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href="/search/?searchtype=author&query=Burgay%2C+M&start=200" class="pagination-link " aria-label="Page 5" aria-current="page">5 </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/2411.14895">arXiv:2411.14895</a> <span> [<a href="https://arxiv.org/pdf/2411.14895">pdf</a>, <a href="https://arxiv.org/format/2411.14895">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/10.1051/0004-6361/202451530">10.1051/0004-6361/202451530 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radio and gamma-ray timing of TRAPUM L-band Fermi pulsar survey discoveries </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Nieder%2C+L">L. Nieder</a>, <a href="/search/astro-ph?searchtype=author&query=Clark%2C+C+J">C. J. Clark</a>, <a href="/search/astro-ph?searchtype=author&query=Freire%2C+P+C+C">P. C. C. Freire</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Thongmeearkom%2C+T">T. Thongmeearkom</a>, <a href="/search/astro-ph?searchtype=author&query=Turner%2C+J+D">J. D. Turner</a>, <a href="/search/astro-ph?searchtype=author&query=Carli%2C+E">E. Carli</a>, <a href="/search/astro-ph?searchtype=author&query=Cognard%2C+I">I. Cognard</a>, <a href="/search/astro-ph?searchtype=author&query=Grie%C3%9Fmeier%2C+J+M">J. M. Grie脽meier</a>, <a href="/search/astro-ph?searchtype=author&query=Karuppusamy%2C+R">R. Karuppusamy</a>, <a href="/search/astro-ph?searchtype=author&query=Bernadich%2C+M+C+i">M. C. i Bernadich</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">V. Venkatraman Krishnan</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=Barr%2C+E+D">E. D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">B. W. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Levin%2C+L">L. Levin</a>, <a href="/search/astro-ph?searchtype=author&query=Ransom%2C+S+M">S. M. Ransom</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabh%2C+P+V">P. V. Padmanabh</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="2411.14895v1-abstract-short" style="display: inline;"> This paper presents the results of a joint radio and gamma-ray timing campaign on the nine millisecond pulsars (MSPs) discovered as part of the L-band targeted survey of Fermi-LAT sources performed in the context of the Transients and Pulsars with MeerKAT (TRAPUM) Large Survey Project. Out of these pulsars, eight are members of binary systems; of these eight, two exhibit extended eclipses of the r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.14895v1-abstract-full').style.display = 'inline'; document.getElementById('2411.14895v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.14895v1-abstract-full" style="display: none;"> This paper presents the results of a joint radio and gamma-ray timing campaign on the nine millisecond pulsars (MSPs) discovered as part of the L-band targeted survey of Fermi-LAT sources performed in the context of the Transients and Pulsars with MeerKAT (TRAPUM) Large Survey Project. Out of these pulsars, eight are members of binary systems; of these eight, two exhibit extended eclipses of the radio emission. Using an initial radio timing solution, pulsations were found in the gamma rays for six of the targets. For these sources, a joint timing analysis of radio times of arrival and gamma-ray photons was performed, using a newly developed code that optimises the parameters through a Markov chain Monte Carlo (MCMC) technique. This approach has allowed us to precisely measure both the short- and long-term timing parameters. This study includes a proper motion measurement for four pulsars, which a gamma ray-only analysis would not have been sensitive to, despite the 15-year span of Fermi data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.14895v1-abstract-full').style.display = 'none'; document.getElementById('2411.14895v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">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">20 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A, 691, A315 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.09288">arXiv:2410.09288</a> <span> [<a href="https://arxiv.org/pdf/2410.09288">pdf</a>, <a href="https://arxiv.org/format/2410.09288">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> The First High Frequency Technosignature Search Survey with the Sardinia Radio Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Manunza%2C+L">Lorenzo Manunza</a>, <a href="/search/astro-ph?searchtype=author&query=Vendrame%2C+A">Alice Vendrame</a>, <a href="/search/astro-ph?searchtype=author&query=Pizzuto%2C+L">Luca Pizzuto</a>, <a href="/search/astro-ph?searchtype=author&query=Mulas%2C+M">Monica Mulas</a>, <a href="/search/astro-ph?searchtype=author&query=Perez%2C+K+I">Karen I. Perez</a>, <a href="/search/astro-ph?searchtype=author&query=Gajjar%2C+V">Vishal Gajjar</a>, <a href="/search/astro-ph?searchtype=author&query=Melis%2C+A">Andrea Melis</a>, <a href="/search/astro-ph?searchtype=author&query=Pilia%2C+M">Maura Pilia</a>, <a href="/search/astro-ph?searchtype=author&query=Perrodin%2C+D">Delphine Perrodin</a>, <a href="/search/astro-ph?searchtype=author&query=Aresu%2C+G">Giambattista Aresu</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">Marta Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Cabras%2C+A">Alessandro Cabras</a>, <a href="/search/astro-ph?searchtype=author&query=Carboni%2C+G">Giuseppe Carboni</a>, <a href="/search/astro-ph?searchtype=author&query=Casu%2C+S">Silvia Casu</a>, <a href="/search/astro-ph?searchtype=author&query=Coiana%2C+T">Tiziana Coiana</a>, <a href="/search/astro-ph?searchtype=author&query=Corongiu%2C+A">Alessandro Corongiu</a>, <a href="/search/astro-ph?searchtype=author&query=Croft%2C+S">Steve Croft</a>, <a href="/search/astro-ph?searchtype=author&query=Egron%2C+E">Elise Egron</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+O+A">Owen A. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Ladu%2C+A">Adelaide Ladu</a>, <a href="/search/astro-ph?searchtype=author&query=Lebofsky%2C+M">Matt Lebofsky</a>, <a href="/search/astro-ph?searchtype=author&query=Loi%2C+F">Francesca Loi</a>, <a href="/search/astro-ph?searchtype=author&query=MacMahon%2C+D">David MacMahon</a>, <a href="/search/astro-ph?searchtype=author&query=Molinari%2C+E">Emilio Molinari</a>, <a href="/search/astro-ph?searchtype=author&query=Murgia%2C+M">Matteo Murgia</a> , et al. (8 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.09288v1-abstract-short" style="display: inline;"> The quest for radio signals from technologically-advanced extraterrestrial intelligence has traditionally concentrated on the vicinity of 1.4 GHz. In this paper, we extend the search to unprecedented territories, detailing our extensive observations at 6 GHz and initiating the first-ever survey at 18 GHz with the Sardinia Radio Telescope (SRT). Our strategy entailed rigorous observation sessions,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.09288v1-abstract-full').style.display = 'inline'; document.getElementById('2410.09288v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.09288v1-abstract-full" style="display: none;"> The quest for radio signals from technologically-advanced extraterrestrial intelligence has traditionally concentrated on the vicinity of 1.4 GHz. In this paper, we extend the search to unprecedented territories, detailing our extensive observations at 6 GHz and initiating the first-ever survey at 18 GHz with the Sardinia Radio Telescope (SRT). Our strategy entailed rigorous observation sessions, totaling 36 hours, directed towards the Galactic Center and 72 selected TESS targets-making this the most comprehensive high-frequency technosignature search to date. Our narrowband signal search found no definitive evidence of drifting signals that could suggest an extraterrestrial origin from the surveyed regions. Nevertheless, our efforts have enabled us to set new constraints on the presence of radio emissions from approximately $5\times 10^{5}$ stars, establishing an isotropic radiated power limit of $1.8\times 10^{19} W$. We also provide a comparative analysis of the 'hits' recorded across both frequencies to highlight the significance of pursuing technosignature searches at higher frequencies, where the spectral landscape is less congested and more conducive to detection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.09288v1-abstract-full').style.display = 'none'; document.getElementById('2410.09288v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to Acta Astronautica</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.04658">arXiv:2410.04658</a> <span> [<a href="https://arxiv.org/pdf/2410.04658">pdf</a>, <a href="https://arxiv.org/format/2410.04658">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/stae2308">10.1093/mnras/stae2308 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> TRAPUM pulsar and transient search in the Sextans A and B galaxies and discovery of background FRB 20210924D </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Carli%2C+E">E. Carli</a>, <a href="/search/astro-ph?searchtype=author&query=Levin%2C+L">L. Levin</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">B. W. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</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=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabh%2C+P+V">P. V. Padmanabh</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">V. Venkatraman Krishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Sridhar%2C+S+S">S. S. Sridhar</a>, <a href="/search/astro-ph?searchtype=author&query=Turner%2C+J+D">J. D. Turner</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.04658v1-abstract-short" style="display: inline;"> The Small and Large Magellanic Clouds are the only galaxies outside our own in which radio pulsars have been discovered to date. The sensitivity of the MeerKAT radio interferometer offers an opportunity to search for a population of more distant extragalactic pulsars. The TRAPUM (TRansients And PUlsars with MeerKAT) collaboration has performed a radio-domain search for pulsars and transients in th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.04658v1-abstract-full').style.display = 'inline'; document.getElementById('2410.04658v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.04658v1-abstract-full" style="display: none;"> The Small and Large Magellanic Clouds are the only galaxies outside our own in which radio pulsars have been discovered to date. The sensitivity of the MeerKAT radio interferometer offers an opportunity to search for a population of more distant extragalactic pulsars. The TRAPUM (TRansients And PUlsars with MeerKAT) collaboration has performed a radio-domain search for pulsars and transients in the dwarf star-forming galaxies Sextans A and B, situated at the edge of the local group 1.4 Mpc away. We conducted three 2-hour multi-beam observations at L-band (856-1712 MHz) with the full array of MeerKAT. No pulsars were found down to a radio pseudo-luminosity upper limit of 7.9$\pm$0.4 Jy kpc$^{2}$ at 1400 MHz, which is 28 times more sensitive than the previous limit from the Murriyang telescope. This luminosity is 30 per cent greater than that of the brightest known radio pulsar and sets a cut-off on the luminosity distributions of the entire Sextans A and B galaxies for unobscured radio pulsars beamed in our direction. A Fast Radio Burst was detected in one of the Sextans A observations at a Dispersion Measure (DM) of 737 pc cm$^{-3}$. We believe this is a background event not associated with the dwarf galaxy due to its large DM and its S/N being strongest in the wide-field incoherent beam of MeerKAT. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.04658v1-abstract-full').style.display = 'none'; document.getElementById('2410.04658v1-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 9 figures, 5 tables. 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/2409.03615">arXiv:2409.03615</a> <span> [<a href="https://arxiv.org/pdf/2409.03615">pdf</a>, <a href="https://arxiv.org/format/2409.03615">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/10.1051/0004-6361/202347482">10.1051/0004-6361/202347482 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Triple trouble with PSR J1618-3921: Mass measurements and orbital dynamics of an eccentric millisecond pulsar </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Grunthal%2C+K">K. Grunthal</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">V. Venkatraman Krishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Freire%2C+P+C+C">P. C. C. Freire</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+A+D">A. D. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+C+-+R">C. -H. R. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cognard%2C+I">I. Cognard</a>, <a href="/search/astro-ph?searchtype=author&query=Guillemot%2C+L">L. Guillemot</a>, <a href="/search/astro-ph?searchtype=author&query=Lower%2C+M+E">M. E. Lower</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Theureau%2C+G">G. Theureau</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.03615v1-abstract-short" style="display: inline;"> PSR J1618-3921 is one of five known millisecond pulsars (MSPs) in eccentric orbits (eMPSs) located in the Galactic plane, whose formation is poorly understood. Earlier studies of these objects revealed significant discrepancies between observation and predictions from standard binary evolution scenarios of pulsar-Helium white dwarf binaries. We conducted observations with the L-band receiver of th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.03615v1-abstract-full').style.display = 'inline'; document.getElementById('2409.03615v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.03615v1-abstract-full" style="display: none;"> PSR J1618-3921 is one of five known millisecond pulsars (MSPs) in eccentric orbits (eMPSs) located in the Galactic plane, whose formation is poorly understood. Earlier studies of these objects revealed significant discrepancies between observation and predictions from standard binary evolution scenarios of pulsar-Helium white dwarf binaries. We conducted observations with the L-band receiver of the MeerKAT radio telescope and the UWL receiver of the Parkes Murriyang radio telescope between 2019 and 2021. These data were added to archival observations. We perform an analysis of this joint 23-year-dataset. We use the recent observations to give a brief account of the emission properties of J1618-3921, including a Rotating Vector model fit of the linear polarisation position angle of the pulsar. The long timing baseline allowed for a highly significant measurement of the rate of advance of periastron of $\dot蠅$. We can only report a low significance detection of the orthometric Shapiro delay parameters $h_3$ and $蟼$, leading to mass estimates of the total and individual binary masses. We detect an unexpected change in the orbital period of, which is an order of magnitude larger and carries an opposite sign to what is expected from Galactic acceleration and the Shklovskii effect. We also detect a significant second derivative of the spin frequency. Furthermore, we report an unexpected, abrupt change of the mean pulse profile in June 2021 with unknown origin. We propose that the anomalous $\dot{P_b}$ and $\ddot{f}$ indicate an additional varying acceleration due to a nearby mass, i.e., the J1618-3921 binary system is likely part of a hierarchical triple. This finding suggests that at least some eMSPs might have formed in triple star systems. Although the uncertainties are large, the binary companion mass is consistent with the $P_b$ - $M_{WD}$ relation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.03615v1-abstract-full').style.display = 'none'; document.getElementById('2409.03615v1-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, 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">17 pages, 11 figures, 3 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 691, A22 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.14384">arXiv:2408.14384</a> <span> [<a href="https://arxiv.org/pdf/2408.14384">pdf</a>, <a href="https://arxiv.org/format/2408.14384">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/10.1051/0004-6361/202450775">10.1051/0004-6361/202450775 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Eighteen new fast radio bursts in the High Time Resolution Universe survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Trudu%2C+M">M. Trudu</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Pilia%2C+M">M. Pilia</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Keane%2C+E+F">E. F. Keane</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Balakrishnan%2C+V">V. Balakrishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Bhandari%2C+S">S. Bhandari</a>, <a href="/search/astro-ph?searchtype=author&query=Bhat%2C+N+D+R">N. D. R. Bhat</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+A">A. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Jameson%2C+A">A. Jameson</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+S">S. Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Keith%2C+M+J">M. J. Keith</a>, <a href="/search/astro-ph?searchtype=author&query=Levin%2C+L">L. Levin</a>, <a href="/search/astro-ph?searchtype=author&query=Ng%2C+C">C. Ng</a>, <a href="/search/astro-ph?searchtype=author&query=Sengar%2C+R">R. Sengar</a>, <a href="/search/astro-ph?searchtype=author&query=Tiburzi%2C+C">C. Tiburzi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.14384v1-abstract-short" style="display: inline;"> Current observational evidence reveals that fast radio bursts (FRBs) exhibit bandwidths ranging from a few dozen MHz to several GHz. Traditional FRB searches primarily employ matched filter methods on time series collapsed across the entire observational bandwidth. However, with modern ultra-wideband receivers featuring GHz-scale observational bandwidths, this approach may overlook a significant n… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.14384v1-abstract-full').style.display = 'inline'; document.getElementById('2408.14384v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.14384v1-abstract-full" style="display: none;"> Current observational evidence reveals that fast radio bursts (FRBs) exhibit bandwidths ranging from a few dozen MHz to several GHz. Traditional FRB searches primarily employ matched filter methods on time series collapsed across the entire observational bandwidth. However, with modern ultra-wideband receivers featuring GHz-scale observational bandwidths, this approach may overlook a significant number of events. We investigate the efficacy of sub-banded searches for FRBs, a technique seeking bursts within limited portions of the bandwidth. These searches aim to enhance the significance of FRB detections by mitigating the impact of noise outside the targeted frequency range, thereby improving signal-to-noise ratios. We conducted a series of Monte Carlo simulations, for the $400$-MHz bandwidth Parkes 21-cm multi-beam (PMB) receiver system and the Parkes Ultra-Wideband Low (UWL) receiver, simulating bursts down to frequency widths of about $100$\,MHz. Additionally, we performed a complete reprocessing of the high-latitude segment of the High Time Resolution Universe South survey (HTRU-S) of the Parkes-Murriyang telescope using sub-banded search techniques. Simulations reveal that a sub-banded search can enhance the burst search efficiency by $67_{-42}^{+133}$ % for the PMB system and $1433_{-126}^{+143}$ % for the UWL receiver. Furthermore, the reprocessing of HTRU led to the confident detection of eighteen new bursts, nearly tripling the count of FRBs found in this survey. These results underscore the importance of employing sub-banded search methodologies to effectively address the often modest spectral occupancy of these signals. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.14384v1-abstract-full').style.display = 'none'; document.getElementById('2408.14384v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication (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 690, A204 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.04899">arXiv:2408.04899</a> <span> [<a href="https://arxiv.org/pdf/2408.04899">pdf</a>, <a href="https://arxiv.org/format/2408.04899">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/stae1917">10.1093/mnras/stae1917 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The TRAPUM Large Magellanic Cloud pulsar survey with MeerKAT I: Survey setup and first seven pulsar discoveries </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Prayag%2C+V">V. Prayag</a>, <a href="/search/astro-ph?searchtype=author&query=Levin%2C+L">L. Levin</a>, <a href="/search/astro-ph?searchtype=author&query=Geyer%2C+M">M. Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">B. W. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Carli%2C+E">E. Carli</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</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=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">V. Venkatraman Krishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Venter%2C+C">C. Venter</a>, <a href="/search/astro-ph?searchtype=author&query=Behrend%2C+J">J. Behrend</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">W. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Horn%2C+D+M">D. M. Horn</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabh%2C+P+V">P. V. Padmanabh</a>, <a href="/search/astro-ph?searchtype=author&query=Ridolfi%2C+A">A. Ridolfi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.04899v1-abstract-short" style="display: inline;"> The Large Magellanic Cloud (LMC) presents a unique environment for pulsar population studies due to its distinct star formation characteristics and proximity to the Milky Way. As part of the TRAPUM (TRAnsients and PUlsars with MeerKAT) Large Survey Project, we are using the core array of the MeerKAT radio telescope (MeerKAT) to conduct a targeted search of the LMC for radio pulsars at L-band frequ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.04899v1-abstract-full').style.display = 'inline'; document.getElementById('2408.04899v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.04899v1-abstract-full" style="display: none;"> The Large Magellanic Cloud (LMC) presents a unique environment for pulsar population studies due to its distinct star formation characteristics and proximity to the Milky Way. As part of the TRAPUM (TRAnsients and PUlsars with MeerKAT) Large Survey Project, we are using the core array of the MeerKAT radio telescope (MeerKAT) to conduct a targeted search of the LMC for radio pulsars at L-band frequencies, 856-1712$\,$MHz. The excellent sensitivity of MeerKAT, coupled with a 2-hour integration time, makes the survey 3 times more sensitive than previous LMC radio pulsar surveys. We report the results from the initial four survey pointings which has resulted in the discovery of seven new radio pulsars, increasing the LMC radio pulsar population by 30 per cent. The pulse periods of these new pulsars range from 278 to 1690$\,$ms, and the highest dispersion measure is 254.20$\,$pc$\,$cm$^{-3}$. We searched for, but did not find any significant pulsed radio emission in a beam centred on the SN$\,$1987A remnant, establishing an upper limit of 6.3$\,渭$Jy on its minimum flux density at 1400$\,$MHz. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.04899v1-abstract-full').style.display = 'none'; document.getElementById('2408.04899v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 4 figures, 4 tables. 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/2408.01965">arXiv:2408.01965</a> <span> [<a href="https://arxiv.org/pdf/2408.01965">pdf</a>, <a href="https://arxiv.org/format/2408.01965">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/stae1897">10.1093/mnras/stae1897 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The TRAPUM Small Magellanic Cloud pulsar survey with MeerKAT -- II. Nine new radio timing solutions and glitches from young pulsars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Carli%2C+E">E. Carli</a>, <a href="/search/astro-ph?searchtype=author&query=Antonopoulou%2C+D">D. Antonopoulou</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Keith%2C+M+J">M. J. Keith</a>, <a href="/search/astro-ph?searchtype=author&query=Levin%2C+L">L. Levin</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Y. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">B. W. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Turner%2C+J+D">J. D. Turner</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</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=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabh%2C+P+V">P. V. Padmanabh</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">V. Venkatraman Krishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Venter%2C+C">C. Venter</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+W">W. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Maitra%2C+C">C. Maitra</a>, <a href="/search/astro-ph?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/astro-ph?searchtype=author&query=Thongmeearkom%2C+T">T. Thongmeearkom</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.01965v1-abstract-short" style="display: inline;"> We report new radio timing solutions from a three-year observing campaign conducted with the MeerKAT and Murriyang telescopes for nine Small Magellanic Cloud pulsars, increasing the number of characterised rotation-powered extragalactic pulsars by 40 per cent. We can infer from our determined parameters that the pulsars are seemingly all isolated, that six are ordinary pulsars, and that three of t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.01965v1-abstract-full').style.display = 'inline'; document.getElementById('2408.01965v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.01965v1-abstract-full" style="display: none;"> We report new radio timing solutions from a three-year observing campaign conducted with the MeerKAT and Murriyang telescopes for nine Small Magellanic Cloud pulsars, increasing the number of characterised rotation-powered extragalactic pulsars by 40 per cent. We can infer from our determined parameters that the pulsars are seemingly all isolated, that six are ordinary pulsars, and that three of the recent MeerKAT discoveries have a young characteristic age of under 100 kyr and have undergone a spin-up glitch. Two of the sources, PSRs J0040$-$7337 and J0048$-$7317, are energetic young pulsars with spin-down luminosities of the order of 10$^{36}$ erg s$^{-1}$. They both experienced a large glitch, with a change in frequency of about 30 $渭$Hz, and a frequency derivative change of order $-10^{-14}$ Hz s$^{-1}$. These glitches, the inferred glitch rate, and the properties of these pulsars (including potentially high inter-glitch braking indices) suggest these neutron stars might be Vela-like repeating glitchers and should be closely monitored in the future. The position and energetics of PSR J0048$-$7317 confirm it is powering a new Pulsar Wind Nebula (PWN) detected as a radio continuum source; and similarly the association of PSR J0040$-$7337 with the PWN of Supernova Remnant (SNR) DEM S5 (for which we present a new Chandra image) is strengthened. Finally, PSR J0040$-$7335 is also contained within the same SNR but is a chance superposition. It has also been seen to glitch with a change of frequency of $10^{-2}$ $渭$Hz. This work more than doubles the characterised population of SMC radio pulsars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.01965v1-abstract-full').style.display = 'none'; document.getElementById('2408.01965v1-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 13 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/2407.03271">arXiv:2407.03271</a> <span> [<a href="https://arxiv.org/pdf/2407.03271">pdf</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/ad5e74">10.3847/1538-4357/ad5e74 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Timing of millisecond pulsars in NGC\,6752 -- III. On the presence of non-luminous matter in the cluster's core </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Corongiu%2C+A">A. Corongiu</a>, <a href="/search/astro-ph?searchtype=author&query=Ridolfi%2C+A">A. Ridolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Abbate%2C+F">F. Abbate</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Geyer%2C+M">M. Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Manchester%2C+R+N">R. N. Manchester</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Freire%2C+P+C+C">P. C. C. Freire</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</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="2407.03271v2-abstract-short" style="display: inline;"> Millisecond pulsars are subject to accelerations in globular clusters (GCs) that manifest themselves in both the first and second spin period time derivatives, and can be used to explore the mass distribution of the potentials they inhabit. Here we report on over 20 yr of pulsar timing observations of five millisecond radio pulsars in the core of the core-collapse GC NGC 6752 with the Parkes (Murr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.03271v2-abstract-full').style.display = 'inline'; document.getElementById('2407.03271v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.03271v2-abstract-full" style="display: none;"> Millisecond pulsars are subject to accelerations in globular clusters (GCs) that manifest themselves in both the first and second spin period time derivatives, and can be used to explore the mass distribution of the potentials they inhabit. Here we report on over 20 yr of pulsar timing observations of five millisecond radio pulsars in the core of the core-collapse GC NGC 6752 with the Parkes (Murriyang) and MeerKAT radio telescopes, which have allowed us to measure the proper motions, positions, and first and second time derivatives of the pulsars. The pulsar timing parameters indicate that all the pulsars in the core experience accelerations and jerks that can be explained only if an amount of nonluminous mass of at least 2.56x10^3 M_SUN is present in the core of NGC 6752. On the other hand, our studies highly disfavor the presence of an intermediate-mass black hole at the center of the cluster, with a mass equal to or greater than ~3000M_SUN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.03271v2-abstract-full').style.display = 'none'; document.getElementById('2407.03271v2-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 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">Published in ApJ. Replaced with the final published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal: The Astrophysical Journal; Volume 972; Year 2024; Page 198 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.12029">arXiv:2405.12029</a> <span> [<a href="https://arxiv.org/pdf/2405.12029">pdf</a>, <a href="https://arxiv.org/format/2405.12029">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stae1310">10.1093/mnras/stae1310 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The TRAPUM Small Magellanic Cloud pulsar survey with MeerKAT: I. Discovery of seven new pulsars and two Pulsar Wind Nebula associations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Carli%2C+E">E. Carli</a>, <a href="/search/astro-ph?searchtype=author&query=Levin%2C+L">L. Levin</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">B. W. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</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=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Geyer%2C+M">M. Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabh%2C+P+V">P. V. Padmanabh</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">V. Venkatraman Krishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+W">W. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Filipovi%C4%87%2C+M+D">M. D. Filipovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Maitra%2C+C">C. Maitra</a>, <a href="/search/astro-ph?searchtype=author&query=Behrend%2C+J">J. Behrend</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">W. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Men%2C+Y+P">Y. P. Men</a>, <a href="/search/astro-ph?searchtype=author&query=Ridolfi%2C+A">A. Ridolfi</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="2405.12029v1-abstract-short" style="display: inline;"> The sensitivity of the MeerKAT radio interferometer is an opportunity to probe deeper into the population of rare and faint extragalactic pulsars. The TRAPUM (TRAnsients and PUlsars with MeerKAT) collaboration has conducted a radio-domain search for accelerated pulsars and transients in the Small Magellanic Cloud (SMC). This partially targeted survey, performed at L-band (856-1712 MHz) with the co… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.12029v1-abstract-full').style.display = 'inline'; document.getElementById('2405.12029v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.12029v1-abstract-full" style="display: none;"> The sensitivity of the MeerKAT radio interferometer is an opportunity to probe deeper into the population of rare and faint extragalactic pulsars. The TRAPUM (TRAnsients and PUlsars with MeerKAT) collaboration has conducted a radio-domain search for accelerated pulsars and transients in the Small Magellanic Cloud (SMC). This partially targeted survey, performed at L-band (856-1712 MHz) with the core array of the MeerKAT telescope in 2-h integrations, is twice as sensitive as the latest SMC radio pulsar survey. We report the discovery of seven new SMC pulsars, doubling this galaxy's radio pulsar population and increasing the total extragalactic population by nearly a quarter. We also carried out a search for accelerated millisecond pulsars in the SMC Globular Cluster NGC 121 using the full array of MeerKAT. This improved the previous upper limit on pulsed radio emission from this cluster by a factor of six. Our discoveries reveal the first radio pulsar-PWN systems in the SMC, with only one such system previously known outside our galaxy (the "Crab pulsar twin" in the Large Magellanic Cloud, PSR J0540$-$6919). We associate the 59 ms pulsar discovery PSR J0040$-$7337, now the fastest spinning radio pulsar in the SMC, with the bow-shock Pulsar Wind Nebula (PWN) of Supernova Remnant DEM S5. We also present a new young pulsar with a 79 ms period, PSR J0048$-$7317, in a PWN recently discovered in a MeerKAT radio continuum image. Using the multi-beam capability of MeerKAT, we localised our pulsar discoveries, and two previous Murriyang discoveries, to a positional uncertainty of a few arcseconds. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.12029v1-abstract-full').style.display = 'none'; document.getElementById('2405.12029v1-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, 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">32 pages, 14 figures, 10 tables. 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/2405.11899">arXiv:2405.11899</a> <span> [<a href="https://arxiv.org/pdf/2405.11899">pdf</a>, <a href="https://arxiv.org/format/2405.11899">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/stae1300">10.1093/mnras/stae1300 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> TRAPUM search for pulsars in supernova remnants and pulsar wind nebulae -- I. Survey description and initial discoveries </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Turner%2C+J+D">J. D. Turner</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">B. W. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Carli%2C+E">E. Carli</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+W">W. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Behrend%2C+J">J. Behrend</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=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">W. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Clark%2C+C+J">C. J. Clark</a>, <a href="/search/astro-ph?searchtype=author&query=Horn%2C+D+M">D. M. Horn</a>, <a href="/search/astro-ph?searchtype=author&query=Keane%2C+E+F">E. F. Keane</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=%C3%BCnkel%2C+L+K">L. K 眉nkel</a>, <a href="/search/astro-ph?searchtype=author&query=Levin%2C+L">L. Levin</a>, <a href="/search/astro-ph?searchtype=author&query=Men%2C+Y+P">Y. P. Men</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabh%2C+P+V">P. V. Padmanabh</a>, <a href="/search/astro-ph?searchtype=author&query=Ridolfi%2C+A">A. Ridolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">V. Venkatraman Krishnan</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="2405.11899v1-abstract-short" style="display: inline;"> We present the description and initial results of the TRAPUM (TRAnsients And PUlsars with MeerKAT) search for pulsars associated with supernova remnants (SNRs), pulsar wind nebulae and unidentified TeV emission. The list of sources to be targeted includes a large number of well-known candidate pulsar locations but also new candidate SNRs identified using a range of criteria. Using the 64-dish Meer… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.11899v1-abstract-full').style.display = 'inline'; document.getElementById('2405.11899v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.11899v1-abstract-full" style="display: none;"> We present the description and initial results of the TRAPUM (TRAnsients And PUlsars with MeerKAT) search for pulsars associated with supernova remnants (SNRs), pulsar wind nebulae and unidentified TeV emission. The list of sources to be targeted includes a large number of well-known candidate pulsar locations but also new candidate SNRs identified using a range of criteria. Using the 64-dish MeerKAT radio telescope, we use an interferometric beamforming technique to tile the potential pulsar locations with coherent beams which we search for radio pulsations, above a signal-to-noise of 9, down to an average flux density upper limit of 30 $渭$Jy. This limit is target-dependent due to the contribution of the sky and nebula to the system temperature. Coherent beams are arranged to overlap at their 50 per cent power radius, so the sensitivity to pulsars is not degraded by more than this amount, though realistically averages around 65 per cent if every location in the beam is considered. We report the discovery of two new pulsars; PSR J1831$-$0941 is an adolescent pulsar likely to be the plerionic engine of the candidate PWN G20.0+0.0, and PSR J1818$-$1502 appears to be an old and faint pulsar that we serendipitously discovered near the centre of a SNR already hosting a compact central object. The survey holds importance for better understanding of neutron star birth rates and the energetics of young pulsars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.11899v1-abstract-full').style.display = 'none'; document.getElementById('2405.11899v1-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, 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">17 pages, 6 figures, 3 tables. 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/2403.17799">arXiv:2403.17799</a> <span> [<a href="https://arxiv.org/pdf/2403.17799">pdf</a>, <a href="https://arxiv.org/format/2403.17799">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/10.1051/0004-6361/202449303">10.1051/0004-6361/202449303 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery and timing of ten new millisecond pulsars in the globular cluster Terzan 5 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Padmanabh%2C+P+V">P. V. Padmanabh</a>, <a href="/search/astro-ph?searchtype=author&query=Ransom%2C+S+M">S. M. Ransom</a>, <a href="/search/astro-ph?searchtype=author&query=Freire%2C+P+C+C">P. C. C. Freire</a>, <a href="/search/astro-ph?searchtype=author&query=Ridolfi%2C+A">A. Ridolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+J+D">J. D. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Choza%2C+C">C. Choza</a>, <a href="/search/astro-ph?searchtype=author&query=Clark%2C+C+J">C. J. Clark</a>, <a href="/search/astro-ph?searchtype=author&query=Abbate%2C+F">F. Abbate</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=DeCesar%2C+M+E">M. E. DeCesar</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">W. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Corongiu%2C+A">A. Corongiu</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Dutta%2C+A">A. Dutta</a>, <a href="/search/astro-ph?searchtype=author&query=Geyer%2C+M">M. Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Hessels%2C+J+W+T">J. W. T. Hessels</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Stairs%2C+I+H">I. H. Stairs</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">B. W. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">V. Venkatraman Krishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Vleeschower%2C+L">L. Vleeschower</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.17799v2-abstract-short" style="display: inline;"> We report the discovery of ten new pulsars in the globular cluster Terzan 5 as part of the Transients and Pulsars with MeerKAT (TRAPUM) Large Survey Project. We observed Terzan 5 at L-band (856--1712 MHz) with the MeerKAT radio telescope for four hours on two epochs, and performed acceleration searches of 45 out of 288 tied-array beams covering the core of the cluster. We obtained phase-connected… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.17799v2-abstract-full').style.display = 'inline'; document.getElementById('2403.17799v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.17799v2-abstract-full" style="display: none;"> We report the discovery of ten new pulsars in the globular cluster Terzan 5 as part of the Transients and Pulsars with MeerKAT (TRAPUM) Large Survey Project. We observed Terzan 5 at L-band (856--1712 MHz) with the MeerKAT radio telescope for four hours on two epochs, and performed acceleration searches of 45 out of 288 tied-array beams covering the core of the cluster. We obtained phase-connected timing solutions for nine discoveries, covering nearly two decades of archival observations from the Green Bank Telescope for all but one. Highlights include PSR J1748$-$2446ao which is an eccentric ($e = 0.32$) wide-orbit (orbital period $P_{\rm b} = 57.55$ d) system. We were able to measure the rate of advance of periastron ($\dot蠅$) for this system allowing us to determine a total mass of $3.17 \pm \, 0.02\, \rm M_{\odot}$. With a minimum companion mass ($M_{\rm c}$) of $\sim 0.8\, \rm M_{\odot}$, PSR J1748$-$2446ao is a candidate double neutron star (DNS) system. If confirmed to be a DNS, it would be the fastest spinning pulsar ($P = 2.27$ ms) and the longest orbital period measured for any known DNS system. PSR J1748$-$2446ap has the second highest eccentricity for any recycled pulsar ($e \sim 0.905$) and for this system we can measure the total mass ($1.997 \pm 0.006\, \rm M_{\odot}$) and also estimate the individual pulsar and companion masses. PSR J1748$-$2446ar is an eclipsing redback (minimum $M_{\rm c} \sim 0.34\, \rm M_{\odot}$) system whose properties confirm it to be the counterpart to a previously published source identified in radio and X-ray imaging. With these discoveries, the total number of confirmed pulsars in Terzan 5 is 49, the highest for any globular cluster so far. These discoveries further enhance the rich set of pulsars known in Terzan 5 and provide scope for a deeper understanding of binary stellar evolution, cluster dynamics and ensemble population studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.17799v2-abstract-full').style.display = 'none'; document.getElementById('2403.17799v2-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 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">23 pages, 11 figures, 5 tables, published 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 686, A166 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.09553">arXiv:2403.09553</a> <span> [<a href="https://arxiv.org/pdf/2403.09553">pdf</a>, <a href="https://arxiv.org/format/2403.09553">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"> A targeted radio pulsar survey of redback candidates with MeerKAT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Thongmeearkom%2C+T">T. Thongmeearkom</a>, <a href="/search/astro-ph?searchtype=author&query=Clark%2C+C+J">C. J. Clark</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=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Nieder%2C+L">L. Nieder</a>, <a href="/search/astro-ph?searchtype=author&query=Freire%2C+P+C+C">P. C. C. Freire</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">B. W. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Ransom%2C+S+M">S. M. Ransom</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Calore%2C+F">F. Calore</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Cognard%2C+I">I. Cognard</a>, <a href="/search/astro-ph?searchtype=author&query=Grie%C3%9Fmeier%2C+J+-">J. -M. Grie脽meier</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Levin%2C+L">L. Levin</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabh%2C+P+V">P. V. Padmanabh</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Ridolfi%2C+A">A. Ridolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">V. Venkatraman Krishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Vleeschower%2C+L">L. Vleeschower</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="2403.09553v1-abstract-short" style="display: inline;"> Redbacks are millisecond pulsar binaries with low mass, irradiated companions. These systems have a rich phenomenology that can be used to probe binary evolution models, pulsar wind physics, and the neutron star mass distribution. A number of high-confidence redback candidates have been identified through searches for variable optical and X-ray sources within the localisation regions of unidentifi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.09553v1-abstract-full').style.display = 'inline'; document.getElementById('2403.09553v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.09553v1-abstract-full" style="display: none;"> Redbacks are millisecond pulsar binaries with low mass, irradiated companions. These systems have a rich phenomenology that can be used to probe binary evolution models, pulsar wind physics, and the neutron star mass distribution. A number of high-confidence redback candidates have been identified through searches for variable optical and X-ray sources within the localisation regions of unidentified but pulsar-like Fermi-LAT gamma-ray sources. However, these candidates remain unconfirmed until pulsations are detected. As part of the TRAPUM project, we searched for radio pulsations from six of these redback candidates with MeerKAT. We discovered three new radio millisecond pulsars, PSRs J0838$-$2527, J0955$-$3947 and J2333$-$5526, confirming their redback nature. PSR J0838$-$2827 remained undetected for two years after our discovery despite repeated observations, likely due to evaporated material absorbing the radio emission for long periods of time. While, to our knowledge, this system has not undergone a transition to an accreting state, the disappearance, likely caused by extreme eclipses, illustrates the transient nature of spider pulsars and the heavy selection bias in uncovering their radio population. Radio timing enabled the detection of gamma-ray pulsations from all three pulsars, from which we obtained 15-year timing solutions. All of these sources exhibit complex orbital period variations consistent with gravitational quadrupole moment variations in the companion stars. These timing solutions also constrain the binary mass ratios, allowing us to narrow down the pulsar masses. We find that PSR J2333$-$5526 may have a neutron star mass in excess of 2 M$_{\odot}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.09553v1-abstract-full').style.display = 'none'; document.getElementById('2403.09553v1-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 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">19 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/2403.01941">arXiv:2403.01941</a> <span> [<a href="https://arxiv.org/pdf/2403.01941">pdf</a>, <a href="https://arxiv.org/ps/2403.01941">ps</a>, <a href="https://arxiv.org/format/2403.01941">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/10.1051/0004-6361/202349033">10.1051/0004-6361/202349033 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing the emission mechanism and nature of the pulsating compact object in the X-ray binary SAX J1324.4-6200 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ducci%2C+L">L. Ducci</a>, <a href="/search/astro-ph?searchtype=author&query=Bozzo%2C+E">E. Bozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Malacaria%2C+C">C. Malacaria</a>, <a href="/search/astro-ph?searchtype=author&query=Ridolfi%2C+A">A. Ridolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Romano%2C+P">P. Romano</a>, <a href="/search/astro-ph?searchtype=author&query=Serim%2C+M+M">M. M. Serim</a>, <a href="/search/astro-ph?searchtype=author&query=Vercellone%2C+S">S. Vercellone</a>, <a href="/search/astro-ph?searchtype=author&query=Santangelo%2C+A">A. Santangelo</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="2403.01941v1-abstract-short" style="display: inline;"> Recently, there has been renewed interest in the Be X-ray binary (Be/XRB) SAX J1324.4-6200 because of its spatial coincidence with a gamma-ray source detected by Fermi/LAT. To explore more thoroughly its properties, new observations were carried out in 2023 by NuSTAR, XMM-Newton, and Swift, jointly covering the energy range 0.2-79 keV. The X-ray spectrum of SAX J1324.4-6200 fits well with an absor… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.01941v1-abstract-full').style.display = 'inline'; document.getElementById('2403.01941v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.01941v1-abstract-full" style="display: none;"> Recently, there has been renewed interest in the Be X-ray binary (Be/XRB) SAX J1324.4-6200 because of its spatial coincidence with a gamma-ray source detected by Fermi/LAT. To explore more thoroughly its properties, new observations were carried out in 2023 by NuSTAR, XMM-Newton, and Swift, jointly covering the energy range 0.2-79 keV. The X-ray spectrum of SAX J1324.4-6200 fits well with an absorbed power law with a high energy cut-off. We measured a NuSTAR spin period of 175.8127 +/- 0.0036 s and an XMM-Newton spin period of 175.862 +/- 0.025 s. All the available spin period measurements of SAX J1324.4-6200, spanning 29 years, are correlated with time, resulting in a remarkably stable spin-down of dP/dt=(6.09 +/- 0.06)*1E-9 s/s. If SAX J1324.4-6200 hosts an accretion powered pulsar, accretion torque models indicate a surface magnetic field of ~1E12-1E13 G. The X-ray properties emerging from our analysis strenghten the hypothesis that SAX J1324.4-6200 belongs to the small group of persistent Be/XRBs. We also performed radio observations with the Parkes Murriyang telescope, to search for radio pulsations. However, no radio pulsations compatible with the rotational ephemeris of SAX J1324.4-6200 were detected. We rule out the hypothesis that SAX J1324.4-6200 is a gamma-ray binary where the emission is produced by interactions between the pulsar and the companion winds. Other models commonly used to account for the production of gamma-rays in accreting pulsars cannot reproduce the bright emission from SAX J1324.4-6200. We examined other mechanisms for the gamma-ray emission and noted that there is a ~0.5% chance probability that an unknown extragalactic AGN observed through the Galactic plane may coincidentally fall within the Fermi/LAT error circle of the source and be the responsible of the gamma-ray emission. [Abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.01941v1-abstract-full').style.display = 'none'; document.getElementById('2403.01941v1-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 685, A148 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.08596">arXiv:2402.08596</a> <span> [<a href="https://arxiv.org/pdf/2402.08596">pdf</a>, <a href="https://arxiv.org/format/2402.08596">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"> An X-ray and radio view of the 2022 reactivation of the magnetar SGRJ1935+2154 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ibrahim%2C+A+Y">A. Y. Ibrahim</a>, <a href="/search/astro-ph?searchtype=author&query=Borghese%2C+A">A. Borghese</a>, <a href="/search/astro-ph?searchtype=author&query=Zelati%2C+F+C">F. Coti Zelati</a>, <a href="/search/astro-ph?searchtype=author&query=Parent%2C+E">E. Parent</a>, <a href="/search/astro-ph?searchtype=author&query=Marino%2C+A">A. Marino</a>, <a href="/search/astro-ph?searchtype=author&query=Ould-Boukattine%2C+O+S">O. S. Ould-Boukattine</a>, <a href="/search/astro-ph?searchtype=author&query=Rea%2C+N">N. Rea</a>, <a href="/search/astro-ph?searchtype=author&query=Ascenzi%2C+S">S. Ascenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Pacholski%2C+D+P">D. P. Pacholski</a>, <a href="/search/astro-ph?searchtype=author&query=Mereghetti%2C+S">S. Mereghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Israel%2C+G+L">G. L. Israel</a>, <a href="/search/astro-ph?searchtype=author&query=Tiengo%2C+A">A. Tiengo</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Turolla%2C+R">R. Turolla</a>, <a href="/search/astro-ph?searchtype=author&query=Zane%2C+S">S. Zane</a>, <a href="/search/astro-ph?searchtype=author&query=Esposito%2C+P">P. Esposito</a>, <a href="/search/astro-ph?searchtype=author&query=Gotz%2C+D">D. Gotz</a>, <a href="/search/astro-ph?searchtype=author&query=Campana%2C+S">S. Campana</a>, <a href="/search/astro-ph?searchtype=author&query=Kirsten%2C+F">F. Kirsten</a>, <a href="/search/astro-ph?searchtype=author&query=Gawronski%2C+M+P">M. P. Gawronski</a>, <a href="/search/astro-ph?searchtype=author&query=Hessels%2C+J+W+T">J. W. T. Hessels</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.08596v1-abstract-short" style="display: inline;"> Recently, the Galactic magnetar SGR J1935+2154 has garnered attention due to its emission of an extremely luminous radio burst, reminiscent of Fast Radio Bursts (FRBs). SGR J1935+2154 is one of the most active magnetars, displaying flaring events nearly every year, including outbursts as well as short and intermediate bursts. Here, we present our results on the properties of the persistent and bur… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08596v1-abstract-full').style.display = 'inline'; document.getElementById('2402.08596v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.08596v1-abstract-full" style="display: none;"> Recently, the Galactic magnetar SGR J1935+2154 has garnered attention due to its emission of an extremely luminous radio burst, reminiscent of Fast Radio Bursts (FRBs). SGR J1935+2154 is one of the most active magnetars, displaying flaring events nearly every year, including outbursts as well as short and intermediate bursts. Here, we present our results on the properties of the persistent and bursting X-ray emission from SGR J1935+2154, during the initial weeks following its outburst on October 10, 2022. The source was observed with XMM-Newton and NuSTAR (quasi-)simultaneously during two epochs, separated by $\sim$5 days. The persistent emission spectrum is well described by an absorbed blackbody plus power-law model up to an energy of $\sim$25 keV. No significant changes were observed in the blackbody temperature ($kT_{\rm BB}\sim$ 0.4 keV) and emitting radius ($R_{\rm BB}\sim$ 1.9 km) between the two epochs. However, we observed a slight variation in the power-law parameters. Moreover, we detected X-ray pulsations in all the datasets and derived a spin period derivative of $\dot{P} = 5.52(5) \times 10^{-11}$ ss. This is 3.8 times larger than the value measured after the first recorded outburst in 2014. Additionally, we performed quasi-simultaneous radio observations using three 25--32-m class radio telescopes for a total of 92.5 hr to search for FRB-like radio bursts and pulsed emission. However, our analysis did not reveal any radio bursts or periodic emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08596v1-abstract-full').style.display = 'none'; document.getElementById('2402.08596v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 6 figures, accepted for publication on 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/2401.09928">arXiv:2401.09928</a> <span> [<a href="https://arxiv.org/pdf/2401.09928">pdf</a>, <a href="https://arxiv.org/format/2401.09928">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"> Mass estimates from optical modelling of the new TRAPUM redback PSR J1910-5320 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dodge%2C+O+G">O. G. Dodge</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=Clark%2C+C+J">C. J. Clark</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Strader%2C+J">J. Strader</a>, <a href="/search/astro-ph?searchtype=author&query=Au%2C+K+-">K. -Y. Au</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">S. Buchner</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=Ferrara%2C+E+C">E. C. Ferrara</a>, <a href="/search/astro-ph?searchtype=author&query=Freire%2C+P+C+C">P. C. C. Freire</a>, <a href="/search/astro-ph?searchtype=author&query=Griessmeier%2C+J+-">J. -M. Griessmeier</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=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+K+-">K. -L. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabh%2C+P+V">P. V. Padmanabh</a>, <a href="/search/astro-ph?searchtype=author&query=Phosrisom%2C+A">A. Phosrisom</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">B. W. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Swihart%2C+S+J">S. J. Swihart</a>, <a href="/search/astro-ph?searchtype=author&query=Thongmeearkom%2C+T">T. Thongmeearkom</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="2401.09928v1-abstract-short" style="display: inline;"> Spider pulsars continue to provide promising candidates for neutron star mass measurements. Here we present the discovery of PSR~J1910$-$5320, a new millisecond pulsar discovered in a MeerKAT observation of an unidentified \textit{Fermi}-LAT gamma-ray source. This pulsar is coincident with a recently identified candidate redback binary, independently discovered through its periodic optical flux an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.09928v1-abstract-full').style.display = 'inline'; document.getElementById('2401.09928v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.09928v1-abstract-full" style="display: none;"> Spider pulsars continue to provide promising candidates for neutron star mass measurements. Here we present the discovery of PSR~J1910$-$5320, a new millisecond pulsar discovered in a MeerKAT observation of an unidentified \textit{Fermi}-LAT gamma-ray source. This pulsar is coincident with a recently identified candidate redback binary, independently discovered through its periodic optical flux and radial velocity. New multi-color optical light curves obtained with ULTRACAM/NTT in combination with MeerKAT timing and updated SOAR/Goodman spectroscopic radial velocity measurements allow a mass constraint for PSR~J1910$-$5320. \texttt{Icarus} optical light curve modelling, with streamlined radial velocity fitting, constrains the orbital inclination and companion velocity, unlocking the binary mass function given the precise radio ephemeris. Our modelling aims to unite the photometric and spectroscopic measurements available by fitting each simultaneously to the same underlying physical model, ensuring self-consistency. This targets centre-of-light radial velocity corrections necessitated by the irradiation endemic to spider systems. Depending on the gravity darkening prescription used, we find a moderate neutron star mass of either $1.6\pm0.2$ or $1.4\pm0.2$ $M_\odot$. The companion mass of either $0.45\pm0.04$ or $0.43^{+0.04}_{-0.03}$ $M_\odot$ also further confirms PSR~J1910$-$5320 as an irradiated redback spider pulsar.radiated redback spider pulsar. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.09928v1-abstract-full').style.display = 'none'; document.getElementById('2401.09928v1-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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 Monthly Notices of the Royal Astronomical Society. 18 pages, 9 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.09872">arXiv:2401.09872</a> <span> [<a href="https://arxiv.org/pdf/2401.09872">pdf</a>, <a href="https://arxiv.org/format/2401.09872">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="General Relativity and Quantum Cosmology">gr-qc</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/10.1126/science.adg3005">10.1126/science.adg3005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A pulsar in a binary with a compact object in the mass gap between neutron stars and black holes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">Ewan D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Dutta%2C+A">Arunima Dutta</a>, <a href="/search/astro-ph?searchtype=author&query=Freire%2C+P+C+C">Paulo C. C. Freire</a>, <a href="/search/astro-ph?searchtype=author&query=Cadelano%2C+M">Mario Cadelano</a>, <a href="/search/astro-ph?searchtype=author&query=Gautam%2C+T">Tasha Gautam</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">Michael Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Pallanca%2C+C">Cristina Pallanca</a>, <a href="/search/astro-ph?searchtype=author&query=Ransom%2C+S+M">Scott M. Ransom</a>, <a href="/search/astro-ph?searchtype=author&query=Ridolfi%2C+A">Alessandro Ridolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">Benjamin W. Stappers</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=Krishnan%2C+V+V">Vivek Venkatraman Krishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Wex%2C+N">Norbert Wex</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">Matthew Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Behrend%2C+J">Jan Behrend</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">Sarah Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">Marta Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">Weiwei Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">David J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+C+-+R">C. -H. Rosie Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Corongiu%2C+A">Alessandro Corongiu</a>, <a href="/search/astro-ph?searchtype=author&query=Geyer%2C+M">Marisa Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Men%2C+Y+P">Y. P. Men</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabh%2C+P+V">Prajwal V. Padmanabh</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">Andrea Possenti</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="2401.09872v1-abstract-short" style="display: inline;"> Among the compact objects observed in gravitational wave merger events a few have masses in the gap between the most massive neutron stars (NSs) and least massive black holes (BHs) known. Their nature and the formation of their merging binaries are not well understood. We report on pulsar timing observations using the Karoo Array Telescope (MeerKAT) of PSR J0514-4002E, an eccentric binary millisec… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.09872v1-abstract-full').style.display = 'inline'; document.getElementById('2401.09872v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.09872v1-abstract-full" style="display: none;"> Among the compact objects observed in gravitational wave merger events a few have masses in the gap between the most massive neutron stars (NSs) and least massive black holes (BHs) known. Their nature and the formation of their merging binaries are not well understood. We report on pulsar timing observations using the Karoo Array Telescope (MeerKAT) of PSR J0514-4002E, an eccentric binary millisecond pulsar in the globular cluster NGC 1851 with a total binary mass of $3.887 \pm 0.004$ solar masses. The companion to the pulsar is a compact object and its mass (between $2.09$ and $2.71$ solar masses, 95% confidence interval) is in the mass gap, so it either is a very massive NS or a low-mass BH. We propose the companion was formed by a merger between two earlier NSs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.09872v1-abstract-full').style.display = 'none'; document.getElementById('2401.09872v1-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">41 pages, 13 figures, 3 tables, to be published in Science</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.08010">arXiv:2401.08010</a> <span> [<a href="https://arxiv.org/pdf/2401.08010">pdf</a>, <a href="https://arxiv.org/format/2401.08010">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"> Long-term study of the 2020 magnetar-like outburst of the young pulsar PSRJ1846-0258 in Kes 75 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sathyaprakash%2C+R">Rajath Sathyaprakash</a>, <a href="/search/astro-ph?searchtype=author&query=Rea%2C+N">Nanda Rea</a>, <a href="/search/astro-ph?searchtype=author&query=Zelati%2C+F+C">Francesco Coti Zelati</a>, <a href="/search/astro-ph?searchtype=author&query=Borghese%2C+A">Alice Borghese</a>, <a href="/search/astro-ph?searchtype=author&query=Pilia%2C+M">Maura Pilia</a>, <a href="/search/astro-ph?searchtype=author&query=Trudu%2C+M">Matteo Trudu</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">Marta Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Turolla%2C+R">Roberto Turolla</a>, <a href="/search/astro-ph?searchtype=author&query=Zane%2C+S">Silvia Zane</a>, <a href="/search/astro-ph?searchtype=author&query=Esposito%2C+P">Paolo Esposito</a>, <a href="/search/astro-ph?searchtype=author&query=Mereghetti%2C+S">Sandro Mereghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Campana%2C+S">Sergio Campana</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B6tz%2C+D">Diego G枚tz</a>, <a href="/search/astro-ph?searchtype=author&query=Ibrahim%2C+A">Abubakr Ibrahim</a>, <a href="/search/astro-ph?searchtype=author&query=Israel%2C+G">GianLuca Israel</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">Andrea Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Tiengo%2C+A">Andrea Tiengo</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="2401.08010v2-abstract-short" style="display: inline;"> Magnetar-like activity has been observed in a large variety of neutron stars. PSR J1846-0258 is a young 327 ms radio-quiet pulsar with a large rotational power ($\sim 8 \times 10^{36}$ erg s$^{-1}$), and resides at the center of the supernova remnant Kes 75. It is one of the rare examples of a high magnetic field pulsar showing characteristics both of magnetars and radio pulsars, and can thus prov… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.08010v2-abstract-full').style.display = 'inline'; document.getElementById('2401.08010v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.08010v2-abstract-full" style="display: none;"> Magnetar-like activity has been observed in a large variety of neutron stars. PSR J1846-0258 is a young 327 ms radio-quiet pulsar with a large rotational power ($\sim 8 \times 10^{36}$ erg s$^{-1}$), and resides at the center of the supernova remnant Kes 75. It is one of the rare examples of a high magnetic field pulsar showing characteristics both of magnetars and radio pulsars, and can thus provide important clues on the differences in the emission mechanisms between these two classes. In 2006, PSR J1846-0258 was detected to undergo an outburst for the first time, accompanied by a large flux increase, millisecond X-ray bursts, significant spectral changes and a large timing glitch. In the period between May-June 2020, after fourteen years of quiescent stable emission, the source underwent a second magnetar-like outburst, which was followed up with several observations by NICER, XMM-Newton, NuSTAR and Swift. In this work, we report on the long-term timing and X-ray spectral properties of the source following the 2020 outburst, and place upper limits on any source activity at radio wavelengths. We demonstrate that the pulsed flux increased by a factor $> 6$ during the outburst, followed by non-trivial variability in the spin-down rate. Our timing analysis shows that the spin frequency and its derivative are clearly affected by magnetospheric activity due to the outburst. We find hints for an oscillation in the frequency derivative with a timescale of 50-60 days, recovering later on to stable quiescence. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.08010v2-abstract-full').style.display = 'none'; document.getElementById('2401.08010v2-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 10 figures; accepted for publication by ApJ; comments are welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.14008">arXiv:2310.14008</a> <span> [<a href="https://arxiv.org/pdf/2310.14008">pdf</a>, <a href="https://arxiv.org/format/2310.14008">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/stad3283">10.1093/mnras/stad3283 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The High Time Resolution Universe Pulsar Survey -- XVIII. The reprocessing of the HTRU-S Low Lat survey around the Galactic centre using a Fast Folding Algorithm pipeline for accelerated pulsars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wongphechauxsorn%2C+J">J. Wongphechauxsorn</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Balakrishnan%2C+V">V. Balakrishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Bernadich%2C+M+C+i">M. C. i Bernadich</a>, <a href="/search/astro-ph?searchtype=author&query=Bhat%2C+N+D+R">N. D. R. Bhat</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+A+D">A. D. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">W. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Flynn%2C+C+M+L">C. M. L. Flynn</a>, <a href="/search/astro-ph?searchtype=author&query=Jameson%2C+A">A. Jameson</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+S">S. Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Keith%2C+M+J">M. J. Keith</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Ng%2C+C">C. Ng</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Sengar%2C+R">R. Sengar</a>, <a href="/search/astro-ph?searchtype=author&query=Shannon%2C+R+M">R. M. Shannon</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B">B. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=van+Straten%2C+W">W. van Straten</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="2310.14008v1-abstract-short" style="display: inline;"> The HTRU-S Low Latitude survey data within 1$^{\circ}$of the Galactic Centre (GC) were searched for pulsars using the Fast Folding Algorithm (FFA). Unlike traditional Fast Fourier Transform (FFT) pipelines, the FFA optimally folds the data for all possible periods over a given range, which is particularly advantageous for pulsars with low-duty cycle. For the first time, a search over acceleration… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.14008v1-abstract-full').style.display = 'inline'; document.getElementById('2310.14008v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.14008v1-abstract-full" style="display: none;"> The HTRU-S Low Latitude survey data within 1$^{\circ}$of the Galactic Centre (GC) were searched for pulsars using the Fast Folding Algorithm (FFA). Unlike traditional Fast Fourier Transform (FFT) pipelines, the FFA optimally folds the data for all possible periods over a given range, which is particularly advantageous for pulsars with low-duty cycle. For the first time, a search over acceleration was included in the FFA to improve its sensitivity to binary pulsars. The steps in dispersion measure (DM) and acceleration were optimised, resulting in a reduction of the number of trials by 86 per cent. This was achieved over a search period range from 0.6-s to 432-s, i.e. 10 per cent of the observation time (4320s), with a maximum DM of 4000 pc cm$^{-3}$ and an acceleration range of $\pm 128$m s$^{-2}$. The search resulted in the re-detections of four known pulsars, including a pulsar which was missed in previous FFT processing of this survey. This result indicates that the FFA pipeline is more sensitive than the FFT pipeline used in the previous processing of the survey within our parameter range. Additionally, we discovered a 1.89-s pulsar, PSR J1746-2829, with a large DM, located~0.5 from the GC. Follow-up observations revealed that this pulsar has a relatively flat spectrum($伪=-0.9\pm0.1$) and has a period derivative of $\sim1.3\times10^{-12}$ s s$^{-1}$, implying a surface magnetic field of $\sim5.2\times10^{13}$ G and a characteristic age of $\sim23000$ yr. While the period, spectral index, and surface magnetic field strength are similar to many radio magnetars, other characteristics such as high linear polarization are absent. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.14008v1-abstract-full').style.display = 'none'; document.getElementById('2310.14008v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">12 pages, 6 figures, 4 tables, Accepted for publication on 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/2309.16067">arXiv:2309.16067</a> <span> [<a href="https://arxiv.org/pdf/2309.16067">pdf</a>, <a href="https://arxiv.org/format/2309.16067">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"> The Polarized Cosmic Hand: IXPE Observations of PSR B1509-58/MSH 15-52 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Romani%2C+R+W">Roger W. Romani</a>, <a href="/search/astro-ph?searchtype=author&query=Wong%2C+J">Josephine Wong</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Lalla%2C+N">Niccolo Di Lalla</a>, <a href="/search/astro-ph?searchtype=author&query=Omodei%2C+N">Nicola Omodei</a>, <a href="/search/astro-ph?searchtype=author&query=Xie%2C+F">Fei Xie</a>, <a href="/search/astro-ph?searchtype=author&query=Ng%2C+C+-">C. -Y. Ng</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrazzoli%2C+R">Riccardo Ferrazzoli</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Marco%2C+A">Alessandro Di Marco</a>, <a href="/search/astro-ph?searchtype=author&query=Bucciantini%2C+N">Niccolo Bucciantini</a>, <a href="/search/astro-ph?searchtype=author&query=Pilia%2C+M">Maura Pilia</a>, <a href="/search/astro-ph?searchtype=author&query=Slane%2C+P">Patrick Slane</a>, <a href="/search/astro-ph?searchtype=author&query=Weisskopf%2C+M+C">Martin C. Weisskopf</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+S">Simon Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">Marta Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Wei%2C+D">Deng Wei</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+Y">Yi-Jung Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+S">Shumeng Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">Lucio A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bachetti%2C+M">Matteo Bachetti</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+L">Luca Baldini</a>, <a href="/search/astro-ph?searchtype=author&query=Baumgartner%2C+W+H">Wayne H. Baumgartner</a>, <a href="/search/astro-ph?searchtype=author&query=Bellazzini%2C+R">Ronaldo Bellazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">Stefano Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+S+D">Stephen D. Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Bonino%2C+R">Raffaella Bonino</a> , et al. (78 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="2309.16067v1-abstract-short" style="display: inline;"> We describe IXPE polarization observations of the Pulsar Wind Nebula (PWN) MSH15-52, the `Cosmic Hand'. We find X-ray polarization across the PWN, with B field vectors generally aligned with filamentary X-ray structures. High significance polarization is seen in arcs surrounding the pulsar and toward the end of the `jet', with polarization degree PD>70%, thus approaching the maximum allowed synchr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.16067v1-abstract-full').style.display = 'inline'; document.getElementById('2309.16067v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.16067v1-abstract-full" style="display: none;"> We describe IXPE polarization observations of the Pulsar Wind Nebula (PWN) MSH15-52, the `Cosmic Hand'. We find X-ray polarization across the PWN, with B field vectors generally aligned with filamentary X-ray structures. High significance polarization is seen in arcs surrounding the pulsar and toward the end of the `jet', with polarization degree PD>70%, thus approaching the maximum allowed synchrotron value. In contrast, the base of the jet has lower polarization, indicating a complex magnetic field at significant angle to the jet axis. We also detect significant polarization from PSR B1509-58 itself. Although only the central pulse-phase bin of the pulse has high individual significance, flanking bins provide lower significance detections and, in conjunction with the X-ray image and radio polarization, can be used to constrain rotating vector model solutions for the pulsar geometry. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.16067v1-abstract-full').style.display = 'none'; document.getElementById('2309.16067v1-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 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">To appear in the Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.00693">arXiv:2309.00693</a> <span> [<a href="https://arxiv.org/pdf/2309.00693">pdf</a>, <a href="https://arxiv.org/format/2309.00693">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="General Relativity and Quantum Cosmology">gr-qc</span> </div> </div> <p class="title is-5 mathjax"> Comparing recent PTA results on the nanohertz stochastic gravitational wave background </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+International+Pulsar+Timing+Array+Collaboration"> The International Pulsar Timing Array Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Agazie%2C+G">G. Agazie</a>, <a href="/search/astro-ph?searchtype=author&query=Antoniadis%2C+J">J. Antoniadis</a>, <a href="/search/astro-ph?searchtype=author&query=Anumarlapudi%2C+A">A. Anumarlapudi</a>, <a href="/search/astro-ph?searchtype=author&query=Archibald%2C+A+M">A. M. Archibald</a>, <a href="/search/astro-ph?searchtype=author&query=Arumugam%2C+P">P. Arumugam</a>, <a href="/search/astro-ph?searchtype=author&query=Arumugam%2C+S">S. Arumugam</a>, <a href="/search/astro-ph?searchtype=author&query=Arzoumanian%2C+Z">Z. Arzoumanian</a>, <a href="/search/astro-ph?searchtype=author&query=Askew%2C+J">J. Askew</a>, <a href="/search/astro-ph?searchtype=author&query=Babak%2C+S">S. Babak</a>, <a href="/search/astro-ph?searchtype=author&query=Bagchi%2C+M">M. Bagchi</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Nielsen%2C+A+-+B">A. -S. Bak Nielsen</a>, <a href="/search/astro-ph?searchtype=author&query=Baker%2C+P+T">P. T. Baker</a>, <a href="/search/astro-ph?searchtype=author&query=Bassa%2C+C+G">C. G. Bassa</a>, <a href="/search/astro-ph?searchtype=author&query=Bathula%2C+A">A. Bathula</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%A9csy%2C+B">B. B茅csy</a>, <a href="/search/astro-ph?searchtype=author&query=Berthereau%2C+A">A. Berthereau</a>, <a href="/search/astro-ph?searchtype=author&query=Bhat%2C+N+D+R">N. D. R. Bhat</a>, <a href="/search/astro-ph?searchtype=author&query=Blecha%2C+L">L. Blecha</a>, <a href="/search/astro-ph?searchtype=author&query=Bonetti%2C+M">M. Bonetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bortolas%2C+E">E. Bortolas</a>, <a href="/search/astro-ph?searchtype=author&query=Brazier%2C+A">A. Brazier</a>, <a href="/search/astro-ph?searchtype=author&query=Brook%2C+P+R">P. R. Brook</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a> , et al. (220 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="2309.00693v1-abstract-short" style="display: inline;"> The Australian, Chinese, European, Indian, and North American pulsar timing array (PTA) collaborations recently reported, at varying levels, evidence for the presence of a nanohertz gravitational wave background (GWB). Given that each PTA made different choices in modeling their data, we perform a comparison of the GWB and individual pulsar noise parameters across the results reported from the PTA… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.00693v1-abstract-full').style.display = 'inline'; document.getElementById('2309.00693v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.00693v1-abstract-full" style="display: none;"> The Australian, Chinese, European, Indian, and North American pulsar timing array (PTA) collaborations recently reported, at varying levels, evidence for the presence of a nanohertz gravitational wave background (GWB). Given that each PTA made different choices in modeling their data, we perform a comparison of the GWB and individual pulsar noise parameters across the results reported from the PTAs that constitute the International Pulsar Timing Array (IPTA). We show that despite making different modeling choices, there is no significant difference in the GWB parameters that are measured by the different PTAs, agreeing within $1蟽$. The pulsar noise parameters are also consistent between different PTAs for the majority of the pulsars included in these analyses. We bridge the differences in modeling choices by adopting a standardized noise model for all pulsars and PTAs, finding that under this model there is a reduction in the tension in the pulsar noise parameters. As part of this reanalysis, we "extended" each PTA's data set by adding extra pulsars that were not timed by that PTA. Under these extensions, we find better constraints on the GWB amplitude and a higher signal-to-noise ratio for the Hellings and Downs correlations. These extensions serve as a prelude to the benefits offered by a full combination of data across all pulsars in the IPTA, i.e., the IPTA's Data Release 3, which will involve not just adding in additional pulsars, but also including data from all three PTAs where any given pulsar is timed by more than as single PTA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.00693v1-abstract-full').style.display = 'none'; document.getElementById('2309.00693v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 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">21 pages, 9 figures, submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.16802">arXiv:2308.16802</a> <span> [<a href="https://arxiv.org/pdf/2308.16802">pdf</a>, <a href="https://arxiv.org/format/2308.16802">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/10.1051/0004-6361/202346953">10.1051/0004-6361/202346953 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MPIfR-MeerKAT Galactic Plane Survey II. The eccentric double neutron star system PSR J1208-5936 and a neutron star merger rate update </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bernadich%2C+M+C+i">M. Colom i Bernadich</a>, <a href="/search/astro-ph?searchtype=author&query=Balakrishnan%2C+V">V. Balakrishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E">E. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Berezina%2C+M">M. Berezina</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">W. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Desvignes%2C+G">G. Desvignes</a>, <a href="/search/astro-ph?searchtype=author&query=Freire%2C+P+C+C">P. C. C. Freire</a>, <a href="/search/astro-ph?searchtype=author&query=Grunthal%2C+K">K. Grunthal</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Men%2C+Y">Y. Men</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabh%2C+P+V">P. V. Padmanabh</a>, <a href="/search/astro-ph?searchtype=author&query=Parthasarathy%2C+A">A. Parthasarathy</a>, <a href="/search/astro-ph?searchtype=author&query=Pillay%2C+D">D. Pillay</a>, <a href="/search/astro-ph?searchtype=author&query=Rammala%2C+I">I. Rammala</a>, <a href="/search/astro-ph?searchtype=author&query=Sengupta%2C+S">S. Sengupta</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">V. Venkatraman Krishnan</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="2308.16802v2-abstract-short" style="display: inline;"> The MMGPS-L is the most sensitive pulsar survey in the Southern Hemisphere. We present a follow-up study of one of these new discoveries, PSR J1208-5936, a 28.71-ms recycled pulsar in a double neutron star system with an orbital period of Pb=0.632 days and an eccentricity of e=0.348. Through timing of almost one year of observations, we detected the relativistic advance of periastron (0.918(1) deg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.16802v2-abstract-full').style.display = 'inline'; document.getElementById('2308.16802v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.16802v2-abstract-full" style="display: none;"> The MMGPS-L is the most sensitive pulsar survey in the Southern Hemisphere. We present a follow-up study of one of these new discoveries, PSR J1208-5936, a 28.71-ms recycled pulsar in a double neutron star system with an orbital period of Pb=0.632 days and an eccentricity of e=0.348. Through timing of almost one year of observations, we detected the relativistic advance of periastron (0.918(1) deg/yr), resulting in a total system mass of Mt=2.586(5) Mo. We also achieved low-significance constraints on the amplitude of the Einstein delay and Shapiro delay, in turn yielding constraints on the pulsar mass (Mp=1.26(+0.13/-0.25) Mo), the companion mass (Mc=1.32(+0.25/-0.13) Mo, and the inclination angle (i=57(12) degrees). This system is highly eccentric compared to other Galactic field double neutron stars with similar periods, possibly hinting at a larger-than-usual supernova kick during the formation of the second-born neutron star. The binary will merge within 7.2(2) Gyr due to the emission of gravitational waves. With the improved sensitivity of the MMGPS-L, we updated the Milky Way neutron star merger rate to be 25(+19/-9) Myr$^{-1}$ within 90% credible intervals, which is lower than previous studies based on known Galactic binaries owing to the lack of further detections despite the highly sensitive nature of the survey. This implies a local cosmic neutron star merger rate of 293(+222/-103} Gpc/yr, consistent with LIGO and Virgo O3 observations. With this, we predict the observation of 10(+8/-4) neutron star merger events during the LIGO-Virgo-KAGRA O4 run. We predict the uncertainties on the component masses and the inclination angle will be reduced to 5x10$^{-3}$ Mo and 0.4 degrees after two decades of timing, and that in at least a decade from now the detection of the shift in Pb and the sky proper motion will serve to make an independent constraint of the distance to the system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.16802v2-abstract-full').style.display = 'none'; document.getElementById('2308.16802v2-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 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 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">Journal ref:</span> A&A 678, A187 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.11132">arXiv:2307.11132</a> <span> [<a href="https://arxiv.org/pdf/2307.11132">pdf</a>, <a href="https://arxiv.org/format/2307.11132">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/acee67">10.3847/1538-4357/acee67 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Third Fermi Large Area Telescope Catalog of Gamma-ray Pulsars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Smith%2C+D+A">David A. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Bruel%2C+P">Philippe Bruel</a>, <a href="/search/astro-ph?searchtype=author&query=Clark%2C+C+J">Colin J. Clark</a>, <a href="/search/astro-ph?searchtype=author&query=Guillemot%2C+L">Lucas Guillemot</a>, <a href="/search/astro-ph?searchtype=author&query=Kerr%2C+M+T">Matthew T. Kerr</a>, <a href="/search/astro-ph?searchtype=author&query=Ray%2C+P">Paul Ray</a>, <a href="/search/astro-ph?searchtype=author&query=Abdollahi%2C+S">Soheila Abdollahi</a>, <a href="/search/astro-ph?searchtype=author&query=Ajello%2C+M">Marco Ajello</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+L">Luca Baldini</a>, <a href="/search/astro-ph?searchtype=author&query=Ballet%2C+J">Jean Ballet</a>, <a href="/search/astro-ph?searchtype=author&query=Baring%2C+M">Matthew Baring</a>, <a href="/search/astro-ph?searchtype=author&query=Bassa%2C+C">Cees Bassa</a>, <a href="/search/astro-ph?searchtype=author&query=Gonzalez%2C+J+B">Josefa Becerra Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=Bellazzini%2C+R">Ronaldo Bellazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Berretta%2C+A">Alessandra Berretta</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharyya%2C+B">Bhaswati Bhattacharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Bissaldi%2C+E">Elisabetta Bissaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bonino%2C+R">Raffaella Bonino</a>, <a href="/search/astro-ph?searchtype=author&query=Bottacini%2C+E">Eugenio Bottacini</a>, <a href="/search/astro-ph?searchtype=author&query=Bregeon%2C+J">Johan Bregeon</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">Marta Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Burnett%2C+T">Toby Burnett</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+R">Rob Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">Fernando Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Caputo%2C+R">Regina Caputo</a> , et al. (134 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="2307.11132v1-abstract-short" style="display: inline;"> We present 294 pulsars found in GeV data from the Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope. Another 33 millisecond pulsars (MSPs) discovered in deep radio searches of LAT sources will likely reveal pulsations once phase-connected rotation ephemerides are achieved. A further dozen optical and/or X-ray binary systems co-located with LAT sources also likely harbor gamma-ray M… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.11132v1-abstract-full').style.display = 'inline'; document.getElementById('2307.11132v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.11132v1-abstract-full" style="display: none;"> We present 294 pulsars found in GeV data from the Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope. Another 33 millisecond pulsars (MSPs) discovered in deep radio searches of LAT sources will likely reveal pulsations once phase-connected rotation ephemerides are achieved. A further dozen optical and/or X-ray binary systems co-located with LAT sources also likely harbor gamma-ray MSPs. This catalog thus reports roughly 340 gamma-ray pulsars and candidates, 10% of all known pulsars, compared to $\leq 11$ known before Fermi. Half of the gamma-ray pulsars are young. Of these, the half that are undetected in radio have a broader Galactic latitude distribution than the young radio-loud pulsars. The others are MSPs, with 6 undetected in radio. Overall, >235 are bright enough above 50 MeV to fit the pulse profile, the energy spectrum, or both. For the common two-peaked profiles, the gamma-ray peak closest to the magnetic pole crossing generally has a softer spectrum. The spectral energy distributions tend to narrow as the spindown power $\dot E$ decreases to its observed minimum near $10^{33}$ erg s$^{-1}$, approaching the shape for synchrotron radiation from monoenergetic electrons. We calculate gamma-ray luminosities when distances are available. Our all-sky gamma-ray sensitivity map is useful for population syntheses. The electronic catalog version provides gamma-ray pulsar ephemerides, properties and fit results to guide and be compared with modeling results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.11132v1-abstract-full').style.display = 'none'; document.getElementById('2307.11132v1-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 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">142 pages. Accepted by the Astrophysical Journal Supplement</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.16228">arXiv:2306.16228</a> <span> [<a href="https://arxiv.org/pdf/2306.16228">pdf</a>, <a href="https://arxiv.org/format/2306.16228">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> <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="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.131.171001">10.1103/PhysRevLett.131.171001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The second data release from the European Pulsar Timing Array: VI. Challenging the ultralight dark matter paradigm </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Smarra%2C+C">Clemente Smarra</a>, <a href="/search/astro-ph?searchtype=author&query=Goncharov%2C+B">Boris Goncharov</a>, <a href="/search/astro-ph?searchtype=author&query=Barausse%2C+E">Enrico Barausse</a>, <a href="/search/astro-ph?searchtype=author&query=Antoniadis%2C+J">J. Antoniadis</a>, <a href="/search/astro-ph?searchtype=author&query=Babak%2C+S">S. Babak</a>, <a href="/search/astro-ph?searchtype=author&query=Nielsen%2C+A+-+B">A. -S. Bak Nielsen</a>, <a href="/search/astro-ph?searchtype=author&query=Bassa%2C+C+G">C. G. Bassa</a>, <a href="/search/astro-ph?searchtype=author&query=Berthereau%2C+A">A. Berthereau</a>, <a href="/search/astro-ph?searchtype=author&query=Bonetti%2C+M">M. Bonetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bortolas%2C+E">E. Bortolas</a>, <a href="/search/astro-ph?searchtype=author&query=Brook%2C+P+R">P. R. Brook</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Caballero%2C+R+N">R. N. Caballero</a>, <a href="/search/astro-ph?searchtype=author&query=Chalumeau%2C+A">A. Chalumeau</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Chanlaridis%2C+S">S. Chanlaridis</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cognard%2C+I">I. Cognard</a>, <a href="/search/astro-ph?searchtype=author&query=Desvignes%2C+G">G. Desvignes</a>, <a href="/search/astro-ph?searchtype=author&query=Falxa%2C+M">M. Falxa</a>, <a href="/search/astro-ph?searchtype=author&query=Ferdman%2C+R+D">R. D. Ferdman</a>, <a href="/search/astro-ph?searchtype=author&query=Franchini%2C+A">A. Franchini</a>, <a href="/search/astro-ph?searchtype=author&query=Gair%2C+J+R">J. R. Gair</a>, <a href="/search/astro-ph?searchtype=author&query=Graikou%2C+E">E. Graikou</a>, <a href="/search/astro-ph?searchtype=author&query=Grie%2C+J+-">J. -M. Grie</a> , et al. (46 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="2306.16228v2-abstract-short" style="display: inline;"> Pulsar Timing Array experiments probe the presence of possible scalar or pseudoscalar ultralight dark matter particles through decade-long timing of an ensemble of galactic millisecond radio pulsars. With the second data release of the European Pulsar Timing Array, we focus on the most robust scenario, in which dark matter interacts only gravitationally with ordinary baryonic matter. Our results s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.16228v2-abstract-full').style.display = 'inline'; document.getElementById('2306.16228v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.16228v2-abstract-full" style="display: none;"> Pulsar Timing Array experiments probe the presence of possible scalar or pseudoscalar ultralight dark matter particles through decade-long timing of an ensemble of galactic millisecond radio pulsars. With the second data release of the European Pulsar Timing Array, we focus on the most robust scenario, in which dark matter interacts only gravitationally with ordinary baryonic matter. Our results show that ultralight particles with masses $10^{-24.0}~\text{eV} \lesssim m \lesssim 10^{-23.3}~\text{eV}$ cannot constitute $100\%$ of the measured local dark matter density, but can have at most local density $蟻\lesssim 0.3$ GeV/cm$^3$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.16228v2-abstract-full').style.display = 'none'; document.getElementById('2306.16228v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">5 pages + acknowledgements + refs, 2 figures. Text and figures match the version published in PRL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.16227">arXiv:2306.16227</a> <span> [<a href="https://arxiv.org/pdf/2306.16227">pdf</a>, <a href="https://arxiv.org/format/2306.16227">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <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="General Relativity and Quantum Cosmology">gr-qc</span> </div> </div> <p class="title is-5 mathjax"> The second data release from the European Pulsar Timing Array: IV. Implications for massive black holes, dark matter and the early Universe </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Antoniadis%2C+J">J. Antoniadis</a>, <a href="/search/astro-ph?searchtype=author&query=Arumugam%2C+P">P. Arumugam</a>, <a href="/search/astro-ph?searchtype=author&query=Arumugam%2C+S">S. Arumugam</a>, <a href="/search/astro-ph?searchtype=author&query=Auclair%2C+P">P. Auclair</a>, <a href="/search/astro-ph?searchtype=author&query=Babak%2C+S">S. Babak</a>, <a href="/search/astro-ph?searchtype=author&query=Bagchi%2C+M">M. Bagchi</a>, <a href="/search/astro-ph?searchtype=author&query=Nielsen%2C+A+-+B">A. -S. Bak Nielsen</a>, <a href="/search/astro-ph?searchtype=author&query=Barausse%2C+E">E. Barausse</a>, <a href="/search/astro-ph?searchtype=author&query=Bassa%2C+C+G">C. G. Bassa</a>, <a href="/search/astro-ph?searchtype=author&query=Bathula%2C+A">A. Bathula</a>, <a href="/search/astro-ph?searchtype=author&query=Berthereau%2C+A">A. Berthereau</a>, <a href="/search/astro-ph?searchtype=author&query=Bonetti%2C+M">M. Bonetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bortolas%2C+E">E. Bortolas</a>, <a href="/search/astro-ph?searchtype=author&query=Brook%2C+P+R">P. R. Brook</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Caballero%2C+R+N">R. N. Caballero</a>, <a href="/search/astro-ph?searchtype=author&query=Caprini%2C+C">C. Caprini</a>, <a href="/search/astro-ph?searchtype=author&query=Chalumeau%2C+A">A. Chalumeau</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Chanlaridis%2C+S">S. Chanlaridis</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cognard%2C+I">I. Cognard</a>, <a href="/search/astro-ph?searchtype=author&query=Crisostomi%2C+M">M. Crisostomi</a>, <a href="/search/astro-ph?searchtype=author&query=Dandapat%2C+S">S. Dandapat</a>, <a href="/search/astro-ph?searchtype=author&query=Deb%2C+D">D. Deb</a> , et al. (89 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="2306.16227v2-abstract-short" style="display: inline;"> The European Pulsar Timing Array (EPTA) and Indian Pulsar Timing Array (InPTA) collaborations have measured a low-frequency common signal in the combination of their second and first data releases respectively, with the correlation properties of a gravitational wave background (GWB). Such signal may have its origin in a number of physical processes including a cosmic population of inspiralling sup… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.16227v2-abstract-full').style.display = 'inline'; document.getElementById('2306.16227v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.16227v2-abstract-full" style="display: none;"> The European Pulsar Timing Array (EPTA) and Indian Pulsar Timing Array (InPTA) collaborations have measured a low-frequency common signal in the combination of their second and first data releases respectively, with the correlation properties of a gravitational wave background (GWB). Such signal may have its origin in a number of physical processes including a cosmic population of inspiralling supermassive black hole binaries (SMBHBs); inflation, phase transitions, cosmic strings and tensor mode generation by non-linear evolution of scalar perturbations in the early Universe; oscillations of the Galactic potential in the presence of ultra-light dark matter (ULDM). At the current stage of emerging evidence, it is impossible to discriminate among the different origins. Therefore, in this paper, we consider each process separately, and investigate the implications of the signal under the hypothesis that it is generated by that specific process. We find that the signal is consistent with a cosmic population of inspiralling SMBHBs, and its relatively high amplitude can be used to place constraints on binary merger timescales and the SMBH-host galaxy scaling relations. If this origin is confirmed, this is the first direct evidence that SMBHBs merge in nature, adding an important observational piece to the puzzle of structure formation and galaxy evolution. As for early Universe processes, the measurement would place tight constraints on the cosmic string tension and on the level of turbulence developed by first-order phase transitions. Other processes would require non-standard scenarios, such as a blue-tilted inflationary spectrum or an excess in the primordial spectrum of scalar perturbations at large wavenumbers. Finally, a ULDM origin of the detected signal is disfavoured, which leads to direct constraints on the abundance of ULDM in our Galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.16227v2-abstract-full').style.display = 'none'; document.getElementById('2306.16227v2-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">30 pages, 23 figures, replaced to match the version published in Astronomy & Astrophysics, note the change in the numbering order in the series (now paper IV)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.16226">arXiv:2306.16226</a> <span> [<a href="https://arxiv.org/pdf/2306.16226">pdf</a>, <a href="https://arxiv.org/format/2306.16226">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> <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="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/10.1051/0004-6361/202348568">10.1051/0004-6361/202348568 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The second data release from the European Pulsar Timing Array V. Search for continuous gravitational wave signals </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Antoniadis%2C+J">J. Antoniadis</a>, <a href="/search/astro-ph?searchtype=author&query=Arumugam%2C+P">P. Arumugam</a>, <a href="/search/astro-ph?searchtype=author&query=Arumugam%2C+S">S. Arumugam</a>, <a href="/search/astro-ph?searchtype=author&query=Babak%2C+S">S. Babak</a>, <a href="/search/astro-ph?searchtype=author&query=Bagchi%2C+M">M. Bagchi</a>, <a href="/search/astro-ph?searchtype=author&query=Nielsen%2C+A+S+B">A. S. Bak Nielsen</a>, <a href="/search/astro-ph?searchtype=author&query=Bassa%2C+C+G">C. G. Bassa</a>, <a href="/search/astro-ph?searchtype=author&query=Bathula%2C+A">A. Bathula</a>, <a href="/search/astro-ph?searchtype=author&query=Berthereau%2C+A">A. Berthereau</a>, <a href="/search/astro-ph?searchtype=author&query=Bonetti%2C+M">M. Bonetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bortolas%2C+E">E. Bortolas</a>, <a href="/search/astro-ph?searchtype=author&query=Brook%2C+P+R">P. R. Brook</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Caballero%2C+R+N">R. N. Caballero</a>, <a href="/search/astro-ph?searchtype=author&query=Chalumeau%2C+A">A. Chalumeau</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Chanlaridis%2C+S">S. Chanlaridis</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cognard%2C+I">I. Cognard</a>, <a href="/search/astro-ph?searchtype=author&query=Dandapat%2C+S">S. Dandapat</a>, <a href="/search/astro-ph?searchtype=author&query=Deb%2C+D">D. Deb</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">S. Desai</a>, <a href="/search/astro-ph?searchtype=author&query=Desvignes%2C+G">G. Desvignes</a>, <a href="/search/astro-ph?searchtype=author&query=Dhanda-Batra%2C+N">N. Dhanda-Batra</a>, <a href="/search/astro-ph?searchtype=author&query=Dwivedi%2C+C">C. Dwivedi</a> , et al. (75 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="2306.16226v3-abstract-short" style="display: inline;"> We present the results of a search for continuous gravitational wave signals (CGWs) in the second data release (DR2) of the European Pulsar Timing Array (EPTA) collaboration. The most significant candidate event from this search has a gravitational wave frequency of 4-5 nHz. Such a signal could be generated by a supermassive black hole binary (SMBHB) in the local Universe. We present the results o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.16226v3-abstract-full').style.display = 'inline'; document.getElementById('2306.16226v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.16226v3-abstract-full" style="display: none;"> We present the results of a search for continuous gravitational wave signals (CGWs) in the second data release (DR2) of the European Pulsar Timing Array (EPTA) collaboration. The most significant candidate event from this search has a gravitational wave frequency of 4-5 nHz. Such a signal could be generated by a supermassive black hole binary (SMBHB) in the local Universe. We present the results of a follow-up analysis of this candidate using both Bayesian and frequentist methods. The Bayesian analysis gives a Bayes factor of 4 in favor of the presence of the CGW over a common uncorrelated noise process, while the frequentist analysis estimates the p-value of the candidate to be 1%, also assuming the presence of common uncorrelated red noise. However, comparing a model that includes both a CGW and a gravitational wave background (GWB) to a GWB only, the Bayes factor in favour of the CGW model is only 0.7. Therefore, we cannot conclusively determine the origin of the observed feature, but we cannot rule it out as a CGW source. We present results of simulations that demonstrate that data containing a weak gravitational wave background can be misinterpreted as data including a CGW and vice versa, providing two plausible explanations of the EPTA DR2 data. Further investigations combining data from all PTA collaborations will be needed to reveal the true origin of this feature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.16226v3-abstract-full').style.display = 'none'; document.getElementById('2306.16226v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">13 figures, 15 pages, accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A118 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.16225">arXiv:2306.16225</a> <span> [<a href="https://arxiv.org/pdf/2306.16225">pdf</a>, <a href="https://arxiv.org/format/2306.16225">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/10.1051/0004-6361/202346842">10.1051/0004-6361/202346842 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The second data release from the European Pulsar Timing Array II. Customised pulsar noise models for spatially correlated gravitational waves </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Antoniadis%2C+J">J. Antoniadis</a>, <a href="/search/astro-ph?searchtype=author&query=Arumugam%2C+P">P. Arumugam</a>, <a href="/search/astro-ph?searchtype=author&query=Arumugam%2C+S">S. Arumugam</a>, <a href="/search/astro-ph?searchtype=author&query=Babak%2C+S">S. Babak</a>, <a href="/search/astro-ph?searchtype=author&query=Bagchi%2C+M">M. Bagchi</a>, <a href="/search/astro-ph?searchtype=author&query=Nielsen%2C+A+S+B">A. S. Bak Nielsen</a>, <a href="/search/astro-ph?searchtype=author&query=Bassa%2C+C+G">C. G. Bassa</a>, <a href="/search/astro-ph?searchtype=author&query=Bathula%2C+A">A. Bathula</a>, <a href="/search/astro-ph?searchtype=author&query=Berthereau%2C+A">A. Berthereau</a>, <a href="/search/astro-ph?searchtype=author&query=Bonetti%2C+M">M. Bonetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bortolas%2C+E">E. Bortolas</a>, <a href="/search/astro-ph?searchtype=author&query=Brook%2C+P+R">P. R. Brook</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Caballero%2C+R+N">R. N. Caballero</a>, <a href="/search/astro-ph?searchtype=author&query=Chalumeau%2C+A">A. Chalumeau</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Chanlaridis%2C+S">S. Chanlaridis</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cognard%2C+I">I. Cognard</a>, <a href="/search/astro-ph?searchtype=author&query=Dandapat%2C+S">S. Dandapat</a>, <a href="/search/astro-ph?searchtype=author&query=Deb%2C+D">D. Deb</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">S. Desai</a>, <a href="/search/astro-ph?searchtype=author&query=Desvignes%2C+G">G. Desvignes</a>, <a href="/search/astro-ph?searchtype=author&query=Dhanda-Batra%2C+N">N. Dhanda-Batra</a>, <a href="/search/astro-ph?searchtype=author&query=Dwivedi%2C+C">C. Dwivedi</a> , et al. (73 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="2306.16225v1-abstract-short" style="display: inline;"> The nanohertz gravitational wave background (GWB) is expected to be an aggregate signal of an ensemble of gravitational waves emitted predominantly by a large population of coalescing supermassive black hole binaries in the centres of merging galaxies. Pulsar timing arrays, ensembles of extremely stable pulsars, are the most precise experiments capable of detecting this background. However, the su… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.16225v1-abstract-full').style.display = 'inline'; document.getElementById('2306.16225v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.16225v1-abstract-full" style="display: none;"> The nanohertz gravitational wave background (GWB) is expected to be an aggregate signal of an ensemble of gravitational waves emitted predominantly by a large population of coalescing supermassive black hole binaries in the centres of merging galaxies. Pulsar timing arrays, ensembles of extremely stable pulsars, are the most precise experiments capable of detecting this background. However, the subtle imprints that the GWB induces on pulsar timing data are obscured by many sources of noise. These must be carefully characterized to increase the sensitivity to the GWB. In this paper, we present a novel technique to estimate the optimal number of frequency coefficients for modelling achromatic and chromatic noise and perform model selection. We also incorporate a new model to fit for scattering variations in the pulsar timing package temponest and created realistic simulations of the European Pulsar Timing Array (EPTA) datasets that allowed us to test the efficacy of our noise modelling algorithms. We present an in-depth analysis of the noise properties of 25 millisecond pulsars (MSPs) that form the second data release (DR2) of the EPTA and investigate the effect of incorporating low-frequency data from the Indian PTA collaboration. We use enterprise and temponest packages to compare noise models with those reported with the EPTA DR1. We find that, while in some pulsars we can successfully disentangle chromatic from achromatic noise owing to the wider frequency coverage in DR2, in others the noise models evolve in a more complicated way. We also find evidence of long-term scattering variations in PSR J1600$-$3053. Through our simulations, we identify intrinsic biases in our current noise analysis techniques and discuss their effect on GWB searches. The results presented here directly help improve sensitivity to the GWB and are already being used as part of global PTA efforts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.16225v1-abstract-full').style.display = 'none'; document.getElementById('2306.16225v1-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 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 6 figures, 9 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 678, A49 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.16224">arXiv:2306.16224</a> <span> [<a href="https://arxiv.org/pdf/2306.16224">pdf</a>, <a href="https://arxiv.org/format/2306.16224">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <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/10.1051/0004-6361/202346841">10.1051/0004-6361/202346841 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The second data release from the European Pulsar Timing Array I. The dataset and timing analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Antoniadis%2C+J">J. Antoniadis</a>, <a href="/search/astro-ph?searchtype=author&query=Babak%2C+S">S. Babak</a>, <a href="/search/astro-ph?searchtype=author&query=Nielsen%2C+A+-+B">A. -S. Bak Nielsen</a>, <a href="/search/astro-ph?searchtype=author&query=Bassa%2C+C+G">C. G. Bassa</a>, <a href="/search/astro-ph?searchtype=author&query=Berthereau%2C+A">A. Berthereau</a>, <a href="/search/astro-ph?searchtype=author&query=Bonetti%2C+M">M. Bonetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bortolas%2C+E">E. Bortolas</a>, <a href="/search/astro-ph?searchtype=author&query=Brook%2C+P+R">P. R. Brook</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Caballero%2C+R+N">R. N. Caballero</a>, <a href="/search/astro-ph?searchtype=author&query=Chalumeau%2C+A">A. Chalumeau</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Chanlaridis%2C+S">S. Chanlaridis</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cognard%2C+I">I. Cognard</a>, <a href="/search/astro-ph?searchtype=author&query=Desvignes%2C+G">G. Desvignes</a>, <a href="/search/astro-ph?searchtype=author&query=Falxa%2C+M">M. Falxa</a>, <a href="/search/astro-ph?searchtype=author&query=Ferdman%2C+R+D">R. D. Ferdman</a>, <a href="/search/astro-ph?searchtype=author&query=Franchini%2C+A">A. Franchini</a>, <a href="/search/astro-ph?searchtype=author&query=Gair%2C+J+R">J. R. Gair</a>, <a href="/search/astro-ph?searchtype=author&query=Goncharov%2C+B">B. Goncharov</a>, <a href="/search/astro-ph?searchtype=author&query=Graikou%2C+E">E. Graikou</a>, <a href="/search/astro-ph?searchtype=author&query=Grie%C3%9Fmeier%2C+J+-">J. -M. Grie脽meier</a>, <a href="/search/astro-ph?searchtype=author&query=Guillemot%2C+L">L. Guillemot</a>, <a href="/search/astro-ph?searchtype=author&query=Guo%2C+Y+J">Y. J. Guo</a> , et al. (44 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="2306.16224v1-abstract-short" style="display: inline;"> Pulsar timing arrays offer a probe of the low-frequency gravitational wave spectrum (1 - 100 nanohertz), which is intimately connected to a number of markers that can uniquely trace the formation and evolution of the Universe. We present the dataset and the results of the timing analysis from the second data release of the European Pulsar Timing Array (EPTA). The dataset contains high-precision pu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.16224v1-abstract-full').style.display = 'inline'; document.getElementById('2306.16224v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.16224v1-abstract-full" style="display: none;"> Pulsar timing arrays offer a probe of the low-frequency gravitational wave spectrum (1 - 100 nanohertz), which is intimately connected to a number of markers that can uniquely trace the formation and evolution of the Universe. We present the dataset and the results of the timing analysis from the second data release of the European Pulsar Timing Array (EPTA). The dataset contains high-precision pulsar timing data from 25 millisecond pulsars collected with the five largest radio telescopes in Europe, as well as the Large European Array for Pulsars. The dataset forms the foundation for the search for gravitational waves by the EPTA, presented in associated papers. We describe the dataset and present the results of the frequentist and Bayesian pulsar timing analysis for individual millisecond pulsars that have been observed over the last ~25 years. We discuss the improvements to the individual pulsar parameter estimates, as well as new measurements of the physical properties of these pulsars and their companions. This data release extends the dataset from EPTA Data Release 1 up to the beginning of 2021, with individual pulsar datasets with timespans ranging from 14 to 25 years. These lead to improved constraints on annual parallaxes, secular variation of the orbital period, and Shapiro delay for a number of sources. Based on these results, we derived astrophysical parameters that include distances, transverse velocities, binary pulsar masses, and annual orbital parallaxes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.16224v1-abstract-full').style.display = 'none'; document.getElementById('2306.16224v1-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 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">29 pages, 9 figures, 13 tables, Astronomy & Astrophysics in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.16214">arXiv:2306.16214</a> <span> [<a href="https://arxiv.org/pdf/2306.16214">pdf</a>, <a href="https://arxiv.org/format/2306.16214">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202346844">10.1051/0004-6361/202346844 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The second data release from the European Pulsar Timing Array III. Search for gravitational wave signals </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Antoniadis%2C+J">J. Antoniadis</a>, <a href="/search/astro-ph?searchtype=author&query=Arumugam%2C+P">P. Arumugam</a>, <a href="/search/astro-ph?searchtype=author&query=Arumugam%2C+S">S. Arumugam</a>, <a href="/search/astro-ph?searchtype=author&query=Babak%2C+S">S. Babak</a>, <a href="/search/astro-ph?searchtype=author&query=Bagchi%2C+M">M. Bagchi</a>, <a href="/search/astro-ph?searchtype=author&query=Nielsen%2C+A+-+B">A. -S. Bak Nielsen</a>, <a href="/search/astro-ph?searchtype=author&query=Bassa%2C+C+G">C. G. Bassa</a>, <a href="/search/astro-ph?searchtype=author&query=Bathula%2C+A">A. Bathula</a>, <a href="/search/astro-ph?searchtype=author&query=Berthereau%2C+A">A. Berthereau</a>, <a href="/search/astro-ph?searchtype=author&query=Bonetti%2C+M">M. Bonetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bortolas%2C+E">E. Bortolas</a>, <a href="/search/astro-ph?searchtype=author&query=Brook%2C+P+R">P. R. Brook</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Caballero%2C+R+N">R. N. Caballero</a>, <a href="/search/astro-ph?searchtype=author&query=Chalumeau%2C+A">A. Chalumeau</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Chanlaridis%2C+S">S. Chanlaridis</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cognard%2C+I">I. Cognard</a>, <a href="/search/astro-ph?searchtype=author&query=Dandapat%2C+S">S. Dandapat</a>, <a href="/search/astro-ph?searchtype=author&query=Deb%2C+D">D. Deb</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">S. Desai</a>, <a href="/search/astro-ph?searchtype=author&query=Desvignes%2C+G">G. Desvignes</a>, <a href="/search/astro-ph?searchtype=author&query=Dhanda-Batra%2C+N">N. Dhanda-Batra</a>, <a href="/search/astro-ph?searchtype=author&query=Dwivedi%2C+C">C. Dwivedi</a> , et al. (73 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="2306.16214v1-abstract-short" style="display: inline;"> We present the results of the search for an isotropic stochastic gravitational wave background (GWB) at nanohertz frequencies using the second data release of the European Pulsar Timing Array (EPTA) for 25 millisecond pulsars and a combination with the first data release of the Indian Pulsar Timing Array (InPTA). We analysed (i) the full 24.7-year EPTA data set, (ii) its 10.3-year subset based on… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.16214v1-abstract-full').style.display = 'inline'; document.getElementById('2306.16214v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.16214v1-abstract-full" style="display: none;"> We present the results of the search for an isotropic stochastic gravitational wave background (GWB) at nanohertz frequencies using the second data release of the European Pulsar Timing Array (EPTA) for 25 millisecond pulsars and a combination with the first data release of the Indian Pulsar Timing Array (InPTA). We analysed (i) the full 24.7-year EPTA data set, (ii) its 10.3-year subset based on modern observing systems, (iii) the combination of the full data set with the first data release of the InPTA for ten commonly timed millisecond pulsars, and (iv) the combination of the 10.3-year subset with the InPTA data. These combinations allowed us to probe the contributions of instrumental noise and interstellar propagation effects. With the full data set, we find marginal evidence for a GWB, with a Bayes factor of four and a false alarm probability of $4\%$. With the 10.3-year subset, we report evidence for a GWB, with a Bayes factor of $60$ and a false alarm probability of about $0.1\%$ ($\gtrsim 3蟽$ significance). The addition of the InPTA data yields results that are broadly consistent with the EPTA-only data sets, with the benefit of better noise modelling. Analyses were performed with different data processing pipelines to test the consistency of the results from independent software packages. The inferred spectrum from the latest EPTA data from new generation observing systems is rather uncertain and in mild tension with the common signal measured in the full data set. However, if the spectral index is fixed at 13/3, the two data sets give a similar amplitude of ($2.5\pm0.7)\times10^{-15}$ at a reference frequency of $1\,{\rm yr}^{-1}$. By continuing our detection efforts as part of the International Pulsar Timing Array (IPTA), we expect to be able to improve the measurement of spatial correlations and better characterise this signal in the coming years. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.16214v1-abstract-full').style.display = 'none'; document.getElementById('2306.16214v1-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 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">21 pages, 14 figures, 4 appendix figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 678, A50 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.13462">arXiv:2306.13462</a> <span> [<a href="https://arxiv.org/pdf/2306.13462">pdf</a>, <a href="https://arxiv.org/format/2306.13462">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/10.1093/mnras/stad1980">10.1093/mnras/stad1980 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Variable Scintillation Arcs of Millisecond Pulsars observed with the Large European Array for Pulsars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Main%2C+R+A">R. A. Main</a>, <a href="/search/astro-ph?searchtype=author&query=Antoniadis%2C+J">J. Antoniadis</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cognard%2C+I">I. Cognard</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+H">H. Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Jang%2C+J">J. Jang</a>, <a href="/search/astro-ph?searchtype=author&query=Karuppusamy%2C+R">R. Karuppusamy</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+K">K. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Y. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Mall%2C+G">G. Mall</a>, <a href="/search/astro-ph?searchtype=author&query=McKee%2C+J+W">J. W. McKee</a>, <a href="/search/astro-ph?searchtype=author&query=Mickaliger%2C+M+B">M. B. Mickaliger</a>, <a href="/search/astro-ph?searchtype=author&query=Perrodin%2C+D">D. Perrodin</a>, <a href="/search/astro-ph?searchtype=author&query=Sanidas%2C+S+A">S. A. Sanidas</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">B. W. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Sprenger%2C+T">T. Sprenger</a>, <a href="/search/astro-ph?searchtype=author&query=Wucknitz%2C+O">O. Wucknitz</a>, <a href="/search/astro-ph?searchtype=author&query=Bassa%2C+C+G">C. G. Bassa</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Concu%2C+R">R. Concu</a>, <a href="/search/astro-ph?searchtype=author&query=Gaikwad%2C+M">M. Gaikwad</a>, <a href="/search/astro-ph?searchtype=author&query=Janssen%2C+G+H">G. H. Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+K+J">K. J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Melis%2C+A">A. Melis</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.13462v1-abstract-short" style="display: inline;"> We present the first large sample of scintillation arcs in millisecond pulsars, analysing 12 sources observed with the Large European Array for Pulsars (LEAP), and the Effelsberg 100\,m telescope. We estimate the delays from multipath propagation, measuring significant correlated changes in scattering timescales over a 10-year timespan. Many sources show compact concentrations of power in the seco… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.13462v1-abstract-full').style.display = 'inline'; document.getElementById('2306.13462v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.13462v1-abstract-full" style="display: none;"> We present the first large sample of scintillation arcs in millisecond pulsars, analysing 12 sources observed with the Large European Array for Pulsars (LEAP), and the Effelsberg 100\,m telescope. We estimate the delays from multipath propagation, measuring significant correlated changes in scattering timescales over a 10-year timespan. Many sources show compact concentrations of power in the secondary spectrum, which in PSRs J0613$-$0200 and J1600$-$3053 can be tracked between observations, and are consistent with compact scattering at fixed angular positions. Other sources such as PSRs J1643$-$1224 and J0621+1002 show diffuse, asymmetric arcs which are likely related to phase-gradients across the scattering screen. PSR B1937+21 shows at least three distinct screens which dominate at different times and evidence of varying screen axes or multi-screen interactions. We model annual and orbital arc curvature variations in PSR J0613$-$0200, providing a measurement of the longitude of ascending node, resolving the sense of the orbital inclination, where our best fit model is of a screen with variable axis of anisotropy over time, corresponding to changes in the scattering of the source. Unmodeled variations of the screen's axis of anisotropy are likely to be a limiting factor in determining orbital parameters with scintillation, requiring careful consideration of variable screen properties, or independent VLBI measurements. Long-term scintillation studies such as this serve as a complementary tool to pulsar timing, to measure a source of correlated noise for pulsar timing arrays, solve pulsar orbits, and to understand the astrophysical origin of scattering screens. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.13462v1-abstract-full').style.display = 'none'; document.getElementById('2306.13462v1-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 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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 to MNRAS, first revision. 18 pages, 16 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/2306.12234">arXiv:2306.12234</a> <span> [<a href="https://arxiv.org/pdf/2306.12234">pdf</a>, <a href="https://arxiv.org/format/2306.12234">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-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/10.1103/PhysRevD.108.123527">10.1103/PhysRevD.108.123527 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Practical approaches to analyzing PTA data: Cosmic strings with six pulsars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Leclere%2C+H+Q">Hippolyte Quelquejay Leclere</a>, <a href="/search/astro-ph?searchtype=author&query=Auclair%2C+P">Pierre Auclair</a>, <a href="/search/astro-ph?searchtype=author&query=Babak%2C+S">Stanislav Babak</a>, <a href="/search/astro-ph?searchtype=author&query=Chalumeau%2C+A">Aur茅lien Chalumeau</a>, <a href="/search/astro-ph?searchtype=author&query=Steer%2C+D+A">Dani猫le A. Steer</a>, <a href="/search/astro-ph?searchtype=author&query=Antoniadis%2C+J">J. Antoniadis</a>, <a href="/search/astro-ph?searchtype=author&query=Nielsen%2C+A+-+B">A. -S. Bak Nielsen</a>, <a href="/search/astro-ph?searchtype=author&query=Bassa%2C+C+G">C. G. Bassa</a>, <a href="/search/astro-ph?searchtype=author&query=Berthereau%2C+A">A. Berthereau</a>, <a href="/search/astro-ph?searchtype=author&query=Bonetti%2C+M">M. Bonetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bortolas%2C+E">E. Bortolas</a>, <a href="/search/astro-ph?searchtype=author&query=Brook%2C+P+R">P. R. Brook</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Caballero%2C+R+N">R. N. Caballero</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Chanlaridis%2C+S">S. Chanlaridis</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cognard%2C+I">I. Cognard</a>, <a href="/search/astro-ph?searchtype=author&query=Desvignes%2C+G">G. Desvignes</a>, <a href="/search/astro-ph?searchtype=author&query=Falxa%2C+M">M. Falxa</a>, <a href="/search/astro-ph?searchtype=author&query=Ferdman%2C+R+D">R. D. Ferdman</a>, <a href="/search/astro-ph?searchtype=author&query=Franchini%2C+A">A. Franchini</a>, <a href="/search/astro-ph?searchtype=author&query=Gair%2C+J+R">J. R. Gair</a>, <a href="/search/astro-ph?searchtype=author&query=Goncharov%2C+B">B. Goncharov</a>, <a href="/search/astro-ph?searchtype=author&query=Graikou%2C+E">E. Graikou</a> , et al. (47 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="2306.12234v3-abstract-short" style="display: inline;"> We search for a stochastic gravitational wave background (SGWB) generated by a network of cosmic strings using six millisecond pulsars from Data Release 2 (DR2) of the European Pulsar Timing Array (EPTA). We perform a Bayesian analysis considering two models for the network of cosmic string loops, and compare it to a simple power-law model which is expected from the population of supermassive blac… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.12234v3-abstract-full').style.display = 'inline'; document.getElementById('2306.12234v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.12234v3-abstract-full" style="display: none;"> We search for a stochastic gravitational wave background (SGWB) generated by a network of cosmic strings using six millisecond pulsars from Data Release 2 (DR2) of the European Pulsar Timing Array (EPTA). We perform a Bayesian analysis considering two models for the network of cosmic string loops, and compare it to a simple power-law model which is expected from the population of supermassive black hole binaries. Our main strong assumption is that the previously reported common red noise process is a SGWB. We find that the one-parameter cosmic string model is slightly favored over a power-law model thanks to its simplicity. If we assume a two-component stochastic signal in the data (supermassive black hole binary population and the signal from cosmic strings), we get a $95\%$ upper limit on the string tension of $\log_{10}(G渭) < -9.9$ ($-10.5$) for the two cosmic string models we consider. In extended two-parameter string models, we were unable to constrain the number of kinks. We test two approximate and fast Bayesian data analysis methods against the most rigorous analysis and find consistent results. These two fast and efficient methods are applicable to all SGWBs, independent of their source, and will be crucial for analysis of extended data sets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.12234v3-abstract-full').style.display = 'none'; document.getElementById('2306.12234v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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, 6 figures; typo corrected in (5)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 108 (2023), 123527 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.18628">arXiv:2305.18628</a> <span> [<a href="https://arxiv.org/pdf/2305.18628">pdf</a>, <a href="https://arxiv.org/format/2305.18628">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/10.1051/0004-6361/202245303">10.1051/0004-6361/202245303 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Simultaneous and panchromatic observations of the Fast Radio Burst FRB 20180916B </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Trudu%2C+M">M. Trudu</a>, <a href="/search/astro-ph?searchtype=author&query=Pilia%2C+M">M. Pilia</a>, <a href="/search/astro-ph?searchtype=author&query=Nicastro%2C+L">L. Nicastro</a>, <a href="/search/astro-ph?searchtype=author&query=Guidorzi%2C+C">C. Guidorzi</a>, <a href="/search/astro-ph?searchtype=author&query=Orlandini%2C+M">M. Orlandini</a>, <a href="/search/astro-ph?searchtype=author&query=Zampieri%2C+L">L. Zampieri</a>, <a href="/search/astro-ph?searchtype=author&query=Marthi%2C+V+R">V. R. Marthi</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosino%2C+F">F. Ambrosino</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Casentini%2C+C">C. Casentini</a>, <a href="/search/astro-ph?searchtype=author&query=Mereminskiy%2C+I">I. Mereminskiy</a>, <a href="/search/astro-ph?searchtype=author&query=Savchenko%2C+V">V. Savchenko</a>, <a href="/search/astro-ph?searchtype=author&query=Palazzi%2C+E">E. Palazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Panessa%2C+F">F. Panessa</a>, <a href="/search/astro-ph?searchtype=author&query=Ridolfi%2C+A">A. Ridolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Verrecchia%2C+F">F. Verrecchia</a>, <a href="/search/astro-ph?searchtype=author&query=Anedda%2C+M">M. Anedda</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardi%2C+G">G. Bernardi</a>, <a href="/search/astro-ph?searchtype=author&query=Bachetti%2C+M">M. Bachetti</a>, <a href="/search/astro-ph?searchtype=author&query=Burenin%2C+R">R. Burenin</a>, <a href="/search/astro-ph?searchtype=author&query=Burtovoi%2C+A">A. Burtovoi</a>, <a href="/search/astro-ph?searchtype=author&query=Casella%2C+P">P. Casella</a>, <a href="/search/astro-ph?searchtype=author&query=Fiori%2C+M">M. Fiori</a>, <a href="/search/astro-ph?searchtype=author&query=Frontera%2C+F">F. Frontera</a> , et al. (25 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.18628v1-abstract-short" style="display: inline;"> Aims. Fast Radio Bursts are bright radio transients whose origin has not yet explained. The search for a multi-wavelength counterpart of those events can put a tight constrain on the emission mechanism and the progenitor source. Methods. We conducted a multi-wavelength observational campaign on FRB 20180916B between October 2020 and August 2021 during eight activity cycles of the source. Observati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.18628v1-abstract-full').style.display = 'inline'; document.getElementById('2305.18628v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.18628v1-abstract-full" style="display: none;"> Aims. Fast Radio Bursts are bright radio transients whose origin has not yet explained. The search for a multi-wavelength counterpart of those events can put a tight constrain on the emission mechanism and the progenitor source. Methods. We conducted a multi-wavelength observational campaign on FRB 20180916B between October 2020 and August 2021 during eight activity cycles of the source. Observations were led in the radio band by the SRT both at 336 MHz and 1547 MHz and the uGMRT at 400 MHz. Simultaneous observations have been conducted by the optical telescopes Asiago (Galileo and Copernico), CMO SAI MSU, CAHA 2.2m, RTT-150 and TNG, and X/Gamma-ray detectors on board the AGILE, Insight-HXMT, INTEGRAL and Swift satellites. Results. We present the detection of 14 new bursts detected with the SRT at 336 MHz and seven new bursts with the uGMRT from this source. We provide the deepest prompt upper limits in the optical band fro FRB 20180916B to date. In fact, the TNG/SiFAP2 observation simultaneous to a burst detection by uGMRT gives an upper limit E_optical / E_radio < 1.3 x 10^2. Another burst detected by the SRT at 336 MHz was also co-observed by Insight-HMXT. The non-detection in the X-rays yields an upper limit (1-30 keV band) of E_X-ray / E_radio in the range of (0.9-1.3) x 10^7, depending on which model is considered for the X-ray emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.18628v1-abstract-full').style.display = 'none'; document.getElementById('2305.18628v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 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">A&A accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 676, A17 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.11263">arXiv:2303.11263</a> <span> [<a href="https://arxiv.org/pdf/2303.11263">pdf</a>, <a href="https://arxiv.org/format/2303.11263">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/acc583">10.3847/1538-4357/acc583 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A young white dwarf orbiting PSR J1835-3259B in the bulge globular cluster NGC 6652 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chen%2C+J">J. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cadelano%2C+M">M. Cadelano</a>, <a href="/search/astro-ph?searchtype=author&query=Pallanca%2C+C">C. Pallanca</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Lanzoni%2C+B">B. Lanzoni</a>, <a href="/search/astro-ph?searchtype=author&query=Istrate%2C+A">A. Istrate</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Freire%2C+P">P. Freire</a>, <a href="/search/astro-ph?searchtype=author&query=Gautam%2C+T">T. Gautam</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Ridolfi%2C+A">A. Ridolfi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.11263v1-abstract-short" style="display: inline;"> We report on the discovery of the companion star to the millisecond pulsar PSR J1835-3259B in the Galactic globular cluster NGC 6652. Taking advantage of deep photometric archival observations acquired through the Hubble Space Telescope in near-ultraviolet and optical bands, we identified a bright and blue object at a position compatible with that of the radio pulsar. The companion is located alon… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.11263v1-abstract-full').style.display = 'inline'; document.getElementById('2303.11263v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.11263v1-abstract-full" style="display: none;"> We report on the discovery of the companion star to the millisecond pulsar PSR J1835-3259B in the Galactic globular cluster NGC 6652. Taking advantage of deep photometric archival observations acquired through the Hubble Space Telescope in near-ultraviolet and optical bands, we identified a bright and blue object at a position compatible with that of the radio pulsar. The companion is located along the helium-core white dwarf cooling sequence and the comparison with binary evolution models provides a mass of $0.17 \pm 0.02~M_\odot$, a surface temperature of $11500\pm1900$ K and a very young cooling age of only $200\pm100$ Myr. The mass and the age of the companion are compatible with a progenitor star of about $0.87~M_{\odot}$, which started transferring mass to the primary during its evolution along the sub-giant branch and stopped during the early red giant branch phase. Combining together the pulsar mass function and the companion mass, we found that this system is observed at an almost edge-on orbit and hosts a neutron star with a mass of $1.44 \pm 0.06~M_\odot$, thus suggesting a highly non-conservative mass accretion phase. The young age of the WD companion is consistent with the scenario of a powerful, relatively young MSP indicated by the earlier detection of gamma-rays from this system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.11263v1-abstract-full').style.display = 'none'; document.getElementById('2303.11263v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 7 figures, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.09231">arXiv:2303.09231</a> <span> [<a href="https://arxiv.org/pdf/2303.09231">pdf</a>, <a href="https://arxiv.org/format/2303.09231">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/stad1900">10.1093/mnras/stad1900 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MPIfR-MeerKAT Galactic Plane survey I -- System setup and early results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Padmanabh%2C+P+V">P. V. Padmanabh</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Sridhar%2C+S+S">S. S. Sridhar</a>, <a href="/search/astro-ph?searchtype=author&query=Rugel%2C+M+R">M. R. Rugel</a>, <a href="/search/astro-ph?searchtype=author&query=Damas-Segovia%2C+A">A. Damas-Segovia</a>, <a href="/search/astro-ph?searchtype=author&query=Jacob%2C+A+M">A. M. Jacob</a>, <a href="/search/astro-ph?searchtype=author&query=Balakrishnan%2C+V">V. Balakrishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Berezina%2C+M">M. Berezina</a>, <a href="/search/astro-ph?searchtype=author&query=Bernadich%2C+M+C+i">M. C. i Bernadich</a>, <a href="/search/astro-ph?searchtype=author&query=Brunthaler%2C+A">A. Brunthaler</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Freire%2C+P+C+C">P. C. C. Freire</a>, <a href="/search/astro-ph?searchtype=author&query=Khan%2C+S">S. Khan</a>, <a href="/search/astro-ph?searchtype=author&query=Kl%C3%B6ckner%2C+H+-">H. -R. Kl枚ckner</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Ma%2C+Y+K">Y. K. Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Mao%2C+S+A">S. A. Mao</a>, <a href="/search/astro-ph?searchtype=author&query=Men%2C+Y+P">Y. P. Men</a>, <a href="/search/astro-ph?searchtype=author&query=Menten%2C+K+M">K. M. Menten</a>, <a href="/search/astro-ph?searchtype=author&query=Sengupta%2C+S">S. Sengupta</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">V. Venkatraman Krishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Wucknitz%2C+O">O. Wucknitz</a>, <a href="/search/astro-ph?searchtype=author&query=Wyrowski%2C+F">F. Wyrowski</a>, <a href="/search/astro-ph?searchtype=author&query=Bezuidenhout%2C+M+C">M. C. Bezuidenhout</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">S. Buchner</a> , et al. (8 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.09231v2-abstract-short" style="display: inline;"> Galactic plane radio surveys play a key role in improving our understanding of a wide range of astrophysical phenomena. Performing such a survey using the latest interferometric telescopes produces large data rates necessitating a shift towards fully or quasi-real-time data analysis with data being stored for only the time required to process them. We present here the overview and setup for the 30… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.09231v2-abstract-full').style.display = 'inline'; document.getElementById('2303.09231v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.09231v2-abstract-full" style="display: none;"> Galactic plane radio surveys play a key role in improving our understanding of a wide range of astrophysical phenomena. Performing such a survey using the latest interferometric telescopes produces large data rates necessitating a shift towards fully or quasi-real-time data analysis with data being stored for only the time required to process them. We present here the overview and setup for the 3000 hour Max-Planck-Institut fuer Radioastronomie (MPIfR) MeerKAT Galactic Plane survey (MMGPS). The survey is unique by operating in a commensal mode, addressing key science objectives of the survey including the discovery of new pulsars and transients as well as studies of Galactic magnetism, the interstellar medium and star formation rates. We explain the strategy coupled with the necessary hardware and software infrastructure needed for data reduction in the imaging, spectral and time domains. We have so far discovered 78 new pulsars including 17 confirmed binary systems of which two are potential double neutron star systems. We have also developed an imaging pipeline sensitive to the order of a few tens of micro-Jansky with a spatial resolution of a few arcseconds. Further science operations with an in-house built S-Band receiver operating between 1.7-3.5 GHz are about to commence. Early spectral line commissioning observations conducted at S-Band, targeting transitions of the key molecular gas tracer CH at 3.3 GHz already illustrate the spectroscopic capabilities of this instrument. These results lay a strong foundation for future surveys with telescopes like the Square Kilometre Array (SKA). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.09231v2-abstract-full').style.display = 'none'; document.getElementById('2303.09231v2-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 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 10 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/2302.00255">arXiv:2302.00255</a> <span> [<a href="https://arxiv.org/pdf/2302.00255">pdf</a>, <a href="https://arxiv.org/format/2302.00255">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/10.1093/mnras/stad508">10.1093/mnras/stad508 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of 37 new pulsars through GPU-accelerated reprocessing of archival data of the Parkes Multibeam Pulsar Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sengar%2C+R">R. Sengar</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Balakrishnan%2C+V">V. Balakrishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Bernadich%2C+M+C+i">M. C. i Bernadich</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Flynn%2C+C+M+L">C. M. L. Flynn</a>, <a href="/search/astro-ph?searchtype=author&query=Shannon%2C+R">R. Shannon</a>, <a href="/search/astro-ph?searchtype=author&query=Stevenson%2C+S">S. Stevenson</a>, <a href="/search/astro-ph?searchtype=author&query=Wongphechauxsorn%2C+J">J. Wongphechauxsorn</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="2302.00255v1-abstract-short" style="display: inline;"> We present the discovery of 37 pulsars from $\sim$ 20 years old archival data of the Parkes Multibeam Pulsar Survey using a new FFT-based search pipeline optimised for discovering narrow-duty cycle pulsars. When developing our pulsar search pipeline, we noticed that the signal-to-noise ratios of folded and optimised pulsars often exceeded that achieved in the spectral domain by a factor of two or… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.00255v1-abstract-full').style.display = 'inline'; document.getElementById('2302.00255v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.00255v1-abstract-full" style="display: none;"> We present the discovery of 37 pulsars from $\sim$ 20 years old archival data of the Parkes Multibeam Pulsar Survey using a new FFT-based search pipeline optimised for discovering narrow-duty cycle pulsars. When developing our pulsar search pipeline, we noticed that the signal-to-noise ratios of folded and optimised pulsars often exceeded that achieved in the spectral domain by a factor of two or greater, in particular for narrow duty cycle ones. Based on simulations, we verified that this is a feature of search codes that sum harmonics incoherently and found that many promising pulsar candidates are revealed when hundreds of candidates per beam with even with modest spectral signal-to-noise ratios of S/N$\sim$5--6 in higher-harmonic folds (up to 32 harmonics) are folded. Of these candidates, 37 were confirmed as new pulsars and a further 37 would have been new discoveries if our search strategies had been used at the time of their initial analysis. While 19 of these newly discovered pulsars have also been independently discovered in more recent pulsar surveys, 18 are exclusive to only the Parkes Multibeam Pulsar Survey data. Some of the notable discoveries include: PSRs J1635$-$47 and J1739$-$31, which show pronounced high-frequency emission; PSRs J1655$-$40 and J1843$-$08, which belong to the nulling/intermittent class of pulsars; and PSR J1636$-$51, which is an interesting binary system in a $\sim$0.75 d orbit and shows hints of eclipsing behaviour -- unusual given the 340 ms rotation period of the pulsar. Our results highlight the importance of reprocessing archival pulsar surveys and using refined search techniques to increase the normal pulsar population. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.00255v1-abstract-full').style.display = 'none'; document.getElementById('2302.00255v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 February, 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">21 pages, 13 Figures, Accepted for publication in Monthly Notices of the Royal Astronomical Society (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/2301.03864">arXiv:2301.03864</a> <span> [<a href="https://arxiv.org/pdf/2301.03864">pdf</a>, <a href="https://arxiv.org/format/2301.03864">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/stad029">10.1093/mnras/stad029 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MeerKAT discovery of 13 new pulsars in Omega Centauri </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">W. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Freire%2C+P+C+C">P. C. C. Freire</a>, <a href="/search/astro-ph?searchtype=author&query=Ridolfi%2C+A">A. Ridolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B">B. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Ransom%2C+S+M">S. M. Ransom</a>, <a href="/search/astro-ph?searchtype=author&query=Levin%2C+L">L. Levin</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=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Abbate%2C+F">F. Abbate</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">V. Venkatraman Krishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabh%2C+P+V">P. V. Padmanabh</a>, <a href="/search/astro-ph?searchtype=author&query=Gautam%2C+T">T. Gautam</a>, <a href="/search/astro-ph?searchtype=author&query=Vleeschower%2C+L">L. Vleeschower</a>, <a href="/search/astro-ph?searchtype=author&query=Geyer%2C+M">M. Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Grie%C3%9Fmeier%2C+J">J-M. Grie脽meier</a>, <a href="/search/astro-ph?searchtype=author&query=Men%2C+Y+P">Y. P. Men</a>, <a href="/search/astro-ph?searchtype=author&query=Balakrishnan%2C+V">V. Balakrishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Bezuidenhout%2C+M+C">M. C. Bezuidenhout</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.03864v1-abstract-short" style="display: inline;"> The most massive globular cluster in our Galaxy, Omega Centauri, is an interesting target for pulsar searches, because of its multiple stellar populations and the intriguing possibility that it was once the nucleus of a galaxy that was absorbed into the Milky Way. The recent discoveries of pulsars in this globular cluster and their association with known X-ray sources was a hint that, given the la… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.03864v1-abstract-full').style.display = 'inline'; document.getElementById('2301.03864v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.03864v1-abstract-full" style="display: none;"> The most massive globular cluster in our Galaxy, Omega Centauri, is an interesting target for pulsar searches, because of its multiple stellar populations and the intriguing possibility that it was once the nucleus of a galaxy that was absorbed into the Milky Way. The recent discoveries of pulsars in this globular cluster and their association with known X-ray sources was a hint that, given the large number of known X-ray sources, there is a much larger undiscovered pulsar population. We used the superior sensitivity of the MeerKAT radio telescope to search for pulsars in Omega Centauri. In this paper, we present some of the first results of this survey, including the discovery of 13 new pulsars; the total number of known pulsars in this cluster currently stands at 18. At least half of them are in binary systems and preliminary orbital constraints suggest that most of the binaries have light companions. We also discuss the ratio between isolated and binaries pulsars and how they were formed in this cluster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.03864v1-abstract-full').style.display = 'none'; document.getElementById('2301.03864v1-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 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.08528">arXiv:2212.08528</a> <span> [<a href="https://arxiv.org/pdf/2212.08528">pdf</a>, <a href="https://arxiv.org/format/2212.08528">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/stac3742">10.1093/mnras/stac3742 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The TRAPUM L-band survey for pulsars in Fermi-LAT gamma-ray sources </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Clark%2C+C+J">C. J. Clark</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=Barr%2C+E+D">E. D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Thongmeearkom%2C+T">T. Thongmeearkom</a>, <a href="/search/astro-ph?searchtype=author&query=Nieder%2C+L">L. Nieder</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B">B. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+W">W. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Mayer%2C+M">M. Mayer</a>, <a href="/search/astro-ph?searchtype=author&query=Phosrisom%2C+A">A. Phosrisom</a>, <a href="/search/astro-ph?searchtype=author&query=Ashok%2C+A">A. Ashok</a>, <a href="/search/astro-ph?searchtype=author&query=Bezuidenhout%2C+M+C">M. C. Bezuidenhout</a>, <a href="/search/astro-ph?searchtype=author&query=Calore%2C+F">F. Calore</a>, <a href="/search/astro-ph?searchtype=author&query=Cognard%2C+I">I. Cognard</a>, <a href="/search/astro-ph?searchtype=author&query=Freire%2C+P+C+C">P. C. C. Freire</a>, <a href="/search/astro-ph?searchtype=author&query=Geyer%2C+M">M. Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Grie%C3%9Fmeier%2C+J+-">J. -M. Grie脽meier</a>, <a href="/search/astro-ph?searchtype=author&query=Karuppusamy%2C+R">R. Karuppusamy</a>, <a href="/search/astro-ph?searchtype=author&query=Levin%2C+L">L. Levin</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabh%2C+P+V">P. V. Padmanabh</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Ransom%2C+S">S. Ransom</a>, <a href="/search/astro-ph?searchtype=author&query=Serylak%2C+M">M. Serylak</a> , et al. (13 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.08528v1-abstract-short" style="display: inline;"> More than 100 millisecond pulsars (MSPs) have been discovered in radio observations of gamma-ray sources detected by the Fermi Large Area Telescope (LAT), but hundreds of pulsar-like sources remain unidentified. Here we present the first results from the targeted survey of Fermi-LAT sources being performed by the Transients and Pulsars with MeerKAT (TRAPUM) Large Survey Project. We observed 79 sou… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.08528v1-abstract-full').style.display = 'inline'; document.getElementById('2212.08528v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.08528v1-abstract-full" style="display: none;"> More than 100 millisecond pulsars (MSPs) have been discovered in radio observations of gamma-ray sources detected by the Fermi Large Area Telescope (LAT), but hundreds of pulsar-like sources remain unidentified. Here we present the first results from the targeted survey of Fermi-LAT sources being performed by the Transients and Pulsars with MeerKAT (TRAPUM) Large Survey Project. We observed 79 sources identified as possible gamma-ray pulsar candidates by a Random Forest classification of unassociated sources from the 4FGL catalogue. Each source was observed for 10 minutes on two separate epochs using MeerKAT's L-band receiver (856-1712 MHz), with typical pulsed flux density sensitivities of $\sim$100$\,渭$Jy. Nine new MSPs were discovered, eight of which are in binary systems, including two eclipsing redbacks and one system, PSR J1526$-$2744, that appears to have a white dwarf companion in an unusually compact 5 hr orbit. We obtained phase-connected timing solutions for two of these MSPs, enabling the detection of gamma-ray pulsations in the Fermi-LAT data. A follow-up search for continuous gravitational waves from PSR J1526$-$2744 in Advanced LIGO data using the resulting Fermi-LAT timing ephemeris yielded no detection, but sets an upper limit on the neutron star ellipticity of $2.45\times10^{-8}$. We also detected X-ray emission from the redback PSR J1803$-$6707 in data from the first eROSITA all-sky survey, likely due to emission from an intra-binary shock. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.08528v1-abstract-full').style.display = 'none'; document.getElementById('2212.08528v1-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 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 8 figures, accepted for publication in MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS, 519, 5590-5606 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.04785">arXiv:2210.04785</a> <span> [<a href="https://arxiv.org/pdf/2210.04785">pdf</a>, <a href="https://arxiv.org/format/2210.04785">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/stac2883">10.1093/mnras/stac2883 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> TRAPUM upper limits on pulsed radio emission for SMC X-ray pulsar J0058-7218 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Carli%2C+E">E. Carli</a>, <a href="/search/astro-ph?searchtype=author&query=Levin%2C+L">L. Levin</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">B. W. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</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=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabh%2C+P+V">P. V. Padmanabh</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">V. Venkatraman Krishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Behrend%2C+J">J. Behrend</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">W. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Men%2C+Y+P">Y. P. Men</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="2210.04785v1-abstract-short" style="display: inline;"> The TRAPUM collaboration has used the MeerKAT telescope to conduct a search for pulsed radio emission from the young Small Magellanic Cloud pulsar J0058-7218 located in the supernova remnant IKT 16, following its discovery in X-rays with XMM-Newton. We report no significant detection of dispersed, pulsed radio emission from this source in three 2-hour L-band observations using the core dishes of M… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.04785v1-abstract-full').style.display = 'inline'; document.getElementById('2210.04785v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.04785v1-abstract-full" style="display: none;"> The TRAPUM collaboration has used the MeerKAT telescope to conduct a search for pulsed radio emission from the young Small Magellanic Cloud pulsar J0058-7218 located in the supernova remnant IKT 16, following its discovery in X-rays with XMM-Newton. We report no significant detection of dispersed, pulsed radio emission from this source in three 2-hour L-band observations using the core dishes of MeerKAT, setting an upper limit of 7.0 渭Jy on its mean flux density at 1284 MHz. This is nearly 7 times deeper than previous radio searches for this pulsar in Parkes L-band observations. This suggests that the radio emission of PSR J0058-7218 is not beamed towards Earth or that PSR J0058-7218 is similar to a handful of Pulsar Wind Nebulae systems that have a very low radio efficiency, such as PSR B0540-6919, the Large Magellanic Cloud Crab pulsar analogue. We have also searched for bright, dispersed, single radio pulses and found no candidates above a fluence of 93 mJy ms at 1284 MHz. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.04785v1-abstract-full').style.display = 'none'; document.getElementById('2210.04785v1-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 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">7 pages, 2 figures, 1 table. 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/2209.11798">arXiv:2209.11798</a> <span> [<a href="https://arxiv.org/pdf/2209.11798">pdf</a>, <a href="https://arxiv.org/format/2209.11798">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> <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/10.1051/0004-6361/202244825">10.1051/0004-6361/202244825 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gravitational signal propagation in the Double Pulsar studied with the MeerKAT telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hu%2C+H">H. Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Wex%2C+N">N. Wex</a>, <a href="/search/astro-ph?searchtype=author&query=Parthasarathy%2C+A">A. Parthasarathy</a>, <a href="/search/astro-ph?searchtype=author&query=Pennucci%2C+T+T">T. T. Pennucci</a>, <a href="/search/astro-ph?searchtype=author&query=Porayko%2C+N+K">N. K. Porayko</a>, <a href="/search/astro-ph?searchtype=author&query=van+Straten%2C+W">W. van Straten</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">V. Venkatraman Krishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Freire%2C+P+C+C">P. C. C. Freire</a>, <a href="/search/astro-ph?searchtype=author&query=Manchester%2C+R+N">R. N. Manchester</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Stairs%2C+I+H">I. H. Stairs</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+A+D">A. D. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Serylak%2C+M">M. Serylak</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.11798v1-abstract-short" style="display: inline;"> The Double Pulsar, PSR J0737-3039A/B, has offered a wealth of gravitational experiments in the strong-field regime, all of which GR has passed with flying colours. In particular, among current gravity experiments that test photon propagation, the Double Pulsar probes the strongest spacetime curvature. Observations with MeerKAT and, in future, the SKA can greatly improve the accuracy of current tes… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.11798v1-abstract-full').style.display = 'inline'; document.getElementById('2209.11798v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.11798v1-abstract-full" style="display: none;"> The Double Pulsar, PSR J0737-3039A/B, has offered a wealth of gravitational experiments in the strong-field regime, all of which GR has passed with flying colours. In particular, among current gravity experiments that test photon propagation, the Double Pulsar probes the strongest spacetime curvature. Observations with MeerKAT and, in future, the SKA can greatly improve the accuracy of current tests and facilitate tests of NLO contributions in both orbital motion and signal propagation. We present our timing analysis of new observations of PSR J0737-3039A, made using the MeerKAT telescope over the last 3 years. The increased timing precision offered by MeerKAT yields a 2 times better measurement of Shapiro delay parameter s and improved mass measurements compared to previous studies. In addition, our results provide an independent confirmation of the NLO signal propagation effects and already surpass the previous measurement from 16-yr data by a factor of 1.65. These effects include the retardation effect due to the movement of B and the deflection of the signal by the gravitational field of B. We also investigate novel effects which are expected. For instance, we search for potential profile variations near superior conjunctions caused by shifts of the line-of-sight due to latitudinal signal deflection and find insignificant evidence with our current data. With simulations, we find that the latitudinal deflection delay is unlikely to be measured with timing because of its correlation with Shapiro delay. Furthermore, although it is currently not possible to detect the expected lensing correction to the Shapiro delay, our simulations suggest that this effect may be measured with the full SKA. Finally, we provide an improved analytical description for the signal propagation in the Double Pulsar system that meets the timing precision expected from future instruments such as the full SKA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.11798v1-abstract-full').style.display = 'none'; document.getElementById('2209.11798v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 13 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 667, A149 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.07880">arXiv:2207.07880</a> <span> [<a href="https://arxiv.org/pdf/2207.07880">pdf</a>, <a href="https://arxiv.org/format/2207.07880">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/ac81c3">10.3847/2041-8213/ac81c3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radio detection of an elusive millisecond pulsar in the Globular Cluster NGC 6397 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+L">Lei Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Ridolfi%2C+A">Alessandro Ridolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Blumer%2C+H">Harsha Blumer</a>, <a href="/search/astro-ph?searchtype=author&query=Freire%2C+P">Paulo Freire</a>, <a href="/search/astro-ph?searchtype=author&query=Manchester%2C+R+N">Richard N. Manchester</a>, <a href="/search/astro-ph?searchtype=author&query=McLaughlin%2C+M">Maura McLaughlin</a>, <a href="/search/astro-ph?searchtype=author&query=Kremer%2C+K">Kyle Kremer</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+A+D">Andrew D. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Z">Zhiyu Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Behrend%2C+J">Jan Behrend</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">Marta Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">Sarah Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">David J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">Weiwei Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+S">Shi Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+Y">Yi Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Fu%2C+X">Xiaoting Fu</a>, <a href="/search/astro-ph?searchtype=author&query=Guo%2C+M">Meng Guo</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+G">George Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Keane%2C+E+F">Evan F. Keane</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">Michael Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Levin%2C+L">Lina Levin</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+X">Xiangdong Li</a>, <a href="/search/astro-ph?searchtype=author&query=Ni%2C+M">Mengmeng Ni</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+J">Jingshan Pan</a> , et al. (10 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2207.07880v1-abstract-short" style="display: inline;"> We report the discovery of a new 5.78 ms-period millisecond pulsar (MSP), PSR J1740-5340B (NGC 6397B), in an eclipsing binary system discovered with the Parkes radio telescope (now also known as Murriyang), Australia, and confirmed with the MeerKAT radio telescope in South Africa. The measured orbital period, 1.97 days, is the longest among all eclipsing binaries in globular clusters (GCs) and con… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.07880v1-abstract-full').style.display = 'inline'; document.getElementById('2207.07880v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.07880v1-abstract-full" style="display: none;"> We report the discovery of a new 5.78 ms-period millisecond pulsar (MSP), PSR J1740-5340B (NGC 6397B), in an eclipsing binary system discovered with the Parkes radio telescope (now also known as Murriyang), Australia, and confirmed with the MeerKAT radio telescope in South Africa. The measured orbital period, 1.97 days, is the longest among all eclipsing binaries in globular clusters (GCs) and consistent with that of the coincident X-ray source U18, previously suggested to be a 'hidden MSP'. Our XMM-Newton observations during NGC 6397B's radio quiescent epochs detected no X-ray flares. NGC 6397B is either a transitional MSP or an eclipsing binary in its initial stage of mass transfer after the companion star left the main sequence. The discovery of NGC 6397B potentially reveals a subgroup of extremely faint and heavily obscured binary pulsars, thus providing a plausible explanation to the apparent dearth of binary neutron stars in core-collapsed GCs as well as a critical constraint on the evolution of GCs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.07880v1-abstract-full').style.display = 'none'; document.getElementById('2207.07880v1-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 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.10045">arXiv:2206.10045</a> <span> [<a href="https://arxiv.org/pdf/2206.10045">pdf</a>, <a href="https://arxiv.org/format/2206.10045">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac1082">10.1093/mnras/stac1082 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detection of quasi-periodic micro-structure in three millisecond pulsars with the Large European Array for Pulsars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liu%2C+K">K. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Antoniadis%2C+J">J. Antoniadis</a>, <a href="/search/astro-ph?searchtype=author&query=Bassa%2C+C+G">C. G. Bassa</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cognard%2C+I">I. Cognard</a>, <a href="/search/astro-ph?searchtype=author&query=Gaikwad%2C+M">M. Gaikwad</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+H">H. Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Jang%2C+J">J. Jang</a>, <a href="/search/astro-ph?searchtype=author&query=Janssen%2C+G+H">G. H. Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Karuppusamy%2C+R">R. Karuppusamy</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+K+J">K. J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Main%2C+R+A">R. A. Main</a>, <a href="/search/astro-ph?searchtype=author&query=Mall%2C+G">G. Mall</a>, <a href="/search/astro-ph?searchtype=author&query=McKee%2C+J+W">J. W. McKee</a>, <a href="/search/astro-ph?searchtype=author&query=Mickaliger%2C+M+B">M. B. Mickaliger</a>, <a href="/search/astro-ph?searchtype=author&query=Perrodin%2C+D">D. Perrodin</a>, <a href="/search/astro-ph?searchtype=author&query=Sanidas%2C+S+A">S. A. Sanidas</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">B. W. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+L">L. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+W+W">W. W. Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Concu%2C+R">R. Concu</a>, <a href="/search/astro-ph?searchtype=author&query=Corongiu%2C+A">A. Corongiu</a>, <a href="/search/astro-ph?searchtype=author&query=Melis%2C+A">A. Melis</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2206.10045v1-abstract-short" style="display: inline;"> We report on the detection of quasi-periodic micro-structure in three millisecond pulsars (MSPs), PSRs J1022+1001, J2145-0750 and J1744-1134, using high time resolution data acquired with the Large European Array for Pulsars at a radio frequency of 1.4 GHz. The occurrence rate of quasi-periodic micro-structure is consistent among pulses with different peak flux densities. Using an auto-correlation… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.10045v1-abstract-full').style.display = 'inline'; document.getElementById('2206.10045v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.10045v1-abstract-full" style="display: none;"> We report on the detection of quasi-periodic micro-structure in three millisecond pulsars (MSPs), PSRs J1022+1001, J2145-0750 and J1744-1134, using high time resolution data acquired with the Large European Array for Pulsars at a radio frequency of 1.4 GHz. The occurrence rate of quasi-periodic micro-structure is consistent among pulses with different peak flux densities. Using an auto-correlation analysis, we measure the periodicity and width of the micro-structure in these three pulsars. The detected micro-structure from PSRs J1022+1001 and J1744-1134 is often highly linearly polarised. In PSR J1022+1001, the linear polarisation position angles of micro-structure pulses are in general flat with a small degree of variation. Using these results, we further examine the frequency and rotational period dependency of micro-structure properties established in previous work, along with the angular beaming and temporal modulation models that explains the appearance of micro-structure. We also discuss a possible link of micro-structure to the properties of some of the recently discovered fast radio bursts which exhibit a very similar emission morphology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.10045v1-abstract-full').style.display = 'none'; document.getElementById('2206.10045v1-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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, 6 figures, 1 table, published in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.04983">arXiv:2205.04983</a> <span> [<a href="https://arxiv.org/pdf/2205.04983">pdf</a>, <a href="https://arxiv.org/format/2205.04983">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/stac1314">10.1093/mnras/stac1314 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The first 7 months of the 2020 X-ray outburst of the magnetar SGR J1935+2154 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Borghese%2C+A">Alice Borghese</a>, <a href="/search/astro-ph?searchtype=author&query=Zelati%2C+F+C">Francesco Coti Zelati</a>, <a href="/search/astro-ph?searchtype=author&query=Israel%2C+G+L">Gian Luca Israel</a>, <a href="/search/astro-ph?searchtype=author&query=Pilia%2C+M">Maura Pilia</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">Marta Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Trudu%2C+M">Matteo Trudu</a>, <a href="/search/astro-ph?searchtype=author&query=Zane%2C+S">Silvia Zane</a>, <a href="/search/astro-ph?searchtype=author&query=Turolla%2C+R">Roberto Turolla</a>, <a href="/search/astro-ph?searchtype=author&query=Rea%2C+N">Nanda Rea</a>, <a href="/search/astro-ph?searchtype=author&query=Esposito%2C+P">Paolo Esposito</a>, <a href="/search/astro-ph?searchtype=author&query=Mereghetti%2C+S">Sandro Mereghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Tiengo%2C+A">Andrea Tiengo</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">Andrea Possenti</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="2205.04983v1-abstract-short" style="display: inline;"> The magnetar SGR J1935+2154 underwent a new active episode on 2020 April 27-28, when a forest of hundreds of X-ray bursts and a large enhancement of the persistent flux were detected. For the first time, a radio burst with properties similar to those of fast radio bursts and with a X-ray counterpart was observed from this source, showing that magnetars can power at least a group of fast radio burs… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.04983v1-abstract-full').style.display = 'inline'; document.getElementById('2205.04983v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.04983v1-abstract-full" style="display: none;"> The magnetar SGR J1935+2154 underwent a new active episode on 2020 April 27-28, when a forest of hundreds of X-ray bursts and a large enhancement of the persistent flux were detected. For the first time, a radio burst with properties similar to those of fast radio bursts and with a X-ray counterpart was observed from this source, showing that magnetars can power at least a group of fast radio bursts. In this paper, we report on the X-ray spectral and timing properties of SGR J1935+2154 based on a long-term monitoring campaign with Chandra, XMM-Newton, NuSTAR, Swift and NICER covering a time span of ~7 months since the outburst onset. The broadband spectrum exhibited a non-thermal power-law component (photon index~1.2) extending up to ~20-25 keV throughout the campaign and a blackbody component with temperature decreasing from ~1.5 keV at the outburst peak to ~0.45 keV in the following months. We found that the luminosity decay is well described by the sum of two exponential functions, reflecting the fast decay (~1 d) at the early stage of the outburst followed by a slower decrease (~30 d). The source reached quiescence about ~80 days after the outburst onset, releasing an energy of ~6e40 erg during the outburst. We detected X-ray pulsations in the XMM-Newton data sets and derived an average spin-down rate of ~3.5e-11 s/s using the spin period measurements derived in this work and three values reported previously during the same active period. Moreover, we report on simultaneous radio observations performed with the Sardinia Radio Telescope. No evidence for periodic or single-pulse radio emission was found. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.04983v1-abstract-full').style.display = 'none'; document.getElementById('2205.04983v1-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 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">17 pages, 5 figures, 4 tables. Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.06869">arXiv:2204.06869</a> <span> [<a href="https://arxiv.org/pdf/2204.06869">pdf</a>, <a href="https://arxiv.org/format/2204.06869">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/10.1093/mnras/stac821">10.1093/mnras/stac821 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The High Time Resolution Universe Pulsar Survey -- XVII. PSR J1325-6253, a low eccentricity double neutron star system from an ultra-stripped supernova </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sengar%2C+R">R. Sengar</a>, <a href="/search/astro-ph?searchtype=author&query=Balakrishnan%2C+V">V. Balakrishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Stevenson%2C+S">S. Stevenson</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Bhat%2C+N+D+R">N. D. R. Bhat</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Bernadich%2C+M+C+i">M. C. i Bernadich</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+A+D">A. D. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">W. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Flynn%2C+C+M+L">C. M. L. Flynn</a>, <a href="/search/astro-ph?searchtype=author&query=Jameson%2C+A">A. Jameson</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+S">S. Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Keith%2C+M+J">M. J. Keith</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Morello%2C+V">V. Morello</a>, <a href="/search/astro-ph?searchtype=author&query=Ng%2C+C">C. Ng</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B">B. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Shannon%2C+R+M">R. M. Shannon</a>, <a href="/search/astro-ph?searchtype=author&query=van+Straten%2C+W">W. van Straten</a>, <a href="/search/astro-ph?searchtype=author&query=Wongphechauxsorn%2C+J">J. Wongphechauxsorn</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.06869v2-abstract-short" style="display: inline;"> The observable population of double neutron star (DNS) systems in the Milky Way allow us to understand the nature of supernovae and binary stellar evolution. Until now, all DNS systems in wide orbits ($ P_{\textrm{orb}}>$ 1~day) have been found to have orbital eccentricities, $e > 0.1$. In this paper, we report the discovery of pulsar PSR J1325$-$6253: a DNS system in a 1.81 day orbit with a surpr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.06869v2-abstract-full').style.display = 'inline'; document.getElementById('2204.06869v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.06869v2-abstract-full" style="display: none;"> The observable population of double neutron star (DNS) systems in the Milky Way allow us to understand the nature of supernovae and binary stellar evolution. Until now, all DNS systems in wide orbits ($ P_{\textrm{orb}}>$ 1~day) have been found to have orbital eccentricities, $e > 0.1$. In this paper, we report the discovery of pulsar PSR J1325$-$6253: a DNS system in a 1.81 day orbit with a surprisingly low eccentricity of just $e = 0.064$. Through 1.4 yr of dedicated timing with the Parkes radio telescope we have been able to measure its rate of advance of periastron, $\dot蠅=0.138 \pm 0.002$ $\rm deg$ $\rm yr^{-1}$. If this induced $\dot蠅$ is solely due to general relativity then the total mass of the system is, $M_{\rm sys} = 2.57 \pm 0.06$ M$_{\odot}$. Assuming an edge-on orbit the minimum companion mass is constrained to be $M_\mathrm{c,min}>0.98$ M$_{\odot}$ which implies the pulsar mass is $M_\mathrm{p,max}<1.59 $ M$_{\odot}$. Its location in the $P$-$\dot{P}$ diagram suggests that, like other DNS systems, PSR J1325$-$6253 is a recycled pulsar and if its mass is similar to the known examples ($>1.3$ M$_\odot$), then the companion neutron star is probably less than $\sim1.25$ M$_\odot$ and the system is inclined at about $50^{\circ}$-$60^{\circ}$. The low eccentricity along with the wide orbit of the system strongly favours a formation scenario involving an ultra-stripped supernova explosion. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.06869v2-abstract-full').style.display = 'none'; document.getElementById('2204.06869v2-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 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 7 figures, 1 table, 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/2204.05334">arXiv:2204.05334</a> <span> [<a href="https://arxiv.org/pdf/2204.05334">pdf</a>, <a href="https://arxiv.org/format/2204.05334">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/stac1041">10.1093/mnras/stac1041 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Four pulsar discoveries in NGC 6624 by TRAPUM using MeerKAT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbate%2C+F">F. Abbate</a>, <a href="/search/astro-ph?searchtype=author&query=Ridolfi%2C+A">A. Ridolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">W. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Freire%2C+P+C+C">P. C. C. Freire</a>, <a href="/search/astro-ph?searchtype=author&query=Gautam%2C+T">T. Gautam</a>, <a href="/search/astro-ph?searchtype=author&query=Grie%C3%9Fmeier%2C+J+M">J. M. Grie脽meier</a>, <a href="/search/astro-ph?searchtype=author&query=K%C3%BCnkel%2C+L">L. K眉nkel</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabh%2C+P+V">P. V. Padmanabh</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Ransom%2C+S">S. Ransom</a>, <a href="/search/astro-ph?searchtype=author&query=Serylak%2C+M">M. Serylak</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">B. W. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">V. Venkatraman Krishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Behrend%2C+J">J. Behrend</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=Levin%2C+L">L. Levin</a>, <a href="/search/astro-ph?searchtype=author&query=Men%2C+Y">Y. Men</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.05334v1-abstract-short" style="display: inline;"> We report 4 new pulsars discovered in the core-collapsed globular cluster (GC) NGC 6624 by the TRAPUM Large Survey Project with the MeerKAT telescope. All of the new pulsars found are isolated. PSR J1823$-$3021I and PSR J1823$-$3021K are millisecond pulsars with period of respectively 4.319 ms and 2.768 ms. PSR J1823$-$3021J is mildly recycled with a period of 20.899 ms, and PSR J1823$-$3022 is a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.05334v1-abstract-full').style.display = 'inline'; document.getElementById('2204.05334v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.05334v1-abstract-full" style="display: none;"> We report 4 new pulsars discovered in the core-collapsed globular cluster (GC) NGC 6624 by the TRAPUM Large Survey Project with the MeerKAT telescope. All of the new pulsars found are isolated. PSR J1823$-$3021I and PSR J1823$-$3021K are millisecond pulsars with period of respectively 4.319 ms and 2.768 ms. PSR J1823$-$3021J is mildly recycled with a period of 20.899 ms, and PSR J1823$-$3022 is a long period pulsar with a period of 2.497 s. The pulsars J1823$-$3021I, J1823$-$3021J, and J1823$-$3021K have position and dispersion measure (DM) compatible with being members of the GC and are therefore associated with NGC 6624. Pulsar J1823$-$3022 is the only pulsar bright enough to be re-detected in archival observations of the cluster. This allowed the determination of a timing solution that spans over two decades. It is not possible at the moment to claim the association of pulsar J1823$-$3022 with the GC given the long period and large offset in position ($\sim 3$ arcminutes) and DM (with a fractional difference of 11 percent compared the average of the pulsars in NGC 6624). The discoveries made use of the beamforming capability of the TRAPUM backend to generate multiple beams in the same field of view which allows sensitive searches to be performed over a few half-light radii from the cluster center and can simultaneously localise the discoveries. The discoveries reflect the properties expected for pulsars in core-collapsed GCs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.05334v1-abstract-full').style.display = 'none'; document.getElementById('2204.05334v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication on Monthly Notices of the Royal Astronomical Society. 11 pages, 6 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.00086">arXiv:2204.00086</a> <span> [<a href="https://arxiv.org/pdf/2204.00086">pdf</a>, <a href="https://arxiv.org/format/2204.00086">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac921">10.1093/mnras/stac921 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discoveries and Timing of Pulsars in NGC 6440 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vleeschower%2C+L">L. Vleeschower</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">B. W. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Ransom%2C+S">S. Ransom</a>, <a href="/search/astro-ph?searchtype=author&query=Ridolfi%2C+A">A. Ridolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">V. Venkatraman Krishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Keith%2C+M+J">M. J. Keith</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Freire%2C+P+C+C">P. C. C. Freire</a>, <a href="/search/astro-ph?searchtype=author&query=Spiewak%2C+R">R. Spiewak</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Bezuidenhout%2C+M+C">M. C. Bezuidenhout</a>, <a href="/search/astro-ph?searchtype=author&query=Ni%C5%A3u%2C+I+C">I. C. Ni牛u</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">W. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Parthasarathy%2C+A">A. Parthasarathy</a>, <a href="/search/astro-ph?searchtype=author&query=DeCesar%2C+M+E">M. E. DeCesar</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Stairs%2C+I+H">I. H. Stairs</a>, <a href="/search/astro-ph?searchtype=author&query=Hessels%2C+J+W+T">J. W. T. Hessels</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.00086v1-abstract-short" style="display: inline;"> Using the MeerKAT radio telescope, a series of observations have been conducted to time the known pulsars and search for new pulsars in the globular cluster NGC 6440. As a result, two pulsars have been discovered, NGC 6440G and NGC 6440H, one of which is isolated and the other a non-eclipsing (at frequencies above 962 MHz) "Black Widow", with a very low mass companion (M$_{\rm c}$ > 0.006 M… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.00086v1-abstract-full').style.display = 'inline'; document.getElementById('2204.00086v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.00086v1-abstract-full" style="display: none;"> Using the MeerKAT radio telescope, a series of observations have been conducted to time the known pulsars and search for new pulsars in the globular cluster NGC 6440. As a result, two pulsars have been discovered, NGC 6440G and NGC 6440H, one of which is isolated and the other a non-eclipsing (at frequencies above 962 MHz) "Black Widow", with a very low mass companion (M$_{\rm c}$ > 0.006 M$_{\odot}$). It joins the other binary pulsars discovered so far in this cluster which all have low companion masses (M$_{\rm c}$ < 0.30 M$_{\odot}$). We present the results of long-term timing solutions obtained using data from both Green Bank and MeerKAT telescopes for these two new pulsars and an analysis of the pulsars NGC 6440C and NGC 6440D. For the isolated pulsar NGC 6440C, we searched for planets using a Markov Chain Monte Carlo technique. We find evidence for significant unmodelled variations but they cannot be well modelled as planets nor as part of a power-law red-noise process. Studies of the eclipses of the "Redback" pulsar NGC 6440D at two different frequency bands reveal a frequency dependence with longer and asymmetric eclipses at lower frequencies (962-1283 MHz). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.00086v1-abstract-full').style.display = 'none'; document.getElementById('2204.00086v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 10 figures, 4 tables. Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.12302">arXiv:2203.12302</a> <span> [<a href="https://arxiv.org/pdf/2203.12302">pdf</a>, <a href="https://arxiv.org/format/2203.12302">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/10.1051/0004-6361/202143006">10.1051/0004-6361/202143006 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> TRAPUM discovery of thirteen new pulsars in NGC 1851 using MeerKAT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ridolfi%2C+A">A. Ridolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Freire%2C+P+C+C">P. C. C. Freire</a>, <a href="/search/astro-ph?searchtype=author&query=Gautam%2C+T">T. Gautam</a>, <a href="/search/astro-ph?searchtype=author&query=Ransom%2C+S+M">S. M. Ransom</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Abbate%2C+F">F. Abbate</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">V. Venkatraman Krishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Vleeschower%2C+L">L. Vleeschower</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">B. W. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">W. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabh%2C+P+V">P. V. Padmanabh</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Levin%2C+L">L. Levin</a>, <a href="/search/astro-ph?searchtype=author&query=Keane%2C+E+F">E. F. Keane</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=Bezuidenhout%2C+M">M. Bezuidenhout</a>, <a href="/search/astro-ph?searchtype=author&query=Grie%C3%9Fmeier%2C+J+-">J. -M. Grie脽meier</a>, <a href="/search/astro-ph?searchtype=author&query=K%C3%BCnkel%2C+L">L. K眉nkel</a>, <a href="/search/astro-ph?searchtype=author&query=Men%2C+Y">Y. Men</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.12302v1-abstract-short" style="display: inline;"> We report the discovery of 13 new pulsars in the globular cluster NGC 1851 by the TRAPUM Large Survey Project using the MeerKAT radio telescope. The discoveries consist of six isolated millisecond pulsars (MSPs) and seven binary pulsars, of which six are MSPs and one is mildly recycled. For all the pulsars, we present the basic kinematic, astrometric, and orbital parameters, where applicable, as w… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.12302v1-abstract-full').style.display = 'inline'; document.getElementById('2203.12302v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.12302v1-abstract-full" style="display: none;"> We report the discovery of 13 new pulsars in the globular cluster NGC 1851 by the TRAPUM Large Survey Project using the MeerKAT radio telescope. The discoveries consist of six isolated millisecond pulsars (MSPs) and seven binary pulsars, of which six are MSPs and one is mildly recycled. For all the pulsars, we present the basic kinematic, astrometric, and orbital parameters, where applicable, as well as their polarimetric properties, when these are measurable. Two of the binary MSPs (PSR J0514-4002D and PSR J0514-4002E) are in wide and extremely eccentric (e > 0.7) orbits with a heavy white dwarf and a neutron star as their companion, respectively. With these discoveries, NGC 1851 is now tied with M28 as the cluster with the third largest number of known pulsars (14). Its pulsar population shows remarkable similarities with that of M28, Terzan 5 and other clusters with comparable structural parameters. The newly-found pulsars are all located in the innermost regions of NGC 1851 and will likely enable, among other things, detailed studies of the cluster structure and dynamics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.12302v1-abstract-full').style.display = 'none'; document.getElementById('2203.12302v1-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 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 6 figures, 3 tables. Accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 664, A27 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.00607">arXiv:2203.00607</a> <span> [<a href="https://arxiv.org/pdf/2203.00607">pdf</a>, <a href="https://arxiv.org/format/2203.00607">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/10.1051/0004-6361/202142670">10.1051/0004-6361/202142670 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The eccentric millisecond pulsar, PSR J0955$-$6150 I: Pulse profile analysis, mass measurements and constraints on binary evolution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Serylak%2C+M">M. Serylak</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">V. Venkatraman Krishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Freire%2C+P+C+C">P. C. C. Freire</a>, <a href="/search/astro-ph?searchtype=author&query=Tauris%2C+T+M">T. M. Tauris</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Geyer%2C+M">M. Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Parthasarathy%2C+A">A. Parthasarathy</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Bernadich%2C+M+C+i">M. C. i Bernadich</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Karastergiou%2C+A">A. Karastergiou</a>, <a href="/search/astro-ph?searchtype=author&query=Lower%2C+M+E">M. E. Lower</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Reardon%2C+D+J">D. J. Reardon</a>, <a href="/search/astro-ph?searchtype=author&query=Shannon%2C+R+M">R. M. Shannon</a>, <a href="/search/astro-ph?searchtype=author&query=Spiewak%2C+R">R. Spiewak</a>, <a href="/search/astro-ph?searchtype=author&query=Stairs%2C+I+H">I. H. Stairs</a>, <a href="/search/astro-ph?searchtype=author&query=van+Straten%2C+W">W. van Straten</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.00607v1-abstract-short" style="display: inline;"> PSR J0955$-$6150 is a member of a class of eccentric MSP+He WD systems (eMSPs), whose binary evolution is poorly understood and believed to be different to that of traditional MSP+He WD systems. Measuring the masses of the stars in this system is important for testing hypotheses for the formation of eMSPs. We have carried out observations of this pulsar with the Parkes and MeerKAT radio telescopes… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.00607v1-abstract-full').style.display = 'inline'; document.getElementById('2203.00607v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.00607v1-abstract-full" style="display: none;"> PSR J0955$-$6150 is a member of a class of eccentric MSP+He WD systems (eMSPs), whose binary evolution is poorly understood and believed to be different to that of traditional MSP+He WD systems. Measuring the masses of the stars in this system is important for testing hypotheses for the formation of eMSPs. We have carried out observations of this pulsar with the Parkes and MeerKAT radio telescopes. Our observations reveal a strong frequency evolution of this pulsar's intensity, with a spectral index ($伪$) of $-3.13(2)$. The sensitivity of MeerKAT has resulted in a $>10$-fold improvement in the timing precision compared to older Parkes observations. Combined with the 8-year timing baseline, it has allowed precise measurements of a proper motion and three orbital "post-Keplerian" parameters: the rate of advance of periastron, $\dot蠅 = 0.00152(1) \, {\rm deg} \, yr^{-1}$ and the orthometric Shapiro delay parameters, $h_3 = 0.89(7) \, 渭$s and $蟼= 0.88(2)$. Assuming general relativity, we obtain $M_{p} = 1.71(2) \, M_{\odot}$ for the mass of the pulsar and $M_{c} = 0.254(2) \, M_{\odot}$ for the mass of the companion; the orbital inclination is 83.2(4) degrees. We find that the spin axis has a misalignment relative to the orbital angular momentum of $> 4.8$ degrees at 99% CI. While the value of $M_{\rm p}$ falls within the wide range observed in eMSPs, $M_{\rm c}$ is significantly smaller than expected, allowing several formation hypotheses being ruled out. $M_{\rm c}$ is also significantly different from the expected value for an ideal low mass X-ray binary evolution scenario. The putative misalignment between the spin axis of the pulsar and the orbital angular momentum suggests that the unknown process that created the orbital eccentricity of the binary was also capable of changing its orbital orientation, an important evidence for understanding the origin of eMSPs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.00607v1-abstract-full').style.display = 'none'; document.getElementById('2203.00607v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 9 figures, 5 tables, accepted for publication by the 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 665, A53 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.11238">arXiv:2201.11238</a> <span> [<a href="https://arxiv.org/pdf/2201.11238">pdf</a>, <a href="https://arxiv.org/format/2201.11238">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/ac4744">10.3847/1538-4357/ac4744 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Two New Black Widow Millisecond Pulsars In M28 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Douglas%2C+A">Andrew Douglas</a>, <a href="/search/astro-ph?searchtype=author&query=Padmanabh%2C+P">Prajwal Padmanabh</a>, <a href="/search/astro-ph?searchtype=author&query=Ransom%2C+S">Scott Ransom</a>, <a href="/search/astro-ph?searchtype=author&query=Ridolfi%2C+A">Alessandro Ridolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Freire%2C+P">Paulo Freire</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">Vivek Venkatraman Krishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E">Ewan Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Pallanca%2C+C">Cristina Pallanca</a>, <a href="/search/astro-ph?searchtype=author&query=Cadelano%2C+M">Mario Cadelano</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">Andrea Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Stairs%2C+I">Ingrid Stairs</a>, <a href="/search/astro-ph?searchtype=author&query=Hessels%2C+J">Jason Hessels</a>, <a href="/search/astro-ph?searchtype=author&query=DeCesar%2C+M">Megan DeCesar</a>, <a href="/search/astro-ph?searchtype=author&query=Lynch%2C+R">Ryan Lynch</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">Matthew Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">Marta Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D">David Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Karuppusamy%2C+R">Ramesh Karuppusamy</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">Michael Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B">Benjamin Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Vleeschower%2C+L">Laila Vleeschower</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="2201.11238v3-abstract-short" style="display: inline;"> We report the discovery of two Black Widow millisecond pulsars in the globular cluster M28 with the MeerKAT telescope. PSR J1824$-$2452M (M28M) is a 4.78-ms pulsar in a $5.82\,$hour orbit and PSR J1824$-$2452N (M28N) is a 3.35-ms pulsar in a $4.76\,$hour orbit. Both pulsars have dispersion measures near $119.30\,$pc$\,$cm$^{-3}$ and have low mass companion stars ($\sim$$0.01-0.03\,$M$_\odot$), whi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.11238v3-abstract-full').style.display = 'inline'; document.getElementById('2201.11238v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.11238v3-abstract-full" style="display: none;"> We report the discovery of two Black Widow millisecond pulsars in the globular cluster M28 with the MeerKAT telescope. PSR J1824$-$2452M (M28M) is a 4.78-ms pulsar in a $5.82\,$hour orbit and PSR J1824$-$2452N (M28N) is a 3.35-ms pulsar in a $4.76\,$hour orbit. Both pulsars have dispersion measures near $119.30\,$pc$\,$cm$^{-3}$ and have low mass companion stars ($\sim$$0.01-0.03\,$M$_\odot$), which do not cause strong radio eclipses or orbital variations. Including these systems, there are now five known black widow pulsars in M28. The pulsar searches were conducted as a part of an initial phase of MeerKAT's globular cluster census (within the TRAPUM Large Survey Project). These faint discoveries demonstrate the advantages of MeerKAT's survey sensitivity over previous searches and we expect to find additional pulsars in continued searches of this cluster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.11238v3-abstract-full').style.display = 'none'; document.getElementById('2201.11238v3-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 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to ApJ on 12/28/2021 2/17/2022: Added Acknowledgements, Software, and Facilities sections. Fixed missing 'Total Proper Motion' units 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/2201.04245">arXiv:2201.04245</a> <span> [<a href="https://arxiv.org/pdf/2201.04245">pdf</a>, <a href="https://arxiv.org/format/2201.04245">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac096">10.1093/mnras/stac096 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Modelling annual scintillation arc variations in PSR J1643-1224 using the Large European Array for Pulsars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mall%2C+G">G. Mall</a>, <a href="/search/astro-ph?searchtype=author&query=Main%2C+R+A">R. A. Main</a>, <a href="/search/astro-ph?searchtype=author&query=Antoniadis%2C+J">J. Antoniadis</a>, <a href="/search/astro-ph?searchtype=author&query=Bassa%2C+C+G">C. G. Bassa</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cognard%2C+I">I. Cognard</a>, <a href="/search/astro-ph?searchtype=author&query=Concu%2C+R">R. Concu</a>, <a href="/search/astro-ph?searchtype=author&query=Corongiu%2C+A">A. Corongiu</a>, <a href="/search/astro-ph?searchtype=author&query=Gaikwad%2C+M">M. Gaikwad</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+H">H. Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Janssen%2C+G+H">G. H. Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Karuppusamy%2C+R">R. Karuppusamy</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+K+J">K. J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+K">K. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=McKee%2C+J+W">J. W. McKee</a>, <a href="/search/astro-ph?searchtype=author&query=Melis%2C+A">A. Melis</a>, <a href="/search/astro-ph?searchtype=author&query=Mickaliger%2C+M+B">M. B. Mickaliger</a>, <a href="/search/astro-ph?searchtype=author&query=Perrodin%2C+D">D. Perrodin</a>, <a href="/search/astro-ph?searchtype=author&query=Pilia%2C+M">M. Pilia</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Reardon%2C+D+J">D. J. Reardon</a>, <a href="/search/astro-ph?searchtype=author&query=Sanidas%2C+S+A">S. A. Sanidas</a>, <a href="/search/astro-ph?searchtype=author&query=Sprenger%2C+T">T. Sprenger</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">B. W. Stappers</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.04245v1-abstract-short" style="display: inline;"> In this work we study variations in the parabolic scintillation arcs of the binary millisecond pulsar PSR J1643-1224 over five years using the Large European Array for Pulsars (LEAP). The 2D power spectrum of scintillation, called the secondary spectrum, often shows a parabolic distribution of power, where the arc curvature encodes the relative velocities and distances of the pulsar, ionised inter… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.04245v1-abstract-full').style.display = 'inline'; document.getElementById('2201.04245v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.04245v1-abstract-full" style="display: none;"> In this work we study variations in the parabolic scintillation arcs of the binary millisecond pulsar PSR J1643-1224 over five years using the Large European Array for Pulsars (LEAP). The 2D power spectrum of scintillation, called the secondary spectrum, often shows a parabolic distribution of power, where the arc curvature encodes the relative velocities and distances of the pulsar, ionised interstellar medium (IISM), and Earth. We observe a clear parabolic scintillation arc which varies in curvature throughout the year. The distribution of power in the secondary spectra are inconsistent with a single scattering screen which is fully 1D, or entirely isotropic. We fit the observed arc curvature variations with two models; an isotropic scattering screen, and a model with two independent 1D screens. We measure the distance to the scattering screen to be in the range 114-223 pc, depending on the model, consistent with the known distance of the foreground large-diameter HII region Sh 2-27 (112+/-17 pc), suggesting that it is the dominant source of scattering. We obtain only weak constraints on the pulsar's orbital inclination and angle of periastron, since the scintillation pattern is not very sensitive to the pulsar's motion, since the screen is much closer to the Earth than the pulsar. More measurements of this kind - where scattering screens can be associated with foreground objects - will help to inform the origins and distribution of scattering screens within our galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.04245v1-abstract-full').style.display = 'none'; document.getElementById('2201.04245v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 6 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/2201.03980">arXiv:2201.03980</a> <span> [<a href="https://arxiv.org/pdf/2201.03980">pdf</a>, <a href="https://arxiv.org/format/2201.03980">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/stab3418">10.1093/mnras/stab3418 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The International Pulsar Timing Array second data release: Search for an isotropic Gravitational Wave Background </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Antoniadis%2C+J">J. Antoniadis</a>, <a href="/search/astro-ph?searchtype=author&query=Arzoumanian%2C+Z">Z. Arzoumanian</a>, <a href="/search/astro-ph?searchtype=author&query=Babak%2C+S">S. Babak</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Nielsen%2C+A+-+B">A. -S. Bak Nielsen</a>, <a href="/search/astro-ph?searchtype=author&query=Baker%2C+P+T">P. T. Baker</a>, <a href="/search/astro-ph?searchtype=author&query=Bassa%2C+C+G">C. G. Bassa</a>, <a href="/search/astro-ph?searchtype=author&query=Becsy%2C+B">B. Becsy</a>, <a href="/search/astro-ph?searchtype=author&query=Berthereau%2C+A">A. Berthereau</a>, <a href="/search/astro-ph?searchtype=author&query=Bonetti%2C+M">M. Bonetti</a>, <a href="/search/astro-ph?searchtype=author&query=Brazier%2C+A">A. Brazier</a>, <a href="/search/astro-ph?searchtype=author&query=Brook%2C+P+R">P. R. Brook</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Burke-Spolaor%2C+S">S. Burke-Spolaor</a>, <a href="/search/astro-ph?searchtype=author&query=Caballero%2C+R+N">R. N. Caballero</a>, <a href="/search/astro-ph?searchtype=author&query=Casey-Clyde%2C+J+A">J. A. Casey-Clyde</a>, <a href="/search/astro-ph?searchtype=author&query=Chalumeau%2C+A">A. Chalumeau</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Charisi%2C+M">M. Charisi</a>, <a href="/search/astro-ph?searchtype=author&query=Chatterjee%2C+S">S. Chatterjee</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cognard%2C+I">I. Cognard</a>, <a href="/search/astro-ph?searchtype=author&query=Cordes%2C+J+M">J. M. Cordes</a>, <a href="/search/astro-ph?searchtype=author&query=Cornish%2C+N+J">N. J. Cornish</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+F">F. Crawford</a> , et al. (101 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.03980v1-abstract-short" style="display: inline;"> We searched for an isotropic stochastic gravitational wave background in the second data release of the International Pulsar Timing Array, a global collaboration synthesizing decadal-length pulsar-timing campaigns in North America, Europe, and Australia. In our reference search for a power law strain spectrum of the form $h_c = A(f/1\,\mathrm{yr}^{-1})^伪$, we found strong evidence for a spectrally… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.03980v1-abstract-full').style.display = 'inline'; document.getElementById('2201.03980v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.03980v1-abstract-full" style="display: none;"> We searched for an isotropic stochastic gravitational wave background in the second data release of the International Pulsar Timing Array, a global collaboration synthesizing decadal-length pulsar-timing campaigns in North America, Europe, and Australia. In our reference search for a power law strain spectrum of the form $h_c = A(f/1\,\mathrm{yr}^{-1})^伪$, we found strong evidence for a spectrally-similar low-frequency stochastic process of amplitude $A = 3.8^{+6.3}_{-2.5}\times10^{-15}$ and spectral index $伪= -0.5 \pm 0.5$, where the uncertainties represent 95\% credible regions, using information from the auto- and cross-correlation terms between the pulsars in the array. For a spectral index of $伪= -2/3$, as expected from a population of inspiralling supermassive black hole binaries, the recovered amplitude is $A = 2.8^{+1.2}_{-0.8}\times10^{-15}$. Nonetheless, no significant evidence of the Hellings-Downs correlations that would indicate a gravitational-wave origin was found. We also analyzed the constituent data from the individual pulsar timing arrays in a consistent way, and clearly demonstrate that the combined international data set is more sensitive. Furthermore, we demonstrate that this combined data set produces comparable constraints to recent single-array data sets which have more data than the constituent parts of the combination. Future international data releases will deliver increased sensitivity to gravitational wave radiation, and significantly increase the detection probability. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.03980v1-abstract-full').style.display = 'none'; document.getElementById('2201.03980v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 12 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/2112.06795">arXiv:2112.06795</a> <span> [<a href="https://arxiv.org/pdf/2112.06795">pdf</a>, <a href="https://arxiv.org/format/2112.06795">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="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/10.1103/PhysRevX.11.041050">10.1103/PhysRevX.11.041050 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Strong-field Gravity Tests with the Double Pulsar </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Stairs%2C+I+H">I. H. Stairs</a>, <a href="/search/astro-ph?searchtype=author&query=Manchester%2C+R+N">R. N. Manchester</a>, <a href="/search/astro-ph?searchtype=author&query=Wex%2C+N">N. Wex</a>, <a href="/search/astro-ph?searchtype=author&query=Deller%2C+A+T">A. T. Deller</a>, <a href="/search/astro-ph?searchtype=author&query=Coles%2C+W+A">W. A. Coles</a>, <a href="/search/astro-ph?searchtype=author&query=Ali%2C+M">M. Ali</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Cognard%2C+I">I. Cognard</a>, <a href="/search/astro-ph?searchtype=author&query=Damour%2C+T">T. Damour</a>, <a href="/search/astro-ph?searchtype=author&query=Desvignes%2C+G">G. Desvignes</a>, <a href="/search/astro-ph?searchtype=author&query=Ferdman%2C+R+D">R. D. Ferdman</a>, <a href="/search/astro-ph?searchtype=author&query=Freire%2C+P+C+C">P. C. C. Freire</a>, <a href="/search/astro-ph?searchtype=author&query=Grondin%2C+S">S. Grondin</a>, <a href="/search/astro-ph?searchtype=author&query=Guillemot%2C+L">L. Guillemot</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+G+B">G. B. Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Janssen%2C+G">G. Janssen</a>, <a href="/search/astro-ph?searchtype=author&query=Karuppusamy%2C+R">R. Karuppusamy</a>, <a href="/search/astro-ph?searchtype=author&query=Lorimer%2C+D+R">D. R. Lorimer</a>, <a href="/search/astro-ph?searchtype=author&query=Lyne%2C+A+G">A. G. Lyne</a>, <a href="/search/astro-ph?searchtype=author&query=McKee%2C+J+W">J. W. McKee</a>, <a href="/search/astro-ph?searchtype=author&query=McLaughlin%2C+M">M. McLaughlin</a>, <a href="/search/astro-ph?searchtype=author&query=Muench%2C+L+E">L. E. Muench</a>, <a href="/search/astro-ph?searchtype=author&query=Perera%2C+B+B+P">B. B. P. Perera</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2112.06795v2-abstract-short" style="display: inline;"> Continued observations of the Double Pulsar, PSR J0737-3039A/B, consisting of two radio pulsars (A and B) that orbit each other with a period of 2.45hr in a mildly eccentric (e=0.088) binary system, have led to large improvements in the measurement of relativistic effects in this system. With a 16-yr data span, the results enable precision tests of theories of gravity for strongly self-gravitating… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.06795v2-abstract-full').style.display = 'inline'; document.getElementById('2112.06795v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.06795v2-abstract-full" style="display: none;"> Continued observations of the Double Pulsar, PSR J0737-3039A/B, consisting of two radio pulsars (A and B) that orbit each other with a period of 2.45hr in a mildly eccentric (e=0.088) binary system, have led to large improvements in the measurement of relativistic effects in this system. With a 16-yr data span, the results enable precision tests of theories of gravity for strongly self-gravitating bodies and also reveal new relativistic effects that have been expected but are now observed for the first time. These include effects of light propagation in strong gravitational fields which are currently not testable by any other method. We observe retardation and aberrational light-bending that allow determination of the pulsar's spin direction. In total, we have detected seven post-Keplerian (PK) parameters, more than for any other binary pulsar. For some of these effects, the measurement precision is so high that for the first time we have to take higher-order contributions into account. These include contributions of A's effective mass loss (due to spin-down) to the observed orbital period decay, a relativistic deformation of the orbit, and effects of the equation of state of super-dense matter on the observed PK parameters via relativistic spin-orbit coupling. We discuss the implications of our findings, including those for the moment of inertia of neutron stars. We present the currently most precise test of general relativity's (GR's) quadrupolar description of gravitational waves, validating GR's prediction at a level of $1.3 \times 10^{-4}$ (95% conf.). We demonstrate the utility of the Double Pulsar for tests of alternative theories by focusing on two specific examples and discuss some implications for studies of the interstellar medium and models for the formation of the Double Pulsar. Finally, we provide context to other types of related experiments and prospects for the future. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.06795v2-abstract-full').style.display = 'none'; document.getElementById('2112.06795v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">56 pages, 23 Figures. Published by Physical Review X. Uploaded ArXiv version is authors' (pre-proof) version with abbreviated abstract. Resubmission for updated acknowledgement information. For final published version see https://link.aps.org/doi/10.1103/PhysRevX.11.041050</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. X 11, 041050 (2021) </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Burgay%2C+M&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Burgay%2C+M&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Burgay%2C+M&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Burgay%2C+M&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Burgay%2C+M&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> <li> <a href="/search/?searchtype=author&query=Burgay%2C+M&start=200" 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