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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Camilo%2C+F&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Camilo%2C+F&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Camilo%2C+F&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Camilo%2C+F&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Camilo%2C+F&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> <li> <a 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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/stae2690">10.1093/mnras/stae2690 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The SARAO MeerKAT Galactic Plane Survey filamentary source catalogue </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Williams%2C+G+M">Gwenllian M. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+M+A">Mark A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Mutale%2C+M">Mubela Mutale</a>, <a href="/search/astro-ph?searchtype=author&query=Rigby%2C+A+J">Andrew J. Rigby</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">Cristobal Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">Simone Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Bietenholz%2C+M">Michael Bietenholz</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+L+D">Loren D. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">Fernando Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Goedhart%2C+S">Sharmila Goedhart</a>, <a href="/search/astro-ph?searchtype=author&query=Jaffa%2C+S+E">Sarah E. Jaffa</a>, <a href="/search/astro-ph?searchtype=author&query=Obonyo%2C+W+O">Willice O. Obonyo</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">Corrado Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">Grazia Umana</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.07852v1-abstract-short" style="display: inline;"> We present a catalogue of filamentary structures identified in the SARAO (South African Radio Astronomy Observatory) MeerKAT 1.3 GHz Galactic Plane Survey (SMGPS). We extract 933 filaments across the survey area, 803 of which (~86%) are associated with extended radio structures (e.g. supernova remnants and HII regions), whilst 130 (~14%) are largely isolated. We classify filaments as thermal or no… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.07852v1-abstract-full').style.display = 'inline'; document.getElementById('2412.07852v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.07852v1-abstract-full" style="display: none;"> We present a catalogue of filamentary structures identified in the SARAO (South African Radio Astronomy Observatory) MeerKAT 1.3 GHz Galactic Plane Survey (SMGPS). We extract 933 filaments across the survey area, 803 of which (~86%) are associated with extended radio structures (e.g. supernova remnants and HII regions), whilst 130 (~14%) are largely isolated. We classify filaments as thermal or non-thermal via their associated mid-infrared emission and find 77/130 (~59%) of the isolated sources are likely to be non-thermal, and are therefore excellent candidates for the first isolated, non-thermal radio filaments observed outside of the Galactic Centre (GC). Comparing the morphological properties of these non-thermal candidates to the non-thermal filaments observed towards the GC we find the GC filaments are on the whole angularly narrower and shorter than those across the SMGPS, potentially an effect of distance. The SMGPS filaments have flux densities similar to those of the GC, however the distribution of the latter extends to higher flux densities. If the SMGPS filaments were closer than the GC population, it would imply a more energetic population of cosmic ray electrons in the GC. We find the filament position angles in the SMGPS are uniformly distributed, implying that the local magnetic field traced by the filaments does not follow the large-scale Galactic field. Finally, although we have clearly shown that filaments are not unique to the GC, the GC nevertheless has the highest density of filaments in the Milky Way. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.07852v1-abstract-full').style.display = 'none'; document.getElementById('2412.07852v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS, 18 pages, 15 figures, 2 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.01153">arXiv:2412.01153</a> <span> [<a href="https://arxiv.org/pdf/2412.01153">pdf</a>, <a href="https://arxiv.org/format/2412.01153">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/stae2571">10.1093/mnras/stae2571 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MeerKAT Pulsar Timing Array: The first search for gravitational waves with the MeerKAT radio telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Miles%2C+M+T">Matthew T. Miles</a>, <a href="/search/astro-ph?searchtype=author&query=Shannon%2C+R+M">Ryan M. Shannon</a>, <a href="/search/astro-ph?searchtype=author&query=Reardon%2C+D+J">Daniel J. Reardon</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">Matthew Bailes</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=Geyer%2C+M">Marisa Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Gitika%2C+P">Pratyasha Gitika</a>, <a href="/search/astro-ph?searchtype=author&query=Grunthal%2C+K">Kathrin Grunthal</a>, <a href="/search/astro-ph?searchtype=author&query=Keith%2C+M+J">Michael J. Keith</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">Michael Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Kulkarni%2C+A+D">Atharva D. Kulkarni</a>, <a href="/search/astro-ph?searchtype=author&query=Nathan%2C+R+S">Rowina S. Nathan</a>, <a href="/search/astro-ph?searchtype=author&query=Parthasarathy%2C+A">Aditya Parthasarathy</a>, <a href="/search/astro-ph?searchtype=author&query=Singha%2C+J">Jaikhomba Singha</a>, <a href="/search/astro-ph?searchtype=author&query=Theureau%2C+G">Gilles Theureau</a>, <a href="/search/astro-ph?searchtype=author&query=Thrane%2C+E">Eric Thrane</a>, <a href="/search/astro-ph?searchtype=author&query=Abbate%2C+F">Federico Abbate</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">Sarah Buchner</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=Camilo%2C+F">Fernando Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Moreschi%2C+B+E">Beatrice E. Moreschi</a>, <a href="/search/astro-ph?searchtype=author&query=Shaifullah%2C+G">Golam Shaifullah</a>, <a href="/search/astro-ph?searchtype=author&query=Shamohammadi%2C+M">Mohsen Shamohammadi</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">Andrea Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">Vivek 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="2412.01153v1-abstract-short" style="display: inline;"> Pulsar Timing Arrays search for nanohertz-frequency gravitational waves by regularly observing ensembles of millisecond pulsars over many years to look for correlated timing residuals. Recently the first evidence for a stochastic gravitational wave background has been presented by the major Arrays, with varying levels of significance ($\sim$2-4$蟽$). In this paper we present the results of backgrou… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.01153v1-abstract-full').style.display = 'inline'; document.getElementById('2412.01153v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.01153v1-abstract-full" style="display: none;"> Pulsar Timing Arrays search for nanohertz-frequency gravitational waves by regularly observing ensembles of millisecond pulsars over many years to look for correlated timing residuals. Recently the first evidence for a stochastic gravitational wave background has been presented by the major Arrays, with varying levels of significance ($\sim$2-4$蟽$). In this paper we present the results of background searches with the MeerKAT Pulsar Timing Array. Although of limited duration (4.5 yr), the $\sim$ 250,000 arrival times with a median error of just $3 渭$s on 83 pulsars make it very sensitive to spatial correlations. Detection of a gravitational wave background requires careful modelling of noise processes to ensure that any correlations represent a fit to the underlying background and not other misspecified processes. Under different assumptions about noise processes we can produce either what appear to be compelling Hellings-Downs correlations of high significance (3-3.4$蟽$) with a spectrum close to that which is predicted, or surprisingly, under slightly different assumptions, ones that are insignificant. This appears to be related to the fact that many of the highest precision MeerKAT Pulsar Timing Array pulsars are in close proximity and dominate the detection statistics. The sky-averaged characteristic strain amplitude of the correlated signal in our most significant model is $h_{c, {\rm yr}} = 7.5^{+0.8}_{-0.9} \times 10^{-15}$ measured at a spectral index of $伪=-0.26$, decreasing to $h_{c, {\rm yr}} = 4.8^{+0.8}_{-0.9} \times 10^{-15}$ when assessed at the predicted $伪=-2/3$. These data will be valuable as the International Pulsar Timing Array project explores the significance of gravitational wave detections and their dependence on the assumed noise models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.01153v1-abstract-full').style.display = 'none'; document.getElementById('2412.01153v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.01148">arXiv:2412.01148</a> <span> [<a href="https://arxiv.org/pdf/2412.01148">pdf</a>, <a href="https://arxiv.org/format/2412.01148">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/stae2572">10.1093/mnras/stae2572 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MeerKAT Pulsar Timing Array: The $4.5$-year data release and the noise and stochastic signals of the millisecond pulsar population </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Miles%2C+M+T">Matthew T. Miles</a>, <a href="/search/astro-ph?searchtype=author&query=Shannon%2C+R+M">Ryan M. Shannon</a>, <a href="/search/astro-ph?searchtype=author&query=Reardon%2C+D+J">Daniel J. Reardon</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">Matthew Bailes</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=Geyer%2C+M">Marisa Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Gitika%2C+P">Pratyasha Gitika</a>, <a href="/search/astro-ph?searchtype=author&query=Grunthal%2C+K">Kathrin Grunthal</a>, <a href="/search/astro-ph?searchtype=author&query=Keith%2C+M+J">Michael J. Keith</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">Michael Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Kulkarni%2C+A+D">Atharva D. Kulkarni</a>, <a href="/search/astro-ph?searchtype=author&query=Nathan%2C+R+S">Rowina S. Nathan</a>, <a href="/search/astro-ph?searchtype=author&query=Parthasarathy%2C+A">Aditya Parthasarathy</a>, <a href="/search/astro-ph?searchtype=author&query=Porayko%2C+N+K">Nataliya K. Porayko</a>, <a href="/search/astro-ph?searchtype=author&query=Singha%2C+J">Jaikhomba Singha</a>, <a href="/search/astro-ph?searchtype=author&query=Theureau%2C+G">Gilles Theureau</a>, <a href="/search/astro-ph?searchtype=author&query=Abbate%2C+F">Federico Abbate</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">Sarah Buchner</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=Camilo%2C+F">Fernando Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Moreschi%2C+B+E">Beatrice E. Moreschi</a>, <a href="/search/astro-ph?searchtype=author&query=Shaifullah%2C+G">Golam Shaifullah</a>, <a href="/search/astro-ph?searchtype=author&query=Shamohammadi%2C+M">Mohsen Shamohammadi</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">Vivek 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="2412.01148v1-abstract-short" style="display: inline;"> Pulsar timing arrays are ensembles of regularly observed millisecond pulsars timed to high precision. Each pulsar in an array could be affected by a suite of noise processes, most of which are astrophysically motivated. Analysing them carefully can be used to understand these physical processes. However, the primary purpose of these experiments is to detect signals that are common to all pulsars,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.01148v1-abstract-full').style.display = 'inline'; document.getElementById('2412.01148v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.01148v1-abstract-full" style="display: none;"> Pulsar timing arrays are ensembles of regularly observed millisecond pulsars timed to high precision. Each pulsar in an array could be affected by a suite of noise processes, most of which are astrophysically motivated. Analysing them carefully can be used to understand these physical processes. However, the primary purpose of these experiments is to detect signals that are common to all pulsars, in particular signals associated with a stochastic gravitational wave background. To detect this, it is paramount to appropriately characterise other signals that may otherwise impact array sensitivity or cause a spurious detection. Here we describe the second data release and first detailed noise analysis of the pulsars in the MeerKAT Pulsar Timing Array, comprising high-cadence and high-precision observations of $83$ millisecond pulsars over $4.5$ years. We use this analysis to search for a common signal in the data, finding a process with an amplitude of $\log_{10}\mathrm{A_{CURN}} = -14.25^{+0.21}_{-0.36}$ and spectral index $纬_\mathrm{CURN} = 3.60^{+1.31}_{-0.89}$. Fixing the spectral index at the value predicted for a background produced by the inspiral of binary supermassive black holes, we measure the amplitude to be $\log_{10}\mathrm{A_{CURN}} = -14.28^{+0.21}_{-0.21}$ at a significance expressed as a Bayes factor of $\ln(\mathcal{B}) = 4.46$. Under both assumptions, the amplitude that we recover is larger than those reported by other PTA experiments. We use the results of this analysis to forecast our sensitivity to a gravitational wave background possessing the spectral properties of the common signal we have measured. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.01148v1-abstract-full').style.display = 'none'; document.getElementById('2412.01148v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.21390">arXiv:2410.21390</a> <span> [<a href="https://arxiv.org/pdf/2410.21390">pdf</a>, <a href="https://arxiv.org/format/2410.21390">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> <p class="title is-5 mathjax"> Bow Shock and Local Bubble Plasma Unveiled by the Scintillating Millisecond Pulsar J0437$-$4715 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Reardon%2C+D+J">Daniel J. Reardon</a>, <a href="/search/astro-ph?searchtype=author&query=Main%2C+R">Robert Main</a>, <a href="/search/astro-ph?searchtype=author&query=Ocker%2C+S+K">Stella Koch Ocker</a>, <a href="/search/astro-ph?searchtype=author&query=Shannon%2C+R+M">Ryan M. Shannon</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">Matthew Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">Fernando Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Geyer%2C+M">Marisa Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Jameson%2C+A">Andrew Jameson</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">Michael Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Parthasarathy%2C+A">Aditya Parthasarathy</a>, <a href="/search/astro-ph?searchtype=author&query=Spiewak%2C+R">Ren茅e Spiewak</a>, <a href="/search/astro-ph?searchtype=author&query=van+Straten%2C+W">Willem van Straten</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">Vivek 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="2410.21390v1-abstract-short" style="display: inline;"> The interstellar medium of the Milky Way contains turbulent plasma with structures driven by energetic processes that fuel star formation and shape the evolution of our Galaxy. Radio waves from pulsars are scattered off the small (au-scale and below) structures, resulting in frequency-dependent interference patterns that are modulated in time because of the relative motions of the pulsar, Earth, a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.21390v1-abstract-full').style.display = 'inline'; document.getElementById('2410.21390v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.21390v1-abstract-full" style="display: none;"> The interstellar medium of the Milky Way contains turbulent plasma with structures driven by energetic processes that fuel star formation and shape the evolution of our Galaxy. Radio waves from pulsars are scattered off the small (au-scale and below) structures, resulting in frequency-dependent interference patterns that are modulated in time because of the relative motions of the pulsar, Earth, and plasma. Power spectral analyses of these patterns show parabolic arcs with curvatures that encode the locations and kinematics of individual structures. Here we report the discovery of at least 25 distinct plasma structures in the direction of the brilliant millisecond pulsar, PSR J0437$-$4715, in observations obtained with the MeerKAT radio telescope. Four arcs reveal structures within 5000 au of the pulsar, from a series of shocks induced as the pulsar and its wind interact with the ambient insterstellar medium. The measured radial distance and velocity of the main shock allows us to solve the shock geometry and space velocity of the pulsar in three dimensions, while the velocity of another structure unexpectedly indicates a back flow from the direction of the shock or pulsar-wind tail. The remaining 21 arcs represent a surprising abundance of structures sustained by turbulence within the Local Bubble -- a region of the interstellar medium thought to be depleted of gas by a series of supernova explosions about 14 Myr ago. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.21390v1-abstract-full').style.display = 'none'; document.getElementById('2410.21390v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 October, 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">46 pages, 10 figures, 1 table, submitted to Nature Astronomy</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.12510">arXiv:2410.12510</a> <span> [<a href="https://arxiv.org/pdf/2410.12510">pdf</a>, <a href="https://arxiv.org/format/2410.12510">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="Plasma Physics">physics.plasm-ph</span> </div> </div> <p class="title is-5 mathjax"> MeerKAT observations of pair-plasma induced birefringence in the double pulsar eclipses </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lower%2C+M+E">M. E. Lower</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+S">S. Johnston</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=Wex%2C+N">N. Wex</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=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Oswald%2C+L+S">L. S. Oswald</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=Serylak%2C+M">M. Serylak</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="2410.12510v1-abstract-short" style="display: inline;"> PSR J0737$-$3039A/B is unique among double neutron star systems. Its near-perfect edge-on orbit causes the fast spinning pulsar A to be eclipsed by the magnetic field of the slow spinning pulsar B. Using high-sensitivity MeerKAT radio observations combined with updated constraints on the system geometry, we studied the impact of these eclipses on the incident polarization properties of pulsar A. A… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.12510v1-abstract-full').style.display = 'inline'; document.getElementById('2410.12510v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.12510v1-abstract-full" style="display: none;"> PSR J0737$-$3039A/B is unique among double neutron star systems. Its near-perfect edge-on orbit causes the fast spinning pulsar A to be eclipsed by the magnetic field of the slow spinning pulsar B. Using high-sensitivity MeerKAT radio observations combined with updated constraints on the system geometry, we studied the impact of these eclipses on the incident polarization properties of pulsar A. Averaging light curves together after correcting for the rotation of pulsar B revealed enormous amounts of circular polarization and rapid changes in the linear polarization position angle, which occur at phases where emission from pulsar A is partially transmitted through the magnetosphere of pulsar B. These behaviours confirm that the eclipse mechanism is the result of synchrotron absorption in a relativistic pair-plasma confined to the closed-field region of pulsar B's truncated dipolar magnetic field. We demonstrate that changes in circular polarization handedness throughout the eclipses are directly tied to the average line of sight magnetic field direction of pulsar B, from which we unambiguously determine the complete magnetic and viewing geometry of the pulsar. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.12510v1-abstract-full').style.display = 'none'; document.getElementById('2410.12510v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 October, 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">8 pages, 6 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/2409.16607">arXiv:2409.16607</a> <span> [<a href="https://arxiv.org/pdf/2409.16607">pdf</a>, <a href="https://arxiv.org/format/2409.16607">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Supernova Remnant Candidates Discovered by the SARAO MeerKAT Galactic Plane Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+L+D">L. D. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Faerber%2C+T">Timothy Faerber</a>, <a href="/search/astro-ph?searchtype=author&query=Bietenholz%2C+M">M. Bietenholz</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Chibueze%2C+J+O">J. O. Chibueze</a>, <a href="/search/astro-ph?searchtype=author&query=Cotton%2C+W+D">W. D. Cotton</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Rigby%2C+A">A. Rigby</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+M+A">M. A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Trigilio%2C+C">C. Trigilio</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+G+M">G. M. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.16607v1-abstract-short" style="display: inline;"> Context. Sensitive radio continuum data could remove the difference between the number of known supernova remnants (SNRs) in the Galaxy compared to that expected, but due to confusion in the Galactic plane, faint SNRs can be challenging to distinguish from brighter HII regions and filamentary radio emission. Aims. We wish to exploit new SARAO MeerKAT 1.3 GHz Galactic Plane Survey (SMGPS) radio con… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.16607v1-abstract-full').style.display = 'inline'; document.getElementById('2409.16607v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.16607v1-abstract-full" style="display: none;"> Context. Sensitive radio continuum data could remove the difference between the number of known supernova remnants (SNRs) in the Galaxy compared to that expected, but due to confusion in the Galactic plane, faint SNRs can be challenging to distinguish from brighter HII regions and filamentary radio emission. Aims. We wish to exploit new SARAO MeerKAT 1.3 GHz Galactic Plane Survey (SMGPS) radio continuum data, which covers $251掳\le l \le 358掳$ and $2掳\le l \le 61掳$ at $|b|\le 1.5掳$, to search for SNR candidates in the Milky Way disk. Methods. We also use MIR data from the Spitzer GLIMPSE, Spitzer MIPSGAL, and WISE surveys to help identify SNR candidates. The identified SNR candidate are sources of extended radio continuum emission that lack MIR counterparts, are not known as HII regions in the WISE Catalog of Galactic HII Regions, and are not known previously as SNRs Results. We locate 237 new Galactic SNR candidates in the SMGPS data. We also identify and confirm the expected radio morphology for 201 objects listed in the literature as being SNRs and 130 previously-identified SNR candidates. The known and candidate SNRs have similar spatial distributions and angular sizes. Conclusions. The SMGPS data allowed us to identify a large population of SNR candidates that can be confirmed as true SNRs using radio polarization measurements or by deriving radio spectral indices. If the 237 candidates are confirmed as true SNRs, it would approximately double the number of known Galactic SNRs in the survey area, alleviating much of the difference between the known and expected populations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.16607v1-abstract-full').style.display = 'none'; document.getElementById('2409.16607v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by A&A. Images and FITS files of each source can be found here: https://doi.org/10.48479/0n8c-5q84</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.11099">arXiv:2408.11099</a> <span> [<a href="https://arxiv.org/pdf/2408.11099">pdf</a>, <a href="https://arxiv.org/format/2408.11099">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"> A GTC spectroscopic study of three spider pulsar companions: line-based temperatures, a new face-on redback, and improved mass constraints </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Simpson%2C+J+A">Jordan A. Simpson</a>, <a href="/search/astro-ph?searchtype=author&query=Linares%2C+M">Manuel Linares</a>, <a href="/search/astro-ph?searchtype=author&query=Casares%2C+J">Jorge Casares</a>, <a href="/search/astro-ph?searchtype=author&query=Shahbaz%2C+T">Tariq Shahbaz</a>, <a href="/search/astro-ph?searchtype=author&query=Sen%2C+B">Bidisha Sen</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">Fernando 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="2408.11099v1-abstract-short" style="display: inline;"> We present GTC-OSIRIS phase-resolved optical spectroscopy of three compact binary MSPs, or `spiders': PSR J1048+2339, PSR J1810+1744, and (for the first time) PSR J1908+2105. For the companion in each system, the temperature is traced throughout its orbit, and radial velocities are measured. The radial velocities are found to vary with the absorption features used when measuring them, resulting in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.11099v1-abstract-full').style.display = 'inline'; document.getElementById('2408.11099v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.11099v1-abstract-full" style="display: none;"> We present GTC-OSIRIS phase-resolved optical spectroscopy of three compact binary MSPs, or `spiders': PSR J1048+2339, PSR J1810+1744, and (for the first time) PSR J1908+2105. For the companion in each system, the temperature is traced throughout its orbit, and radial velocities are measured. The radial velocities are found to vary with the absorption features used when measuring them, resulting in a lower radial velocity curve semi-amplitude measured from the day side of two of the systems when compared to the night: for J1048 ($K_\mathrm{day} = 344 \pm 4$ km s$^{-1}$, $K_\mathrm{night} = 372 \pm 3$ km s$^{-1}$) and, tentatively, for J1810 ($K_\mathrm{day} = 448 \pm 19$ km s$^{-1}$, $K_\mathrm{night} = 491 \pm 32$ km s$^{-1}$). With existing inclination constraints, this gives the neutron star (NS) and companion masses $M_\mathrm{NS} = 1.50 - 2.04$ $M_\odot$ and $M_2 = 0.32 - 0.40$ $M_\odot$ for J1048, and $M_\mathrm{NS} > 1.7$ $M_\odot$ and $M_2 = 0.05 - 0.08$ $M_\odot$ for J1810. For J1908, we find an upper limit of $K_2 < 32$ km s$^{-1}$, which constrains its mass ratio $q = M_2 / M_\mathrm{NS} > 0.55$ and inclination $i < 6.0^\circ$, revealing the previously misunderstood system to be the highest mass ratio, lowest inclination redback yet. This raises questions for the origins of its substantial radio eclipses. Additionally, we find evidence of asymmetric heating in J1048 and J1810, and signs of metal enrichment in J1908. We also explore the impact of inclination on spectroscopic temperatures, and demonstrate that the temperature measured at quadrature ($蠁= 0.25, 0.75$) is essentially independent of inclination, and thus can provide additional constraints on photometric modelling. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.11099v1-abstract-full').style.display = 'none'; document.getElementById('2408.11099v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to MNRAS. 18 pages, 19 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.07727">arXiv:2408.07727</a> <span> [<a href="https://arxiv.org/pdf/2408.07727">pdf</a>, <a href="https://arxiv.org/ps/2408.07727">ps</a>, <a href="https://arxiv.org/format/2408.07727">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202450766">10.1051/0004-6361/202450766 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MeerKAT reveals a ghostly thermal radio ring towards the Galactic Centre </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Filipovic%2C+M+D">M. D. Filipovic</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Cotton%2C+W+D">W. D. Cotton</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C">C. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Cerrigone%2C+L">L. Cerrigone</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+S">S. Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">A. M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Jarrett%2C+T">T. Jarrett</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B">B. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Lazarevic%2C+S">S. Lazarevic</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Lundqvist%2C+P">P. Lundqvist</a>, <a href="/search/astro-ph?searchtype=author&query=Mackey%2C+J">J. Mackey</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">R. P. Norris</a>, <a href="/search/astro-ph?searchtype=author&query=Payne%2C+J">J. Payne</a>, <a href="/search/astro-ph?searchtype=author&query=Rowell%2C+G">G. Rowell</a>, <a href="/search/astro-ph?searchtype=author&query=Riggi%2C+S">S. Riggi</a>, <a href="/search/astro-ph?searchtype=author&query=Rizzo%2C+J+R">J. R. Rizzo</a>, <a href="/search/astro-ph?searchtype=author&query=Ruggeri%2C+A+C">A. C. Ruggeri</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.07727v1-abstract-short" style="display: inline;"> We present the serendipitous discovery of a new radio-continuum ring-like object nicknamed Kyklos (J1802-3353), with MeerKAT UHF and L-band observations. The radio ring, which resembles the recently discovered odd radio circles (ORCs), has a diameter of 80 arcsec and is located just 6 deg from the Galactic plane. However, Kyklos exhibits an atypical thermal radio-continuum spectrum (伪 = -0.1 +/- 0… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.07727v1-abstract-full').style.display = 'inline'; document.getElementById('2408.07727v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.07727v1-abstract-full" style="display: none;"> We present the serendipitous discovery of a new radio-continuum ring-like object nicknamed Kyklos (J1802-3353), with MeerKAT UHF and L-band observations. The radio ring, which resembles the recently discovered odd radio circles (ORCs), has a diameter of 80 arcsec and is located just 6 deg from the Galactic plane. However, Kyklos exhibits an atypical thermal radio-continuum spectrum (伪 = -0.1 +/- 0.3), which led us to explore different possible formation scenarios. We concluded that a circumstellar shell around an evolved massive star, possibly a Wolf-Rayet, is the most convincing explanation with the present data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.07727v1-abstract-full').style.display = 'none'; document.getElementById('2408.07727v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 5 figures, accepted in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.15563">arXiv:2407.15563</a> <span> [<a href="https://arxiv.org/pdf/2407.15563">pdf</a>, <a href="https://arxiv.org/format/2407.15563">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"> Study of consecutive eclipses of pulsar J0024$-$7204O </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=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=Buchner%2C+S">S. Buchner</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=Zhang%2C+L">L. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Corongiu%2C+A">A. Corongiu</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</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="2407.15563v1-abstract-short" style="display: inline;"> The eclipses seen in the radio emission of some pulsars can be invaluable to study the properties of the material from the companion stripped away by the pulsar. We present a study of six consecutive eclipses of PSR J0024-7204O in the globular cluster 47 Tucanae as seen by the MeerKAT radio telescope in the UHF (544-1088 MHz) band. A high scintillation state boosted the signal during one of the or… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.15563v1-abstract-full').style.display = 'inline'; document.getElementById('2407.15563v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.15563v1-abstract-full" style="display: none;"> The eclipses seen in the radio emission of some pulsars can be invaluable to study the properties of the material from the companion stripped away by the pulsar. We present a study of six consecutive eclipses of PSR J0024-7204O in the globular cluster 47 Tucanae as seen by the MeerKAT radio telescope in the UHF (544-1088 MHz) band. A high scintillation state boosted the signal during one of the orbits and allowed a detailed study of the eclipse properties. We measure significant dispersion measure (DM) variations and detect strong scattering that seems to be the dominating mechanism of the eclipses at these frequencies. A complete drop in the linear polarization together with a small increase in the rotation measure suggests the presence of a magnetic field of $\sim 2$ mG. The study of multiple eclipses allowed us to measure difference in the lengths of the eclipses and DM differences of $\sim 0.01$ pc cm$^{-3}$ in consecutive orbits. One orbit in particular shows a delay in recovery of the linear polarization and a visible delay in the arrival of the pulses caused by a stronger scattering event. We suggest that these are caused by a higher variance of density fluctuations during the event. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.15563v1-abstract-full').style.display = 'none'; document.getElementById('2407.15563v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 July, 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">14 pages, 8 figures, 9 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/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/2407.01773">arXiv:2407.01773</a> <span> [<a href="https://arxiv.org/pdf/2407.01773">pdf</a>, <a href="https://arxiv.org/format/2407.01773">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> An Image-Based Search for Pulsar Candidates in the MeerKAT Bulge Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Frail%2C+D+A">Dale A. Frail</a>, <a href="/search/astro-ph?searchtype=author&query=Polisensky%2C+E">Emil Polisensky</a>, <a href="/search/astro-ph?searchtype=author&query=Hyman%2C+S+D">Scott D. Hyman</a>, <a href="/search/astro-ph?searchtype=author&query=Cotton%2C+W+M">W. M. Cotton</a>, <a href="/search/astro-ph?searchtype=author&query=Kassim%2C+N+E">Namir E. Kassim</a>, <a href="/search/astro-ph?searchtype=author&query=Silverstein%2C+M+L">Michele L. Silverstein</a>, <a href="/search/astro-ph?searchtype=author&query=Sengar%2C+R">Rahul Sengar</a>, <a href="/search/astro-ph?searchtype=author&query=Kaplan%2C+D+L">David L. Kaplan</a>, <a href="/search/astro-ph?searchtype=author&query=Calore%2C+F">Francesca Calore</a>, <a href="/search/astro-ph?searchtype=author&query=Berteaud%2C+J">Joanna Berteaud</a>, <a href="/search/astro-ph?searchtype=author&query=Clavel%2C+M">Maica Clavel</a>, <a href="/search/astro-ph?searchtype=author&query=Geyer%2C+M">Marisa Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Legodi%2C+S">Samuel Legodi</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V">Vasaant Krishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">Sarah Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">Fernando 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="2407.01773v2-abstract-short" style="display: inline;"> We report on the results of an image-based search for pulsar candidates toward the Galactic bulge. We used mosaic images from the MeerKAT radio telescope, that were taken as part of a 173 deg**2 survey of the bulge and Galactic center of our Galaxy at L band (856-1712 MHz) in all four Stokes I, Q, U and V. The image root-mean-square noise levels of 12-17 uJy/ba represent a significant increase in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.01773v2-abstract-full').style.display = 'inline'; document.getElementById('2407.01773v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.01773v2-abstract-full" style="display: none;"> We report on the results of an image-based search for pulsar candidates toward the Galactic bulge. We used mosaic images from the MeerKAT radio telescope, that were taken as part of a 173 deg**2 survey of the bulge and Galactic center of our Galaxy at L band (856-1712 MHz) in all four Stokes I, Q, U and V. The image root-mean-square noise levels of 12-17 uJy/ba represent a significant increase in sensitivity over past image-based pulsar searches. Our primary search criterion was circular polarization, but we used other criteria including linear polarization, in-band spectral index, compactness, variability and multi-wavelength counterparts to select pulsar candidates. We first demonstrate the efficacy of this technique by searching for polarized emission from known pulsars, and comparing our results with measurements from the literature. Our search resulted in a sample of 75 polarized pulsar candidates. Bright stars or young stellar objects were associated with 28 of these sources, including a small sample of highly polarized dwarf stars with pulsar-like steep spectra. Comparing the properties of this sample with the known pulsars, we identified 30 compelling candidates for pulsation follow-up, including two sources with both strong circular and linear polarization. The remaining 17 sources are either pulsars or stars, but we cannot rule out an extragalactic origin or image artifacts among the brighter, flat spectrum objects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.01773v2-abstract-full').style.display = 'none'; document.getElementById('2407.01773v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 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">28 pages, 10 figures, 6 tables. ApJ, 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/2406.04674">arXiv:2406.04674</a> <span> [<a href="https://arxiv.org/pdf/2406.04674">pdf</a>, <a href="https://arxiv.org/format/2406.04674">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"> VLBA Astrometry of the Fastest-spinning Magnetar Swift J1818.0-1607: A Large Trigonometric Distance & A Small Transverse Velocity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ding%2C+H">Hao Ding</a>, <a href="/search/astro-ph?searchtype=author&query=Lower%2C+M+E">Marcus E. Lower</a>, <a href="/search/astro-ph?searchtype=author&query=Deller%2C+A+T">Adam T. Deller</a>, <a href="/search/astro-ph?searchtype=author&query=Shannon%2C+R+M">Ryan M. Shannon</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">Fernando Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Sarkissian%2C+J">John Sarkissian</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="2406.04674v1-abstract-short" style="display: inline;"> In addition to being the most magnetic objects in the known universe, magnetars are the only objects observed to generate fast-radio-burst-like emissions. The formation mechanism of magnetars is still highly debated, and may potentially be probed with the magnetar velocity distribution. We carried out a 3-year-long astrometric campaign on Swift J1818.0-1607 -- the fastest-spinning magnetar, using… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.04674v1-abstract-full').style.display = 'inline'; document.getElementById('2406.04674v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.04674v1-abstract-full" style="display: none;"> In addition to being the most magnetic objects in the known universe, magnetars are the only objects observed to generate fast-radio-burst-like emissions. The formation mechanism of magnetars is still highly debated, and may potentially be probed with the magnetar velocity distribution. We carried out a 3-year-long astrometric campaign on Swift J1818.0-1607 -- the fastest-spinning magnetar, using the Very Long Baseline Array. After applying the phase-calibrating 1D interpolation strategy, we obtained a small proper motion of 8.5 $\mathrm{mas~yr^{-1}}$ magnitude, and a parallax of $0.12\pm0.02$ mas (uncertainties at $1\,蟽$ confidence throughout the Letter) for Swift J1818.0-1607. The latter is the second magnetar parallax, and is among the smallest neutron star parallaxes ever determined. From the parallax, we derived the distance $9.4^{+2.0}_{-1.6}$ kpc, which locates Swift J1818.0-1607 at the far side of the Galactic central region. Combined with the distance, the small proper motion leads to a transverse peculiar velocity $v_\perp=48^{+50}_{-16}$ $\mathrm{km~s^{-1}}$ -- a new lower limit to magnetar $v_\perp$. Incorporating previous $v_\perp$ estimates of seven other magnetars, we acquired $v_\perp=149^{+132}_{-68}$ $\mathrm{km~s^{-1}}$ for the sample of astrometrically studied magnetars, corresponding to the three-dimensional space velocity $\sim190^{+168}_{-87}$ $\mathrm{km~s^{-1}}$, smaller than the average level of young pulsars. Additionally, we found that the magnetar velocity sample does not follow the unimodal young pulsar velocity distribution reported by Hobbs et al. at $>2\,蟽$ confidence, while loosely agreeing with more recent bimodal young pulsar velocity distributions derived from relatively small samples of quality astrometric determinations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.04674v1-abstract-full').style.display = 'none'; document.getElementById('2406.04674v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 4 figures, 4 tables, accepted for publication in ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.15629">arXiv:2405.15629</a> <span> [<a href="https://arxiv.org/pdf/2405.15629">pdf</a>, <a href="https://arxiv.org/format/2405.15629">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> HI Galaxy Signatures in the SARAO MeerKAT Galactic Plane Survey -- III. Unveiling the obscured part of the Vela Supercluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rajohnson%2C+S+H+A">Sambatriniaina H. A. Rajohnson</a>, <a href="/search/astro-ph?searchtype=author&query=Kraan-Korteweg%2C+R+C">Ren茅e C. Kraan-Korteweg</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+H">Hao Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Frank%2C+B+S">Bradley S. Frank</a>, <a href="/search/astro-ph?searchtype=author&query=Steyn%2C+N">Nadia Steyn</a>, <a href="/search/astro-ph?searchtype=author&query=Kurapati%2C+S">Sushma Kurapati</a>, <a href="/search/astro-ph?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/astro-ph?searchtype=author&query=Staveley-Smith%2C+L">Lister Staveley-Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Serra%2C+P">Paolo Serra</a>, <a href="/search/astro-ph?searchtype=author&query=Goedhart%2C+S">Sharmila Goedhart</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">Fernando 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="2405.15629v1-abstract-short" style="display: inline;"> We conducted a search for HI emission of the gas-rich galaxies in the Vela region ($260^{\circ} \leq \ell \leq 290^{\circ}, -2^{\circ} \leq b \leq 1^{\circ}$) to explore the Vela Supercluster (VSCL) at $V_\mathrm{hel} \sim 18000$ km s$^{-1}$, largely obscured by Galactic dust. Within the mostly RFI-free band ($250 < V_\mathrm{hel} < 25000$ km s$^{-1}$) of MeerKAT, the analysis focuses on $157$ hex… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.15629v1-abstract-full').style.display = 'inline'; document.getElementById('2405.15629v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.15629v1-abstract-full" style="display: none;"> We conducted a search for HI emission of the gas-rich galaxies in the Vela region ($260^{\circ} \leq \ell \leq 290^{\circ}, -2^{\circ} \leq b \leq 1^{\circ}$) to explore the Vela Supercluster (VSCL) at $V_\mathrm{hel} \sim 18000$ km s$^{-1}$, largely obscured by Galactic dust. Within the mostly RFI-free band ($250 < V_\mathrm{hel} < 25000$ km s$^{-1}$) of MeerKAT, the analysis focuses on $157$ hexagonally distributed pointings extracted from the SARAO MeerKAT Galactic Plane Survey located in the Vela region (Vela$-$SMGPS). These were combined into 10 contiguous mosaics, covering a ${\sim}90$ deg$^2$ area. Among the $843$ HI detected sources, 39 were previously discovered in the Parkes HIZOA survey ($V_\mathrm{hel} < 12000$ km s$^{-1}$; rms $\sim 6$ mJy beam$^{-1}$). With the improved rms level of the Vela$-$SMGPS, i.e., $0.29 - 0.56$ mJy beam$^{-1}$, our study unveils nearly 12 times more detections (471 candidates) in that same velocity range. We furthermore could identify $187$ galaxy candidates with an HI mass limit reaching $\log (M_{\rm HI}/\rm M_{\odot}) = 9.44$ in the VSCL velocity range $V_\mathrm{hel} \sim 19500 \pm 3500$ km s$^{-1}$. We find indications of two wall-like overdensities that confirm the original suspicion that these walls intersect at low latitudes around longitudes of $\ell \sim 272^{\circ} - 278^{\circ}$. We also find a strong signature most likely associated with the Hydra/Antlia extension and evidence of a previously unknown narrow filament at $V_\mathrm{hel} \sim 12000$ km s$^{-1}$. This paper demonstrates the efficiency of systematic HI surveys with the SKA precursor MeerKAT, even in the most obscured part of the Zone of Avoidance (ZOA). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.15629v1-abstract-full').style.display = 'none'; document.getElementById('2405.15629v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS, this version contains the full catalogue of detections</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.09366">arXiv:2402.09366</a> <span> [<a href="https://arxiv.org/pdf/2402.09366">pdf</a>, <a href="https://arxiv.org/format/2402.09366">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/ad2994">10.3847/1538-4357/ad2994 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A 350-MHz Green Bank Telescope Survey of Unassociated Fermi LAT Sources: Discovery and Timing of Ten Millisecond Pulsars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bangale%2C+P">P. Bangale</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharyya%2C+B">B. Bhattacharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</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=Cognard%2C+I">I. Cognard</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=Ferrara%2C+E+C">E. C. Ferrara</a>, <a href="/search/astro-ph?searchtype=author&query=Gentile%2C+P">P. Gentile</a>, <a href="/search/astro-ph?searchtype=author&query=Guillemot%2C+L">L. Guillemot</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=Johnson%2C+T+J">T. J. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Kerr%2C+M">M. Kerr</a>, <a href="/search/astro-ph?searchtype=author&query=McLaughlin%2C+M+A">M. A. McLaughlin</a>, <a href="/search/astro-ph?searchtype=author&query=Nieder%2C+L">L. Nieder</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=Ray%2C+P+S">P. S. Ray</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts%2C+M+S+E">M. S. E. Roberts</a>, <a href="/search/astro-ph?searchtype=author&query=Roy%2C+J">J. Roy</a>, <a href="/search/astro-ph?searchtype=author&query=Sanpa-Arsa%2C+S">S. Sanpa-Arsa</a>, <a href="/search/astro-ph?searchtype=author&query=Theureau%2C+G">G. Theureau</a>, <a href="/search/astro-ph?searchtype=author&query=Wolff%2C+M+T">M. T. Wolff</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="2402.09366v1-abstract-short" style="display: inline;"> We have searched for radio pulsations towards 49 Fermi Large Area Telescope (LAT) 1FGL Catalog $纬$-ray sources using the Green Bank Telescope at 350 MHz. We detected 18 millisecond pulsars (MSPs) in blind searches of the data; 10 of these were discoveries unique to our survey. Sixteen are binaries, with eight having short orbital periods $P_B < 1$ day. No radio pulsations from young pulsars were d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.09366v1-abstract-full').style.display = 'inline'; document.getElementById('2402.09366v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.09366v1-abstract-full" style="display: none;"> We have searched for radio pulsations towards 49 Fermi Large Area Telescope (LAT) 1FGL Catalog $纬$-ray sources using the Green Bank Telescope at 350 MHz. We detected 18 millisecond pulsars (MSPs) in blind searches of the data; 10 of these were discoveries unique to our survey. Sixteen are binaries, with eight having short orbital periods $P_B < 1$ day. No radio pulsations from young pulsars were detected, although three targets are coincident with apparently radio-quiet $纬$-ray pulsars discovered in LAT data. Here, we give an overview of the survey and present radio and $纬$-ray timing results for the 10 MSPs discovered. These include the only isolated MSP discovered in our survey and six short-$P_B$ binary MSPs. Of these, three have very low-mass companions ($M_c$ $\ll$ 0.1M$_{\odot}$) and hence belong to the class of black widow pulsars. Two have more massive, non-degenerate companions with extensive radio eclipses and orbitally modulated X-ray emission consistent with the redback class. Significant $纬$-ray pulsations have been detected from nine of the discoveries. This survey and similar efforts suggest that the majority of Galactic $纬$-ray sources at high Galactic latitudes are either MSPs or relatively nearby non-recycled pulsars, with the latter having on average a much smaller radio/$纬$-ray beaming ratio as compared to MSPs. It also confirms that past surveys suffered from an observational bias against finding short-$P_B$ MSP systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.09366v1-abstract-full').style.display = 'none'; document.getElementById('2402.09366v1-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 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">Accepted for publication in ApJ (25 pages, 15 figues, 4 tables)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ, Vol 966, 20 pp. (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.11024">arXiv:2401.11024</a> <span> [<a href="https://arxiv.org/pdf/2401.11024">pdf</a>, <a href="https://arxiv.org/format/2401.11024">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The MeerKAT 1.3 GHz Survey of the Small Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cotton%2C+W">W. Cotton</a>, <a href="/search/astro-ph?searchtype=author&query=Filipovic%2C+M+D">M. D. Filipovic</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Indebetouw%2C+R">R. Indebetouw</a>, <a href="/search/astro-ph?searchtype=author&query=Alsaberi%2C+R+Z+E">R. Z. E. Alsaberi</a>, <a href="/search/astro-ph?searchtype=author&query=Anih%2C+J+O">J. O. Anih</a>, <a href="/search/astro-ph?searchtype=author&query=Baker%2C+M">M. Baker</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian%2C+T+.+S">T . S. Bastian</a>, <a href="/search/astro-ph?searchtype=author&query=Bojicic%2C+I">I. Bojicic</a>, <a href="/search/astro-ph?searchtype=author&query=Carli%2C+E">E. Carli</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+E+J">E. J. Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+S">S. Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/astro-ph?searchtype=author&query=Levin%2C+L">L. Levin</a>, <a href="/search/astro-ph?searchtype=author&query=Luken%2C+K">K. Luken</a>, <a href="/search/astro-ph?searchtype=author&query=Pennock%2C+C+.+M">C . M. Pennock</a>, <a href="/search/astro-ph?searchtype=author&query=Rajabpour%2C+N">N. Rajabpour</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=van+Loon%2C+J+T">J. Th. van Loon</a>, <a href="/search/astro-ph?searchtype=author&query=Zijlstra%2C+A+A">A. A. Zijlstra</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Geyer%2C+M">M. Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Goedhart%2C+S">S. Goedhart</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="2401.11024v1-abstract-short" style="display: inline;"> We present new radio continuum images and a source catalogue from the MeerKAT survey in the direction of the Small Magellanic Cloud (SMC). The observations, at a central frequency of 1.3 GHz across a bandwidth of 0.8 GHz, encompass a field of view ~7 x 7 degrees and result in images with resolution of 8 arcsec. The median broad-band Stokes I image Root Mean Squared noise value is ~11 microJy/beam.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.11024v1-abstract-full').style.display = 'inline'; document.getElementById('2401.11024v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.11024v1-abstract-full" style="display: none;"> We present new radio continuum images and a source catalogue from the MeerKAT survey in the direction of the Small Magellanic Cloud (SMC). The observations, at a central frequency of 1.3 GHz across a bandwidth of 0.8 GHz, encompass a field of view ~7 x 7 degrees and result in images with resolution of 8 arcsec. The median broad-band Stokes I image Root Mean Squared noise value is ~11 microJy/beam. The catalogue produced from these images contains 108,330 point sources and 517 compact extended sources. We also describe a UHF (544-1088 MHz) single pointing observation. We report the detection of a new confirmed Supernova Remnant (SNR) (MCSNR J0100-7211) with an X-ray magnetar at its centre and 10 new SNR candidates. This is in addition to the detection of 21 previously confirmed SNRs and two previously noted SNR candidates. Our new SNR candidates have typical surface brightness an order of magnitude below those previously known, and on the whole they are larger. The high sensitivity of the MeerKAT survey also enabled us to detect the bright end of the SMC Planetary Nebulae (PNe) sample - point-like radio emission is associated with 38 of 102 optically known PNe, of which 19 are new detections. Lastly, we present the detection of three foreground radio stars amidst 11 circularly polarised sources, and a few examples of morphologically interesting background radio galaxies from which the radio ring galaxy ESO 029-G034 may represent a new type of radio object. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.11024v1-abstract-full').style.display = 'none'; document.getElementById('2401.11024v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 January, 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">31 pages, 27 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/2401.06963">arXiv:2401.06963</a> <span> [<a href="https://arxiv.org/pdf/2401.06963">pdf</a>, <a href="https://arxiv.org/format/2401.06963">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"> MeerKAT Pulsar Timing Array parallaxes and proper motions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shamohammadi%2C+M">Mohsen Shamohammadi</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">Matthew Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Flynn%2C+C">Christopher Flynn</a>, <a href="/search/astro-ph?searchtype=author&query=Reardon%2C+D+J">Daniel J. Reardon</a>, <a href="/search/astro-ph?searchtype=author&query=Shannon%2C+R+M">Ryan M. Shannon</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">Sarah Buchner</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=Camilo%2C+F">Fernando Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Coronigu%2C+A">Alessandro Coronigu</a>, <a href="/search/astro-ph?searchtype=author&query=Geyer%2C+M">Marisa Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">Michael Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Miles%2C+M">Matthew Miles</a>, <a href="/search/astro-ph?searchtype=author&query=Spiewak%2C+R">Renee Spiewak</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="2401.06963v1-abstract-short" style="display: inline;"> We have determined positions, proper motions, and parallaxes of $77$ millisecond pulsars (MSPs) from $\sim3$ years of MeerKAT radio telescope observations. Our timing and noise analyses enable us to measure $35$ significant parallaxes ($12$ of them for the first time) and $69$ significant proper motions. Eight pulsars near the ecliptic have an accurate proper motion in ecliptic longitude only. PSR… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.06963v1-abstract-full').style.display = 'inline'; document.getElementById('2401.06963v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.06963v1-abstract-full" style="display: none;"> We have determined positions, proper motions, and parallaxes of $77$ millisecond pulsars (MSPs) from $\sim3$ years of MeerKAT radio telescope observations. Our timing and noise analyses enable us to measure $35$ significant parallaxes ($12$ of them for the first time) and $69$ significant proper motions. Eight pulsars near the ecliptic have an accurate proper motion in ecliptic longitude only. PSR~J0955$-$6150 has a good upper limit on its very small proper motion ($<$0.4 mas yr$^{-1}$). We used pulsars with accurate parallaxes to study the MSP velocities. This yields $39$ MSP transverse velocities, and combined with MSPs in the literature (excluding those in Globular Clusters) we analyse $66$ MSPs in total. We find that MSPs have, on average, much lower velocities than normal pulsars, with a mean transverse velocity of only $78(8)$ km s$^{-1}$ (MSPs) compared with $246(21)$ km s$^{-1}$ (normal pulsars). We found no statistical differences between the velocity distributions of isolated and binary millisecond pulsars. From Galactocentric cylindrical velocities of the MSPs, we derive 3-D velocity dispersions of $蟽_蟻$, $蟽_蠁$, $蟽_{z}$ = $63(11)$, $48(8)$, $19(3)$ km s$^{-1}$. We measure a mean asymmetric drift with amplitude $38(11)$ km s$^{-1}$, consistent with expectation for MSPs, given their velocity dispersions and ages. The MSP velocity distribution is consistent with binary evolution models that predict very few MSPs with velocities $>300$ km s$^{-1}$ and a mild anticorrelation of transverse velocity with orbital period. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.06963v1-abstract-full').style.display = 'none'; document.getElementById('2401.06963v1-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.12165">arXiv:2312.12165</a> <span> [<a href="https://arxiv.org/pdf/2312.12165">pdf</a>, <a href="https://arxiv.org/format/2312.12165">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> The RATT PARROT: serendipitous discovery of a peculiarly scintillating pulsar in MeerKAT imaging observations of the Great Saturn-Jupiter Conjunction of 2020. I. Dynamic imaging and data analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Smirnov%2C+O+M">O. M. Smirnov</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=Tasse%2C+C">C. Tasse</a>, <a href="/search/astro-ph?searchtype=author&query=Bester%2C+H+L">H. L. Bester</a>, <a href="/search/astro-ph?searchtype=author&query=Bignall%2C+H">H. Bignall</a>, <a href="/search/astro-ph?searchtype=author&query=Walker%2C+M+A">M. A. Walker</a>, <a href="/search/astro-ph?searchtype=author&query=Caleb%2C+M">M. Caleb</a>, <a href="/search/astro-ph?searchtype=author&query=Rajwade%2C+K+M">K. M. Rajwade</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Woudt%2C+P">P. Woudt</a>, <a href="/search/astro-ph?searchtype=author&query=Ivchenko%2C+M">M. Ivchenko</a>, <a href="/search/astro-ph?searchtype=author&query=Roth%2C+L">L. Roth</a>, <a href="/search/astro-ph?searchtype=author&query=Noordam%2C+J+E">J. E. Noordam</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="2312.12165v2-abstract-short" style="display: inline;"> We report on a radiopolarimetric observation of the Saturn-Jupiter Great Conjunction of 2020 using the MeerKAT L-band system, initially carried out for science verification purposes, which yielded a serendipitous discovery of a pulsar. The radiation belts of Jupiter are very bright and time variable: coupled with the sensitivity of MeerKAT, this necessitated development of dynamic imaging techniqu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.12165v2-abstract-full').style.display = 'inline'; document.getElementById('2312.12165v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.12165v2-abstract-full" style="display: none;"> We report on a radiopolarimetric observation of the Saturn-Jupiter Great Conjunction of 2020 using the MeerKAT L-band system, initially carried out for science verification purposes, which yielded a serendipitous discovery of a pulsar. The radiation belts of Jupiter are very bright and time variable: coupled with the sensitivity of MeerKAT, this necessitated development of dynamic imaging techniques, reported on in this work. We present a deep radio "movie" revealing Jupiter's rotating magnetosphere, a radio detection of Callisto, and numerous background radio galaxies. We also detect a bright radio transient in close vicinity to Saturn, lasting approximately 45 minutes. Follow-up deep imaging observations confirmed this as a faint compact variable radio source, and yielded detections of pulsed emission by the commensal MeerTRAP search engine, establishing the object's nature as a radio emitting neutron star, designated PSR J2009-2026. A further observation combining deep imaging with the PTUSE pulsar backend measured detailed dynamic spectra for the object. While qualitatively consistent with scintillation, the magnitude of the magnification events and the characteristic timescales are odd. We are tentatively designating this object a pulsar with anomalous refraction recurring on odd timescales (PARROT). As part of this investigation, we present a pipeline for detection of variable sources in imaging data, with dynamic spectra and lightcurves as the products, and compare dynamic spectra obtained from visibility data with those yielded by PTUSE. We discuss MeerKAT's capabilities and prospects for detecting more of such transients and variables. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.12165v2-abstract-full').style.display = 'none'; document.getElementById('2312.12165v2-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 17 figures, submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.07275">arXiv:2312.07275</a> <span> [<a href="https://arxiv.org/pdf/2312.07275">pdf</a>, <a href="https://arxiv.org/format/2312.07275">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The SARAO MeerKAT 1.3 GHz Galactic Plane Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Goedhart%2C+S">S. Goedhart</a>, <a href="/search/astro-ph?searchtype=author&query=Cotton%2C+W+D">W. D. Cotton</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+M+A">M. A. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Umana%2C+G">G. Umana</a>, <a href="/search/astro-ph?searchtype=author&query=Bietenholz%2C+M">M. Bietenholz</a>, <a href="/search/astro-ph?searchtype=author&query=Woudt%2C+P+A">P. A. Woudt</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+L+D">L. D. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Bordiu%2C+C">C. Bordiu</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+D+A+H">D. A. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Buemi%2C+C+S">C. S. Buemi</a>, <a href="/search/astro-ph?searchtype=author&query=Bufano%2C+F">F. Bufano</a>, <a href="/search/astro-ph?searchtype=author&query=Cavallaro%2C+F">F. Cavallaro</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+H">H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chibueze%2C+J+O">J. O. Chibueze</a>, <a href="/search/astro-ph?searchtype=author&query=Egbo%2C+D">D. Egbo</a>, <a href="/search/astro-ph?searchtype=author&query=Frank%2C+B+S">B. S. Frank</a>, <a href="/search/astro-ph?searchtype=author&query=Hoare%2C+M+G">M. G. Hoare</a>, <a href="/search/astro-ph?searchtype=author&query=Ingallinera%2C+A">A. Ingallinera</a>, <a href="/search/astro-ph?searchtype=author&query=Irabor%2C+T">T. Irabor</a>, <a href="/search/astro-ph?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/astro-ph?searchtype=author&query=Kurapati%2C+S">S. Kurapati</a>, <a href="/search/astro-ph?searchtype=author&query=Leto%2C+P">P. Leto</a>, <a href="/search/astro-ph?searchtype=author&query=Loru%2C+S">S. Loru</a>, <a href="/search/astro-ph?searchtype=author&query=Mutale%2C+M">M. Mutale</a> , et al. (105 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.07275v2-abstract-short" style="display: inline;"> We present the SARAO MeerKAT Galactic Plane Survey (SMGPS), a 1.3 GHz continuum survey of almost half of the Galactic Plane (251掳$\le l \le$ 358掳and 2掳$\le l \le$ 61掳at $|b| \le 1.5掳$). SMGPS is the largest, most sensitive and highest angular resolution 1 GHz survey of the Plane yet carried out, with an angular resolution of 8" and a broadband RMS sensitivity of $\sim$10--20 $渭$ Jy/beam. Here we d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.07275v2-abstract-full').style.display = 'inline'; document.getElementById('2312.07275v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.07275v2-abstract-full" style="display: none;"> We present the SARAO MeerKAT Galactic Plane Survey (SMGPS), a 1.3 GHz continuum survey of almost half of the Galactic Plane (251掳$\le l \le$ 358掳and 2掳$\le l \le$ 61掳at $|b| \le 1.5掳$). SMGPS is the largest, most sensitive and highest angular resolution 1 GHz survey of the Plane yet carried out, with an angular resolution of 8" and a broadband RMS sensitivity of $\sim$10--20 $渭$ Jy/beam. Here we describe the first publicly available data release from SMGPS which comprises data cubes of frequency-resolved images over 908--1656 MHz, power law fits to the images, and broadband zeroth moment integrated intensity images. A thorough assessment of the data quality and guidance for future usage of the data products are given. Finally, we discuss the tremendous potential of SMGPS by showcasing highlights of the Galactic and extragalactic science that it permits. These highlights include the discovery of a new population of non-thermal radio filaments; identification of new candidate supernova remnants, pulsar wind nebulae and planetary nebulae; improved radio/mid-IR classification of rare Luminous Blue Variables and discovery of associated extended radio nebulae; new radio stars identified by Bayesian cross-matching techniques; the realisation that many of the largest radio-quiet WISE HII region candidates are not true HII regions; and a large sample of previously undiscovered background HI galaxies in the Zone of Avoidance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.07275v2-abstract-full').style.display = 'none'; document.getElementById('2312.07275v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS. The data release is live and links can be found in the Data Availability Statement in the paper</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.05237">arXiv:2312.05237</a> <span> [<a href="https://arxiv.org/pdf/2312.05237">pdf</a>, <a href="https://arxiv.org/format/2312.05237">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad3823">10.1093/mnras/stad3823 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HI Galaxy Signatures in the SARAO MeerKAT Galactic Plane Survey -- II. The Local Void and its substructure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kurapati%2C+S">Sushma Kurapati</a>, <a href="/search/astro-ph?searchtype=author&query=Kraan-Korteweg%2C+R+C">Ren茅e C. Kraan-Korteweg</a>, <a href="/search/astro-ph?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+H">Hao Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Rajohnson%2C+S+H+A">Sambatriniaina H. A. Rajohnson</a>, <a href="/search/astro-ph?searchtype=author&query=Steyn%2C+N">Nadia Steyn</a>, <a href="/search/astro-ph?searchtype=author&query=Frank%2C+B">Bradley Frank</a>, <a href="/search/astro-ph?searchtype=author&query=Serra%2C+P">Paolo Serra</a>, <a href="/search/astro-ph?searchtype=author&query=Goedhart%2C+S">Sharmila Goedhart</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">Fernando 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="2312.05237v1-abstract-short" style="display: inline;"> The Local Void is one of the nearest large voids, located at a distance of 23 Mpc. It lies largely behind the Galactic Bulge and is therefore extremely difficult to observe. We use HI 21 cm emission observations from the SARAO MeerKAT Galactic Plane Survey (SMGPS) to study the Local Void and its surroundings over the Galactic longitude range 329$^{\circ}< \ell <$ 55$^{\circ}$, Galactic latitude… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.05237v1-abstract-full').style.display = 'inline'; document.getElementById('2312.05237v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.05237v1-abstract-full" style="display: none;"> The Local Void is one of the nearest large voids, located at a distance of 23 Mpc. It lies largely behind the Galactic Bulge and is therefore extremely difficult to observe. We use HI 21 cm emission observations from the SARAO MeerKAT Galactic Plane Survey (SMGPS) to study the Local Void and its surroundings over the Galactic longitude range 329$^{\circ}< \ell <$ 55$^{\circ}$, Galactic latitude $|b| <$ 1.5$^{\circ}$, and redshift $cz <$ 7500 km/s. We have detected 291 galaxies to median rms sensitivity of 0.44 mJy per beam per 44 km/s channel. We find 17 galaxies deep inside the Void, 96 at the border of the Void, while the remaining 178 galaxies are in average density environments. The extent of the Void is ~ 58 Mpc. It is severely under-dense for the longitude range 350$^{\circ}< \ell <$ 35$^{\circ}$ up to redshift $z <$ 4500 km/s. The galaxies in the Void tend to have \HI masses that are lower (by approximately 0.25 dex) than their average density counterparts. We find several potential candidates for small groups of galaxies, of which two groups (with 3 members and 5 members) in the Void show signs of filamentary substructure within the Void. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.05237v1-abstract-full').style.display = 'none'; document.getElementById('2312.05237v1-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS; 16 pages, 14 figures, Supplementary data are available online at 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/2312.03545">arXiv:2312.03545</a> <span> [<a href="https://arxiv.org/pdf/2312.03545">pdf</a>, <a href="https://arxiv.org/format/2312.03545">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> HI Galaxy Signatures in the SARAO MeerKAT Galactic Plane Survey $-$ I. Probing the richness of the Great Attractor Wall across the inner Zone of Avoidance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Steyn%2C+N">Nadia Steyn</a>, <a href="/search/astro-ph?searchtype=author&query=Kraan-Korteweg%2C+R+C">Ren茅e C. Kraan-Korteweg</a>, <a href="/search/astro-ph?searchtype=author&query=Rajohnson%2C+S+H+A">Sambatriniaina H. A. Rajohnson</a>, <a href="/search/astro-ph?searchtype=author&query=Kurapati%2C+S">Sushma Kurapati</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+H">Hao Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Frank%2C+B">Bradley Frank</a>, <a href="/search/astro-ph?searchtype=author&query=Serra%2C+P">Paolo Serra</a>, <a href="/search/astro-ph?searchtype=author&query=Staveley-Smith%2C+L">Lister Staveley-Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">Fernando Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Goedhart%2C+S">Sharmila Goedhart</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.03545v1-abstract-short" style="display: inline;"> This paper presents the first HI results extracted from the SARAO MeerKAT Galactic Plane Survey (SMGPS) $-$ a narrow strip ($b \sim 3^\circ$) along the southern Milky Way. The primary goal consisted in tracing the Great Attractor (GA) Wall across the innermost Zone of Avoidance. We reduced a segment spanning the longitude range $302^\circ \leq \ell \leq 332^\circ$ for the redshift range… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.03545v1-abstract-full').style.display = 'inline'; document.getElementById('2312.03545v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.03545v1-abstract-full" style="display: none;"> This paper presents the first HI results extracted from the SARAO MeerKAT Galactic Plane Survey (SMGPS) $-$ a narrow strip ($b \sim 3^\circ$) along the southern Milky Way. The primary goal consisted in tracing the Great Attractor (GA) Wall across the innermost Zone of Avoidance. We reduced a segment spanning the longitude range $302^\circ \leq \ell \leq 332^\circ$ for the redshift range $z \leq 0.08$. The superb SMGPS sensitivity (rms = 0.3-0.5 mJy beam$^{-1}$ per 44 kms$^{-1}$ channel) and angular resolution ($\sim$ 31" $\times$ 26") lead to a detection limit of log$(M_{\rm HI}/$M$_\odot) \geq$ 8.5 at the GA distance ($V_{\rm hel} \sim 3500 - 6500$ kms$^{-1}$). A total of 477 galaxy candidates were identified over the full redshift range. A comparison of the few HI detections with counterparts in the literature (mostly HIZOA) found the HI fluxes and other HI parameters to be highly consistent. The continuation of the GA Wall is confirmed through a prominent overdensity of $N = 214$ detections in the GA distance range. At higher latitudes, the wall moves to higher redshifts, supportive of a possible link with the Ophiuchus cluster located behind the Galactic Bulge. This deep interferometric HI survey demonstrates the power of the SMGPS in improving our insight of large-scale structures at these extremely low latitudes, despite the high obscuration and continuum background. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.03545v1-abstract-full').style.display = 'none'; document.getElementById('2312.03545v1-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 7 figures, 2 appendices of 12 pages. Journal reference: MNRAS Letters, accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.12140">arXiv:2311.12140</a> <span> [<a href="https://arxiv.org/pdf/2311.12140">pdf</a>, <a href="https://arxiv.org/format/2311.12140">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"> MeerKAT 1.3 GHz Observations of Supernova Remnants </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cotton%2C+W">William Cotton</a>, <a href="/search/astro-ph?searchtype=author&query=Kothes%2C+R">R. Kothes</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Chandra%2C+P">P. Chandra</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Nyamai%2C+M">M. Nyamai</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.12140v1-abstract-short" style="display: inline;"> We present full Stokes MeerKAT L band (856--1712\,MHz) observations of \chg{36} high latitude supernova remnants. Sensitive, high dynamic range images show a wealth of structure. G15.1$-$1.6 appears to be an HII region rather than an SNR. G30.7$-$2.0 consists of three background extragalactic sources which appear to form an arc when imaged with much lower resolution. At least half of the remnants… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.12140v1-abstract-full').style.display = 'inline'; document.getElementById('2311.12140v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.12140v1-abstract-full" style="display: none;"> We present full Stokes MeerKAT L band (856--1712\,MHz) observations of \chg{36} high latitude supernova remnants. Sensitive, high dynamic range images show a wealth of structure. G15.1$-$1.6 appears to be an HII region rather than an SNR. G30.7$-$2.0 consists of three background extragalactic sources which appear to form an arc when imaged with much lower resolution. At least half of the remnants in the sample contain ``blowouts'', or ``ears'' showing these to be a common feature. Analysis of the polarimetric data reveals details of the magnetic field structure in the emitting regions of the remnants as well as magnetized thermal plasma in front of polarized emission. The chance alignment of G327.6+14.6 with a background AGN with very extended polarized jets allows testing for the presence of Faraday effects in the interior of the remnant. Scant evidence of Faraday rotating material is found in the interior of this remnant. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.12140v1-abstract-full').style.display = 'none'; document.getElementById('2311.12140v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">41 pages, 58 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/2311.06445">arXiv:2311.06445</a> <span> [<a href="https://arxiv.org/pdf/2311.06445">pdf</a>, <a href="https://arxiv.org/format/2311.06445">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/10.1051/0004-6361/202347857">10.1051/0004-6361/202347857 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A MeerKAT view of the double pulsar eclipses -- Geodetic precession of pulsar B and system geometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lower%2C+M+E">M. E. Lower</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</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=Breton%2C+R+P">R. P. Breton</a>, <a href="/search/astro-ph?searchtype=author&query=Wex%2C+N">N. Wex</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+S">S. Johnston</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=Hu%2C+H">H. Hu</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=Blackmon%2C+V+A">V. A. Blackmon</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</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=Geyer%2C+M">M. Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Karastergiou%2C+A">A. Karastergiou</a>, <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+J">J. van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=McLaughlin%2C+M+A">M. A. McLaughlin</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=Stairs%2C+I+H">I. H. Stairs</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.06445v2-abstract-short" style="display: inline;"> The double pulsar system, PSR J0737$-$3039A/B, consists of two neutron stars bound together in a highly relativistic orbit that is viewed nearly edge-on from the Earth. This alignment results in brief radio eclipses of the fast-rotating pulsar A when it passes behind the toroidal magnetosphere of the slow-rotating pulsar B. The morphology of these eclipses is strongly dependent on the geometric or… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.06445v2-abstract-full').style.display = 'inline'; document.getElementById('2311.06445v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.06445v2-abstract-full" style="display: none;"> The double pulsar system, PSR J0737$-$3039A/B, consists of two neutron stars bound together in a highly relativistic orbit that is viewed nearly edge-on from the Earth. This alignment results in brief radio eclipses of the fast-rotating pulsar A when it passes behind the toroidal magnetosphere of the slow-rotating pulsar B. The morphology of these eclipses is strongly dependent on the geometric orientation and rotation phase of pulsar B, and their time-evolution can be used to constrain the geodetic precession rate of the pulsar. We demonstrate a Bayesian inference framework for modelling eclipse light-curves obtained with MeerKAT between 2019-2023. Using a hierarchical inference approach, we obtained a precession rate of $惟_{\rm SO}^{\rm B} = {5.16^{\circ}}^{+0.32^{\circ}}_{-0.34^{\circ}}$ yr$^{-1}$ for pulsar B, consistent with predictions from General Relativity to a relative uncertainty of 6.5%. This updated measurement provides a 6.1% test of relativistic spin-orbit coupling in the strong-field regime. We show that a simultaneous fit to all of our observed eclipses can in principle return a $\sim$1.5% test of spin-orbit coupling. However, systematic effects introduced by the current geometric orientation of pulsar B along with inconsistencies between the observed and predicted eclipse light curves result in difficult to quantify uncertainties. Assuming the validity of General Relativity, we definitively show that the spin-axis of pulsar B is misaligned from the total angular momentum vector by $40.6^{\circ} \pm 0.1^{\circ}$ and that the orbit of the system is inclined by approximately $90.5^{\circ}$ from the direction of our line of sight. Our measured geometry for pulsar B suggests the largely empty emission cone contains an elongated horseshoe shaped beam centered on the magnetic axis, and that it may not be re-detected as a radio pulsar until early-2035. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.06445v2-abstract-full').style.display = 'none'; document.getElementById('2311.06445v2-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Abridged abstract. 13 pages, 9 figures and 2 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 682, A26 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.04195">arXiv:2311.04195</a> <span> [<a href="https://arxiv.org/pdf/2311.04195">pdf</a>, <a href="https://arxiv.org/format/2311.04195">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/10.1038/s41550-024-02225-8">10.1038/s41550-024-02225-8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Linear to circular conversion in the polarized radio emission of a magnetar </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lower%2C+M+E">Marcus E. Lower</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+S">Simon Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Lyutikov%2C+M">Maxim Lyutikov</a>, <a href="/search/astro-ph?searchtype=author&query=Melrose%2C+D+B">Donald B. Melrose</a>, <a href="/search/astro-ph?searchtype=author&query=Shannon%2C+R+M">Ryan M. Shannon</a>, <a href="/search/astro-ph?searchtype=author&query=Weltevrede%2C+P">Patrick Weltevrede</a>, <a href="/search/astro-ph?searchtype=author&query=Caleb%2C+M">Manisha Caleb</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">Fernando Camilo</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=Dai%2C+S">Shi Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+G">George Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+D">Di Li</a>, <a href="/search/astro-ph?searchtype=author&query=Rajwade%2C+K+M">Kaustubh M. Rajwade</a>, <a href="/search/astro-ph?searchtype=author&query=Reynolds%2C+J+E">John E. Reynolds</a>, <a href="/search/astro-ph?searchtype=author&query=Sarkissian%2C+J+M">John M. Sarkissian</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">Benjamin W. Stappers</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.04195v2-abstract-short" style="display: inline;"> Radio emission from magnetars provides a unique probe of the relativistic, magnetized plasma within the near-field environment of these ultra-magnetic neutron stars. The transmitted waves can undergo birefringent and dispersive propagation effects that result in frequency-dependent conversions of linear to circularly polarized radiation and vice-versa, thus necessitating classification when relati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.04195v2-abstract-full').style.display = 'inline'; document.getElementById('2311.04195v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.04195v2-abstract-full" style="display: none;"> Radio emission from magnetars provides a unique probe of the relativistic, magnetized plasma within the near-field environment of these ultra-magnetic neutron stars. The transmitted waves can undergo birefringent and dispersive propagation effects that result in frequency-dependent conversions of linear to circularly polarized radiation and vice-versa, thus necessitating classification when relating the measured polarization to the intrinsic properties of neutron star and fast radio burst (FRB) emission sites. We report the detection of such behavior in 0.7-4 GHz observations of the P = 5.54 s radio magnetar XTE J1810$-$197 following its 2018 outburst. The phenomenon is restricted to a narrow range of pulse phase centered around the magnetic meridian. Its temporal evolution is closely coupled to large-scale variations in magnetic topology that originate from either plastic motion of an active region on the magnetar surface or free precession of the neutron star crust. Our model of the effect deviates from simple theoretical expectations for radio waves propagating through a magnetized plasma. Birefringent self-coupling between the transmitted wave modes, line-of-sight variations in the magnetic field direction and differences in particle charge or energy distributions above the magnetic pole are explored as possible explanations. We discuss potential links between the immediate magneto-ionic environments of magnetars and those of FRB progenitors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.04195v2-abstract-full').style.display = 'none'; document.getElementById('2311.04195v2-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages (inc. extended data and supplementary materials), 12 figures, 3 tables. Published in Nature Astronomy</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.17701">arXiv:2310.17701</a> <span> [<a href="https://arxiv.org/pdf/2310.17701">pdf</a>, <a href="https://arxiv.org/format/2310.17701">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Confirmation of a Substantial Discrepancy between Radio and UV--IR Measures of the Star Formation Rate Density at 0.2 < z < 1.3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Matthews%2C+A+M">A. M Matthews</a>, <a href="/search/astro-ph?searchtype=author&query=Kelson%2C+D+D">D. D. Kelson</a>, <a href="/search/astro-ph?searchtype=author&query=Newman%2C+A+B">A. B. Newman</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Condon%2C+J+J">J. J. Condon</a>, <a href="/search/astro-ph?searchtype=author&query=Cotton%2C+W+D">W. D. Cotton</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">M. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Jarrett%2C+T+H">T. H. Jarrett</a>, <a href="/search/astro-ph?searchtype=author&query=Lacy%2C+M">M. Lacy</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="2310.17701v2-abstract-short" style="display: inline;"> We present the initial sample of redshifts for 3,839 galaxies in the MeerKAT DEEP2 field -- the deepest $\sim$1.4\,GHz radio field yet observed. Using a spectrophotometric technique combining coarse optical spectra with broadband photometry, we obtain redshifts with $蟽_z \leq 0.01(1+z)$. The resulting radio luminosity functions between $0.2<z<1.3$ from our sample of 3,839 individual galaxies are i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.17701v2-abstract-full').style.display = 'inline'; document.getElementById('2310.17701v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.17701v2-abstract-full" style="display: none;"> We present the initial sample of redshifts for 3,839 galaxies in the MeerKAT DEEP2 field -- the deepest $\sim$1.4\,GHz radio field yet observed. Using a spectrophotometric technique combining coarse optical spectra with broadband photometry, we obtain redshifts with $蟽_z \leq 0.01(1+z)$. The resulting radio luminosity functions between $0.2<z<1.3$ from our sample of 3,839 individual galaxies are in remarkable agreement with those inferred from modeling radio source counts, confirming an excess in radio-based SFRD$(z$) measurements at late times compared to those from the UV--IR. Several sources of systematic error are discussed -- with most having the potential of exacerbating the discrepancy -- with the conclusion that significant work remains to have confidence in a full accounting of the star formation budget of the universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.17701v2-abstract-full').style.display = 'none'; document.getElementById('2310.17701v2-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 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">11 pages, 4 figures, accepted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/2303.02834">arXiv:2303.02834</a> <span> [<a href="https://arxiv.org/pdf/2303.02834">pdf</a>, <a href="https://arxiv.org/format/2303.02834">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/stad704">10.1093/mnras/stad704 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Timing of Pulsars in the Globular Cluster Omega Centauri </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dai%2C+S">S. Dai</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+S">S. Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Kerr%2C+M">M. Kerr</a>, <a href="/search/astro-ph?searchtype=author&query=Berteaud%2C+J">J. Berteaud</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharyya%2C+B">B. Bhattacharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Keane%2C+E">E. Keane</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="2303.02834v1-abstract-short" style="display: inline;"> We present the timing of the first five millisecond pulsars discovered in the globular cluster Omega Centauri and the discovery of a pulsar with a spin period of 3.68 ms. With a timing baseline of $\sim$3.5 yr we are able to measure the derivative of the spin frequency ($\dot谓$) for the first five pulsars. Upper limits on the pulsar line-of-sight acceleration are estimated and compared with predic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.02834v1-abstract-full').style.display = 'inline'; document.getElementById('2303.02834v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.02834v1-abstract-full" style="display: none;"> We present the timing of the first five millisecond pulsars discovered in the globular cluster Omega Centauri and the discovery of a pulsar with a spin period of 3.68 ms. With a timing baseline of $\sim$3.5 yr we are able to measure the derivative of the spin frequency ($\dot谓$) for the first five pulsars. Upper limits on the pulsar line-of-sight acceleration are estimated and compared with predictions based on analytical models of the cluster. We find that PSRs J1326$-$4728B and D show large negative accelerations, which are in tension with the minimum acceleration predicted by analytical models. We searched for pulsed $纬$-ray signals using 14.3 yr of data from the Fermi Large Area Telescope. Although we found no evidence for $纬$-ray pulsations, PSRs~J1326$-$4728A, B, C and E are associated with X-ray sources. This suggests that the observed $纬$-ray emission from Omega Centauri is likely caused by the emission of the ensemble of MSPs. Finally, the linearly polarised emission from PSR J1326$-$4728A yields a rotation measure of $-18\pm8$ rad m$^{-2}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.02834v1-abstract-full').style.display = 'none'; document.getElementById('2303.02834v1-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 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">8 pages, 5 figures, MNRAS accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.07397">arXiv:2302.07397</a> <span> [<a href="https://arxiv.org/pdf/2302.07397">pdf</a>, <a href="https://arxiv.org/format/2302.07397">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/acbc7c">10.3847/1538-4357/acbc7c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The 2022 high-energy outburst and radio disappearing act of the magnetar 1E 1547.0-5408 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lower%2C+M+E">Marcus E. Lower</a>, <a href="/search/astro-ph?searchtype=author&query=Younes%2C+G">George Younes</a>, <a href="/search/astro-ph?searchtype=author&query=Scholz%2C+P">Paul Scholz</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">Fernando Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+L">Liam Dunn</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+S">Simon Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Enoto%2C+T">Teruaki Enoto</a>, <a href="/search/astro-ph?searchtype=author&query=Sarkissian%2C+J+M">John M. Sarkissian</a>, <a href="/search/astro-ph?searchtype=author&query=Reynolds%2C+J+E">John E. Reynolds</a>, <a href="/search/astro-ph?searchtype=author&query=Palmer%2C+D+M">David M. Palmer</a>, <a href="/search/astro-ph?searchtype=author&query=Arzoumanian%2C+Z">Zaven Arzoumanian</a>, <a href="/search/astro-ph?searchtype=author&query=Baring%2C+M+G">Matthew G. Baring</a>, <a href="/search/astro-ph?searchtype=author&query=Gendreau%2C+K">Keith Gendreau</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B6%C4%9F%C3%BC%C5%9F%2C+E">Ersin G枚臒眉艧</a>, <a href="/search/astro-ph?searchtype=author&query=Guillot%2C+S">Sebastien Guillot</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Horst%2C+A+J">Alexander J. van der Horst</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+C">Chin-Ping Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Kouveliotou%2C+C">Chryssa Kouveliotou</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+L">Lin Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Malacaria%2C+C">Christian Malacaria</a>, <a href="/search/astro-ph?searchtype=author&query=Stewart%2C+R">Rachael Stewart</a>, <a href="/search/astro-ph?searchtype=author&query=Wadiasingh%2C+Z">Zorawar Wadiasingh</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="2302.07397v2-abstract-short" style="display: inline;"> We report the radio and high-energy properties of a new outburst from the radio-loud magnetar 1E 1547.0$-$5408. Following the detection of a short burst from the source with Swift-BAT on 2022 April 7, observations by NICER detected an increased flux peaking at $(6.0 \pm 0.4) \times 10^{-11}$ erg s$^{-1}$ cm$^{-2}$ in the soft X-ray band, falling to the baseline level of $1.7\times10^{-11}$ erg s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.07397v2-abstract-full').style.display = 'inline'; document.getElementById('2302.07397v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.07397v2-abstract-full" style="display: none;"> We report the radio and high-energy properties of a new outburst from the radio-loud magnetar 1E 1547.0$-$5408. Following the detection of a short burst from the source with Swift-BAT on 2022 April 7, observations by NICER detected an increased flux peaking at $(6.0 \pm 0.4) \times 10^{-11}$ erg s$^{-1}$ cm$^{-2}$ in the soft X-ray band, falling to the baseline level of $1.7\times10^{-11}$ erg s$^{-1}$ cm$^{-2}$ over a 17-day period. Joint spectroscopic measurements by NICER and NuSTAR indicated no change in the hard non-thermal tail despite the prominent increase in soft X-rays. Observations at radio wavelengths with Murriyang, the 64-m Parkes radio telescope, revealed that the persistent radio emission from the magnetar disappeared at least 22 days prior to the initial Swift-BAT detection and was re-detected two weeks later. Such behavior is unprecedented in a radio-loud magnetar, and may point to an unnoticed slow rise in the high-energy activity prior to the detected short-bursts. Finally, our combined radio and X-ray timing revealed the outburst coincided with a spin-up glitch, where the spin-frequency and spin-down rate increased by $0.2 \pm 0.1$ $渭$Hz and $(-2.4 \pm 0.1) \times 10^{-12}$ s$^{-2}$ respectively. A linear increase in spin-down rate of $(-2.0 \pm 0.1) \times 10^{-19}$ s$^{-3}$ was also observed over 147 d of post-outburst timing. Our results suggest that the outburst may have been associated with a reconfiguration of the quasi-polar field lines, likely signalling a changing twist, accompanied by spatially broader heating of the surface and a brief quenching of the radio signal, yet without any measurable impact on the hard X-ray properties. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.07397v2-abstract-full').style.display = 'none'; document.getElementById('2302.07397v2-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 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">Accepted to ApJ, 18 pages, 7 figures. Fixed typo in abstract and discussion</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.10995">arXiv:2301.10995</a> <span> [<a href="https://arxiv.org/pdf/2301.10995">pdf</a>, <a href="https://arxiv.org/format/2301.10995">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/10.1038/s41550-022-01874-x">10.1038/s41550-022-01874-x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Neutron star mass estimates from gamma-ray eclipses in spider millisecond pulsar binaries </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=Kerr%2C+M">M. Kerr</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=Bhattacharyya%2C+B">B. Bhattacharyya</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=Bruel%2C+P">P. Bruel</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">W. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cognard%2C+I">I. Cognard</a>, <a href="/search/astro-ph?searchtype=author&query=Cromartie%2C+H+T">H. T. Cromartie</a>, <a href="/search/astro-ph?searchtype=author&query=Deneva%2C+J">J. Deneva</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=Guillemot%2C+L">L. Guillemot</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=Lyne%2C+A+G">A. G. Lyne</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+D+M">D. Mata S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Nieder%2C+L">L. Nieder</a>, <a href="/search/astro-ph?searchtype=author&query=Phillips%2C+C">C. Phillips</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=Ray%2C+P+S">P. S. Ray</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts%2C+M+S+E">M. S. E. Roberts</a>, <a href="/search/astro-ph?searchtype=author&query=Roy%2C+J">J. Roy</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+D+A">D. A. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Spiewak%2C+R">R. Spiewak</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="2301.10995v1-abstract-short" style="display: inline;"> Reliable neutron star mass measurements are key to determining the equation-of-state of cold nuclear matter, but these are rare. "Black Widows" and "Redbacks" are compact binaries consisting of millisecond pulsars and semi-degenerate companion stars. Spectroscopy of the optically bright companions can determine their radial velocities, providing inclination-dependent pulsar mass estimates. While i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.10995v1-abstract-full').style.display = 'inline'; document.getElementById('2301.10995v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.10995v1-abstract-full" style="display: none;"> Reliable neutron star mass measurements are key to determining the equation-of-state of cold nuclear matter, but these are rare. "Black Widows" and "Redbacks" are compact binaries consisting of millisecond pulsars and semi-degenerate companion stars. Spectroscopy of the optically bright companions can determine their radial velocities, providing inclination-dependent pulsar mass estimates. While inclinations can be inferred from subtle features in optical light curves, such estimates may be systematically biased due to incomplete heating models and poorly-understood variability. Using data from the Fermi Large Area Telescope, we have searched for gamma-ray eclipses from 49 spider systems, discovering significant eclipses in 7 systems, including the prototypical black widow PSR B1957$+$20. Gamma-ray eclipses require direct occultation of the pulsar by the companion, and so the detection, or significant exclusion, of a gamma-ray eclipse strictly limits the binary inclination angle, providing new robust, model-independent pulsar mass constraints. For PSR B1957$+$20, the eclipse implies a much lighter pulsar ($M_{\rm psr} = 1.81 \pm 0.07\,M_{\odot}$) than inferred from optical light curve modelling. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.10995v1-abstract-full').style.display = 'none'; document.getElementById('2301.10995v1-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 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">31 pages, 4 figures, includes supplementary tables; published in Nature Astronomy</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.07132">arXiv:2301.07132</a> <span> [<a href="https://arxiv.org/pdf/2301.07132">pdf</a>, <a href="https://arxiv.org/format/2301.07132">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/stad203">10.1093/mnras/stad203 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A black widow population dissection through HiPERCAM multi-band light curve modelling </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+D+M">D. Mata S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Kennedy%2C+M+R">M. R. Kennedy</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=Dhillon%2C+V+S">V. S. Dhillon</a>, <a href="/search/astro-ph?searchtype=author&query=Voisin%2C+G">G. Voisin</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Littlefair%2C+S">S. Littlefair</a>, <a href="/search/astro-ph?searchtype=author&query=Marsh%2C+T+R">T. R. Marsh</a>, <a href="/search/astro-ph?searchtype=author&query=Stringer%2C+J">J. Stringer</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="2301.07132v1-abstract-short" style="display: inline;"> Black widows are extreme millisecond pulsar binaries where the pulsar wind ablates their low-mass companion stars. Their optical light curves vary periodically due to the high irradiation and tidal distortion of the companion, which allows us to infer the binary parameters. We present simultaneous multi-band observations obtained with the HIPERCAM instrument at the 10.4-m GTC telescope for six of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.07132v1-abstract-full').style.display = 'inline'; document.getElementById('2301.07132v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.07132v1-abstract-full" style="display: none;"> Black widows are extreme millisecond pulsar binaries where the pulsar wind ablates their low-mass companion stars. Their optical light curves vary periodically due to the high irradiation and tidal distortion of the companion, which allows us to infer the binary parameters. We present simultaneous multi-band observations obtained with the HIPERCAM instrument at the 10.4-m GTC telescope for six of these systems. The combination of this five-band fast photometer with the world's largest optical telescope enables us to inspect the light curve range near minima. We present the first light curve for PSR J1641+8049, as well as attain a significant increase in signal-to-noise and cadence compared with previous publications for the remaining 5 targets: PSR J0023+0923, PSR J0251+2606, PSR J0636+5129, PSR J0952-0607 and PSR J1544+4937. We report on the results of the light curve modelling with the Icarus code for all six systems, which reveals some of the hottest and densest companion stars known. We compare the parameters derived with the limited but steadily growing black widow population for which optical modelling is available. We find some expected correlations, such as that between the companion star mean density and the orbital period of the system, but also a puzzling positive correlation between the orbital inclination and the irradiation temperature of the companion. We propose such a correlation would arise if pulsars with magnetic axis orthogonal to their spin axis are capable of irradiating their companions to a higher degree. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.07132v1-abstract-full').style.display = 'none'; document.getElementById('2301.07132v1-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 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages (+12 pages for appendix), 12 figures (+13 in the appendix), 3 tables (1 in the appendix). Accepted for publication in MNRAS on 2023 January 17th</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/2212.04648">arXiv:2212.04648</a> <span> [<a href="https://arxiv.org/pdf/2212.04648">pdf</a>, <a href="https://arxiv.org/format/2212.04648">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/stac3644">10.1093/mnras/stac3644 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MeerKAT Pulsar Timing Array: First Data Release </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Miles%2C+M+T">Matthew T. Miles</a>, <a href="/search/astro-ph?searchtype=author&query=Shannon%2C+R+M">Ryan M. Shannon</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">Matthew Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Reardon%2C+D+J">Daniel J. Reardon</a>, <a href="/search/astro-ph?searchtype=author&query=Keith%2C+M+J">Michael J. Keith</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=Parthasarathy%2C+A">Aditya Parthasarathy</a>, <a href="/search/astro-ph?searchtype=author&query=Shamohammadi%2C+M">Mohsen Shamohammadi</a>, <a href="/search/astro-ph?searchtype=author&query=Spiewak%2C+R">Renee Spiewak</a>, <a href="/search/astro-ph?searchtype=author&query=van+Straten%2C+W">Willem van Straten</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">Sarah Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">Fernando Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Geyer%2C+M">Marisa Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Karastergiou%2C+A">Aris Karastergiou</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">Michael Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Serylak%2C+M">Maciej Serylak</a>, <a href="/search/astro-ph?searchtype=author&query=Theureau%2C+G">Gilles Theureau</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">Vivek 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="2212.04648v1-abstract-short" style="display: inline;"> We present the first 2.5 years of data from the MeerKAT Pulsar Timing Array (MPTA), part of MeerTime, a MeerKAT Large Survey Project. The MPTA aims to precisely measure pulse arrival times from an ensemble of 88 pulsars visible from the Southern Hemisphere, with the goal of contributing to the search, detection and study of nanohertz-frequency gravitational waves as part of the International Pulsa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.04648v1-abstract-full').style.display = 'inline'; document.getElementById('2212.04648v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.04648v1-abstract-full" style="display: none;"> We present the first 2.5 years of data from the MeerKAT Pulsar Timing Array (MPTA), part of MeerTime, a MeerKAT Large Survey Project. The MPTA aims to precisely measure pulse arrival times from an ensemble of 88 pulsars visible from the Southern Hemisphere, with the goal of contributing to the search, detection and study of nanohertz-frequency gravitational waves as part of the International Pulsar Timing Array. This project makes use of the MeerKAT telescope, and operates with a typical observing cadence of two weeks using the L-band receiver that records data from 856-1712 MHz. We provide a comprehensive description of the observing system, software, and pipelines used and developed for the MeerTime project. The data products made available as part of this data release are from the 78 pulsars that had at least $30$ observations between the start of the MeerTime programme in February 2019 and October 2021. These include both sub-banded and band-averaged arrival times, as well as the initial timing ephemerides, noise models, and the frequency-dependent standard templates (portraits) used to derive pulse arrival times. After accounting for detected noise processes in the data, the frequency-averaged residuals of $67$ of the pulsars achieved a root-mean-square residual precision of $< 1 渭\rm{s}$. We also present a novel recovery of the clock correction waveform solely from pulsar timing residuals, and an exploration into preliminary findings of interest to the international pulsar timing community. The arrival times, standards and full Stokes parameter calibrated pulsar timing archives are publicly available. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.04648v1-abstract-full').style.display = 'none'; document.getElementById('2212.04648v1-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 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 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/2211.03815">arXiv:2211.03815</a> <span> [<a href="https://arxiv.org/pdf/2211.03815">pdf</a>, <a href="https://arxiv.org/format/2211.03815">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/stac3248">10.1093/mnras/stac3248 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A MeerKAT look at the polarization of 47 Tucanae pulsars: magnetic field implications </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=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=Buchner%2C+S">S. Buchner</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=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+A">A. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Parthasarathy%2C+A">A. Parthasarathy</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=Chen%2C+W">W. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</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=Mao%2C+S+A">S. A. Mao</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=Ransom%2C+S+M">S. M. Ransom</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=Zhang%2C+L">L. Zhang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.03815v1-abstract-short" style="display: inline;"> We present the polarization profiles of 22 pulsars in the globular cluster 47 Tucanae using observations from the MeerKAT radio telescope at UHF-band (544-1088 MHz) and report precise values of dispersion measure (DM) and rotation measure (RM). We use these measurements to investigate the presence of turbulence in electron density and magnetic fields. The structure function of DM shows a break at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.03815v1-abstract-full').style.display = 'inline'; document.getElementById('2211.03815v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.03815v1-abstract-full" style="display: none;"> We present the polarization profiles of 22 pulsars in the globular cluster 47 Tucanae using observations from the MeerKAT radio telescope at UHF-band (544-1088 MHz) and report precise values of dispersion measure (DM) and rotation measure (RM). We use these measurements to investigate the presence of turbulence in electron density and magnetic fields. The structure function of DM shows a break at $\sim 30$ arcsec ($\sim 0.6$ pc at the distance of 47 Tucanae) that suggests the presence of turbulence in the gas in the cluster driven by the motion of wind-shedding stars. On the other hand, the structure function of RM does not show evidence of a break. This non-detection could be explained either by the limited number of pulsars or by the effects of the intervening gas in the Galaxy along the line of sight. Future pulsar discoveries in the cluster could help confirm the presence and localise the turbulence. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.03815v1-abstract-full').style.display = 'none'; document.getElementById('2211.03815v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS, 14 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/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/2206.10732">arXiv:2206.10732</a> <span> [<a href="https://arxiv.org/pdf/2206.10732">pdf</a>, <a href="https://arxiv.org/ps/2206.10732">ps</a>, <a href="https://arxiv.org/format/2206.10732">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/stac1696">10.1093/mnras/stac1696 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Statistical Properties of the Population of the Galactic Center Filaments II: The Spacing Between Filaments </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yusef-Zadeh%2C+F">F. Yusef-Zadeh</a>, <a href="/search/astro-ph?searchtype=author&query=Arendt%2C+R+G">R. G. Arendt</a>, <a href="/search/astro-ph?searchtype=author&query=Wardle%2C+M">M. Wardle</a>, <a href="/search/astro-ph?searchtype=author&query=Boldyrev%2C+S">S. Boldyrev</a>, <a href="/search/astro-ph?searchtype=author&query=Heywood%2C+I">I. Heywood</a>, <a href="/search/astro-ph?searchtype=author&query=Cotton%2C+W">W. Cotton</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="2206.10732v1-abstract-short" style="display: inline;"> We carry out a population study of magnetized radio filaments in the Galactic center using MeerKAT data by focusing on the spacing between the filaments that are grouped. The morphology of a sample of 43 groupings containing 174 magnetized radio filaments are presented. Many grouped filaments show harp-like, fragmented cometary tail-like, or loop-like structures in contrast to many straight filame… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.10732v1-abstract-full').style.display = 'inline'; document.getElementById('2206.10732v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.10732v1-abstract-full" style="display: none;"> We carry out a population study of magnetized radio filaments in the Galactic center using MeerKAT data by focusing on the spacing between the filaments that are grouped. The morphology of a sample of 43 groupings containing 174 magnetized radio filaments are presented. Many grouped filaments show harp-like, fragmented cometary tail-like, or loop-like structures in contrast to many straight filaments running mainly perpendicular to the Galactic plane. There are many striking examples of a single filament splitting into two prongs at a junction, suggestive of a flow of plasma along the filaments. Spatial variations in spectral index, brightness, bending and sharpening along the filaments indicate that they are evolving on a 10^{5-6}-year time scale. The mean spacings between parallel filaments in a given grouping peaks at $\sim16''$. We argue by modeling that the filaments in a grouping all lie on the same plane and that the groupings are isotropically oriented in 3D space. One candidate for the origin of filamentation is interaction with an obstacle, which could be a compact radio source, before a filament splits and bends into multiple filaments. In this picture, the obstacle or sets the length scale of the separation between the filaments. Another possibility is synchrotron cooling instability occurring in cometary tails formed as a result of the interaction of cosmic-ray driven Galactic center outflow with obstacles such as stellar winds. In this picture, the mean spacing and the mean width of the filaments are expected to be a fraction of a parsec, consistent with observed spacing. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.10732v1-abstract-full').style.display = 'none'; document.getElementById('2206.10732v1-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, 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">53 pages, 32 figures, MNRS (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/2205.06600">arXiv:2205.06600</a> <span> [<a href="https://arxiv.org/pdf/2205.06600">pdf</a>, <a href="https://arxiv.org/ps/2205.06600">ps</a>, <a href="https://arxiv.org/format/2205.06600">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/ac6fd3">10.3847/1538-4357/ac6fd3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Curious Case of the "Heartworm" Nebula </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cotton%2C+W+D">W. D. Cotton</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+W">W. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Condon%2C+J+J">J. J. Condon</a>, <a href="/search/astro-ph?searchtype=author&query=Forbrich%2C+J">J. Forbrich</a>, <a href="/search/astro-ph?searchtype=author&query=Heywood%2C+I">I. Heywood</a>, <a href="/search/astro-ph?searchtype=author&query=Hugo%2C+B">B. Hugo</a>, <a href="/search/astro-ph?searchtype=author&query=Legodi%2C+S">S. Legodi</a>, <a href="/search/astro-ph?searchtype=author&query=Mauch%2C+T">T. Mauch</a>, <a href="/search/astro-ph?searchtype=author&query=Predehl%2C+P">P. Predehl</a>, <a href="/search/astro-ph?searchtype=author&query=Slane%2C+P">P. Slane</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+M+A">M. A. Thompson</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="2205.06600v1-abstract-short" style="display: inline;"> The curious Galactic features near G357.2$-$0.2 were observed with the MeerKAT radio interferometer array in the UHF and L bands (0.56--1.68 GHz). There are two possibly related features: a newly identified faint heart-shaped partial shell (the "Heart"), and a series of previously known but now much better imaged narrow, curved features (the "Worm") interior to the heart. Polarized emission sugges… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.06600v1-abstract-full').style.display = 'inline'; document.getElementById('2205.06600v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.06600v1-abstract-full" style="display: none;"> The curious Galactic features near G357.2$-$0.2 were observed with the MeerKAT radio interferometer array in the UHF and L bands (0.56--1.68 GHz). There are two possibly related features: a newly identified faint heart-shaped partial shell (the "Heart"), and a series of previously known but now much better imaged narrow, curved features (the "Worm") interior to the heart. Polarized emission suggests that much of the emission is nonthermal and is embedded in a dense plasma. The filaments of the worm appear to be magnetic structures powered by embedded knots that are sites of particle acceleration. The morphology of the worm broadly resembles some known pulsar wind nebulae (PWNe) but there is no known pulsar or PWN which could be powering this structure. We also present eROSITA observations of the field; no part of the nebula is detected in X-rays, but the current limits do not preclude the existence of a pulsar/PWN of intermediate spin-down luminosity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.06600v1-abstract-full').style.display = 'none'; document.getElementById('2205.06600v1-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 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">14 pages, 14 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/2204.04115">arXiv:2204.04115</a> <span> [<a href="https://arxiv.org/pdf/2204.04115">pdf</a>, <a href="https://arxiv.org/format/2204.04115">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1017/pasa.2022.19">10.1017/pasa.2022.19 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MeerTime Pulsar Timing Array -- A Census of Emission Properties and Timing Potential </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Spiewak%2C+R">R. Spiewak</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Miles%2C+M+T">M. T. Miles</a>, <a href="/search/astro-ph?searchtype=author&query=Parthasarathy%2C+A">A. Parthasarathy</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=Shamohammadi%2C+M">M. Shamohammadi</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=Bhat%2C+N+D+R">N. D. R. Bhat</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=Geyer%2C+M">M. Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+S">S. Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Karastergiou%2C+A">A. Karastergiou</a>, <a href="/search/astro-ph?searchtype=author&query=Keith%2C+M">M. Keith</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Serylak%2C+M">M. Serylak</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=Theureau%2C+G">G. Theureau</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="2204.04115v1-abstract-short" style="display: inline;"> MeerTime is a five-year Large Survey Project to time pulsars with MeerKAT, the 64-dish South African precursor to the Square Kilometre Array. The science goals for the programme include timing millisecond pulsars (MSPs) to high precision (< 1 $渭$s) to study the Galactic MSP population and to contribute to global efforts to detect nanohertz gravitational waves with the International Pulsar Timing A… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.04115v1-abstract-full').style.display = 'inline'; document.getElementById('2204.04115v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.04115v1-abstract-full" style="display: none;"> MeerTime is a five-year Large Survey Project to time pulsars with MeerKAT, the 64-dish South African precursor to the Square Kilometre Array. The science goals for the programme include timing millisecond pulsars (MSPs) to high precision (< 1 $渭$s) to study the Galactic MSP population and to contribute to global efforts to detect nanohertz gravitational waves with the International Pulsar Timing Array (IPTA). In order to plan for the remainder of the programme and to use the allocated time most efficiently, we have conducted an initial census with the MeerKAT "L-band" receiver of 189 MSPs visible to MeerKAT and here present their dispersion measures, polarization profiles, polarization fractions, rotation measures, flux density measurements, spectral indices, and timing potential. As all of these observations are taken with the same instrument (which uses coherent dedispersion, interferometric polarization calibration techniques, and a uniform flux scale), they present an excellent resource for population studies. We used wideband pulse portraits as timing standards for each MSP and demonstrated that the MeerTime Pulsar Timing Array (MPTA) can already contribute significantly to the IPTA as it currently achieves better than 1 $渭$s timing accuracy on 89 MSPs (observed with fortnightly cadence). By the conclusion of the initial five-year MeerTime programme in July 2024, the MPTA will be extremely significant in global efforts to detect the gravitational wave background with a contribution to the detection statistic comparable to other long-standing timing programmes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.04115v1-abstract-full').style.display = 'none'; document.getElementById('2204.04115v1-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 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 to PASA. 27 figures. Data to be made available under the DOI 10.5281/zenodo.5347875 at the time of publication</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/2202.04783">arXiv:2202.04783</a> <span> [<a href="https://arxiv.org/pdf/2202.04783">pdf</a>, <a href="https://arxiv.org/format/2202.04783">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/ac49ef">10.3847/1538-4357/ac49ef <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery, Timing, and Multiwavelength Observations of the Black Widow Millisecond Pulsar PSR J1555-2908 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ray%2C+P+S">Paul S. Ray</a>, <a href="/search/astro-ph?searchtype=author&query=Nieder%2C+L">Lars Nieder</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=Ransom%2C+S+M">Scott M. Ransom</a>, <a href="/search/astro-ph?searchtype=author&query=Cromartie%2C+H+T">H. Thankful Cromartie</a>, <a href="/search/astro-ph?searchtype=author&query=Frail%2C+D+A">Dale A. Frail</a>, <a href="/search/astro-ph?searchtype=author&query=Mooley%2C+K+P">Kunal P. Mooley</a>, <a href="/search/astro-ph?searchtype=author&query=Intema%2C+H">Huib Intema</a>, <a href="/search/astro-ph?searchtype=author&query=Jagannathan%2C+P">Preshanth Jagannathan</a>, <a href="/search/astro-ph?searchtype=author&query=Demorest%2C+P">Paul Demorest</a>, <a href="/search/astro-ph?searchtype=author&query=Stovall%2C+K">Kevin Stovall</a>, <a href="/search/astro-ph?searchtype=author&query=Halpern%2C+J+P">Jules P. Halpern</a>, <a href="/search/astro-ph?searchtype=author&query=Deneva%2C+J">Julia Deneva</a>, <a href="/search/astro-ph?searchtype=author&query=Guillot%2C+S">Sebastien Guillot</a>, <a href="/search/astro-ph?searchtype=author&query=Kerr%2C+M">Matthew Kerr</a>, <a href="/search/astro-ph?searchtype=author&query=Swihart%2C+S+J">Samuel J. Swihart</a>, <a href="/search/astro-ph?searchtype=author&query=Bruel%2C+P">Philippe Bruel</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">Ben W. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Lyne%2C+A">Andrew Lyne</a>, <a href="/search/astro-ph?searchtype=author&query=Mickaliger%2C+M">Mitch Mickaliger</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">Fernando Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrara%2C+E+C">Elizabeth C. Ferrara</a>, <a href="/search/astro-ph?searchtype=author&query=Wolff%2C+M+T">Michael T. Wolff</a>, <a href="/search/astro-ph?searchtype=author&query=Michelson%2C+P+F">P. F. Michelson</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="2202.04783v1-abstract-short" style="display: inline;"> We report the discovery of PSR J1555-2908, a 1.79 ms radio and gamma-ray pulsar in a 5.6 hr binary system with a minimum companion mass of 0.052 $M_\odot$. This fast and energetic ($\dot E = 3 \times 10^{35}$ erg/s) millisecond pulsar was first detected as a gamma-ray point source in Fermi LAT sky survey observations. Guided by a steep spectrum radio point source in the Fermi error region, we perf… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.04783v1-abstract-full').style.display = 'inline'; document.getElementById('2202.04783v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.04783v1-abstract-full" style="display: none;"> We report the discovery of PSR J1555-2908, a 1.79 ms radio and gamma-ray pulsar in a 5.6 hr binary system with a minimum companion mass of 0.052 $M_\odot$. This fast and energetic ($\dot E = 3 \times 10^{35}$ erg/s) millisecond pulsar was first detected as a gamma-ray point source in Fermi LAT sky survey observations. Guided by a steep spectrum radio point source in the Fermi error region, we performed a search at 820 MHz with the Green Bank Telescope that first discovered the pulsations. The initial radio pulse timing observations provided enough information to seed a search for gamma-ray pulsations in the LAT data, from which we derive a timing solution valid for the full Fermi mission. In addition to the radio and gamma-ray pulsation discovery and timing, we searched for X-ray pulsations using NICER but no significant pulsations were detected. We also obtained time-series r-band photometry that indicates strong heating of the companion star by the pulsar wind. Material blown off the heated companion eclipses the 820 MHz radio pulse during inferior conjunction of the companion for ~10% of the orbit, which is twice the angle subtended by its Roche lobe in an edge-on system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.04783v1-abstract-full').style.display = 'none'; document.getElementById('2202.04783v1-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 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">15 pages, 6 figures, accepted by 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/2201.10552">arXiv:2201.10552</a> <span> [<a href="https://arxiv.org/pdf/2201.10552">pdf</a>, <a href="https://arxiv.org/ps/2201.10552">ps</a>, <a href="https://arxiv.org/format/2201.10552">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ac4802">10.3847/2041-8213/ac4802 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Statistical Properties of the Population of the Galactic Center Filaments: The Spectral Index and Equipartition Magnetic Field </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yusef-Zadeh%2C+F">F. Yusef-Zadeh</a>, <a href="/search/astro-ph?searchtype=author&query=Arendt%2C+R+G">R. G. Arendt</a>, <a href="/search/astro-ph?searchtype=author&query=Wardle%2C+M">M. Wardle</a>, <a href="/search/astro-ph?searchtype=author&query=Heywood%2C+I">I. Heywood</a>, <a href="/search/astro-ph?searchtype=author&query=Cotton%2C+W+D">W. D. Cotton</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a> </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="2201.10552v1-abstract-short" style="display: inline;"> We present high-pass filtered continuum images of the inner $3.5^\circ\times2.5^\circ$ of the Galactic center at 20 cm with $6.4''$ resolution. These mosaic images are taken with MeerKAT and reveal a large number of narrow filaments, roughly an order of magnitude increase in their numbers compared to past measurements. For the first time, we carry out population studies of the spectral index and m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.10552v1-abstract-full').style.display = 'inline'; document.getElementById('2201.10552v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.10552v1-abstract-full" style="display: none;"> We present high-pass filtered continuum images of the inner $3.5^\circ\times2.5^\circ$ of the Galactic center at 20 cm with $6.4''$ resolution. These mosaic images are taken with MeerKAT and reveal a large number of narrow filaments, roughly an order of magnitude increase in their numbers compared to past measurements. For the first time, we carry out population studies of the spectral index and magnetic field of the entire region. The mean spectral indices of the filaments are steeper than supernova remnants (SNRs) (-0.62) with a value of $伪\sim-0.83$. The variation in $伪$ is much larger than for the SNRs, suggesting that these characteristics have a different origin. A large-scale cosmic-ray driven wind has recently been proposed to explain the origin of filaments and the large-scale 430 pc bipolar radio and X-ray structure. This favors the possibility that the large-scale bipolar radio/X-ray structure is produced by past activity of Sgr A* rather than coordinated burst of supernovae. A trend of steeper indices is also noted with increasing distance from the Galactic plane. This could be explained either by synchrotron cooling or weak shocks accelerating cosmic-ray particles in the context of the cosmic-ray driven wind. The mean magnetic field strengths along the filaments ranges from $\sim100$ to 400 $渭$G depending on the assumed ratio of cosmic-ray protons to electrons. Given that there is a high cosmic ray pressure in the Galactic center, the large equipartition magnetic field implies that the magnetic field is weak in most of the interstellar volume of the Galactic center. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.10552v1-abstract-full').style.display = 'none'; document.getElementById('2201.10552v1-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 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">15 pages, 9 figures, accepted for publication in Astrophysical Journal Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.10541">arXiv:2201.10541</a> <span> [<a href="https://arxiv.org/pdf/2201.10541">pdf</a>, <a href="https://arxiv.org/ps/2201.10541">ps</a>, <a href="https://arxiv.org/format/2201.10541">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac449a">10.3847/1538-4357/ac449a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The 1.28 GHz MeerKAT Galactic Center Mosaic </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Heywood%2C+I">I. Heywood</a>, <a href="/search/astro-ph?searchtype=author&query=Rammala%2C+I">I. Rammala</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Cotton%2C+W+D">W. D. Cotton</a>, <a href="/search/astro-ph?searchtype=author&query=Yusef-Zadeh%2C+F">F. Yusef-Zadeh</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R+M">R. M. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+G">G. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Aldera%2C+M+A">M. A. Aldera</a>, <a href="/search/astro-ph?searchtype=author&query=Asad%2C+K+M+B">K. M. B. Asad</a>, <a href="/search/astro-ph?searchtype=author&query=Bauermeister%2C+E+F">E. F. Bauermeister</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+T+G+H">T. G. H. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Bester%2C+H+L">H. L. Bester</a>, <a href="/search/astro-ph?searchtype=author&query=Bode%2C+W+A">W. A. Bode</a>, <a href="/search/astro-ph?searchtype=author&query=Botha%2C+D+H">D. H. Botha</a>, <a href="/search/astro-ph?searchtype=author&query=Botha%2C+A+G">A. G. Botha</a>, <a href="/search/astro-ph?searchtype=author&query=Brederode%2C+L+R+S">L. R. S. Brederode</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S">S. Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Burger%2C+J+P">J. P. Burger</a>, <a href="/search/astro-ph?searchtype=author&query=Cheetham%2C+T">T. Cheetham</a>, <a href="/search/astro-ph?searchtype=author&query=de+Villiers%2C+D+I+L">D. I. L. de Villiers</a>, <a href="/search/astro-ph?searchtype=author&query=Dikgale-Mahlakoana%2C+M+A">M. A. Dikgale-Mahlakoana</a>, <a href="/search/astro-ph?searchtype=author&query=Toit%2C+L+J+d">L. J. du Toit</a>, <a href="/search/astro-ph?searchtype=author&query=Esterhuyse%2C+S+W+P">S. W. P. Esterhuyse</a>, <a href="/search/astro-ph?searchtype=author&query=Fanaroff%2C+B+L">B. L. Fanaroff</a> , et al. (86 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="2201.10541v3-abstract-short" style="display: inline;"> The inner $\sim$200 pc region of the Galaxy contains a 4 million M$_{\odot}$ supermassive black hole (SMBH), significant quantities of molecular gas, and star formation and cosmic ray energy densities that are roughly two orders of magnitude higher than the corresponding levels in the Galactic disk. At a distance of only 8.2 kpc, the region presents astronomers with a unique opportunity to study a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.10541v3-abstract-full').style.display = 'inline'; document.getElementById('2201.10541v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.10541v3-abstract-full" style="display: none;"> The inner $\sim$200 pc region of the Galaxy contains a 4 million M$_{\odot}$ supermassive black hole (SMBH), significant quantities of molecular gas, and star formation and cosmic ray energy densities that are roughly two orders of magnitude higher than the corresponding levels in the Galactic disk. At a distance of only 8.2 kpc, the region presents astronomers with a unique opportunity to study a diverse range of energetic astrophysical phenomena, from stellar objects in extreme environments, to the SMBH and star-formation driven feedback processes that are known to influence the evolution of galaxies as a whole. We present a new survey of the Galactic center conducted with the South African MeerKAT radio telescope. Radio imaging offers a view that is unaffected by the large quantities of dust that obscure the region at other wavelengths, and a scene of striking complexity is revealed. We produce total intensity and spectral index mosaics of the region from 20 pointings (144 hours on-target in total), covering 6.5 square degrees with an angular resolution of 4$"$,at a central frequency of 1.28 GHz. Many new features are revealed for the first time due to a combination of MeerKAT's high sensitivity, exceptional $u,v$-plane coverage, and geographical vantage point. We highlight some initial survey results, including new supernova remnant candidates, many new non-thermal filament complexes, and enhanced views of the Radio Arc Bubble, Sgr A and Sgr B regions. This project is a SARAO public legacy survey, and the image products are made available with this article. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.10541v3-abstract-full').style.display = 'none'; document.getElementById('2201.10541v3-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 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 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">29 pages, 15 figures, 3 tables, accepted for publication in the The Astrophysical Journal. Replacement arXiv version with higher quality 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/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> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.05673">arXiv:2111.05673</a> <span> [<a href="https://arxiv.org/pdf/2111.05673">pdf</a>, <a href="https://arxiv.org/format/2111.05673">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202141488">10.1051/0004-6361/202141488 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MeerKAT Galaxy Cluster Legacy Survey I. Survey Overview and Highlights </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Knowles%2C+K">K. Knowles</a>, <a href="/search/astro-ph?searchtype=author&query=Cotton%2C+W+D">W. D. Cotton</a>, <a href="/search/astro-ph?searchtype=author&query=Rudnick%2C+L">L. Rudnick</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Goedhart%2C+S">S. Goedhart</a>, <a href="/search/astro-ph?searchtype=author&query=Deane%2C+R">R. Deane</a>, <a href="/search/astro-ph?searchtype=author&query=Ramatsoku%2C+M">M. Ramatsoku</a>, <a href="/search/astro-ph?searchtype=author&query=Bietenholz%2C+M+F">M. F. Bietenholz</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%BCggen%2C+M">M. Br眉ggen</a>, <a href="/search/astro-ph?searchtype=author&query=Button%2C+C">C. Button</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+H">H. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chibueze%2C+J+O">J. O. Chibueze</a>, <a href="/search/astro-ph?searchtype=author&query=Clarke%2C+T+E">T. E. Clarke</a>, <a href="/search/astro-ph?searchtype=author&query=de+Gasperin%2C+F">F. de Gasperin</a>, <a href="/search/astro-ph?searchtype=author&query=Ianjamasimanana%2C+R">R. Ianjamasimanana</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%B3zsa%2C+G+I+G">G. I. G. J贸zsa</a>, <a href="/search/astro-ph?searchtype=author&query=Hilton%2C+M">M. Hilton</a>, <a href="/search/astro-ph?searchtype=author&query=Kesebonye%2C+K+C">K. C. Kesebonye</a>, <a href="/search/astro-ph?searchtype=author&query=Kolokythas%2C+K">K. Kolokythas</a>, <a href="/search/astro-ph?searchtype=author&query=Kraan-Korteweg%2C+R+C">R. C. Kraan-Korteweg</a>, <a href="/search/astro-ph?searchtype=author&query=Lawrie%2C+G">G. Lawrie</a>, <a href="/search/astro-ph?searchtype=author&query=Lochner%2C+M">M. Lochner</a>, <a href="/search/astro-ph?searchtype=author&query=Loubser%2C+S+I">S. I. Loubser</a>, <a href="/search/astro-ph?searchtype=author&query=Marchegiani%2C+P">P. Marchegiani</a>, <a href="/search/astro-ph?searchtype=author&query=Mhlahlo%2C+N">N. Mhlahlo</a> , et al. (126 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="2111.05673v1-abstract-short" style="display: inline;"> MeerKAT's large number of antennas, spanning 8 km with a densely packed 1 km core, create a powerful instrument for wide-area surveys, with high sensitivity over a wide range of angular scales. The MeerKAT Galaxy Cluster Legacy Survey (MGCLS) is a programme of long-track MeerKAT L-band (900-1670 MHz) observations of 115 galaxy clusters, observed for $\sim$6-10 hours each in full polarisation. The… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05673v1-abstract-full').style.display = 'inline'; document.getElementById('2111.05673v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.05673v1-abstract-full" style="display: none;"> MeerKAT's large number of antennas, spanning 8 km with a densely packed 1 km core, create a powerful instrument for wide-area surveys, with high sensitivity over a wide range of angular scales. The MeerKAT Galaxy Cluster Legacy Survey (MGCLS) is a programme of long-track MeerKAT L-band (900-1670 MHz) observations of 115 galaxy clusters, observed for $\sim$6-10 hours each in full polarisation. The first legacy product data release (DR1), made available with this paper, includes the MeerKAT visibilities, basic image cubes at $\sim$8" resolution, and enhanced spectral and polarisation image cubes at $\sim$8" and 15" resolutions. Typical sensitivities for the full-resolution MGCLS image products are $\sim$3-5 渭Jy/beam. The basic cubes are full-field and span 4 deg^2. The enhanced products consist of the inner 1.44 deg^2 field of view, corrected for the primary beam. The survey is fully sensitive to structures up to $\sim$10' scales and the wide bandwidth allows spectral and Faraday rotation mapping. HI mapping at 209 kHz resolution can be done at $0<z<0.09$ and $0.19<z<0.48$. In this paper, we provide an overview of the survey and DR1 products, including caveats for usage. We present some initial results from the survey, both for their intrinsic scientific value and to highlight the capabilities for further exploration with these data. These include a primary beam-corrected compact source catalogue of $\sim$626,000 sources for the full survey, and an optical/infrared cross-matched catalogue for compact sources in Abell 209 and Abell S295. We examine dust unbiased star-formation rates as a function of clustercentric radius in Abell 209 and present a catalogue of 99 diffuse cluster sources (56 are new), some of which have no suitable characterisation. We also highlight some of the radio galaxies which challenge current paradigms and present first results from HI studies of four targets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05673v1-abstract-full').style.display = 'none'; document.getElementById('2111.05673v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">43 pages, 33 figures, 6 tables. Accepted for publication in Astronomy and Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.03946">arXiv:2108.03946</a> <span> [<a href="https://arxiv.org/pdf/2108.03946">pdf</a>, <a href="https://arxiv.org/format/2108.03946">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/stab2474">10.1093/mnras/stab2474 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Timing observations of three Galactic millisecond pulsars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lorimer%2C+D+R">D. R. Lorimer</a>, <a href="/search/astro-ph?searchtype=author&query=Kawash%2C+A+M">A. M. Kawash</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=Smith%2C+D+A">D. A. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Kerr%2C+M">M. Kerr</a>, <a href="/search/astro-ph?searchtype=author&query=McLaughlin%2C+M+A">M. A. McLaughlin</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=Spiewak%2C+R">R. Spiewak</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">E. Barr</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=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+S">S. Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Jankowski%2C+F">F. Jankowski</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=Keith%2C+M">M. Keith</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> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2108.03946v2-abstract-short" style="display: inline;"> We report observed and derived timing parameters for three millisecond pulsars (MSPs) from observations collected with the Parkes 64-m telescope, Murriyang. The pulsars were found during re-processing of archival survey data by Mickaliger et al. One of the new pulsars (PSR J1546-5925) has a spin period $P=7.8$ ms and is isolated. The other two (PSR J0921-5202 with $P=9.7$ ms and PSR J1146-6610 wit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.03946v2-abstract-full').style.display = 'inline'; document.getElementById('2108.03946v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.03946v2-abstract-full" style="display: none;"> We report observed and derived timing parameters for three millisecond pulsars (MSPs) from observations collected with the Parkes 64-m telescope, Murriyang. The pulsars were found during re-processing of archival survey data by Mickaliger et al. One of the new pulsars (PSR J1546-5925) has a spin period $P=7.8$ ms and is isolated. The other two (PSR J0921-5202 with $P=9.7$ ms and PSR J1146-6610 with $P=3.7$ ms) are in binary systems around low-mass ($>0.2 M_{\odot}$) companions. Their respective orbital periods are $38$.2 d and $62.8$ d. While PSR J0921-5202 has a low orbital eccentricity $e=1.3 \times 10^{-5}$, in keeping with many other Galactic MSPs, PSR J1146-6610 has a significantly larger eccentricity, $e = 7.4 \times 10^{-3}$. This makes it a likely member of a group of eccentric MSP-He white dwarf binary systems in the Galactic disk whose formation is poorly understood. Two of the pulsars are co-located with previously unidentified point sources discovered with the Fermi satellite's Large Area Telescope, but no $纬$-ray pulsations have been detected, likely due to their low spin-down powers. We also show that, particularly in terms of orbital diversity, the current sample of MSPs is far from complete and is subject to a number of selection biases. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.03946v2-abstract-full').style.display = 'none'; document.getElementById('2108.03946v2-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 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">8 pages, 2 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/2108.02320">arXiv:2108.02320</a> <span> [<a href="https://arxiv.org/pdf/2108.02320">pdf</a>, <a href="https://arxiv.org/format/2108.02320">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/10.3847/1538-4357/ac375d">10.3847/1538-4357/ac375d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Study of 72 pulsars discovered in the PALFA survey: Timing analysis, glitch activity, emission variability, and a pulsar in an eccentric binary </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Parent%2C+E">E. Parent</a>, <a href="/search/astro-ph?searchtype=author&query=Sewalls%2C+H">H. Sewalls</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=Matheny%2C+T">T. Matheny</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=Perera%2C+B+B+P">B. B. P. Perera</a>, <a href="/search/astro-ph?searchtype=author&query=Cardoso%2C+F">F. Cardoso</a>, <a href="/search/astro-ph?searchtype=author&query=McLaughlin%2C+M+A">M. A. McLaughlin</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+B">B. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Brazier%2C+A">A. Brazier</a>, <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Chatterjee%2C+S">S. Chatterjee</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=Crawford%2C+F">F. Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=Deneva%2C+J+S">J. S. Deneva</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+F+A">F. A. Dong</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=Fonseca%2C+E">E. Fonseca</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=Kaspi%2C+V+M">V. M. Kaspi</a>, <a href="/search/astro-ph?searchtype=author&query=Knispel%2C+B">B. Knispel</a>, <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+J">J. van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=Lynch%2C+R+S">R. S. Lynch</a>, <a href="/search/astro-ph?searchtype=author&query=Meyers%2C+B+M">B. M. Meyers</a>, <a href="/search/astro-ph?searchtype=author&query=McKee%2C+J+W">J. W. McKee</a> , et al. (9 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2108.02320v3-abstract-short" style="display: inline;"> We present new discoveries and results from long-term timing of 72 pulsars discovered in the Arecibo PALFA survey, including precise determination of astrometric and spin parameters, and flux density and scatter broadening measurements at 1.4 GHz. Notable discoveries include two young pulsars (characteristic ages $\sim$30 kyr) with no apparent supernova remnant associations, three mode changing, 1… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.02320v3-abstract-full').style.display = 'inline'; document.getElementById('2108.02320v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.02320v3-abstract-full" style="display: none;"> We present new discoveries and results from long-term timing of 72 pulsars discovered in the Arecibo PALFA survey, including precise determination of astrometric and spin parameters, and flux density and scatter broadening measurements at 1.4 GHz. Notable discoveries include two young pulsars (characteristic ages $\sim$30 kyr) with no apparent supernova remnant associations, three mode changing, 12 nulling and two intermittent pulsars. We detected eight glitches in five pulsars. Among them is PSR J1939+2609, an apparently old pulsar (characteristic age $\sim$1 Gy), and PSR J1954+2529, which likely belongs to a newly-emerging class of binary pulsars. The latter is the only pulsar among the 72 that is clearly not isolated: a non-recycled neutron star with a 931-ms spin period in an eccentric ($e\,=\,0.114$) wide ($P_b\,=\,82.7\,$d) orbit with a companion of undetermined nature having a minimum mass of $\sim0.6\,M_{\odot}$. Since operations at Arecibo ceased in 2020 August, we give a final tally of PALFA sky coverage, and compare its 207 pulsar discoveries to the known population. On average, they are 50% more distant than other Galactic plane radio pulsars; PALFA millisecond pulsars (MSP) have twice the dispersion measure per unit spin period than the known population of MSP in the Plane. The four intermittent pulsars discovered by PALFA more than double the population of such objects, which should help to improve our understanding of pulsar magnetosphere physics. The statistics for these, RRATS, and nulling pulsars suggest that there are many more of these objects in the Galaxy than was previously thought. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.02320v3-abstract-full').style.display = 'none'; document.getElementById('2108.02320v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">39 pages, 18 figures, 9 tables. 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/2106.05340">arXiv:2106.05340</a> <span> [<a href="https://arxiv.org/pdf/2106.05340">pdf</a>, <a href="https://arxiv.org/format/2106.05340">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac0880">10.3847/1538-4357/ac0880 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Threads, Ribbons, and Rings in the Radio Galaxy IC 4296 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Condon%2C+J+J">J. J. Condon</a>, <a href="/search/astro-ph?searchtype=author&query=Cotton%2C+W+D">W. D. Cotton</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+S+V">S. V. White</a>, <a href="/search/astro-ph?searchtype=author&query=Legodi%2C+S">S. Legodi</a>, <a href="/search/astro-ph?searchtype=author&query=Goedhart%2C+S">S. Goedhart</a>, <a href="/search/astro-ph?searchtype=author&query=McAlpine%2C+K">K. McAlpine</a>, <a href="/search/astro-ph?searchtype=author&query=Ratcliffe%2C+S+M">S. M. Ratcliffe</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="2106.05340v1-abstract-short" style="display: inline;"> The nearby elliptical galaxy IC4296 has produced a large (510 kpc) low-luminosity radio source with typical FR I core/jet/lobe morphology. The unprecedented combination of brightness sensitivity, dynamic range, and angular resolution of a new 1.28 GHz MeerKAT continuum image reveals striking new morphological features which we call threads, ribbons, and rings. The threads are faint narrow emission… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.05340v1-abstract-full').style.display = 'inline'; document.getElementById('2106.05340v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.05340v1-abstract-full" style="display: none;"> The nearby elliptical galaxy IC4296 has produced a large (510 kpc) low-luminosity radio source with typical FR I core/jet/lobe morphology. The unprecedented combination of brightness sensitivity, dynamic range, and angular resolution of a new 1.28 GHz MeerKAT continuum image reveals striking new morphological features which we call threads, ribbons, and rings. The threads are faint narrow emission features originating where helical Kelvin-Helmholtz instabilities disrupt the main radio jets. The ribbons are smooth regions between the jets and the lobes, and they appear to be relics of jets powered by earlier activity that have since come into pressure equilibrium. Vortex rings in the outer portions of the lobes and their backflows indicate that the straight outer jets and ribbons are inclined by $i = 60 \pm 5^\circ$ from the line-of-sight, in agreement with photometric, geometric, and gas-dynamical estimates of inclination angles near the nucleus. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.05340v1-abstract-full').style.display = 'none'; document.getElementById('2106.05340v1-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 12 figures ApJ accepted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.00386">arXiv:2106.00386</a> <span> [<a href="https://arxiv.org/pdf/2106.00386">pdf</a>, <a href="https://arxiv.org/format/2106.00386">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/ac0720">10.3847/1538-4357/ac0720 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radio Detection of PSR J1813-1749 in HESS J1813-178: The Most Scattered Pulsar Known </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Camilo%2C+F">F. Camilo</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=Halpern%2C+J+P">J. P. Halpern</a>, <a href="/search/astro-ph?searchtype=author&query=Roshi%2C+D+A">D. A. Roshi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.00386v1-abstract-short" style="display: inline;"> The 44.7 ms X-ray pulsar in the supernova remnant G12.82-0.02/HESS J1813-178 has the second highest spin-down luminosity of known pulsars in the Galaxy, with E-dot=5.6e37 erg/s. Using the Green Bank Telescope, we have detected radio pulsations from PSR J1813-1749 at 4.4-10.2 GHz. The pulse is highly scattered, with an exponential decay timescale 蟿longer than that of any other pulsar at these frequ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.00386v1-abstract-full').style.display = 'inline'; document.getElementById('2106.00386v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.00386v1-abstract-full" style="display: none;"> The 44.7 ms X-ray pulsar in the supernova remnant G12.82-0.02/HESS J1813-178 has the second highest spin-down luminosity of known pulsars in the Galaxy, with E-dot=5.6e37 erg/s. Using the Green Bank Telescope, we have detected radio pulsations from PSR J1813-1749 at 4.4-10.2 GHz. The pulse is highly scattered, with an exponential decay timescale 蟿longer than that of any other pulsar at these frequencies. A point source detected at this position by Dzib et al. in several observations with the Jansky Very Large Array can be attributed to the pulsed emission. The steep dependence of 蟿on observing frequency explains why all previous pulsation searches at lower frequencies failed (蟿~0.25 s at 2 GHz). The large dispersion measure, DM=1087 pc/cc, indicates a distance of either 6.2 or 12 kpc according to two widely used models of the electron density distribution in the Galaxy. These disfavor a previously suggested association with a young stellar cluster at the closer distance of 4.8 kpc. The high X-ray measured column density of ~1e23/cm^2 also supports a large distance. If at d~12 kpc, HESS J1813-178 would be one of the most luminous TeV sources in the Galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.00386v1-abstract-full').style.display = 'none'; document.getElementById('2106.00386v1-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by ApJ; 8 pages, 7 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/2103.04800">arXiv:2103.04800</a> <span> [<a href="https://arxiv.org/pdf/2103.04800">pdf</a>, <a href="https://arxiv.org/format/2103.04800">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/stab790">10.1093/mnras/stab790 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Eight new millisecond pulsars from the first MeerKAT globular cluster census </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=Gautam%2C+T">T. Gautam</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=Ransom%2C+S+M">S. M. Ransom</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+S+J">S. J. Buchner</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=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</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=Abbate%2C+F">F. Abbate</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=Camilo%2C+F">F. Camilo</a>, <a href="/search/astro-ph?searchtype=author&query=Corongiu%2C+A">A. Corongiu</a>, <a href="/search/astro-ph?searchtype=author&query=Jameson%2C+A">A. Jameson</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=Vleeschower%2C+L">L. Vleeschower</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=Geyer%2C+M">M. Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Karastergiou%2C+A">A. Karastergiou</a>, <a href="/search/astro-ph?searchtype=author&query=Karuppusamy%2C+R">R. Karuppusamy</a>, <a href="/search/astro-ph?searchtype=author&query=Parthasarathy%2C+A">A. Parthasarathy</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=Serylak%2C+M">M. Serylak</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="2103.04800v1-abstract-short" style="display: inline;"> We have used the central 44 antennas of the new 64-dish MeerKAT radio telescope array to conduct a deep search for new pulsars in the core of nine globular clusters. This has led to the discovery of eight new millisecond pulsars in six different clusters. Two new binaries, 47 Tuc ac and 47 Tuc ad, are eclipsing "spiders", featuring compact orbits ($\lesssim 0.32$ days), very low-mass companions an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.04800v1-abstract-full').style.display = 'inline'; document.getElementById('2103.04800v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.04800v1-abstract-full" style="display: none;"> We have used the central 44 antennas of the new 64-dish MeerKAT radio telescope array to conduct a deep search for new pulsars in the core of nine globular clusters. This has led to the discovery of eight new millisecond pulsars in six different clusters. Two new binaries, 47 Tuc ac and 47 Tuc ad, are eclipsing "spiders", featuring compact orbits ($\lesssim 0.32$ days), very low-mass companions and regular occultations of their pulsed emission. The other three new binary pulsars (NGC 6624G, M62G, and Ter 5 an) are in wider ($> 0.7$ days) orbits, with companions that are likely to be white dwarfs or neutron stars. NGC 6624G has a large eccentricity of $e\simeq 0.38$, which enabled us to detect the rate of advance of periastron. This suggests that the system is massive, with a total mass of $M{\rm tot} = 2.65 \pm 0.07$ M$_{\odot}$. Likewise, for Ter 5 an, with $e \simeq 0.0066$, we obtain $M{\rm tot}= 2.97 \pm 0.52$ M$_{\odot}$. The other three new discoveries (NGC 6522D, NGC 6624H and NGC 6752F) are faint isolated pulsars. Finally, we have used the whole MeerKAT array and synthesized 288 beams, covering an area of $\sim2$ arcmin in radius around the center of NGC 6624. This has allowed us to localize many of the pulsars in the cluster, demonstrating the beamforming capabilities of the TRAPUM software backend and paving the way for the upcoming MeerKAT globular cluster pulsar survey. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.04800v1-abstract-full').style.display = 'none'; document.getElementById('2103.04800v1-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 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 10 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/2102.05160">arXiv:2102.05160</a> <span> [<a href="https://arxiv.org/pdf/2102.05160">pdf</a>, <a href="https://arxiv.org/format/2102.05160">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/10.1093/mnras/stab375">10.1093/mnras/stab375 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Relativistic Binary Programme on MeerKAT: Science objectives and first results </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=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=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=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=Cognard%2C+I">I. Cognard</a>, <a href="/search/astro-ph?searchtype=author&query=Gautam%2C+T">T. Gautam</a>, <a href="/search/astro-ph?searchtype=author&query=Geyer%2C+M">M. Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Guillemot%2C+L">L. Guillemot</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">G. Janssen</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=Parthasarathy%2C+A">A. Parthasarathy</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=Reardon%2C+D+J">D. J. Reardon</a>, <a href="/search/astro-ph?searchtype=author&query=Ridolfi%2C+A">A. Ridolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Serylak%2C+M">M. Serylak</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=Theureau%2C+G">G. Theureau</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="2102.05160v2-abstract-short" style="display: inline;"> We describe the ongoing Relativistic Binary programme (RelBin), a part of the MeerTime large survey project with the MeerKAT radio telescope. RelBin is primarily focused on observations of relativistic effects in binary pulsars to enable measurements of neutron star masses and tests of theories of gravity. We selected 25 pulsars as an initial high priority list of targets based on their characteri… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.05160v2-abstract-full').style.display = 'inline'; document.getElementById('2102.05160v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.05160v2-abstract-full" style="display: none;"> We describe the ongoing Relativistic Binary programme (RelBin), a part of the MeerTime large survey project with the MeerKAT radio telescope. RelBin is primarily focused on observations of relativistic effects in binary pulsars to enable measurements of neutron star masses and tests of theories of gravity. We selected 25 pulsars as an initial high priority list of targets based on their characteristics and observational history with other telescopes. In this paper, we provide an outline of the programme, present polarisation calibrated pulse profiles for all selected pulsars as a reference catalogue along with updated dispersion measures. We report Faraday rotation measures for 24 pulsars, twelve of which have been measured for the first time. More than a third of our selected pulsars show a flat position angle swing confirming earlier observations. We demonstrate the ability of the Rotating Vector Model (RVM), fitted here to seven binary pulsars, including the Double Pulsar (PSR J0737$-$3039A), to obtain information about the orbital inclination angle. We present a high time resolution light curve of the eclipse of PSR J0737$-$3039A by the companion's magnetosphere, a high-phase resolution position angle swing for PSR J1141$-$6545, an improved detection of the Shapiro delay of PSR J1811$-$2405, and pulse scattering measurements for PSRs J1227$-$6208, J1757$-$1854, and J1811$-$1736. Finally, we demonstrate that timing observations with MeerKAT improve on existing data sets by a factor of, typically, 2-3, sometimes by an order of magnitude. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.05160v2-abstract-full').style.display = 'none'; document.getElementById('2102.05160v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages 16 figures, published in MNRAS (replaced earlier submission after small changes added in proofs)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.08531">arXiv:2101.08531</a> <span> [<a href="https://arxiv.org/pdf/2101.08531">pdf</a>, <a href="https://arxiv.org/format/2101.08531">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/stab037">10.1093/mnras/stab037 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurements of pulse jitter and single-pulse variability in millisecond pulsars using MeerKAT </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=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=Oslowski%2C+S">S. Oslowski</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+S">S. Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Spiewak%2C+R">R. Spiewak</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=Kramer%2C+M">M. Kramer</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=Pennucici%2C+T+T">T. T. Pennucici</a>, <a href="/search/astro-ph?searchtype=author&query=Abbate%2C+F">F. Abbate</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>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Geyer%2C+M">M. Geyer</a>, <a href="/search/astro-ph?searchtype=author&query=Hugo%2C+B">B. Hugo</a>, <a href="/search/astro-ph?searchtype=author&query=Jameson%2C+A">A. Jameson</a>, <a href="/search/astro-ph?searchtype=author&query=Karastergiou%2C+A">A. Karastergiou</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=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="2101.08531v1-abstract-short" style="display: inline;"> Using the state-of-the-art SKA precursor, the MeerKAT radio telescope, we explore the limits to precision pulsar timing of millisecond pulsars achievable due to pulse stochasticity (jitter). We report new jitter measurements in 15 of the 29 pulsars in our sample and find that the levels of jitter can vary dramatically between them. For some, like the 2.2~ms pulsar PSR J2241--5236, we measure an im… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.08531v1-abstract-full').style.display = 'inline'; document.getElementById('2101.08531v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.08531v1-abstract-full" style="display: none;"> Using the state-of-the-art SKA precursor, the MeerKAT radio telescope, we explore the limits to precision pulsar timing of millisecond pulsars achievable due to pulse stochasticity (jitter). We report new jitter measurements in 15 of the 29 pulsars in our sample and find that the levels of jitter can vary dramatically between them. For some, like the 2.2~ms pulsar PSR J2241--5236, we measure an implied jitter of just $\sim$ 4~ns/hr, while others like the 3.9~ms PSR J0636--3044 are limited to $\sim$ 100 ns/hr. While it is well known that jitter plays a central role to limiting the precision measurements of arrival times for high signal-to-noise ratio observations, its role in the measurement of dispersion measure (DM) has not been reported, particularly in broad-band observations. Using the exceptional sensitivity of MeerKAT, we explored this on the bright millisecond pulsar PSR J0437--4715 by exploring the DM of literally every pulse. We found that the derived single pulse DMs vary by typically 0.0085 cm$^{-3}$ pc from the mean, and that the best DM estimate is limited by the differential pulse jitter across the band. We postulate that all millisecond pulsars will have their own limit on DM precision which can only be overcome with longer integrations. Using high-time resolution filterbank data of 9 $渭$s, we also present a statistical analysis of single pulse phenomenology. Finally, we discuss optimization strategies for the MeerKAT pulsar timing program and its role in the context of the International Pulsar Timing Array (IPTA). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.08531v1-abstract-full').style.display = 'none'; document.getElementById('2101.08531v1-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 9 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> https://ui.adsabs.harvard.edu/abs/2021MNRAS.tmp...69P/abstract </p> </li> </ol> <nav 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