal the presence of a ring-like molecular structure surrounding the star. Morphology and kinematics of the gas are consistent with a slowly expanding torus located near the equatorial plane of AG Car. Using non-LTE line modelling, we derived the physical parameters of the gas, which is warm (50 K) and moderately dense (10$^3$ cm$^{-3}$. The total mass of molecular gas in the ring is 2.7$\pm$0.9 solar masses. We analysed the radio continuum map, which depicts a point-like source surrounded by a shallow nebula. From the flux of the point-like source, we derived a current mass-loss date of $1.55\pm0.21\times10^{-5}$ solar masses / yr. Finally, to better understand the complex circumstellar environment of AG Car, we put the newly detected ring in relation to the main nebula of dust and ionised gas. We discuss possible formation scenarios for the ring, namely, the accumulation of interstellar material due to the action of the stellar wind, the remnant of a close binary interaction or merger, and an equatorially enhanced mass-loss episode. If molecular gas formed in situ as a result of a mass eruption, it would account for at least a 30$\%$ of the total mass ejected by AG Car. This detection adds a new piece to the puzzle of the complex mass-loss history of AG Car, providing new clues about the interplay between LBV stars and their surroundings. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.08161v1-abstract-full').style.display = 'none'; document.getElementById('2011.08161v1-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 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">16 pages, 13 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/2009.09948">arXiv:2009.09948</a> <span> [<a href="https://arxiv.org/pdf/2009.09948">pdf</a>, <a href="https://arxiv.org/format/2009.09948">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/staa2868">10.1093/mnras/staa2868 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New high-frequency radio observations of the Cygnus Loop supernova remnant with the Italian radio telescopes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Pellizzoni%2C+A">A. Pellizzoni</a>, <a href="/search/astro-ph?searchtype=author&query=Egron%2C+E">E. Egron</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Morlino%2C+G">G. Morlino</a>, <a href="/search/astro-ph?searchtype=author&query=Celli%2C+S">S. Celli</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Iacolina%2C+M+N">M. N. Iacolina</a>, <a href="/search/astro-ph?searchtype=author&query=Righini%2C+S">S. Righini</a>, <a href="/search/astro-ph?searchtype=author&query=Reich%2C+P">P. Reich</a>, <a href="/search/astro-ph?searchtype=author&query=Mulas%2C+S">S. Mulas</a>, <a href="/search/astro-ph?searchtype=author&query=Marongiu%2C+M">M. Marongiu</a>, <a href="/search/astro-ph?searchtype=author&query=Pilia%2C+M">M. Pilia</a>, <a href="/search/astro-ph?searchtype=author&query=Melis%2C+A">A. Melis</a>, <a href="/search/astro-ph?searchtype=author&query=Concu%2C+R">R. Concu</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+M">M. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C">C. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Schillir%C3%B2%2C+F">F. Schillir貌</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="2009.09948v1-abstract-short" style="display: inline;"> Supernova remnants (SNRs) represent a powerful laboratory to study the Cosmic-Ray acceleration processes at the shocks, and their relation to the properties of the circumstellar medium. With the aim of studying the high-frequency radio emission and investigating the energy distribution of accelerated electrons and the magnetic field conditions, we performed single-dish observations of the large an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.09948v1-abstract-full').style.display = 'inline'; document.getElementById('2009.09948v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.09948v1-abstract-full" style="display: none;"> Supernova remnants (SNRs) represent a powerful laboratory to study the Cosmic-Ray acceleration processes at the shocks, and their relation to the properties of the circumstellar medium. With the aim of studying the high-frequency radio emission and investigating the energy distribution of accelerated electrons and the magnetic field conditions, we performed single-dish observations of the large and complex Cygnus Loop SNR from 7.0 to 24.8 GHz with the Medicina and the Sardinia Radio Telescope, focusing on the northern filament (NGC 6992) and the southern shell. Both regions show a spectrum well fitted by a power-law function ($S\propto谓^{-伪}$), with spectral index $伪=0.45\pm0.05$ for NGC 6992 and $伪=0.49\pm0.01$ for the southern shell and without any indication of a spectral break. The spectra are significantly flatter than the whole Cygnus Loop spectrum ($伪=0.54\pm0.01$), suggesting a departure from the plain shock acceleration mechanisms, which for NGC 6992 could be related to the ongoing transition towards a radiative shock. We model the integrated spectrum of the whole SNR considering the evolution of the maximum energy and magnetic field amplification. Through the radio spectral parameters, we infer a magnetic field at the shock of 10 $渭$G. This value is compatible with a pure adiabatic compression of the interstellar magnetic field, suggesting that the amplification process is currently inefficient. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.09948v1-abstract-full').style.display = 'none'; document.getElementById('2009.09948v1-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 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">19 pages, 13 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.02363">arXiv:2009.02363</a> <span> [<a href="https://arxiv.org/pdf/2009.02363">pdf</a>, <a href="https://arxiv.org/ps/2009.02363">ps</a>, <a href="https://arxiv.org/format/2009.02363">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/mnrasl/slaa157">10.1093/mnrasl/slaa157 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The auroral radio emission of the magnetic B-type star rho OphC </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Leone%2C+F">F. Leone</a>, <a href="/search/astro-ph?searchtype=author&query=Pillitteri%2C+I">I. Pillitteri</a>, <a href="/search/astro-ph?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Oskinova%2C+L+M">L. M. Oskinova</a>, <a href="/search/astro-ph?searchtype=author&query=Ignace%2C+R">R. Ignace</a>, <a href="/search/astro-ph?searchtype=author&query=Krticka%2C+J">J. Krticka</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Catanzaro%2C+G">G. Catanzaro</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Schilliro%2C+F">F. Schilliro</a>, <a href="/search/astro-ph?searchtype=author&query=Agliozzo%2C+C">C. Agliozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+N+M">N. M. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Giarrusso%2C+M">M. Giarrusso</a>, <a href="/search/astro-ph?searchtype=author&query=Robrade%2C+J">J. Robrade</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="2009.02363v1-abstract-short" style="display: inline;"> The non-thermal radio emission of main-sequence early-type stars is a signature of stellar magnetism. We present multi-wavelength (1.6-16.7 GHz) ATCA measurements of the early-type magnetic star rho OphC, which is a flat-spectrum non-thermal radio source. The rho OphC radio emission is partially circularly polarized with a steep spectral dependence: the fraction of polarized emission is about 60%… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.02363v1-abstract-full').style.display = 'inline'; document.getElementById('2009.02363v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.02363v1-abstract-full" style="display: none;"> The non-thermal radio emission of main-sequence early-type stars is a signature of stellar magnetism. We present multi-wavelength (1.6-16.7 GHz) ATCA measurements of the early-type magnetic star rho OphC, which is a flat-spectrum non-thermal radio source. The rho OphC radio emission is partially circularly polarized with a steep spectral dependence: the fraction of polarized emission is about 60% at the lowest frequency sub-band (1.6 GHz) while is undetected at 16.7 GHz. This is clear evidence of coherent Auroral Radio Emission (ARE) from the rho OphC magnetosphere. Interestingly, the detection of the rho OphC's ARE is not related to a peculiar rotational phase. This is a consequence of the stellar geometry, which makes the strongly anisotropic radiation beam of the amplified radiation always pointed towards Earth. The circular polarization sign evidences mainly amplification of the ordinary mode of the electromagnetic wave, consistent with a maser amplification occurring within dense regions. This is indirect evidence of the plasma evaporation from the polar caps, a phenomenon responsible for the thermal X-ray aurorae. rho OphC is not the first early-type magnetic star showing the O-mode dominated ARE but is the first star with the ARE always on view. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.02363v1-abstract-full').style.display = 'none'; document.getElementById('2009.02363v1-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> 4 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">5 pages, 4 figures; accepted to MNRAS Letter</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.06222">arXiv:2007.06222</a> <span> [<a href="https://arxiv.org/pdf/2007.06222">pdf</a>, <a href="https://arxiv.org/format/2007.06222">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</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/10.1007/978-3-030-52243-8_43">10.1007/978-3-030-52243-8_43 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Toward porting Astrophysics Visual Analytics Services to the European Open Science Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sciacca%2C+E">Eva Sciacca</a>, <a href="/search/astro-ph?searchtype=author&query=Vitello%2C+F">Fabio Vitello</a>, <a href="/search/astro-ph?searchtype=author&query=Becciani%2C+U">Ugo Becciani</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">Cristobal Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">Filomena Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Calanducci%2C+A">Antonio Calanducci</a>, <a href="/search/astro-ph?searchtype=author&query=Costa%2C+A">Alessandro Costa</a>, <a href="/search/astro-ph?searchtype=author&query=Raciti%2C+M">Mario Raciti</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">Simone Riggi</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="2007.06222v1-abstract-short" style="display: inline;"> The European Open Science Cloud (EOSC) aims to create a federated environment for hosting and processing research data to support science in all disciplines without geographical boundaries, such that data, software, methods and publications can be shared as part of an Open Science community of practice. This work presents the ongoing activities related to the implementation of visual analytics ser… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.06222v1-abstract-full').style.display = 'inline'; document.getElementById('2007.06222v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.06222v1-abstract-full" style="display: none;"> The European Open Science Cloud (EOSC) aims to create a federated environment for hosting and processing research data to support science in all disciplines without geographical boundaries, such that data, software, methods and publications can be shared as part of an Open Science community of practice. This work presents the ongoing activities related to the implementation of visual analytics services, integrated into EOSC, towards addressing the diverse astrophysics user communities needs. These services rely on visualisation to manage the data life cycle process under FAIR principles, integrating data processing for imaging and multidimensional map creation and mosaicing, and applying machine learning techniques for detection of structures in large scale multidimensional maps. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.06222v1-abstract-full').style.display = 'none'; document.getElementById('2007.06222v1-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> 13 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proceedings of the 2020 Computing Conference article has been queued for publication in the Proceedings of the 2020 Computing Conference. Article queued for publication in the Proceedings of the 2020 Computing Conference </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.05374">arXiv:2004.05374</a> <span> [<a href="https://arxiv.org/pdf/2004.05374">pdf</a>, <a href="https://arxiv.org/format/2004.05374">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Methodology">stat.ME</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Applications">stat.AP</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/10.1016/j.nima.2015.01.063">10.1016/j.nima.2015.01.063 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Handling missing data in a neural network approach for the identification of charged particles in a multilayer detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+D">D. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+F">F. Riggi</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="2004.05374v1-abstract-short" style="display: inline;"> Identification of charged particles in a multilayer detector by the energy loss technique may also be achieved by the use of a neural network. The performance of the network becomes worse when a large fraction of information is missing, for instance due to detector inefficiencies. Algorithms which provide a way to impute missing information have been developed over the past years. Among the variou… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.05374v1-abstract-full').style.display = 'inline'; document.getElementById('2004.05374v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.05374v1-abstract-full" style="display: none;"> Identification of charged particles in a multilayer detector by the energy loss technique may also be achieved by the use of a neural network. The performance of the network becomes worse when a large fraction of information is missing, for instance due to detector inefficiencies. Algorithms which provide a way to impute missing information have been developed over the past years. Among the various approaches, we focused on normal mixtures models in comparison with standard mean imputation and multiple imputation methods. Further, to account for the intrinsic asymmetry of the energy loss data, we considered skew-normal mixture models and provided a closed form implementation in the Expectation-Maximization (EM) algorithm framework to handle missing patterns. The method has been applied to a test case where the energy losses of pions, kaons and protons in a six-layers Silicon detector are considered as input neurons to a neural network. Results are given in terms of reconstruction efficiency and purity of the various species in different momentum bins. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.05374v1-abstract-full').style.display = 'none'; document.getElementById('2004.05374v1-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">14 pages, 8 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nucl. Instr. and Methods in Physics Research A 780 (2015) 81-90 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.09251">arXiv:2002.09251</a> <span> [<a href="https://arxiv.org/pdf/2002.09251">pdf</a>, <a href="https://arxiv.org/ps/2002.09251">ps</a>, <a href="https://arxiv.org/format/2002.09251">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/staa587">10.1093/mnras/staa587 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evidence for radio and X-ray auroral emissions from the magnetic B-type star rho Oph A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Leone%2C+F">F. Leone</a>, <a href="/search/astro-ph?searchtype=author&query=Pillitteri%2C+I">I. Pillitteri</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Oskinova%2C+L+M">L. M. Oskinova</a>, <a href="/search/astro-ph?searchtype=author&query=Ignace%2C+R">R. Ignace</a>, <a href="/search/astro-ph?searchtype=author&query=Krticka%2C+J">J. Krticka</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Catanzaro%2C+G">G. Catanzaro</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Agliozzo%2C+C">C. Agliozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+N+M">N. M. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Munari%2C+M">M. Munari</a>, <a href="/search/astro-ph?searchtype=author&query=Gangi%2C+M">M. Gangi</a>, <a href="/search/astro-ph?searchtype=author&query=Giarrusso%2C+M">M. Giarrusso</a>, <a href="/search/astro-ph?searchtype=author&query=Robrade%2C+J">J. Robrade</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="2002.09251v2-abstract-short" style="display: inline;"> We present new ATCA multi-wavelength radio measurements (range 2.1-21.2 GHz) of the early-type magnetic star rho Oph A, performed in March 2019 during 3 different observing sessions. These new ATCA observations evidence a clear rotational modulation of the stellar radio emission and the detection of coherent auroral radio emission from rho Oph A at 2.1 GHz. We collected high-resolution optical spe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.09251v2-abstract-full').style.display = 'inline'; document.getElementById('2002.09251v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.09251v2-abstract-full" style="display: none;"> We present new ATCA multi-wavelength radio measurements (range 2.1-21.2 GHz) of the early-type magnetic star rho Oph A, performed in March 2019 during 3 different observing sessions. These new ATCA observations evidence a clear rotational modulation of the stellar radio emission and the detection of coherent auroral radio emission from rho Oph A at 2.1 GHz. We collected high-resolution optical spectra of rho Oph A acquired by several instruments over a time span of about ten years. We also report new magnetic field measurements of rho Oph A that, together with the radio light curves and the temporal variation of the equivalent width of the HeI line (lambda=5015 Angstrom), were used to constrain the rotation period and the stellar magnetic field geometry. The above results have been used to model the stellar radio emission, modelling that allowed us to constrain the physical condition of rho Oph A's magnetosphere. Past XMM measurements showed periodic X-ray pulses from rho Oph A. We correlate the X-ray light curve with the magnetic field geometry of rho Oph A. The already published XMM data have been re-analyzed showing that the X-ray spectra of rho Oph A are compatible with the presence of a non-thermal X-ray component. We discuss a scenario where the emission phenomena occurring at the extremes of the electromagnetic spectrum, radio and X-ray, are directly induced by the same plasma process. We interpret the observed X-ray and radio features of rho Oph A as having an auroral origin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.09251v2-abstract-full').style.display = 'none'; document.getElementById('2002.09251v2-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> 26 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">20 pages, 13 figures; 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/1910.11592">arXiv:1910.11592</a> <span> [<a href="https://arxiv.org/pdf/1910.11592">pdf</a>, <a href="https://arxiv.org/format/1910.11592">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/stz2982">10.1093/mnras/stz2982 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Study of the Galactic radio sources in the SCORPIO survey resolved by ATCA at 2.1 GHz </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Franzen%2C+T+M+O">T. M. O. Franzen</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Schillir%C3%B2%2C+F">F. Schillir貌</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Agliozzo%2C+C">C. Agliozzo</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="1910.11592v1-abstract-short" style="display: inline;"> We present a catalogue of a large sample of extended radio sources in the SCORPIO field, observed and resolved by the Australia Telescope Compact Array. SCORPIO, a pathfinder project for addressing the early operations of the Australia SKA Pathfinder, is a survey of ~5 square degrees between 1.4 and 3.1 GHz, centered at l=343.5掳, b=0.75掳 and with an angular resolution of about 10 arcsec. It is aim… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.11592v1-abstract-full').style.display = 'inline'; document.getElementById('1910.11592v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.11592v1-abstract-full" style="display: none;"> We present a catalogue of a large sample of extended radio sources in the SCORPIO field, observed and resolved by the Australia Telescope Compact Array. SCORPIO, a pathfinder project for addressing the early operations of the Australia SKA Pathfinder, is a survey of ~5 square degrees between 1.4 and 3.1 GHz, centered at l=343.5掳, b=0.75掳 and with an angular resolution of about 10 arcsec. It is aimed at understanding the scientific and technical challenges to be faced by future Galactic surveys. With a mean sensitivity around 100 $渭$Jy/beam and the possibility to recover angular scales at least up to 4 arcmin, we extracted 99 extended sources, 35 of them detected for the first time. Among the 64 known sources 55 had at least a tentative classification in literature. Studying the radio morphology and comparing the radio emission with infrared we propose as candidates 6 new H II regions, 2 new planetary nebulae, 2 new luminous blue variable or Wolf--Rayet stars and 3 new supernova remnants. This study provides an overview of the potentiality of future radio surveys in terms of Galactic source extraction and characterization and a discussion on the difficulty to reduce and analyze interferometric data on the Galactic plane. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.11592v1-abstract-full').style.display = 'none'; document.getElementById('1910.11592v1-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, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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/astro-ph?searchtype=author&query=Joseph%2C+T+D">T. D. Joseph</a>, <a href="/search/astro-ph?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=Boji%C4%8Di%C4%87%2C+I">I. Boji膷i膰</a>, <a href="/search/astro-ph?searchtype=author&query=Alexander%2C+E+L">E. L. Alexander</a>, <a href="/search/astro-ph?searchtype=author&query=Wong%2C+G+F">G. F. Wong</a>, <a href="/search/astro-ph?searchtype=author&query=Andernach%2C+H">H. Andernach</a>, <a href="/search/astro-ph?searchtype=author&query=Leverenz%2C+H">H. Leverenz</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Alsaberi%2C+R+Z+E">R. Z. E. Alsaberi</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+C">C. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+L+A">L. A. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Bozzetto%2C+L+M">L. M. Bozzetto</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Bunton%2C+J+D">J. D. Bunton</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Collier%2C+J+D">J. D. Collier</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9nes%2C+H">H. D茅nes</a>, <a href="/search/astro-ph?searchtype=author&query=Fukui%2C+Y">Y. Fukui</a>, <a href="/search/astro-ph?searchtype=author&query=Galvin%2C+T">T. Galvin</a>, <a href="/search/astro-ph?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Kapinska%2C+A+D">A. D. Kapinska</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/astro-ph?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/1909.06116">arXiv:1909.06116</a> <span> [<a href="https://arxiv.org/pdf/1909.06116">pdf</a>, <a href="https://arxiv.org/format/1909.06116">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Computation">stat.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Machine Learning">stat.ML</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/10.1017/pasa.2019.29">10.1017/pasa.2019.29 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CAESAR source finder: recent developments and testing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Vitello%2C+F">F. Vitello</a>, <a href="/search/astro-ph?searchtype=author&query=Becciani%2C+U">U. Becciani</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C">C. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Calanducci%2C+A">A. Calanducci</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Costa%2C+A">A. Costa</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Schillir%C3%B2%2C+F">F. Schillir貌</a>, <a href="/search/astro-ph?searchtype=author&query=Sciacca%2C+E">E. Sciacca</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</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="1909.06116v1-abstract-short" style="display: inline;"> A new era in radioastronomy will begin with the upcoming large-scale surveys planned at the Australian Square Kilometre Array Pathfinder (ASKAP). ASKAP started its Early Science program in October 2017 and several target fields were observed during the array commissioning phase. The SCORPIO field was the first observed in the Galactic Plane in Band 1 (792-1032 MHz) using 15 commissioned antennas.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.06116v1-abstract-full').style.display = 'inline'; document.getElementById('1909.06116v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.06116v1-abstract-full" style="display: none;"> A new era in radioastronomy will begin with the upcoming large-scale surveys planned at the Australian Square Kilometre Array Pathfinder (ASKAP). ASKAP started its Early Science program in October 2017 and several target fields were observed during the array commissioning phase. The SCORPIO field was the first observed in the Galactic Plane in Band 1 (792-1032 MHz) using 15 commissioned antennas. The achieved sensitivity and large field of view already allow to discover new sources and survey thousands of existing ones with improved precision with respect to previous surveys. Data analysis is currently ongoing to deliver the first source catalogue. Given the increased scale of the data, source extraction and characterization, even in this Early Science phase, have to be carried out in a mostly automated way. This process presents significant challenges due to the presence of extended objects and diffuse emission close to the Galactic Plane. In this context we have extended and optimized a novel source finding tool, named CAESAR , to allow extraction of both compact and extended sources from radio maps. A number of developments have been done driven by the analysis of the SCORPIO map and in view of the future ASKAP Galactic Plane survey. The main goals are the improvement of algorithm performances and scalability as well as of software maintainability and usability within the radio community. In this paper we present the current status of CAESAR and report a first systematic characterization of its performance for both compact and extended sources using simulated maps. Future prospects are discussed in light of the obtained results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.06116v1-abstract-full').style.display = 'none'; document.getElementById('1909.06116v1-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> 13 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">15 pages, 10 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Publications of the Astronomical Society of Australia, 2019, 36, E037 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1809.07504">arXiv:1809.07504</a> <span> [<a href="https://arxiv.org/pdf/1809.07504">pdf</a>, <a href="https://arxiv.org/ps/1809.07504">ps</a>, <a href="https://arxiv.org/format/1809.07504">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/mnrasl/sly179">10.1093/mnrasl/sly179 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The polarization mode of the auroral radio emission from the early-type star HD142301 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Oskinova%2C+L+M">L. M. Oskinova</a>, <a href="/search/astro-ph?searchtype=author&query=Ignace%2C+R">R. Ignace</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+N+M">N. M. Phillips</a>, <a href="/search/astro-ph?searchtype=author&query=Agliozzo%2C+C">C. Agliozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Todt%2C+H">H. Todt</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Leone%2C+F">F. Leone</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="1809.07504v1-abstract-short" style="display: inline;"> We report the detection of the auroral radio emission from the early-type magnetic star HD142301. New VLA observations of HD142301 detected highly polarized amplified emission occurring at fixed stellar orientations. The coherent emission mechanism responsible for the stellar auroral radio emission amplifies the radiation within a narrow beam, making the star where this phenomenon occurs similar t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.07504v1-abstract-full').style.display = 'inline'; document.getElementById('1809.07504v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1809.07504v1-abstract-full" style="display: none;"> We report the detection of the auroral radio emission from the early-type magnetic star HD142301. New VLA observations of HD142301 detected highly polarized amplified emission occurring at fixed stellar orientations. The coherent emission mechanism responsible for the stellar auroral radio emission amplifies the radiation within a narrow beam, making the star where this phenomenon occurs similar to a radio lighthouse. The elementary emission process responsible for the auroral radiation mainly amplifies one of the two magneto-ionic modes of the electromagnetic wave. This explains why the auroral pulses are highly circularly polarized. The auroral radio emission of HD142301 is characterized by a reversal of the sense of polarization as the star rotates. The effective magnetic field curve of HD142301 is also available making it possible to correlate the transition from the left to the right-hand circular polarization sense (and vice-versa) of the auroral pulses with the known orientation of the stellar magnetic field. The results presented in this letter have implications for the estimation of the dominant magneto-ionic mode amplified within the HD142301 magnetosphere. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.07504v1-abstract-full').style.display = 'none'; document.getElementById('1809.07504v1-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 September, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2018. </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">5 pages, 4 figures; accepted to MNRAS Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1803.08338">arXiv:1803.08338</a> <span> [<a href="https://arxiv.org/pdf/1803.08338">pdf</a>, <a href="https://arxiv.org/format/1803.08338">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/sty2280">10.1093/mnras/sty2280 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detection of Alpha Centauri at radio wavelengths: chromospheric emission and search for star-planet interaction </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Agliozzo%2C+C">C. Agliozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</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="1803.08338v2-abstract-short" style="display: inline;"> At radio wavelengths, solar-type stars emit thermal free-free and gyroresonance, gyrosynchrotron, and impulsive coherent emission. Thermal free-free emission originates at layers where the optical depth is close to unit, while high brightness temperature, variable emission, can be due to flares via gyrosynchrotron emission. We observed the alpha Cen system with the Australian Telescope Compact Arr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.08338v2-abstract-full').style.display = 'inline'; document.getElementById('1803.08338v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1803.08338v2-abstract-full" style="display: none;"> At radio wavelengths, solar-type stars emit thermal free-free and gyroresonance, gyrosynchrotron, and impulsive coherent emission. Thermal free-free emission originates at layers where the optical depth is close to unit, while high brightness temperature, variable emission, can be due to flares via gyrosynchrotron emission. We observed the alpha Cen system with the Australian Telescope Compact Array at 2 GHz for three days and 17 GHz for one day. Both stars have been detected at 17 GHz, while only an upper limit has been obtained at low frequency despite the longer integration time. The brightness temperatures are consistent with the temperature of the upper chromosphere of the Sun. Inverting the formulae of the free-free emission, the average electron density of the plasma has been inferred. The same procedure was applied to the data in the millimetre recently acquired with ALMA. A comparison with the atmospheric solar models reveals a higher level of activity in alpha Cen B rather than in alpha Cen A, even if still at quiescent level. The non detection at 2 GHz allows us to put a lower limit in the filling factor of active regions. The claimed detection of an Earth size planet in close orbit to alpha Cen B, although doubtful, opens the opportunity to check the existence of Star-Planet Magnetic Interaction (SPMI). We constructed dynamic spectra in the 1.3 - 2.9 GHz of the 2 stars to search for time-variable coherent emission but obtained a null result. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.08338v2-abstract-full').style.display = 'none'; document.getElementById('1803.08338v2-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 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 March, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2018. </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">Submitted to MNRAS, 9 pages, 7 Figures, MNRAS, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1711.06263">arXiv:1711.06263</a> <span> [<a href="https://arxiv.org/pdf/1711.06263">pdf</a>, <a href="https://arxiv.org/format/1711.06263">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/stx2560">10.1093/mnras/stx2560 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First Extended Catalogue of Galactic Bubbles InfraRed Fluxes from WISE and Herschel Surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Carey%2C+D">D. Carey</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C">C. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Bulpitt%2C+A">A. Bulpitt</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Molinari%2C+S">S. Molinari</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="1711.06263v1-abstract-short" style="display: inline;"> In this paper, we present the first extended catalogue of far-infrared fluxes of Galactic bubbles. Fluxes were estimated for 1814 bubbles, defined here as the `golden sample', and were selected from the Milky Way Project First Data Release (Simpson et al.) The golden sample was comprised of bubbles identified within the Wide-field Infrared Survey Explorer (WISE) dataset (using 12- and 22-$渭$m imag… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.06263v1-abstract-full').style.display = 'inline'; document.getElementById('1711.06263v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1711.06263v1-abstract-full" style="display: none;"> In this paper, we present the first extended catalogue of far-infrared fluxes of Galactic bubbles. Fluxes were estimated for 1814 bubbles, defined here as the `golden sample', and were selected from the Milky Way Project First Data Release (Simpson et al.) The golden sample was comprised of bubbles identified within the Wide-field Infrared Survey Explorer (WISE) dataset (using 12- and 22-$渭$m images) and Herschel data (using 70-, 160-, 250-, 350- and 500-$渭$m wavelength images). Flux estimation was achieved initially via classical aperture photometry and then by an alternative image analysis algorithm that used active contours. The accuracy of the two methods was tested by comparing the estimated fluxes for a sample of bubbles, made up of 126 H II regions and 43 planetary nebulae, which were identified by Anderson et al. The results of this paper demonstrate that a good agreement between the two was found. This is by far the largest and most homogeneous catalogue of infrared fluxes measured for Galactic bubbles and it is a step towards the fully automated analysis of astronomical datasets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.06263v1-abstract-full').style.display = 'none'; document.getElementById('1711.06263v1-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 November, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">22 pages, 16 figures, 10 tables, published on MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS, 473, 3671-3692 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1710.04702">arXiv:1710.04702</a> <span> [<a href="https://arxiv.org/pdf/1710.04702">pdf</a>, <a href="https://arxiv.org/format/1710.04702">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> <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/stx2445">10.1093/mnras/stx2445 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SCORPIO-II: Spectral indices of weak Galactic radio sources </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Franzen%2C+T+M+O">T. M. O. Franzen</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Marvil%2C+J">J. Marvil</a>, <a href="/search/astro-ph?searchtype=author&query=Agliozzo%2C+C">C. Agliozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</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="1710.04702v1-abstract-short" style="display: inline;"> In the next few years the classification of radio sources observed by the large surveys will be a challenging problem, and spectral index is a powerful tool for addressing it. Here we present an algorithm to estimate the spectral index of sources from multiwavelength radio images. We have applied our algorithm to SCORPIO (Umana et al. 2015), a Galactic Plane survey centred around 2.1 GHz carried o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.04702v1-abstract-full').style.display = 'inline'; document.getElementById('1710.04702v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1710.04702v1-abstract-full" style="display: none;"> In the next few years the classification of radio sources observed by the large surveys will be a challenging problem, and spectral index is a powerful tool for addressing it. Here we present an algorithm to estimate the spectral index of sources from multiwavelength radio images. We have applied our algorithm to SCORPIO (Umana et al. 2015), a Galactic Plane survey centred around 2.1 GHz carried out with ATCA, and found we can measure reliable spectral indices only for sources stronger than 40 times the rms noise. Above a threshold of 1 mJy, the source density in SCORPIO is 20 percent greater than in a typical extra-galactic field, like ATLAS (Norris et al. 2006), because of the presence of Galactic sources. Among this excess population, 16 sources per square degree have a spectral index of about zero, suggesting optically thin thermal emission such as Hii regions and planetary nebulae, while 12 per square degree present a rising spectrum, suggesting optically thick thermal emission such as stars and UCHii regions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.04702v1-abstract-full').style.display = 'none'; document.getElementById('1710.04702v1-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> 26 September, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">12 pages, 11 figures, accepted by 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/1612.05039">arXiv:1612.05039</a> <span> [<a href="https://arxiv.org/pdf/1612.05039">pdf</a>, <a href="https://arxiv.org/ps/1612.05039">ps</a>, <a href="https://arxiv.org/format/1612.05039">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</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/stw3074">10.1093/mnras/stw3074 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Exploring the multifaceted circumstellar environment of the Luminous Blue Variable HR Carinae </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Agliozzo%2C+C">C. Agliozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Molinari%2C+S">S. Molinari</a>, <a href="/search/astro-ph?searchtype=author&query=Schillir%C3%B2%2C+F">F. Schillir貌</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="1612.05039v1-abstract-short" style="display: inline;"> We present a multi-wavelength study of the Galactic Luminous Blue Variable HR Carinae, based on new high resolution mid-infrared (IR) and radio images obtained with the Very Large Telescope (VLT) and the Australia Telescope Compact Array (ATCA), which have been complemented by far-infrared Herschel-PACS observations and ATCA archive data. The Herschel images reveal the large-scale distribution of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.05039v1-abstract-full').style.display = 'inline'; document.getElementById('1612.05039v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1612.05039v1-abstract-full" style="display: none;"> We present a multi-wavelength study of the Galactic Luminous Blue Variable HR Carinae, based on new high resolution mid-infrared (IR) and radio images obtained with the Very Large Telescope (VLT) and the Australia Telescope Compact Array (ATCA), which have been complemented by far-infrared Herschel-PACS observations and ATCA archive data. The Herschel images reveal the large-scale distribution of the dusty emitting nebula, which extends mainly to the North-East direction, up to 70 arcsec from the central star, and is oriented along the direction of the space motion of the star. In the mid-infrared images, the brightness distribution is characterized by two arc-shaped structures, tracing an inner envelope surrounding the central star more closely. At radio wavelengths, the ionized gas emission lies on the opposite side of the cold dust with respect to the position of the star, as if the ionized front was confined by the surrounding medium in the North-South direction. The comparison with previous data indicates significant changes in the radio nebula morphology and in the mass-loss rate from the central star, which has increased from 6.1$\times10^{-6}$ M$_{\odot}$yr$^{-1}$ in 1994-1995 to $1.17\times10^{-5}$ M$_{\odot}$yr$^{-1}$ in 2014. We investigate possible scenarios that could have generated the complex circumstellar environment revealed by our multi-wavelength data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.05039v1-abstract-full').style.display = 'none'; document.getElementById('1612.05039v1-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 December, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">MNRAS, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1609.00003">arXiv:1609.00003</a> <span> [<a href="https://arxiv.org/pdf/1609.00003">pdf</a>, <a href="https://arxiv.org/format/1609.00003">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/stw2053">10.1093/mnras/stw2053 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High-resolution Very Large Array observations of 18 MIPSGAL bubbles </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">Adriano Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">Corrado Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">Paolo Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">Grazia Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C">Carla Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">Filomena Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Agliozzo%2C+C">Claudia Agliozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">Simone Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Flagey%2C+N">Nicolas Flagey</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+K">Kevin Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">Luciano Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">Francesco Cavallaro</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="1609.00003v1-abstract-short" style="display: inline;"> We present radio observations of 18 MIPSGAL bubbles performed at 5 GHz (6 cm) with the Karl G. Jansky Very Large Array in configuration B and BnA. The observations were aimed at understanding what kind of information high-resolution and high-sensitivity radio maps can supply on the circumstellar envelopes of different kinds of evolved stars and what their comparison with infrared images with simil… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.00003v1-abstract-full').style.display = 'inline'; document.getElementById('1609.00003v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1609.00003v1-abstract-full" style="display: none;"> We present radio observations of 18 MIPSGAL bubbles performed at 5 GHz (6 cm) with the Karl G. Jansky Very Large Array in configuration B and BnA. The observations were aimed at understanding what kind of information high-resolution and high-sensitivity radio maps can supply on the circumstellar envelopes of different kinds of evolved stars and what their comparison with infrared images with similar resolution can tell us. We found that the 18 bubbles can be grouped into five categories according to their radio morphology. The three bubbles presenting a central point source in the radio images all correspond to luminous blue variable star candidates. Eleven bubbles show an elliptical shape and the total lack of a central object in the radio, and are likely associated with planetary nebulae. Under this assumption we derive their distance, their ionized mass and their distribution on the Galactic plane. We discuss the possibility that the MIPSGAL bubbles catalogue (428 objects) may contain a large fraction of all Galactic planetary nebulae located at a distance between 1.4 kpc and 6.9 kpc and lying in the MIPSGAL field of view. Among the remaining bubbles we identify also a H II region and a proto-planetary nebula candidate. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.00003v1-abstract-full').style.display = 'none'; document.getElementById('1609.00003v1-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> 31 August, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2016. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1605.01852">arXiv:1605.01852</a> <span> [<a href="https://arxiv.org/pdf/1605.01852">pdf</a>, <a href="https://arxiv.org/format/1605.01852">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</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/stw982">10.1093/mnras/stw982 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Automated detection of extended sources in radio maps: progress from the SCORPIO survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Schillir%C3%B2%2C+F">F. Schillir貌</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</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="1605.01852v1-abstract-short" style="display: inline;"> Automated source extraction and parameterization represents a crucial challenge for the next-generation radio interferometer surveys, such as those performed with the Square Kilometre Array (SKA) and its precursors. In this paper we present a new algorithm, dubbed CAESAR (Compact And Extended Source Automated Recognition), to detect and parametrize extended sources in radio interferometric maps. I… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.01852v1-abstract-full').style.display = 'inline'; document.getElementById('1605.01852v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1605.01852v1-abstract-full" style="display: none;"> Automated source extraction and parameterization represents a crucial challenge for the next-generation radio interferometer surveys, such as those performed with the Square Kilometre Array (SKA) and its precursors. In this paper we present a new algorithm, dubbed CAESAR (Compact And Extended Source Automated Recognition), to detect and parametrize extended sources in radio interferometric maps. It is based on a pre-filtering stage, allowing image denoising, compact source suppression and enhancement of diffuse emission, followed by an adaptive superpixel clustering stage for final source segmentation. A parameterization stage provides source flux information and a wide range of morphology estimators for post-processing analysis. We developed CAESAR in a modular software library, including also different methods for local background estimation and image filtering, along with alternative algorithms for both compact and diffuse source extraction. The method was applied to real radio continuum data collected at the Australian Telescope Compact Array (ATCA) within the SCORPIO project, a pathfinder of the ASKAP-EMU survey. The source reconstruction capabilities were studied over different test fields in the presence of compact sources, imaging artefacts and diffuse emission from the Galactic plane and compared with existing algorithms. When compared to a human-driven analysis, the designed algorithm was found capable of detecting known target sources and regions of diffuse emission, outperforming alternative approaches over the considered fields. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.01852v1-abstract-full').style.display = 'none'; document.getElementById('1605.01852v1-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, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">15 pages, 9 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1604.03637">arXiv:1604.03637</a> <span> [<a href="https://arxiv.org/pdf/1604.03637">pdf</a>, <a href="https://arxiv.org/format/1604.03637">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</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"> The Pierre Auger Observatory Upgrade - Preliminary Design Report </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aab%2C+A">A. Aab</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Allison%2C+P">P. Allison</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">N. Arsene</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/astro-ph?searchtype=author&query=Avenier%2C+M">M. Avenier</a> , et al. (440 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="1604.03637v1-abstract-short" style="display: inline;"> The Pierre Auger Observatory has begun a major Upgrade of its already impressive capabilities, with an emphasis on improved mass composition determination using the surface detectors of the Observatory. Known as AugerPrime, the upgrade will include new 4 m$^2$ plastic scintillator detectors on top of all 1660 water-Cherenkov detectors, updated and more flexible surface detector electronics, a larg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.03637v1-abstract-full').style.display = 'inline'; document.getElementById('1604.03637v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1604.03637v1-abstract-full" style="display: none;"> The Pierre Auger Observatory has begun a major Upgrade of its already impressive capabilities, with an emphasis on improved mass composition determination using the surface detectors of the Observatory. Known as AugerPrime, the upgrade will include new 4 m$^2$ plastic scintillator detectors on top of all 1660 water-Cherenkov detectors, updated and more flexible surface detector electronics, a large array of buried muon detectors, and an extended duty cycle for operations of the fluorescence detectors. This Preliminary Design Report was produced by the Collaboration in April 2015 as an internal document and information for funding agencies. It outlines the scientific and technical case for AugerPrime. We now release it to the public via the arXiv server. We invite you to review the large number of fundamental results already achieved by the Observatory and our plans for the future. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.03637v1-abstract-full').style.display = 'none'; document.getElementById('1604.03637v1-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 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">201 pages</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1603.05866">arXiv:1603.05866</a> <span> [<a href="https://arxiv.org/pdf/1603.05866">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> An Innovative Workspace for The Cherenkov Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Costa%2C+A">Alessandro Costa</a>, <a href="/search/astro-ph?searchtype=author&query=Sciacca%2C+E">Eva Sciacca</a>, <a href="/search/astro-ph?searchtype=author&query=Becciani%2C+U">Ugo Becciani</a>, <a href="/search/astro-ph?searchtype=author&query=Massimino%2C+P">Piero Massimino</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">Simone Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez%2C+D">David Sanchez</a>, <a href="/search/astro-ph?searchtype=author&query=Vitello%2C+F">Fabio Vitello</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="1603.05866v2-abstract-short" style="display: inline;"> The Cherenkov Telescope Array (CTA) is an initiative to build the next generation, ground-based gamma-ray observatories. We present a prototype workspace developed at INAF that aims at providing innovative solutions for the CTA community. The workspace leverages open source technologies providing web access to a set of tools widely used by the CTA community. Two different user interaction models,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1603.05866v2-abstract-full').style.display = 'inline'; document.getElementById('1603.05866v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1603.05866v2-abstract-full" style="display: none;"> The Cherenkov Telescope Array (CTA) is an initiative to build the next generation, ground-based gamma-ray observatories. We present a prototype workspace developed at INAF that aims at providing innovative solutions for the CTA community. The workspace leverages open source technologies providing web access to a set of tools widely used by the CTA community. Two different user interaction models, connected to an authentication and authorization infrastructure, have been implemented in this workspace. The first one is a workflow management system accessed via a science gateway (based on the Liferay platform) and the second one is an interactive virtual desktop environment. The integrated workflow system allows to run applications used in astronomy and physics researches into distributed computing infrastructures (ranging from clusters to grids and clouds). The interactive desktop environment allows to use many software packages without any installation on local desktops exploiting their native graphical user interfaces. The science gateway and the interactive desktop environment are connected to the authentication and authorization infrastructure composed by a Shibboleth identity provider and a Grouper authorization solution. The Grouper released attributes are consumed by the science gateway to authorize the access to specific web resources and the role management mechanism in Liferay provides the attribute-role mapping. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1603.05866v2-abstract-full').style.display = 'none'; document.getElementById('1603.05866v2-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> 31 March, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 March, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2016. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1504.05397">arXiv:1504.05397</a> <span> [<a href="https://arxiv.org/pdf/1504.05397">pdf</a>, <a href="https://arxiv.org/format/1504.05397">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/10.1103/PhysRevD.91.092008">10.1103/PhysRevD.91.092008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An improved limit to the diffuse flux of ultra-high energy neutrinos from the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aab%2C+A">Alexander Aab</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">Pedro Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">Marco Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Ahn%2C+E">Eun-Joo Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">Imen Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I">Ivone Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">Ingomar Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Allison%2C+P">Patrick Allison</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">Alejandro Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Castillo%2C+J+A">Jesus Alvarez Castillo</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">Jaime Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">Rafael Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosio%2C+M">Michelangelo Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aminaei%2C+A">Amin Aminaei</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">Luis Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">Sofia Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">Carla Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Aranda%2C+V+M">Victor Manuel Aranda</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">Fernando Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">Nicusor Arsene</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H+G">Hern谩n Gonzalo Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">Pedro Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">Julien Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Ave%2C+M">Maximo Ave</a> , et al. (440 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="1504.05397v2-abstract-short" style="display: inline;"> Neutrinos in the cosmic ray flux with energies near 1 EeV and above are detectable with the Surface Detector array of the Pierre Auger Observatory. We report here on searches through Auger data from 1 January 2004 until 20 June 2013. No neutrino candidates were found, yielding a limit to the diffuse flux of ultra-high energy neutrinos that challenges the Waxman-Bahcall bound predictions. Neutrino… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.05397v2-abstract-full').style.display = 'inline'; document.getElementById('1504.05397v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1504.05397v2-abstract-full" style="display: none;"> Neutrinos in the cosmic ray flux with energies near 1 EeV and above are detectable with the Surface Detector array of the Pierre Auger Observatory. We report here on searches through Auger data from 1 January 2004 until 20 June 2013. No neutrino candidates were found, yielding a limit to the diffuse flux of ultra-high energy neutrinos that challenges the Waxman-Bahcall bound predictions. Neutrino identification is attempted using the broad time-structure of the signals expected in the SD stations, and is efficiently done for neutrinos of all flavors interacting in the atmosphere at large zenith angles, as well as for "Earth-skimming" neutrino interactions in the case of tau neutrinos. In this paper the searches for downward-going neutrinos in the zenith angle bins $60^\circ-75^\circ$ and $75^\circ-90^\circ$ as well as for upward-going neutrinos, are combined to give a single limit. The $90\%$ C.L. single-flavor limit to the diffuse flux of ultra-high energy neutrinos with an $E^{-2}$ spectrum in the energy range $1.0 \times 10^{17}$ eV - $2.5 \times 10^{19}$ eV is $E_谓^2 dN_谓/dE_谓< 6.4 \times 10^{-9}~ {\rm GeV~ cm^{-2}~ s^{-1}~ sr^{-1}}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.05397v2-abstract-full').style.display = 'none'; document.getElementById('1504.05397v2-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 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 April, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">Replaced with published version. Added journal reference and DOI</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-15-150-AD-AE-CD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 91, 092008 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1503.07786">arXiv:1503.07786</a> <span> [<a href="https://arxiv.org/pdf/1503.07786">pdf</a>, <a href="https://arxiv.org/format/1503.07786">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="High Energy Physics - Experiment">hep-ex</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/10.1088/1475-7516/2015/08/049">10.1088/1475-7516/2015/08/049 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the cosmic ray spectrum above $4{\times}10^{18}$ eV using inclined events detected with the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aab%2C+A">Alexander Aab</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">Pedro Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">Marco Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Ahn%2C+E">Eun-Joo Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">Imen Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I">Ivone Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">Ingomar Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Allison%2C+P">Patrick Allison</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">Alejandro Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Castillo%2C+J+A">Jesus Alvarez Castillo</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">Jaime Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">Rafael Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosio%2C+M">Michelangelo Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aminaei%2C+A">Amin Aminaei</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">Luis Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">Sofia Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">Carla Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Aranda%2C+V+M">Victor Manuel Aranda</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">Fernando Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">Nicusor Arsene</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H+G">Hern谩n Gonzalo Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">Pedro Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">Julien Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Ave%2C+M">Maximo Ave</a> , et al. (439 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="1503.07786v2-abstract-short" style="display: inline;"> A measurement of the cosmic-ray spectrum for energies exceeding $4{\times}10^{18}$ eV is presented, which is based on the analysis of showers with zenith angles greater than $60^{\circ}$ detected with the Pierre Auger Observatory between 1 January 2004 and 31 December 2013. The measured spectrum confirms a flux suppression at the highest energies. Above $5.3{\times}10^{18}$ eV, the "ankle", the fl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.07786v2-abstract-full').style.display = 'inline'; document.getElementById('1503.07786v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1503.07786v2-abstract-full" style="display: none;"> A measurement of the cosmic-ray spectrum for energies exceeding $4{\times}10^{18}$ eV is presented, which is based on the analysis of showers with zenith angles greater than $60^{\circ}$ detected with the Pierre Auger Observatory between 1 January 2004 and 31 December 2013. The measured spectrum confirms a flux suppression at the highest energies. Above $5.3{\times}10^{18}$ eV, the "ankle", the flux can be described by a power law $E^{-纬}$ with index $纬=2.70 \pm 0.02 \,\text{(stat)} \pm 0.1\,\text{(sys)}$ followed by a smooth suppression region. For the energy ($E_\text{s}$) at which the spectral flux has fallen to one-half of its extrapolated value in the absence of suppression, we find $E_\text{s}=(5.12\pm0.25\,\text{(stat)}^{+1.0}_{-1.2}\,\text{(sys)}){\times}10^{19}$ eV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.07786v2-abstract-full').style.display = 'none'; document.getElementById('1503.07786v2-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 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 March, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">Replaced with published version. Added journal reference and DOI</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-15-099-AD-AE-CD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 08 (2015) 049 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1409.3128">arXiv:1409.3128</a> <span> [<a href="https://arxiv.org/pdf/1409.3128">pdf</a>, <a href="https://arxiv.org/ps/1409.3128">ps</a>, <a href="https://arxiv.org/format/1409.3128">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</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/794/2/172">10.1088/0004-637X/794/2/172 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searches for Large-Scale Anisotropy in the Arrival Directions of Cosmic Rays Detected above Energy of $10^{19}$ eV at the Pierre Auger Observatory and the Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Auger%2C+T+P">The Pierre Auger</a>, <a href="/search/astro-ph?searchtype=author&query=Collaborations%2C+T+A">Telescope Array Collaborations</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Aab%2C+A">A. Aab</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Allison%2C+P">P. Allison</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a> , et al. (584 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="1409.3128v1-abstract-short" style="display: inline;"> Spherical harmonic moments are well-suited for capturing anisotropy at any scale in the flux of cosmic rays. An unambiguous measurement of the full set of spherical harmonic coefficients requires full-sky coverage. This can be achieved by combining data from observatories located in both the northern and southern hemispheres. To this end, a joint analysis using data recorded at the Telescope Array… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.3128v1-abstract-full').style.display = 'inline'; document.getElementById('1409.3128v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1409.3128v1-abstract-full" style="display: none;"> Spherical harmonic moments are well-suited for capturing anisotropy at any scale in the flux of cosmic rays. An unambiguous measurement of the full set of spherical harmonic coefficients requires full-sky coverage. This can be achieved by combining data from observatories located in both the northern and southern hemispheres. To this end, a joint analysis using data recorded at the Telescope Array and the Pierre Auger Observatory above $10^{19}$ eV is presented in this work. The resulting multipolar expansion of the flux of cosmic rays allows us to perform a series of anisotropy searches, and in particular to report on the angular power spectrum of cosmic rays above $10^{19}$ eV. No significant deviation from isotropic expectations is found throughout the analyses performed. Upper limits on the amplitudes of the dipole and quadrupole moments are derived as a function of the direction in the sky, varying between 7% and 13% for the dipole and between 7% and 10% for a symmetric quadrupole. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.3128v1-abstract-full').style.display = 'none'; document.getElementById('1409.3128v1-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 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">33 pages, 13 figures, to appear in The Astrophysical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ, 794, 172 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1407.3214">arXiv:1407.3214</a> <span> [<a href="https://arxiv.org/pdf/1407.3214">pdf</a>, <a href="https://arxiv.org/ps/1407.3214">ps</a>, <a href="https://arxiv.org/format/1407.3214">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="High Energy Physics - Experiment">hep-ex</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/10.1088/1475-7516/2014/08/019">10.1088/1475-7516/2014/08/019 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Reconstruction of inclined air showers detected with the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aab%2C+A">A. Aab</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Allison%2C+P">P. Allison</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Ave%2C+M">M. Ave</a> , et al. (463 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="1407.3214v1-abstract-short" style="display: inline;"> We describe the method devised to reconstruct inclined cosmic-ray air showers with zenith angles greater than $60^\circ$ detected with the surface array of the Pierre Auger Observatory. The measured signals at the ground level are fitted to muon density distributions predicted with atmospheric cascade models to obtain the relative shower size as an overall normalization parameter. The method is ev… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.3214v1-abstract-full').style.display = 'inline'; document.getElementById('1407.3214v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1407.3214v1-abstract-full" style="display: none;"> We describe the method devised to reconstruct inclined cosmic-ray air showers with zenith angles greater than $60^\circ$ detected with the surface array of the Pierre Auger Observatory. The measured signals at the ground level are fitted to muon density distributions predicted with atmospheric cascade models to obtain the relative shower size as an overall normalization parameter. The method is evaluated using simulated showers to test its performance. The energy of the cosmic rays is calibrated using a sub-sample of events reconstructed with both the fluorescence and surface array techniques. The reconstruction method described here provides the basis of complementary analyses including an independent measurement of the energy spectrum of ultra-high energy cosmic rays using very inclined events collected by the Pierre Auger Observatory. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.3214v1-abstract-full').style.display = 'none'; document.getElementById('1407.3214v1-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 July, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">27 pages, 19 figures, accepted for publication in Journal of Cosmology and Astroparticle Physics (JCAP)</span> </p> </li> </ol> <nav class="pagination 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