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breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Saikia%2C+P&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Saikia%2C+P&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Saikia%2C+P&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/2411.00013">arXiv:2411.00013</a> <span> [<a href="https://arxiv.org/pdf/2411.00013">pdf</a>, <a href="https://arxiv.org/ps/2411.00013">ps</a>, <a href="https://arxiv.org/format/2411.00013">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Number Theory">math.NT</span> </div> </div> <p class="title is-5 mathjax"> Further Arithmetic Properties of Overcubic Partition Triples </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Saikia%2C+M+P">Manjil P. Saikia</a>, <a href="/search/?searchtype=author&query=Sarma%2C+A">Abhishek Sarma</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="2411.00013v1-abstract-short" style="display: inline;"> In this short note, we prove several new congruences for the overcubic partition triples function, using both elementary techniques and the theory of modular forms. These extend the recent list of such congruences given by Nayaka, Dharmendra, and Kumar (2024). We also generalize overcubic partition triples to overcubic partition $k$-tuples and prove a few arithmetic properties for these type of pa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.00013v1-abstract-full').style.display = 'inline'; document.getElementById('2411.00013v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.00013v1-abstract-full" style="display: none;"> In this short note, we prove several new congruences for the overcubic partition triples function, using both elementary techniques and the theory of modular forms. These extend the recent list of such congruences given by Nayaka, Dharmendra, and Kumar (2024). We also generalize overcubic partition triples to overcubic partition $k$-tuples and prove a few arithmetic properties for these type of partitions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.00013v1-abstract-full').style.display = 'none'; document.getElementById('2411.00013v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 October, 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">12 pages, to appear in the Bulletin of the Australian Mathematical Society</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 11P81; 11P83 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.23335">arXiv:2410.23335</a> <span> [<a href="https://arxiv.org/pdf/2410.23335">pdf</a>, <a href="https://arxiv.org/format/2410.23335">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> <p class="title is-5 mathjax"> Do Neutron Star Ultra-Luminous X-Ray Sources Masquerade as Intermediate Mass Black Holes in Radio and X-Ray? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Panurach%2C+T">Teresa Panurach</a>, <a href="/search/?searchtype=author&query=Dage%2C+K+C">Kristen C. Dage</a>, <a href="/search/?searchtype=author&query=Urquhart%2C+R">Ryan Urquhart</a>, <a href="/search/?searchtype=author&query=Plotkin%2C+R+M">Richard M. Plotkin</a>, <a href="/search/?searchtype=author&query=Paul%2C+J+D">Jeremiah D. Paul</a>, <a href="/search/?searchtype=author&query=Bahramian%2C+A">Arash Bahramian</a>, <a href="/search/?searchtype=author&query=Brumback%2C+M+C">McKinley C. Brumback</a>, <a href="/search/?searchtype=author&query=Galvin%2C+T+J">Timothy J. Galvin</a>, <a href="/search/?searchtype=author&query=Molina%2C+I">Isabella Molina</a>, <a href="/search/?searchtype=author&query=Miller-Jones%2C+J+C+A">James C. A. Miller-Jones</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">Payaswini Saikia</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="2410.23335v1-abstract-short" style="display: inline;"> Ultraluminous X-ray sources (ULXs) were once largely believed to be powered by super-Eddington accretion onto stellar-mass black holes, although in some rare cases, ULXs also serve as potential candidates for (sub-Eddington) intermediate mass black holes. However, a total of eight ULXs have now been confirmed to be powered by neutron stars, thanks to observed pulsations, and may act as contaminant… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.23335v1-abstract-full').style.display = 'inline'; document.getElementById('2410.23335v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.23335v1-abstract-full" style="display: none;"> Ultraluminous X-ray sources (ULXs) were once largely believed to be powered by super-Eddington accretion onto stellar-mass black holes, although in some rare cases, ULXs also serve as potential candidates for (sub-Eddington) intermediate mass black holes. However, a total of eight ULXs have now been confirmed to be powered by neutron stars, thanks to observed pulsations, and may act as contaminants for radio/X-ray selection of intermediate mass black holes. Here we present the first comprehensive radio study of seven known neutron star ULXs using new and archival data from the Karl G. Jansky Very Large Array and the Australia Telescope Compact Array, combined with the literature. Across this sample there is only one confident radio detection, from the Galactic neutron star ULX Swift J0243.6+6124. The other six objects in our sample are extragalactic, and only one has coincident radio emission, which we conclude is most likely contamination from a background HII region. We conclude that with current facilities, neutron star ULXs do not produce significant enough radio emission to cause them to be misidentified as radio/X-ray selected intermediate mass black hole candidates. Thus, if background star formation has been properly considered, the current study indicates that a ULX with a compact radio counterpart is not likely to be a neutron star. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.23335v1-abstract-full').style.display = 'none'; document.getElementById('2410.23335v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">14 pages, 2 figures, accepted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.23324">arXiv:2410.23324</a> <span> [<a href="https://arxiv.org/pdf/2410.23324">pdf</a>, <a href="https://arxiv.org/format/2410.23324">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Combinatorics">math.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Discrete Mathematics">cs.DM</span> </div> </div> <p class="title is-5 mathjax"> Symmetric Domino Tilings of Aztec Diamonds </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Paul%2C+P">Pravakar Paul</a>, <a href="/search/?searchtype=author&query=Saikia%2C+M+P">Manjil P. Saikia</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="2410.23324v1-abstract-short" style="display: inline;"> In this paper, we give inductive sum formulas to calculate the number of diagonally symmetric, and diagonally \& anti-diagonally symmetric domino tilings of Aztec Diamonds. As a byproduct, we also find such a formula for the unrestricted case as well. Our proofs rely on a new technique for counting the number of perfect matchings of graphs, proposed by the authors recently. </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.23324v1-abstract-full" style="display: none;"> In this paper, we give inductive sum formulas to calculate the number of diagonally symmetric, and diagonally \& anti-diagonally symmetric domino tilings of Aztec Diamonds. As a byproduct, we also find such a formula for the unrestricted case as well. Our proofs rely on a new technique for counting the number of perfect matchings of graphs, proposed by the authors recently. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.23324v1-abstract-full').style.display = 'none'; document.getElementById('2410.23324v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">19 pages, 11 figures, 3 tables, comments are welcome</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> Primary 05C30; Secondary 05A15; 05C70; 52C20; 68R10 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.15852">arXiv:2410.15852</a> <span> [<a href="https://arxiv.org/pdf/2410.15852">pdf</a>, <a href="https://arxiv.org/ps/2410.15852">ps</a>, <a href="https://arxiv.org/format/2410.15852">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Combinatorics">math.CO</span> </div> </div> <p class="title is-5 mathjax"> Combinatorial Proofs of Some Results of Andrews and El Bachraoui </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Mahanta%2C+P+J">Pankaj Jyoti Mahanta</a>, <a href="/search/?searchtype=author&query=Saikia%2C+M+P">Manjil P. Saikia</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="2410.15852v1-abstract-short" style="display: inline;"> Recently, Andrews and El Bachraoui (2024) proved three very interesting $q$-series identities, from which three simple looking identities involving certain restricted partitions into distinct even parts and $4$-regular partitions follow. In this short note, we give combinatorial proofs of these identities. We also prove the counterpart identities for the restricted partitions into distinct odd par… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.15852v1-abstract-full').style.display = 'inline'; document.getElementById('2410.15852v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.15852v1-abstract-full" style="display: none;"> Recently, Andrews and El Bachraoui (2024) proved three very interesting $q$-series identities, from which three simple looking identities involving certain restricted partitions into distinct even parts and $4$-regular partitions follow. In this short note, we give combinatorial proofs of these identities. We also prove the counterpart identities for the restricted partitions into distinct odd parts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.15852v1-abstract-full').style.display = 'none'; document.getElementById('2410.15852v1-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">5 pages</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 05A17; 11P81 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.01034">arXiv:2410.01034</a> <span> [<a href="https://arxiv.org/pdf/2410.01034">pdf</a>, <a href="https://arxiv.org/format/2410.01034">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"> Finding radio transients with anomaly detection and active learning based on volunteer classifications </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Andersson%2C+A">Alex Andersson</a>, <a href="/search/?searchtype=author&query=Lintott%2C+C">Chris Lintott</a>, <a href="/search/?searchtype=author&query=Fender%2C+R">Rob Fender</a>, <a href="/search/?searchtype=author&query=Lochner%2C+M">Michelle Lochner</a>, <a href="/search/?searchtype=author&query=Woudt%2C+P">Patrick Woudt</a>, <a href="/search/?searchtype=author&query=Eijnden%2C+J+v+d">Jakob van den Eijnden</a>, <a href="/search/?searchtype=author&query=van+der+Horst%2C+A">Alexander van der Horst</a>, <a href="/search/?searchtype=author&query=Horesh%2C+A">Assaf Horesh</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">Payaswini Saikia</a>, <a href="/search/?searchtype=author&query=Sivakoff%2C+G+R">Gregory R. Sivakoff</a>, <a href="/search/?searchtype=author&query=Tremou%2C+L">Lilia Tremou</a>, <a href="/search/?searchtype=author&query=Vaccari%2C+M">Mattia Vaccari</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="2410.01034v1-abstract-short" style="display: inline;"> In this work we explore the applicability of unsupervised machine learning algorithms to the task of finding radio transients. Facilities such as the Square Kilometre Array (SKA) will provide huge volumes of data in which to detect rare transients; the challenge for astronomers is how to find them. We demonstrate the effectiveness of anomaly detection algorithms using 1.3 GHz light curves from the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.01034v1-abstract-full').style.display = 'inline'; document.getElementById('2410.01034v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.01034v1-abstract-full" style="display: none;"> In this work we explore the applicability of unsupervised machine learning algorithms to the task of finding radio transients. Facilities such as the Square Kilometre Array (SKA) will provide huge volumes of data in which to detect rare transients; the challenge for astronomers is how to find them. We demonstrate the effectiveness of anomaly detection algorithms using 1.3 GHz light curves from the SKA precursor MeerKAT. We make use of three sets of descriptive parameters ('feature sets') as applied to two anomaly detection techniques in the Astronomaly package and analyse our performance by comparison with citizen science labels on the same dataset. By using transients found by volunteers as our ground truth, we demonstrate that anomaly detection techniques can recall over half of the radio transients in the 10 per cent of the data with the highest anomaly scores. We find that the choice of anomaly detection algorithm makes a minimal (sub-one per cent) level difference, but that feature set choice is crucial, especially when considering available resources for human inspection and/or follow-up. Active learning, where human labels are given for just 2 per cent of the data, improves recall by up to 10 percentage points, depending on the feature-model pair. The best performing feature-model pairs result in a factor of 5 times fewer sources requiring vetting by experts. This is the first effort to apply anomaly detection techniques to finding radio transients and shows great promise for application to other datasets, and as a real-time transient detection system for upcoming large surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.01034v1-abstract-full').style.display = 'none'; document.getElementById('2410.01034v1-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">Submitted to MNRAS, comments welcome! 17 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/2409.02929">arXiv:2409.02929</a> <span> [<a href="https://arxiv.org/pdf/2409.02929">pdf</a>, <a href="https://arxiv.org/ps/2409.02929">ps</a>, <a href="https://arxiv.org/format/2409.02929">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Number Theory">math.NT</span> </div> </div> <p class="title is-5 mathjax"> Arithmetic Properties modulo powers of $2$ and $3$ for Overpartition $k$-Tuples with Odd Parts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Das%2C+H">Hirakjyoti Das</a>, <a href="/search/?searchtype=author&query=Saikia%2C+M+P">Manjil P. Saikia</a>, <a href="/search/?searchtype=author&query=Sarma%2C+A">Abhishek Sarma</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="2409.02929v1-abstract-short" style="display: inline;"> Recently, Drema and N. Saikia (2023) and M. P. Saikia, Sarma, and Sellers (2023) proved several congruences modulo powers of $2$ for overpartition triples with odd parts. In this paper, we study further divisibility properties of overpartition $k$-tuples with odd parts using elementary means as well as properties of modular forms. In particular, we prove several congruences modulo multiples of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.02929v1-abstract-full').style.display = 'inline'; document.getElementById('2409.02929v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.02929v1-abstract-full" style="display: none;"> Recently, Drema and N. Saikia (2023) and M. P. Saikia, Sarma, and Sellers (2023) proved several congruences modulo powers of $2$ for overpartition triples with odd parts. In this paper, we study further divisibility properties of overpartition $k$-tuples with odd parts using elementary means as well as properties of modular forms. In particular, we prove several congruences modulo multiples of $3$, and an infinite family of congruences modulo powers of $3$; we also prove some cases of a conjecture of Saikia, Sarma, and Sellers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.02929v1-abstract-full').style.display = 'none'; document.getElementById('2409.02929v1-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, 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">21 pages</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 11P81; 11P83 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.10273">arXiv:2408.10273</a> <span> [<a href="https://arxiv.org/pdf/2408.10273">pdf</a>, <a href="https://arxiv.org/format/2408.10273">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Combinatorics">math.CO</span> </div> </div> <p class="title is-5 mathjax"> A Novel Approach to Counting Perfect Matchings of Graphs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Paul%2C+P">Pravakar Paul</a>, <a href="/search/?searchtype=author&query=Saikia%2C+M+P">Manjil P. Saikia</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="2408.10273v1-abstract-short" style="display: inline;"> We build a new perspective to count perfect matchings of a given graph. This idea is motivated by a construction on the relative cohomology group of surfaces. As an application of our theory, we reprove the celebrated Aztec Diamond theorem, and show how alternating sign matrices naturally arises through this framework. </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.10273v1-abstract-full" style="display: none;"> We build a new perspective to count perfect matchings of a given graph. This idea is motivated by a construction on the relative cohomology group of surfaces. As an application of our theory, we reprove the celebrated Aztec Diamond theorem, and show how alternating sign matrices naturally arises through this framework. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.10273v1-abstract-full').style.display = 'none'; document.getElementById('2408.10273v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 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">22 pages, 16 figures, comments are welcome</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> Primary 05C30; Secondary 05A15; 05C70; 18A10; 52C20 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.06856">arXiv:2408.06856</a> <span> [<a href="https://arxiv.org/pdf/2408.06856">pdf</a>, <a href="https://arxiv.org/format/2408.06856">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> <p class="title is-5 mathjax"> X-ray and optical polarization aligned with the radio jet ejecta in GX 339-4 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Mastroserio%2C+G">G. Mastroserio</a>, <a href="/search/?searchtype=author&query=De+Marco%2C+B">B. De Marco</a>, <a href="/search/?searchtype=author&query=Baglio%2C+M+C">M. C. Baglio</a>, <a href="/search/?searchtype=author&query=Carotenuto%2C+F">F. Carotenuto</a>, <a href="/search/?searchtype=author&query=Fabiani%2C+S">S. Fabiani</a>, <a href="/search/?searchtype=author&query=Russell%2C+T+D">T. D. Russell</a>, <a href="/search/?searchtype=author&query=Capitanio%2C+F">F. Capitanio</a>, <a href="/search/?searchtype=author&query=Cavecchi%2C+Y">Y. Cavecchi</a>, <a href="/search/?searchtype=author&query=Motta%2C+S">S. Motta</a>, <a href="/search/?searchtype=author&query=Russell%2C+D+M">D. M. Russell</a>, <a href="/search/?searchtype=author&query=Dovciak%2C+M">M. Dovciak</a>, <a href="/search/?searchtype=author&query=Del+Santo%2C+M">M. Del Santo</a>, <a href="/search/?searchtype=author&query=Alabarta%2C+K">K. Alabarta</a>, <a href="/search/?searchtype=author&query=Ambrifi%2C+A">A. Ambrifi</a>, <a href="/search/?searchtype=author&query=Campana%2C+S">S. Campana</a>, <a href="/search/?searchtype=author&query=Casella%2C+P">P. Casella</a>, <a href="/search/?searchtype=author&query=Covino%2C+S">S. Covino</a>, <a href="/search/?searchtype=author&query=Illiano%2C+G">G. Illiano</a>, <a href="/search/?searchtype=author&query=Kara%2C+E">E. Kara</a>, <a href="/search/?searchtype=author&query=Lai%2C+E+V">E. V. Lai</a>, <a href="/search/?searchtype=author&query=Lodato%2C+G">G. Lodato</a>, <a href="/search/?searchtype=author&query=Manca%2C+A">A. Manca</a>, <a href="/search/?searchtype=author&query=Mariani%2C+I">I. Mariani</a>, <a href="/search/?searchtype=author&query=Marino%2C+A">A. Marino</a>, <a href="/search/?searchtype=author&query=Miceli%2C+C">C. Miceli</a> , et al. (5 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="2408.06856v1-abstract-short" style="display: inline;"> We present the first X-ray polarization measurements of GX 339-4. IXPE observed this source twice during its 2023-2024 outburst, once in the soft-intermediate state and again during a soft state. The observation taken during the intermediate state shows significant ($4蟽$) polarization degree P = $1.3\% \pm 0.3\%$ and polarization angle $胃$ = -74\degree $\pm$ 7\degree only in the 3 - 8 keV band. FO… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.06856v1-abstract-full').style.display = 'inline'; document.getElementById('2408.06856v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.06856v1-abstract-full" style="display: none;"> We present the first X-ray polarization measurements of GX 339-4. IXPE observed this source twice during its 2023-2024 outburst, once in the soft-intermediate state and again during a soft state. The observation taken during the intermediate state shows significant ($4蟽$) polarization degree P = $1.3\% \pm 0.3\%$ and polarization angle $胃$ = -74\degree $\pm$ 7\degree only in the 3 - 8 keV band. FORS2 at VLT observed the source simultaneously detecting optical polarization in the B, V, R, I bands (between $0.1%$ and $0.7\%$), all roughly aligned with the X-ray polarization. We also detect a discrete jet knot from radio observations taken later in time; this knot would have been ejected from the system around the same time as the hard-to-soft X-ray state transition and a bright radio flare occurred $\sim$3 months earlier. The proper motion of the jet knot provides a direct measurement of the jet orientation angle on the plane of the sky at the time of the ejection. We find that both the X-ray and optical polarization angles are aligned with the direction of the ballistic jet. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.06856v1-abstract-full').style.display = 'none'; document.getElementById('2408.06856v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 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">Submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.21509">arXiv:2407.21509</a> <span> [<a href="https://arxiv.org/pdf/2407.21509">pdf</a>, <a href="https://arxiv.org/format/2407.21509">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> <p class="title is-5 mathjax"> Radio observations of the 2022 outburst of the transitional Z-Atoll source XTE J1701-462 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Gasealahwe%2C+K+V+S">K. V. S. Gasealahwe</a>, <a href="/search/?searchtype=author&query=Monageng%2C+I+M">I. M. Monageng</a>, <a href="/search/?searchtype=author&query=Fender%2C+R+P">R. P. Fender</a>, <a href="/search/?searchtype=author&query=Woudt%2C+P+A">P. A. Woudt</a>, <a href="/search/?searchtype=author&query=Hughes%2C+A+K">A. K. Hughes</a>, <a href="/search/?searchtype=author&query=Motta%2C+S+E">S. E. Motta</a>, <a href="/search/?searchtype=author&query=Eijnden%2C+J+v+d">J. van den Eijnden</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">P. Saikia</a>, <a href="/search/?searchtype=author&query=Tremou%2C+E">E. Tremou</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="2407.21509v1-abstract-short" style="display: inline;"> XTE J1701-462 is a neutron star low mass X-ray binary (NS LMXB) discovered in 2006 as the first system to demonstrate unambiguously that the `Atoll' and `Z' classes of accreting neutron stars are separated by accretion rate. Radio observations during the 2006/7 outburst provided evidence for the formation of a relativistic jet, as now expected for all accreting neutron star and black hole X-ray bi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.21509v1-abstract-full').style.display = 'inline'; document.getElementById('2407.21509v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.21509v1-abstract-full" style="display: none;"> XTE J1701-462 is a neutron star low mass X-ray binary (NS LMXB) discovered in 2006 as the first system to demonstrate unambiguously that the `Atoll' and `Z' classes of accreting neutron stars are separated by accretion rate. Radio observations during the 2006/7 outburst provided evidence for the formation of a relativistic jet, as now expected for all accreting neutron star and black hole X-ray binaries at high accretion rates. The source entered a new outburst in 2022, and we report 29 observations made with the MeerKAT radio telescope. The first radio detection was on the 16th September 2022, we continued detecting the source until mid-December 2022. Thereafter, establishing radio upper limits till 25 March 2023. We present the radio analysis alongside analysis of contemporaneous X-ray observations from MAXI. The radio light curve shows evidence for at least three flare-like events over the first hundred days, the most luminous of which has an associated minimum energy of $1\times10^{38}$ erg. We provide a detailed comparison with the 2006/7 outburst, and demonstrate that we detected radio emission from the source for considerably longer in the more recent outburst, although this is probably a function of sampling. We further constrain the radio emission from the source to have a polarisation of less than 9% at the time of 2022 IXPE detection of X-ray polarisation. Finally, we place the source in the radio -- X-ray plane, demonstrating that when detected in radio it sits in a comparable region of parameter space to the other Z-sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.21509v1-abstract-full').style.display = 'none'; document.getElementById('2407.21509v1-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">8 pages, 4 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/2407.10850">arXiv:2407.10850</a> <span> [<a href="https://arxiv.org/pdf/2407.10850">pdf</a>, <a href="https://arxiv.org/ps/2407.10850">ps</a>, <a href="https://arxiv.org/format/2407.10850">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> <p class="title is-5 mathjax"> LeMMINGs. Multi-wavelength constraints on the co-existence of nuclear star clusters and AGN in nucleated galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Dullo%2C+B+T">B. T. Dullo</a>, <a href="/search/?searchtype=author&query=Knapen%2C+J+H">J. H. Knapen</a>, <a href="/search/?searchtype=author&query=Baldi%2C+R+D">R. D. Baldi</a>, <a href="/search/?searchtype=author&query=Williams%2C+D+R+A">D. R. A. Williams</a>, <a href="/search/?searchtype=author&query=Beswick%2C+R+J">R. J. Beswick</a>, <a href="/search/?searchtype=author&query=McHardy%2C+I+M">I. M. McHardy</a>, <a href="/search/?searchtype=author&query=Green%2C+D+A">D. A. Green</a>, <a href="/search/?searchtype=author&query=de+Paz%2C+A+G">A. Gil de Paz</a>, <a href="/search/?searchtype=author&query=Aalto%2C+S">S. Aalto</a>, <a href="/search/?searchtype=author&query=Alberdi%2C+A">A. Alberdi</a>, <a href="/search/?searchtype=author&query=Argo%2C+M+K">M. K. Argo</a>, <a href="/search/?searchtype=author&query=Gallagher%2C+J+S">J. S. Gallagher</a>, <a href="/search/?searchtype=author&query=Kl%C3%B6ckner%2C+H+-">H. -R. Kl枚ckner</a>, <a href="/search/?searchtype=author&query=Marcaide%2C+J+M">J. M. Marcaide</a>, <a href="/search/?searchtype=author&query=Mutie%2C+I+M">I. M. Mutie</a>, <a href="/search/?searchtype=author&query=Saikia%2C+D+J">D. J. Saikia</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">P. Saikia</a>, <a href="/search/?searchtype=author&query=Stevens%2C+I+R">I. R. Stevens</a>, <a href="/search/?searchtype=author&query=Torrej%C3%B3n%2C+S">S. Torrej贸n</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="2407.10850v1-abstract-short" style="display: inline;"> [Abridged] The relation between nuclear star clusters (NSCs) and the growth of the central SMBHs, as well as their connection to the properties of the host galaxies, is crucial for understanding the evolution of galaxies. Recent observations have revealed that about 10 per cent of nucleated galaxies host hybrid nuclei, consisting of both NSCs and accreting SMBHs that power active galactic nuclei (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.10850v1-abstract-full').style.display = 'inline'; document.getElementById('2407.10850v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.10850v1-abstract-full" style="display: none;"> [Abridged] The relation between nuclear star clusters (NSCs) and the growth of the central SMBHs, as well as their connection to the properties of the host galaxies, is crucial for understanding the evolution of galaxies. Recent observations have revealed that about 10 per cent of nucleated galaxies host hybrid nuclei, consisting of both NSCs and accreting SMBHs that power active galactic nuclei (AGN). Motivated by the potential of the recently published multi-wavelength data sets from LeMMINGs survey, here we present the most thorough investigation to date of the incidence of hybrid nuclei in a large sample of 100 nearby nucleated galaxies (10 E, 25 S0, 63 S, and 2 Irr), covering a wide range in stellar mass ($M_{*,\rm gal} \sim 10^{8.7}-10^{12}~\rm M_{sun}$). We identify the nuclei and derive their properties by performing detailed 1D and 2D multi-component decompositions of the optical and near-infrared $HST$ stellar light distributions of the galaxies using S茅rsic and core-S茅rsic models. Our AGN diagnostics are based on homogeneously derived nuclear 1.5 GHz $e$-MERLIN radio, $Chandra$ X-ray (0.3--10 keV) and optical emission-line data. We determine the nucleation fraction ($f_{\rm nuc} $) as the relative incidence of nuclei across the LeMMINGs $HST$ sample and find $f_{\rm nuc} =~ $100/149 (= 67 $\pm$ 7 per cent), confirming previous work, with a peak value of 49/56~(= $88 \pm 13$ per cent) at bulge masses $M_{*,\rm bulge} \sim 10^{9.4}$- $10^{10.8}~\rm M_{sun}$. We identify 30 nucleated LeMMINGs galaxies that are optically active, radio-detected and X-ray luminous ($L_{X} > 10^{39}$ erg s$^{-1}$). This indicates that our nucleated sample has a lower limit $\sim$ 30 per cent occupancy of hybrid nuclei, which is a function of $M_{*,\rm bulge}$ and $M_{*,\rm gal}$. We find that hybrid nuclei have a number density of $(1.5 \pm 0.4) \times 10^{-5}$ Mpc$^{-3}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.10850v1-abstract-full').style.display = 'none'; document.getElementById('2407.10850v1-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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 MNRAS (21 pages, 10 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/2407.00380">arXiv:2407.00380</a> <span> [<a href="https://arxiv.org/pdf/2407.00380">pdf</a>, <a href="https://arxiv.org/format/2407.00380">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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Particle acceleration at the bow shock of runaway star LS 2355: non-thermal radio emission but no $纬$-ray counterpart </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Eijnden%2C+J+v+d">J. van den Eijnden</a>, <a href="/search/?searchtype=author&query=Mohamed%2C+S">S. Mohamed</a>, <a href="/search/?searchtype=author&query=Carotenuto%2C+F">F. Carotenuto</a>, <a href="/search/?searchtype=author&query=Motta%2C+S">S. Motta</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">P. Saikia</a>, <a href="/search/?searchtype=author&query=Williams-Baldwin%2C+D+R+A">D. R. A. Williams-Baldwin</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="2407.00380v1-abstract-short" style="display: inline;"> Massive stars that travel at supersonic speeds can create bow shocks as their stellar winds interact with the surrounding interstellar medium. These bow shocks - prominent sites for mechanical feedback of individual massive stars - are predominantly observed in the infrared band. Confirmed high-energy emission from stellar bow shocks has remained elusive and confirmed radio counterparts, while ris… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.00380v1-abstract-full').style.display = 'inline'; document.getElementById('2407.00380v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.00380v1-abstract-full" style="display: none;"> Massive stars that travel at supersonic speeds can create bow shocks as their stellar winds interact with the surrounding interstellar medium. These bow shocks - prominent sites for mechanical feedback of individual massive stars - are predominantly observed in the infrared band. Confirmed high-energy emission from stellar bow shocks has remained elusive and confirmed radio counterparts, while rising in recent years, remain rare. Here, we present an in-depth multi-wavelength exploration of the bow shock driven by LS 2355, focusing on its non-thermal properties. Using the most-recent Fermi source catalogue, we rule out its previously-proposed association with an unidentified $纬$-ray source. Furthermore, we use deep ASKAP observations from the Rapid ASKAP Continuum Survey and the Evolutionary Map of the Universe survey to identify a non-thermal radio counterpart: the third spectrally confirmed non-thermal bow shock counterpart after BD +43$^{\rm o}$ 3654 and BD +60$^{\rm o}$ 2522. We finally use WISE IR data and Gaia to study the surrounding ISM and update the motion of LS 2355. Specifically, we derive a substantially reduced stellar velocity, $v_* = 7.0\pm2.5$ km/s, compared to previous estimates. The observed non-thermal properties of the bow shock can be explained by an interaction between the wind of LS 2355 and a dense HII region, at a magnetic field close to the maximum magnetic field strength allowed by the compressibility of the ISM. Similar to earlier works, we find that the thermal radio emission of the shocked ISM is likely to be substantially suppressed for it to be consistent with the observed radio spectrum. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.00380v1-abstract-full').style.display = 'none'; document.getElementById('2407.00380v1-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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 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/2402.08237">arXiv:2402.08237</a> <span> [<a href="https://arxiv.org/pdf/2402.08237">pdf</a>, <a href="https://arxiv.org/format/2402.08237">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad24ef">10.3847/1538-4357/ad24ef <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A multi-wavelength study of the hard and soft states of MAXI J1820+070 during its 2018 outburst </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Banerjee%2C+S">Srimanta Banerjee</a>, <a href="/search/?searchtype=author&query=Dewangan%2C+G+C">Gulab C. Dewangan</a>, <a href="/search/?searchtype=author&query=Knigge%2C+C">Christian Knigge</a>, <a href="/search/?searchtype=author&query=Georganti%2C+M">Maria Georganti</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">Poshak Gandhi</a>, <a href="/search/?searchtype=author&query=Mithun%2C+N+P+S">N. P. S. Mithun</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">Payaswini Saikia</a>, <a href="/search/?searchtype=author&query=Bhattacharya%2C+D">Dipankar Bhattacharya</a>, <a href="/search/?searchtype=author&query=Russell%2C+D+M">David M. Russell</a>, <a href="/search/?searchtype=author&query=Lewis%2C+F">Fraser Lewis</a>, <a href="/search/?searchtype=author&query=Zdziarski%2C+A+A">Andrzej A. Zdziarski</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="2402.08237v1-abstract-short" style="display: inline;"> We present a comprehensive multi-wavelength spectral analysis of the black hole X-ray binary MAXI J1820+070 during its 2018 outburst, utilizing AstroSat far UV, soft and hard X-ray data, along with (quasi-)simultaneous optical and X-ray data from Las Cumbres Observatory and NICER, respectively. In the soft state, we detect soft X-ray and UV/optical excess components over and above the intrinsic ac… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08237v1-abstract-full').style.display = 'inline'; document.getElementById('2402.08237v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.08237v1-abstract-full" style="display: none;"> We present a comprehensive multi-wavelength spectral analysis of the black hole X-ray binary MAXI J1820+070 during its 2018 outburst, utilizing AstroSat far UV, soft and hard X-ray data, along with (quasi-)simultaneous optical and X-ray data from Las Cumbres Observatory and NICER, respectively. In the soft state, we detect soft X-ray and UV/optical excess components over and above the intrinsic accretion disk emission ($kT_{\rm in}\sim 0.58$ keV) and a steep X-ray power-law component. The soft X-ray excess is consistent with a high-temperature blackbody ($kT\sim 0.79$ keV), while the UV/optical excess is described by UV emission lines and two low-temperature blackbody components ($kT\sim 3.87$ eV and $\sim 0.75$ eV). Employing continuum spectral fitting, we determine the black hole spin parameter ($a=0.77\pm0.21$), using the jet inclination angle of $64^{\circ}\pm5^{\circ}$ and a mass spanning $5-10M_{\odot}$. In the hard state, we observe a significantly enhanced optical/UV excess component, indicating a stronger reprocessed emission in the outer disk. Broad-band X-ray spectroscopy in the hard state reveals a two-component corona, each associated with its reflection component, in addition to the disk emission ($kT_{\rm in}\sim 0.19$ keV). The softer coronal component dominates the bolometric X-ray luminosity and produces broader relativistic reflection features, while the harder component gets reflected far from the inner disk, yielding narrow reflection features. Furthermore, our analysis in the hard state suggests a substantial truncation of the inner disk ($\gtrsim 51$ gravitational radii) and a high disk density ($\sim 10^{20}\ \rm cm^{-3}$). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08237v1-abstract-full').style.display = 'none'; document.getElementById('2402.08237v1-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 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">29 pages, 19 figures, 8 Tables, Accepted for publication 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, 964, 189 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.12011">arXiv:2312.12011</a> <span> [<a href="https://arxiv.org/pdf/2312.12011">pdf</a>, <a href="https://arxiv.org/ps/2312.12011">ps</a>, <a href="https://arxiv.org/format/2312.12011">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Number Theory">math.NT</span> </div> </div> <p class="title is-5 mathjax"> Arithmetic properties modulo powers of $2$ for overpartition $k$-tuples with odd parts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Saikia%2C+M+P">Manjil P. Saikia</a>, <a href="/search/?searchtype=author&query=Sarma%2C+A">Abhishek Sarma</a>, <a href="/search/?searchtype=author&query=Sellers%2C+J+A">James A. Sellers</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="2312.12011v2-abstract-short" style="display: inline;"> Recently, Drema and Saikia (2023) proved several congruences modulo powers of 2 and 3 for overpartition triples with odd parts. We extend their list substantially. We prove several congruences modulo powers of 2 for overpartition k-tuples with odd parts, along with a few infinite families of congruences for overpartition triples with odd parts and for overpartition k-tuples with odd parts (for k =… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.12011v2-abstract-full').style.display = 'inline'; document.getElementById('2312.12011v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.12011v2-abstract-full" style="display: none;"> Recently, Drema and Saikia (2023) proved several congruences modulo powers of 2 and 3 for overpartition triples with odd parts. We extend their list substantially. We prove several congruences modulo powers of 2 for overpartition k-tuples with odd parts, along with a few infinite families of congruences for overpartition triples with odd parts and for overpartition k-tuples with odd parts (for k = 4 and for odd k). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.12011v2-abstract-full').style.display = 'none'; document.getElementById('2312.12011v2-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 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">25 pages, final version, typos and minor errors fixed after referee report, Theorem 2.3 strengthened, to appear in the Journal of the Ramanujan Mathematical Society</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 11P81; 11P83 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.11523">arXiv:2311.11523</a> <span> [<a href="https://arxiv.org/pdf/2311.11523">pdf</a>, <a href="https://arxiv.org/format/2311.11523">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad1a10">10.3847/1538-4357/ad1a10 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Chasing the break: Tracing the full evolution of a black hole X-ray binary jet with multi-wavelength spectral modeling </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Echibur%C3%BA-Trujillo%2C+C">Constanza Echibur煤-Trujillo</a>, <a href="/search/?searchtype=author&query=Tetarenko%2C+A+J">Alexandra J. Tetarenko</a>, <a href="/search/?searchtype=author&query=Haggard%2C+D">Daryl Haggard</a>, <a href="/search/?searchtype=author&query=Russell%2C+T+D">Thomas D. Russell</a>, <a href="/search/?searchtype=author&query=Koljonen%2C+K+I+I">Karri I. I. Koljonen</a>, <a href="/search/?searchtype=author&query=Bahramian%2C+A">Arash Bahramian</a>, <a href="/search/?searchtype=author&query=Wang%2C+J">Jingyi Wang</a>, <a href="/search/?searchtype=author&query=Bremer%2C+M">Michael Bremer</a>, <a href="/search/?searchtype=author&query=Bright%2C+J">Joe Bright</a>, <a href="/search/?searchtype=author&query=Casella%2C+P">Piergiorgio Casella</a>, <a href="/search/?searchtype=author&query=Russell%2C+D+M">David M. Russell</a>, <a href="/search/?searchtype=author&query=Altamirano%2C+D">Diego Altamirano</a>, <a href="/search/?searchtype=author&query=Baglio%2C+M+C">M. Cristina Baglio</a>, <a href="/search/?searchtype=author&query=Belloni%2C+T">Tomaso Belloni</a>, <a href="/search/?searchtype=author&query=Ceccobello%2C+C">Chiara Ceccobello</a>, <a href="/search/?searchtype=author&query=Corbel%2C+S">Stephane Corbel</a>, <a href="/search/?searchtype=author&query=Trigo%2C+M+D">Maria Diaz Trigo</a>, <a href="/search/?searchtype=author&query=Maitra%2C+D">Dipankar Maitra</a>, <a href="/search/?searchtype=author&query=Gabuya%2C+A">Aldrin Gabuya</a>, <a href="/search/?searchtype=author&query=Gallo%2C+E">Elena Gallo</a>, <a href="/search/?searchtype=author&query=Heinz%2C+S">Sebastian Heinz</a>, <a href="/search/?searchtype=author&query=Homan%2C+J">Jeroen Homan</a>, <a href="/search/?searchtype=author&query=Kara%2C+E">Erin Kara</a>, <a href="/search/?searchtype=author&query=K%C3%B6rding%2C+E">Elmar K枚rding</a>, <a href="/search/?searchtype=author&query=Lewis%2C+F">Fraser Lewis</a> , et al. (13 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="2311.11523v2-abstract-short" style="display: inline;"> Black hole X-ray binaries (BH XRBs) are ideal targets to study the connection between accretion inflow and jet outflow. Here we present quasi-simultaneous, multi-wavelength observations of the Galactic black hole system MAXI J1820+070, throughout its 2018-2019 outburst. Our data set includes coverage from the radio through X-ray bands from 17 different instruments/telescopes, and encompasses 19 ep… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.11523v2-abstract-full').style.display = 'inline'; document.getElementById('2311.11523v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.11523v2-abstract-full" style="display: none;"> Black hole X-ray binaries (BH XRBs) are ideal targets to study the connection between accretion inflow and jet outflow. Here we present quasi-simultaneous, multi-wavelength observations of the Galactic black hole system MAXI J1820+070, throughout its 2018-2019 outburst. Our data set includes coverage from the radio through X-ray bands from 17 different instruments/telescopes, and encompasses 19 epochs over a 7 month time period, resulting in one of the most well-sampled multi-wavelength data sets of a BH XRB outburst to date. With our data, we compile and model the broad-band spectra of this source using a phenomenological model that includes emission from the jet, companion star, and accretion flow. This modeling allows us to track the evolution of the spectral break in the jet spectrum, a key observable that samples the jet launching region. We find that the spectral break location changes over at least $\approx3$ orders of magnitude in electromagnetic frequency over this period. Using these spectral break measurements, we link the full cycle of jet behavior, including the rising, quenching, and re-ignition, to the changing accretion flow properties as the source evolves through its different accretion states. Our analyses show a consistent jet behavior with other sources in similar phases of their outbursts, reinforcing that the jet quenching and recovery may be a global feature of BH XRB systems in outburst. Our results also provide valuable evidence supporting a close connection between the geometry of the inner accretion flow and the base of the jet. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.11523v2-abstract-full').style.display = 'none'; document.getElementById('2311.11523v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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 ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2024 ApJ 962 116 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.03460">arXiv:2311.03460</a> <span> [<a href="https://arxiv.org/pdf/2311.03460">pdf</a>, <a href="https://arxiv.org/format/2311.03460">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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The omnipresent flux-dependent optical dips of the black hole transient Swift J1357.2-0933 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Panizo-Espinar%2C+G">G. Panizo-Espinar</a>, <a href="/search/?searchtype=author&query=Mu%C3%B1oz-Darias%2C+T">T. Mu帽oz-Darias</a>, <a href="/search/?searchtype=author&query=Padilla%2C+M+A">M. Armas Padilla</a>, <a href="/search/?searchtype=author&query=Jim%C3%A9nez-Ibarra%2C+F">F. Jim茅nez-Ibarra</a>, <a href="/search/?searchtype=author&query=S%C3%A1nchez%2C+D+M">D. Mata S谩nchez</a>, <a href="/search/?searchtype=author&query=Yanes-Rizo%2C+I+V">I. V. Yanes-Rizo</a>, <a href="/search/?searchtype=author&query=Alabarta%2C+K">K. Alabarta</a>, <a href="/search/?searchtype=author&query=Baglio%2C+M+C">M. C. Baglio</a>, <a href="/search/?searchtype=author&query=Caruso%2C+E">E. Caruso</a>, <a href="/search/?searchtype=author&query=Casares%2C+J">J. Casares</a>, <a href="/search/?searchtype=author&query=Corral-Santana%2C+J+M">J. M. Corral-Santana</a>, <a href="/search/?searchtype=author&query=Lewis%2C+F">F. Lewis</a>, <a href="/search/?searchtype=author&query=Russell%2C+D+M">D. M. Russell</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">P. Saikia</a>, <a href="/search/?searchtype=author&query=S%C3%A1nchez-Sierras%2C+J">J. S谩nchez-Sierras</a>, <a href="/search/?searchtype=author&query=Shahbaz%2C+T">T. Shahbaz</a>, <a href="/search/?searchtype=author&query=Torres%2C+M+A+P">M. A. P. Torres</a>, <a href="/search/?searchtype=author&query=Vincentelli%2C+F">F. Vincentelli</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="2311.03460v1-abstract-short" style="display: inline;"> Swift J1357.2-0933 is a black hole transient of particular interest due to the optical, recurrent dips found during its first two outbursts (in 2011 and 2017), with no obvious X-ray equivalent. We present fast optical photometry during its two most recent outbursts, in 2019 and 2021. Our observations reveal that the optical dips were present in every observed outburst of the source, although they… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.03460v1-abstract-full').style.display = 'inline'; document.getElementById('2311.03460v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.03460v1-abstract-full" style="display: none;"> Swift J1357.2-0933 is a black hole transient of particular interest due to the optical, recurrent dips found during its first two outbursts (in 2011 and 2017), with no obvious X-ray equivalent. We present fast optical photometry during its two most recent outbursts, in 2019 and 2021. Our observations reveal that the optical dips were present in every observed outburst of the source, although they were shallower and showed longer recurrence periods in the two most recent and fainter events. We perform a global study of the dips properties in the four outbursts, and find that they do not follow a common temporal evolution. In addition, we discover a correlation with the X-ray and optical fluxes, with dips being more profound and showing shorter recurrence periods for brighter stages. This trend seems to extend even to the faintest, quiescent states of the source. Finally, we discuss these results in the context of the possible connection between optical dips and outflows found in previous works. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.03460v1-abstract-full').style.display = 'none'; document.getElementById('2311.03460v1-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 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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 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/2307.13263">arXiv:2307.13263</a> <span> [<a href="https://arxiv.org/pdf/2307.13263">pdf</a>, <a href="https://arxiv.org/format/2307.13263">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"> Evidence for low power radio jet-ISM interaction at 10 parsec in the dwarf AGN host NGC 4395 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Nandi%2C+P">Payel Nandi</a>, <a href="/search/?searchtype=author&query=Stalin%2C+C+S">C. S. Stalin</a>, <a href="/search/?searchtype=author&query=Saikia%2C+D+J">D. J. Saikia</a>, <a href="/search/?searchtype=author&query=Riffel%2C+R+A">Rogemar A. Riffel</a>, <a href="/search/?searchtype=author&query=Manna%2C+A">Arijit Manna</a>, <a href="/search/?searchtype=author&query=Pal%2C+S">Sabyasachi Pal</a>, <a href="/search/?searchtype=author&query=Dors%2C+O+L">O. L. Dors</a>, <a href="/search/?searchtype=author&query=Wylezalek%2C+D">Dominika Wylezalek</a>, <a href="/search/?searchtype=author&query=Paliya%2C+V+S">Vaidehi S. Paliya</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">P. Saikia</a>, <a href="/search/?searchtype=author&query=Dabhade%2C+P">Pratik Dabhade</a>, <a href="/search/?searchtype=author&query=Patig%2C+M">Markus-Kissler Patig</a>, <a href="/search/?searchtype=author&query=Sagar%2C+R">Ram Sagar</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="2307.13263v3-abstract-short" style="display: inline;"> Black hole driven outflows in galaxies hosting active galactic nuclei (AGN) may interact with their interstellar medium (ISM) affecting star formation. Such feedback processes, reminiscent of those seen in massive galaxies, have been reported recently in some dwarf galaxies. However, such studies have usually been on kiloparsec and larger scales and our knowledge on the smallest spatial scales to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.13263v3-abstract-full').style.display = 'inline'; document.getElementById('2307.13263v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.13263v3-abstract-full" style="display: none;"> Black hole driven outflows in galaxies hosting active galactic nuclei (AGN) may interact with their interstellar medium (ISM) affecting star formation. Such feedback processes, reminiscent of those seen in massive galaxies, have been reported recently in some dwarf galaxies. However, such studies have usually been on kiloparsec and larger scales and our knowledge on the smallest spatial scales to which these feedback processes can operate is unclear. Here we demonstrate radio jet$-$ISM interaction on the scale of an asymmetric triple radio structure of $\sim$ 10 parsec size in NGC 4395. This triple radio structure is seen in the 15 GHz continuum image and the two asymmetric jet-like structures are situated on either side of the radio core that coincides with the optical {\it Gaia} position. The high resolution radio image and the extended [OIII]$位$5007 emission, indicative of an outflow, are spatially coincident and are consistent with the interpretation of a low power radio jet interacting with the ISM. Modelling of the spectral lines using {\tt MAPPINGS}, and estimation of temperature using optical integral field spectroscopic data suggest shock ionization of the gas. The continuum emission at 237 GHz, though weak, was found to spatially coincide with the AGN. However, the CO(2$-$1) line emission was found to be displaced by around 20 parsec northward of the AGN core. The spatial coincidence of molecular H$_2$$位$2.4085 along the jet direction, the morphology of ionised [OIII]$位$5007 and displacement of the CO(2$-$1) emission argues for conditions less favourable for star formation in the central $\sim$ 10 parsec region. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.13263v3-abstract-full').style.display = 'none'; document.getElementById('2307.13263v3-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 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">20 pages, 18 figures, accepted for the publication of 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/2307.08407">arXiv:2307.08407</a> <span> [<a href="https://arxiv.org/pdf/2307.08407">pdf</a>, <a href="https://arxiv.org/format/2307.08407">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/stad2044">10.1093/mnras/stad2044 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Clockwise evolution in the hardness-intensity diagram of the black hole X-ray binary Swift J1910.2-0546 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Saikia%2C+P">Payaswini Saikia</a>, <a href="/search/?searchtype=author&query=Russell%2C+D+M">David M. Russell</a>, <a href="/search/?searchtype=author&query=Pirbhoy%2C+S+F">Saarah F. Pirbhoy</a>, <a href="/search/?searchtype=author&query=Baglio%2C+M+C">M. C. Baglio</a>, <a href="/search/?searchtype=author&query=Bramich%2C+M">M. Bramich</a>, <a href="/search/?searchtype=author&query=Alabarta%2C+K">Kevin Alabarta</a>, <a href="/search/?searchtype=author&query=Lewis%2C+F">Fraser Lewis</a>, <a href="/search/?searchtype=author&query=Charles%2C+P">Phil Charles</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="2307.08407v1-abstract-short" style="display: inline;"> We present a detailed study of optical data from the 2012 outburst of the candidate black hole X-ray binary Swift J1910.2-0546 using the Faulkes Telescope and Las Cumbres Observatory (LCO). We analyse the peculiar spectral state changes of Swift J1910.2-0546 in different energy bands, and characterise how the optical and UV emission correlates with the unusual spectral state evolution. Using vario… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.08407v1-abstract-full').style.display = 'inline'; document.getElementById('2307.08407v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.08407v1-abstract-full" style="display: none;"> We present a detailed study of optical data from the 2012 outburst of the candidate black hole X-ray binary Swift J1910.2-0546 using the Faulkes Telescope and Las Cumbres Observatory (LCO). We analyse the peculiar spectral state changes of Swift J1910.2-0546 in different energy bands, and characterise how the optical and UV emission correlates with the unusual spectral state evolution. Using various diagnostic tools like the optical/X-ray correlation and spectral energy distributions, we disentangle the different emission processes contributing towards the optical flux of the system. When Swift J1910.2-0546 transitions to the pure hard state, we find significant optical brightening of the source along with a dramatic change in the optical colour due to the onset of a jet during the spectral state transition. For the rest of the spectral states, the optical/UV emission is mostly dominated by an X-ray irradiated disk. From our high cadence optical study, we have discovered a putative modulation. Assuming that this modulation arises from a superhump, we suggest Swift J1910.2-0546 to have an orbital period of 2.25-2.47 hr, which would make it the shortest orbital period black hole X-ray binary known to date. Finally, from the state transition luminosity of the source, we find that the distance to the source is likely to be ~4.5-20.8 kpc, which is also supported by the comparative position of the source in the global optical/X-ray correlation of a large sample of black hole and neutron star X-ray binaries. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.08407v1-abstract-full').style.display = 'none'; document.getElementById('2307.08407v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">Published at MNRAS, 12 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/2305.14509">arXiv:2305.14509</a> <span> [<a href="https://arxiv.org/pdf/2305.14509">pdf</a>, <a href="https://arxiv.org/format/2305.14509">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202346418">10.1051/0004-6361/202346418 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Matter ejections behind the highs and lows of the transitional millisecond pulsar PSR J1023+0038 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Baglio%2C+M+C">M. C. Baglio</a>, <a href="/search/?searchtype=author&query=Zelati%2C+F+C">F. Coti Zelati</a>, <a href="/search/?searchtype=author&query=Campana%2C+S">S. Campana</a>, <a href="/search/?searchtype=author&query=Busquet%2C+G">G. Busquet</a>, <a href="/search/?searchtype=author&query=D%27Avanzo%2C+P">P. D'Avanzo</a>, <a href="/search/?searchtype=author&query=Giarratana%2C+S">S. Giarratana</a>, <a href="/search/?searchtype=author&query=Giroletti%2C+M">M. Giroletti</a>, <a href="/search/?searchtype=author&query=Ambrosino%2C+F">F. Ambrosino</a>, <a href="/search/?searchtype=author&query=Crespi%2C+S">S. Crespi</a>, <a href="/search/?searchtype=author&query=Zanon%2C+A+M">A. Miraval Zanon</a>, <a href="/search/?searchtype=author&query=Hou%2C+X">X. Hou</a>, <a href="/search/?searchtype=author&query=Li%2C+D">D. Li</a>, <a href="/search/?searchtype=author&query=Li%2C+J">J. Li</a>, <a href="/search/?searchtype=author&query=Wang%2C+P">P. Wang</a>, <a href="/search/?searchtype=author&query=Russell%2C+D+M">D. M. Russell</a>, <a href="/search/?searchtype=author&query=Torres%2C+D+F">D. F. Torres</a>, <a href="/search/?searchtype=author&query=Alabarta%2C+K">K. Alabarta</a>, <a href="/search/?searchtype=author&query=Casella%2C+P">P. Casella</a>, <a href="/search/?searchtype=author&query=Covino%2C+S">S. Covino</a>, <a href="/search/?searchtype=author&query=Bramich%2C+D+M">D. M. Bramich</a>, <a href="/search/?searchtype=author&query=de+Martino%2C+D">D. de Martino</a>, <a href="/search/?searchtype=author&query=M%C3%A9ndez%2C+M">M. M茅ndez</a>, <a href="/search/?searchtype=author&query=Motta%2C+S+E">S. E. Motta</a>, <a href="/search/?searchtype=author&query=Papitto%2C+A">A. Papitto</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">P. Saikia</a> , et al. (1 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="2305.14509v2-abstract-short" style="display: inline;"> Transitional millisecond pulsars are an emerging class of sources that link low-mass X-ray binaries to millisecond radio pulsars in binary systems. These pulsars alternate between a radio pulsar state and an active low-luminosity X-ray disc state. During the active state, these sources exhibit two distinct emission modes (high and low) that alternate unpredictably, abruptly, and incessantly. X-ray… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.14509v2-abstract-full').style.display = 'inline'; document.getElementById('2305.14509v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.14509v2-abstract-full" style="display: none;"> Transitional millisecond pulsars are an emerging class of sources that link low-mass X-ray binaries to millisecond radio pulsars in binary systems. These pulsars alternate between a radio pulsar state and an active low-luminosity X-ray disc state. During the active state, these sources exhibit two distinct emission modes (high and low) that alternate unpredictably, abruptly, and incessantly. X-ray to optical pulsations are observed only during the high mode. The root cause of this puzzling behaviour remains elusive. This paper presents the results of the most extensive multi-wavelength campaign ever conducted on the transitional pulsar prototype, PSR J1023+0038, covering from the radio to X-rays. The campaign was carried out over two nights in June 2021 and involved 12 different telescopes and instruments, including XMM-Newton, HST, VLT/FORS2 (in polarimetric mode), ALMA, VLA, and FAST. By modelling the broadband spectral energy distributions in both emission modes, we show that the mode switches are caused by changes in the innermost region of the accretion disc. These changes trigger the emission of discrete mass ejections, which occur on top of a compact jet, as testified by the detection of at least one short-duration millimetre flare with ALMA at the high-to-low mode switch. The pulsar is subsequently re-enshrouded, completing our picture of the mode switches. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.14509v2-abstract-full').style.display = 'none'; document.getElementById('2305.14509v2-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 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">25 pages, 12 figures, 9 tables. Accepted for publication on Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 677, A30 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.14157">arXiv:2304.14157</a> <span> [<a href="https://arxiv.org/pdf/2304.14157">pdf</a>, <a href="https://arxiv.org/format/2304.14157">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> <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/10.1093/mnras/stad1298">10.1093/mnras/stad1298 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Bursts from Space: MeerKAT - The first citizen science project dedicated to commensal radio transients </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Andersson%2C+A">Alex Andersson</a>, <a href="/search/?searchtype=author&query=Lintott%2C+C">Chris Lintott</a>, <a href="/search/?searchtype=author&query=Fender%2C+R">Rob Fender</a>, <a href="/search/?searchtype=author&query=Bright%2C+J">Joe Bright</a>, <a href="/search/?searchtype=author&query=Carotenuto%2C+F">Francesco Carotenuto</a>, <a href="/search/?searchtype=author&query=Driessen%2C+L">Laura Driessen</a>, <a href="/search/?searchtype=author&query=Espinasse%2C+M">Mathilde Espinasse</a>, <a href="/search/?searchtype=author&query=Gaseahalwe%2C+K">Kelebogile Gaseahalwe</a>, <a href="/search/?searchtype=author&query=Heywood%2C+I">Ian Heywood</a>, <a href="/search/?searchtype=author&query=van+der+Horst%2C+A+J">Alexander J. van der Horst</a>, <a href="/search/?searchtype=author&query=Motta%2C+S">Sara Motta</a>, <a href="/search/?searchtype=author&query=Rhodes%2C+L">Lauren Rhodes</a>, <a href="/search/?searchtype=author&query=Tremou%2C+E">Evangelia Tremou</a>, <a href="/search/?searchtype=author&query=Williams%2C+D+R+A">David R. A. Williams</a>, <a href="/search/?searchtype=author&query=Woudt%2C+P">Patrick Woudt</a>, <a href="/search/?searchtype=author&query=Zhang%2C+X">Xian Zhang</a>, <a href="/search/?searchtype=author&query=Bloemen%2C+S">Steven Bloemen</a>, <a href="/search/?searchtype=author&query=Groot%2C+P">Paul Groot</a>, <a href="/search/?searchtype=author&query=Vreeswijk%2C+P">Paul Vreeswijk</a>, <a href="/search/?searchtype=author&query=Giarratana%2C+S">Stefano Giarratana</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">Payaswini Saikia</a>, <a href="/search/?searchtype=author&query=Andersson%2C+J">Jonas Andersson</a>, <a href="/search/?searchtype=author&query=Arroyo%2C+L+R">Lizzeth Ruiz Arroyo</a>, <a href="/search/?searchtype=author&query=Baert%2C+L">Lo茂c Baert</a>, <a href="/search/?searchtype=author&query=Baumann%2C+M">Matthew Baumann</a> , et al. (18 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="2304.14157v1-abstract-short" style="display: inline;"> The newest generation of radio telescopes are able to survey large areas with high sensitivity and cadence, producing data volumes that require new methods to better understand the transient sky. Here we describe the results from the first citizen science project dedicated to commensal radio transients, using data from the MeerKAT telescope with weekly cadence. Bursts from Space: MeerKAT was launc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.14157v1-abstract-full').style.display = 'inline'; document.getElementById('2304.14157v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.14157v1-abstract-full" style="display: none;"> The newest generation of radio telescopes are able to survey large areas with high sensitivity and cadence, producing data volumes that require new methods to better understand the transient sky. Here we describe the results from the first citizen science project dedicated to commensal radio transients, using data from the MeerKAT telescope with weekly cadence. Bursts from Space: MeerKAT was launched late in 2021 and received ~89000 classifications from over 1000 volunteers in 3 months. Our volunteers discovered 142 new variable sources which, along with the known transients in our fields, allowed us to estimate that at least 2.1 per cent of radio sources are varying at 1.28 GHz at the sampled cadence and sensitivity, in line with previous work. We provide the full catalogue of these sources, the largest of candidate radio variables to date. Transient sources found with archival counterparts include a pulsar (B1845-01) and an OH maser star (OH 30.1-0.7), in addition to the recovery of known stellar flares and X-ray binary jets in our observations. Data from the MeerLICHT optical telescope, along with estimates of long time-scale variability induced by scintillation, imply that the majority of the new variables are active galactic nuclei. This tells us that citizen scientists can discover phenomena varying on time-scales from weeks to several years. The success both in terms of volunteer engagement and scientific merit warrants the continued development of the project, whilst we use the classifications from volunteers to develop machine learning techniques for finding transients. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.14157v1-abstract-full').style.display = 'none'; document.getElementById('2304.14157v1-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">Accepted to MNRAS, 14 pages + an appendix containing our main data table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.06642">arXiv:2304.06642</a> <span> [<a href="https://arxiv.org/pdf/2304.06642">pdf</a>, <a href="https://arxiv.org/ps/2304.06642">ps</a>, <a href="https://arxiv.org/format/2304.06642">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/stad1122">10.1093/mnras/stad1122 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LeMMINGs. VI. Connecting nuclear activity to bulge properties of active and inactive galaxies: radio scaling relations and galaxy environment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Dullo%2C+B+T">B. T. Dullo</a>, <a href="/search/?searchtype=author&query=Knapen%2C+J+H">J. H. Knapen</a>, <a href="/search/?searchtype=author&query=Beswick%2C+R+J">R. J. Beswick</a>, <a href="/search/?searchtype=author&query=Baldi%2C+R+D">R. D. Baldi</a>, <a href="/search/?searchtype=author&query=Williams%2C+D+R+A">D. R. A. Williams</a>, <a href="/search/?searchtype=author&query=McHardy%2C+I+M">I. M. McHardy</a>, <a href="/search/?searchtype=author&query=Green%2C+D+A">D. A. Green</a>, <a href="/search/?searchtype=author&query=de+Paz%2C+A+G">A. Gil de Paz</a>, <a href="/search/?searchtype=author&query=Aalto%2C+S">S. Aalto</a>, <a href="/search/?searchtype=author&query=Alberdi%2C+A">A. Alberdi</a>, <a href="/search/?searchtype=author&query=Argo%2C+M+K">M. K. Argo</a>, <a href="/search/?searchtype=author&query=Kl%C3%B6ckner%2C+H+-">H. -R. Kl枚ckner</a>, <a href="/search/?searchtype=author&query=Mutie%2C+I+M">I. M. Mutie</a>, <a href="/search/?searchtype=author&query=Saikia%2C+D+J">D. J. Saikia</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">P. Saikia</a>, <a href="/search/?searchtype=author&query=Stevens%2C+I+R">I. R. Stevens</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="2304.06642v1-abstract-short" style="display: inline;"> Multiwavelength studies indicate that nuclear activity and bulge properties are closely related, but the details remain unclear. To study this further, we combine $Hubble~Space~Telescope$ bulge structural and photometric properties with 1.5 GHz, $e$-MERLIN nuclear radio continuum data from the LeMMINGs survey for a large sample of 173 `active' galaxies (LINERs and Seyferts) and `inactive' galaxies… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.06642v1-abstract-full').style.display = 'inline'; document.getElementById('2304.06642v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.06642v1-abstract-full" style="display: none;"> Multiwavelength studies indicate that nuclear activity and bulge properties are closely related, but the details remain unclear. To study this further, we combine $Hubble~Space~Telescope$ bulge structural and photometric properties with 1.5 GHz, $e$-MERLIN nuclear radio continuum data from the LeMMINGs survey for a large sample of 173 `active' galaxies (LINERs and Seyferts) and `inactive' galaxies (H IIs and absorption line galaxies, ALGs). Dividing our sample into active and inactive, they define distinct (radio core luminosity)$-$(bulge mass), L_R,core-M_*,bulge, relations, with a mass turnover at M_*, bulge ~ 10^(9.8 +- 0.3) M_sun (supermassive black hole mass M_BH ~ 10^(6.8 +- 0.3) M_sun), which marks the transition from AGN-dominated nuclear radio emission in more massive bulges to that mainly driven by stellar processes in low-mass bulges. None of our 10/173 bulgeless galaxies host an AGN. The AGN fraction increases with increasing M_*, bulge such that f_optical_AGN $\propto$ M_*,bulge^(0.24 +- 0.06) and f_radio_AGN $\propto$ M_*,bulge^(0.24 +- 0.05). Between M_*,bulge ~ 10^8.5 and 10^11.3 M_sun, f_optical_AGN steadily rises from 15 +- 4 to 80 +- 5 per cent. We find that at fixed bulge mass, the radio loudness, nuclear radio activity and the (optical and radio) AGN fraction exhibit no dependence on environment. Radio-loud hosts preferentially possess an early-type morphology than radio-quiet hosts, the two types are however indistinguishable in terms of bulge S茅rsic index and ellipticity, while results on the bulge inner logarithmic profile slope are inconclusive. We finally discuss the importance of bulge mass in determining the AGN triggering processes, including potential implications for the nuclear radio emission in nearby galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.06642v1-abstract-full').style.display = 'none'; document.getElementById('2304.06642v1-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 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">27 pages, 15 figures, 4 tables, 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/2304.02046">arXiv:2304.02046</a> <span> [<a href="https://arxiv.org/pdf/2304.02046">pdf</a>, <a href="https://arxiv.org/format/2304.02046">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acc8cc">10.3847/1538-4357/acc8cc <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Seven reflares, a mini-outburst and an outburst : High amplitude optical variations in the black hole X-ray binary Swift J1910.2-0546 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Saikia%2C+P">Payaswini Saikia</a>, <a href="/search/?searchtype=author&query=Russell%2C+D+M">David M. Russell</a>, <a href="/search/?searchtype=author&query=Pirbhoy%2C+S+F">Saarah F. Pirbhoy</a>, <a href="/search/?searchtype=author&query=Baglio%2C+M+C">M. C. Baglio</a>, <a href="/search/?searchtype=author&query=Bramich%2C+D+M">D. M. Bramich</a>, <a href="/search/?searchtype=author&query=Alabarta%2C+K">Kevin Alabarta</a>, <a href="/search/?searchtype=author&query=Lewis%2C+F">Fraser Lewis</a>, <a href="/search/?searchtype=author&query=Charles%2C+P">Phil Charles</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="2304.02046v1-abstract-short" style="display: inline;"> We present long-term (2012-2022) optical monitoring of the candidate black hole X-ray binary Swift J1910.2-0546 with the Faulkes Telescopes and Las Cumbres Observatory (LCO) network. Following its initial bright 2012 outburst, we find that the source displayed a series of at least 7 quasi-periodic, high amplitude (~3 mags) optical reflares in 2013, with a recurrence time increasing from ~42 days t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.02046v1-abstract-full').style.display = 'inline'; document.getElementById('2304.02046v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.02046v1-abstract-full" style="display: none;"> We present long-term (2012-2022) optical monitoring of the candidate black hole X-ray binary Swift J1910.2-0546 with the Faulkes Telescopes and Las Cumbres Observatory (LCO) network. Following its initial bright 2012 outburst, we find that the source displayed a series of at least 7 quasi-periodic, high amplitude (~3 mags) optical reflares in 2013, with a recurrence time increasing from ~42 days to ~49 days. In 2014, the source experienced a mini-outburst with two peaks in the optical. We also study the recent 2022 outburst of the source at optical wavelengths, and perform a comparative analysis with the earlier rebrightenings. A single X-ray detection and only two radio detections were obtained during the 2013 reflaring period, and only optical detections were acquired in 2014. During the reflaring in both 2013 and 2014, the source showed bluer-when-brighter behavior, having optical colors consistent with a blackbody heating and cooling between 4500 and 9500 K, i.e. the temperature range in which hydrogen starts to ionize. Finally, we compare the flaring behavior of the source to re-brightening events in other X-ray binaries. We show that the repeated reflarings of Swift J1910.2-0546 are highly unusual, and propose that they arise from a sequence of repetitive heating and cooling front reflections travelling through the accretion disk. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.02046v1-abstract-full').style.display = 'none'; document.getElementById('2304.02046v1-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 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">Accepted for publication in ApJ, appendix will appear at the published version of 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/2303.11154">arXiv:2303.11154</a> <span> [<a href="https://arxiv.org/pdf/2303.11154">pdf</a>, <a href="https://arxiv.org/ps/2303.11154">ps</a>, <a href="https://arxiv.org/format/2303.11154">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/10.1051/0004-6361/202345913">10.1051/0004-6361/202345913 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LeMMINGs. V. Nuclear activity and bulge properties: a detailed multi-component decomposition of $e$-MERLIN Palomar galaxies with $HST$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Dullo%2C+B+T">B. T. Dullo</a>, <a href="/search/?searchtype=author&query=Knapen%2C+J+H">J. H. Knapen</a>, <a href="/search/?searchtype=author&query=Beswick%2C+R+J">R. J. Beswick</a>, <a href="/search/?searchtype=author&query=Baldi%2C+R+D">R. D. Baldi</a>, <a href="/search/?searchtype=author&query=Williams%2C+D+R+A">D. R. A. Williams</a>, <a href="/search/?searchtype=author&query=McHardy%2C+I+M">I. M. McHardy</a>, <a href="/search/?searchtype=author&query=Gallagher%2C+J+S">J. S. Gallagher</a>, <a href="/search/?searchtype=author&query=Aalto%2C+S">S. Aalto</a>, <a href="/search/?searchtype=author&query=Argo%2C+M+K">M. K. Argo</a>, <a href="/search/?searchtype=author&query=de+Paz%2C+A+G">A. Gil de Paz</a>, <a href="/search/?searchtype=author&query=Kl%C3%B6ckner%2C+H+-">H. -R. Kl枚ckner</a>, <a href="/search/?searchtype=author&query=Marcaide%2C+J+M">J. M. Marcaide</a>, <a href="/search/?searchtype=author&query=Mundell%2C+C+G">C. G. Mundell</a>, <a href="/search/?searchtype=author&query=Mutie%2C+I+M">I. M. Mutie</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">P. Saikia</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="2303.11154v1-abstract-short" style="display: inline;"> [Abridged] We use high-resolution $HST$ imaging and $e$-MERLIN 1.5-GHz observations of galaxy cores from the LeMMINGs survey to investigate the relation between optical structural properties and nuclear radio emission for a large sample of galaxies. We perform accurate, multi-component decompositions of new surface brightness profiles extracted from $HST$ images for 163 LeMMINGs galaxies and fit u… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.11154v1-abstract-full').style.display = 'inline'; document.getElementById('2303.11154v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.11154v1-abstract-full" style="display: none;"> [Abridged] We use high-resolution $HST$ imaging and $e$-MERLIN 1.5-GHz observations of galaxy cores from the LeMMINGs survey to investigate the relation between optical structural properties and nuclear radio emission for a large sample of galaxies. We perform accurate, multi-component decompositions of new surface brightness profiles extracted from $HST$ images for 163 LeMMINGs galaxies and fit up to six galaxy components (e.g., bulges, discs, AGN, bars, rings, spiral arms, and nuclear star clusters) simultaneously with S茅rsic and/or core-S茅rsic models. By adding such decomposition data for 10 LeMMINGs galaxies from our past work, the final sample of 173 nearby galaxies (102 Ss, 42 S0s, 23 Es plus 6 Irr) with bulge stellar mass (typically) M_*, bulge ~ 10^6-10^12.5 M_sun, encompasses all optical spectral classes (LINER, Seyfert, ALG and H II). We show that the bulge mass can be significantly overestimated in many galaxies when components such as bars, rings and spirals are not included in the fits. We additionally implement a Monte Carlo method to determine errors on bulge, disc and other fitted structural parameters. Moving (in the opposite direction) across the Hubble sequence, i.e., from the irregular to elliptical galaxies, we confirm that bulges become larger, more prominent and round. Such bulge dominance is associated with a brighter radio core luminosity. We also find that the radio detection fraction increases with bulge mass. At M_*,bulge > 10^11 M_sun, the radio detection fraction is 77%, declining to 24% for M_bulge < 10^10 M_sun. Furthermore, we observe core-S茅rsic bulges tend to be systematically round and to possess high radio core luminosities and boxy-distorted or pure elliptical isophotes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.11154v1-abstract-full').style.display = 'none'; document.getElementById('2303.11154v1-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">102 pages, 26 figures, 10 tables, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 675, A105 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.01750">arXiv:2302.01750</a> <span> [<a href="https://arxiv.org/pdf/2302.01750">pdf</a>, <a href="https://arxiv.org/ps/2302.01750">ps</a>, <a href="https://arxiv.org/format/2302.01750">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Number Theory">math.NT</span> </div> </div> <p class="title is-5 mathjax"> Ramanujan-type Congruences for Partition $k$-Tuples with $5$-Cores </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Saikia%2C+M+P">Manjil P. Saikia</a>, <a href="/search/?searchtype=author&query=Sarma%2C+A">Abhishek Sarma</a>, <a href="/search/?searchtype=author&query=Talukdar%2C+P">Pranjal Talukdar</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="2302.01750v1-abstract-short" style="display: inline;"> We prove several Ramanujan-type congruences modulo powers of $5$ for partition $k$-tuples with $5$-cores, for $k=2, 3, 4$. We also prove some new infinite families of congruences modulo powers of primes for $k$-tuples with $p$-cores, where $p$ is a prime. </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.01750v1-abstract-full" style="display: none;"> We prove several Ramanujan-type congruences modulo powers of $5$ for partition $k$-tuples with $5$-cores, for $k=2, 3, 4$. We also prove some new infinite families of congruences modulo powers of primes for $k$-tuples with $p$-cores, where $p$ is a prime. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.01750v1-abstract-full').style.display = 'none'; document.getElementById('2302.01750v1-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 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">10 pages, comments are welcome</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 11P81; 11P83 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.09849">arXiv:2301.09849</a> <span> [<a href="https://arxiv.org/pdf/2301.09849">pdf</a>, <a href="https://arxiv.org/ps/2301.09849">ps</a>, <a href="https://arxiv.org/format/2301.09849">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Combinatorics">math.CO</span> </div> </div> <p class="title is-5 mathjax"> Extensions of some results of Jovovic and Dhar </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Mahanta%2C+P+J">Pankaj Jyoti Mahanta</a>, <a href="/search/?searchtype=author&query=Saikia%2C+M+P">Manjil P. Saikia</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="2301.09849v2-abstract-short" style="display: inline;"> We look at extensions of formulas given by Jovovic and recently proved by Dhar on integer partitions where the smallest part occurs at least $m$ times and on integer partitions with fixed differences between the largest and smallest parts where the smallest part occurs at least $k$ times. Our results extend Dhar's results for the $m=2$ and $k=1$ cases to the general cases for arbitrary $m$ and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.09849v2-abstract-full').style.display = 'inline'; document.getElementById('2301.09849v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.09849v2-abstract-full" style="display: none;"> We look at extensions of formulas given by Jovovic and recently proved by Dhar on integer partitions where the smallest part occurs at least $m$ times and on integer partitions with fixed differences between the largest and smallest parts where the smallest part occurs at least $k$ times. Our results extend Dhar's results for the $m=2$ and $k=1$ cases to the general cases for arbitrary $m$ and $k$. We also look at analogous results for overpartitions and $\ell$-regular partitions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.09849v2-abstract-full').style.display = 'none'; document.getElementById('2301.09849v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 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">15 pages, accepted version (Journal of the Ramanujan Mathematical Society)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 11P81; 05A17 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.09846">arXiv:2301.09846</a> <span> [<a href="https://arxiv.org/pdf/2301.09846">pdf</a>, <a href="https://arxiv.org/ps/2301.09846">ps</a>, <a href="https://arxiv.org/format/2301.09846">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Number Theory">math.NT</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/s40590-022-00487-8">10.1007/s40590-022-00487-8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Some Missed Congruences modulo powers of $2$ for $t$-colored overpartitions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Saikia%2C+M+P">Manjil P. Saikia</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="2301.09846v1-abstract-short" style="display: inline;"> Recently, Nayaka and Naika (2022) proved several congruences modulo $16$ and $32$ for $t$-colored overpartitions with $t=5,7,11$ and $13$. We extend their list using an algorithmic technique. </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.09846v1-abstract-full" style="display: none;"> Recently, Nayaka and Naika (2022) proved several congruences modulo $16$ and $32$ for $t$-colored overpartitions with $t=5,7,11$ and $13$. We extend their list using an algorithmic technique. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.09846v1-abstract-full').style.display = 'none'; document.getElementById('2301.09846v1-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, 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">7 pages, published</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 11P81; 11P83 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Bolet铆n de la Sociedad Matem谩tica Mexicana, 2023, 29 (1), Article 15, 10 pp </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.09845">arXiv:2301.09845</a> <span> [<a href="https://arxiv.org/pdf/2301.09845">pdf</a>, <a href="https://arxiv.org/ps/2301.09845">ps</a>, <a href="https://arxiv.org/format/2301.09845">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Number Theory">math.NT</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Combinatorics">math.CO</span> </div> </div> <p class="title is-5 mathjax"> Biases in Non-Unitary Partitions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Mahanta%2C+P+J">Pankaj Jyoti Mahanta</a>, <a href="/search/?searchtype=author&query=Saikia%2C+M+P">Manjil P. Saikia</a>, <a href="/search/?searchtype=author&query=Sarma%2C+A">Abhishek Sarma</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="2301.09845v1-abstract-short" style="display: inline;"> Recently, the concept of parity bias in integer partitions has been studied by several authors. We continue this study here, but for non-unitary partitions (namely, partitions with parts greater than $1$). We prove analogous results for these restricted partitions as those that have been obtained by Kim, Kim, and Lovejoy (2020) and Kim and Kim (2021). We also look at inequalities between two class… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.09845v1-abstract-full').style.display = 'inline'; document.getElementById('2301.09845v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.09845v1-abstract-full" style="display: none;"> Recently, the concept of parity bias in integer partitions has been studied by several authors. We continue this study here, but for non-unitary partitions (namely, partitions with parts greater than $1$). We prove analogous results for these restricted partitions as those that have been obtained by Kim, Kim, and Lovejoy (2020) and Kim and Kim (2021). We also look at inequalities between two classes of partitions studied by Andrews (2019) where the parts are separated by parity (either all odd parts are smaller than all even parts or vice versa). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.09845v1-abstract-full').style.display = 'none'; document.getElementById('2301.09845v1-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, 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">11 pages</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 05A17; 11P83 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.10228">arXiv:2209.10228</a> <span> [<a href="https://arxiv.org/pdf/2209.10228">pdf</a>, <a href="https://arxiv.org/format/2209.10228">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/stac2700">10.1093/mnras/stac2700 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radio observations of the Black Hole X-ray Binary EXO 1846-031 re-awakening from a 34-year slumber </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Williams%2C+D+R+A">D. R. A. Williams</a>, <a href="/search/?searchtype=author&query=Motta%2C+S+E">S. E. Motta</a>, <a href="/search/?searchtype=author&query=Fender%2C+R">R. Fender</a>, <a href="/search/?searchtype=author&query=Miller-Jones%2C+J+C+A">J. C. A. Miller-Jones</a>, <a href="/search/?searchtype=author&query=Neilsen%2C+J">J. Neilsen</a>, <a href="/search/?searchtype=author&query=Allison%2C+J+R">J. R. Allison</a>, <a href="/search/?searchtype=author&query=Bright%2C+J">J. Bright</a>, <a href="/search/?searchtype=author&query=Heywood%2C+I">I. Heywood</a>, <a href="/search/?searchtype=author&query=Jacob%2C+P+F+L">P. F. L. Jacob</a>, <a href="/search/?searchtype=author&query=Rhodes%2C+L">L. Rhodes</a>, <a href="/search/?searchtype=author&query=Tremou%2C+E">E. Tremou</a>, <a href="/search/?searchtype=author&query=Woudt%2C+P">P. Woudt</a>, <a href="/search/?searchtype=author&query=Eijnden%2C+J+v+d">J. van den Eijnden</a>, <a href="/search/?searchtype=author&query=Carotenuto%2C+F">F. Carotenuto</a>, <a href="/search/?searchtype=author&query=Green%2C+D+A">D. A. Green</a>, <a href="/search/?searchtype=author&query=Titterington%2C+D">D. Titterington</a>, <a href="/search/?searchtype=author&query=van+der+Horst%2C+A+J">A. J. van der Horst</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">P. Saikia</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="2209.10228v1-abstract-short" style="display: inline;"> We present radio [1.3 GHz MeerKAT, 4-8 GHz Karl G. Jansky Very Large Array (VLA) and 15.5 GHz Arcminute Microkelvin Imager Large Array (AMI-LA)] and X-ray (Swift and MAXI) data from the 2019 outburst of the candidate Black Hole X-ray Binary (BHXB) EXO 1846-031. We compute a Hardness-Intensity diagram, which shows the characteristic q-shaped hysteresis of BHXBs in outburst. EXO 1846-031 was monitor… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.10228v1-abstract-full').style.display = 'inline'; document.getElementById('2209.10228v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.10228v1-abstract-full" style="display: none;"> We present radio [1.3 GHz MeerKAT, 4-8 GHz Karl G. Jansky Very Large Array (VLA) and 15.5 GHz Arcminute Microkelvin Imager Large Array (AMI-LA)] and X-ray (Swift and MAXI) data from the 2019 outburst of the candidate Black Hole X-ray Binary (BHXB) EXO 1846-031. We compute a Hardness-Intensity diagram, which shows the characteristic q-shaped hysteresis of BHXBs in outburst. EXO 1846-031 was monitored weekly with MeerKAT and approximately daily with AMI-LA. The VLA observations provide sub-arcsecond-resolution images at key points in the outburst, showing moving radio components. The radio and X-ray light curves broadly follow each other, showing a peak on ~MJD 58702, followed by a short decline before a second peak between ~MJD 58731-58739. We estimate the minimum energy of these radio flares from equipartition, calculating values of $E_{\rm min} \sim$ 4$\times$10$^{41}$ and 5$\times$10$^{42}$ erg, respectively. The exact date of the return to `quiescence' is missed in the X-ray and radio observations, but we suggest that it likely occurred between MJD 58887 and 58905. From the Swift X-ray flux on MJD 58905 and assuming the soft-to-hard transition happened at 0.3-3 per cent Eddington, we calculate a distance range of 2.4-7.5\,kpc. We computed the radio:X-ray plane for EXO 1846-031 in the `hard' state, showing that it is most likely a `radio-quiet' BH, preferentially at 4.5 kpc. Using this distance and a jet inclination angle of $胃$=73$^{\circ}$, the VLA data place limits on the intrinsic jet speed of $尾_{\rm int} = 0.29c$, indicating sub-luminal jet motion. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.10228v1-abstract-full').style.display = 'none'; document.getElementById('2209.10228v1-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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 on 20 September 2022, 17 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/2208.00788">arXiv:2208.00788</a> <span> [<a href="https://arxiv.org/pdf/2208.00788">pdf</a>, <a href="https://arxiv.org/format/2208.00788">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="Artificial Intelligence">cs.AI</span> </div> </div> <p class="title is-5 mathjax"> A Hybrid CNN-LSTM model for Video Deepfake Detection by Leveraging Optical Flow Features </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Saikia%2C+P">Pallabi Saikia</a>, <a href="/search/?searchtype=author&query=Dholaria%2C+D">Dhwani Dholaria</a>, <a href="/search/?searchtype=author&query=Yadav%2C+P">Priyanka Yadav</a>, <a href="/search/?searchtype=author&query=Patel%2C+V">Vaidehi Patel</a>, <a href="/search/?searchtype=author&query=Roy%2C+M">Mohendra Roy</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="2208.00788v1-abstract-short" style="display: inline;"> Deepfakes are the synthesized digital media in order to create ultra-realistic fake videos to trick the spectator. Deep generative algorithms, such as, Generative Adversarial Networks(GAN) are widely used to accomplish such tasks. This approach synthesizes pseudo-realistic contents that are very difficult to distinguish by traditional detection methods. In most cases, Convolutional Neural Network(… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.00788v1-abstract-full').style.display = 'inline'; document.getElementById('2208.00788v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.00788v1-abstract-full" style="display: none;"> Deepfakes are the synthesized digital media in order to create ultra-realistic fake videos to trick the spectator. Deep generative algorithms, such as, Generative Adversarial Networks(GAN) are widely used to accomplish such tasks. This approach synthesizes pseudo-realistic contents that are very difficult to distinguish by traditional detection methods. In most cases, Convolutional Neural Network(CNN) based discriminators are being used for detecting such synthesized media. However, it emphasise primarily on the spatial attributes of individual video frames, thereby fail to learn the temporal information from their inter-frame relations. In this paper, we leveraged an optical flow based feature extraction approach to extract the temporal features, which are then fed to a hybrid model for classification. This hybrid model is based on the combination of CNN and recurrent neural network (RNN) architectures. The hybrid model provides effective performance on open source data-sets such as, DFDC, FF++ and Celeb-DF. This proposed method shows an accuracy of 66.26%, 91.21% and 79.49% in DFDC, FF++, and Celeb-DF respectively with a very reduced No of sample size of approx 100 samples(frames). This promises early detection of fake contents compared to existing modalities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.00788v1-abstract-full').style.display = 'none'; document.getElementById('2208.00788v1-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> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Copyright is with IEEE, Paper No: 832, IJCNN, 2022 IEEE World Congress on Computational Intelligence </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.13500">arXiv:2207.13500</a> <span> [<a href="https://arxiv.org/pdf/2207.13500">pdf</a>, <a href="https://arxiv.org/format/2207.13500">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Social and Information Networks">cs.SI</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Computation and Language">cs.CL</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Information Retrieval">cs.IR</span> </div> </div> <p class="title is-5 mathjax"> Modelling Social Context for Fake News Detection: A Graph Neural Network Based Approach </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Saikia%2C+P">Pallabi Saikia</a>, <a href="/search/?searchtype=author&query=Gundale%2C+K">Kshitij Gundale</a>, <a href="/search/?searchtype=author&query=Jain%2C+A">Ankit Jain</a>, <a href="/search/?searchtype=author&query=Jadeja%2C+D">Dev Jadeja</a>, <a href="/search/?searchtype=author&query=Patel%2C+H">Harvi Patel</a>, <a href="/search/?searchtype=author&query=Roy%2C+M">Mohendra Roy</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="2207.13500v1-abstract-short" style="display: inline;"> Detection of fake news is crucial to ensure the authenticity of information and maintain the news ecosystems reliability. Recently, there has been an increase in fake news content due to the recent proliferation of social media and fake content generation techniques such as Deep Fake. The majority of the existing modalities of fake news detection focus on content based approaches. However, most of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.13500v1-abstract-full').style.display = 'inline'; document.getElementById('2207.13500v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.13500v1-abstract-full" style="display: none;"> Detection of fake news is crucial to ensure the authenticity of information and maintain the news ecosystems reliability. Recently, there has been an increase in fake news content due to the recent proliferation of social media and fake content generation techniques such as Deep Fake. The majority of the existing modalities of fake news detection focus on content based approaches. However, most of these techniques fail to deal with ultra realistic synthesized media produced by generative models. Our recent studies find that the propagation characteristics of authentic and fake news are distinguishable, irrespective of their modalities. In this regard, we have investigated the auxiliary information based on social context to detect fake news. This paper has analyzed the social context of fake news detection with a hybrid graph neural network based approach. This hybrid model is based on integrating a graph neural network on the propagation of news and bi directional encoder representations from the transformers model on news content to learn the text features. Thus this proposed approach learns the content as well as the context features and hence able to outperform the baseline models with an f1 score of 0.91 on PolitiFact and 0.93 on the Gossipcop dataset, respectively <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.13500v1-abstract-full').style.display = 'none'; document.getElementById('2207.13500v1-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 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">Journal ref:</span> copyright with IEEE, Paper No: 834, IJCNN, 2022 IEEE World Congress on Computational Intelligence </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.03962">arXiv:2207.03962</a> <span> [<a href="https://arxiv.org/pdf/2207.03962">pdf</a>, <a href="https://arxiv.org/format/2207.03962">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/stac2392">10.1093/mnras/stac2392 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MeerKAT radio observations of the neutron star low-mass X-ray binary Cen X-4 at low accretion rates </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Eijnden%2C+J+v+d">J. van den Eijnden</a>, <a href="/search/?searchtype=author&query=Fender%2C+R">R. Fender</a>, <a href="/search/?searchtype=author&query=Miller-Jones%2C+J+C+A">J. C. A. Miller-Jones</a>, <a href="/search/?searchtype=author&query=Russell%2C+T+D">T. D. Russell</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">P. Saikia</a>, <a href="/search/?searchtype=author&query=Sivakoff%2C+G+R">G. R. Sivakoff</a>, <a href="/search/?searchtype=author&query=Carotenuto%2C+F">F. Carotenuto</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="2207.03962v2-abstract-short" style="display: inline;"> Centaurus X-4 (Cen X-4) is a relatively nearby neutron star low-mass X-ray binary that showed outbursts in 1969 and 1979, but has not shown a full outburst since. Due to its proximity and sustained period of quiescence, it is a prime target to study the coupling between accretion and jet ejection in quiescent neutron star low-mass X-ray binaries. Here, we present four MeerKAT radio observations at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.03962v2-abstract-full').style.display = 'inline'; document.getElementById('2207.03962v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.03962v2-abstract-full" style="display: none;"> Centaurus X-4 (Cen X-4) is a relatively nearby neutron star low-mass X-ray binary that showed outbursts in 1969 and 1979, but has not shown a full outburst since. Due to its proximity and sustained period of quiescence, it is a prime target to study the coupling between accretion and jet ejection in quiescent neutron star low-mass X-ray binaries. Here, we present four MeerKAT radio observations at 1.3 GHz of Cen X-4, combined with NICER and Swift X-ray monitoring. During the first and most sensitive observation, Cen X-4 was in a fully quiescent X-ray state. The three later and shorter observations targeted a brief period of faint X-ray activity in January 2021, which has been referred to as a 'mis-fired' outburst. Cen X-4 is not detected in any of the four MeerKAT observations. We place these radio non-detections on the X-ray -- radio luminosity diagram, improving the constraints on the correlation between the two luminosities from earlier quiescent radio studies. We confirm that Cen X-4 is radio fainter than the transitional milli-second pulsar PSR J1023+0038 at the same X-ray luminosity. We discuss the radio behaviour of accreting neutron stars at low X-ray luminosity more generally and finally comment on future observing campaigns. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.03962v2-abstract-full').style.display = 'none'; document.getElementById('2207.03962v2-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 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 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">12 pages, 4 figures, 2 tables. 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/2205.04452">arXiv:2205.04452</a> <span> [<a href="https://arxiv.org/pdf/2205.04452">pdf</a>, <a href="https://arxiv.org/format/2205.04452">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac6ce1">10.3847/1538-4357/ac6ce1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A multi-wavelength study of GRS 1716-249 in outburst : constraints on its system parameters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Saikia%2C+P">Payaswini Saikia</a>, <a href="/search/?searchtype=author&query=Russell%2C+D+M">David M. Russell</a>, <a href="/search/?searchtype=author&query=Baglio%2C+M+C">M. C. Baglio</a>, <a href="/search/?searchtype=author&query=Bramich%2C+D+M">D. M. Bramich</a>, <a href="/search/?searchtype=author&query=Casella%2C+P">Piergiorgio Casella</a>, <a href="/search/?searchtype=author&query=Trigo%2C+M+D">M. Diaz Trigo</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">Poshak Gandhi</a>, <a href="/search/?searchtype=author&query=Jiang%2C+J">Jiachen Jiang</a>, <a href="/search/?searchtype=author&query=Maccarone%2C+T">Thomas Maccarone</a>, <a href="/search/?searchtype=author&query=Soria%2C+R">Roberto Soria</a>, <a href="/search/?searchtype=author&query=Noori%2C+H+A">Hind Al Noori</a>, <a href="/search/?searchtype=author&query=Yazeedi%2C+A+A">Aisha Al Yazeedi</a>, <a href="/search/?searchtype=author&query=Alabarta%2C+K">Kevin Alabarta</a>, <a href="/search/?searchtype=author&query=Belloni%2C+T">Tomaso Belloni</a>, <a href="/search/?searchtype=author&query=Bel%2C+M+C">Marion Cadolle Bel</a>, <a href="/search/?searchtype=author&query=Ceccobello%2C+C">Chiara Ceccobello</a>, <a href="/search/?searchtype=author&query=Corbel%2C+S">Stephane Corbel</a>, <a href="/search/?searchtype=author&query=Fender%2C+R">Rob Fender</a>, <a href="/search/?searchtype=author&query=Gallo%2C+E">Elena Gallo</a>, <a href="/search/?searchtype=author&query=Homan%2C+J">Jeroen Homan</a>, <a href="/search/?searchtype=author&query=Koljonen%2C+K">Karri Koljonen</a>, <a href="/search/?searchtype=author&query=Lewis%2C+F">Fraser Lewis</a>, <a href="/search/?searchtype=author&query=Markoff%2C+S+B">Sera B. Markoff</a>, <a href="/search/?searchtype=author&query=Miller-Jones%2C+J+C+A">James C. A. Miller-Jones</a>, <a href="/search/?searchtype=author&query=Rodriguez%2C+J">Jerome Rodriguez</a> , et al. (5 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="2205.04452v1-abstract-short" style="display: inline;"> We present a detailed study of the evolution of the Galactic black hole transient GRS 1716-249 during its 2016-2017 outburst at optical (Las Cumbres Observatory), mid-infrared (Very Large Telescope), near-infrared (Rapid Eye Mount telescope), and ultraviolet (the Neil Gehrels Swift Observatory Ultraviolet/Optical Telescope) wavelengths, along with archival radio and X-ray data. We show that the op… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.04452v1-abstract-full').style.display = 'inline'; document.getElementById('2205.04452v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.04452v1-abstract-full" style="display: none;"> We present a detailed study of the evolution of the Galactic black hole transient GRS 1716-249 during its 2016-2017 outburst at optical (Las Cumbres Observatory), mid-infrared (Very Large Telescope), near-infrared (Rapid Eye Mount telescope), and ultraviolet (the Neil Gehrels Swift Observatory Ultraviolet/Optical Telescope) wavelengths, along with archival radio and X-ray data. We show that the optical/near-infrared and UV emission of the source mainly originates from a multi-temperature accretion disk, while the mid-infrared and radio emission are dominated by synchrotron emission from a compact jet. The optical/UV flux density is correlated with the X-ray emission when the source is in the hard state, consistent with an X-ray irradiated accretion disk with an additional contribution from the viscous disk during the outburst fade. We also report the long-term optical light curve of the source and find that the quiescent i-band magnitude is 21.39$\pm$0.15 mag. Furthermore, we discuss how previous estimates of the system parameters of the source are based on various incorrect assumptions, and so are likely to be inaccurate. By comparing our GRS 1716-249 dataset to those of other outbursting black hole X-ray binaries, we find that while GRS 1716-249 shows similar X-ray behaviour, it is noticeably optically fainter, if the literature distance of 2.4 kpc is adopted. Using several lines of reasoning, we argue that the source distance is further than previously assumed in the literature, likely within 4-17 kpc, with a most likely range of $\sim$4-8 kpc. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.04452v1-abstract-full').style.display = 'none'; document.getElementById('2205.04452v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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 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/2204.00030">arXiv:2204.00030</a> <span> [<a href="https://arxiv.org/pdf/2204.00030">pdf</a>, <a href="https://arxiv.org/format/2204.00030">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="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/10.3847/1538-4357/ac63ad">10.3847/1538-4357/ac63ad <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A misfired outburst in the neutron star X-ray binary Centaurus X-4 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Baglio%2C+M+C">M. C. Baglio</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">P. Saikia</a>, <a href="/search/?searchtype=author&query=Russell%2C+D+M">D. M. Russell</a>, <a href="/search/?searchtype=author&query=Homan%2C+J">J. Homan</a>, <a href="/search/?searchtype=author&query=Waterval%2C+S">S. Waterval</a>, <a href="/search/?searchtype=author&query=Bramich%2C+D+M">D. M. Bramich</a>, <a href="/search/?searchtype=author&query=Campana%2C+S">S. Campana</a>, <a href="/search/?searchtype=author&query=Lewis%2C+F">F. Lewis</a>, <a href="/search/?searchtype=author&query=Eijnden%2C+J+V+d">J. Van den Eijnden</a>, <a href="/search/?searchtype=author&query=Alabarta%2C+K">K. Alabarta</a>, <a href="/search/?searchtype=author&query=Covino%2C+S">S. Covino</a>, <a href="/search/?searchtype=author&query=D%27Avanzo%2C+P">P. D'Avanzo</a>, <a href="/search/?searchtype=author&query=Goldoni%2C+P">P. Goldoni</a>, <a href="/search/?searchtype=author&query=Masetti%2C+N">N. Masetti</a>, <a href="/search/?searchtype=author&query=Mu%C3%B1oz-Darias%2C+T">T. Mu帽oz-Darias</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="2204.00030v1-abstract-short" style="display: inline;"> We report on a long-term optical monitoring of the neutron star X-ray binary Centaurus X-4 performed during the last 13.5 years. This source has been in quiescence since its outburst in 1979. Our monitoring reveals the overall evolution of the accretion disc; we detect short-duration flares, likely originating also in the disc, superimposed with a small-amplitude (< 0.1 mag) ellipsoidal modulation… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.00030v1-abstract-full').style.display = 'inline'; document.getElementById('2204.00030v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.00030v1-abstract-full" style="display: none;"> We report on a long-term optical monitoring of the neutron star X-ray binary Centaurus X-4 performed during the last 13.5 years. This source has been in quiescence since its outburst in 1979. Our monitoring reveals the overall evolution of the accretion disc; we detect short-duration flares, likely originating also in the disc, superimposed with a small-amplitude (< 0.1 mag) ellipsoidal modulation from the companion star due to geometrical effects. A long-term (~2300 days) downward trend, followed by a shorter (~1000 days) upward one, is observed in the disc light curve. Such a rise in the optical has been observed for other X-ray binaries preceding outbursts, as predicted by the disc instability model. For Cen X-4, the rise of the optical flux proceeded for ~3 years, and culminated in a flux increase at all wavelengths (optical-UV-X-rays) at the end of 2020. This increase faded after ~2 weeks, without giving rise to a full outburst. We suggest that the propagation of an inside-out heating front was ignited due to a partial ionization of hydrogen in the inner disc. The propagation might have stalled soon after the ignition due to the increasing surface density in the disc that the front encountered while propagating outwards. The stall was likely eased by the low level irradiation of the outer regions of the large accretion disc, as shown by the slope of the optical/X-ray correlation, suggesting that irradiation does not play a strong role in the optical, compared to other sources of emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.00030v1-abstract-full').style.display = 'none'; document.getElementById('2204.00030v1-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, 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">18 pages, 10 figures, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.10842">arXiv:2203.10842</a> <span> [<a href="https://arxiv.org/pdf/2203.10842">pdf</a>, <a href="https://arxiv.org/format/2203.10842">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> <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/stac823">10.1093/mnras/stac823 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radio detections of IR-selected runaway stellar bow shocks </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Eijnden%2C+J+V+d">J. Van den Eijnden</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">P. Saikia</a>, <a href="/search/?searchtype=author&query=Mohamed%2C+S">S. Mohamed</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="2203.10842v1-abstract-short" style="display: inline;"> Massive stars moving at supersonic peculiar velocities through the interstellar medium (ISM) can create bow shocks, arc-like structures at the interface between the stellar wind and the ISM. Many such bow shocks have been detected and catalogued at IR wavelengths, but detections in other wavebands remain rare. Strikingly, while electrons are expected to be accelerated in the bow shock and their no… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.10842v1-abstract-full').style.display = 'inline'; document.getElementById('2203.10842v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.10842v1-abstract-full" style="display: none;"> Massive stars moving at supersonic peculiar velocities through the interstellar medium (ISM) can create bow shocks, arc-like structures at the interface between the stellar wind and the ISM. Many such bow shocks have been detected and catalogued at IR wavelengths, but detections in other wavebands remain rare. Strikingly, while electrons are expected to be accelerated in the bow shock and their non-thermal emission may include synchrotron emission at low frequencies, only two massive runaway stellar bow shocks have to date been detected in the radio band. Here, we examine a sample of fifty IR-detected bow shocks from the E-BOSS catalogues in recently released radio images from the Rapid ASKAP Continuum Survey (RACS). We identify three confident and three likely counterparts, as well as three inconclusive candidates requiring confirmation via follow-up observations. These detections significantly increase the number of known radio massive stellar bow shocks and highlight the advantage of dedicated searches with current and next-generation radio telescopes. We investigate the underlying radio emission mechanism for these radio sources, finding a mix of free-free-dominated and synchrotron-dominated systems. We also discuss the non-detected targets by putting constraints on their emission properties and investigating their detectability with future observations. Finally, we propose several future avenues of research to advance the study and understanding of bow shocks at radio frequencies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.10842v1-abstract-full').style.display = 'none'; document.getElementById('2203.10842v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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, 12 figures, 3 tables. Resubmitted to MNRAS after final round of very minor referee comments</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.10590">arXiv:2111.10590</a> <span> [<a href="https://arxiv.org/pdf/2111.10590">pdf</a>, <a href="https://arxiv.org/ps/2111.10590">ps</a>, <a href="https://arxiv.org/format/2111.10590">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Combinatorics">math.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Number Theory">math.NT</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.ejc.2022.103522">10.1016/j.ejc.2022.103522 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Parity biases in partitions and restricted partitions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Banerjee%2C+K">Koustav Banerjee</a>, <a href="/search/?searchtype=author&query=Bhattacharjee%2C+S">Sreerupa Bhattacharjee</a>, <a href="/search/?searchtype=author&query=Dastidar%2C+M+G">Manosij Ghosh Dastidar</a>, <a href="/search/?searchtype=author&query=Mahanta%2C+P+J">Pankaj Jyoti Mahanta</a>, <a href="/search/?searchtype=author&query=Saikia%2C+M+P">Manjil P. Saikia</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.10590v2-abstract-short" style="display: inline;"> Let $p_{o}(n)$ (resp. $p_{e}(n)$) denote the number of partitions of $n$ with more odd parts (resp. even parts) than even parts (resp. odd parts). Recently, Kim, Kim, and Lovejoy proved that $p_{o}(n)>p_{e}(n)$ for all $n>2$ and conjectured that $d_{o}(n)>d_{e}(n)$ for all $n>19$ where $d_{o}(n)$ (resp. $d_{e}(n)$) denote the number of partitions into distinct parts having more odd parts (resp. ev… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.10590v2-abstract-full').style.display = 'inline'; document.getElementById('2111.10590v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.10590v2-abstract-full" style="display: none;"> Let $p_{o}(n)$ (resp. $p_{e}(n)$) denote the number of partitions of $n$ with more odd parts (resp. even parts) than even parts (resp. odd parts). Recently, Kim, Kim, and Lovejoy proved that $p_{o}(n)>p_{e}(n)$ for all $n>2$ and conjectured that $d_{o}(n)>d_{e}(n)$ for all $n>19$ where $d_{o}(n)$ (resp. $d_{e}(n)$) denote the number of partitions into distinct parts having more odd parts (resp. even parts) than even parts (resp. odd parts). In this paper we provide combinatorial proofs for both the result and the conjecture of Kim, Kim and Lovejoy. In addition, we show that if we restrict the smallest part of the partition to be $2$, then the parity bias is reversed. That is, if $q_{o}(n)$ (resp. $q_{e}(n)$) denote the number of partitions of $n$ with more odd parts (resp. even parts) than even parts (resp. odd parts) where the smallest part is at least $2$, then we have $q_o(n)<q_e(n)$ for all $n>7$. We also look at some more parity biases in partitions with restricted parts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.10590v2-abstract-full').style.display = 'none'; document.getElementById('2111.10590v2-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 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, revised based on referee reports</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 05A17; 05A20; 11P83 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> European Journal of Combinatorics, Volume 103, July 2022, 103522 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.10587">arXiv:2111.10587</a> <span> [<a href="https://arxiv.org/pdf/2111.10587">pdf</a>, <a href="https://arxiv.org/ps/2111.10587">ps</a>, <a href="https://arxiv.org/format/2111.10587">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Combinatorics">math.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/10.1142/S1793042122500592">10.1142/S1793042122500592 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Refinement of some partition identities of Merca and Yee </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Mahanta%2C+P+J">Pankaj Jyoti Mahanta</a>, <a href="/search/?searchtype=author&query=Saikia%2C+M+P">Manjil P. Saikia</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.10587v1-abstract-short" style="display: inline;"> Recently, Merca and Yee proved some partition identities involving two new partition statistics. We refine these statistics and generalize the results of Merca and Yee. We also correct a small mistake in a result of Merca and Yee. </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.10587v1-abstract-full" style="display: none;"> Recently, Merca and Yee proved some partition identities involving two new partition statistics. We refine these statistics and generalize the results of Merca and Yee. We also correct a small mistake in a result of Merca and Yee. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.10587v1-abstract-full').style.display = 'none'; document.getElementById('2111.10587v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, final version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 11P83; 11P84; 05A17; 05A19 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.10159">arXiv:2111.10159</a> <span> [<a href="https://arxiv.org/pdf/2111.10159">pdf</a>, <a href="https://arxiv.org/format/2111.10159">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/stab3395">10.1093/mnras/stab3395 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MeerKAT discovery of radio emission from the Vela X-1 bow shock </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Eijnden%2C+J+v+d">J. van den Eijnden</a>, <a href="/search/?searchtype=author&query=Heywood%2C+I">I. Heywood</a>, <a href="/search/?searchtype=author&query=Fender%2C+R">R. Fender</a>, <a href="/search/?searchtype=author&query=Mohamed%2C+S">S. Mohamed</a>, <a href="/search/?searchtype=author&query=Sivakoff%2C+G+R">G. R. Sivakoff</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">P. Saikia</a>, <a href="/search/?searchtype=author&query=Russell%2C+T+D">T. D. Russell</a>, <a href="/search/?searchtype=author&query=Motta%2C+S">S. Motta</a>, <a href="/search/?searchtype=author&query=Miller-Jones%2C+J+C+A">J. C. A. Miller-Jones</a>, <a href="/search/?searchtype=author&query=Woudt%2C+P+A">P. A. Woudt</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.10159v2-abstract-short" style="display: inline;"> Vela X-1 is a runaway X-ray binary system hosting a massive donor star, whose strong stellar wind creates a bow shock as it interacts with the interstellar medium. This bow shock has previously been detected in H$伪$ and IR, but, similar to all but one bow shock from a massive runaway star (BD+43$^{\rm o}$3654), has escaped detection in other wavebands. We report on the discovery of $1.3$ GHz radio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.10159v2-abstract-full').style.display = 'inline'; document.getElementById('2111.10159v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.10159v2-abstract-full" style="display: none;"> Vela X-1 is a runaway X-ray binary system hosting a massive donor star, whose strong stellar wind creates a bow shock as it interacts with the interstellar medium. This bow shock has previously been detected in H$伪$ and IR, but, similar to all but one bow shock from a massive runaway star (BD+43$^{\rm o}$3654), has escaped detection in other wavebands. We report on the discovery of $1.3$ GHz radio emission from the Vela X-1 bow shock with the MeerKAT telescope. The MeerKAT observations reveal how the radio emission closely traces the H$伪$ line emission, both in the bow shock and in the larger-scale diffuse structures known from existing H$伪$ surveys. The Vela X-1 bow shock is the first stellar-wind-driven radio bow shock detected around an X-ray binary. In the absence of a radio spectral index measurement, we explore other avenues to constrain the radio emission mechanism. We find that thermal/free-free emission can account for the radio and H$伪$ properties, for a combination of electron temperature and density consistent with earlier estimates of ISM density and the shock enhancement. In this explanation, the presence of a local ISM over-density is essential for the detection of radio emission. Alternatively, we consider a non-thermal/synchrotron scenario, evaluating the magnetic field and broad-band spectrum of the shock. However, we find that exceptionally high fractions ($\gtrsim 13$%) of the kinetic wind power would need to be injected into the relativistic electron population to explain the radio emission. Assuming lower fractions implies a hybrid scenario, dominated by free-free radio emission. Finally, we speculate about the detectability of radio bow shocks and whether it requires exceptional ISM or stellar wind properties. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.10159v2-abstract-full').style.display = 'none'; document.getElementById('2111.10159v2-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages including appendices, 12 figures; accepted for publication in MNRAS. Updated version with minor corrections to reference list</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.09077">arXiv:2111.09077</a> <span> [<a href="https://arxiv.org/pdf/2111.09077">pdf</a>, <a href="https://arxiv.org/format/2111.09077">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/stab3310">10.1093/mnras/stab3310 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LeMMINGs IV: The X-ray properties of a statistically-complete sample of the nuclei in active and inactive galaxies from the Palomar sample </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Williams%2C+D+R+A">D. R. A. Williams</a>, <a href="/search/?searchtype=author&query=Pahari%2C+M">M. Pahari</a>, <a href="/search/?searchtype=author&query=Baldi%2C+R+D">R. D. Baldi</a>, <a href="/search/?searchtype=author&query=McHardy%2C+I+M">I. M. McHardy</a>, <a href="/search/?searchtype=author&query=Mathur%2C+S">S. Mathur</a>, <a href="/search/?searchtype=author&query=Beswick%2C+R+J">R. J. Beswick</a>, <a href="/search/?searchtype=author&query=Beri%2C+A">A. Beri</a>, <a href="/search/?searchtype=author&query=Boorman%2C+P">P. Boorman</a>, <a href="/search/?searchtype=author&query=Aalto%2C+S">S. Aalto</a>, <a href="/search/?searchtype=author&query=Alberdi%2C+A">A. Alberdi</a>, <a href="/search/?searchtype=author&query=Argo%2C+M+K">M. K. Argo</a>, <a href="/search/?searchtype=author&query=Dullo%2C+B+T">B. T. Dullo</a>, <a href="/search/?searchtype=author&query=Fenech%2C+D+M">D. M. Fenech</a>, <a href="/search/?searchtype=author&query=Green%2C+D+A">D. A. Green</a>, <a href="/search/?searchtype=author&query=Knapen%2C+J+H">J. H. Knapen</a>, <a href="/search/?searchtype=author&query=Mart%C3%AD-Vidal%2C+I">I. Mart铆-Vidal</a>, <a href="/search/?searchtype=author&query=Moldon%2C+J">J. Moldon</a>, <a href="/search/?searchtype=author&query=Mundell%2C+C+G">C. G. Mundell</a>, <a href="/search/?searchtype=author&query=Muxlow%2C+T+W+B">T. W. B. Muxlow</a>, <a href="/search/?searchtype=author&query=Panessa%2C+F">F. Panessa</a>, <a href="/search/?searchtype=author&query=P%C3%A9rez-Torres%2C+M">M. P茅rez-Torres</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">P. Saikia</a>, <a href="/search/?searchtype=author&query=Shankar%2C+F">F. Shankar</a>, <a href="/search/?searchtype=author&query=Stevens%2C+I+R">I. R. Stevens</a>, <a href="/search/?searchtype=author&query=Uttley%2C+P">P. Uttley</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.09077v1-abstract-short" style="display: inline;"> All 280 of the statistically-complete Palomar sample of nearby (<120 Mpc) galaxies dec > 20 degrees have been observed at 1.5 GHz as part of the LeMMINGs e-MERLIN legacy survey. Here, we present Chandra X-ray observations of the nuclei of 213 of these galaxies, including a statistically-complete sub-set of 113 galaxies in the declination range 40 degrees to 65 degrees. We observed galaxies of all… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.09077v1-abstract-full').style.display = 'inline'; document.getElementById('2111.09077v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.09077v1-abstract-full" style="display: none;"> All 280 of the statistically-complete Palomar sample of nearby (<120 Mpc) galaxies dec > 20 degrees have been observed at 1.5 GHz as part of the LeMMINGs e-MERLIN legacy survey. Here, we present Chandra X-ray observations of the nuclei of 213 of these galaxies, including a statistically-complete sub-set of 113 galaxies in the declination range 40 degrees to 65 degrees. We observed galaxies of all optical spectral types, including 'active' galaxies (e.g., LINERs and Seyferts) and 'inactive' galaxies like HII galaxies and absorption line galaxies (ALG). The X-ray flux limit of our survey is 1.65$\times$10$^{-14}$~erg s$^{-1}$ cm$^{-2}$ (0.3$-$10 keV). We detect X-ray emission coincident within 2-arcsec of the nucleus in 150/213 galaxies, including 13/14 Seyferts, 68/77 LINERs, 13/22 ALGs and 56/100 HII galaxies, but cannot completely rule out contamination from non-AGN processes in sources with nuclear luminosities <10$^{39}$ erg s$^{-1}$. We construct an X-ray Luminosity function (XLF) and find that the local galaxy XLF, when including all AGN types, can be represented as a single power-law of slope $-0.54 \pm 0.06$. The Eddington ratio of the Seyferts is usually 2-4 decades higher than that of the LINERs, ALGs and HII galaxies, which are mostly detected with Eddington ratios <10$^{-3}$. Using [O III] line measurements and BH masses from the literature, we show that LINERs, HII galaxies and ALGs follow similar correlations to low luminosities, suggesting that some 'inactive' galaxies may harbour AGN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.09077v1-abstract-full').style.display = 'none'; document.getElementById('2111.09077v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages + 42 pages of online supplementary material 15 figures, 7 tables (additional 150 figures and 6 tables in online supplementary material) Accepted for publication in MNRAS, 15th November 2021</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.06205">arXiv:2109.06205</a> <span> [<a href="https://arxiv.org/pdf/2109.06205">pdf</a>, <a href="https://arxiv.org/format/2109.06205">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div 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/stab2613">10.1093/mnras/stab2613 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LeMMINGs. III. The e-MERLIN Legacy Survey of the Palomar sample. Exploring the origin of nuclear radio emission in active and inactive galaxies through the [O III] -- radio connection </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Baldi%2C+R+D">R. D. Baldi</a>, <a href="/search/?searchtype=author&query=Williams%2C+D+R+A">D. R. A. Williams</a>, <a href="/search/?searchtype=author&query=Beswick%2C+R+J">R. J. Beswick</a>, <a href="/search/?searchtype=author&query=McHardy%2C+I">I. McHardy</a>, <a href="/search/?searchtype=author&query=Dullo%2C+B+T">B. T. Dullo</a>, <a href="/search/?searchtype=author&query=Knapen%2C+J+H">J. H. Knapen</a>, <a href="/search/?searchtype=author&query=Zanisi%2C+L">L. Zanisi</a>, <a href="/search/?searchtype=author&query=Argo%2C+M+K">M. K. Argo</a>, <a href="/search/?searchtype=author&query=Aalto%2C+S">S. Aalto</a>, <a href="/search/?searchtype=author&query=Alberdi%2C+A">A. Alberdi</a>, <a href="/search/?searchtype=author&query=Baan%2C+W+A">W. A. Baan</a>, <a href="/search/?searchtype=author&query=Bendo%2C+G+J">G. J. Bendo</a>, <a href="/search/?searchtype=author&query=Fenech%2C+D+M">D. M. Fenech</a>, <a href="/search/?searchtype=author&query=Green%2C+D+A">D. A. Green</a>, <a href="/search/?searchtype=author&query=Kl%C3%B6ckner%2C+H+-">H. -R. Kl枚ckner</a>, <a href="/search/?searchtype=author&query=K%C3%B6rding%2C+E">E. K枚rding</a>, <a href="/search/?searchtype=author&query=Maccarone%2C+T+J">T. J. Maccarone</a>, <a href="/search/?searchtype=author&query=Marcaide%2C+J+M">J. M. Marcaide</a>, <a href="/search/?searchtype=author&query=Mutie%2C+I">I. Mutie</a>, <a href="/search/?searchtype=author&query=Panessa%2C+F">F. Panessa</a>, <a href="/search/?searchtype=author&query=P%C3%A9rez-Torres%2C+M+A">M. A. P茅rez-Torres</a>, <a href="/search/?searchtype=author&query=Romero-Ca%C3%B1izales%2C+C">C. Romero-Ca帽izales</a>, <a href="/search/?searchtype=author&query=Saikia%2C+D+J">D. J. Saikia</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">P. Saikia</a>, <a href="/search/?searchtype=author&query=Shankar%2C+F">F. Shankar</a> , et al. (9 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="2109.06205v1-abstract-short" style="display: inline;"> What determines the nuclear radio emission in local galaxies? We combine optical [O III] line emission, robust black hole (BH) mass estimates, and high-resolution e-MERLIN 1.5-GHz data, from the LeMMINGs survey, of a statistically-complete sample of 280 nearby, optically active (LINER and Seyfert) and inactive HII and Absorption line galaxies [ALG]) galaxies. Using [O III] luminosity (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.06205v1-abstract-full').style.display = 'inline'; document.getElementById('2109.06205v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.06205v1-abstract-full" style="display: none;"> What determines the nuclear radio emission in local galaxies? We combine optical [O III] line emission, robust black hole (BH) mass estimates, and high-resolution e-MERLIN 1.5-GHz data, from the LeMMINGs survey, of a statistically-complete sample of 280 nearby, optically active (LINER and Seyfert) and inactive HII and Absorption line galaxies [ALG]) galaxies. Using [O III] luminosity ($L_{\rm [O~III]}$) as a proxy for the accretion power, local galaxies follow distinct sequences in the optical-radio planes of BH activity, which suggest different origins of the nuclear radio emission for the optical classes. The 1.5-GHz radio luminosity of their parsec-scale cores ($L_{\rm core}$) is found to scale with BH mass ($M_{\rm BH}$) and [O~III] luminosity. Below $M_{\rm BH} \sim$10$^{6.5}$ M$_{\odot}$, stellar processes from non-jetted HII galaxies dominate with $L_{\rm core} \propto M_{\rm BH}^{0.61\pm0.33}$ and $L_{\rm core} \propto L_{\rm [O~III]}^{0.79\pm0.30}$. Above $M_{\rm BH} \sim$10$^{6.5}$ M$_{\odot}$, accretion-driven processes dominate with $L_{\rm core} \propto M_{\rm BH}^{1.5-1.65}$ and $L_{\rm core} \propto L_{\rm [O~III]}^{0.99-1.31}$ for active galaxies: radio-quiet/loud LINERs, Seyferts and jetted HII galaxies always display (although low) signatures of radio-emitting BH activity, with $L_{\rm 1.5\, GHz}\gtrsim$10$^{19.8}$ W Hz$^{-1}$ and $M_{\rm BH}\gtrsim10^{7}$ M$_{\odot}$, on a broad range of Eddington-scaled accretion rates ($\dot{m}$). Radio-quiet and radio-loud LINERs are powered by low-$\dot{m}$ discs launching sub-relativistic and relativistic jets, respectively. Low-power slow jets and disc/corona winds from moderately high to high-$\dot{m}$ discs account for the compact and edge-brightened jets of Seyferts, respectively. Jetted HII galaxies may host weakly active BHs. Fuel-starved BHs and recurrent activity account for ALG properties. [abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.06205v1-abstract-full').style.display = 'none'; document.getElementById('2109.06205v1-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">Accpeted for publication on MNRAS (27 pages, 9 Figures, 3 Tables, Appendix 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/2011.03062">arXiv:2011.03062</a> <span> [<a href="https://arxiv.org/pdf/2011.03062">pdf</a>, <a href="https://arxiv.org/format/2011.03062">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div 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/staa3519">10.1093/mnras/staa3519 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LeMMINGs. II. The e-MERLIN legacy survey of nearby galaxies. The deepest radio view of the Palomar sample on parsec scale </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Baldi%2C+R+D">R. D. Baldi</a>, <a href="/search/?searchtype=author&query=Williams%2C+D+R+A">D. R. A. Williams</a>, <a href="/search/?searchtype=author&query=McHardy%2C+I+M">I. M. McHardy</a>, <a href="/search/?searchtype=author&query=Beswick%2C+R+J">R. J. Beswick</a>, <a href="/search/?searchtype=author&query=Brinks%2C+E">E. Brinks</a>, <a href="/search/?searchtype=author&query=Dullo%2C+B+T">B. T. Dullo</a>, <a href="/search/?searchtype=author&query=Knapen%2C+J+H">J. H. Knapen</a>, <a href="/search/?searchtype=author&query=Argo%2C+M+K">M. K. Argo</a>, <a href="/search/?searchtype=author&query=Aalto%2C+S">S. Aalto</a>, <a href="/search/?searchtype=author&query=Alberdi%2C+A">A. Alberdi</a>, <a href="/search/?searchtype=author&query=Baan%2C+W+A">W. A. Baan</a>, <a href="/search/?searchtype=author&query=Bendo%2C+G+J">G. J. Bendo</a>, <a href="/search/?searchtype=author&query=Corbel%2C+S">S. Corbel</a>, <a href="/search/?searchtype=author&query=Fenech%2C+D+M">D. M. Fenech</a>, <a href="/search/?searchtype=author&query=Gallagher%2C+J+S">J. S. Gallagher</a>, <a href="/search/?searchtype=author&query=Green%2C+D+A">D. A. Green</a>, <a href="/search/?searchtype=author&query=Kennicutt%2C+R+C">R. C. Kennicutt</a>, <a href="/search/?searchtype=author&query=Kl%C3%B6ckner%2C+H+-">H. -R. Kl枚ckner</a>, <a href="/search/?searchtype=author&query=K%C3%B6rding%2C+E">E. K枚rding</a>, <a href="/search/?searchtype=author&query=Maccarone%2C+T+J">T. J. Maccarone</a>, <a href="/search/?searchtype=author&query=Muxlow%2C+T+W+B">T. W. B. Muxlow</a>, <a href="/search/?searchtype=author&query=Mundell%2C+C+G">C. G. Mundell</a>, <a href="/search/?searchtype=author&query=Panessa%2C+F">F. Panessa</a>, <a href="/search/?searchtype=author&query=Peck%2C+A+B">A. B. Peck</a>, <a href="/search/?searchtype=author&query=P%C3%A9rez-Torres%2C+M+A">M. A. P茅rez-Torres</a> , et al. (8 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="2011.03062v1-abstract-short" style="display: inline;"> We present the second data release of high-resolution ($\leq0.2$ arcsec) 1.5-GHz radio images of 177 nearby galaxies from the Palomar sample, observed with the e-MERLIN array, as part of the LeMMINGs (Legacy e-MERLIN Multi-band Imaging of Nearby Galaxy Sample) survey. Together with the 103 targets of the first LeMMINGs data release, this represents a complete sample of 280 local active (LINER and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.03062v1-abstract-full').style.display = 'inline'; document.getElementById('2011.03062v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.03062v1-abstract-full" style="display: none;"> We present the second data release of high-resolution ($\leq0.2$ arcsec) 1.5-GHz radio images of 177 nearby galaxies from the Palomar sample, observed with the e-MERLIN array, as part of the LeMMINGs (Legacy e-MERLIN Multi-band Imaging of Nearby Galaxy Sample) survey. Together with the 103 targets of the first LeMMINGs data release, this represents a complete sample of 280 local active (LINER and Seyfert) and inactive galaxies HII galaxies and Absorption Line Galaxies, ALG). This large program is the deepest radio survey of the local Universe, $\gtrsim$10$^{17.6}$ W Hz$^{-1}$, regardless of the host and nuclear type: we detect radio emission $\gtrsim$0.25 mJy beam$^{-1}$ for 125/280 galaxies (44.6 per cent) with sizes of typically $\lesssim$100 pc. Of those 125, 106 targets show a core which coincides within 1.2 arcsec with the optical nucleus. Although we observed mostly cores, around one third of the detected galaxies features jetted morphologies. The detected radio core luminosities of the sample range between $\sim$10$^{34}$ and 10$^{40}$ erg s$^{-1}$. LINERs and Seyferts are the most luminous sources, whereas HII galaxies are the least. LINERs show FRI-like core-brightened radio structures, while Seyferts reveal the highest fraction of symmetric morphologies. The majority of HII galaxies have single radio core or complex extended structures, which probably conceal a nuclear starburst and/or a weak active nucleus (seven of them show clear jets). ALGs, which are typically found in evolved ellipticals, although the least numerous, exhibit on average the most luminous radio structures, similar to LINERs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.03062v1-abstract-full').style.display = 'none'; document.getElementById('2011.03062v1-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 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">Accepted for publication on MNRAS (48 pages, 7 figures, 10 tables, Appendix)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.15176">arXiv:2010.15176</a> <span> [<a href="https://arxiv.org/pdf/2010.15176">pdf</a>, <a href="https://arxiv.org/ps/2010.15176">ps</a>, <a href="https://arxiv.org/format/2010.15176">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="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/10.3847/1538-4357/abc685">10.3847/1538-4357/abc685 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing jet launching in neutron star X-ray binaries: the variable and polarized jet of SAX J1808.4-3658 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Baglio%2C+M+C">M. C. Baglio</a>, <a href="/search/?searchtype=author&query=Russell%2C+D+M">D. M. Russell</a>, <a href="/search/?searchtype=author&query=Crespi%2C+S">S. Crespi</a>, <a href="/search/?searchtype=author&query=Covino%2C+S">S. Covino</a>, <a href="/search/?searchtype=author&query=Johar%2C+A">A. Johar</a>, <a href="/search/?searchtype=author&query=Homan%2C+J">J. Homan</a>, <a href="/search/?searchtype=author&query=Bramich%2C+D+M">D. M. Bramich</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">P. Saikia</a>, <a href="/search/?searchtype=author&query=Campana%2C+S">S. Campana</a>, <a href="/search/?searchtype=author&query=D%27Avanzo%2C+P">P. D'Avanzo</a>, <a href="/search/?searchtype=author&query=Fender%2C+R+P">R. P. Fender</a>, <a href="/search/?searchtype=author&query=Goldoni%2C+P">P. Goldoni</a>, <a href="/search/?searchtype=author&query=Goodwin%2C+A+J">A. J. Goodwin</a>, <a href="/search/?searchtype=author&query=Lewis%2C+F">F. Lewis</a>, <a href="/search/?searchtype=author&query=Masetti%2C+N">N. Masetti</a>, <a href="/search/?searchtype=author&query=Zanon%2C+A+M">A. Miraval Zanon</a>, <a href="/search/?searchtype=author&query=Motta%2C+S+E">S. E. Motta</a>, <a href="/search/?searchtype=author&query=Mu%C3%B1oz-Darias%2C+T">T. Mu帽oz-Darias</a>, <a href="/search/?searchtype=author&query=Shahbaz%2C+T">T. Shahbaz</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2010.15176v1-abstract-short" style="display: inline;"> We report on an optical photometric and polarimetric campaign on the accreting millisecond X-ray pulsar (AMXP) SAX J1808.4-3658 during its 2019 outburst. The emergence of a low-frequency excess in the spectral energy distribution in the form of a red excess above the disc spectrum (seen most prominently in z, i and R-bands) is observed as the outburst evolves. This is indicative of optically thin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.15176v1-abstract-full').style.display = 'inline'; document.getElementById('2010.15176v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.15176v1-abstract-full" style="display: none;"> We report on an optical photometric and polarimetric campaign on the accreting millisecond X-ray pulsar (AMXP) SAX J1808.4-3658 during its 2019 outburst. The emergence of a low-frequency excess in the spectral energy distribution in the form of a red excess above the disc spectrum (seen most prominently in z, i and R-bands) is observed as the outburst evolves. This is indicative of optically thin synchrotron emission due to a jet, as seen previously in this source and in other AMXPs during outburst. At the end of the outburst decay, the source entered a reflaring state. The low-frequency excess is still observed during the reflares. Our optical (BVRI) polarimetric campaign shows variable linear polarization (LP) throughout the outburst. We show that this is intrinsic to the source, with low-level but significant detections (0.2-2%) in all bands. The LP spectrum is red during both the main outburst and the reflaring state, favoring a jet origin for this variable polarization over other interpretations, such as Thomson scattering with free electrons from the disc or the propelled matter. During the reflaring state, a few episodes with stronger LP level (1-2 %) are observed. The low-level, variable LP is suggestive of strongly tangled magnetic fields near the base of the jet. These results clearly demonstrate how polarimetry is a powerful tool for probing the magnetic field structure in X-ray binary jets, similar to AGN jets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.15176v1-abstract-full').style.display = 'none'; document.getElementById('2010.15176v1-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 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.11096">arXiv:2008.11096</a> <span> [<a href="https://arxiv.org/pdf/2008.11096">pdf</a>, <a href="https://arxiv.org/ps/2008.11096">ps</a>, <a href="https://arxiv.org/format/2008.11096">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Number Theory">math.NT</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.jnt.2020.05.003">10.1016/j.jnt.2020.05.003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Some properties of Zumkeller numbers and $k$-layered numbers </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Mahanta%2C+P+J">Pankaj Jyoti Mahanta</a>, <a href="/search/?searchtype=author&query=Saikia%2C+M+P">Manjil P. Saikia</a>, <a href="/search/?searchtype=author&query=Yaqubi%2C+D">Daniel Yaqubi</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="2008.11096v1-abstract-short" style="display: inline;"> Generalizing the concept of a perfect number is a Zumkeller or integer perfect number that was introduced by Zumkeller in 2003. The positive integer $n$ is a Zumkeller number if its divisors can be partitioned into two sets with the same sum, which will be $蟽(n)/2$. Generalizing even further, we call $n$ a $k$-layered number if its divisors can be partitioned into $k$ sets with equal sum. In thi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.11096v1-abstract-full').style.display = 'inline'; document.getElementById('2008.11096v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.11096v1-abstract-full" style="display: none;"> Generalizing the concept of a perfect number is a Zumkeller or integer perfect number that was introduced by Zumkeller in 2003. The positive integer $n$ is a Zumkeller number if its divisors can be partitioned into two sets with the same sum, which will be $蟽(n)/2$. Generalizing even further, we call $n$ a $k$-layered number if its divisors can be partitioned into $k$ sets with equal sum. In this paper, we completely characterize Zumkeller numbers with two distinct prime factors and give some bounds for prime factorization in case of Zumkeller numbers with more than two distinct prime factors. We also characterize $k$-layered numbers with two distinct prime factors and even $k$-layered numbers with more than two distinct odd prime factors. Some other results concerning these numbers and their relationship with practical numbers and Harmonic mean numbers are also discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.11096v1-abstract-full').style.display = 'none'; document.getElementById('2008.11096v1-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 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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, accepted version, to appear in the Journal of Number Theory</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 11A25; 11B75; 11D99 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.04842">arXiv:2008.04842</a> <span> [<a href="https://arxiv.org/pdf/2008.04842">pdf</a>, <a href="https://arxiv.org/format/2008.04842">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Combinatorics">math.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Number Theory">math.NT</span> </div> </div> <p class="title is-5 mathjax"> Some New and Old Gibonacci Identities </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Mahanta%2C+P+J">Pankaj Jyoti Mahanta</a>, <a href="/search/?searchtype=author&query=Saikia%2C+M+P">Manjil P. Saikia</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="2008.04842v1-abstract-short" style="display: inline;"> We present a different combinatorial interpretations of Lucas and Gibonacci numbers. Using these interpretations we prove several new identities, and simplify the proofs of several known identities. Some open problems are discussed towards the end of the paper. </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.04842v1-abstract-full" style="display: none;"> We present a different combinatorial interpretations of Lucas and Gibonacci numbers. Using these interpretations we prove several new identities, and simplify the proofs of several known identities. Some open problems are discussed towards the end of the paper. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.04842v1-abstract-full').style.display = 'none'; document.getElementById('2008.04842v1-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 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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, comments are welcome</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 11B39; 11B37; 05A19; 05A15; 11B75 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.04841">arXiv:2008.04841</a> <span> [<a href="https://arxiv.org/pdf/2008.04841">pdf</a>, <a href="https://arxiv.org/format/2008.04841">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Combinatorics">math.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Number Theory">math.NT</span> </div> </div> <p class="title is-5 mathjax"> A family of lacunary recurrences for Lucas Numbers </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Mahanta%2C+P+J">Pankaj Jyoti Mahanta</a>, <a href="/search/?searchtype=author&query=Saikia%2C+M+P">Manjil P. Saikia</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="2008.04841v1-abstract-short" style="display: inline;"> We prove an infinite family of lacunary recurrences for the Lucas numbers using combinatorial means. </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.04841v1-abstract-full" style="display: none;"> We prove an infinite family of lacunary recurrences for the Lucas numbers using combinatorial means. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.04841v1-abstract-full').style.display = 'none'; document.getElementById('2008.04841v1-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 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">6 pages, accepted version, to appear in the Fibonacci Quarterly</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 05A19; 11B39; 11B37 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.08399">arXiv:2002.08399</a> <span> [<a href="https://arxiv.org/pdf/2002.08399">pdf</a>, <a href="https://arxiv.org/ps/2002.08399">ps</a>, <a href="https://arxiv.org/format/2002.08399">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/staa1182">10.1093/mnras/staa1182 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The appearance of a compact jet in the soft-intermediate state of 4U 1543-47 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Russell%2C+D+M">D. M. Russell</a>, <a href="/search/?searchtype=author&query=Casella%2C+P">P. Casella</a>, <a href="/search/?searchtype=author&query=Kalemci%2C+E">E. Kalemci</a>, <a href="/search/?searchtype=author&query=Motlagh%2C+A+V">A. Vahdat Motlagh</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">P. Saikia</a>, <a href="/search/?searchtype=author&query=Pirbhoy%2C+S+F">S. F. Pirbhoy</a>, <a href="/search/?searchtype=author&query=Maitra%2C+D">D. Maitra</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2002.08399v1-abstract-short" style="display: inline;"> Recent advancements in the understanding of jet-disc coupling in black hole candidate X-ray binaries (BHXBs) have provided close links between radio jet emission and X-ray spectral and variability behaviour. In 'soft' X-ray states the jets are suppressed, but the current picture lacks an understanding of the X-ray features associated with the quenching or recovering of these jets. Here we show tha… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.08399v1-abstract-full').style.display = 'inline'; document.getElementById('2002.08399v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.08399v1-abstract-full" style="display: none;"> Recent advancements in the understanding of jet-disc coupling in black hole candidate X-ray binaries (BHXBs) have provided close links between radio jet emission and X-ray spectral and variability behaviour. In 'soft' X-ray states the jets are suppressed, but the current picture lacks an understanding of the X-ray features associated with the quenching or recovering of these jets. Here we show that a brief, ~4 day infrared (IR) brightening during a predominantly soft X-ray state of the BHXB 4U 1543-47 is contemporaneous with a strong X-ray Type B quasi-periodic oscillation (QPO), a slight spectral hardening and an increase in the rms variability, indicating an excursion to the soft-intermediate state (SIMS). This IR 'flare' has a spectral index consistent with optically thin synchrotron emission and most likely originates from the steady, compact jet. This core jet emitting in the IR is usually only associated with the hard state, and its appearance during the SIMS places the 'jet line' between the SIMS and the soft state in the hardness-intensity diagram for this source. IR emission is produced in a small region of the jets close to where they are launched (~ 0.1 light-seconds), and the timescale of the IR flare in 4U 1543-47 is far too long to be caused by a single, discrete ejection. We also present a summary of the evolution of the jet and X-ray spectral/variability properties throughout the whole outburst, constraining the jet contribution to the X-ray flux during the decay. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.08399v1-abstract-full').style.display = 'none'; document.getElementById('2002.08399v1-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 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">Accepted to MNRAS. 11 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/1910.01151">arXiv:1910.01151</a> <span> [<a href="https://arxiv.org/pdf/1910.01151">pdf</a>, <a href="https://arxiv.org/format/1910.01151">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab4a09">10.3847/1538-4357/ab4a09 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Lorentz Factors of compact jets in Black hole X-ray binaries </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Saikia%2C+P">Payaswini Saikia</a>, <a href="/search/?searchtype=author&query=Russell%2C+D+M">David M. Russell</a>, <a href="/search/?searchtype=author&query=Bramich%2C+D+M">D. M. Bramich</a>, <a href="/search/?searchtype=author&query=Miller-Jones%2C+J+C+A">James C. A. Miller-Jones</a>, <a href="/search/?searchtype=author&query=Baglio%2C+M+C">Maria Cristina Baglio</a>, <a href="/search/?searchtype=author&query=Degenaar%2C+N">Nathalie Degenaar</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="1910.01151v1-abstract-short" style="display: inline;"> Compact, continuously launched jets in black hole X-ray binaries (BHXBs) produce radio to optical-infrared synchrotron emission. In most BHXBs, an infrared (IR) excess (above the disc component) is observed when the jet is present in the hard spectral state. We investigate why some BHXBs have prominent IR excesses and some do not, quantified by the amplitude of the IR quenching or recovery over th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.01151v1-abstract-full').style.display = 'inline'; document.getElementById('1910.01151v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.01151v1-abstract-full" style="display: none;"> Compact, continuously launched jets in black hole X-ray binaries (BHXBs) produce radio to optical-infrared synchrotron emission. In most BHXBs, an infrared (IR) excess (above the disc component) is observed when the jet is present in the hard spectral state. We investigate why some BHXBs have prominent IR excesses and some do not, quantified by the amplitude of the IR quenching or recovery over the transition from/to the hard state. We find that the amplitude of the IR excess can be explained by inclination dependent beaming of the jet synchrotron emission, and the projected area of the accretion disc. Furthermore, we see no correlation between the expected and the observed IR excess for Lorentz factor 1, which is strongly supportive of relativistic beaming of the IR emission, confirming that the IR excess is produced by synchrotron emission in a relativistic outflow. Using the amplitude of the jet fade and recovery over state transitions and the known orbital parameters, we constrain for the first time the bulk Lorentz factor range of compact jets in several BHXBs (with all the well-constrained Lorentz factors lying in the range of $螕$ = 1.3 - 3.5). Under the assumption that the Lorentz factor distribution of BHXB jets is a power-law, we find that N($螕$) $\propto 螕^{ -1.88^{+0.27}_{-0.34}}$. We also find that the very high amplitude IR fade/recovery seen repeatedly in the BHXB GX 339-4 favors a low inclination angle ($< 15^\circ$) of the jet. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.01151v1-abstract-full').style.display = 'none'; document.getElementById('1910.01151v1-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 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">23 pages, 10 figures; Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1907.12011">arXiv:1907.12011</a> <span> [<a href="https://arxiv.org/pdf/1907.12011">pdf</a>, <a href="https://arxiv.org/format/1907.12011">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Distributed, Parallel, and Cluster Computing">cs.DC</span> </div> </div> <p class="title is-5 mathjax"> Distributed Approximation Algorithms for Steiner Tree in the $\mathcal{CONGESTED}$ $\mathcal{CLIQUE}$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Saikia%2C+P">Parikshit Saikia</a>, <a href="/search/?searchtype=author&query=Karmakar%2C+S">Sushanta Karmakar</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="1907.12011v2-abstract-short" style="display: inline;"> The \emph{Steiner tree} problem is one of the fundamental and classical problems in combinatorial optimization. In this paper, we study this problem in the $\mathcal{CONGESTED}$ $\mathcal{CLIQUE}$ model of distributed computing and present two deterministic distributed approximation algorithms for the same. The first algorithm computes a Steiner tree in $\tilde{O}(n^{1/3})$ rounds and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.12011v2-abstract-full').style.display = 'inline'; document.getElementById('1907.12011v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1907.12011v2-abstract-full" style="display: none;"> The \emph{Steiner tree} problem is one of the fundamental and classical problems in combinatorial optimization. In this paper, we study this problem in the $\mathcal{CONGESTED}$ $\mathcal{CLIQUE}$ model of distributed computing and present two deterministic distributed approximation algorithms for the same. The first algorithm computes a Steiner tree in $\tilde{O}(n^{1/3})$ rounds and $\tilde{O}(n^{7/3})$ messages for a given connected undirected weighted graph of $n$ nodes. Note here that $\tilde{O}(\cdot)$ notation hides polylogarithmic factors in $n$. The second one computes a Steiner tree in $O(S + \log\log n)$ rounds and $O(S (n - t)^2 + n^2)$ messages, where $S$ and $t$ are the \emph{shortest path diameter} and the number of \emph{terminal} nodes respectively in the given input graph. Both the algorithms admit an approximation factor of $2(1 - 1/\ell)$, where $\ell$ is the number of terminal leaf nodes in the optimal Steiner tree. For graphs with $S = 蠅(n^{1/3} \log n)$, the first algorithm exhibits better performance than the second one in terms of the round complexity. On the other hand, for graphs with $S = \tilde{o}(n^{1/3})$, the second algorithm outperforms the first one in terms of the round complexity. In fact when $S = O(\log\log n)$ then the second algorithm admits a round complexity of $O(\log\log n)$ and message complexity of $\tilde{O}(n^2)$. To the best of our knowledge, this is the first work to study the Steiner tree problem in the $\mathcal{CONGESTED}$ $\mathcal{CLIQUE}$ model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.12011v2-abstract-full').style.display = 'none'; document.getElementById('1907.12011v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 July, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 July, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">22 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/1906.09947">arXiv:1906.09947</a> <span> [<a href="https://arxiv.org/pdf/1906.09947">pdf</a>, <a href="https://arxiv.org/ps/1906.09947">ps</a>, <a href="https://arxiv.org/format/1906.09947">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Number Theory">math.NT</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/10.1142/S1793557120501260">10.1142/S1793557120501260 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On Deficient Perfect Numbers with Four Distinct Prime Factors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Dutta%2C+P">Parama Dutta</a>, <a href="/search/?searchtype=author&query=Saikia%2C+M+P">Manjil P. Saikia</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="1906.09947v1-abstract-short" style="display: inline;"> For a positive integer $n$, if $蟽(n)$ denotes the sum of the positive divisors of $n$, then $n$ is called a deficient perfect number if $蟽(n)=2n-d$ for some positive divisor $d$ of $n$. In this paper, we prove some results about odd deficient perfect numbers with four distinct prime factors. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1906.09947v1-abstract-full" style="display: none;"> For a positive integer $n$, if $蟽(n)$ denotes the sum of the positive divisors of $n$, then $n$ is called a deficient perfect number if $蟽(n)=2n-d$ for some positive divisor $d$ of $n$. In this paper, we prove some results about odd deficient perfect numbers with four distinct prime factors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.09947v1-abstract-full').style.display = 'none'; document.getElementById('1906.09947v1-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 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">11 pages, preprint version (journal version may differ). To appear in Asian-European Journal of Mathematics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> Primary 11A25; Secondary 11A41; 11B99 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1906.07723">arXiv:1906.07723</a> <span> [<a href="https://arxiv.org/pdf/1906.07723">pdf</a>, <a href="https://arxiv.org/format/1906.07723">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Combinatorics">math.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Mathematical Physics">math-ph</span> </div> </div> <p class="title is-5 mathjax"> Refined Enumeration of Symmetry Classes of Alternating Sign Matrices </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fischer%2C+I">Ilse Fischer</a>, <a href="/search/?searchtype=author&query=Saikia%2C+M+P">Manjil P. Saikia</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="1906.07723v1-abstract-short" style="display: inline;"> We prove refined enumeration results on several symmetry classes as well as related classes of alternating sign matrices with respect to classical boundary statistics, using the six-vertex model of statistical physics. More precisely, we study vertically symmetric, vertically and horizontally symmetric, vertically and horizontally perverse, off-diagonally and off-antidiagonally symmetric, vertical… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.07723v1-abstract-full').style.display = 'inline'; document.getElementById('1906.07723v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1906.07723v1-abstract-full" style="display: none;"> We prove refined enumeration results on several symmetry classes as well as related classes of alternating sign matrices with respect to classical boundary statistics, using the six-vertex model of statistical physics. More precisely, we study vertically symmetric, vertically and horizontally symmetric, vertically and horizontally perverse, off-diagonally and off-antidiagonally symmetric, vertically and off-diagonally symmetric, quarter turn symmetric as well as quasi quarter turn symmetric alternating sign matrices. Our results prove conjectures of Fischer, Duchon and Robbins. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.07723v1-abstract-full').style.display = 'none'; document.getElementById('1906.07723v1-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 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">42 pages, 19 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 05A05; 05A15; 05A19; 05E05; 15B35; 52C20; 82B20; 82B23 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1905.13294">arXiv:1905.13294</a> <span> [<a href="https://arxiv.org/pdf/1905.13294">pdf</a>, <a href="https://arxiv.org/format/1905.13294">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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"> A Review of Deep Learning with Special Emphasis on Architectures, Applications and Recent Trends </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Sengupta%2C+S">Saptarshi Sengupta</a>, <a href="/search/?searchtype=author&query=Basak%2C+S">Sanchita Basak</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">Pallabi Saikia</a>, <a href="/search/?searchtype=author&query=Paul%2C+S">Sayak Paul</a>, <a href="/search/?searchtype=author&query=Tsalavoutis%2C+V">Vasilios Tsalavoutis</a>, <a href="/search/?searchtype=author&query=Atiah%2C+F">Frederick Atiah</a>, <a href="/search/?searchtype=author&query=Ravi%2C+V">Vadlamani Ravi</a>, <a href="/search/?searchtype=author&query=Peters%2C+A">Alan Peters</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="1905.13294v3-abstract-short" style="display: inline;"> Deep learning has solved a problem that as little as five years ago was thought by many to be intractable - the automatic recognition of patterns in data; and it can do so with accuracy that often surpasses human beings. It has solved problems beyond the realm of traditional, hand-crafted machine learning algorithms and captured the imagination of practitioners trying to make sense out of the floo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.13294v3-abstract-full').style.display = 'inline'; document.getElementById('1905.13294v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1905.13294v3-abstract-full" style="display: none;"> Deep learning has solved a problem that as little as five years ago was thought by many to be intractable - the automatic recognition of patterns in data; and it can do so with accuracy that often surpasses human beings. It has solved problems beyond the realm of traditional, hand-crafted machine learning algorithms and captured the imagination of practitioners trying to make sense out of the flood of data that now inundates our society. As public awareness of the efficacy of DL increases so does the desire to make use of it. But even for highly trained professionals it can be daunting to approach the rapidly increasing body of knowledge produced by experts in the field. Where does one start? How does one determine if a particular model is applicable to their problem? How does one train and deploy such a network? A primer on the subject can be a good place to start. With that in mind, we present an overview of some of the key multilayer ANNs that comprise DL. We also discuss some new automatic architecture optimization protocols that use multi-agent approaches. Further, since guaranteeing system uptime is becoming critical to many computer applications, we include a section on using neural networks for fault detection and subsequent mitigation. This is followed by an exploratory survey of several application areas where DL has emerged as a game-changing technology: anomalous behavior detection in financial applications or in financial time-series forecasting, predictive and prescriptive analytics, medical image processing and analysis and power systems research. The thrust of this review is to outline emerging areas of application-oriented research within the DL community as well as to provide a reference to researchers seeking to use it in their work for what it does best: statistical pattern recognition with unparalleled learning capacity with the ability to scale with information. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.13294v3-abstract-full').style.display = 'none'; document.getElementById('1905.13294v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 July, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">29 pages, 11 figures, 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/1807.08762">arXiv:1807.08762</a> <span> [<a href="https://arxiv.org/pdf/1807.08762">pdf</a>, <a href="https://arxiv.org/ps/1807.08762">ps</a>, <a href="https://arxiv.org/format/1807.08762">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="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/10.3847/1538-4357/aae532">10.3847/1538-4357/aae532 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A wildly flickering jet in the black hole X-ray binary MAXI J1535-571 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Baglio%2C+M+C">M. C. Baglio</a>, <a href="/search/?searchtype=author&query=Russell%2C+D+M">D. M. Russell</a>, <a href="/search/?searchtype=author&query=Casella%2C+P">P. Casella</a>, <a href="/search/?searchtype=author&query=Noori%2C+H+A">H. Al Noori</a>, <a href="/search/?searchtype=author&query=Yazeedi%2C+A+A">A. Al Yazeedi</a>, <a href="/search/?searchtype=author&query=Belloni%2C+T">T. Belloni</a>, <a href="/search/?searchtype=author&query=Buckley%2C+D+A+H">D. A. H. Buckley</a>, <a href="/search/?searchtype=author&query=Bel%2C+M+C">M. Cadolle Bel</a>, <a href="/search/?searchtype=author&query=Ceccobello%2C+C">C. Ceccobello</a>, <a href="/search/?searchtype=author&query=Corbel%2C+S">S. Corbel</a>, <a href="/search/?searchtype=author&query=Zelati%2C+F+C">F. Coti Zelati</a>, <a href="/search/?searchtype=author&query=Trigo%2C+M+D">M. Diaz Trigo</a>, <a href="/search/?searchtype=author&query=Fender%2C+R+P">R. P. Fender</a>, <a href="/search/?searchtype=author&query=Gallo%2C+E">E. Gallo</a>, <a href="/search/?searchtype=author&query=Gandhi%2C+P">P. Gandhi</a>, <a href="/search/?searchtype=author&query=Homan%2C+J">J. Homan</a>, <a href="/search/?searchtype=author&query=koljonen%2C+K+I+I">K. I. I. koljonen</a>, <a href="/search/?searchtype=author&query=lewis%2C+F">F. lewis</a>, <a href="/search/?searchtype=author&query=Maccarone%2C+T+J">T. J. Maccarone</a>, <a href="/search/?searchtype=author&query=Malzac%2C+J">J. Malzac</a>, <a href="/search/?searchtype=author&query=Markoff%2C+S">S. Markoff</a>, <a href="/search/?searchtype=author&query=Miller-Jones%2C+J+C+A">J. C. A. Miller-Jones</a>, <a href="/search/?searchtype=author&query=O%27Brien%2C+K">K. O'Brien</a>, <a href="/search/?searchtype=author&query=Russell%2C+T+D">T. D. Russell</a>, <a href="/search/?searchtype=author&query=Saikia%2C+P">P. Saikia</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1807.08762v2-abstract-short" style="display: inline;"> We report on the results of optical, near-infrared (NIR) and mid-infrared observations of the black hole X-ray binary candidate (BHB) MAXI J1535-571 during its 2017/2018 outburst. During the first part of the outburst (MJD 58004-58012), the source shows an optical-NIR spectrum that is consistent with an optically thin synchrotron power-law from a jet. After MJD 58015, however, the source faded con… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.08762v2-abstract-full').style.display = 'inline'; document.getElementById('1807.08762v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1807.08762v2-abstract-full" style="display: none;"> We report on the results of optical, near-infrared (NIR) and mid-infrared observations of the black hole X-ray binary candidate (BHB) MAXI J1535-571 during its 2017/2018 outburst. During the first part of the outburst (MJD 58004-58012), the source shows an optical-NIR spectrum that is consistent with an optically thin synchrotron power-law from a jet. After MJD 58015, however, the source faded considerably, the drop in flux being much more evident at lower frequencies. Before the fading, we measure a de-reddened flux density of $\gtrsim$100 mJy in the mid-infrared, making MAXI J1535-571 one of the brightest mid-infrared BHBs known so far. A significant softening of the X-ray spectrum is evident contemporaneous with the infrared fade. We interpret it as due to the suppression of the jet emission, similar to the accretion-ejection coupling seen in other BHBs. However, MAXI J1535-571 did not transition smoothly to the soft state, instead showing X-ray hardness deviations, associated with infrared flaring. We also present the first mid-IR variability study of a BHB on minute timescales, with a fractional rms variability of the light curves of $\sim 15-22 \%$, which is similar to that expected from the internal shock jet model, and much higher than the optical fractional rms ($\lesssim 7 \%$). These results represent an excellent case of multi-wavelength jet spectral-timing and demonstrate how rich, multi-wavelength time-resolved data of X-ray binaries over accretion state transitions can help refining models of the disk-jet connection and jet launching in these systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.08762v2-abstract-full').style.display = 'none'; document.getElementById('1807.08762v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 September, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">20 pages, 8 figures. Accepted for publication in the ApJ</span> </p> </li> </ol> <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=Saikia%2C+P&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Saikia%2C+P&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Saikia%2C+P&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> 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