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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Galloway%2C+D+K&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Galloway%2C+D+K&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Galloway%2C+D+K&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Galloway%2C+D+K&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </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/2411.03272">arXiv:2411.03272</a> <span> [<a href="https://arxiv.org/pdf/2411.03272">pdf</a>, <a href="https://arxiv.org/format/2411.03272">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"> Optical evolution of AT 2024wpp: the high-velocity outflows in Cow-like transients are consistent with high spherical symmetry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pursiainen%2C+M">M. Pursiainen</a>, <a href="/search/astro-ph?searchtype=author&query=Killestein%2C+T+L">T. L. Killestein</a>, <a href="/search/astro-ph?searchtype=author&query=Kuncarayakti%2C+H">H. Kuncarayakti</a>, <a href="/search/astro-ph?searchtype=author&query=Charalampopoulos%2C+P">P. Charalampopoulos</a>, <a href="/search/astro-ph?searchtype=author&query=Lyman%2C+J">J. Lyman</a>, <a href="/search/astro-ph?searchtype=author&query=Kotak%2C+R">R. Kotak</a>, <a href="/search/astro-ph?searchtype=author&query=Leloudas%2C+G">G. Leloudas</a>, <a href="/search/astro-ph?searchtype=author&query=Coppejans%2C+D">D. Coppejans</a>, <a href="/search/astro-ph?searchtype=author&query=Kravtsov%2C+T">T. Kravtsov</a>, <a href="/search/astro-ph?searchtype=author&query=Maeda%2C+K">K. Maeda</a>, <a href="/search/astro-ph?searchtype=author&query=Nagao%2C+T">T. Nagao</a>, <a href="/search/astro-ph?searchtype=author&query=Taguchi%2C+K">K. Taguchi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Dhillon%2C+V+S">V. S. Dhillon</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+A">A. Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Neill%2C+D">D. O'Neill</a>, <a href="/search/astro-ph?searchtype=author&query=Steeghs%2C+D">D. Steeghs</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="2411.03272v1-abstract-short" style="display: inline;"> We present the analysis of optical data of a bright and extremely-rapidly evolving transient, AT2024wpp, whose properties are similar to the enigmatic AT2018cow (aka the Cow). AT2024wpp rose to a peak brightness of c=-21.9mag in 4.3d and remained above the half-maximum brightness for only 6.7d. The blackbody fits to the multi-band photometry show that the event remained persistently hot (T>20000K)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.03272v1-abstract-full').style.display = 'inline'; document.getElementById('2411.03272v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.03272v1-abstract-full" style="display: none;"> We present the analysis of optical data of a bright and extremely-rapidly evolving transient, AT2024wpp, whose properties are similar to the enigmatic AT2018cow (aka the Cow). AT2024wpp rose to a peak brightness of c=-21.9mag in 4.3d and remained above the half-maximum brightness for only 6.7d. The blackbody fits to the multi-band photometry show that the event remained persistently hot (T>20000K) with a rapidly receding photosphere (v~11500km/s) until the end of the photometric dataset at +16.1d post-discovery. This behaviour mimics that of AT2018cow, albeit with a several times larger photosphere. The spectra are consistent with blackbody emission throughout our spectral sequence ending at +21.9d, showing a tentative, very broad emission feature at 5500脜 -- implying that the optical photosphere is likely within a near-relativistic outflow. Furthermore, reports of strong X-ray and radio emission cement the nature of AT2024wpp as a likely Cow-like transient. AT2024wpp is only the second event of the class with optical polarimetry. Our BVRI observations obtained from +6.1 to +14.4d show a low polarisation of P<0.5% across all bands, similar to AT2018cow that was consistent with P~0% during the same outflow-driven phase. In the absence of evidence for a preferential viewing angle, it is unlikely that both events would have shown low polarisation in the case that their photospheres were aspherical. As such, we conclude that the near-relativistic outflows launched in these events are likely highly spherical, but polarimetric observations of further events are crucial to constrain their ejecta geometry and stratification in detail. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.03272v1-abstract-full').style.display = 'none'; document.getElementById('2411.03272v1-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, 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">10 pages, 6 figures. Submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.14147">arXiv:2409.14147</a> <span> [<a href="https://arxiv.org/pdf/2409.14147">pdf</a>, <a href="https://arxiv.org/format/2409.14147">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"> SN 2023tsz: A helium-interaction driven supernova in a very low-mass galaxy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Warwick%2C+B">B. Warwick</a>, <a href="/search/astro-ph?searchtype=author&query=Lyman%2C+J">J. Lyman</a>, <a href="/search/astro-ph?searchtype=author&query=Pursiainen%2C+M">M. Pursiainen</a>, <a href="/search/astro-ph?searchtype=author&query=Coppejans%2C+D+L">D. L. Coppejans</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+G+T">G. T. Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Killestein%2C+T+L">T. L. Killestein</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+A">A. Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Oates%2C+S+R">S. R. Oates</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J+P">J. P. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Aryan%2C+A">A. Aryan</a>, <a href="/search/astro-ph?searchtype=author&query=Breton%2C+R+P">R. P. Breton</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+T+W">T. W. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Clark%2C+P">P. Clark</a>, <a href="/search/astro-ph?searchtype=author&query=Dhillon%2C+V+S">V. S. Dhillon</a>, <a href="/search/astro-ph?searchtype=author&query=Dyer%2C+M+J">M. J. Dyer</a>, <a href="/search/astro-ph?searchtype=author&query=Gal-Yam%2C+A">A. Gal-Yam</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Guti%C3%A9rrez%2C+C+P">C. P. Guti茅rrez</a>, <a href="/search/astro-ph?searchtype=author&query=Gromadzki%2C+M">M. Gromadzki</a>, <a href="/search/astro-ph?searchtype=author&query=Inserra%2C+C">C. Inserra</a>, <a href="/search/astro-ph?searchtype=author&query=Jim%C3%A9nez-Ibarra%2C+F">F. Jim茅nez-Ibarra</a>, <a href="/search/astro-ph?searchtype=author&query=Kelsey%2C+L">L. Kelsey</a>, <a href="/search/astro-ph?searchtype=author&query=Kotak%2C+R">R. Kotak</a> , et al. (27 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="2409.14147v1-abstract-short" style="display: inline;"> SN 2023tsz is a Type Ibn supernova (SNe Ibn) discovered in an extremely low-mass host. SNe Ibn are an uncommon subtype of stripped-envelope core-collapse SNe. They are characterised by narrow helium emission lines in their spectra and are believed to originate from the collapse of massive Wolf-Rayet (WR) stars, though their progenitor systems still remain poorly understood. In terms of energetics… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.14147v1-abstract-full').style.display = 'inline'; document.getElementById('2409.14147v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.14147v1-abstract-full" style="display: none;"> SN 2023tsz is a Type Ibn supernova (SNe Ibn) discovered in an extremely low-mass host. SNe Ibn are an uncommon subtype of stripped-envelope core-collapse SNe. They are characterised by narrow helium emission lines in their spectra and are believed to originate from the collapse of massive Wolf-Rayet (WR) stars, though their progenitor systems still remain poorly understood. In terms of energetics and spectrophotometric evolution, SN 2023tsz is largely a typical example of the class, although line profile asymmetries in the nebular phase are seen, which may indicate the presence of dust formation or unshocked circumstellar material. Intriguingly, SN 2023tsz is located in an extraordinarily low-mass host galaxy that is in the 2nd percentile for SESN host masses and star formation rates (SFR). The host has a radius of 1.0 kpc, a $g$-band absolute magnitude of $-12.73$, and an estimated metallicity of $\log(Z_{*}/Z_{\odot}$) = $-1.56$. The SFR and metallicity of the host galaxy raise questions about the progenitor of SN 2023tsz. The low SFR suggests that a star with sufficient mass to evolve into a WR would be uncommon in this galaxy. Further, the very low-metallicity is a challenge for single stellar evolution to enable H and He stripping of the progenitor and produce a SN Ibn explosion. The host galaxy of SN 2023tsz adds another piece to the ongoing puzzle of SNe Ibn progenitors, and demonstrates that they can occur in hosts too faint to be observed in contemporary sky surveys at a more typical SN Ibn redshift. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.14147v1-abstract-full').style.display = 'none'; document.getElementById('2409.14147v1-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, 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">14 pages, 10 figures, submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.17176">arXiv:2407.17176</a> <span> [<a href="https://arxiv.org/pdf/2407.17176">pdf</a>, <a href="https://arxiv.org/format/2407.17176">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> The Gravitational-wave Optical Transient Observer (GOTO) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dyer%2C+M+J">Martin J. Dyer</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">Kendall Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Jim%C3%A9nez-Ibarra%2C+F">Felipe Jim茅nez-Ibarra</a>, <a href="/search/astro-ph?searchtype=author&query=Lyman%2C+J">Joseph Lyman</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">Krzysztof Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Steeghs%2C+D">Danny Steeghs</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">Duncan K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Dhillon%2C+V+S">Vik S. Dhillon</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Brien%2C+P">Paul O'Brien</a>, <a href="/search/astro-ph?searchtype=author&query=Ramsay%2C+G">Gavin Ramsay</a>, <a href="/search/astro-ph?searchtype=author&query=Noysena%2C+K">Kanthanakorn Noysena</a>, <a href="/search/astro-ph?searchtype=author&query=Kotak%2C+R">Rubina Kotak</a>, <a href="/search/astro-ph?searchtype=author&query=Breton%2C+R">Rene Breton</a>, <a href="/search/astro-ph?searchtype=author&query=Nuttall%2C+L">Laura Nuttall</a>, <a href="/search/astro-ph?searchtype=author&query=Pall%C3%A9%2C+E">Enric Pall茅</a>, <a href="/search/astro-ph?searchtype=author&query=Pollacco%2C+D">Don Pollacco</a>, <a href="/search/astro-ph?searchtype=author&query=Killestein%2C+T">Tom Killestein</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+A">Amit Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Neill%2C+D">David O'Neill</a>, <a href="/search/astro-ph?searchtype=author&query=Kelsey%2C+L">Lisa Kelsey</a>, <a href="/search/astro-ph?searchtype=author&query=Godson%2C+B">Ben Godson</a>, <a href="/search/astro-ph?searchtype=author&query=Jarvis%2C+D">Dan Jarvis</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="2407.17176v1-abstract-short" style="display: inline;"> The Gravitational-wave Optical Transient Observer (GOTO) is a project dedicated to identifying optical counter-parts to gravitational-wave detections using a network of dedicated, wide-field telescopes. After almost a decade of design, construction, and commissioning work, the GOTO network is now fully operational with two antipodal sites: La Palma in the Canary Islands and Siding Spring in Austra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.17176v1-abstract-full').style.display = 'inline'; document.getElementById('2407.17176v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.17176v1-abstract-full" style="display: none;"> The Gravitational-wave Optical Transient Observer (GOTO) is a project dedicated to identifying optical counter-parts to gravitational-wave detections using a network of dedicated, wide-field telescopes. After almost a decade of design, construction, and commissioning work, the GOTO network is now fully operational with two antipodal sites: La Palma in the Canary Islands and Siding Spring in Australia. Both sites host two independent robotic mounts, each with a field-of-view of 44 square degrees formed by an array of eight 40 cm telescopes, resulting in an instantaneous 88 square degree field-of-view per site. All four telescopes operate as a single integrated network, with the ultimate aim of surveying the entire sky every 2-3 days and allowing near-24-hour response to transient events within a minute of their detection. In the modern era of transient astronomy, automated telescopes like GOTO form a vital link between multi-messenger discovery facilities and in-depth follow-up by larger telescopes. GOTO is already producing a wide range of scientific results, assisted by an efficient discovery pipeline and a successful citizen science project: Kilonova Seekers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.17176v1-abstract-full').style.display = 'none'; document.getElementById('2407.17176v1-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 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, 5 figures, submitted to SPIE Astronomical Telescopes + Instrumentation 2024</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.02334">arXiv:2406.02334</a> <span> [<a href="https://arxiv.org/pdf/2406.02334">pdf</a>, <a href="https://arxiv.org/format/2406.02334">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"> $\textit{Kilonova Seekers}$: the GOTO project for real-time citizen science in time-domain astrophysics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Killestein%2C+T+L">T. L. Killestein</a>, <a href="/search/astro-ph?searchtype=author&query=Kelsey%2C+L">L. Kelsey</a>, <a href="/search/astro-ph?searchtype=author&query=Wickens%2C+E">E. Wickens</a>, <a href="/search/astro-ph?searchtype=author&query=Nuttall%2C+L">L. Nuttall</a>, <a href="/search/astro-ph?searchtype=author&query=Lyman%2C+J">J. Lyman</a>, <a href="/search/astro-ph?searchtype=author&query=Krawczyk%2C+C">C. Krawczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Dyer%2C+M+J">M. J. Dyer</a>, <a href="/search/astro-ph?searchtype=author&query=Jim%C3%A9nez-Ibarra%2C+F">F. Jim茅nez-Ibarra</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Neill%2C+D">D. O'Neill</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+A">A. Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Steeghs%2C+D">D. Steeghs</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Dhillon%2C+V+S">V. S. Dhillon</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Brien%2C+P">P. O'Brien</a>, <a href="/search/astro-ph?searchtype=author&query=Ramsay%2C+G">G. Ramsay</a>, <a href="/search/astro-ph?searchtype=author&query=Noysena%2C+K">K. Noysena</a>, <a href="/search/astro-ph?searchtype=author&query=Kotak%2C+R">R. Kotak</a>, <a href="/search/astro-ph?searchtype=author&query=Breton%2C+R+P">R. P. Breton</a>, <a href="/search/astro-ph?searchtype=author&query=Pall%C3%A9%2C+E">E. Pall茅</a>, <a href="/search/astro-ph?searchtype=author&query=Pollacco%2C+D">D. Pollacco</a>, <a href="/search/astro-ph?searchtype=author&query=Awiphan%2C+S">S. Awiphan</a>, <a href="/search/astro-ph?searchtype=author&query=Belkin%2C+S">S. Belkin</a>, <a href="/search/astro-ph?searchtype=author&query=Chote%2C+P">P. Chote</a> , et al. (29 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="2406.02334v2-abstract-short" style="display: inline;"> Time-domain astrophysics continues to grow rapidly, with the inception of new surveys drastically increasing data volumes. Democratised, distributed approaches to training sets for machine learning classifiers are crucial to make the most of this torrent of discovery -- with citizen science approaches proving effective at meeting these requirements. In this paper, we describe the creation of and t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.02334v2-abstract-full').style.display = 'inline'; document.getElementById('2406.02334v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.02334v2-abstract-full" style="display: none;"> Time-domain astrophysics continues to grow rapidly, with the inception of new surveys drastically increasing data volumes. Democratised, distributed approaches to training sets for machine learning classifiers are crucial to make the most of this torrent of discovery -- with citizen science approaches proving effective at meeting these requirements. In this paper, we describe the creation of and the initial results from the $\textit{Kilonova Seekers}$ citizen science project, built to find transient phenomena from the GOTO telescopes in near real-time. $\textit{Kilonova Seekers}$ launched in July 2023 and received over 600,000 classifications from approximately 2,000 volunteers over the course of the LIGO-Virgo-KAGRA O4a observing run. During this time, the project has yielded 20 discoveries, generated a `gold-standard' training set of 17,682 detections for augmenting deep-learned classifiers, and measured the performance and biases of Zooniverse volunteers on real-bogus classification. This project will continue throughout the lifetime of GOTO, pushing candidates at ever-greater cadence, and directly facilitate the next-generation classification algorithms currently in development. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.02334v2-abstract-full').style.display = 'none'; document.getElementById('2406.02334v2-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">20 pages, 15 figures. Accepted 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/2405.10717">arXiv:2405.10717</a> <span> [<a href="https://arxiv.org/pdf/2405.10717">pdf</a>, <a href="https://arxiv.org/format/2405.10717">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"> Constraining the Properties of the Thermonuclear Burst Oscillation Source XTE J1814-338 Through Pulse Profile Modelling </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kini%2C+Y">Yves Kini</a>, <a href="/search/astro-ph?searchtype=author&query=Salmi%2C+T">Tuomo Salmi</a>, <a href="/search/astro-ph?searchtype=author&query=Vinciguerra%2C+S">Serena Vinciguerra</a>, <a href="/search/astro-ph?searchtype=author&query=Watts%2C+A+L">Anna L. Watts</a>, <a href="/search/astro-ph?searchtype=author&query=Bilous%2C+A">Anna Bilous</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">Duncan K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Wateren%2C+E">Emma van der Wateren</a>, <a href="/search/astro-ph?searchtype=author&query=Khalsa%2C+G+P">Guru Partap Khalsa</a>, <a href="/search/astro-ph?searchtype=author&query=Bogdanov%2C+S">Slavko Bogdanov</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">Johannes Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Suleimanov%2C+V">Valery Suleimanov</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="2405.10717v2-abstract-short" style="display: inline;"> Pulse profile modelling (PPM) is a comprehensive relativistic ray-tracing technique employed to determine the properties of neutron stars. In this study, we apply this technique to the Type I X-ray burster and accretion-powered millisecond pulsar XTE J1814-338, extracting its fundamental properties using PPM of its thermonuclear burst oscillations. Using data from its 2003 outburst, and a single u… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.10717v2-abstract-full').style.display = 'inline'; document.getElementById('2405.10717v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.10717v2-abstract-full" style="display: none;"> Pulse profile modelling (PPM) is a comprehensive relativistic ray-tracing technique employed to determine the properties of neutron stars. In this study, we apply this technique to the Type I X-ray burster and accretion-powered millisecond pulsar XTE J1814-338, extracting its fundamental properties using PPM of its thermonuclear burst oscillations. Using data from its 2003 outburst, and a single uniform temperature hot spot model, we infer XTE J1814-338 to be located at a distance of $7.2^{+0.3}_{-0.4}$ kpc, with a mass of $1.21^{+0.05}_{-0.05}$ M$_\odot$ and an equatorial radius of $7.0^{+0.4}_{-0.4}$ km. Our results also offer insight into the time evolution of the hot spot but point to some potential shortcomings of the single uniform temperature hot spot model. We explore the implications of this result, including what we can learn about thermonuclear burst oscillation mechanisms and the importance of modelling the accretion contribution to the emission during the burst. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.10717v2-abstract-full').style.display = 'none'; document.getElementById('2405.10717v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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. The Zenodo link is public</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.16471">arXiv:2403.16471</a> <span> [<a href="https://arxiv.org/pdf/2403.16471">pdf</a>, <a href="https://arxiv.org/format/2403.16471">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"> Inferring system parameters from the bursts of the accretion-powered pulsar IGR J17498-2921 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Goodwin%2C+A+J">A. J. Goodwin</a>, <a href="/search/astro-ph?searchtype=author&query=Hilder%2C+T">T. Hilder</a>, <a href="/search/astro-ph?searchtype=author&query=Waterson%2C+L">L. Waterson</a>, <a href="/search/astro-ph?searchtype=author&query=Cup%C3%A1k%2C+M">M. Cup谩k</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.16471v2-abstract-short" style="display: inline;"> Thermonuclear (type-I) bursts exhibit properties that depend both on the local surface conditions of the neutron stars on which they ignite, as well as the physical parameters of the host binary system. However, constraining the system parameters requires a comprehensive method to compare the observed bursts to simulations. We have further developed the beansp code for this purpose and analysed th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.16471v2-abstract-full').style.display = 'inline'; document.getElementById('2403.16471v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.16471v2-abstract-full" style="display: none;"> Thermonuclear (type-I) bursts exhibit properties that depend both on the local surface conditions of the neutron stars on which they ignite, as well as the physical parameters of the host binary system. However, constraining the system parameters requires a comprehensive method to compare the observed bursts to simulations. We have further developed the beansp code for this purpose and analysed the bursts observed from IGR J17498-2921, a 401-Hz accretion-powered pulsar, discovered during it's 2011 outburst. We find good agreement with a model having H-deficient fuel with X = 0.15 +/- 0.4, and CNO metallicity Z=0.0014^{+0.0004}_{-0.0003}, about a tenth of the solar value. The model has the system at a distance of 5.7^{+0.6}_{-0.5} kpc, with a massive (approx. 2 M_sun) neutron star and a likely inclination of 60 deg. We also re-analysed the data from the 2002 outburst of the accretion-powered millisecond pulsar SAX J1808.4-3658. For that system we find a substantially closer distance than previously inferred, at 2.7 +/- 0.3 kpc, likely driven by a larger degree of burst emission anisotropy. The other system parameters are largely consistent with the previous analysis. We briefly discuss the implications for the evolution of these two systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.16471v2-abstract-full').style.display = 'none'; document.getElementById('2403.16471v2-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 7 figures, accompanying data at https://dx.doi.org/ 10.26180/24773367; accepted by MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.05236">arXiv:2309.05236</a> <span> [<a href="https://arxiv.org/pdf/2309.05236">pdf</a>, <a href="https://arxiv.org/format/2309.05236">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"> Discovery of millihertz Quasi-Periodic Oscillations in the Low Mass X-Ray Binary XTE J1701$-$462 from a Search of the RXTE Legacy data set </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tse%2C+K">Kaho Tse</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">Duncan K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Heger%2C+A">Alexander Heger</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.05236v2-abstract-short" style="display: inline;"> We report the detection of millihertz quasi-periodic oscillations ($\mathrm{mHz}$ QPOs) from the low-mass X-ray binary XTE J1701$-$462. The discovery came from a search of the legacy data set of the Rossi X-ray Timing Explorer, in order to detect the periodic signals in all observations of sources exhibiting thermonuclear bursts. We found that $47$ out of $860$ observations of XTE J1701$-$462; cov… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.05236v2-abstract-full').style.display = 'inline'; document.getElementById('2309.05236v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.05236v2-abstract-full" style="display: none;"> We report the detection of millihertz quasi-periodic oscillations ($\mathrm{mHz}$ QPOs) from the low-mass X-ray binary XTE J1701$-$462. The discovery came from a search of the legacy data set of the Rossi X-ray Timing Explorer, in order to detect the periodic signals in all observations of sources exhibiting thermonuclear bursts. We found that $47$ out of $860$ observations of XTE J1701$-$462; covering the 2006-7 outburst exhibits signals with a significance above the detection threshold, which was determined separately for each observation via a Monte Carlo approach. We chose the four strongest candidates, each with maximum power exceeding $4蟽$ of the simulated wavelet noise power distribution, to demonstrate the properties of the QPOs. The frequencies of the signals in the four observations are $\sim 3.5\;\text{to}\;5.6\; \mathrm{mHz}$, and the fractional R.M.S. amplitudes vary between $0.74 \pm 0.05\,\%$ and $3.54 \pm 0.04\,\%$. Although previously reported signals in other sources typically disappear immediately before a burst, we do not observe this behaviour in XTE J1701$-$462. Instead, we found that the QPOs and bursts occurred in separate accretion regimes. When the persistent luminosity dropped near the end of the outburst, the source showed bursts and no QPOs were detected, which is the behaviour predicted by theory for the transition from stable to unstable burning. On the basis of this new detection, we reassess the cases for identifying these $\mathrm{mHz}$ QPOs in this and other sources as arising from marginally stable burning. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.05236v2-abstract-full').style.display = 'none'; document.getElementById('2309.05236v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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, 5 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/2308.03499">arXiv:2308.03499</a> <span> [<a href="https://arxiv.org/pdf/2308.03499">pdf</a>, <a href="https://arxiv.org/ps/2308.03499">ps</a>, <a href="https://arxiv.org/format/2308.03499">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/stad374">10.1093/mnras/stad374 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A catalogue of unusually long thermonuclear bursts on neutron stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Alizai%2C+K">Khaled Alizai</a>, <a href="/search/astro-ph?searchtype=author&query=Chenevez%2C+J">J茅r么me Chenevez</a>, <a href="/search/astro-ph?searchtype=author&query=Cumming%2C+A">Andrew Cumming</a>, <a href="/search/astro-ph?searchtype=author&query=Degenaar%2C+N">Nathalie Degenaar</a>, <a href="/search/astro-ph?searchtype=author&query=Falanga%2C+M">Maurizio Falanga</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">Duncan K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Zand%2C+J+J+M+i+%60">Jean J. M. in `t Zand</a>, <a href="/search/astro-ph?searchtype=author&query=Jaisawal%2C+G+K">Gaurava K. Jaisawal</a>, <a href="/search/astro-ph?searchtype=author&query=Keek%2C+L">Laurens Keek</a>, <a href="/search/astro-ph?searchtype=author&query=Kuulkers%2C+E">Erik Kuulkers</a>, <a href="/search/astro-ph?searchtype=author&query=Lampe%2C+N">Nathanael Lampe</a>, <a href="/search/astro-ph?searchtype=author&query=Schatz%2C+H">Hendrik Schatz</a>, <a href="/search/astro-ph?searchtype=author&query=Serino%2C+M">Motoko Serino</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="2308.03499v1-abstract-short" style="display: inline;"> Rare, energetic (long) thermonuclear (Type I) X-ray bursts are classified either as intermediate-duration or superbursts, based on their duration. Intermediate-duration bursts lasting a few to tens of minutes are thought to arise from the thermonuclear runaway of a relatively thick (10^10 g/cm2) helium layer, while superbursts lasting hours are attributed to the detonation of an underlying carbon… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.03499v1-abstract-full').style.display = 'inline'; document.getElementById('2308.03499v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.03499v1-abstract-full" style="display: none;"> Rare, energetic (long) thermonuclear (Type I) X-ray bursts are classified either as intermediate-duration or superbursts, based on their duration. Intermediate-duration bursts lasting a few to tens of minutes are thought to arise from the thermonuclear runaway of a relatively thick (10^10 g/cm2) helium layer, while superbursts lasting hours are attributed to the detonation of an underlying carbon layer. We present a catalogue of 84 long thermonuclear bursts from 40 low-mass X-ray binaries, and defined from a new set of criteria distinguishing them from the more frequent short bursts. The three criteria are: (1) a total energy release larger than 10^40 erg, (2) a photospheric radius expansion phase longer than 10 s, and (3) a burst time-scale longer than 70 s. This work is based on a comprehensive systematic analysis of 70 bursts found with INTEGRAL, RXTE, Swift, BeppoSAX, MAXI, and NICER, as well as 14 long bursts from the literature that were detected with earlier generations of X-ray instruments. For each burst, we measure its peak flux and fluence, which eventually allows us to confirm the distinction between intermediate-duration bursts and superbursts. Additionally, we list 18 bursts that only partially meet the above inclusion criteria, possibly bridging the gap between normal and intermediate-duration bursts. With this catalogue, we significantly increase the number of long-duration bursts included in the MINBAR and thereby provide a substantial sample of these rare X-ray bursts for further study. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.03499v1-abstract-full').style.display = 'none'; document.getElementById('2308.03499v1-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in MNRAS, 20 pages, 7 figures, 4 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Monthly Notices of the Royal Astronomical Society, 2023, Vol. 521, pp. 3608-3624 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.02098">arXiv:2307.02098</a> <span> [<a href="https://arxiv.org/pdf/2307.02098">pdf</a>, <a href="https://arxiv.org/format/2307.02098">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41586-023-06759-1">10.1038/s41586-023-06759-1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> JWST detection of heavy neutron capture elements in a compact object merger </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Levan%2C+A">A. Levan</a>, <a href="/search/astro-ph?searchtype=author&query=Gompertz%2C+B+P">B. P. Gompertz</a>, <a href="/search/astro-ph?searchtype=author&query=Salafia%2C+O+S">O. S. Salafia</a>, <a href="/search/astro-ph?searchtype=author&query=Bulla%2C+M">M. Bulla</a>, <a href="/search/astro-ph?searchtype=author&query=Burns%2C+E">E. Burns</a>, <a href="/search/astro-ph?searchtype=author&query=Hotokezaka%2C+K">K. Hotokezaka</a>, <a href="/search/astro-ph?searchtype=author&query=Izzo%2C+L">L. Izzo</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+G+P">G. P. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Malesani%2C+D+B">D. B. Malesani</a>, <a href="/search/astro-ph?searchtype=author&query=Oates%2C+S+R">S. R. Oates</a>, <a href="/search/astro-ph?searchtype=author&query=Ravasio%2C+M+E">M. E. Ravasio</a>, <a href="/search/astro-ph?searchtype=author&query=Escorial%2C+A+R">A. Rouco Escorial</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+B">B. Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Sarin%2C+N">N. Sarin</a>, <a href="/search/astro-ph?searchtype=author&query=Schulze%2C+S">S. Schulze</a>, <a href="/search/astro-ph?searchtype=author&query=Tanvir%2C+N+R">N. R. Tanvir</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+G">G. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Brammer%2C+G+B">G. B. Brammer</a>, <a href="/search/astro-ph?searchtype=author&query=Christensen%2C+L">L. Christensen</a>, <a href="/search/astro-ph?searchtype=author&query=Dhillon%2C+V+S">V. S. Dhillon</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+P+A">P. A. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Fausnaugh%2C+M">M. Fausnaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Fong%2C+W+-">W. -F. Fong</a>, <a href="/search/astro-ph?searchtype=author&query=Fruchter%2C+A+S">A. S. Fruchter</a> , et al. (58 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="2307.02098v1-abstract-short" style="display: inline;"> The mergers of binary compact objects such as neutron stars and black holes are of central interest to several areas of astrophysics, including as the progenitors of gamma-ray bursts (GRBs), sources of high-frequency gravitational waves and likely production sites for heavy element nucleosynthesis via rapid neutron capture (the r-process). These heavy elements include some of great geophysical, bi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.02098v1-abstract-full').style.display = 'inline'; document.getElementById('2307.02098v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.02098v1-abstract-full" style="display: none;"> The mergers of binary compact objects such as neutron stars and black holes are of central interest to several areas of astrophysics, including as the progenitors of gamma-ray bursts (GRBs), sources of high-frequency gravitational waves and likely production sites for heavy element nucleosynthesis via rapid neutron capture (the r-process). These heavy elements include some of great geophysical, biological and cultural importance, such as thorium, iodine and gold. Here we present observations of the exceptionally bright gamma-ray burst GRB 230307A. We show that GRB 230307A belongs to the class of long-duration gamma-ray bursts associated with compact object mergers, and contains a kilonova similar to AT2017gfo, associated with the gravitational-wave merger GW170817. We obtained James Webb Space Telescope mid-infrared (mid-IR) imaging and spectroscopy 29 and 61 days after the burst. The spectroscopy shows an emission line at 2.15 microns which we interpret as tellurium (atomic mass A=130), and a very red source, emitting most of its light in the mid-IR due to the production of lanthanides. These observations demonstrate that nucleosynthesis in GRBs can create r-process elements across a broad atomic mass range and play a central role in heavy element nucleosynthesis across the Universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.02098v1-abstract-full').style.display = 'none'; document.getElementById('2307.02098v1-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 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">Submitted. Comments welcome! Nature (2023)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.14491">arXiv:2305.14491</a> <span> [<a href="https://arxiv.org/pdf/2305.14491">pdf</a>, <a href="https://arxiv.org/ps/2305.14491">ps</a>, <a href="https://arxiv.org/format/2305.14491">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/stad1703">10.1093/mnras/stad1703 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> GRB 201015A and the nature of low-luminosity soft gamma-ray bursts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Patel%2C+M">M. Patel</a>, <a href="/search/astro-ph?searchtype=author&query=Gompertz%2C+B+P">B. P. Gompertz</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Brien%2C+P+T">P. T. O'Brien</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+G+P">G. P. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Starling%2C+R+L+C">R. L. C. Starling</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+P+A">P. A Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Amati%2C+L">L. Amati</a>, <a href="/search/astro-ph?searchtype=author&query=Levan%2C+A+J">A. J. Levan</a>, <a href="/search/astro-ph?searchtype=author&query=Nicholl%2C+M">M. Nicholl</a>, <a href="/search/astro-ph?searchtype=author&query=Lyman%2C+J">J. Lyman</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Dyer%2C+M+J">M. J. Dyer</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Steeghs%2C+D">D. Steeghs</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Dhillon%2C+V+S">V. S. Dhillon</a>, <a href="/search/astro-ph?searchtype=author&query=Ramsay%2C+G">G. Ramsay</a>, <a href="/search/astro-ph?searchtype=author&query=Noysena%2C+K">K. Noysena</a>, <a href="/search/astro-ph?searchtype=author&query=Kotak%2C+R">R. Kotak</a>, <a href="/search/astro-ph?searchtype=author&query=Breton%2C+R+P">R. P. Breton</a>, <a href="/search/astro-ph?searchtype=author&query=Nuttall%2C+L+K">L. K. Nuttall</a>, <a href="/search/astro-ph?searchtype=author&query=Palle%2C+E">E. Palle</a>, <a href="/search/astro-ph?searchtype=author&query=Pollacco%2C+D">D. Pollacco</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.14491v1-abstract-short" style="display: inline;"> GRB 201015A is a peculiarly low luminosity, spectrally soft gamma-ray burst (GRB), with $T_{\rm 90} = 9.8 \pm 3.5$ s (time interval of detection of 90\% of photons from the GRB), and an associated supernova (likely to be type Ic or Ic-BL). GRB 201015A has an isotropic energy $E_{纬,\rm iso} = 1.75 ^{+0.60} _{-0.53} \times 10^{50}$ erg, and photon index $螕= 3.00 ^{+0.50} _{-0.42}$ (15-150 keV). It f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.14491v1-abstract-full').style.display = 'inline'; document.getElementById('2305.14491v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.14491v1-abstract-full" style="display: none;"> GRB 201015A is a peculiarly low luminosity, spectrally soft gamma-ray burst (GRB), with $T_{\rm 90} = 9.8 \pm 3.5$ s (time interval of detection of 90\% of photons from the GRB), and an associated supernova (likely to be type Ic or Ic-BL). GRB 201015A has an isotropic energy $E_{纬,\rm iso} = 1.75 ^{+0.60} _{-0.53} \times 10^{50}$ erg, and photon index $螕= 3.00 ^{+0.50} _{-0.42}$ (15-150 keV). It follows the Amati relation, a correlation between $E_{纬,\rm iso}$ and spectral peak energy $E_{\rm p}$ followed by long GRBs. It appears exceptionally soft based on $螕$, the hardness ratio of HR = $0.47 \pm 0.24$, and low-$E_{\rm p}$, so we have compared it to other GRBs sharing these properties. These events can be explained by shock breakout, poorly collimated jets, and off-axis viewing. Follow-up observations of the afterglow taken in the X-ray, optical, and radio, reveal a surprisingly late flattening in the X-ray from $t = (2.61 \pm 1.27)\times 10^4$ s to $t = 1.67 ^{+1.14} _{-0.65} \times 10^6$ s. We fit the data to closure relations describing the synchrotron emission, finding the electron spectral index to be $p = 2.42 ^{+0.44} _{-0.30}$, and evidence of late-time energy injection with coefficient $q = 0.24 ^{+0.24} _{-0.18}$. The jet half opening angle lower limit ($胃_{j} \ge 16^{\circ}$) is inferred from the non-detection of a jet break. The launch of SVOM and Einstein Probe in 2023, should enable detection of more low luminosity events like this, providing a fuller picture of the variety of GRBs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.14491v1-abstract-full').style.display = 'none'; document.getElementById('2305.14491v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 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">15 pages, 4 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/2305.10627">arXiv:2305.10627</a> <span> [<a href="https://arxiv.org/pdf/2305.10627">pdf</a>, <a href="https://arxiv.org/format/2305.10627">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"> Time-independent Simulations of Steady-State Accretion with Nuclear Burning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tse%2C+K">Kaho Tse</a>, <a href="/search/astro-ph?searchtype=author&query=Heger%2C+A">Alexander Heger</a>, <a href="/search/astro-ph?searchtype=author&query=Hirai%2C+R">Ryosuke Hirai</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">Duncan K. Galloway</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.10627v2-abstract-short" style="display: inline;"> We construct a new formulation that allows efficient exploration of steady-state accretion processes onto compact objects. Accretion onto compact objects is a common scenario in astronomy. These systems serve as laboratories to probe the nuclear burning of the accreted matter. Conventional stellar evolution codes have been developed to simulate in detail the nuclear reactions on the compact object… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.10627v2-abstract-full').style.display = 'inline'; document.getElementById('2305.10627v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.10627v2-abstract-full" style="display: none;"> We construct a new formulation that allows efficient exploration of steady-state accretion processes onto compact objects. Accretion onto compact objects is a common scenario in astronomy. These systems serve as laboratories to probe the nuclear burning of the accreted matter. Conventional stellar evolution codes have been developed to simulate in detail the nuclear reactions on the compact objects. In order to follow the case of steady burning, however, using these codes can be very expensive as they are designed to follow a time-dependent problem. Here we introduce our new code $\textsc{StarShot}$, which resolves the structure of the compact objects for the case of stable thermonuclear burning, and is able to follow all nuclear species using an adaptive nuclear reaction network and adaptive zoning. Compared to dynamical codes, the governing equations can be reduced to time-independent forms under the assumption of steady-state accretion. We show an application to accreting low mass X-ray binaries (LMXBs) with accretion onto a neutron-star as compact object. The computational efficiency of $\textsc{StarShot}$ allows us to explore the parameter space for stable burning regimes, and can be used to generate initial conditions for time-dependent evolution models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.10627v2-abstract-full').style.display = 'none'; document.getElementById('2305.10627v2-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 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 4 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/2302.00018">arXiv:2302.00018</a> <span> [<a href="https://arxiv.org/pdf/2302.00018">pdf</a>, <a href="https://arxiv.org/format/2302.00018">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad366">10.1093/mnras/stad366 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Precision Ephemerides for Gravitational-wave Searches -- IV: Corrected and refined ephemeris for Scorpius X-1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Killestein%2C+T+L">T. L. Killestein</a>, <a href="/search/astro-ph?searchtype=author&query=Mould%2C+M">M. Mould</a>, <a href="/search/astro-ph?searchtype=author&query=Steeghs%2C+D">D. Steeghs</a>, <a href="/search/astro-ph?searchtype=author&query=Casares%2C+J">J. Casares</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Whelan%2C+J+T">J. T. Whelan</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.00018v3-abstract-short" style="display: inline;"> Low-mass X-ray binaries have long been theorised as potential sources of continuous gravitational-wave radiation, yet there is no observational evidence from recent LIGO/Virgo observing runs. Even for the theoretically 'loudest' source, Sco X-1, the upper limit on gravitational-wave strain has been pushed ever lower. Such searches require precise measurements of the source properties for sufficien… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.00018v3-abstract-full').style.display = 'inline'; document.getElementById('2302.00018v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.00018v3-abstract-full" style="display: none;"> Low-mass X-ray binaries have long been theorised as potential sources of continuous gravitational-wave radiation, yet there is no observational evidence from recent LIGO/Virgo observing runs. Even for the theoretically 'loudest' source, Sco X-1, the upper limit on gravitational-wave strain has been pushed ever lower. Such searches require precise measurements of the source properties for sufficient sensitivity and computational feasibility. Collating over 20 years of high-quality spectroscopic observations of the system, we present a precise and comprehensive ephemeris for Sco X-1 through radial velocity measurements, performing a full homogeneous reanalysis of all relevant datasets and correcting previous analyses. Our Bayesian approach accounts for observational systematics and maximises not only precision, but also the fidelity of uncertainty estimates - crucial for informing principled continuous-wave searches. Our extensive dataset and analysis also enables us to construct the highest signal-to-noise, highest resolution phase-averaged spectrum of a low-mass X-ray binary to date. Doppler tomography reveals intriguing transient structures present in the accretion disk and flow driven by modulation of the accretion rate, necessitating further characterisation of the system at high temporal and spectral resolution. Our ephemeris corrects and supersedes previous ephemerides, and provides a factor three reduction in the number of templates in the search space, facilitating precision searches for continuous gravitational-wave emission from Sco X-1 throughout the upcoming LIGO/Virgo/KAGRA O4 observing run and beyond. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.00018v3-abstract-full').style.display = 'none'; document.getElementById('2302.00018v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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">14 pages, 11 figures, accepted in MNRAS - updated version to fix typographical error (precision of Porb) in Table 2</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.03598">arXiv:2210.03598</a> <span> [<a href="https://arxiv.org/pdf/2210.03598">pdf</a>, <a href="https://arxiv.org/format/2210.03598">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ac98c9">10.3847/1538-4365/ac98c9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Robust inference of neutron-star parameters from thermonuclear burst observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+Z">Z. Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Goodwin%2C+A+J">A. J. Goodwin</a>, <a href="/search/astro-ph?searchtype=author&query=He%2C+C+-">C. -C. He</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.03598v1-abstract-short" style="display: inline;"> Thermonuclear (type-I) bursts arise from unstable ignition of accumulated fuel on the surface of neutron stars in low-mass X-ray binaries. Measurements of burst properties in principle enable observers to infer the properties of the host neutron star and mass donors, but a number of confounding astrophysical effects contribute to systematic uncertainties. Here we describe some commonly-used approa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.03598v1-abstract-full').style.display = 'inline'; document.getElementById('2210.03598v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.03598v1-abstract-full" style="display: none;"> Thermonuclear (type-I) bursts arise from unstable ignition of accumulated fuel on the surface of neutron stars in low-mass X-ray binaries. Measurements of burst properties in principle enable observers to infer the properties of the host neutron star and mass donors, but a number of confounding astrophysical effects contribute to systematic uncertainties. Here we describe some commonly-used approaches for determining system parameters, including composition of the burst fuel, and introduce a new suite of software tools, concord, intended to fully account for astrophysical uncertainties. Comparison of observed burst properties with the predictions of numerical models is a complementary method of constraining host properties, and the tools presented here are intended to make comprehensive model-observation comparisons straightforward. When combined with the extensive samples of burst observations accumulated by X-ray observatories, these software tools will provide a step-change in the amount of information that can be inferred about typical burst sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.03598v1-abstract-full').style.display = 'none'; document.getElementById('2210.03598v1-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 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 11 figures, 1 table & 1 machine-readable table as supplementary data; submitted to ApJS. Accompanying software package available at https://github.com/outs1der/concord</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.06375">arXiv:2209.06375</a> <span> [<a href="https://arxiv.org/pdf/2209.06375">pdf</a>, <a href="https://arxiv.org/format/2209.06375">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="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/stac3103">10.1093/mnras/stac3103 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Self-Supervised Clustering on Image-Subtracted Data with Deep-Embedded Self-Organizing Map </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mong%2C+Y+-">Y. -L. Mong</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Killestein%2C+T+L">T. L. Killestein</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Dyer%2C+M">M. Dyer</a>, <a href="/search/astro-ph?searchtype=author&query=Cutter%2C+R">R. Cutter</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+M+J+I">M. J. I. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Lyman%2C+J">J. Lyman</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Steeghs%2C+D">D. Steeghs</a>, <a href="/search/astro-ph?searchtype=author&query=Dhillon%2C+V">V. Dhillon</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Brien%2C+P">P. O'Brien</a>, <a href="/search/astro-ph?searchtype=author&query=Ramsay%2C+G">G. Ramsay</a>, <a href="/search/astro-ph?searchtype=author&query=Noysena%2C+K">K. Noysena</a>, <a href="/search/astro-ph?searchtype=author&query=Kotak%2C+R">R. Kotak</a>, <a href="/search/astro-ph?searchtype=author&query=Breton%2C+R">R. Breton</a>, <a href="/search/astro-ph?searchtype=author&query=Nuttall%2C+L">L. Nuttall</a>, <a href="/search/astro-ph?searchtype=author&query=Palle%2C+E">E. Palle</a>, <a href="/search/astro-ph?searchtype=author&query=Pollacco%2C+D">D. Pollacco</a>, <a href="/search/astro-ph?searchtype=author&query=Thrane%2C+E">E. Thrane</a>, <a href="/search/astro-ph?searchtype=author&query=Awiphan%2C+S">S. Awiphan</a>, <a href="/search/astro-ph?searchtype=author&query=Burhanudin%2C+U">U. Burhanudin</a>, <a href="/search/astro-ph?searchtype=author&query=Chote%2C+P">P. Chote</a>, <a href="/search/astro-ph?searchtype=author&query=Chrimes%2C+A">A. Chrimes</a>, <a href="/search/astro-ph?searchtype=author&query=Daw%2C+E">E. Daw</a> , et al. (23 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="2209.06375v1-abstract-short" style="display: inline;"> Developing an effective automatic classifier to separate genuine sources from artifacts is essential for transient follow-ups in wide-field optical surveys. The identification of transient detections from the subtraction artifacts after the image differencing process is a key step in such classifiers, known as real-bogus classification problem. We apply a self-supervised machine learning model, th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.06375v1-abstract-full').style.display = 'inline'; document.getElementById('2209.06375v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.06375v1-abstract-full" style="display: none;"> Developing an effective automatic classifier to separate genuine sources from artifacts is essential for transient follow-ups in wide-field optical surveys. The identification of transient detections from the subtraction artifacts after the image differencing process is a key step in such classifiers, known as real-bogus classification problem. We apply a self-supervised machine learning model, the deep-embedded self-organizing map (DESOM) to this "real-bogus" classification problem. DESOM combines an autoencoder and a self-organizing map to perform clustering in order to distinguish between real and bogus detections, based on their dimensionality-reduced representations. We use 32x32 normalized detection thumbnails as the input of DESOM. We demonstrate different model training approaches, and find that our best DESOM classifier shows a missed detection rate of 6.6% with a false positive rate of 1.5%. DESOM offers a more nuanced way to fine-tune the decision boundary identifying likely real detections when used in combination with other types of classifiers, for example built on neural networks or decision trees. We also discuss other potential usages of DESOM and its limitations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.06375v1-abstract-full').style.display = 'none'; document.getElementById('2209.06375v1-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.14901">arXiv:2208.14901</a> <span> [<a href="https://arxiv.org/pdf/2208.14901">pdf</a>, <a href="https://arxiv.org/format/2208.14901">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.2629369">10.1117/12.2629369 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gravitational-wave Optical Transient Observer (GOTO) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dyer%2C+M+J">Martin J. Dyer</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">Kendall Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Lyman%2C+J">Joe Lyman</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">Krzysztof Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Steeghs%2C+D">Danny Steeghs</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">Duncan K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Dhillon%2C+V+S">Vik S Dhillon</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Brien%2C+P">Paul O'Brien</a>, <a href="/search/astro-ph?searchtype=author&query=Ramsay%2C+G">Gavin Ramsay</a>, <a href="/search/astro-ph?searchtype=author&query=Noysena%2C+K">Kanthanakorn Noysena</a>, <a href="/search/astro-ph?searchtype=author&query=Kotak%2C+R">Rubina Kotak</a>, <a href="/search/astro-ph?searchtype=author&query=Breton%2C+R">Rene Breton</a>, <a href="/search/astro-ph?searchtype=author&query=Nuttall%2C+L">Laura Nuttall</a>, <a href="/search/astro-ph?searchtype=author&query=Pall%C3%A9%2C+E">Enric Pall茅</a>, <a href="/search/astro-ph?searchtype=author&query=Pollacco%2C+D">Don Pollacco</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="2208.14901v1-abstract-short" style="display: inline;"> The Gravitational-wave Optical Transient Observer (GOTO) is a wide-field telescope project focused on detecting optical counterparts to gravitational-wave sources. Each GOTO robotic mount holds eight 40 cm telescopes, giving an overall field of view of 40 square degrees. As of 2022 the first two GOTO mounts have been commissioned at the Roque de los Muchachos Observatory on La Palma, Canary Island… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.14901v1-abstract-full').style.display = 'inline'; document.getElementById('2208.14901v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.14901v1-abstract-full" style="display: none;"> The Gravitational-wave Optical Transient Observer (GOTO) is a wide-field telescope project focused on detecting optical counterparts to gravitational-wave sources. Each GOTO robotic mount holds eight 40 cm telescopes, giving an overall field of view of 40 square degrees. As of 2022 the first two GOTO mounts have been commissioned at the Roque de los Muchachos Observatory on La Palma, Canary Islands, and construction of the second node with two additional 8-telescope mounts has begin at Siding Spring Observatory in New South Wales, Australia. Once fully operational each GOTO mount will be networked to form a robotic, multi-site observatory, which will survey the entire visible sky every two nights and enable rapid follow-up detections of transient sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.14901v1-abstract-full').style.display = 'none'; document.getElementById('2208.14901v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 August, 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">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 5 figures, submitted to SPIE Astronomical Telescopes + Instrumentation 2022</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proc. SPIE 12182, Ground-based and Airborne Telescopes IX, 121821Y (29 August 2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.07996">arXiv:2205.07996</a> <span> [<a href="https://arxiv.org/pdf/2205.07996">pdf</a>, <a href="https://arxiv.org/format/2205.07996">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1361-6471/ac8890">10.1088/1361-6471/ac8890 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Horizons: Nuclear Astrophysics in the 2020s and Beyond </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Schatz%2C+H">H. Schatz</a>, <a href="/search/astro-ph?searchtype=author&query=Reyes%2C+A+D+B">A. D. Becerril Reyes</a>, <a href="/search/astro-ph?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+E+F">E. F. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Chatziioannou%2C+K">K. Chatziioannou</a>, <a href="/search/astro-ph?searchtype=author&query=Chipps%2C+K+A">K. A. Chipps</a>, <a href="/search/astro-ph?searchtype=author&query=Deibel%2C+C+M">C. M. Deibel</a>, <a href="/search/astro-ph?searchtype=author&query=Ezzeddine%2C+R">R. Ezzeddine</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Hansen%2C+C+J">C. J. Hansen</a>, <a href="/search/astro-ph?searchtype=author&query=Herwig%2C+F">F. Herwig</a>, <a href="/search/astro-ph?searchtype=author&query=Ji%2C+A+P">A. P. Ji</a>, <a href="/search/astro-ph?searchtype=author&query=Lugaro%2C+M">M. Lugaro</a>, <a href="/search/astro-ph?searchtype=author&query=Meisel%2C+Z">Z. Meisel</a>, <a href="/search/astro-ph?searchtype=author&query=Norman%2C+D">D. Norman</a>, <a href="/search/astro-ph?searchtype=author&query=Read%2C+J+S">J. S. Read</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts%2C+L+F">L. F. Roberts</a>, <a href="/search/astro-ph?searchtype=author&query=Spyrou%2C+A">A. Spyrou</a>, <a href="/search/astro-ph?searchtype=author&query=Tews%2C+I">I. Tews</a>, <a href="/search/astro-ph?searchtype=author&query=Timmes%2C+F+X">F. X. Timmes</a>, <a href="/search/astro-ph?searchtype=author&query=Travaglio%2C+C">C. Travaglio</a>, <a href="/search/astro-ph?searchtype=author&query=Vassh%2C+N">N. Vassh</a>, <a href="/search/astro-ph?searchtype=author&query=Abia%2C+C">C. Abia</a>, <a href="/search/astro-ph?searchtype=author&query=Adsley%2C+P">P. Adsley</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+S">S. Agarwal</a> , et al. (140 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="2205.07996v1-abstract-short" style="display: inline;"> Nuclear Astrophysics is a field at the intersection of nuclear physics and astrophysics, which seeks to understand the nuclear engines of astronomical objects and the origin of the chemical elements. This white paper summarizes progress and status of the field, the new open questions that have emerged, and the tremendous scientific opportunities that have opened up with major advances in capabilit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.07996v1-abstract-full').style.display = 'inline'; document.getElementById('2205.07996v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.07996v1-abstract-full" style="display: none;"> Nuclear Astrophysics is a field at the intersection of nuclear physics and astrophysics, which seeks to understand the nuclear engines of astronomical objects and the origin of the chemical elements. This white paper summarizes progress and status of the field, the new open questions that have emerged, and the tremendous scientific opportunities that have opened up with major advances in capabilities across an ever growing number of disciplines and subfields that need to be integrated. We take a holistic view of the field discussing the unique challenges and opportunities in nuclear astrophysics in regards to science, diversity, education, and the interdisciplinarity and breadth of the field. Clearly nuclear astrophysics is a dynamic field with a bright future that is entering a new era of discovery opportunities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.07996v1-abstract-full').style.display = 'none'; document.getElementById('2205.07996v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 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">96 pages. Submitted to Journal of Physics G</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LA-UR-22-23997 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.10416">arXiv:2111.10416</a> <span> [<a href="https://arxiv.org/pdf/2111.10416">pdf</a>, <a href="https://arxiv.org/format/2111.10416">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stab3402">10.1093/mnras/stab3402 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The return of the spin period in DW Cnc and evidence of new high state outbursts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Duffy%2C+C">C. Duffy</a>, <a href="/search/astro-ph?searchtype=author&query=Ramsay%2C+G">G. Ramsay</a>, <a href="/search/astro-ph?searchtype=author&query=Steeghs%2C+D">D. Steeghs</a>, <a href="/search/astro-ph?searchtype=author&query=Kennedy%2C+M+R">M. R. Kennedy</a>, <a href="/search/astro-ph?searchtype=author&query=West%2C+R+G">R. G. West</a>, <a href="/search/astro-ph?searchtype=author&query=Wheatley%2C+P+J">P. J. Wheatley</a>, <a href="/search/astro-ph?searchtype=author&query=Dhillon%2C+V+S">V. S. Dhillon</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Dyer%2C+M+J">M. J. Dyer</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Gill%2C+S">S. Gill</a>, <a href="/search/astro-ph?searchtype=author&query=Acton%2C+J+S">J. S. Acton</a>, <a href="/search/astro-ph?searchtype=author&query=Burleigh%2C+M+R">M. R. Burleigh</a>, <a href="/search/astro-ph?searchtype=author&query=Casewell%2C+S+L">S. L. Casewell</a>, <a href="/search/astro-ph?searchtype=author&query=Goad%2C+M+R">M. R. Goad</a>, <a href="/search/astro-ph?searchtype=author&query=Henderson%2C+B+A">B. A. Henderson</a>, <a href="/search/astro-ph?searchtype=author&query=Tilbrook%2C+R+H">R. H. Tilbrook</a>, <a href="/search/astro-ph?searchtype=author&query=Str%C3%B8m%2C+P+A">P. A. Str酶m</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+D+R">D. R. Anderson</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="2111.10416v1-abstract-short" style="display: inline;"> DW Cnc is an intermediate polar which has previously been observed in both high and low states. Observations of the high state of DW Cnc have previously revealed a spin period at ~ 38.6 min, however observations from the 2018/19 low state showed no evidence of the spin period. We present results from our analysis of 12 s cadence photometric data collected by NGTS of DW Cnc during the high state wh… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.10416v1-abstract-full').style.display = 'inline'; document.getElementById('2111.10416v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.10416v1-abstract-full" style="display: none;"> DW Cnc is an intermediate polar which has previously been observed in both high and low states. Observations of the high state of DW Cnc have previously revealed a spin period at ~ 38.6 min, however observations from the 2018/19 low state showed no evidence of the spin period. We present results from our analysis of 12 s cadence photometric data collected by NGTS of DW Cnc during the high state which began in 2019. Following the previously reported suppression of the spin period signal we identify the return of this signal during the high state, consistent with previous observations of it. We identify this as the restarting of accretion during the high state. We further identified three short outbursts lasting ~ 1 d in DW Cnc with a mean recurrence time of ~ 60 d and an amplitude of ~ 1 mag. These are the first outbursts identified in DW Cnc since 2008. Due to the short nature of these events we identify them not as a result of accretion instabilities but instead either from instabilities originating from the interaction of the magnetorotational instability in the accretion disc and the magnetic field generated by the white dwarf or the result of magnetic gating. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.10416v1-abstract-full').style.display = 'none'; document.getElementById('2111.10416v1-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 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">Accepted to MNRAS; 8 pages, 4 figues</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.05539">arXiv:2110.05539</a> <span> [<a href="https://arxiv.org/pdf/2110.05539">pdf</a>, <a href="https://arxiv.org/format/2110.05539">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 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/stac013">10.1093/mnras/stac013 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gravitational-wave Optical Transient Observer (GOTO): prototype performance and prospects for transient science </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Steeghs%2C+D">D. Steeghs</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Dyer%2C+M+J">M. J. Dyer</a>, <a href="/search/astro-ph?searchtype=author&query=Lyman%2C+J">J. Lyman</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Cutter%2C+R">R. Cutter</a>, <a href="/search/astro-ph?searchtype=author&query=Mong%2C+Y+L">Y. L. Mong</a>, <a href="/search/astro-ph?searchtype=author&query=Dhillon%2C+V">V. Dhillon</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Brien%2C+P">P. O'Brien</a>, <a href="/search/astro-ph?searchtype=author&query=Ramsay%2C+G">G. Ramsay</a>, <a href="/search/astro-ph?searchtype=author&query=Poshyachinda%2C+S">S. Poshyachinda</a>, <a href="/search/astro-ph?searchtype=author&query=Kotak%2C+R">R. Kotak</a>, <a href="/search/astro-ph?searchtype=author&query=Nuttall%2C+L+K">L. K. Nuttall</a>, <a href="/search/astro-ph?searchtype=author&query=Palle%2C+E">E. Palle</a>, <a href="/search/astro-ph?searchtype=author&query=Breton%2C+R+P">R. P. Breton</a>, <a href="/search/astro-ph?searchtype=author&query=Pollacco%2C+D">D. Pollacco</a>, <a href="/search/astro-ph?searchtype=author&query=Thrane%2C+E">E. Thrane</a>, <a href="/search/astro-ph?searchtype=author&query=Aukkaravittayapun%2C+S">S. Aukkaravittayapun</a>, <a href="/search/astro-ph?searchtype=author&query=Awiphan%2C+S">S. Awiphan</a>, <a href="/search/astro-ph?searchtype=author&query=Burhanudin%2C+U">U. Burhanudin</a>, <a href="/search/astro-ph?searchtype=author&query=Chote%2C+P">P. Chote</a>, <a href="/search/astro-ph?searchtype=author&query=Chrimes%2C+A">A. Chrimes</a>, <a href="/search/astro-ph?searchtype=author&query=Daw%2C+E">E. Daw</a>, <a href="/search/astro-ph?searchtype=author&query=Duffy%2C+C">C. Duffy</a> , et al. (28 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="2110.05539v1-abstract-short" style="display: inline;"> The Gravitational-wave Optical Transient Observer (GOTO) is an array of wide-field optical telescopes, designed to exploit new discoveries from the next generation of gravitational wave detectors (LIGO, Virgo, KAGRA), study rapidly evolving transients, and exploit multi-messenger opportunities arising from neutrino and very high energy gamma-ray triggers. In addition to a rapid response mode, the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.05539v1-abstract-full').style.display = 'inline'; document.getElementById('2110.05539v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.05539v1-abstract-full" style="display: none;"> The Gravitational-wave Optical Transient Observer (GOTO) is an array of wide-field optical telescopes, designed to exploit new discoveries from the next generation of gravitational wave detectors (LIGO, Virgo, KAGRA), study rapidly evolving transients, and exploit multi-messenger opportunities arising from neutrino and very high energy gamma-ray triggers. In addition to a rapid response mode, the array will also perform a sensitive, all-sky transient survey with few day cadence. The facility features a novel, modular design with multiple 40-cm wide-field reflectors on a single mount. In June 2017 the GOTO collaboration deployed the initial project prototype, with 4 telescope units, at the Roque de los Muchachos Observatory (ORM), La Palma, Canary Islands. Here we describe the deployment, commissioning, and performance of the prototype hardware, and discuss the impact of these findings on the final GOTO design. We also offer an initial assessment of the science prospects for the full GOTO facility that employs 32 telescope units across two sites. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.05539v1-abstract-full').style.display = 'none'; document.getElementById('2110.05539v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 16 Figures, accepted for publication in Monthly Notices of the Royal Astronomical Society</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.11802">arXiv:2108.11802</a> <span> [<a href="https://arxiv.org/pdf/2108.11802">pdf</a>, <a href="https://arxiv.org/format/2108.11802">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/stab2499">10.1093/mnras/stab2499 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searching For Fermi GRB Optical Counterparts With The Prototype Gravitational-Wave Optical Transient Observer (GOTO) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mong%2C+Y+-">Y. -L. Mong</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Dyer%2C+M">M. Dyer</a>, <a href="/search/astro-ph?searchtype=author&query=Cutter%2C+R">R. Cutter</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+M+J+I">M. J. I. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Lyman%2C+J">J. Lyman</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Steeghs%2C+D">D. Steeghs</a>, <a href="/search/astro-ph?searchtype=author&query=Dhillon%2C+V">V. Dhillon</a>, <a href="/search/astro-ph?searchtype=author&query=OBrien%2C+P">P. OBrien</a>, <a href="/search/astro-ph?searchtype=author&query=Ramsay%2C+G">G. Ramsay</a>, <a href="/search/astro-ph?searchtype=author&query=Noysena%2C+K">K. Noysena</a>, <a href="/search/astro-ph?searchtype=author&query=Kotak%2C+R">R. Kotak</a>, <a href="/search/astro-ph?searchtype=author&query=Breton%2C+R">R. Breton</a>, <a href="/search/astro-ph?searchtype=author&query=Nuttall%2C+L">L. Nuttall</a>, <a href="/search/astro-ph?searchtype=author&query=Palle%2C+E">E. Palle</a>, <a href="/search/astro-ph?searchtype=author&query=Pollacco%2C+D">D. Pollacco</a>, <a href="/search/astro-ph?searchtype=author&query=Thrane%2C+E">E. Thrane</a>, <a href="/search/astro-ph?searchtype=author&query=Awiphan%2C+S">S. Awiphan</a>, <a href="/search/astro-ph?searchtype=author&query=Burhanudin%2C+U">U. Burhanudin</a>, <a href="/search/astro-ph?searchtype=author&query=Chote%2C+P">P. Chote</a>, <a href="/search/astro-ph?searchtype=author&query=Chrimes%2C+A">A. Chrimes</a>, <a href="/search/astro-ph?searchtype=author&query=Daw%2C+E">E. Daw</a>, <a href="/search/astro-ph?searchtype=author&query=Duffy%2C+C">C. Duffy</a> , et al. (23 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="2108.11802v1-abstract-short" style="display: inline;"> The typical detection rate of $\sim1$ gamma-ray burst (GRB) per day by the \emph{Fermi} Gamma-ray Burst Monitor (GBM) provides a valuable opportunity to further our understanding of GRB physics. However, the large uncertainty of the \emph{Fermi} localization typically prevents rapid identification of multi-wavelength counterparts. We report the follow-up of 93 \emph{Fermi} GRBs with the Gravitatio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.11802v1-abstract-full').style.display = 'inline'; document.getElementById('2108.11802v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.11802v1-abstract-full" style="display: none;"> The typical detection rate of $\sim1$ gamma-ray burst (GRB) per day by the \emph{Fermi} Gamma-ray Burst Monitor (GBM) provides a valuable opportunity to further our understanding of GRB physics. However, the large uncertainty of the \emph{Fermi} localization typically prevents rapid identification of multi-wavelength counterparts. We report the follow-up of 93 \emph{Fermi} GRBs with the Gravitational-wave Optical Transient Observer (GOTO) prototype on La Palma. We selected 53 events (based on favourable observing conditions) for detailed analysis, and to demonstrate our strategy of searching for optical counterparts. We apply a filtering process consisting of both automated and manual steps to 60\,085 candidates initially, rejecting all but 29, arising from 15 events. With $\approx3$ GRB afterglows expected to be detectable with GOTO from our sample, most of the candidates are unlikely to be related to the GRBs. Since we did not have multiple observations for those candidates, we cannot confidently confirm the association between the transients and the GRBs. Our results show that GOTO can effectively search for GRB optical counterparts thanks to its large field of view of $\approx40$ square degrees and its depth of $\approx20$ mag. We also detail several methods to improve our overall performance for future follow-up programs of \emph{Fermi} GRBs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.11802v1-abstract-full').style.display = 'none'; document.getElementById('2108.11802v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.13803">arXiv:2105.13803</a> <span> [<a href="https://arxiv.org/pdf/2105.13803">pdf</a>, <a href="https://arxiv.org/format/2105.13803">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/stab3095">10.1093/mnras/stab3095 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Deep searches for X-ray pulsations from Scorpius X-1 and Cygnus X-2 in support of continuous gravitational wave searches </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Galaudage%2C+S">Shanika Galaudage</a>, <a href="/search/astro-ph?searchtype=author&query=Wette%2C+K">Karl Wette</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">Duncan K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Messenger%2C+C">Chris Messenger</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="2105.13803v1-abstract-short" style="display: inline;"> Neutron stars in low mass X-ray binaries are hypothesised to emit continuous gravitational waves that may be detectable by ground-based observatories. The torque balance model predicts that a higher accretion rate produces larger-amplitude gravitational waves, hence low mass X-ray binaries with high X-ray flux are promising targets for gravitational wave searches. The detection of X-ray pulsations… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.13803v1-abstract-full').style.display = 'inline'; document.getElementById('2105.13803v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.13803v1-abstract-full" style="display: none;"> Neutron stars in low mass X-ray binaries are hypothesised to emit continuous gravitational waves that may be detectable by ground-based observatories. The torque balance model predicts that a higher accretion rate produces larger-amplitude gravitational waves, hence low mass X-ray binaries with high X-ray flux are promising targets for gravitational wave searches. The detection of X-ray pulsations would identify the spin frequency of these neutron stars, and thereby improve the sensitivity of continuous gravitational-wave searches by reducing the volume of the search parameter space. We perform a semi-coherent search for pulsations in the two low mass X-ray binaries Scorpius X-1 and Cygnus X-2 using X-ray data from the \textit{ Rossi X-ray Timing Explorer} Proportional Counter Array. We find no clear evidence for pulsations, and obtain upper limits (at $90\%$ confidence) on the fractional pulse amplitude, with the most stringent being $0.034\%$ for Scorpius X-1 and $0.23\%$ for Cygnus X-2. These upper limits improve upon those of Vaughan et al. (1994) by factors of $\sim 8.2$ and $\sim 1.6$ respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.13803v1-abstract-full').style.display = 'none'; document.getElementById('2105.13803v1-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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, 11 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS 509, 1745--1754 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.11169">arXiv:2105.11169</a> <span> [<a href="https://arxiv.org/pdf/2105.11169">pdf</a>, <a href="https://arxiv.org/format/2105.11169">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stab1545">10.1093/mnras/stab1545 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Light curve classification with recurrent neural networks for GOTO: dealing with imbalanced data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Burhanudin%2C+U+F">U. F. Burhanudin</a>, <a href="/search/astro-ph?searchtype=author&query=Maund%2C+J+R">J. R. Maund</a>, <a href="/search/astro-ph?searchtype=author&query=Killestein%2C+T">T. Killestein</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Dyer%2C+M+J">M. J. Dyer</a>, <a href="/search/astro-ph?searchtype=author&query=Lyman%2C+J">J. Lyman</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Cutter%2C+R">R. Cutter</a>, <a href="/search/astro-ph?searchtype=author&query=Mong%2C+Y+-">Y. -L. Mong</a>, <a href="/search/astro-ph?searchtype=author&query=Steeghs%2C+D">D. Steeghs</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Dhillon%2C+V">V. Dhillon</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Brien%2C+P">P. O'Brien</a>, <a href="/search/astro-ph?searchtype=author&query=Ramsay%2C+G">G. Ramsay</a>, <a href="/search/astro-ph?searchtype=author&query=Noysena%2C+K">K. Noysena</a>, <a href="/search/astro-ph?searchtype=author&query=Kotak%2C+R">R. Kotak</a>, <a href="/search/astro-ph?searchtype=author&query=Breton%2C+R+P">R. P. Breton</a>, <a href="/search/astro-ph?searchtype=author&query=Nuttall%2C+L">L. Nuttall</a>, <a href="/search/astro-ph?searchtype=author&query=Pall%C3%A9%2C+E">E. Pall茅</a>, <a href="/search/astro-ph?searchtype=author&query=Pollacco%2C+D">D. Pollacco</a>, <a href="/search/astro-ph?searchtype=author&query=Thrane%2C+E">E. Thrane</a>, <a href="/search/astro-ph?searchtype=author&query=Awiphan%2C+S">S. Awiphan</a>, <a href="/search/astro-ph?searchtype=author&query=Chote%2C+P">P. Chote</a>, <a href="/search/astro-ph?searchtype=author&query=Chrimes%2C+A">A. Chrimes</a>, <a href="/search/astro-ph?searchtype=author&query=Daw%2C+E">E. Daw</a> , et al. (20 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="2105.11169v2-abstract-short" style="display: inline;"> The advent of wide-field sky surveys has led to the growth of transient and variable source discoveries. The data deluge produced by these surveys has necessitated the use of machine learning (ML) and deep learning (DL) algorithms to sift through the vast incoming data stream. A problem that arises in real-world applications of learning algorithms for classification is imbalanced data, where a cla… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.11169v2-abstract-full').style.display = 'inline'; document.getElementById('2105.11169v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.11169v2-abstract-full" style="display: none;"> The advent of wide-field sky surveys has led to the growth of transient and variable source discoveries. The data deluge produced by these surveys has necessitated the use of machine learning (ML) and deep learning (DL) algorithms to sift through the vast incoming data stream. A problem that arises in real-world applications of learning algorithms for classification is imbalanced data, where a class of objects within the data is underrepresented, leading to a bias for over-represented classes in the ML and DL classifiers. We present a recurrent neural network (RNN) classifier that takes in photometric time-series data and additional contextual information (such as distance to nearby galaxies and on-sky position) to produce real-time classification of objects observed by the Gravitational-wave Optical Transient Observer (GOTO), and use an algorithm-level approach for handling imbalance with a focal loss function. The classifier is able to achieve an Area Under the Curve (AUC) score of 0.972 when using all available photometric observations to classify variable stars, supernovae, and active galactic nuclei. The RNN architecture allows us to classify incomplete light curves, and measure how performance improves as more observations are included. We also investigate the role that contextual information plays in producing reliable object classification. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.11169v2-abstract-full').style.display = 'none'; document.getElementById('2105.11169v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 12 figures, to be published in Monthly Notices of the Royal Astronomical Society</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.10108">arXiv:2105.10108</a> <span> [<a href="https://arxiv.org/pdf/2105.10108">pdf</a>, <a href="https://arxiv.org/format/2105.10108">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"> CDF-S XT1: The off-axis afterglow of a neutron star merger at $z=2.23$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sarin%2C+N">Nikhil Sarin</a>, <a href="/search/astro-ph?searchtype=author&query=Ashton%2C+G">Gregory Ashton</a>, <a href="/search/astro-ph?searchtype=author&query=Lasky%2C+P+D">Paul D. Lasky</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">Kendall Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Mong%2C+Y">Yik-Lun Mong</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">Duncan K. Galloway</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="2105.10108v1-abstract-short" style="display: inline;"> CDF-S XT1 is a fast-rising non-thermal X-ray transient detected by \textit{Chandra} in the Deep-Field South Survey. Although various hypotheses have been suggested, the origin of this transient remains unclear. Here, we show that the observations of CDF-S XT1 are well explained as the X-ray afterglow produced by a relativistic structured jet viewed off-axis. We measure properties of the jet, showi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.10108v1-abstract-full').style.display = 'inline'; document.getElementById('2105.10108v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.10108v1-abstract-full" style="display: none;"> CDF-S XT1 is a fast-rising non-thermal X-ray transient detected by \textit{Chandra} in the Deep-Field South Survey. Although various hypotheses have been suggested, the origin of this transient remains unclear. Here, we show that the observations of CDF-S XT1 are well explained as the X-ray afterglow produced by a relativistic structured jet viewed off-axis. We measure properties of the jet, showing that they are similar to those of GRB170817A, albeit at cosmological distances. We measure the observers viewing angle to be $胃_{\textrm{obs}} = 10^{\circ}\pm3^{\circ}$ and the core of the ultra-relativistic jet to be $胃_{\textrm{core}} = 4.4^{\circ}\pm0.9^{\circ}$, where the uncertainties are the $68\%$ credible interval. The inferred properties and host galaxy combined with Hubble, radio, and optical non detections favour the hypothesis that CDF-S XT1 is the off-axis afterglow of a binary neutron star merger. We find that other previously suggested hypotheses are unable to explain all properties of CDF-S XT1. At a redshift of $z=2.23$, this is potentially the most distant observed neutron star merger to date and the first orphan afterglow of a short gamma-ray burst. We discuss the implications of a binary neutron star merger at such a high redshift for the star-formation rate in the early Universe, the nucleosynthesis of heavy elements, and the prospect of identifying other off-axis afterglows. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.10108v1-abstract-full').style.display = 'none'; document.getElementById('2105.10108v1-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">Submitted to ApJL, 8 Pages, 3 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/2105.05128">arXiv:2105.05128</a> <span> [<a href="https://arxiv.org/pdf/2105.05128">pdf</a>, <a href="https://arxiv.org/format/2105.05128">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1017/pasa.2021.19">10.1017/pasa.2021.19 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Processing GOTO data with the Rubin Observatory LSST Science Pipelines II: Forced Photometry and light curves </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Makrygianni%2C+L">L. Makrygianni</a>, <a href="/search/astro-ph?searchtype=author&query=Mullaney%2C+J">J. Mullaney</a>, <a href="/search/astro-ph?searchtype=author&query=Dhillon%2C+V">V. Dhillon</a>, <a href="/search/astro-ph?searchtype=author&query=Littlefair%2C+S">S. Littlefair</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Dyer%2C+M+J">M. J. Dyer</a>, <a href="/search/astro-ph?searchtype=author&query=Lyman%2C+J">J. Lyman</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Cutter%2C+R">R. Cutter</a>, <a href="/search/astro-ph?searchtype=author&query=Mong%2C+Y+-">Y. -L. Mong</a>, <a href="/search/astro-ph?searchtype=author&query=Steeghs%2C+D">D. Steeghs</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Brien%2C+P">P. O'Brien</a>, <a href="/search/astro-ph?searchtype=author&query=Ramsay%2C+G">G. Ramsay</a>, <a href="/search/astro-ph?searchtype=author&query=Poshyachinda%2C+S">S. Poshyachinda</a>, <a href="/search/astro-ph?searchtype=author&query=Kotak%2C+R">R. Kotak</a>, <a href="/search/astro-ph?searchtype=author&query=Nuttall%2C+L">L. Nuttall</a>, <a href="/search/astro-ph?searchtype=author&query=Pall%C3%A9%2C+E">E. Pall茅</a>, <a href="/search/astro-ph?searchtype=author&query=Pollacco%2C+D">D. Pollacco</a>, <a href="/search/astro-ph?searchtype=author&query=Thrane%2C+E">E. Thrane</a>, <a href="/search/astro-ph?searchtype=author&query=Aukkaravittayapun%2C+S">S. Aukkaravittayapun</a>, <a href="/search/astro-ph?searchtype=author&query=Awiphan%2C+S">S. Awiphan</a>, <a href="/search/astro-ph?searchtype=author&query=Breton%2C+R">R. Breton</a>, <a href="/search/astro-ph?searchtype=author&query=Burhanudin%2C+U">U. Burhanudin</a>, <a href="/search/astro-ph?searchtype=author&query=Chote%2C+P">P. Chote</a> , et al. (23 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="2105.05128v1-abstract-short" style="display: inline;"> We have adapted the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) Science Pipelines to process data from the Gravitational-Wave Optical Transient Observer (GOTO) prototype. In this paper, we describe how we used the Rubin Observatory LSST Science Pipelines to conduct forced photometry measurements on nightly GOTO data. By comparing the photometry measurements of sources taken on… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.05128v1-abstract-full').style.display = 'inline'; document.getElementById('2105.05128v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.05128v1-abstract-full" style="display: none;"> We have adapted the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) Science Pipelines to process data from the Gravitational-Wave Optical Transient Observer (GOTO) prototype. In this paper, we describe how we used the Rubin Observatory LSST Science Pipelines to conduct forced photometry measurements on nightly GOTO data. By comparing the photometry measurements of sources taken on multiple nights, we find that the precision of our photometry is typically better than 20~mmag for sources brighter than 16 mag. We also compare our photometry measurements against colour-corrected PanSTARRS photometry, and find that the two agree to within 10~mmag (1$蟽$) for bright (i.e., $\sim14^{\rm th}$~mag) sources to 200~mmag for faint (i.e., $\sim18^{\rm th}$~mag) sources. Additionally, we compare our results to those obtained by GOTO's own in-house pipeline, {\sc gotophoto}, and obtain similar results. Based on repeatability measurements, we measure a $5蟽$ L-band survey depth of between 19 and 20 magnitudes, depending on observing conditions. We assess, using repeated observations of non-varying standard SDSS stars, the accuracy of our uncertainties, which we find are typically overestimated by roughly a factor of two for bright sources (i.e., $<15^{\rm th}$~mag), but slightly underestimated (by roughly a factor of 1.25) for fainter sources ($>17^{\rm th}$~mag). Finally, we present lightcurves for a selection of variable sources, and compare them to those obtained with the Zwicky Transient Factory and GAIA. Despite the Rubin Observatory LSST Science Pipelines still undergoing active development, our results show that they are already delivering robust forced photometry measurements from GOTO data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.05128v1-abstract-full').style.display = 'none'; document.getElementById('2105.05128v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in PASA</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.11687">arXiv:2102.11687</a> <span> [<a href="https://arxiv.org/pdf/2102.11687">pdf</a>, <a href="https://arxiv.org/format/2102.11687">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/10.1051/0004-6361/202140360">10.1051/0004-6361/202140360 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Broad-band X-ray spectra and timing of the accretion-powered millisecond pulsar Swift J1756.9$-$2508 during its 2018 and 2019 outbursts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+Z+S">Z. S. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Kuiper%2C+L">L. Kuiper</a>, <a href="/search/astro-ph?searchtype=author&query=Falanga%2C+M">M. Falanga</a>, <a href="/search/astro-ph?searchtype=author&query=Poutanen%2C+J">J. Poutanen</a>, <a href="/search/astro-ph?searchtype=author&query=Tsygankov%2C+S+S">S. S. Tsygankov</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Bozzo%2C+E">E. Bozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+Y+Y">Y. Y. Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+Y">Y. Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+S+N">S. N. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+S">S. Zhang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2102.11687v2-abstract-short" style="display: inline;"> The accreting millisecond X-ray pulsar Swift J1756.9$-$2508 went into outburst in April 2018 and June 2019, 8.7 yr after the previous activity period. We investigated the temporal, timing and spectral properties of these two outbursts using data from NICER, XMM-Newton, NuSTAR, INTEGRAL, Swift and Insight-HXMT. The two outbursts exhibited similar broad-band spectra and X-ray pulse profiles. For the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.11687v2-abstract-full').style.display = 'inline'; document.getElementById('2102.11687v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.11687v2-abstract-full" style="display: none;"> The accreting millisecond X-ray pulsar Swift J1756.9$-$2508 went into outburst in April 2018 and June 2019, 8.7 yr after the previous activity period. We investigated the temporal, timing and spectral properties of these two outbursts using data from NICER, XMM-Newton, NuSTAR, INTEGRAL, Swift and Insight-HXMT. The two outbursts exhibited similar broad-band spectra and X-ray pulse profiles. For the first time, we report the detection of the pulsed emission up to $\sim100$ keV observed by Insight-HXMT during the 2018 outburst. We also found the pulsation up to $\sim60$ keV observed by NICER and NuSTAR during the 2019 outburst. We performed a coherent timing analysis combining the data from two outbursts. The binary system is well described by a constant orbital period over a time span of $\sim12$ years. The time-averaged broad-band spectra are well fitted by an absorbed thermal Comptonization model in a slab geometry with the electron temperature $kT_{\rm e}=40$-50 keV, Thomson optical depth $蟿\sim 1.3$, blackbody seed photon temperature $kT_{\rm bb,seed}\sim $0.7-0.8 keV and hydrogen column density of $N_{\rm H}\sim 4.2\times10^{22}$ cm$^{-2}$. We searched the available data for type-I (thermonuclear) X-ray bursts, but found none, which is unsurprising given the estimated low peak accretion rate ($\approx0.05$ of the Eddington rate) and generally low expected burst rates for hydrogen-poor fuel. Based on the history of four outbursts to date, we estimate the long-term average accretion rate at roughly $5\times10^{-12}\ M_\odot\,{\rm yr}^{-1}$ for an assumed distance of 8 kpc. The expected mass transfer rate driven by gravitational radiation in the binary implies the source can be no closer than 4 kpc. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.11687v2-abstract-full').style.display = 'none'; document.getElementById('2102.11687v2-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 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in 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 649, A76 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.09892">arXiv:2102.09892</a> <span> [<a href="https://arxiv.org/pdf/2102.09892">pdf</a>, <a href="https://arxiv.org/format/2102.09892">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 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/stab633">10.1093/mnras/stab633 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Transient-optimised real-bogus classification with Bayesian Convolutional Neural Networks -- sifting the GOTO candidate stream </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Killestein%2C+T+L">T. L. Killestein</a>, <a href="/search/astro-ph?searchtype=author&query=Lyman%2C+J">J. Lyman</a>, <a href="/search/astro-ph?searchtype=author&query=Steeghs%2C+D">D. Steeghs</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Dyer%2C+M+J">M. J. Dyer</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Cutter%2C+R">R. Cutter</a>, <a href="/search/astro-ph?searchtype=author&query=Mong%2C+Y+-">Y. -L. Mong</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Dhillon%2C+V">V. Dhillon</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Brien%2C+P">P. O'Brien</a>, <a href="/search/astro-ph?searchtype=author&query=Ramsay%2C+G">G. Ramsay</a>, <a href="/search/astro-ph?searchtype=author&query=Poshyachinda%2C+S">S. Poshyachinda</a>, <a href="/search/astro-ph?searchtype=author&query=Kotak%2C+R">R. Kotak</a>, <a href="/search/astro-ph?searchtype=author&query=Breton%2C+R+P">R. P. Breton</a>, <a href="/search/astro-ph?searchtype=author&query=Nuttall%2C+L+K">L. K. Nuttall</a>, <a href="/search/astro-ph?searchtype=author&query=Pall%C3%A9%2C+E">E. Pall茅</a>, <a href="/search/astro-ph?searchtype=author&query=Pollacco%2C+D">D. Pollacco</a>, <a href="/search/astro-ph?searchtype=author&query=Thrane%2C+E">E. Thrane</a>, <a href="/search/astro-ph?searchtype=author&query=Aukkaravittayapun%2C+S">S. Aukkaravittayapun</a>, <a href="/search/astro-ph?searchtype=author&query=Awiphan%2C+S">S. Awiphan</a>, <a href="/search/astro-ph?searchtype=author&query=Burhanudin%2C+U">U. Burhanudin</a>, <a href="/search/astro-ph?searchtype=author&query=Chote%2C+P">P. Chote</a>, <a href="/search/astro-ph?searchtype=author&query=Chrimes%2C+A">A. Chrimes</a>, <a href="/search/astro-ph?searchtype=author&query=Daw%2C+E">E. Daw</a> , et al. (23 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="2102.09892v1-abstract-short" style="display: inline;"> Large-scale sky surveys have played a transformative role in our understanding of astrophysical transients, only made possible by increasingly powerful machine learning-based filtering to accurately sift through the vast quantities of incoming data generated. In this paper, we present a new real-bogus classifier based on a Bayesian convolutional neural network that provides nuanced, uncertainty-aw… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.09892v1-abstract-full').style.display = 'inline'; document.getElementById('2102.09892v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.09892v1-abstract-full" style="display: none;"> Large-scale sky surveys have played a transformative role in our understanding of astrophysical transients, only made possible by increasingly powerful machine learning-based filtering to accurately sift through the vast quantities of incoming data generated. In this paper, we present a new real-bogus classifier based on a Bayesian convolutional neural network that provides nuanced, uncertainty-aware classification of transient candidates in difference imaging, and demonstrate its application to the datastream from the GOTO wide-field optical survey. Not only are candidates assigned a well-calibrated probability of being real, but also an associated confidence that can be used to prioritise human vetting efforts and inform future model optimisation via active learning. To fully realise the potential of this architecture, we present a fully-automated training set generation method which requires no human labelling, incorporating a novel data-driven augmentation method to significantly improve the recovery of faint and nuclear transient sources. We achieve competitive classification accuracy (FPR and FNR both below 1%) compared against classifiers trained with fully human-labelled datasets, whilst being significantly quicker and less labour-intensive to build. This data-driven approach is uniquely scalable to the upcoming challenges and data needs of next-generation transient surveys. We make our data generation and model training codes available to the community. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.09892v1-abstract-full').style.display = 'none'; document.getElementById('2102.09892v1-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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, 12 figures, resubmitted to MNRAS following reviewer 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/2102.04428">arXiv:2102.04428</a> <span> [<a href="https://arxiv.org/pdf/2102.04428">pdf</a>, <a href="https://arxiv.org/format/2102.04428">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stab389">10.1093/mnras/stab389 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evidence that short period AM CVn systems are diverse in outburst behaviour </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Duffy%2C+C">C. Duffy</a>, <a href="/search/astro-ph?searchtype=author&query=Ramsay%2C+G">G. Ramsay</a>, <a href="/search/astro-ph?searchtype=author&query=Steeghs%2C+D">D. Steeghs</a>, <a href="/search/astro-ph?searchtype=author&query=Dhillon%2C+V">V. Dhillon</a>, <a href="/search/astro-ph?searchtype=author&query=Kennedy%2C+M+R">Mark R. Kennedy</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+D+M">D. Mata S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Dyer%2C+M">M. Dyer</a>, <a href="/search/astro-ph?searchtype=author&query=Lyman%2C+J">J. Lyman</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Brien%2C+P">P. O'Brien</a>, <a href="/search/astro-ph?searchtype=author&query=Noysena%2C+K">K. Noysena</a>, <a href="/search/astro-ph?searchtype=author&query=Nuttall%2C+L">L. Nuttall</a>, <a href="/search/astro-ph?searchtype=author&query=Pollacco%2C+D">D. Pollacco</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="2102.04428v1-abstract-short" style="display: inline;"> We present results of our analysis of up to 15 years of photometric data from eight AM CVn systems with orbital periods between 22.5 and 26.8 min. Our data has been collected from the GOTO, ZTF, Pan-STARRS, ASAS-SN and Catalina all-sky surveys and amateur observations collated by the AAVSO. We find evidence that these interacting ultra-compact binaries show a similar diversity of long term optical… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.04428v1-abstract-full').style.display = 'inline'; document.getElementById('2102.04428v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.04428v1-abstract-full" style="display: none;"> We present results of our analysis of up to 15 years of photometric data from eight AM CVn systems with orbital periods between 22.5 and 26.8 min. Our data has been collected from the GOTO, ZTF, Pan-STARRS, ASAS-SN and Catalina all-sky surveys and amateur observations collated by the AAVSO. We find evidence that these interacting ultra-compact binaries show a similar diversity of long term optical properties as the hydrogen accreting dwarf novae. We found that AM CVn systems in the previously identified accretion disc instability region are not a homogenous group. Various members of the analysed sample exhibit behaviour reminiscent of Z Cam systems with long super outbursts and standstills, SU UMa systems with regular, shorter super outbursts, and nova-like systems which appear only in a high state. The addition of TESS full frame images of one of these systems, KL Dra, reveals the first evidence for normal outbursts appearing as a precursor to super outbursts in an AM CVn system. Our results will inform theoretical modelling of the outbursts of hydrogen deficient systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.04428v1-abstract-full').style.display = 'none'; document.getElementById('2102.04428v1-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 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">11 Pages, 7 Figures, 2 Tables. Accepted for publication in MNRAS. Author's final submitted version</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.02686">arXiv:2012.02686</a> <span> [<a href="https://arxiv.org/pdf/2012.02686">pdf</a>, <a href="https://arxiv.org/format/2012.02686">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.2561506">10.1117/12.2561506 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Developing the GOTO telescope control system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dyer%2C+M+J">Martin J. Dyer</a>, <a href="/search/astro-ph?searchtype=author&query=Dhillon%2C+V+S">Vik S. Dhillon</a>, <a href="/search/astro-ph?searchtype=author&query=Littlefair%2C+S">Stuart Littlefair</a>, <a href="/search/astro-ph?searchtype=author&query=Steeghs%2C+D">Danny Steeghs</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">Krzysztof Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Chote%2C+P">Paul Chote</a>, <a href="/search/astro-ph?searchtype=author&query=Lyman%2C+J">Joseph Lyman</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">Duncan K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">Kendall Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Mong%2C+Y+L">Yik Lun Mong</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.02686v1-abstract-short" style="display: inline;"> The Gravitational-wave Optical Transient Observer (GOTO) is a wide-field telescope project focused on detecting optical counterparts to gravitational-wave sources. The GOTO Telescope Control System (G-TeCS) is a custom robotic control system which autonomously manages the GOTO telescope hardware and nightly operations. Since the commissioning the GOTO prototype on La Palma in 2017, development of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02686v1-abstract-full').style.display = 'inline'; document.getElementById('2012.02686v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.02686v1-abstract-full" style="display: none;"> The Gravitational-wave Optical Transient Observer (GOTO) is a wide-field telescope project focused on detecting optical counterparts to gravitational-wave sources. The GOTO Telescope Control System (G-TeCS) is a custom robotic control system which autonomously manages the GOTO telescope hardware and nightly operations. Since the commissioning the GOTO prototype on La Palma in 2017, development of the control system has focused on the alert handling and scheduling systems. These allow GOTO to receive and process transient alerts and then schedule and carry out observations, all without the need for human involvement. GOTO is ultimately anticipated to include multiple telescope arrays on independent mounts, both on La Palma and at a southern site in Australia. When complete these mounts will be linked to form a single multi-site observatory, requiring more advanced scheduling systems to best optimise survey and follow-up observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02686v1-abstract-full').style.display = 'none'; document.getElementById('2012.02686v1-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 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 6 figures, 2 tables, submitted to SPIE Astronomical Telescopes + Instrumentation 2020</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proc. SPIE 11452, Software and Cyberinfrastructure for Astronomy VI, 114521Q (13 December 2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.02685">arXiv:2012.02685</a> <span> [<a href="https://arxiv.org/pdf/2012.02685">pdf</a>, <a href="https://arxiv.org/format/2012.02685">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="General Relativity and Quantum Cosmology">gr-qc</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/10.1117/12.2561008">10.1117/12.2561008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Gravitational-wave Optical Transient Observer (GOTO) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dyer%2C+M+J">Martin J. Dyer</a>, <a href="/search/astro-ph?searchtype=author&query=Steeghs%2C+D">Danny Steeghs</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">Duncan K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Dhillon%2C+V+S">Vik S. Dhillon</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Brien%2C+P">Paul O'Brien</a>, <a href="/search/astro-ph?searchtype=author&query=Ramsay%2C+G">Gavin Ramsay</a>, <a href="/search/astro-ph?searchtype=author&query=Noysena%2C+K">Kanthanakorn Noysena</a>, <a href="/search/astro-ph?searchtype=author&query=Pall%C3%A9%2C+E">Enric Pall茅</a>, <a href="/search/astro-ph?searchtype=author&query=Kotak%2C+R">Rubina Kotak</a>, <a href="/search/astro-ph?searchtype=author&query=Breton%2C+R">Rene Breton</a>, <a href="/search/astro-ph?searchtype=author&query=Nuttall%2C+L">Laura Nuttall</a>, <a href="/search/astro-ph?searchtype=author&query=Pollacco%2C+D">Don Pollacco</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">Krzysztof Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Lyman%2C+J">Joseph Lyman</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">Kendall Ackley</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.02685v1-abstract-short" style="display: inline;"> The Gravitational-wave Optical Transient Observer (GOTO) is a wide-field telescope project focused on detecting optical counterparts to gravitational-wave sources. GOTO uses arrays of 40 cm unit telescopes (UTs) on a shared robotic mount, which scales to provide large fields of view in a cost-effective manner. A complete GOTO mount uses 8 unit telescopes to give an overall field of view of 40 squa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02685v1-abstract-full').style.display = 'inline'; document.getElementById('2012.02685v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.02685v1-abstract-full" style="display: none;"> The Gravitational-wave Optical Transient Observer (GOTO) is a wide-field telescope project focused on detecting optical counterparts to gravitational-wave sources. GOTO uses arrays of 40 cm unit telescopes (UTs) on a shared robotic mount, which scales to provide large fields of view in a cost-effective manner. A complete GOTO mount uses 8 unit telescopes to give an overall field of view of 40 square degrees, and can reach a depth of 20th magnitude in three minutes. The GOTO-4 prototype was inaugurated with 4 unit telescopes in 2017 on La Palma, and was upgraded to a full 8-telescope array in 2020. A second 8-UT mount will be installed on La Palma in early 2021, and another GOTO node with two more mount systems is planned for a southern site in Australia. When complete, each mount will be networked to form a robotic, dual-hemisphere observatory, which will survey the entire visible sky every few nights and enable rapid follow-up detections of transient sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02685v1-abstract-full').style.display = 'none'; document.getElementById('2012.02685v1-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 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 5 figures, 1 table, submitted to SPIE Astronomical Telescopes + Instrumentation 2020</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proc. SPIE 11445, Ground-based and Airborne Telescopes VIII, 114457G (13 December 2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.15142">arXiv:2010.15142</a> <span> [<a href="https://arxiv.org/pdf/2010.15142">pdf</a>, <a href="https://arxiv.org/format/2010.15142">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1017/pasa.2020.45">10.1017/pasa.2020.45 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Processing GOTO data with the Rubin Observatory LSST Science Pipelines I : Production of coadded frames </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mullaney%2C+J+R">J. R. Mullaney</a>, <a href="/search/astro-ph?searchtype=author&query=Makrygianni%2C+L">L. Makrygianni</a>, <a href="/search/astro-ph?searchtype=author&query=Dhillon%2C+V">V. Dhillon</a>, <a href="/search/astro-ph?searchtype=author&query=Littlefair%2C+S">S. Littlefair</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Dyer%2C+M">M. Dyer</a>, <a href="/search/astro-ph?searchtype=author&query=Lyman%2C+J">J. Lyman</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Cutter%2C+R">R. Cutter</a>, <a href="/search/astro-ph?searchtype=author&query=Mong%2C+Y+L">Y. L. Mong</a>, <a href="/search/astro-ph?searchtype=author&query=Steeghs%2C+D">D. Steeghs</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Brien%2C+P">P. O'Brien</a>, <a href="/search/astro-ph?searchtype=author&query=Ramsay%2C+G">G. Ramsay</a>, <a href="/search/astro-ph?searchtype=author&query=Poshyachinda%2C+S">S. Poshyachinda</a>, <a href="/search/astro-ph?searchtype=author&query=Kotak%2C+R">R. Kotak</a>, <a href="/search/astro-ph?searchtype=author&query=Nuttall%2C+L">L. Nuttall</a>, <a href="/search/astro-ph?searchtype=author&query=Pall%C3%A9%2C+E">E. Pall茅</a>, <a href="/search/astro-ph?searchtype=author&query=Pollacco%2C+D">D. Pollacco</a>, <a href="/search/astro-ph?searchtype=author&query=Thrane%2C+E">E. Thrane</a>, <a href="/search/astro-ph?searchtype=author&query=Aukkaravittayapun%2C+S">S. Aukkaravittayapun</a>, <a href="/search/astro-ph?searchtype=author&query=Awiphan%2C+S">S. Awiphan</a>, <a href="/search/astro-ph?searchtype=author&query=Breton%2C+R">R. Breton</a>, <a href="/search/astro-ph?searchtype=author&query=Burhanudin%2C+U">U. Burhanudin</a>, <a href="/search/astro-ph?searchtype=author&query=Chote%2C+P">P. Chote</a> , et al. (22 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="2010.15142v1-abstract-short" style="display: inline;"> The past few decades have seen the burgeoning of wide field, high cadence surveys, the most formidable of which will be the Legacy Survey of Space and Time (LSST) to be conducted by the Vera C. Rubin Observatory. So new is the field of systematic time-domain survey astronomy, however, that major scientific insights will continue to be obtained using smaller, more flexible systems than the LSST. On… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.15142v1-abstract-full').style.display = 'inline'; document.getElementById('2010.15142v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.15142v1-abstract-full" style="display: none;"> The past few decades have seen the burgeoning of wide field, high cadence surveys, the most formidable of which will be the Legacy Survey of Space and Time (LSST) to be conducted by the Vera C. Rubin Observatory. So new is the field of systematic time-domain survey astronomy, however, that major scientific insights will continue to be obtained using smaller, more flexible systems than the LSST. One such example is the Gravitational-wave Optical Transient Observer (GOTO), whose primary science objective is the optical follow-up of Gravitational Wave events. The amount and rate of data production by GOTO and other wide-area, high-cadence surveys presents a significant challenge to data processing pipelines which need to operate in near real-time to fully exploit the time-domain. In this study, we adapt the Rubin Observatory LSST Science Pipelines to process GOTO data, thereby exploring the feasibility of using this "off-the-shelf" pipeline to process data from other wide-area, high-cadence surveys. In this paper, we describe how we use the LSST Science Pipelines to process raw GOTO frames to ultimately produce calibrated coadded images and photometric source catalogues. After comparing the measured astrometry and photometry to those of matched sources from PanSTARRS DR1, we find that measured source positions are typically accurate to sub-pixel levels, and that measured L-band photometries are accurate to $\sim50$ mmag at $m_L\sim16$ and $\sim200$ mmag at $m_L\sim18$. These values compare favourably to those obtained using GOTO's primary, in-house pipeline, GOTOPHOTO, in spite of both pipelines having undergone further development and improvement beyond the implementations used in this study. Finally, we release a generic "obs package" that others can build-upon should they wish to use the LSST Science Pipelines to process data from other facilities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.15142v1-abstract-full').style.display = 'none'; document.getElementById('2010.15142v1-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">17 pages, 13 figures. Accepted for publication in PASA</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.01536">arXiv:2009.01536</a> <span> [<a href="https://arxiv.org/pdf/2009.01536">pdf</a>, <a href="https://arxiv.org/format/2009.01536">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/staa3224">10.1093/mnras/staa3224 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detection of Millihertz Quasi-Periodic Oscillations in the X-Ray Binary 1RXS J180408.9$-$342058 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tse%2C+K">Kaho Tse</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">Duncan K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Chou%2C+Y">Yi Chou</a>, <a href="/search/astro-ph?searchtype=author&query=Heger%2C+A">Alexander Heger</a>, <a href="/search/astro-ph?searchtype=author&query=Hsieh%2C+H">Hung-En Hsieh</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2009.01536v2-abstract-short" style="display: inline;"> Millihertz quasi-periodic oscillations (mHz QPOs) observed in neutron-star low-mass X-ray binaries (NS LMXBs) are generally explained as marginally stable thermonuclear burning on the neutron star surface. We report the discovery of mHz QPOs in an XMM-Newton observation of the transient 1RXS J180408.9$-$342058, during a regular bursting phase of its 2015 outburst. We found significant periodic sig… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.01536v2-abstract-full').style.display = 'inline'; document.getElementById('2009.01536v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.01536v2-abstract-full" style="display: none;"> Millihertz quasi-periodic oscillations (mHz QPOs) observed in neutron-star low-mass X-ray binaries (NS LMXBs) are generally explained as marginally stable thermonuclear burning on the neutron star surface. We report the discovery of mHz QPOs in an XMM-Newton observation of the transient 1RXS J180408.9$-$342058, during a regular bursting phase of its 2015 outburst. We found significant periodic signals in the March observation, with frequencies in the range $5-8\,\mathrm{mHz}$, superimposed on a strong $\sim1/f$ power-law noise continuum. Neither the QPO signals nor the power-law noise were present during the April observation, which exhibited a $2.5\times$ higher luminosity and had correspondingly more frequent bursts. When present, the QPO signal power decreases during bursts and disappears afterwards, similar to the behaviour in other sources. 1RXS J180408.9$-$342058 is the eighth source known to date that exhibits such QPOs driven by thermonuclear burning. We examine the range of properties of the QPO signals in different sources. Whereas the observed oscillation profile is similar to that predicted by numerical models, the amplitudes are significantly higher, challenging their explanation as originating from marginally stable burning. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.01536v2-abstract-full').style.display = 'none'; document.getElementById('2009.01536v2-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 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 6 figures, 1 table, accepted by MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.08081">arXiv:2007.08081</a> <span> [<a href="https://arxiv.org/pdf/2007.08081">pdf</a>, <a href="https://arxiv.org/ps/2007.08081">ps</a>, <a href="https://arxiv.org/format/2007.08081">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/staa2858">10.1093/mnras/staa2858 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The efficiency of nuclear burning during thermonuclear (Type I) bursts as a function of accretion rate </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cavecchi%2C+Y">Y. Cavecchi</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Goodwin%2C+A+J">A. J. Goodwin</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+Z">Z. Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Heger%2C+A">A. Heger</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2007.08081v1-abstract-short" style="display: inline;"> We measured the thermonuclear burning efficiency as a function of accretion rate for the Type I X-ray bursts of five low-mass X-ray binary systems. We chose sources with measured neutron star spins and a substantial population of bursts from a large observational sample. The general trend for the burst rate is qualitatively the same for all sources; the burst rate first increases with the accretio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.08081v1-abstract-full').style.display = 'inline'; document.getElementById('2007.08081v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.08081v1-abstract-full" style="display: none;"> We measured the thermonuclear burning efficiency as a function of accretion rate for the Type I X-ray bursts of five low-mass X-ray binary systems. We chose sources with measured neutron star spins and a substantial population of bursts from a large observational sample. The general trend for the burst rate is qualitatively the same for all sources; the burst rate first increases with the accretion rate up to a maximum, above which the burst rate declines, despite the increasing accretion rate. At higher accretion rates, when the burst rate decreases, the 伪-value (the ratio of accretion energy and burst energy) increases by up to a factor of 10 above that in the rising burst rate regime. These observations are contrary to the predictions of 1D numerical models, but can be explained as the consequence of a zone of stable burning on the neutron star surface, which expands with increasing accretion rate. The stable burning also "pollutes" the unstable burning layer with ashes, contributing to the change in burst properties measured in the falling burst rate regime. We find that the mass accretion rate at which the burst rate begins to decrease is anti-correlated with the spin of the neutron star. We conclude that the neutron star spin is a key factor, moderating the nuclear burning stability, via the local accretion rate and fuel composition over the star. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.08081v1-abstract-full').style.display = 'none'; document.getElementById('2007.08081v1-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.03128">arXiv:2007.03128</a> <span> [<a href="https://arxiv.org/pdf/2007.03128">pdf</a>, <a href="https://arxiv.org/format/2007.03128">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1017/pasa.2020.39">10.1017/pasa.2020.39 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Neutron Star Extreme Matter Observatory: A kilohertz-band gravitational-wave detector in the global network </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Agrawal%2C+P">P. Agrawal</a>, <a href="/search/astro-ph?searchtype=author&query=Altin%2C+P">P. Altin</a>, <a href="/search/astro-ph?searchtype=author&query=Ashton%2C+G">G. Ashton</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Baltinas%2C+E">E. Baltinas</a>, <a href="/search/astro-ph?searchtype=author&query=Barbuio%2C+A">A. Barbuio</a>, <a href="/search/astro-ph?searchtype=author&query=Beniwal%2C+D">D. Beniwal</a>, <a href="/search/astro-ph?searchtype=author&query=Blair%2C+C">C. Blair</a>, <a href="/search/astro-ph?searchtype=author&query=Blair%2C+D">D. Blair</a>, <a href="/search/astro-ph?searchtype=author&query=Bolingbroke%2C+G+N">G. N. Bolingbroke</a>, <a href="/search/astro-ph?searchtype=author&query=Bossilkov%2C+V">V. Bossilkov</a>, <a href="/search/astro-ph?searchtype=author&query=Boublil%2C+S+S">S. Shachar Boublil</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+D+D">D. D. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Burridge%2C+B+J">B. J. Burridge</a>, <a href="/search/astro-ph?searchtype=author&query=Bustillo%2C+J+C">J. Calderon Bustillo</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+J">J. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+H+T">H. Tuong Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Carlin%2C+J+B">J. B. Carlin</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+S">S. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Charlton%2C+P">P. Charlton</a>, <a href="/search/astro-ph?searchtype=author&query=Chatterjee%2C+C">C. Chatterjee</a>, <a href="/search/astro-ph?searchtype=author&query=Chattopadhyay%2C+D">D. Chattopadhyay</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+X">X. Chen</a> , et al. (139 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="2007.03128v2-abstract-short" style="display: inline;"> Gravitational waves from coalescing neutron stars encode information about nuclear matter at extreme densities, inaccessible by laboratory experiments. The late inspiral is influenced by the presence of tides, which depend on the neutron star equation of state. Neutron star mergers are expected to often produce rapidly-rotating remnant neutron stars that emit gravitational waves. These will provid… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.03128v2-abstract-full').style.display = 'inline'; document.getElementById('2007.03128v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.03128v2-abstract-full" style="display: none;"> Gravitational waves from coalescing neutron stars encode information about nuclear matter at extreme densities, inaccessible by laboratory experiments. The late inspiral is influenced by the presence of tides, which depend on the neutron star equation of state. Neutron star mergers are expected to often produce rapidly-rotating remnant neutron stars that emit gravitational waves. These will provide clues to the extremely hot post-merger environment. This signature of nuclear matter in gravitational waves contains most information in the 2-4 kHz frequency band, which is outside of the most sensitive band of current detectors. We present the design concept and science case for a neutron star extreme matter observatory (NEMO): a gravitational-wave interferometer optimized to study nuclear physics with merging neutron stars. The concept uses high circulating laser power, quantum squeezing and a detector topology specifically designed to achieve the high-frequency sensitivity necessary to probe nuclear matter using gravitational waves. Above one kHz, the proposed strain sensitivity is comparable to full third-generation detectors at a fraction of the cost. Such sensitivity changes expected event rates for detection of post-merger remnants from approximately one per few decades with two A+ detectors to a few per year, and potentially allows for the first gravitational-wave observations of supernovae, isolated neutron stars, and other exotica. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.03128v2-abstract-full').style.display = 'none'; document.getElementById('2007.03128v2-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">v1</span> submitted 6 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in PASA</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> PASA (2020) 37, e047 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.02872">arXiv:2006.02872</a> <span> [<a href="https://arxiv.org/pdf/2006.02872">pdf</a>, <a href="https://arxiv.org/format/2006.02872">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/staa2588">10.1093/mnras/staa2588 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Enhanced optical activity 12 days before X-ray activity, and a 4 day X-ray delay during outburst rise, in a low-mass X-ray binary </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Goodwin%2C+A+J">A. J. Goodwin</a>, <a href="/search/astro-ph?searchtype=author&query=Russell%2C+D+M">D. M. Russell</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Baglio%2C+M+C">M. C. Baglio</a>, <a href="/search/astro-ph?searchtype=author&query=Parikh%2C+A+S">A. S. Parikh</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D+A+H">D. A. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Homan%2C+J">J. Homan</a>, <a href="/search/astro-ph?searchtype=author&query=Bramich%2C+D+M">D. M. Bramich</a>, <a href="/search/astro-ph?searchtype=author&query=Zand%2C+J+J+M+i+%27">J. J. M. in 't Zand</a>, <a href="/search/astro-ph?searchtype=author&query=Heinke%2C+C+O">C. O. Heinke</a>, <a href="/search/astro-ph?searchtype=author&query=Kotze%2C+E+J">E. J. Kotze</a>, <a href="/search/astro-ph?searchtype=author&query=de+Martino%2C+D">D. de Martino</a>, <a href="/search/astro-ph?searchtype=author&query=Papitto%2C+A">A. Papitto</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+F">F. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Wijnands%2C+R">R. Wijnands</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="2006.02872v2-abstract-short" style="display: inline;"> X-ray transients, such as accreting neutron stars, periodically undergo outbursts, thought to be caused by a thermal-viscous instability in the accretion disk. Usually outbursts of accreting neutron stars are identified when the accretion disk has undergone an instability, and the persistent X-ray flux has risen to a threshold detectable by all sky monitors on X-ray space observatories. Here we pr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.02872v2-abstract-full').style.display = 'inline'; document.getElementById('2006.02872v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.02872v2-abstract-full" style="display: none;"> X-ray transients, such as accreting neutron stars, periodically undergo outbursts, thought to be caused by a thermal-viscous instability in the accretion disk. Usually outbursts of accreting neutron stars are identified when the accretion disk has undergone an instability, and the persistent X-ray flux has risen to a threshold detectable by all sky monitors on X-ray space observatories. Here we present the earliest known combined optical, UV, and X-ray monitoring observations of the outburst onset of an accreting neutron star low mass X-ray binary system. We observed a significant, continuing increase in the optical i'-band magnitude starting on July 25, 12 days before the first X-ray detection with Swift/XRT and NICER (August 6), during the onset of the 2019 outburst of SAX J1808.4-3658. We also observed a 4 day optical to X-ray rise delay, and a 2 day UV to X-ray delay, at the onset of the outburst. We present the multiwavelength observations that were obtained, discussing the theory of outbursts in X-ray transients, including the disk instability model, and the implications of the delay. This work is an important confirmation of the delay in optical to X-ray emission during the onset of outbursts in low mass X-ray binaries, which has only previously been measured with less sensitive all sky monitors. We find observational evidence that the outburst is triggered by ionisation of hydrogen in the disk. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.02872v2-abstract-full').style.display = 'none'; document.getElementById('2006.02872v2-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">12 pages, 5 figures, accepted by MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.00025">arXiv:2004.00025</a> <span> [<a href="https://arxiv.org/pdf/2004.00025">pdf</a>, <a href="https://arxiv.org/format/2004.00025">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/staa1845">10.1093/mnras/staa1845 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searching for Electromagnetic Counterparts to Gravitational-wave Merger Events with the Prototype Gravitational-wave Optical Transient Observer (GOTO-4) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gompertz%2C+B+P">B. P. Gompertz</a>, <a href="/search/astro-ph?searchtype=author&query=Cutter%2C+R">R. Cutter</a>, <a href="/search/astro-ph?searchtype=author&query=Steeghs%2C+D">D. Steeghs</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Lyman%2C+J">J. Lyman</a>, <a href="/search/astro-ph?searchtype=author&query=Ulaczyk%2C+K">K. Ulaczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Dyer%2C+M+J">M. J. Dyer</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Dhillon%2C+V+S">V. S. Dhillon</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Brien%2C+P+T">P. T. O'Brien</a>, <a href="/search/astro-ph?searchtype=author&query=Ramsay%2C+G">G. Ramsay</a>, <a href="/search/astro-ph?searchtype=author&query=Poshyachinda%2C+S">S. Poshyachinda</a>, <a href="/search/astro-ph?searchtype=author&query=Kotak%2C+R">R. Kotak</a>, <a href="/search/astro-ph?searchtype=author&query=Nuttall%2C+L">L. Nuttall</a>, <a href="/search/astro-ph?searchtype=author&query=Breton%2C+R+P">R. P. Breton</a>, <a href="/search/astro-ph?searchtype=author&query=Pall%C3%A9%2C+E">E. Pall茅</a>, <a href="/search/astro-ph?searchtype=author&query=Pollacco%2C+D">D. Pollacco</a>, <a href="/search/astro-ph?searchtype=author&query=Thrane%2C+E">E. Thrane</a>, <a href="/search/astro-ph?searchtype=author&query=Aukkaravittayapun%2C+S">S. Aukkaravittayapun</a>, <a href="/search/astro-ph?searchtype=author&query=Awiphan%2C+S">S. Awiphan</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+M+J+I">M. J. I. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Burhanudin%2C+U">U. Burhanudin</a>, <a href="/search/astro-ph?searchtype=author&query=Chote%2C+P">P. Chote</a>, <a href="/search/astro-ph?searchtype=author&query=Chrimes%2C+A+A">A. A. Chrimes</a>, <a href="/search/astro-ph?searchtype=author&query=Daw%2C+E">E. Daw</a> , et al. (27 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="2004.00025v2-abstract-short" style="display: inline;"> We report the results of optical follow-up observations of 29 gravitational-wave triggers during the first half of the LIGO-Virgo Collaboration (LVC) O3 run with the Gravitational-wave Optical Transient Observer (GOTO) in its prototype 4-telescope configuration (GOTO-4). While no viable electromagnetic counterpart candidate was identified, we estimate our 3D (volumetric) coverage using test light… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.00025v2-abstract-full').style.display = 'inline'; document.getElementById('2004.00025v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.00025v2-abstract-full" style="display: none;"> We report the results of optical follow-up observations of 29 gravitational-wave triggers during the first half of the LIGO-Virgo Collaboration (LVC) O3 run with the Gravitational-wave Optical Transient Observer (GOTO) in its prototype 4-telescope configuration (GOTO-4). While no viable electromagnetic counterpart candidate was identified, we estimate our 3D (volumetric) coverage using test light curves of on- and off-axis gamma-ray bursts and kilonovae. In cases where the source region was observable immediately, GOTO-4 was able to respond to a GW alert in less than a minute. The average time of first observation was $8.79$ hours after receiving an alert ($9.90$ hours after trigger). A mean of $732.3$ square degrees were tiled per event, representing on average $45.3$ per cent of the LVC probability map, or $70.3$ per cent of the observable probability. This coverage will further improve as the facility scales up alongside the localisation performance of the evolving gravitational-wave detector network. Even in its 4-telescope prototype configuration, GOTO is capable of detecting AT2017gfo-like kilonovae beyond 200~Mpc in favourable observing conditions. We cannot currently place meaningful electromagnetic limits on the population of distant ($\hat{D}_L = 1.3$~Gpc) binary black hole mergers because our test models are too faint to recover at this distance. However, as GOTO is upgraded towards its full 32-telescope, 2 node (La Palma \& Australia) configuration, it is expected to be sufficiently sensitive to cover the predicted O4 binary neutron star merger volume, and will be able to respond to both northern and southern triggers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.00025v2-abstract-full').style.display = 'none'; document.getElementById('2004.00025v2-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 7 figures, 3 tables. Accepted for publication in MNRAS. Author's final submitted version</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2003.00685">arXiv:2003.00685</a> <span> [<a href="https://arxiv.org/pdf/2003.00685">pdf</a>, <a href="https://arxiv.org/format/2003.00685">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ab9f2e">10.3847/1538-4365/ab9f2e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Multi-INstrument Burst ARchive (MINBAR) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Zand%2C+J+J+M+i+%27">J. J. M. in 't Zand</a>, <a href="/search/astro-ph?searchtype=author&query=Chenevez%2C+J">J. Chenevez</a>, <a href="/search/astro-ph?searchtype=author&query=W%C3%B6rpel%2C+H">H. W枚rpel</a>, <a href="/search/astro-ph?searchtype=author&query=Keek%2C+L">L. Keek</a>, <a href="/search/astro-ph?searchtype=author&query=Ootes%2C+L">L. Ootes</a>, <a href="/search/astro-ph?searchtype=author&query=Watts%2C+A+L">A. L. Watts</a>, <a href="/search/astro-ph?searchtype=author&query=Gisler%2C+L">L. Gisler</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Fernandez%2C+C">C. Sanchez-Fernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Kuulkers%2C+E">E. Kuulkers</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="2003.00685v3-abstract-short" style="display: inline;"> We present the largest sample of type-I (thermonuclear) X-ray bursts yet assembled, comprising 7083 bursts from 85 bursting sources. The sample is drawn from observations with Xenon-filled proportional counters on the long-duration satellites RXTE, BeppoSAX and INTEGRAL, between 1996 February 8, and 2012 May 3. The burst sources were drawn from a comprehensive catalog of 115 burst sources, assembl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.00685v3-abstract-full').style.display = 'inline'; document.getElementById('2003.00685v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.00685v3-abstract-full" style="display: none;"> We present the largest sample of type-I (thermonuclear) X-ray bursts yet assembled, comprising 7083 bursts from 85 bursting sources. The sample is drawn from observations with Xenon-filled proportional counters on the long-duration satellites RXTE, BeppoSAX and INTEGRAL, between 1996 February 8, and 2012 May 3. The burst sources were drawn from a comprehensive catalog of 115 burst sources, assembled from earlier catalogs and the literature. We carried out a consistent analysis for each burst lightcurve (normalised to the relative instrumental effective area), and provide measurements of rise time, peak intensity, burst timescale, and fluence. For bursts observed with the RXTE/PCA and BeppoSAX/WFC we also provide time-resolved spectroscopy, including estimates of bolometric peak flux and fluence, and spectral parameters at the peak of the burst. For 950 bursts observed with the PCA from sources with previously detected burst oscillations, we include an analysis of the high-time resolution data, providing information on the detectability and amplitude of the oscillations, as well as where in the burst they are found. We also present analysis of 118848 observations of the burst sources within the sample timeframe. We extracted 3-25 keV X-ray spectra from most observations, and (for observations meeting our signal-to-noise criterion), we provide measurements of the flux, spectral colours, and for selected sources, the position on the colour-colour diagram, for the best-fit spectral model. We present a description of the sample, a summary of the science investigations completed to date, and suggestions for further studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.00685v3-abstract-full').style.display = 'none'; document.getElementById('2003.00685v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">105 pages, 34 figures, 18 tables; machine-readable sample data tables available via https://doi.org/10.26180/5e4a697d9b8b6; web interface to sample data available via http://burst.sci.monash.edu. Updated observation numbers to reflect final data table versions, slight modifications to text to preserve table ordering. Now published by ApJS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal Supplement Series, Volume 249, Number 2, 2020 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.12154">arXiv:2002.12154</a> <span> [<a href="https://arxiv.org/pdf/2002.12154">pdf</a>, <a href="https://arxiv.org/ps/2002.12154">ps</a>, <a href="https://arxiv.org/format/2002.12154">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/10.1051/0004-6361/202037812">10.1051/0004-6361/202037812 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High-energy characteristics of the accretion-powered millisecond pulsar IGR J17591-2342 during its 2018 outburst </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kuiper%2C+L">L. Kuiper</a>, <a href="/search/astro-ph?searchtype=author&query=Tsygankov%2C+S+S">S. S. Tsygankov</a>, <a href="/search/astro-ph?searchtype=author&query=Falanga%2C+M">M. Falanga</a>, <a href="/search/astro-ph?searchtype=author&query=Mereminskij%2C+I+A">I. A. Mereminskij</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Poutanen%2C+J">J. Poutanen</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Z">Z. Li</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="2002.12154v1-abstract-short" style="display: inline;"> IGR J17591-2342 is a recently INTEGRAL discovered accreting millisecond X-ray pulsar that went into outburst around July 21, 2018. To better understand the physics acting in these systems during the outburst episode we performed detailed temporal-, timing- and spectral analyses across the 0.3-300 keV band using data from NICER, XMM-Newton, NuSTAR and INTEGRAL. The hard X-ray 20-60 keV outburst pro… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.12154v1-abstract-full').style.display = 'inline'; document.getElementById('2002.12154v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.12154v1-abstract-full" style="display: none;"> IGR J17591-2342 is a recently INTEGRAL discovered accreting millisecond X-ray pulsar that went into outburst around July 21, 2018. To better understand the physics acting in these systems during the outburst episode we performed detailed temporal-, timing- and spectral analyses across the 0.3-300 keV band using data from NICER, XMM-Newton, NuSTAR and INTEGRAL. The hard X-ray 20-60 keV outburst profile is composed of four flares. During the maximum of the last flare we discovered a type-I thermonuclear burst in INTEGRAL JEM-X data. We derived a distance of 7.6+/-0.7 kpc, adopting Eddington luminosity limited photospheric radius expansion burst emission and assuming anisotropic emission. In the timing analysis using all NICER 1-10 keV monitoring data we observed a rather complex behaviour starting with a spin-up period, followed by a frequency drop, a episode of constant frequency and concluding with irregular behaviour till the end of the outburst. The 1-50 keV phase distributions of the pulsed emission, detected up to $\sim$ 120 keV using INTEGRAL ISGRI data, was decomposed in three Fourier harmonics showing that the pulsed fraction of the fundamental increases from ~10% to ~17% going from ~1.5 to ~4 keV, while the harder photons arrive earlier than the soft photons for energies <10 keV. The total emission spectrum of IGR J17591-2342 across the 0.3-150 keV band could adequately be fitted in terms of an absorbed compPS model yielding as best fit parameters a column density of N_H=(2.09+/-0.05) x 10^{22} /cm2, a blackbody seed photon temperature kT_bb,seed of 0.64+/- 0.02 keV, electron temperature kT_e=38.8+/-1.2 keV and Thomson optical depth Tau_T=1.59+/-0.04. The fit normalisation results in an emission area radius of 11.3+/-0.5 km adopting a distance of 7.6 kpc. Finally, the results are discussed within the framework of accretion physics- and X-ray thermonuclear burst theory. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.12154v1-abstract-full').style.display = 'none'; document.getElementById('2002.12154v1-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 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">Submitted to A&A, 15 pages</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 641, A37 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.01950">arXiv:2002.01950</a> <span> [<a href="https://arxiv.org/pdf/2002.01950">pdf</a>, <a href="https://arxiv.org/format/2002.01950">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <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/10.1051/0004-6361/202037669">10.1051/0004-6361/202037669 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observational constraints on the optical and near-infrared emission from the neutron star-black hole binary merger S190814bv </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Amati%2C+L">L. Amati</a>, <a href="/search/astro-ph?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+F+E">F. E. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Benetti%2C+S">S. Benetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardini%2C+M+G">M. G. Bernardini</a>, <a href="/search/astro-ph?searchtype=author&query=Bhirombhakdi%2C+K">K. Bhirombhakdi</a>, <a href="/search/astro-ph?searchtype=author&query=Botticella%2C+M+T">M. T. Botticella</a>, <a href="/search/astro-ph?searchtype=author&query=Branchesi%2C+M">M. Branchesi</a>, <a href="/search/astro-ph?searchtype=author&query=Brocato%2C+E">E. Brocato</a>, <a href="/search/astro-ph?searchtype=author&query=Bruun%2C+S+H">S. H. Bruun</a>, <a href="/search/astro-ph?searchtype=author&query=Bulla%2C+M">M. Bulla</a>, <a href="/search/astro-ph?searchtype=author&query=Campana%2C+S">S. Campana</a>, <a href="/search/astro-ph?searchtype=author&query=Cappellaro%2C+E">E. Cappellaro</a>, <a href="/search/astro-ph?searchtype=author&query=Castro-Tirado%2C+A+J">A. J. Castro-Tirado</a>, <a href="/search/astro-ph?searchtype=author&query=Chambers%2C+K+C">K. C. Chambers</a>, <a href="/search/astro-ph?searchtype=author&query=Chaty%2C+S">S. Chaty</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+T+-">T. -W. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Ciolfi%2C+R">R. Ciolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Coleiro%2C+A">A. Coleiro</a>, <a href="/search/astro-ph?searchtype=author&query=Copperwheat%2C+C+M">C. M. Copperwheat</a>, <a href="/search/astro-ph?searchtype=author&query=Covino%2C+S">S. Covino</a>, <a href="/search/astro-ph?searchtype=author&query=Cutter%2C+R">R. Cutter</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Ammando%2C+F">F. D'Ammando</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Avanzo%2C+P">P. D'Avanzo</a> , et al. (129 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="2002.01950v2-abstract-short" style="display: inline;"> On 2019 August 14, the LIGO and Virgo interferometers detected a high-significance event labelled S190814bv. Preliminary analysis of the GW data suggests that the event was likely due to the merger of a compact binary system formed by a BH and a NS. ElectromagNetic counterparts of GRAvitational wave sources at the VEry Large Telescope (ENGRAVE) collaboration members carried out an intensive multi-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.01950v2-abstract-full').style.display = 'inline'; document.getElementById('2002.01950v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.01950v2-abstract-full" style="display: none;"> On 2019 August 14, the LIGO and Virgo interferometers detected a high-significance event labelled S190814bv. Preliminary analysis of the GW data suggests that the event was likely due to the merger of a compact binary system formed by a BH and a NS. ElectromagNetic counterparts of GRAvitational wave sources at the VEry Large Telescope (ENGRAVE) collaboration members carried out an intensive multi-epoch, multi-instrument observational campaign to identify the possible optical/near infrared counterpart of the event. In addition, the ATLAS, GOTO, GRAWITA-VST, Pan-STARRS and VINROUGE projects also carried out a search on this event. Our observations allow us to place limits on the presence of any counterpart and discuss the implications for the kilonova (KN) possibly generated by this NS-BH merger, and for the strategy of future searches. Altogether, our observations allow us to exclude a KN with large ejecta mass $M\gtrsim 0.1\,\mathrm{M_\odot}$ to a high ($>90\%$) confidence, and we can exclude much smaller masses in a subsample of our observations. This disfavours the tidal disruption of the neutron star during the merger. Despite the sensitive instruments involved in the campaign, given the distance of S190814bv we could not reach sufficiently deep limits to constrain a KN comparable in luminosity to AT 2017gfo on a large fraction of the localisation probability. This suggests that future (likely common) events at a few hundreds Mpc will be detected only by large facilities with both high sensitivity and large field of view. Galaxy-targeted observations can reach the needed depth over a relevant portion of the localisation probability with a smaller investment of resources, but the number of galaxies to be targeted in order to get a fairly complete coverage is large, even in the case of a localisation as good as that of this event. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.01950v2-abstract-full').style.display = 'none'; document.getElementById('2002.01950v2-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 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 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">52 pages, revised version now accepted for publication in A&A. Abstract abridged to meet arXiv requirements</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 643, A113 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.07977">arXiv:1909.07977</a> <span> [<a href="https://arxiv.org/pdf/1909.07977">pdf</a>, <a href="https://arxiv.org/format/1909.07977">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/staa1054">10.1093/mnras/staa1054 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multi-epoch X-ray burst modelling: MCMC with large grids of 1D simulations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+Z">Zac Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Heger%2C+A">Alexander Heger</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">Duncan K. Galloway</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1909.07977v2-abstract-short" style="display: inline;"> Type-I X-ray bursts are recurring thermonuclear explosions on the surface of accreting neutron stars. Matching observed bursts to computational models can help to constrain system properties, such as the neutron star mass and radius, crustal heating rates, and the accreted fuel composition, but systematic parameter studies to date have been limited. We apply Markov chain Monte Carlo methods to 1D… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.07977v2-abstract-full').style.display = 'inline'; document.getElementById('1909.07977v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.07977v2-abstract-full" style="display: none;"> Type-I X-ray bursts are recurring thermonuclear explosions on the surface of accreting neutron stars. Matching observed bursts to computational models can help to constrain system properties, such as the neutron star mass and radius, crustal heating rates, and the accreted fuel composition, but systematic parameter studies to date have been limited. We apply Markov chain Monte Carlo methods to 1D burst models for the first time, and obtain system parameter estimations for the `Clocked Burster', GS 1826$-$238, by fitting multiple observed epochs simultaneously. We explore multiple parameters which are often held constant, including the neutron star mass, crustal heating rate, and hydrogen composition. To improve the computational efficiency, we precompute a grid of 3840 KEPLER models - the largest set of 1D burst simulations to date - and by interpolating over the model grid, we can rapidly sample burst predictions. We obtain estimates for a CNO metallicity of $Z_\mathrm{CNO} = 0.010^{+0.005}_{-0.004}$, a hydrogen fraction of $X_0 = 0.74^{+0.02}_{-0.03}$, a distance of $d \sqrt{尉_\mathrm{b}} = 6.5^{+0.4}_{-0.6}\, \mathrm{kpc}$, and a system inclination of $i = {69^{+2}_{-3}}^{\circ}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.07977v2-abstract-full').style.display = 'none'; document.getElementById('1909.07977v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 10 figures, 3 tables. Updated Figs 3 and A1, minor corrections. Accepted by MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1908.03373">arXiv:1908.03373</a> <span> [<a href="https://arxiv.org/pdf/1908.03373">pdf</a>, <a href="https://arxiv.org/ps/1908.03373">ps</a>, <a href="https://arxiv.org/format/1908.03373">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/ab3a37">10.3847/1538-4357/ab3a37 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NICER observes a secondary peak in the decay of a thermonuclear burst from 4U 1608-52 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jaisawal%2C+G+K">Gaurava K. Jaisawal</a>, <a href="/search/astro-ph?searchtype=author&query=Chenevez%2C+J">J茅r么me Chenevez</a>, <a href="/search/astro-ph?searchtype=author&query=Bult%2C+P">Peter Bult</a>, <a href="/search/astro-ph?searchtype=author&query=Zand%2C+J+J+M+i+%27">J. J. M. in 't Zand</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">Duncan K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Strohmayer%2C+T+E">Tod E. Strohmayer</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCver%2C+T">Tolga G眉ver</a>, <a href="/search/astro-ph?searchtype=author&query=Adkins%2C+P">Phillip Adkins</a>, <a href="/search/astro-ph?searchtype=author&query=Altamirano%2C+D">Diego Altamirano</a>, <a href="/search/astro-ph?searchtype=author&query=Arzoumanian%2C+Z">Zaven Arzoumanian</a>, <a href="/search/astro-ph?searchtype=author&query=Chakrabarty%2C+D">Deepto Chakrabarty</a>, <a href="/search/astro-ph?searchtype=author&query=Coopersmith%2C+J">Jonathan Coopersmith</a>, <a href="/search/astro-ph?searchtype=author&query=Gendreau%2C+K+C">Keith C. Gendreau</a>, <a href="/search/astro-ph?searchtype=author&query=Guillot%2C+S">Sebastien Guillot</a>, <a href="/search/astro-ph?searchtype=author&query=Keek%2C+L">Laurens Keek</a>, <a href="/search/astro-ph?searchtype=author&query=Ludlam%2C+R+M">Renee M. Ludlam</a>, <a href="/search/astro-ph?searchtype=author&query=Malacaria%2C+C">Christian Malacaria</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="1908.03373v1-abstract-short" style="display: inline;"> We report for the first time below 1.5 keV, the detection of a secondary peak in an Eddington-limited thermonuclear X-ray burst observed by the Neutron Star Interior Composition Explorer (NICER) from the low-mass X-ray binary 4U 1608-52. Our time-resolved spectroscopy of the burst is consistent with a model consisting of a varying-temperature blackbody, and an evolving persistent flux contribution… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.03373v1-abstract-full').style.display = 'inline'; document.getElementById('1908.03373v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.03373v1-abstract-full" style="display: none;"> We report for the first time below 1.5 keV, the detection of a secondary peak in an Eddington-limited thermonuclear X-ray burst observed by the Neutron Star Interior Composition Explorer (NICER) from the low-mass X-ray binary 4U 1608-52. Our time-resolved spectroscopy of the burst is consistent with a model consisting of a varying-temperature blackbody, and an evolving persistent flux contribution, likely attributed to the accretion process. The dip in the burst intensity before the secondary peak is also visible in the bolometric flux. Prior to the dip, the blackbody temperature reached a maximum of $\approx3$ keV. Our analysis suggests that the dip and secondary peak are not related to photospheric expansion, varying circumstellar absorption, or scattering. Instead, we discuss the observation in the context of hydrodynamical instabilities, thermonuclear flame spreading models, and re-burning in the cooling tail of the burst. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.03373v1-abstract-full').style.display = 'none'; document.getElementById('1908.03373v1-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, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">8 pages, 6 figures, 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> The Astrophysical Journal, 883:61 (7pp), 2019 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1907.00996">arXiv:1907.00996</a> <span> [<a href="https://arxiv.org/pdf/1907.00996">pdf</a>, <a href="https://arxiv.org/format/1907.00996">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/stz2638">10.1093/mnras/stz2638 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Bayesian Approach to Matching Thermonuclear X-ray Burst Observations with Models </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Goodwin%2C+A+J">A. J. Goodwin</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Heger%2C+A">A. Heger</a>, <a href="/search/astro-ph?searchtype=author&query=Cumming%2C+A">A. Cumming</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+Z">Z. Johnston</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="1907.00996v2-abstract-short" style="display: inline;"> We present a new method of matching observations of Type I (thermonuclear) X-ray bursts with models, comparing the predictions of a semi-analytic ignition model with X-ray observations of the accretion-powered millisecond pulsar SAX J1808.4--3658 in outburst. We used a Bayesian analysis approach to marginalise over the parameters of interest and determine parameters such as fuel composition, dista… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.00996v2-abstract-full').style.display = 'inline'; document.getElementById('1907.00996v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1907.00996v2-abstract-full" style="display: none;"> We present a new method of matching observations of Type I (thermonuclear) X-ray bursts with models, comparing the predictions of a semi-analytic ignition model with X-ray observations of the accretion-powered millisecond pulsar SAX J1808.4--3658 in outburst. We used a Bayesian analysis approach to marginalise over the parameters of interest and determine parameters such as fuel composition, distance/anisotropy factors, neutron star mass and neutron star radius. Our study includes a treatment of the system inclination effects, inferring that the rotation axis of the system is inclined $\left(69^{+4}_{-2}\right)^\circ$ from the observers line of sight, assuming a flat disc model. This method can be applied to any accreting source that exhibits Type I X-ray bursts. We find a hydrogen mass fraction of $0.57^{+0.13}_{-0.14}$ and CNO metallicity of $0.013^{+0.006}_{-0.004}$ for the accreted fuel is required by the model to match the observed burst energies, for a distance to the source of $3.3^{+0.3}_{-0.2}\,\mathrm{kpc}$. We infer a neutron star mass of $1.5^{+0.6}_{-0.3}\,\mathrm{M}_{\odot}$ and radius of $11.8^{+1.3}_{-0.9}\,\mathrm{km}$ for a surface gravity of $1.9^{+0.7}_{-0.4}\times10^{14}\,\mathrm{cm}\,\mathrm{s}^{-2}$ for SAX J1808.4--3658. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.00996v2-abstract-full').style.display = 'none'; document.getElementById('1907.00996v2-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 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 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">14 pages, 10 figures, revised version 1, accepted by MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.10970">arXiv:1904.10970</a> <span> [<a href="https://arxiv.org/pdf/1904.10970">pdf</a>, <a href="https://arxiv.org/format/1904.10970">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/stz1094">10.1093/mnras/stz1094 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> XMMU J181227.8-181234: a new ultracompact X-ray binary candidate </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Goodwin%2C+A+J">A. J. Goodwin</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Zand%2C+J+J+M+i+%27">J. J. M. in 't Zand</a>, <a href="/search/astro-ph?searchtype=author&query=Kuulkers%2C+E">E. Kuulkers</a>, <a href="/search/astro-ph?searchtype=author&query=Bilous%2C+A">A. Bilous</a>, <a href="/search/astro-ph?searchtype=author&query=Keek%2C+L">L. Keek</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="1904.10970v1-abstract-short" style="display: inline;"> We report the discovery of Type I (thermonuclear) X-ray bursts from the transient source XMMU J181227.8-181234 = XTE J1812-182. We found 7 X-ray bursts in Rossi X-ray Timing Explorer observations during the 2008 outburst, confirming the source as a neutron star low mass X-ray binary. Based on the measured burst fluence and the average recurrence time of 1.4$^{+0.9}_{-0.5}$ hr, we deduce that the s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.10970v1-abstract-full').style.display = 'inline'; document.getElementById('1904.10970v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.10970v1-abstract-full" style="display: none;"> We report the discovery of Type I (thermonuclear) X-ray bursts from the transient source XMMU J181227.8-181234 = XTE J1812-182. We found 7 X-ray bursts in Rossi X-ray Timing Explorer observations during the 2008 outburst, confirming the source as a neutron star low mass X-ray binary. Based on the measured burst fluence and the average recurrence time of 1.4$^{+0.9}_{-0.5}$ hr, we deduce that the source is accreting almost pure helium ($X \leq 0.1$) fuel. Two bursts occurred just 18 minutes apart; the first short waiting time bursts observed in a source accreting hydrogen-poor fuel. Taking into consideration the effects on the burst and persistent flux due to the inferred system inclination of $30\pm{10}$ degrees, we estimate the distance to be $14\pm{2}$ kpc, where we report the statistical uncertainty but note that there could be up to $20\%$ variation in the distance due to systematic effects discussed in the paper. The corresponding maximum accretion rate is $0.30\pm0.05$ times the Eddington limit. Based on the low hydrogen content of the accreted fuel and the short average recurrence time, we classify the source as a transient ultracompact low-mass X-ray binary. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.10970v1-abstract-full').style.display = 'none'; document.getElementById('1904.10970v1-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 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">10 pages, 6 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/1812.04023">arXiv:1812.04023</a> <span> [<a href="https://arxiv.org/pdf/1812.04023">pdf</a>, <a href="https://arxiv.org/format/1812.04023">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s11433-017-9186-1">10.1007/s11433-017-9186-1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observatory science with eXTP </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zand%2C+J+J+M+i+%27">Jean J. M. in 't Zand</a>, <a href="/search/astro-ph?searchtype=author&query=Bozzo%2C+E">Enrico Bozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Qu%2C+J">Jinlu Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+X">Xiang-Dong Li</a>, <a href="/search/astro-ph?searchtype=author&query=Amati%2C+L">Lorenzo Amati</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Y">Yang Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Donnarumma%2C+I">Immacolata Donnarumma</a>, <a href="/search/astro-ph?searchtype=author&query=Doroshenko%2C+V">Victor Doroshenko</a>, <a href="/search/astro-ph?searchtype=author&query=Drake%2C+S+A">Stephen A. Drake</a>, <a href="/search/astro-ph?searchtype=author&query=Hernanz%2C+M">Margarita Hernanz</a>, <a href="/search/astro-ph?searchtype=author&query=Jenke%2C+P+A">Peter A. Jenke</a>, <a href="/search/astro-ph?searchtype=author&query=Maccarone%2C+T+J">Thomas J. Maccarone</a>, <a href="/search/astro-ph?searchtype=author&query=Mahmoodifar%2C+S">Simin Mahmoodifar</a>, <a href="/search/astro-ph?searchtype=author&query=de+Martino%2C+D">Domitilla de Martino</a>, <a href="/search/astro-ph?searchtype=author&query=De+Rosa%2C+A">Alessandra De Rosa</a>, <a href="/search/astro-ph?searchtype=author&query=Rossi%2C+E+M">Elena M. Rossi</a>, <a href="/search/astro-ph?searchtype=author&query=Rowlinson%2C+A">Antonia Rowlinson</a>, <a href="/search/astro-ph?searchtype=author&query=Sala%2C+G">Gloria Sala</a>, <a href="/search/astro-ph?searchtype=author&query=Stratta%2C+G">Giulia Stratta</a>, <a href="/search/astro-ph?searchtype=author&query=Tauris%2C+T+M">Thomas M. Tauris</a>, <a href="/search/astro-ph?searchtype=author&query=Wilms%2C+J">Joern Wilms</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+X">Xuefeng Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+P">Ping Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">Iv谩n Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Altamirano%2C+D">Diego Altamirano</a> , et al. (159 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="1812.04023v1-abstract-short" style="display: inline;"> In this White Paper we present the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to Observatory Science targets. These include flaring stars, supernova remnants, accreting white dwarfs, low and high mass X-ray binaries, radio quiet and radio loud active galactic nuclei, tidal disruption events, and gamma-ray bursts. eXTP will be excellently suited to stu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.04023v1-abstract-full').style.display = 'inline'; document.getElementById('1812.04023v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1812.04023v1-abstract-full" style="display: none;"> In this White Paper we present the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to Observatory Science targets. These include flaring stars, supernova remnants, accreting white dwarfs, low and high mass X-ray binaries, radio quiet and radio loud active galactic nuclei, tidal disruption events, and gamma-ray bursts. eXTP will be excellently suited to study one common aspect of these objects: their often transient nature. Developed by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Science, the eXTP mission is expected to be launched in the mid 2020s. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.04023v1-abstract-full').style.display = 'none'; document.getElementById('1812.04023v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 December, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">Accepted for publication on Sci. China Phys. Mech. Astron. (2019)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1810.05490">arXiv:1810.05490</a> <span> [<a href="https://arxiv.org/pdf/1810.05490">pdf</a>, <a href="https://arxiv.org/format/1810.05490">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/10.1051/0004-6361/201833857">10.1051/0004-6361/201833857 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Mixed H/He bursts in SAX J1748.9-2021 during the spectral change of its 2015 outburst </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+Z">Zhaosheng Li</a>, <a href="/search/astro-ph?searchtype=author&query=De+Falco%2C+V">V. De Falco</a>, <a href="/search/astro-ph?searchtype=author&query=Falanga%2C+M">M. Falanga</a>, <a href="/search/astro-ph?searchtype=author&query=Bozzo%2C+E">E. Bozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Kuiper%2C+L">L. Kuiper</a>, <a href="/search/astro-ph?searchtype=author&query=Poutanen%2C+J">J. Poutanen</a>, <a href="/search/astro-ph?searchtype=author&query=Cumming%2C+A">A. Cumming</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+S">Shu Zhang</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="1810.05490v1-abstract-short" style="display: inline;"> SAX J1748.9-2021 is a transiently accreting X-ray millisecond pulsar. It is also known as an X-ray burster source discovered by Beppo-SAX. We analysed the persistent emission and type-I X-ray burst properties during its 2015 outburst. The source varied from hard to soft state within half day. We modeled the broad-band spectra of the persistent emission in the 1 - 250 keV energy band for both spect… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.05490v1-abstract-full').style.display = 'inline'; document.getElementById('1810.05490v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1810.05490v1-abstract-full" style="display: none;"> SAX J1748.9-2021 is a transiently accreting X-ray millisecond pulsar. It is also known as an X-ray burster source discovered by Beppo-SAX. We analysed the persistent emission and type-I X-ray burst properties during its 2015 outburst. The source varied from hard to soft state within half day. We modeled the broad-band spectra of the persistent emission in the 1 - 250 keV energy band for both spectral states using the quasi-simultaneous INTEGRAL and Swift data. The broad-band spectra are well fitted by an absorbed thermal Componization model, compps, in a slab geometry. The best-fits for the two states indicate significantly different plasma temperature of 18 and 5 keV and the Thomson optical depth of 3 and 4, respectively. In total, 56 type-I X-ray bursts were observed during the 2015 outburst, of which 26 detected by INTEGRAL in the hard state, 25 by XMM-Newton in the soft state, and 5 by Swift in both states. As the object transited from the hard to the soft state, the recurrence time for X-ray bursts decreased from $\approx 2$ to $\approx1$ hr. The relation between the recurrence time, $ 螖t_{\rm rec}$, and the local mass accretion rate per unit area onto the compact object, $\dot m$, is fitted by a power-law model, and yielded as best fit at $螖t_{\rm rec} \sim \langle \dot{m} \rangle^{-1.02\pm0.03}$ using all X-ray bursts. In both cases, the observed recurrence times are consistent with the mixed hydrogen/helium bursts. We also discuss the effects of type-I X-ray bursts prior to the hard to soft transition. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.05490v1-abstract-full').style.display = 'none'; document.getElementById('1810.05490v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 October, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">Accepted for publication in A&A, 6 pages, 4 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 620, A114 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1808.02225">arXiv:1808.02225</a> <span> [<a href="https://arxiv.org/pdf/1808.02225">pdf</a>, <a href="https://arxiv.org/format/1808.02225">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/aaeed2">10.3847/1538-4357/aaeed2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Neutrino Losses in Type I Thermonuclear X-ray Bursts: An Improved Nuclear Energy Generation Approximation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Goodwin%2C+A+J">Adelle J. Goodwin</a>, <a href="/search/astro-ph?searchtype=author&query=Heger%2C+A">Alexander Heger</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">Duncan K. Galloway</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="1808.02225v3-abstract-short" style="display: inline;"> Type I X-ray bursts are thermonuclear explosions on the surface of accreting neutron stars. Hydrogen rich X-ray bursts burn protons far from the line of stability and can release energy in the form of neutrinos from $尾$-decays. We have estimated, for the first time, the neutrino fluxes of Type I bursts for a range of initial conditions based on the predictions of a 1D implicit hydrodynamics code,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.02225v3-abstract-full').style.display = 'inline'; document.getElementById('1808.02225v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.02225v3-abstract-full" style="display: none;"> Type I X-ray bursts are thermonuclear explosions on the surface of accreting neutron stars. Hydrogen rich X-ray bursts burn protons far from the line of stability and can release energy in the form of neutrinos from $尾$-decays. We have estimated, for the first time, the neutrino fluxes of Type I bursts for a range of initial conditions based on the predictions of a 1D implicit hydrodynamics code, KEPLER, which calculates the complete nuclear reaction network. We find that neutrino losses are between $6.7 \times 10^{-5}$ and $0.14$ of the total energy per nucleon, Q$_{nuc}$, depending upon the hydrogen fraction in the fuel. These values are significantly below the $35\,\%$ value for neutrino losses often adopted in recent literature for the rp-process. The discrepancy arises because it is only at $尾$-decays that $\approx35\,\%$ of energy is lost due to neutrino emission, whereas there are no neutrino losses in $(p,纬)$ and $(伪,p)$ reactions. Using the total measured burst energies from KEPLER for a range of initial conditions, we have determined an approximation formula for the total energy per nucleon released during an X-ray burst, Q$_{nuc}$=1.31+6.95$\bar{X} - 1.92\bar{X}^2 $MeV/nucleon, where $\bar{X}$ is the average hydrogen mass fraction of the ignition column, with an RMS error of $0.052\,$Mev/nucleon. We provide a detailed analysis of the nuclear energy output of a burst and find an incomplete extraction of mass excess in the burst fuel, with $14\,\%$ of the mass excess in the fuel not being extracted. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.02225v3-abstract-full').style.display = 'none'; document.getElementById('1808.02225v3-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 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">8 pages, 5 figures, published 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/1806.01418">arXiv:1806.01418</a> <span> [<a href="https://arxiv.org/pdf/1806.01418">pdf</a>, <a href="https://arxiv.org/format/1806.01418">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/sty1441">10.1093/mnras/sty1441 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Precision ephemerides for gravitational-wave searches -- III. Revised system parameters of Sco X-1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wang%2C+L">L. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Steeghs%2C+D">D. Steeghs</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">D. K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Marsh%2C+T">T. Marsh</a>, <a href="/search/astro-ph?searchtype=author&query=Casares%2C+J">J. Casares</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="1806.01418v1-abstract-short" style="display: inline;"> Neutron stars in low-mass X-ray binaries are considered promising candidate sources of continuous gravitational-waves. These neutron stars are typically rotating many hundreds of times a second. The process of accretion can potentially generate and support non-axisymmetric distortions to the compact object, resulting in persistent emission of gravitational-waves. We present a study of existing opt… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.01418v1-abstract-full').style.display = 'inline'; document.getElementById('1806.01418v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1806.01418v1-abstract-full" style="display: none;"> Neutron stars in low-mass X-ray binaries are considered promising candidate sources of continuous gravitational-waves. These neutron stars are typically rotating many hundreds of times a second. The process of accretion can potentially generate and support non-axisymmetric distortions to the compact object, resulting in persistent emission of gravitational-waves. We present a study of existing optical spectroscopic data for Sco X-1, a prime target for continuous gravitational-wave searches, with the aim of providing revised constraints on key orbital parameters required for a directed search with advanced-LIGO data. From a circular orbit fit to an improved radial velocity curve of the Bowen emission components, we derived an updated orbital period and ephemeris. Centre of symmetry measurements from the Bowen Doppler tomogram yield a centre of the disc component of 90 km $\mathrm{s^{-1}}$, which we interpret as a revised upper limit to the projected orbital velocity of the NS $K_1$. By implementing Monte Carlo binary parameter calculations, and imposing new limits on $K_1$ and the rotational broadening, we obtained a complete set of dynamical system parameter constraints including a new range for $K_1$ of 40--90 km $\mathrm{s^{-1}}$. Finally, we discussed the implications of the updated orbital parameters for future continuous-waves searches. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.01418v1-abstract-full').style.display = 'none'; document.getElementById('1806.01418v1-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 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">11 pages, 7 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/1805.10065">arXiv:1805.10065</a> <span> [<a href="https://arxiv.org/pdf/1805.10065">pdf</a>, <a href="https://arxiv.org/ps/1805.10065">ps</a>, <a href="https://arxiv.org/format/1805.10065">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/10.3847/2041-8213/aad09c">10.3847/2041-8213/aad09c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Millisecond oscillations in the bursting flux of SAX J1810.8-2609 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bilous%2C+A+V">Anna V Bilous</a>, <a href="/search/astro-ph?searchtype=author&query=Watts%2C+A+L">Anna L Watts</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">Duncan K Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Zand%2C+J+J+M+i+%27">Jean J M in 't Zand</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="1805.10065v1-abstract-short" style="display: inline;"> SAX J1810.8-2609 is a faint X-ray transient, mostly known for its abnormally low quiescent thermal luminosity, which disagrees with standard cooling models. It is also one of a small sample of stars whose mass and radius have been estimated using spectral modeling of one of its thermonuclear bursts. Here we report the discovery of millisecond oscillations in a type I thermonuclear X-ray burst from… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.10065v1-abstract-full').style.display = 'inline'; document.getElementById('1805.10065v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1805.10065v1-abstract-full" style="display: none;"> SAX J1810.8-2609 is a faint X-ray transient, mostly known for its abnormally low quiescent thermal luminosity, which disagrees with standard cooling models. It is also one of a small sample of stars whose mass and radius have been estimated using spectral modeling of one of its thermonuclear bursts. Here we report the discovery of millisecond oscillations in a type I thermonuclear X-ray burst from SAX J1810.8-2609 observed by RXTE during the 2007 outburst. A strong signal (Leahy-normalized power of 71.5, 4.5e-9 chance of coincidence with a conservative estimate for the number of trials) was present at 531.8 Hz during the decay of one out of six bursts observed. Oscillations were detected for about 6 seconds, during which their frequency increased from 531.4 to 531.9 Hz in a manner similar to other burst oscillation sources. The millisecond oscillations discovered pinpoint the spin frequency of the neutron star, which is important for the spectral modeling, associated mass-radius inference, and understanding the evolutionary status and cooling behavior of the star. As of April 2018 the source is in outburst again, providing a fleeting opportunity to acquire new material for the burst oscillation searches. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.10065v1-abstract-full').style.display = 'none'; document.getElementById('1805.10065v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 May, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">4 pages, 2 figures, submitted to ApJ letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1804.03380">arXiv:1804.03380</a> <span> [<a href="https://arxiv.org/pdf/1804.03380">pdf</a>, <a href="https://arxiv.org/format/1804.03380">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/10.3847/2041-8213/aabd32">10.3847/2041-8213/aabd32 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Influence of Stellar Spin on Ignition of Thermonuclear Runaways </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">Duncan K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Zand%2C+J+J+M+i+%27">Jean J. M. in 't Zand</a>, <a href="/search/astro-ph?searchtype=author&query=Chenevez%2C+J">J茅r么me Chenevez</a>, <a href="/search/astro-ph?searchtype=author&query=Keek%2C+L">Laurens Keek</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Fernandez%2C+C">Celia Sanchez-Fernandez</a>, <a href="/search/astro-ph?searchtype=author&query=W%C3%B6rpel%2C+H">Hauke W枚rpel</a>, <a href="/search/astro-ph?searchtype=author&query=Lampe%2C+N">Nathanael Lampe</a>, <a href="/search/astro-ph?searchtype=author&query=Kuulkers%2C+E">Erik Kuulkers</a>, <a href="/search/astro-ph?searchtype=author&query=Watts%2C+A">Anna Watts</a>, <a href="/search/astro-ph?searchtype=author&query=Ootes%2C+L">Laura Ootes</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="1804.03380v1-abstract-short" style="display: inline;"> Runaway thermonuclear burning of a layer of accumulated fuel on the surface of a compact star provides a brief but intense display of stellar nuclear processes. For neutron stars accreting from a binary companion, these events manifest as thermonuclear (type-I) X-ray bursts, and recur on typical timescales of hours to days. We measured the burst rate as a function of accretion rate, from seven neu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.03380v1-abstract-full').style.display = 'inline'; document.getElementById('1804.03380v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1804.03380v1-abstract-full" style="display: none;"> Runaway thermonuclear burning of a layer of accumulated fuel on the surface of a compact star provides a brief but intense display of stellar nuclear processes. For neutron stars accreting from a binary companion, these events manifest as thermonuclear (type-I) X-ray bursts, and recur on typical timescales of hours to days. We measured the burst rate as a function of accretion rate, from seven neutron stars with known spin rates, using a burst sample accumulated over several decades. At the highest accretion rates, the burst rate is lower for faster spinning stars. The observations imply that fast (> 400 Hz) rotation encourages stabilization of nuclear burning, suggesting a dynamical dependence of nuclear ignition on the spin rate. This dependence is unexpected, because faster rotation entails less shear between the surrounding accretion disk and the star. Large-scale circulation in the fuel layer, leading to enhanced mixing of the burst ashes into the fuel layer, may explain this behavior; further numerical simulations are required to confirm. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.03380v1-abstract-full').style.display = 'none'; document.getElementById('1804.03380v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">9 pages, 2 figures; accepted for publication by Astrophysical Journal Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1803.00223">arXiv:1803.00223</a> <span> [<a href="https://arxiv.org/pdf/1803.00223">pdf</a>, <a href="https://arxiv.org/format/1803.00223">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/10.1017/S1743921318002363">10.1017/S1743921318002363 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High-energy transients: thermonuclear (type-I) X-ray bursts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">Duncan K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+Z">Zac Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Goodwin%2C+A">Adelle Goodwin</a>, <a href="/search/astro-ph?searchtype=author&query=Heger%2C+A">Alexander Heger</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1803.00223v4-abstract-short" style="display: inline;"> Many distinct classes of high-energy variability have been observed in astrophysical sources, on a range of timescales. The widest range (spanning microseconds-decades) is found in accreting, stellar-mass compact objects, including neutron stars and black holes. Neutron stars are of particular observational interest, as they exhibit surface effects giving rise to phenomena (thermonuclear bursts an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.00223v4-abstract-full').style.display = 'inline'; document.getElementById('1803.00223v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1803.00223v4-abstract-full" style="display: none;"> Many distinct classes of high-energy variability have been observed in astrophysical sources, on a range of timescales. The widest range (spanning microseconds-decades) is found in accreting, stellar-mass compact objects, including neutron stars and black holes. Neutron stars are of particular observational interest, as they exhibit surface effects giving rise to phenomena (thermonuclear bursts and pulsations) not seen in black holes. Here we briefly review the present understanding of thermonuclear (type-I) X-ray bursts. These events are powered by an extensive chain of nuclear reactions, which are in many cases unique to these environments. Thermonuclear bursts have been exploited over the last few years as an avenue to measure the neutron star mass and radius, although the contribution of systematic errors to these measurements remains contentious. We describe recent efforts to better match burst models to observations, with a view to resolving some of the astrophysical uncertainties related to these events. These efforts have good prospects for providing complementary information to nuclear experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.00223v4-abstract-full').style.display = 'none'; document.getElementById('1803.00223v4-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 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 March, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 1 figure, lightly edited version of the paper to appear in the proceedings of IAU Symposium 339, "Southern Horizons in Time Domain Astronomy", Stellenbosch, South Africa, November 2017. v4 corrected reference to Insight-HXMT (not HMXT!)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1712.06227">arXiv:1712.06227</a> <span> [<a href="https://arxiv.org/pdf/1712.06227">pdf</a>, <a href="https://arxiv.org/format/1712.06227">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/978-3-662-62110-3_5">10.1007/978-3-662-62110-3_5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Thermonuclear X-ray bursts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">Duncan K. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Keek%2C+L">Laurens Keek</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="1712.06227v1-abstract-short" style="display: inline;"> Type-I X-ray bursts arise from unstable thermonuclear burning of accreted fuel on the surface of neutron stars. In this chapter we review the fundamental physics of the burning processes, and summarise the observational, numerical, and nuclear experimental progress over the preceding decade. We describe the current understanding of the conditions that lead to burst ignition, and the influence of t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1712.06227v1-abstract-full').style.display = 'inline'; document.getElementById('1712.06227v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1712.06227v1-abstract-full" style="display: none;"> Type-I X-ray bursts arise from unstable thermonuclear burning of accreted fuel on the surface of neutron stars. In this chapter we review the fundamental physics of the burning processes, and summarise the observational, numerical, and nuclear experimental progress over the preceding decade. We describe the current understanding of the conditions that lead to burst ignition, and the influence of the burst fuel on the observational characteristics. We provide an overview of the processes which shape the burst X-ray spectrum, including the observationally elusive discrete spectral features. We report on the studies of timing behaviour related to nuclear burning, including burst oscillations and mHz quasi-periodic oscillations. We describe the increasing role of nuclear experimental physics in the interpretation of astrophysical data and models. We survey the simulation projects that have taken place to date, and chart the increasing dialogue between modellers, observers, and nuclear experimentalists. Finally, we identify some open problems with prospects of a resolution within the timescale of the next such review. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1712.06227v1-abstract-full').style.display = 'none'; document.getElementById('1712.06227v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 December, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">57 pages, 14 figures; review to appear in "Timing Neutron Stars: Pulsations, Oscillations and Explosions", Editors: Tomaso Belloni and Mariano Mendez (ASSL, Springer)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1711.04389">arXiv:1711.04389</a> <span> [<a href="https://arxiv.org/pdf/1711.04389">pdf</a>, <a href="https://arxiv.org/ps/1711.04389">ps</a>, <a href="https://arxiv.org/format/1711.04389">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/aa9897">10.3847/1538-4357/aa9897 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On the dependence of X-ray burst rate on accretion and spin rate </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cavecchi%2C+Y">Yuri Cavecchi</a>, <a href="/search/astro-ph?searchtype=author&query=Watts%2C+A+L">Anna L. Watts</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+D+K">Duncan K. Galloway</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1711.04389v1-abstract-short" style="display: inline;"> Nuclear burning and its dependence on the mass accretion rate are fundamental ingredients for describing the complicated observational phenomenology of neutron stars in binary systems. Motivated by high quality burst rate data emerging from large statistical studies, we report general calculations relating bursting rate to mass accretion rate and neutron star rotation frequency. In this first work… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.04389v1-abstract-full').style.display = 'inline'; document.getElementById('1711.04389v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1711.04389v1-abstract-full" style="display: none;"> Nuclear burning and its dependence on the mass accretion rate are fundamental ingredients for describing the complicated observational phenomenology of neutron stars in binary systems. Motivated by high quality burst rate data emerging from large statistical studies, we report general calculations relating bursting rate to mass accretion rate and neutron star rotation frequency. In this first work we neglect general relativistic effects and accretion topology, though we discuss where their inclusion should play a role. The relations we derive are suitable for different burning regimes and provide a direct link between parameters predicted by theory and what is to be expected in observations. We illustrate this for analytical relations of different unstable burning regimes that operate on the surface of an accreting neutron star. We also use the observed behaviour of burst rate to suggest new constraints on burning parameters. We are able to provide an explanation for the long standing problem of the observed decrease of burst rate with increasing mass accretion that follows naturally from these calculations: when accretion rate crosses a certain threshold, ignition moves away from its initially preferential site and this can cause a net reduction of the burst rate due to the effects of local conditions that set local differences in both burst rate and stabilization criteria. We show under which conditions this can happen even if locally the burst rate keeps increasing with accretion. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.04389v1-abstract-full').style.display = 'none'; document.getElementById('1711.04389v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 November, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication on 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 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