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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=Petroff%2C+E&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Petroff%2C+E&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Petroff%2C+E&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.22468">arXiv:2410.22468</a> <span> [<a href="https://arxiv.org/pdf/2410.22468">pdf</a>, <a href="https://arxiv.org/format/2410.22468">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> frb-voe: A Real-time Virtual Observatory Event Alert Service for Fast Radio Bursts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+C">Thomas C. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Zwaniga%2C+A+V">Andrew V. Zwaniga</a>, <a href="/search/astro-ph?searchtype=author&query=Brar%2C+C">Charanjot Brar</a>, <a href="/search/astro-ph?searchtype=author&query=Kaspi%2C+V+M">Victoria M. Kaspi</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">Emily Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">Mohit Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+P+J">P. J. Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+A+M">Amanda M. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Joseph%2C+R+C">Ronny C. Joseph</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K+W">Kiyoshi W. Masui</a>, <a href="/search/astro-ph?searchtype=author&query=Pandhi%2C+A">Ayush Pandhi</a>, <a href="/search/astro-ph?searchtype=author&query=Pleunis%2C+Z">Ziggy Pleunis</a>, <a href="/search/astro-ph?searchtype=author&query=Scholz%2C+P">Paul Scholz</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+K">Kaitlyn Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Tendulkar%2C+S">Shriharsh Tendulkar</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="2410.22468v1-abstract-short" style="display: inline;"> We present frb-voe, a publicly available software package that enables radio observatories to broadcast fast radio burst (FRB) alerts to subscribers through low-latency virtual observatory events (VOEvents). We describe a use-case of frb-voe by the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst (CHIME/FRB) Collaboration, which has broadcast thousands of FRB alerts to subscribers w… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.22468v1-abstract-full').style.display = 'inline'; document.getElementById('2410.22468v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.22468v1-abstract-full" style="display: none;"> We present frb-voe, a publicly available software package that enables radio observatories to broadcast fast radio burst (FRB) alerts to subscribers through low-latency virtual observatory events (VOEvents). We describe a use-case of frb-voe by the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst (CHIME/FRB) Collaboration, which has broadcast thousands of FRB alerts to subscribers worldwide. Using this service, observers have daily opportunities to conduct rapid multi-wavelength follow-up observations of new FRB sources. Alerts are distributed as machine-readable reports and as emails containing FRB metadata, and are available to the public within approximately 13 seconds of detection. A sortable database and a downloadable JSON file containing FRB metadata from all broadcast alerts can be found on the CHIME/FRB public webpage. The frb-voe service also provides users with the ability to retrieve FRB names from the Transient Name Server (TNS) through the frb-voe client user interface (CLI). The frb-voe service can act as a foundation on which any observatory that detects FRBs can build its own VOEvent broadcasting service to contribute to the coordinated multi-wavelength follow-up of astrophysical transients. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.22468v1-abstract-full').style.display = 'none'; document.getElementById('2410.22468v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to The Astronomical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.00482">arXiv:2406.00482</a> <span> [<a href="https://arxiv.org/pdf/2406.00482">pdf</a>, <a href="https://arxiv.org/format/2406.00482">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"> Comprehensive analysis of the Apertif Fast Radio Burst sample: similarities with young, energetic neutron stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pastor-Marazuela%2C+I">In茅s Pastor-Marazuela</a>, <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+J">Joeri van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=Bilous%2C+A">Anna Bilous</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">Liam Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Maan%2C+Y">Yogesh Maan</a>, <a href="/search/astro-ph?searchtype=author&query=Oostrum%2C+L">Leon Oostrum</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">Emily Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Vohl%2C+D">Dany Vohl</a>, <a href="/search/astro-ph?searchtype=author&query=Hess%2C+K+M">Kelley M. Hess</a>, <a href="/search/astro-ph?searchtype=author&query=Orr%C3%B9%2C+E">Emanuela Orr霉</a>, <a href="/search/astro-ph?searchtype=author&query=Sclocco%2C+A">Alessio Sclocco</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Yuyang Wang</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="2406.00482v2-abstract-short" style="display: inline;"> Understanding the origin of fast radio bursts (FRBs) has become the main science driver of recent dedicated FRB surveys. Between July 2019 and February 2022, we carried out ALERT, an FRB survey at 1370 MHz using the Apertif instrument installed at the Westerbork Synthesis Radio Telescope (WSRT). Here we report the detection of 18 new FRBs, and we study the properties of the entire 24 burst sample… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.00482v2-abstract-full').style.display = 'inline'; document.getElementById('2406.00482v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.00482v2-abstract-full" style="display: none;"> Understanding the origin of fast radio bursts (FRBs) has become the main science driver of recent dedicated FRB surveys. Between July 2019 and February 2022, we carried out ALERT, an FRB survey at 1370 MHz using the Apertif instrument installed at the Westerbork Synthesis Radio Telescope (WSRT). Here we report the detection of 18 new FRBs, and we study the properties of the entire 24 burst sample detected during the survey. For five bursts, we identify host galaxy candidates with >50% probability association. We observe an average linear polarisation fraction of $\sim$43% and an average circular polarisation fraction consistent with 0%. A third of the FRBs display multiple components. The sample next reveals a population of highly scattered bursts, which is most likely to have been produced in the immediate circumburst environment. Furthermore, two FRBs show evidence for high rotation measures, reaching |RM|>$10^3$ rad m$^{-2}$ in the source reference frames. Together, the scattering and rotation measures ALERT finds prove that a large fraction of FRBs are embedded in complex media such as star forming regions or supernova remnants. Through the discovery of the third most dispersed FRB so far, we show that one-off FRBs can emit at frequencies in excess of 6 GHz. Finally, we determine an FRB all-sky rate of $459^{+208}_{-155}$ sky$^{-1}$ day$^{-1}$ above a fluence limit of 4.1 Jy ms, and a fluence cumulative distribution with a power law index $纬=-1.23\pm0.06\pm0.2$, which is roughly consistent with the Euclidean Universe predictions. Through the high resolution in time, frequency, polarisation and localisation that ALERT featured, we were able to determine the morphological complexity, polarisation, local scattering and magnetic environment, and high-frequency luminosity of FRBs. We find all these strongly resemble those seen in young, energetic, highly magnetised neutron stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.00482v2-abstract-full').style.display = 'none'; document.getElementById('2406.00482v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 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">40 pages (including 11 of appendix), 37 figures, 5 tables. Accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.07898">arXiv:2402.07898</a> <span> [<a href="https://arxiv.org/pdf/2402.07898">pdf</a>, <a href="https://arxiv.org/format/2402.07898">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> CHIME/FRB Outriggers: KKO Station System and Commissioning Results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lanman%2C+A+E">Adam E. Lanman</a>, <a href="/search/astro-ph?searchtype=author&query=Andrew%2C+S">Shion Andrew</a>, <a href="/search/astro-ph?searchtype=author&query=Lazda%2C+M">Mattias Lazda</a>, <a href="/search/astro-ph?searchtype=author&query=Shah%2C+V">Vishwangi Shah</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Balasubramanian%2C+A">Arvind Balasubramanian</a>, <a href="/search/astro-ph?searchtype=author&query=Bandura%2C+K">Kevin Bandura</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+P+J">P. J. Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Brar%2C+C">Charanjot Brar</a>, <a href="/search/astro-ph?searchtype=author&query=Carlson%2C+M">Mark Carlson</a>, <a href="/search/astro-ph?searchtype=author&query=Cliche%2C+J">Jean-Fran莽ois Cliche</a>, <a href="/search/astro-ph?searchtype=author&query=Gusinskaia%2C+N">Nina Gusinskaia</a>, <a href="/search/astro-ph?searchtype=author&query=Hendricksen%2C+I+T">Ian T. Hendricksen</a>, <a href="/search/astro-ph?searchtype=author&query=Kaczmarek%2C+J+F">J. F. Kaczmarek</a>, <a href="/search/astro-ph?searchtype=author&query=Landecker%2C+T">Tom Landecker</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">Calvin Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Mckinven%2C+R">Ryan Mckinven</a>, <a href="/search/astro-ph?searchtype=author&query=Mena-Parra%2C+J">Juan Mena-Parra</a>, <a href="/search/astro-ph?searchtype=author&query=Milutinovic%2C+N">Nikola Milutinovic</a>, <a href="/search/astro-ph?searchtype=author&query=Nimmo%2C+K">Kenzie Nimmo</a>, <a href="/search/astro-ph?searchtype=author&query=Pearlman%2C+A+B">Aaron B. Pearlman</a>, <a href="/search/astro-ph?searchtype=author&query=Renard%2C+A">Andre Renard</a>, <a href="/search/astro-ph?searchtype=author&query=Rahman%2C+M">Mubdi Rahman</a>, <a href="/search/astro-ph?searchtype=author&query=Shaw%2C+J+R">J. Richard Shaw</a>, <a href="/search/astro-ph?searchtype=author&query=Siegel%2C+S+R">Seth R. Siegel</a> , et al. (21 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="2402.07898v2-abstract-short" style="display: inline;"> Localizing fast radio bursts (FRBs) to their host galaxies is an essential step to better understanding their origins and using them as cosmic probes. The CHIME/FRB Outrigger program aims to add VLBI-localization capabilities to CHIME, such that FRBs may be localized to tens of milliarcsecond precision at the time of their discovery, more than sufficient for host galaxy identification. The first-b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.07898v2-abstract-full').style.display = 'inline'; document.getElementById('2402.07898v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.07898v2-abstract-full" style="display: none;"> Localizing fast radio bursts (FRBs) to their host galaxies is an essential step to better understanding their origins and using them as cosmic probes. The CHIME/FRB Outrigger program aims to add VLBI-localization capabilities to CHIME, such that FRBs may be localized to tens of milliarcsecond precision at the time of their discovery, more than sufficient for host galaxy identification. The first-built outrigger telescope is KKO, located 66 kilometers west of CHIME. Cross-correlating KKO with CHIME can achieve arcsecond-scale localization in right ascension while avoiding the worst effects of the ionosphere. This paper presents measurements of KKO's performance throughout its commissioning phase, as well as a summary of its design and function. We demonstrate KKO's capabilities as a standalone instrument by producing full-sky images, mapping the angular and frequency structure of the primary beam, and measuring feed positions. To demonstrate the localization capabilities of the CHIME -- KKO baseline, we collected five separate observations each for a set of twenty bright pulsars, and aimed to measure their positions to within 5~arcseconds. All of these pulses were successfully localized to within this specification. The next two outriggers are expected to be commissioned in 2024, and will enable subarcsecond localizations for approximately hundreds of FRBs each year. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.07898v2-abstract-full').style.display = 'none'; document.getElementById('2402.07898v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 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">41 pages, 17 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/2401.17378">arXiv:2401.17378</a> <span> [<a href="https://arxiv.org/pdf/2401.17378">pdf</a>, <a href="https://arxiv.org/format/2401.17378">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"> Polarization properties of 128 non-repeating fast radio bursts from the first CHIME/FRB baseband catalog </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pandhi%2C+A">Ayush Pandhi</a>, <a href="/search/astro-ph?searchtype=author&query=Pleunis%2C+Z">Ziggy Pleunis</a>, <a href="/search/astro-ph?searchtype=author&query=Mckinven%2C+R">Ryan Mckinven</a>, <a href="/search/astro-ph?searchtype=author&query=Gaensler%2C+B+M">B. M. Gaensler</a>, <a href="/search/astro-ph?searchtype=author&query=Su%2C+J">Jianing Su</a>, <a href="/search/astro-ph?searchtype=author&query=Ng%2C+C">Cherry Ng</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">Mohit Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Brar%2C+C">Charanjot Brar</a>, <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">Tomas Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+A+M">Amanda M. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Curtin%2C+A+P">Alice P. Curtin</a>, <a href="/search/astro-ph?searchtype=author&query=Kaspi%2C+V+M">Victoria M. Kaspi</a>, <a href="/search/astro-ph?searchtype=author&query=Lazda%2C+M">Mattias Lazda</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">Calvin Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+D">Dongzi Li</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K+W">Kiyoshi W. Masui</a>, <a href="/search/astro-ph?searchtype=author&query=Michilli%2C+D">Daniele Michilli</a>, <a href="/search/astro-ph?searchtype=author&query=Nimmo%2C+K">Kenzie Nimmo</a>, <a href="/search/astro-ph?searchtype=author&query=Pearlman%2C+A">Aaron Pearlman</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">Emily Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Rafiei-Ravandi%2C+M">Masoud Rafiei-Ravandi</a>, <a href="/search/astro-ph?searchtype=author&query=Sand%2C+K+R">Ketan R. Sand</a>, <a href="/search/astro-ph?searchtype=author&query=Scholz%2C+P">Paul Scholz</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+K">Kaitlyn Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+K">Kendrick Smith</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.17378v2-abstract-short" style="display: inline;"> We present a 400-800 MHz polarimetric analysis of 128 non-repeating fast radio bursts (FRBs) from the first CHIME/FRB baseband catalog, increasing the total number of FRB sources with polarization properties by a factor of ~3. 89 FRBs have >6$蟽$ linearly polarized detections, 29 FRBs fall below this significance threshold and are deemed linearly unpolarized, and for 10 FRBs the polarization data a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17378v2-abstract-full').style.display = 'inline'; document.getElementById('2401.17378v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.17378v2-abstract-full" style="display: none;"> We present a 400-800 MHz polarimetric analysis of 128 non-repeating fast radio bursts (FRBs) from the first CHIME/FRB baseband catalog, increasing the total number of FRB sources with polarization properties by a factor of ~3. 89 FRBs have >6$蟽$ linearly polarized detections, 29 FRBs fall below this significance threshold and are deemed linearly unpolarized, and for 10 FRBs the polarization data are contaminated by instrumental polarization. For the 89 polarized FRBs, we find Faraday rotation measure (RM) amplitudes, after subtracting approximate Milky Way contributions, in the range 0.5-1160 rad m$^{-2}$ with a median of 53.8 rad m$^{-2}$. Most non-repeating FRBs in our sample have RMs consistent with Milky Way-like host galaxies and their linear polarization fractions range from <10% to 100% with a median of 63%. We see marginal evidence that non-repeating FRBs have more constraining lower limits than repeating FRBs for the host electron-density-weighted line-of-sight magnetic field strength. We classify the non-repeating FRB polarization position angle (PA) profiles into four archetypes: (i) single component with constant PA (57% of the sample), (ii) single component with variable PA (10%), (iii) multiple components with a single constant PA (22%), and (iv) multiple components with different or variable PAs (11%). We see no evidence for population-wide frequency-dependent depolarization and, therefore, the spread in the distribution of fractional linear polarization is likely intrinsic to the FRB emission mechanism. Finally, we present a novel method to derive redshift lower limits for polarized FRBs without host galaxy identification and test this method on 20 FRBs with independently measured redshifts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17378v2-abstract-full').style.display = 'none'; document.getElementById('2401.17378v2-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 30 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">44 pages, 18 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/2312.14133">arXiv:2312.14133</a> <span> [<a href="https://arxiv.org/pdf/2312.14133">pdf</a>, <a href="https://arxiv.org/format/2312.14133">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"> Morphologies of Bright Complex Fast Radio Bursts with CHIME/FRB Voltage Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Faber%2C+J+T">Jakob T. Faber</a>, <a href="/search/astro-ph?searchtype=author&query=Michilli%2C+D">Daniele Michilli</a>, <a href="/search/astro-ph?searchtype=author&query=Mckinven%2C+R">Ryan Mckinven</a>, <a href="/search/astro-ph?searchtype=author&query=Su%2C+J">Jianing Su</a>, <a href="/search/astro-ph?searchtype=author&query=Pearlman%2C+A+B">Aaron B. Pearlman</a>, <a href="/search/astro-ph?searchtype=author&query=Nimmo%2C+K">Kenzie Nimmo</a>, <a href="/search/astro-ph?searchtype=author&query=Main%2C+R+A">Robert A. Main</a>, <a href="/search/astro-ph?searchtype=author&query=Kaspi%2C+V">Victoria Kaspi</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">Mohit Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Chatterjee%2C+S">Shami Chatterjee</a>, <a href="/search/astro-ph?searchtype=author&query=Curtin%2C+A+P">Alice P. Curtin</a>, <a href="/search/astro-ph?searchtype=author&query=Dobbs%2C+M">Matt Dobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Eadie%2C+G">Gwendolyn Eadie</a>, <a href="/search/astro-ph?searchtype=author&query=Gaensler%2C+B+M">B. M. Gaensler</a>, <a href="/search/astro-ph?searchtype=author&query=Kader%2C+Z">Zarif Kader</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">Calvin Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K+W">Kiyoshi W. Masui</a>, <a href="/search/astro-ph?searchtype=author&query=Pandhi%2C+A">Ayush Pandhi</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">Emily Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Pleunis%2C+Z">Ziggy Pleunis</a>, <a href="/search/astro-ph?searchtype=author&query=Rafiei-Ravandi%2C+M">Masoud Rafiei-Ravandi</a>, <a href="/search/astro-ph?searchtype=author&query=Sand%2C+K+R">Ketan R. Sand</a>, <a href="/search/astro-ph?searchtype=author&query=Scholz%2C+P">Paul Scholz</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+K">Kaitlyn Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+K">Kendrick Smith</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.14133v2-abstract-short" style="display: inline;"> We present the discovery of twelve thus far non-repeating fast radio burst (FRB) sources, detected by the Canadian Hydrogen Intensity Mapping Experiment (CHIME) telescope. These sources were selected from a database comprising of order $10^3$ CHIME/FRB full-array raw voltage data recordings, based on their exceptionally high brightness and complex morphology. Our study examines the time-frequency… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.14133v2-abstract-full').style.display = 'inline'; document.getElementById('2312.14133v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.14133v2-abstract-full" style="display: none;"> We present the discovery of twelve thus far non-repeating fast radio burst (FRB) sources, detected by the Canadian Hydrogen Intensity Mapping Experiment (CHIME) telescope. These sources were selected from a database comprising of order $10^3$ CHIME/FRB full-array raw voltage data recordings, based on their exceptionally high brightness and complex morphology. Our study examines the time-frequency characteristics of these bursts, including drifting, microstructure, and periodicities. The events in this sample display a variety of unique drifting phenomenologies that deviate from the linear negative drifting phenomenon seen in many repeating FRBs, and motivate a possible new framework for classifying drifting archetypes. Additionally, we detect microstructure features of duration $\lesssim$ 50 $渭s$ in seven events, with some as narrow as $\approx$ 7 $渭s$. We find no evidence of significant periodicities. Furthermore, we report the polarization characteristics of seven events, including their polarization fractions and Faraday rotation measures (RMs). The observed $|\mathrm{RM}|$ values span a wide range of $17.24(2)$ - $328.06(2) \mathrm{~rad~m}^{-2}$, with linear polarization fractions between $0.340(1)$ - $0.946(3)$. The morphological properties of the bursts in our sample appear broadly consistent with predictions from both relativistic shock and magnetospheric models of FRB emission, as well as propagation through discrete ionized plasma structures. We address these models and discuss how they can be tested using our improved understanding of morphological archetypes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.14133v2-abstract-full').style.display = 'none'; document.getElementById('2312.14133v2-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 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">29 pages, 14 figures, submitted to ApJ, comments appreciated</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.00111">arXiv:2311.00111</a> <span> [<a href="https://arxiv.org/pdf/2311.00111">pdf</a>, <a href="https://arxiv.org/format/2311.00111">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"> Updating the first CHIME/FRB catalog of fast radio bursts with baseband data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+T+C">The CHIME/FRB Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+B+C">Bridget C. Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Andrew%2C+S">Shion Andrew</a>, <a href="/search/astro-ph?searchtype=author&query=Bandura%2C+K">Kevin Bandura</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">Mohit Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+P+J">P. J. Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Brar%2C+C">Charanjot Brar</a>, <a href="/search/astro-ph?searchtype=author&query=Breitman%2C+D">Daniela Breitman</a>, <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">Tomas Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Chawla%2C+P">Pragya Chawla</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+A+M">Amanda M. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Curtin%2C+A+P">Alice P. Curtin</a>, <a href="/search/astro-ph?searchtype=author&query=Dobbs%2C+M">Matt Dobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+F+A">Fengqiu Adam Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Eadie%2C+G">Gwendolyn Eadie</a>, <a href="/search/astro-ph?searchtype=author&query=Fonseca%2C+E">Emmanuel Fonseca</a>, <a href="/search/astro-ph?searchtype=author&query=Gaensler%2C+B+M">B. M. Gaensler</a>, <a href="/search/astro-ph?searchtype=author&query=Giri%2C+U">Utkarsh Giri</a>, <a href="/search/astro-ph?searchtype=author&query=Herrera-Martin%2C+A">Antonio Herrera-Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+H">Hans Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Ibik%2C+A+L">Adaeze L. Ibik</a>, <a href="/search/astro-ph?searchtype=author&query=Joseph%2C+R+C">Ronniy C. Joseph</a>, <a href="/search/astro-ph?searchtype=author&query=Kaczmarek%2C+J+F">J. F. Kaczmarek</a> , et al. (36 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.00111v2-abstract-short" style="display: inline;"> In 2021, a catalog of 536 fast radio bursts (FRBs) detected with the Canadian Hydrogen Intensity Mapping Experiment (CHIME) radio telescope was released by the CHIME/FRB Collaboration. This large collection of bursts, observed with a single instrument and uniform selection effects, has advanced our understanding of the FRB population. Here we update the results for 140 of these FRBs for which chan… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.00111v2-abstract-full').style.display = 'inline'; document.getElementById('2311.00111v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.00111v2-abstract-full" style="display: none;"> In 2021, a catalog of 536 fast radio bursts (FRBs) detected with the Canadian Hydrogen Intensity Mapping Experiment (CHIME) radio telescope was released by the CHIME/FRB Collaboration. This large collection of bursts, observed with a single instrument and uniform selection effects, has advanced our understanding of the FRB population. Here we update the results for 140 of these FRBs for which channelized raw voltage ('baseband') data are available. With the voltages measured by the telescope's antennas, it is possible to maximize the telescope sensitivity in any direction within the primary beam, an operation called 'beamforming'. This allows us to increase the signal-to-noise ratio (S/N) of the bursts and to localize them to sub-arcminute precision. The improved localization is also used to correct the beam response of the instrument and to measure fluxes and fluences with a ~10% uncertainty. Additionally, the time resolution is increased by three orders of magnitude relative to that in the first CHIME/FRB catalog, and, applying coherent dedispersion, burst morphologies can be studied in detail. Polarization information is also available for the full sample of 140 FRBs, providing an unprecedented dataset to study the polarization properties of the population. We release the baseband data beamformed to the most probable position of each FRB. These data are analyzed in detail in a series of accompanying papers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.00111v2-abstract-full').style.display = 'none'; document.getElementById('2311.00111v2-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.09608">arXiv:2308.09608</a> <span> [<a href="https://arxiv.org/pdf/2308.09608">pdf</a>, <a href="https://arxiv.org/format/2308.09608">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Statistical association between the candidate repeating FRB 20200320A and a galaxy group </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rafiei-Ravandi%2C+M">Masoud Rafiei-Ravandi</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+K+M">Kendrick M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Michilli%2C+D">D. Michilli</a>, <a href="/search/astro-ph?searchtype=author&query=Pleunis%2C+Z">Ziggy Pleunis</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">Mohit Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Dobbs%2C+M">Matt Dobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Eadie%2C+G+M">Gwendolyn M. Eadie</a>, <a href="/search/astro-ph?searchtype=author&query=Fonseca%2C+E">Emmanuel Fonseca</a>, <a href="/search/astro-ph?searchtype=author&query=Gaensler%2C+B+M">B. M. Gaensler</a>, <a href="/search/astro-ph?searchtype=author&query=Kaczmarek%2C+J">Jane Kaczmarek</a>, <a href="/search/astro-ph?searchtype=author&query=Kaspi%2C+V+M">Victoria M. Kaspi</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">Calvin Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+D">Dongzi Li</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K+W">Kiyoshi W. Masui</a>, <a href="/search/astro-ph?searchtype=author&query=Pandhi%2C+A">Ayush Pandhi</a>, <a href="/search/astro-ph?searchtype=author&query=Pearlman%2C+A+B">Aaron B. Pearlman</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">Emily Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Rahman%2C+M">Mubdi Rahman</a>, <a href="/search/astro-ph?searchtype=author&query=Scholz%2C+P">Paul Scholz</a>, <a href="/search/astro-ph?searchtype=author&query=Stenning%2C+D+C">David C. Stenning</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.09608v2-abstract-short" style="display: inline;"> We present results from angular cross-correlations between select samples of CHIME/FRB repeaters and galaxies in three photometric galaxy surveys, which have shown correlations with the first CHIME/FRB catalog containing repeating and nonrepeating sources: WISE$\times$SCOS, DESI-BGS, and DESI-LRG. We find a statistically significant correlation ($p$-value $<0.001$, after accounting for look-elsewh… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.09608v2-abstract-full').style.display = 'inline'; document.getElementById('2308.09608v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.09608v2-abstract-full" style="display: none;"> We present results from angular cross-correlations between select samples of CHIME/FRB repeaters and galaxies in three photometric galaxy surveys, which have shown correlations with the first CHIME/FRB catalog containing repeating and nonrepeating sources: WISE$\times$SCOS, DESI-BGS, and DESI-LRG. We find a statistically significant correlation ($p$-value $<0.001$, after accounting for look-elsewhere factors) between a sample of repeaters with extragalactic dispersion measure DM $>395$ pc cm$^{-3}$ and WISE$\times$SCOS galaxies with redshift $z>0.275$. We demonstrate that the correlation arises surprisingly because of a statistical association between FRB 20200320A (extragalactic DM $\approx550$ pc cm$^{-3}$) and a galaxy group in the same dark matter halo at redshift $z\approx0.32$. We estimate that the host halo, along with an intervening halo at redshift $z\approx0.12$, accounts for at least $\sim$$30\%$ of the extragalactic DM. Our results strongly motivate incorporating galaxy group and cluster catalogs into direct host association pipelines for FRBs with $\lesssim$$1'$ localization precision, effectively utilizing the two-point information to constrain FRB properties such as their redshift and DM distributions. In addition, we find marginal evidence for a negative correlation at 99.4% CL between a sample of repeating FRBs with baseband data (median extragalactic DM $=354$ pc cm$^{-3}$) and DESI-LRG galaxies with redshift $0.3\le z<0.45$, suggesting that the repeaters might be more prone than apparent nonrepeaters to propagation effects in FRB-galaxy correlations due to intervening free electrons over angular scales $\sim$$0\mbox{$.\!\!^\circ$}5$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.09608v2-abstract-full').style.display = 'none'; document.getElementById('2308.09608v2-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 4 figures, 3 tables, published in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.09502">arXiv:2307.09502</a> <span> [<a href="https://arxiv.org/pdf/2307.09502">pdf</a>, <a href="https://arxiv.org/format/2307.09502">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/10.1038/s41550-024-02357-x">10.1038/s41550-024-02357-x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A fast radio burst localized at detection to an edge-on galaxy using very-long-baseline interferometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">Tomas Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">Calvin Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Sanghavi%2C+P">Pranav Sanghavi</a>, <a href="/search/astro-ph?searchtype=author&query=Mena-Parra%2C+J">Juan Mena-Parra</a>, <a href="/search/astro-ph?searchtype=author&query=Cary%2C+S">Savannah Cary</a>, <a href="/search/astro-ph?searchtype=author&query=Mckinven%2C+R">Ryan Mckinven</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">Mohit Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K+W">Kiyoshi W. Masui</a>, <a href="/search/astro-ph?searchtype=author&query=Michilli%2C+D">Daniele Michilli</a>, <a href="/search/astro-ph?searchtype=author&query=Bandura%2C+K">Kevin Bandura</a>, <a href="/search/astro-ph?searchtype=author&query=Chatterjee%2C+S">Shami Chatterjee</a>, <a href="/search/astro-ph?searchtype=author&query=Peterson%2C+J+B">Jeffrey B. Peterson</a>, <a href="/search/astro-ph?searchtype=author&query=Kaczmarek%2C+J">Jane Kaczmarek</a>, <a href="/search/astro-ph?searchtype=author&query=Patel%2C+C">Chitrang Patel</a>, <a href="/search/astro-ph?searchtype=author&query=Rahman%2C+M">Mubdi Rahman</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+K">Kaitlyn Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Vanderlinde%2C+K">Keith Vanderlinde</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+S">Sabrina Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Brar%2C+C">Charanjot Brar</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+P+J">P. J. Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Breitman%2C+D">Daniela Breitman</a>, <a href="/search/astro-ph?searchtype=author&query=Chawla%2C+P">Pragya Chawla</a>, <a href="/search/astro-ph?searchtype=author&query=Curtin%2C+A+P">Alice P. Curtin</a>, <a href="/search/astro-ph?searchtype=author&query=Dobbs%2C+M">Matt Dobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+F+A">Fengqiu Adam Dong</a> , et al. (26 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.09502v4-abstract-short" style="display: inline;"> Fast radio bursts (FRBs) are millisecond-duration, luminous radio transients of extragalactic origin. These events have been used to trace the baryonic structure of the Universe using their dispersion measure (DM) assuming that the contribution from host galaxies can be reliably estimated. However, contributions from the immediate environment of an FRB may dominate the observed DM, thus making red… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.09502v4-abstract-full').style.display = 'inline'; document.getElementById('2307.09502v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.09502v4-abstract-full" style="display: none;"> Fast radio bursts (FRBs) are millisecond-duration, luminous radio transients of extragalactic origin. These events have been used to trace the baryonic structure of the Universe using their dispersion measure (DM) assuming that the contribution from host galaxies can be reliably estimated. However, contributions from the immediate environment of an FRB may dominate the observed DM, thus making redshift estimates challenging without a robust host galaxy association. Furthermore, while at least one Galactic burst has been associated with a magnetar, other localized FRBs argue against magnetars as the sole progenitor model. Precise localization within the host galaxy can discriminate between progenitor models, a major goal of the field. Until now, localizations on this spatial scale have only been carried out in follow-up observations of repeating sources. Here we demonstrate the localization of FRB 20210603A with very long baseline interferometry (VLBI) on two baselines, using data collected only at the time of detection. We localize the burst to SDSS J004105.82+211331.9, an edge-on galaxy at $z\approx 0.177$, and detect recent star formation in the kiloparsec-scale vicinity of the burst. The edge-on inclination of the host galaxy allows for a unique comparison between the line of sight towards the FRB and lines of sight towards known Galactic pulsars. The DM, Faraday rotation measure (RM), and scattering suggest a progenitor coincident with the host galactic plane, strengthening the link between the environment of FRB 20210603A and the disk of its host galaxy. Single-pulse VLBI localizations of FRBs to within their host galaxies, following the one presented here, will further constrain the origins and host environments of one-off FRBs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.09502v4-abstract-full').style.display = 'none'; document.getElementById('2307.09502v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 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">40 pages, 13 figures, accepted for publication in Nature Astronomy, changed title</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.05839">arXiv:2307.05839</a> <span> [<a href="https://arxiv.org/pdf/2307.05839">pdf</a>, <a href="https://arxiv.org/format/2307.05839">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> A CHIME/FRB study of burst rate and morphological evolution of the periodically repeating FRB 20180916B </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sand%2C+K+R">Ketan R. Sand</a>, <a href="/search/astro-ph?searchtype=author&query=Breitman%2C+D">Daniela Breitman</a>, <a href="/search/astro-ph?searchtype=author&query=Michilli%2C+D">Daniele Michilli</a>, <a href="/search/astro-ph?searchtype=author&query=Kaspi%2C+V+M">Victoria M. Kaspi</a>, <a href="/search/astro-ph?searchtype=author&query=Chawla%2C+P">Pragya Chawla</a>, <a href="/search/astro-ph?searchtype=author&query=Fonseca%2C+E">Emmanuel Fonseca</a>, <a href="/search/astro-ph?searchtype=author&query=Mckinven%2C+R">Ryan Mckinven</a>, <a href="/search/astro-ph?searchtype=author&query=Nimmo%2C+K">Kenzie Nimmo</a>, <a href="/search/astro-ph?searchtype=author&query=Pleunis%2C+Z">Ziggy Pleunis</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+K">Kaitlyn Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+B+C">Bridget C. Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">Mohit Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+P+J">P. J. Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Brar%2C+C">Charanjot Brar</a>, <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">Tomas Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+A+M">Amanda M. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Curtin%2C+A+P">Alice P. Curtin</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+F+A">Fengqiu Adam Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Eadie%2C+G+M">Gwendolyn M. Eadie</a>, <a href="/search/astro-ph?searchtype=author&query=Gaensler%2C+B+M">B. M. Gaensler</a>, <a href="/search/astro-ph?searchtype=author&query=Kaczmarek%2C+J">Jane Kaczmarek</a>, <a href="/search/astro-ph?searchtype=author&query=Lanman%2C+A">Adam Lanman</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">Calvin Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K+W">Kiyoshi W. Masui</a>, <a href="/search/astro-ph?searchtype=author&query=Rahman%2C+M">Mubdi Rahman</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="2307.05839v1-abstract-short" style="display: inline;"> FRB 20180916B is a repeating Fast Radio Burst (FRB) with a 16.3-day periodicity in its activity. In this study, we present morphological properties of 60 FRB 20180916B bursts detected by CHIME/FRB between 2018 August and 2021 December. We recorded raw voltage data for 45 of these bursts, enabling microseconds time resolution in some cases. We studied variation of spectro-temporal properties with t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.05839v1-abstract-full').style.display = 'inline'; document.getElementById('2307.05839v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.05839v1-abstract-full" style="display: none;"> FRB 20180916B is a repeating Fast Radio Burst (FRB) with a 16.3-day periodicity in its activity. In this study, we present morphological properties of 60 FRB 20180916B bursts detected by CHIME/FRB between 2018 August and 2021 December. We recorded raw voltage data for 45 of these bursts, enabling microseconds time resolution in some cases. We studied variation of spectro-temporal properties with time and activity phase. We find that the variation in Dispersion Measure (DM) is $\lesssim$1 pc cm$^{-3}$ and that there is burst-to-burst variation in scattering time estimates ranging from $\sim$0.16 to over 2 ms, with no discernible trend with activity phase for either property. Furthermore, we find no DM and scattering variability corresponding to the recent change in rotation measure from the source, which has implications for the immediate environment of the source. We find that FRB 20180916B has thus far shown no epochs of heightened activity as have been seen in other active repeaters by CHIME/FRB, with its burst count consistent with originating from a Poissonian process. We also observe no change in the value of the activity period over the duration of our observations and set a 1$蟽$ upper limit of $1.5\times10^{-4}$ day day$^{-1}$ on the absolute period derivative. Finally, we discuss constraints on progenitor models yielded by our results, noting that our upper limits on changes in scattering and dispersion measure as a function of phase do not support models invoking a massive binary companion star as the origin of the 16.3-day periodicity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.05839v1-abstract-full').style.display = 'none'; document.getElementById('2307.05839v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 July, 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">25 pages, 10 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.08386">arXiv:2302.08386</a> <span> [<a href="https://arxiv.org/pdf/2302.08386">pdf</a>, <a href="https://arxiv.org/format/2302.08386">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/acd188">10.3847/1538-4357/acd188 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Revealing the Dynamic Magneto-ionic Environments of Repeating Fast Radio Burst Sources through Multi-year Polarimetric Monitoring with CHIME/FRB </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mckinven%2C+R">R. Mckinven</a>, <a href="/search/astro-ph?searchtype=author&query=Gaensler%2C+B+M">B. M. Gaensler</a>, <a href="/search/astro-ph?searchtype=author&query=Michilli%2C+D">D. Michilli</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K">K. Masui</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=Su%2C+J">J. Su</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">M. Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">T. Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Chawla%2C+P">P. Chawla</a>, <a href="/search/astro-ph?searchtype=author&query=F."> F.</a>, <a href="/search/astro-ph?searchtype=author&query=Dong"> Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Fonseca%2C+E">E. Fonseca</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">C. Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">E. Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Pleunis%2C+Z">Z. Pleunis</a>, <a href="/search/astro-ph?searchtype=author&query=Rafiei-Ravandi%2C+M">M. Rafiei-Ravandi</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=Tendulkar%2C+S">S. Tendulkar</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+D+Z">D. Z. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Ng%2C+C">C. Ng</a>, <a href="/search/astro-ph?searchtype=author&query=Patel%2C+C">C. Patel</a>, <a href="/search/astro-ph?searchtype=author&query=Pearlman%2C+A+B">A. B. Pearlman</a>, <a href="/search/astro-ph?searchtype=author&query=Rahman%2C+M">M. Rahman</a>, <a href="/search/astro-ph?searchtype=author&query=Sand%2C+K+R">K. R. Sand</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+K">K. Shin</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="2302.08386v1-abstract-short" style="display: inline;"> Fast radio bursts (FRBs) display a confounding variety of burst properties and host galaxy associations. Repeating FRBs offer insight into the FRB population by enabling spectral, temporal and polarimetric properties to be tracked over time. Here, we report on the polarized observations of 12 repeating sources using multi-year monitoring with the Canadian Hydrogen Intensity Mapping Experiment (CHI… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.08386v1-abstract-full').style.display = 'inline'; document.getElementById('2302.08386v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.08386v1-abstract-full" style="display: none;"> Fast radio bursts (FRBs) display a confounding variety of burst properties and host galaxy associations. Repeating FRBs offer insight into the FRB population by enabling spectral, temporal and polarimetric properties to be tracked over time. Here, we report on the polarized observations of 12 repeating sources using multi-year monitoring with the Canadian Hydrogen Intensity Mapping Experiment (CHIME) over 400-800 MHz. We observe significant RM variations from many sources in our sample, including RM changes of several hundred $\rm{rad\, m^{-2}}$ over month timescales from FRBs 20181119A, 20190303A and 20190417A, and more modest RM variability ($\rm{螖RM \lesssim}$ few tens rad m$^{-2}$) from FRBs 20181030A, 20190208A, 20190213B and 20190117A over equivalent timescales. Several repeaters display a frequency dependent degree of linear polarization that is consistent with depolarization via scattering. Combining our measurements of RM variations with equivalent constraints on DM variability, we estimate the average line-of-sight magnetic field strength in the local environment of each repeater. In general, repeating FRBs display RM variations that are more prevalent/extreme than those seen from radio pulsars in the Milky Way and the Magellanic Clouds, suggesting repeating FRBs and pulsars occupy distinct magneto-ionic environments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.08386v1-abstract-full').style.display = 'none'; document.getElementById('2302.08386v1-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.08762">arXiv:2301.08762</a> <span> [<a href="https://arxiv.org/pdf/2301.08762">pdf</a>, <a href="https://arxiv.org/format/2301.08762">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </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/acc6c1">10.3847/1538-4357/acc6c1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CHIME/FRB Discovery of 25 Repeating Fast Radio Burst Sources </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+T+C">The CHIME/FRB Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+B+C">Bridget C. Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Bandura%2C+K">Kevin Bandura</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">Mohit Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+P+J">P. J. Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Brar%2C+C">Charanjot Brar</a>, <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">Tomas Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Chatterjee%2C+S">S. Chatterjee</a>, <a href="/search/astro-ph?searchtype=author&query=Chawla%2C+P">Pragya Chawla</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+A+M">Amanda M. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Curtin%2C+A+P">Alice P. Curtin</a>, <a href="/search/astro-ph?searchtype=author&query=Dobbs%2C+M">Matt Dobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+F+A">Fengqiu Adam Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Faber%2C+J+T">Jakob T. Faber</a>, <a href="/search/astro-ph?searchtype=author&query=Fandino%2C+M">Mateus Fandino</a>, <a href="/search/astro-ph?searchtype=author&query=Fonseca%2C+E">Emmanuel Fonseca</a>, <a href="/search/astro-ph?searchtype=author&query=Gaensler%2C+B+M">B. M. Gaensler</a>, <a href="/search/astro-ph?searchtype=author&query=Giri%2C+U">Utkarsh Giri</a>, <a href="/search/astro-ph?searchtype=author&query=Herrera-Martin%2C+A">Antonio Herrera-Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+A+S">Alex S. Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Ibik%2C+A">Adaeze Ibik</a>, <a href="/search/astro-ph?searchtype=author&query=Josephy%2C+A">Alexander Josephy</a>, <a href="/search/astro-ph?searchtype=author&query=Kaczmarek%2C+J+F">Jane F. Kaczmarek</a>, <a href="/search/astro-ph?searchtype=author&query=Kader%2C+Z">Zarif Kader</a> , et al. (35 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="2301.08762v2-abstract-short" style="display: inline;"> We present the discovery of 25 new repeating fast radio burst (FRB) sources found among CHIME/FRB events detected between 2019 September 30 and 2021 May 1. The sources were found using a new clustering algorithm that looks for multiple events co-located on the sky having similar dispersion measures (DMs). The new repeaters have DMs ranging from $\sim$220 pc cm$^{-3}$ to $\sim$1700 pc cm$^{-3}$, an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.08762v2-abstract-full').style.display = 'inline'; document.getElementById('2301.08762v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.08762v2-abstract-full" style="display: none;"> We present the discovery of 25 new repeating fast radio burst (FRB) sources found among CHIME/FRB events detected between 2019 September 30 and 2021 May 1. The sources were found using a new clustering algorithm that looks for multiple events co-located on the sky having similar dispersion measures (DMs). The new repeaters have DMs ranging from $\sim$220 pc cm$^{-3}$ to $\sim$1700 pc cm$^{-3}$, and include sources having exhibited as few as two bursts to as many as twelve. We report a statistically significant difference in both the DM and extragalactic DM (eDM) distributions between repeating and apparently nonrepeating sources, with repeaters having lower mean DM and eDM, and we discuss the implications. We find no clear bimodality between the repetition rates of repeaters and upper limits on repetition from apparently nonrepeating sources after correcting for sensitivity and exposure effects, although some active repeating sources stand out as anomalous. We measure the repeater fraction over time and find that it tends to an equilibrium of $2.6_{-2.6}^{+2.9}$% over our total time-on-sky thus far. We also report on 14 more sources which are promising repeating FRB candidates and which merit follow-up observations for confirmation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.08762v2-abstract-full').style.display = 'none'; document.getElementById('2301.08762v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 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">ApJ in press. Comments are still welcome and follow-up observations are encouraged!</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.11941">arXiv:2212.11941</a> <span> [<a href="https://arxiv.org/pdf/2212.11941">pdf</a>, <a href="https://arxiv.org/format/2212.11941">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/accf89">10.3847/1538-4357/accf89 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sub-arcminute localization of 13 repeating fast radio bursts detected by CHIME/FRB </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Michilli%2C+D">Daniele Michilli</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">Mohit Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Brar%2C+C">Charanjot Brar</a>, <a href="/search/astro-ph?searchtype=author&query=Patel%2C+C">Chitrang Patel</a>, <a href="/search/astro-ph?searchtype=author&query=Gaensler%2C+B+M">B. M. Gaensler</a>, <a href="/search/astro-ph?searchtype=author&query=Kaspi%2C+V+M">Victoria M. Kaspi</a>, <a href="/search/astro-ph?searchtype=author&query=Kirichenko%2C+A">Aida Kirichenko</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K+W">Kiyoshi W. Masui</a>, <a href="/search/astro-ph?searchtype=author&query=Sand%2C+K+R">Ketan R. Sand</a>, <a href="/search/astro-ph?searchtype=author&query=Scholz%2C+P">Paul Scholz</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+K">Kaitlyn Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Stairs%2C+I">Ingrid Stairs</a>, <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">Tomas Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+A+M">Amanda M. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Dobbs%2C+M">Matt Dobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+F+A">Fengqiu Adam Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Fonseca%2C+E">Emmanuel Fonseca</a>, <a href="/search/astro-ph?searchtype=author&query=Ibik%2C+A">Adaeze Ibik</a>, <a href="/search/astro-ph?searchtype=author&query=Kaczmarek%2C+J">Jane Kaczmarek</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">Calvin Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Pearlman%2C+A+B">Aaron B. Pearlman</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">Emily Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Pleunis%2C+Z">Ziggy Pleunis</a>, <a href="/search/astro-ph?searchtype=author&query=Rafiei-Ravandi%2C+M">Masoud Rafiei-Ravandi</a>, <a href="/search/astro-ph?searchtype=author&query=Sanghavi%2C+P">Pranav Sanghavi</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.11941v1-abstract-short" style="display: inline;"> We report on improved sky localizations of thirteen repeating fast radio bursts (FRBs) discovered by CHIME/FRB via the use of interferometric techniques on channelized voltages from the telescope. These so-called 'baseband localizations' improve the localization uncertainty area presented in past studies by more than three orders of magnitude. The improved localization regions are provided for the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.11941v1-abstract-full').style.display = 'inline'; document.getElementById('2212.11941v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.11941v1-abstract-full" style="display: none;"> We report on improved sky localizations of thirteen repeating fast radio bursts (FRBs) discovered by CHIME/FRB via the use of interferometric techniques on channelized voltages from the telescope. These so-called 'baseband localizations' improve the localization uncertainty area presented in past studies by more than three orders of magnitude. The improved localization regions are provided for the full sample of FRBs to enable follow-up studies. The localization uncertainties, together with limits on the source distances from their dispersion measures (DMs), allow us to identify likely host galaxies for two of the FRB sources. FRB 20180814A lives in a massive passive red spiral at z~0.068 with very little indication of star formation, while FRB 20190303A resides in a merging pair of spiral galaxies at z~0.064 undergoing significant star formation. These galaxies show very different characteristics, further confirming the presence of FRB progenitors in a variety of environments even among the repeating sub-class. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.11941v1-abstract-full').style.display = 'none'; document.getElementById('2212.11941v1-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 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.00803">arXiv:2208.00803</a> <span> [<a href="https://arxiv.org/pdf/2208.00803">pdf</a>, <a href="https://arxiv.org/format/2208.00803">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/ace52f">10.3847/1538-4357/ace52f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Limits on Fast Radio Burst-like Counterparts to Gamma-ray Bursts using CHIME/FRB </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Curtin%2C+A+P">Alice P. Curtin</a>, <a href="/search/astro-ph?searchtype=author&query=Tendulkar%2C+S+P">Shriharsh P. Tendulkar</a>, <a href="/search/astro-ph?searchtype=author&query=Josephy%2C+A">Alexander Josephy</a>, <a href="/search/astro-ph?searchtype=author&query=Chawla%2C+P">Pragya Chawla</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+B">Bridget Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Kaspi%2C+V+M">Victoria M. Kaspi</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">Mohit Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">Tomas Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+A">Amanda Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+F+A">Fengqiu Adam Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Fonseca%2C+E">Emmanuel Fonseca</a>, <a href="/search/astro-ph?searchtype=author&query=Gaensler%2C+B+M">B. M. Gaensler</a>, <a href="/search/astro-ph?searchtype=author&query=Kaczmarek%2C+J+F">Jane F. Kaczmarek</a>, <a href="/search/astro-ph?searchtype=author&query=Lanmnan%2C+A+E">Adam E. Lanmnan</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">Calvin Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Pearlman%2C+A+B">Aaron B. Pearlman</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">Emily Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Pleunis%2C+Z">Ziggy Pleunis</a>, <a href="/search/astro-ph?searchtype=author&query=Rafiei-Ravandi%2C+M">Masoud Rafiei-Ravandi</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=Shin%2C+K">Kaitlyn Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Scholz%2C+P">Paul Scholz</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+K">Kendrick Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Stairs%2C+I">Ingrid 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="2208.00803v2-abstract-short" style="display: inline;"> Fast Radio Bursts (FRBs) are a class of highly energetic, mostly extragalactic radio transients lasting for a few milliseconds. While over 600 FRBs have been published so far, their origins are presently unclear, with some theories for extragalactic FRBs predicting accompanying high-energy emission. In this work, we use the Canadian Hydrogen Intensity Mapping Experiment (CHIME) Fast Radio Burst (C… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.00803v2-abstract-full').style.display = 'inline'; document.getElementById('2208.00803v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.00803v2-abstract-full" style="display: none;"> Fast Radio Bursts (FRBs) are a class of highly energetic, mostly extragalactic radio transients lasting for a few milliseconds. While over 600 FRBs have been published so far, their origins are presently unclear, with some theories for extragalactic FRBs predicting accompanying high-energy emission. In this work, we use the Canadian Hydrogen Intensity Mapping Experiment (CHIME) Fast Radio Burst (CHIME/FRB) Project to explore whether any FRB-like radio emission coincides in space and time with 81 gamma-ray bursts (GRBs) detected between 2018 July 17 and 2019 July 8 by Swift/BAT and Fermi/GBM. We do not find any statistically significant, coincident pairs within 3sigma of each other's spatial localization regions and within a time difference of up to one week. In addition to searching for spatial matches between known FRBs and known GRBs, we use CHIME/FRB to constrain FRB-like radio emission before, at the time of, or after the reported high-energy emission at the position of 39 GRBs. Our most constraining radio flux limits in the 400- to 800-MHz band for short gamma-ray bursts (SGRBs) are <50 Jy at 18.6 ks pre-high-energy emission, and <5 Jy at 28.4 ks post-high-energy emission, assuming a 10-ms radio burst width with each limit valid for 60 seconds. We use these limits to constrain models that predict FRB-like prompt radio emission before and after SGRBs. We also place limits as low as 2 Jy for long gamma-ray bursts (LGRBs), but there are no strong theoretical predictions for coincident FRB-like radio emission for LGRBs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.00803v2-abstract-full').style.display = 'none'; document.getElementById('2208.00803v2-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 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 5 tables, 10 figures; Submitted to ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 954 154 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.12362">arXiv:2205.12362</a> <span> [<a href="https://arxiv.org/pdf/2205.12362">pdf</a>, <a href="https://arxiv.org/format/2205.12362">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202244107">10.1051/0004-6361/202244107 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Apertif Radio Transient System (ARTS): Design, Commissioning, Data Release, and Detection of the first 5 Fast Radio Bursts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+J">Joeri van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=Kooistra%2C+E">Eric Kooistra</a>, <a href="/search/astro-ph?searchtype=author&query=Oostrum%2C+L">Leon Oostrum</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">Liam Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Hargreaves%2C+J+E">J. E. Hargreaves</a>, <a href="/search/astro-ph?searchtype=author&query=Maan%2C+Y">Yogesh Maan</a>, <a href="/search/astro-ph?searchtype=author&query=Pastor-Marazuela%2C+I">In茅s Pastor-Marazuela</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">Emily Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Schuur%2C+D">Daniel van der Schuur</a>, <a href="/search/astro-ph?searchtype=author&query=Sclocco%2C+A">Alessio Sclocco</a>, <a href="/search/astro-ph?searchtype=author&query=Straal%2C+S+M">Samayra M. Straal</a>, <a href="/search/astro-ph?searchtype=author&query=Vohl%2C+D">Dany Vohl</a>, <a href="/search/astro-ph?searchtype=author&query=Wijnholds%2C+S+J">Stefan J. Wijnholds</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">Elizabeth A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">Bj枚rn Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=Attema%2C+J">Jisk Attema</a>, <a href="/search/astro-ph?searchtype=author&query=Bassa%2C+C">Cees Bassa</a>, <a href="/search/astro-ph?searchtype=author&query=Bast%2C+J+E">Jeanette E. Bast</a>, <a href="/search/astro-ph?searchtype=author&query=Bilous%2C+A">Anna Bilous</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Boersma%2C+O+M">Oliver M. Boersma</a>, <a href="/search/astro-ph?searchtype=author&query=van+Cappellen%2C+W+A">Wim A. van Cappellen</a>, <a href="/search/astro-ph?searchtype=author&query=Coolen%2C+A+H+W+M">Arthur H. W. M. Coolen</a>, <a href="/search/astro-ph?searchtype=author&query=Damstra%2C+S">Sieds Damstra</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9nes%2C+H">Helga D茅nes</a> , et al. (27 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2205.12362v2-abstract-short" style="display: inline;"> Fast Radio Bursts must be powered by uniquely energetic emission mechanisms. This requirement has eliminated a number of possible source types, but several remain. Identifying the physical nature of Fast Radio Burst (FRB) emitters arguably requires good localisation of more detections, and broadband studies enabled by real-time alerting. We here present the Apertif Radio Transient System (ARTS), a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.12362v2-abstract-full').style.display = 'inline'; document.getElementById('2205.12362v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.12362v2-abstract-full" style="display: none;"> Fast Radio Bursts must be powered by uniquely energetic emission mechanisms. This requirement has eliminated a number of possible source types, but several remain. Identifying the physical nature of Fast Radio Burst (FRB) emitters arguably requires good localisation of more detections, and broadband studies enabled by real-time alerting. We here present the Apertif Radio Transient System (ARTS), a supercomputing radio-telescope instrument that performs real-time FRB detection and localisation on the Westerbork Synthesis Radio Telescope (WSRT) interferometer. It reaches coherent-addition sensitivity over the entire field of the view of the primary dish beam. After commissioning results verified the system performed as planned, we initiated the Apertif FRB survey (ALERT). Over the first 5 weeks we observed at design sensitivity in 2019, we detected 5 new FRBs, and interferometrically localised each of these to 0.4--10 sq. arcmin. All detections are broad band and very narrow, of order 1 ms duration, and unscattered. Dispersion measures are generally high. Only through the very high time and frequency resolution of ARTS are these hard-to-find FRBs detected, producing an unbiased view of the intrinsic population properties. Most localisation regions are small enough to rule out the presence of associated persistent radio sources. Three FRBs cut through the halos of M31 and M33. We demonstrate that Apertif can localise one-off FRBs with an accuracy that maps magneto-ionic material along well-defined lines of sight. The rate of 1 every ~7 days next ensures a considerable number of new sources are detected for such study. The combination of detection rate and localisation accuracy exemplified by the 5 first ARTS FRBs thus marks a new phase in which a growing number of bursts can be used to probe our Universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.12362v2-abstract-full').style.display = 'none'; document.getElementById('2205.12362v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 672, A117 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.09221">arXiv:2205.09221</a> <span> [<a href="https://arxiv.org/pdf/2205.09221">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/acc65f">10.3847/1538-4357/acc65f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Large Scale Magneto-ionic Fluctuation in the Local Environment of Periodic Fast Radio Burst Source, FRB 20180916B </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mckinven%2C+R">R. Mckinven</a>, <a href="/search/astro-ph?searchtype=author&query=Gaensler%2C+B+M">B. M. Gaensler</a>, <a href="/search/astro-ph?searchtype=author&query=Michilli%2C+D">D. Michilli</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K">K. Masui</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=Bhardwaj%2C+M">M. Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">T. Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Chawla%2C+P">P. Chawla</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+F+A">F. Adam Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Fonseca%2C+E">E. Fonseca</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">C. Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+D+Z">D. Z. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Ng%2C+C">C. Ng</a>, <a href="/search/astro-ph?searchtype=author&query=Patel%2C+C">C. Patel</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">E. Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Pearlman%2C+A+B">A. B. Pearlman</a>, <a href="/search/astro-ph?searchtype=author&query=Pleunis%2C+Z">Z. Pleunis</a>, <a href="/search/astro-ph?searchtype=author&query=Rafiei-Ravandi%2C+M">M. Rafiei-Ravandi</a>, <a href="/search/astro-ph?searchtype=author&query=Rahman%2C+M">M. Rahman</a>, <a href="/search/astro-ph?searchtype=author&query=Sand%2C+K+R">K. R. Sand</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+K">K. Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Scholz%2C+P">P. Scholz</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=Smith%2C+K">K. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Su%2C+J">J. Su</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2205.09221v1-abstract-short" style="display: inline;"> Fast radio burst (FRB) source 20180916B exhibits a 16.33-day periodicity in its burst activity. It is as of yet unclear what proposed mechanism produces the activity, but polarization information is a key diagnostic. Here, we report on the polarization properties of 44 bursts from FRB 20180916B detected between 2018 December and 2021 December by CHIME/FRB, the FRB project on the Canadian Hydrogen… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.09221v1-abstract-full').style.display = 'inline'; document.getElementById('2205.09221v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.09221v1-abstract-full" style="display: none;"> Fast radio burst (FRB) source 20180916B exhibits a 16.33-day periodicity in its burst activity. It is as of yet unclear what proposed mechanism produces the activity, but polarization information is a key diagnostic. Here, we report on the polarization properties of 44 bursts from FRB 20180916B detected between 2018 December and 2021 December by CHIME/FRB, the FRB project on the Canadian Hydrogen Intensity Mapping Experiment the Canadian Hydrogen Intensity Mapping Experiment. In contrast to previous observations, we find significant variations in the Faraday rotation measure (RM) of FRB 20180916B. Over the nine month period 2021 April$-$2021 December we observe an apparent secular increase in $\rm{RM}$ of $\sim 50 \; \rm{rad\, m^{-2}}$ (a fractional change of over $40\%$) that is accompanied by a possible drift of the emitting band to lower frequencies. This interval displays very little variation in the dispersion measure ($螖\rm{DM}\lesssim 0.8\; \rm{pc\, cm^{-3}}$) which indicates that the observed RM evolution is likely produced from coherent changes in the Faraday-active medium's magnetic field. Burst-to-burst RM variations appear unrelated to the activity cycle phase. The degree of linear polarization of our burst sample ($\gtrsim 80\%$) is consistent with the negligible depolarization expected for this source in the 400-800 MHz bandpass of CHIME. FRB 20180916B joins other repeating FRBs in displaying substantial RM variations between bursts. This is consistent with the notion that repeater progenitors may be associated with young stellar populations by their preferential occupation of dynamic magnetized environments commonly found in supernova remnants, pulsar wind nebulae or near high mass stellar companions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.09221v1-abstract-full').style.display = 'none'; document.getElementById('2205.09221v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.06014">arXiv:2204.06014</a> <span> [<a href="https://arxiv.org/pdf/2204.06014">pdf</a>, <a href="https://arxiv.org/format/2204.06014">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.106.043016">10.1103/PhysRevD.106.043016 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A High-Time Resolution Search for Compact Objects using Fast Radio Burst Gravitational Lens Interferometry with CHIME/FRB </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kader%2C+Z">Zarif Kader</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">Calvin Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Dobbs%2C+M">Matt Dobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K+W">Kiyoshi W. Masui</a>, <a href="/search/astro-ph?searchtype=author&query=Michilli%2C+D">Daniele Michilli</a>, <a href="/search/astro-ph?searchtype=author&query=Mena-Parra%2C+J">Juan Mena-Parra</a>, <a href="/search/astro-ph?searchtype=author&query=Mckinven%2C+R">Ryan Mckinven</a>, <a href="/search/astro-ph?searchtype=author&query=Ng%2C+C">Cherry Ng</a>, <a href="/search/astro-ph?searchtype=author&query=Bandura%2C+K">Kevin Bandura</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">Mohit Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Brar%2C+C">Charanjot Brar</a>, <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">Tomas Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Chawla%2C+P">Pragya Chawla</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+F+A">Fengqiu Adam Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Good%2C+D">Deborah Good</a>, <a href="/search/astro-ph?searchtype=author&query=Kaspi%2C+V">Victoria Kaspi</a>, <a href="/search/astro-ph?searchtype=author&query=Lanman%2C+A+E">Adam E. Lanman</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+H">Hsiu-Hsien Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Meyers%2C+B+W">Bradley W. Meyers</a>, <a href="/search/astro-ph?searchtype=author&query=Pearlman%2C+A+B">Aaron B. Pearlman</a>, <a href="/search/astro-ph?searchtype=author&query=Pen%2C+U">Ue-Li Pen</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">Emily Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Pleunis%2C+Z">Ziggy Pleunis</a>, <a href="/search/astro-ph?searchtype=author&query=Rafiei-Ravandi%2C+M">Masoud Rafiei-Ravandi</a>, <a href="/search/astro-ph?searchtype=author&query=Rahman%2C+M">Mubdi Rahman</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="2204.06014v1-abstract-short" style="display: inline;"> The gravitational field of compact objects, such as primordial black holes, can create multiple images of background sources. For transients such as fast radio bursts (FRBs), these multiple images can be resolved in the time domain. Under certain circumstances, these images not only have similar burst morphologies but are also phase-coherent at the electric field level. With a novel dechannelizati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.06014v1-abstract-full').style.display = 'inline'; document.getElementById('2204.06014v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.06014v1-abstract-full" style="display: none;"> The gravitational field of compact objects, such as primordial black holes, can create multiple images of background sources. For transients such as fast radio bursts (FRBs), these multiple images can be resolved in the time domain. Under certain circumstances, these images not only have similar burst morphologies but are also phase-coherent at the electric field level. With a novel dechannelization algorithm and a matched filtering technique, we search for repeated copies of the same electric field waveform in observations of FRBs detected by the FRB backend of the Canadian Hydrogen Mapping Intensity Experiment (CHIME). An interference fringe from a coherent gravitational lensing signal will appear in the time-lag domain as a statistically-significant peak in the time-lag autocorrelation function. We calibrate our statistical significance using telescope data containing no FRB signal. Our dataset consists of $\sim$100-ms long recordings of voltage data from 172 FRB events, dechannelized to 1.25-ns time resolution. This coherent search algorithm allows us to search for gravitational lensing signatures from compact objects in the mass range of $10^{-4}-10^{4} ~\mathrm{M_{\odot}}$. After ruling out an anomalous candidate due to diffractive scintillation, we find no significant detections of gravitational lensing in the 172 FRB events that have been analyzed. In a companion work [Leung, Kader+2022], we interpret the constraints on dark matter from this search. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.06014v1-abstract-full').style.display = 'none'; document.getElementById('2204.06014v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 April, 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">23 pages, 13 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.06001">arXiv:2204.06001</a> <span> [<a href="https://arxiv.org/pdf/2204.06001">pdf</a>, <a href="https://arxiv.org/format/2204.06001">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.106.043017">10.1103/PhysRevD.106.043017 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraining Primordial Black Holes using Fast Radio Burst Gravitational-Lens Interferometry with CHIME/FRB </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">Calvin Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Kader%2C+Z">Zarif Kader</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K+W">Kiyoshi W. Masui</a>, <a href="/search/astro-ph?searchtype=author&query=Dobbs%2C+M">Matt Dobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Michilli%2C+D">Daniele Michilli</a>, <a href="/search/astro-ph?searchtype=author&query=Mena-Parra%2C+J">Juan Mena-Parra</a>, <a href="/search/astro-ph?searchtype=author&query=Mckinven%2C+R">Ryan Mckinven</a>, <a href="/search/astro-ph?searchtype=author&query=Ng%2C+C">Cherry Ng</a>, <a href="/search/astro-ph?searchtype=author&query=Bandura%2C+K">Kevin Bandura</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">Mohit Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Brar%2C+C">Charanjot Brar</a>, <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">Tomas Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Chawla%2C+P">Pragya Chawla</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+F+A">Fengqiu Adam Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Good%2C+D">Deborah Good</a>, <a href="/search/astro-ph?searchtype=author&query=Kaspi%2C+V">Victoria Kaspi</a>, <a href="/search/astro-ph?searchtype=author&query=Lanman%2C+A+E">Adam E. Lanman</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+H">Hsiu-Hsien Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Meyers%2C+B+W">Bradley W. Meyers</a>, <a href="/search/astro-ph?searchtype=author&query=Pearlman%2C+A+B">Aaron B. Pearlman</a>, <a href="/search/astro-ph?searchtype=author&query=Pen%2C+U">Ue-Li Pen</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">Emily Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Pleunis%2C+Z">Ziggy Pleunis</a>, <a href="/search/astro-ph?searchtype=author&query=Rafiei-Ravandi%2C+M">Masoud Rafiei-Ravandi</a>, <a href="/search/astro-ph?searchtype=author&query=Rahman%2C+M">Mubdi Rahman</a> , et al. (8 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.06001v1-abstract-short" style="display: inline;"> Fast radio bursts (FRBs) represent an exciting frontier in the study of gravitational lensing, due to their brightness, extragalactic nature, and the compact, coherent characteristics of their emission. In a companion work [Kader, Leung+2022], we use a novel interferometric method to search for gravitationally lensed FRBs in the time domain using bursts detected by CHIME/FRB. There, we dechanneliz… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.06001v1-abstract-full').style.display = 'inline'; document.getElementById('2204.06001v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.06001v1-abstract-full" style="display: none;"> Fast radio bursts (FRBs) represent an exciting frontier in the study of gravitational lensing, due to their brightness, extragalactic nature, and the compact, coherent characteristics of their emission. In a companion work [Kader, Leung+2022], we use a novel interferometric method to search for gravitationally lensed FRBs in the time domain using bursts detected by CHIME/FRB. There, we dechannelize and autocorrelate electric field data at a time resolution of 1.25 ns. This enables a search for FRBs whose emission is coherently deflected by gravitational lensing around a foreground compact object such as a primordial black hole (PBH). Here, we use our non-detection of lensed FRBs to place novel constraints on the PBH abundance outside the Local Group. We use a novel two-screen model to take into account decoherence from scattering screens in our constraints. Our constraints are subject to a single astrophysical model parameter -- the effective distance between an FRB source and the scattering screen, for which we adopt a fiducial distance of 1 parsec. We find that coherent FRB lensing is a sensitive probe of sub-solar mass compact objects. Having observed no lenses in $172$ bursts from $114$ independent sightlines through the cosmic web, we constrain the fraction of dark matter made of compact objects, such as PBHs, to be $f \lesssim 0.8$, if their masses are $\sim 10^{-3} M_{\odot}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.06001v1-abstract-full').style.display = 'none'; document.getElementById('2204.06001v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 April, 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">20 pages, 5 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.12038">arXiv:2203.12038</a> <span> [<a href="https://arxiv.org/pdf/2203.12038">pdf</a>, <a href="https://arxiv.org/format/2203.12038">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"> Search for Gravitational Waves Associated with Fast Radio Bursts Detected by CHIME/FRB During the LIGO--Virgo Observing Run O3a </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+LIGO+Scientific+Collaboration"> The LIGO Scientific Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+Virgo+Collaboration"> the Virgo Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=the+KAGRA+Collaboration"> the KAGRA Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+t+C">the CHIME/FRB Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+R">R. Abbott</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=Acernese%2C+F">F. Acernese</a>, <a href="/search/astro-ph?searchtype=author&query=Ackley%2C+K">K. Ackley</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+N">N. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Adya%2C+V+B">V. B. Adya</a>, <a href="/search/astro-ph?searchtype=author&query=Affeldt%2C+C">C. Affeldt</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwal%2C+D">D. Agarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Agathos%2C+M">M. Agathos</a>, <a href="/search/astro-ph?searchtype=author&query=Agatsuma%2C+K">K. Agatsuma</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+N">N. Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Aguiar%2C+O+D">O. D. Aguiar</a>, <a href="/search/astro-ph?searchtype=author&query=Aiello%2C+L">L. Aiello</a>, <a href="/search/astro-ph?searchtype=author&query=Ain%2C+A">A. Ain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Akutsu%2C+T">T. Akutsu</a>, <a href="/search/astro-ph?searchtype=author&query=Albanesi%2C+S">S. Albanesi</a>, <a href="/search/astro-ph?searchtype=author&query=Allocca%2C+A">A. Allocca</a> , et al. (1633 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="2203.12038v1-abstract-short" style="display: inline;"> We search for gravitational-wave transients associated with fast radio bursts (FRBs) detected by the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst Project (CHIME/FRB), during the first part of the third observing run of Advanced LIGO and Advanced Virgo (1 April 2019 15:00 UTC-1 Oct 2019 15:00 UTC). Triggers from 22 FRBs were analyzed with a search that targets compact binary coal… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.12038v1-abstract-full').style.display = 'inline'; document.getElementById('2203.12038v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.12038v1-abstract-full" style="display: none;"> We search for gravitational-wave transients associated with fast radio bursts (FRBs) detected by the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst Project (CHIME/FRB), during the first part of the third observing run of Advanced LIGO and Advanced Virgo (1 April 2019 15:00 UTC-1 Oct 2019 15:00 UTC). Triggers from 22 FRBs were analyzed with a search that targets compact binary coalescences with at least one neutron star component. A targeted search for generic gravitational-wave transients was conducted on 40 FRBs. We find no significant evidence for a gravitational-wave association in either search. Given the large uncertainties in the distances of the FRBs inferred from the dispersion measures in our sample, however, this does not conclusively exclude any progenitor models that include emission of a gravitational wave of the types searched for from any of these FRB events. We report $90\%$ confidence lower bounds on the distance to each FRB for a range of gravitational-wave progenitor models. By combining the inferred maximum distance information for each FRB with the sensitivity of the gravitational-wave searches, we set upper limits on the energy emitted through gravitational waves for a range of emission scenarios. We find values of order $10^{51}$-$10^{57}$ erg for a range of different emission models with central gravitational wave frequencies in the range 70-3560 Hz. Finally, we also found no significant coincident detection of gravitational waves with the repeater, FRB 20200120E, which is the closest known extragalactic FRB. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.12038v1-abstract-full').style.display = 'none'; document.getElementById('2203.12038v1-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 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">35 pages, 6 figures, 8 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> P2100124 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.08002">arXiv:2202.08002</a> <span> [<a href="https://arxiv.org/pdf/2202.08002">pdf</a>, <a href="https://arxiv.org/format/2202.08002">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/10.1051/0004-6361/202243339">10.1051/0004-6361/202243339 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A fast radio burst with sub-millisecond quasi-periodic structure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pastor-Marazuela%2C+I">In茅s Pastor-Marazuela</a>, <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+J">Joeri van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=Bilous%2C+A">Anna Bilous</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">Liam Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Maan%2C+Y">Yogesh Maan</a>, <a href="/search/astro-ph?searchtype=author&query=Oostrum%2C+L">Leon Oostrum</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">Emily Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Straal%2C+S">Samayra Straal</a>, <a href="/search/astro-ph?searchtype=author&query=Vohl%2C+D">Dany Vohl</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">E. A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">B. Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=Attema%2C+J">Jisk Attema</a>, <a href="/search/astro-ph?searchtype=author&query=Boersma%2C+O+M">Oliver M. Boersma</a>, <a href="/search/astro-ph?searchtype=author&query=Brink%2C+R+v+d">R. van den Brink</a>, <a href="/search/astro-ph?searchtype=author&query=van+Cappellen%2C+W+A">W. A. van Cappellen</a>, <a href="/search/astro-ph?searchtype=author&query=Coolen%2C+A+H+W+M">A. H. W. M. Coolen</a>, <a href="/search/astro-ph?searchtype=author&query=Damstra%2C+S">S. Damstra</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9nes%2C+H">H. D茅nes</a>, <a href="/search/astro-ph?searchtype=author&query=Hess%2C+K+M">K. M. Hess</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Hulst%2C+J+M">J. M. van der Hulst</a>, <a href="/search/astro-ph?searchtype=author&query=Hut%2C+B">B. Hut</a>, <a href="/search/astro-ph?searchtype=author&query=Kutkin%2C+A">A. Kutkin</a>, <a href="/search/astro-ph?searchtype=author&query=Loose%2C+G+M">G. Marcel Loose</a>, <a href="/search/astro-ph?searchtype=author&query=Lucero%2C+D+M">D. M. Lucero</a>, <a href="/search/astro-ph?searchtype=author&query=Mika%2C+%C3%81">脕. Mika</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="2202.08002v1-abstract-short" style="display: inline;"> Fast radio bursts (FRBs) are extragalactic radio transients of extraordinary luminosity. Studying the diverse temporal and spectral behaviour recently observed in a number of FRBs may help determine the nature of the entire class. For example, a fast spinning or highly magnetised neutron star might generate the rotation-powered acceleration required to explain the bright emission. Periodic, sub-se… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.08002v1-abstract-full').style.display = 'inline'; document.getElementById('2202.08002v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.08002v1-abstract-full" style="display: none;"> Fast radio bursts (FRBs) are extragalactic radio transients of extraordinary luminosity. Studying the diverse temporal and spectral behaviour recently observed in a number of FRBs may help determine the nature of the entire class. For example, a fast spinning or highly magnetised neutron star might generate the rotation-powered acceleration required to explain the bright emission. Periodic, sub-second components, suggesting such rotation, were recently reported in one FRB, and potentially in two more. Here we report the discovery of FRB 20201020A with Apertif, an FRB showing five components regularly spaced by 0.415 ms. This sub-millisecond structure in FRB 20201020A carries important clues about the progenitor of this FRB specifically, and potentially about that of FRBs in general. We thus contrast its features to the predictions of the main FRB source models. We perform a timing analysis of the FRB 20201020A components to determine the significance of the periodicity. We compare these against the timing properties of the previously reported CHIME FRBs with sub-second quasi-periodic components, and against two Apertif bursts from repeating FRB 20180916B that show complex time-frequency structure. We find the periodicity of FRB 20201020A to be marginally significant at 2.5$蟽$. Its repeating subcomponents cannot be explained as a pulsar rotation since the required spin rate of over 2 kHz exceeds the limits set by typical neutron star equations of state and observations. The fast periodicity is also in conflict with a compact object merger scenario. These quasi-periodic components could, however, be caused by equidistant emitting regions in the magnetosphere of a magnetar. The sub-millisecond spacing of the components in FRB 20201020A, the smallest observed so far in a one-off FRB, may rule out both neutron-star rotation and binary mergers as the direct source of quasi-periodic FRBs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.08002v1-abstract-full').style.display = 'none'; document.getElementById('2202.08002v1-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 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">13 pages, 6 figures, 3 tables, supplementary material. Submitted to A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 678, A149 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.02382">arXiv:2111.02382</a> <span> [<a href="https://arxiv.org/pdf/2111.02382">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/ac6cee">10.3847/1538-4357/ac6cee <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multiband Detection of Repeating FRB 20180916B </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sand%2C+K+R">Ketan R. Sand</a>, <a href="/search/astro-ph?searchtype=author&query=Faber%2C+J">Jakob Faber</a>, <a href="/search/astro-ph?searchtype=author&query=Gajjar%2C+V">Vishal Gajjar</a>, <a href="/search/astro-ph?searchtype=author&query=Michilli%2C+D">Daniele Michilli</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+B+C">Bridget C. Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Joshi%2C+B+C">Bhal Chandra Joshi</a>, <a href="/search/astro-ph?searchtype=author&query=Kudale%2C+S">Sanjay Kudale</a>, <a href="/search/astro-ph?searchtype=author&query=Pilia%2C+M">Maura Pilia</a>, <a href="/search/astro-ph?searchtype=author&query=Brzycki%2C+B">Bryan Brzycki</a>, <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">Tomas Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Croft%2C+S">Steve Croft</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+B">Biprateep Dey</a>, <a href="/search/astro-ph?searchtype=author&query=John%2C+H">Hoang John</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">Calvin Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Mckinven%2C+R">Ryan Mckinven</a>, <a href="/search/astro-ph?searchtype=author&query=Ng%2C+C">Cherry Ng</a>, <a href="/search/astro-ph?searchtype=author&query=Pearlman%2C+A+B">Aaron B. Pearlman</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">Emily Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Price%2C+D+C">Danny C. Price</a>, <a href="/search/astro-ph?searchtype=author&query=Siemion%2C+A">Andrew Siemion</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+K">Kendrick Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Tendulkar%2C+S+P">Shriharsh P. Tendulkar</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.02382v2-abstract-short" style="display: inline;"> We present a multiband study of FRB 20180916B, a repeating source with a 16.3 day periodicity. We report the detection of 4, 1 and 7 bursts from observations spanning 3 days using upgraded Giant Metrewave Radio Telescope (300-500 MHz), Canadian Hydrogen Intensity Mapping Experiment (400-800 MHz) and Green Bank Telescope (600-1000 MHz), respectively. We report the first-ever detection of the source… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.02382v2-abstract-full').style.display = 'inline'; document.getElementById('2111.02382v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.02382v2-abstract-full" style="display: none;"> We present a multiband study of FRB 20180916B, a repeating source with a 16.3 day periodicity. We report the detection of 4, 1 and 7 bursts from observations spanning 3 days using upgraded Giant Metrewave Radio Telescope (300-500 MHz), Canadian Hydrogen Intensity Mapping Experiment (400-800 MHz) and Green Bank Telescope (600-1000 MHz), respectively. We report the first-ever detection of the source in the 800-1000 MHz range along with one of the widest instantaneous bandwidth detection (200 MHz) at lower frequencies. We identify 30 $渭$s wide structures in one of the bursts at 800 MHz, making it the lowest frequency detection of such structures for this FRB thus far. There is also a clear indication of high activity of the source at a higher frequency during earlier phases of the activity cycle. We identify a gradual decrease in the rotation measure over two years and no significant variations in the dispersion measure. We derive useful conclusions about progenitor scenarios, energy distribution, emission mechanisms, and variation of downward drift rate of emission with frequency. Our results reinforce that multiband observations are an effective approach to study repeaters and even one-off events to better understand their varying activity and spectral anomalies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.02382v2-abstract-full').style.display = 'none'; document.getElementById('2111.02382v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 10 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 932 98 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.14234">arXiv:2109.14234</a> <span> [<a href="https://arxiv.org/pdf/2109.14234">pdf</a>, <a href="https://arxiv.org/format/2109.14234">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202141739">10.1051/0004-6361/202141739 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Apertif, Phased Array Feeds for the Westerbork Synthesis Radio Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=van+Cappellen%2C+W+A">W. A. van Cappellen</a>, <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T+A">T. A. Oosterloo</a>, <a href="/search/astro-ph?searchtype=author&query=Verheijen%2C+M+A+W">M. A. W. Verheijen</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">E. A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">B. Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=Braun%2C+R">R. Braun</a>, <a href="/search/astro-ph?searchtype=author&query=Hess%2C+K+M">K. M. Hess</a>, <a href="/search/astro-ph?searchtype=author&query=Holties%2C+H">H. Holties</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Hulst%2C+J+M">J. M. van der Hulst</a>, <a href="/search/astro-ph?searchtype=author&query=Hut%2C+B">B. Hut</a>, <a href="/search/astro-ph?searchtype=author&query=Kooistra%2C+E">E. Kooistra</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=Loose%2C+G+M">G. M. Loose</a>, <a href="/search/astro-ph?searchtype=author&query=Morganti%2C+R">R. Morganti</a>, <a href="/search/astro-ph?searchtype=author&query=Moss%2C+V+A">V. A. Moss</a>, <a href="/search/astro-ph?searchtype=author&query=Orr%C3%BA%2C+E">E. Orr煤</a>, <a href="/search/astro-ph?searchtype=author&query=Ruiter%2C+M">M. Ruiter</a>, <a href="/search/astro-ph?searchtype=author&query=Schoenmakers%2C+A+P">A. P. Schoenmakers</a>, <a href="/search/astro-ph?searchtype=author&query=Vermaas%2C+N+J">N. J. Vermaas</a>, <a href="/search/astro-ph?searchtype=author&query=Wijnholds%2C+S+J">S. J. Wijnholds</a>, <a href="/search/astro-ph?searchtype=author&query=van+Amesfoort%2C+A+S">A. S. van Amesfoort</a>, <a href="/search/astro-ph?searchtype=author&query=Arts%2C+M+J">M. J. Arts</a>, <a href="/search/astro-ph?searchtype=author&query=Attema%2C+J+J">J. J. Attema</a>, <a href="/search/astro-ph?searchtype=author&query=Bakker%2C+L">L. Bakker</a>, <a href="/search/astro-ph?searchtype=author&query=Bassa%2C+C+G">C. G. Bassa</a> , et al. (65 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.14234v2-abstract-short" style="display: inline;"> We describe the APERture Tile In Focus (Apertif) system, a phased array feed (PAF) upgrade of the Westerbork Synthesis Radio Telescope which has transformed this telescope into a high-sensitivity, wide field-of-view L-band imaging and transient survey instrument. Using novel PAF technology, up to 40 partially overlapping beams can be formed on the sky simultaneously, significantly increasing the s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.14234v2-abstract-full').style.display = 'inline'; document.getElementById('2109.14234v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.14234v2-abstract-full" style="display: none;"> We describe the APERture Tile In Focus (Apertif) system, a phased array feed (PAF) upgrade of the Westerbork Synthesis Radio Telescope which has transformed this telescope into a high-sensitivity, wide field-of-view L-band imaging and transient survey instrument. Using novel PAF technology, up to 40 partially overlapping beams can be formed on the sky simultaneously, significantly increasing the survey speed of the telescope. With this upgraded instrument, an imaging survey covering an area of 2300 deg2 is being performed which will deliver both continuum and spectral line data sets, of which the first data has been publicly released. In addition, a time domain transient and pulsar survey covering 15,000 deg2 is in progress. An overview of the Apertif science drivers, hardware and software of the upgraded telescope is presented, along with its key performance characteristics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.14234v2-abstract-full').style.display = 'none'; document.getElementById('2109.14234v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 42 figures, accepted for publication by 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 658, A146 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.09254">arXiv:2109.09254</a> <span> [<a href="https://arxiv.org/pdf/2109.09254">pdf</a>, <a href="https://arxiv.org/format/2109.09254">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/ac4bc7">10.3847/1538-4357/ac4bc7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A sudden period of high activity from repeating Fast Radio Burst 20201124A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lanman%2C+A+E">Adam E. Lanman</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+B+C">Bridget C. Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Chawla%2C+P">Pragya Chawla</a>, <a href="/search/astro-ph?searchtype=author&query=Josephy%2C+A">Alexander Josephy</a>, <a href="/search/astro-ph?searchtype=author&query=Noble%2C+G">Gavin Noble</a>, <a href="/search/astro-ph?searchtype=author&query=Kaspi%2C+V+M">Victoria M. Kaspi</a>, <a href="/search/astro-ph?searchtype=author&query=Bandura%2C+K">Kevin Bandura</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">Mohit Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+P+J">Patrick J. Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Brar%2C+C">Charanjot Brar</a>, <a href="/search/astro-ph?searchtype=author&query=Breitman%2C+D">Daniela Breitman</a>, <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">Tomas Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+F">Fengqi Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Fonseca%2C+E">Emmanuel Fonseca</a>, <a href="/search/astro-ph?searchtype=author&query=Gaensler%2C+B+M">Bryan M. Gaensler</a>, <a href="/search/astro-ph?searchtype=author&query=Good%2C+D">Deborah Good</a>, <a href="/search/astro-ph?searchtype=author&query=Kaczmarek%2C+J">Jane Kaczmarek</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">Calvin Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K+W">Kiyoshi W. Masui</a>, <a href="/search/astro-ph?searchtype=author&query=Meyers%2C+B+W">Bradley W. Meyers</a>, <a href="/search/astro-ph?searchtype=author&query=Ng%2C+C">Cherry Ng</a>, <a href="/search/astro-ph?searchtype=author&query=Patel%2C+C">Chitrang Patel</a>, <a href="/search/astro-ph?searchtype=author&query=Pearlman%2C+A+B">Aaron B. Pearlman</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">Emily Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Pleunis%2C+Z">Ziggy Pleunis</a> , et al. (8 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.09254v3-abstract-short" style="display: inline;"> The repeating FRB 20201124A was first discovered by CHIME/FRB in November of 2020, after which it was seen to repeat a few times over several months. It entered a period of high activity in April of 2021, at which time several observatories recorded tens to hundreds more bursts from the source. These follow-up observations enabled precise localization and host galaxy identification. In this paper,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.09254v3-abstract-full').style.display = 'inline'; document.getElementById('2109.09254v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.09254v3-abstract-full" style="display: none;"> The repeating FRB 20201124A was first discovered by CHIME/FRB in November of 2020, after which it was seen to repeat a few times over several months. It entered a period of high activity in April of 2021, at which time several observatories recorded tens to hundreds more bursts from the source. These follow-up observations enabled precise localization and host galaxy identification. In this paper, we report on the CHIME/FRB-detected bursts from FRB 20201124A, including their best-fit morphologies, fluences, and arrival times. The large exposure time of the CHIME/FRB telescope to the location of this source allows us to constrain its rates of activity. We analyze the repetition rates over different spans of time, constraining the rate prior to discovery to $< 3.4$ day$^{-1}$ (at 3$蟽$), and demonstrate significant change in the event rate following initial detection. Lastly, we perform a maximum-likelihood estimation of a power-law luminosity function, finding a best-fit index $伪= -4.6 \pm 1.3 \pm 0.6$, with a break at a fluence threshold of $F_{\rm min} \sim 16.6$~Jy~ms, consistent with the fluence completeness limit of the observations. This index is consistent within uncertainties with those of other repeating FRBs for which it has been determined. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.09254v3-abstract-full').style.display = 'none'; document.getElementById('2109.09254v3-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 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 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/2109.08500">arXiv:2109.08500</a> <span> [<a href="https://arxiv.org/pdf/2109.08500">pdf</a>, <a href="https://arxiv.org/format/2109.08500">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/10.1051/0004-6361/202142242">10.1051/0004-6361/202142242 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dual-frequency single-pulse study of PSR B0950+08 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bilous%2C+A+V">A. V. Bilous</a>, <a href="/search/astro-ph?searchtype=author&query=Griessmeier%2C+J+M">J. M. Griessmeier</a>, <a href="/search/astro-ph?searchtype=author&query=Pennucci%2C+T">T. Pennucci</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+Z">Z. Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Bondonneau%2C+L">L. Bondonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Kondratiev%2C+V">V. Kondratiev</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=Maan%2C+Y">Y. Maan</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">L. Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Oostrum%2C+L+C">L. C. Oostrum</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">E. Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Verbiest%2C+J+P+W">J. P. W. Verbiest</a>, <a href="/search/astro-ph?searchtype=author&query=Vohl%2C+D">D. Vohl</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=Shaifullah%2C+G">G. Shaifullah</a>, <a href="/search/astro-ph?searchtype=author&query=Theureau%2C+G">G. Theureau</a>, <a href="/search/astro-ph?searchtype=author&query=Ulyanov%2C+O+M">O. M. Ulyanov</a>, <a href="/search/astro-ph?searchtype=author&query=Cecconi%2C+B">B. Cecconi</a>, <a href="/search/astro-ph?searchtype=author&query=Coolen%2C+A+H">A. H. Coolen</a>, <a href="/search/astro-ph?searchtype=author&query=Corbel%2C+S">S. Corbel</a>, <a href="/search/astro-ph?searchtype=author&query=Damstra%2C+S">S. Damstra</a>, <a href="/search/astro-ph?searchtype=author&query=Denes%2C+H">H. Denes</a>, <a href="/search/astro-ph?searchtype=author&query=Girard%2C+J+N">J. N. Girard</a>, <a href="/search/astro-ph?searchtype=author&query=Hut%2C+B">B. Hut</a>, <a href="/search/astro-ph?searchtype=author&query=Ivashina%2C+M">M. Ivashina</a> , et al. (11 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2109.08500v2-abstract-short" style="display: inline;"> PSR B0950+08 is a bright non-recycled pulsar whose single-pulse fluence variability is reportedly large. Based on observations at two widely separated frequencies, 55 MHz (NenuFAR) and 1.4 GHz (Westerbork Synthesis Radio Telescope), we review the properties of these single pulses. We conclude that they are more similar to ordinary pulses of radio emission than to a special kind of short and bright… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.08500v2-abstract-full').style.display = 'inline'; document.getElementById('2109.08500v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.08500v2-abstract-full" style="display: none;"> PSR B0950+08 is a bright non-recycled pulsar whose single-pulse fluence variability is reportedly large. Based on observations at two widely separated frequencies, 55 MHz (NenuFAR) and 1.4 GHz (Westerbork Synthesis Radio Telescope), we review the properties of these single pulses. We conclude that they are more similar to ordinary pulses of radio emission than to a special kind of short and bright Giant Pulses, observed from only a handful of pulsars. We argue that temporal variation of properties of interstellar medium along the line of sight to this nearby pulsar, namely the fluctuating size of decorrelation bandwidth of diffractive scintillation makes important contribution to observed single-pulse fluence variability. We further present interesting structures in the low-frequency single-pulse spectra that resemble the "sad trombones" seen in Fast Radio Bursts (FRBs); although for PSR B0950+08 the upward frequency drift is also routinely present. We explain these spectral features with radius-to-frequency mapping, similar to the model developed by Wang et al. (2019) for FRBs. Finally, we speculate that microsecond-scale fluence variability of the general pulsar population remains poorly known, and that its further study may bring important clues about the nature of FRBs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.08500v2-abstract-full').style.display = 'none'; document.getElementById('2109.08500v2-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 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by A&A. This version includes a number of minor corrections, including corrected FRB luminosities on the time-luminosity phase-space plot for radio pulses from neutron stars and repeating FRBs</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 658, A143 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.12122">arXiv:2108.12122</a> <span> [<a href="https://arxiv.org/pdf/2108.12122">pdf</a>, <a href="https://arxiv.org/format/2108.12122">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ac223b">10.3847/2041-8213/ac223b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Local Universe Host for the Repeating Fast Radio Burst FRB 20181030A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">M. Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Kirichenko%2C+A+Y">A. Yu. Kirichenko</a>, <a href="/search/astro-ph?searchtype=author&query=Michilli%2C+D">D. Michilli</a>, <a href="/search/astro-ph?searchtype=author&query=Mayya%2C+Y+D">Y. D. Mayya</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=Gaensler%2C+B+M">B. M. Gaensler</a>, <a href="/search/astro-ph?searchtype=author&query=Rahman%2C+M">M. Rahman</a>, <a href="/search/astro-ph?searchtype=author&query=Tendulkar%2C+S+P">S. P. Tendulkar</a>, <a href="/search/astro-ph?searchtype=author&query=Fonseca%2C+E">E. Fonseca</a>, <a href="/search/astro-ph?searchtype=author&query=Josephy%2C+A">Alexander Josephy</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">C. Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Merryfield%2C+M">Marcus Merryfield</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">Emily Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Pleunis%2C+Z">Z. Pleunis</a>, <a href="/search/astro-ph?searchtype=author&query=Sanghavi%2C+P">Pranav Sanghavi</a>, <a href="/search/astro-ph?searchtype=author&query=Scholz%2C+P">P. Scholz</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+K">K. Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+K+M">Kendrick M. Smith</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="2108.12122v1-abstract-short" style="display: inline;"> We report on the host association of FRB 20181030A, a repeating fast radio burst (FRB) with a low dispersion measure (DM, 103.5 pc cm$^{-3}$) discovered by CHIME/FRB Collaboration et al. (2019a). Using baseband voltage data saved for its repeat bursts, we localize the FRB to a sky area of 5.3 sq. arcmin (90% confidence). Within the FRB localization region, we identify NGC 3252 as the most promisin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.12122v1-abstract-full').style.display = 'inline'; document.getElementById('2108.12122v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.12122v1-abstract-full" style="display: none;"> We report on the host association of FRB 20181030A, a repeating fast radio burst (FRB) with a low dispersion measure (DM, 103.5 pc cm$^{-3}$) discovered by CHIME/FRB Collaboration et al. (2019a). Using baseband voltage data saved for its repeat bursts, we localize the FRB to a sky area of 5.3 sq. arcmin (90% confidence). Within the FRB localization region, we identify NGC 3252 as the most promising host, with an estimated chance coincidence probability $< 2.5 \times 10^{-3}$. Moreover, we do not find any other galaxy with M$_{r} < -15$ AB mag within the localization region to the maximum estimated FRB redshift of 0.05. This rules out a dwarf host 5 times less luminous than any FRB host discovered to date. NGC 3252 is a star-forming spiral galaxy, and at a distance of $\approx$ 20 Mpc, it is one of the closest FRB hosts discovered thus far. From our archival radio data search, we estimate a 3$蟽$ upper limit on the luminosity of a persistent compact radio source (source size $<$ 0.3 kpc at 20 Mpc) at 3 GHz to be ${\rm 2 \times 10^{26} erg~s^{-1} Hz^{-1}}$, at least 1500 times smaller than that of the FRB 20121102A persistent radio source. We also argue that a population of young millisecond magnetars alone cannot explain the observed volumetric rate of repeating FRBs. Finally, FRB 20181030A is a promising source for constraining FRB emission models due to its proximity, and we strongly encourage its multi-wavelength follow-up. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.12122v1-abstract-full').style.display = 'none'; document.getElementById('2108.12122v1-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">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">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/2107.10858">arXiv:2107.10858</a> <span> [<a href="https://arxiv.org/pdf/2107.10858">pdf</a>, <a href="https://arxiv.org/format/2107.10858">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac49e1">10.3847/1538-4357/ac49e1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Modeling Fast Radio Burst Dispersion and Scattering Properties in the First CHIME/FRB Catalog </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chawla%2C+P">P. Chawla</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=Ransom%2C+S+M">S. M. Ransom</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">M. Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+P+J">P. J. Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Breitman%2C+D">D. Breitman</a>, <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">T. Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cubranic%2C+D">D. Cubranic</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+F+Q">F. Q. Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Fonseca%2C+E">E. Fonseca</a>, <a href="/search/astro-ph?searchtype=author&query=Gaensler%2C+B+M">B. M. Gaensler</a>, <a href="/search/astro-ph?searchtype=author&query=Giri%2C+U">U. Giri</a>, <a href="/search/astro-ph?searchtype=author&query=Josephy%2C+A">A. Josephy</a>, <a href="/search/astro-ph?searchtype=author&query=Kaczmarek%2C+J+F">J. F. Kaczmarek</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">C. Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K+W">K. W. Masui</a>, <a href="/search/astro-ph?searchtype=author&query=Mena-Parra%2C+J">J. Mena-Parra</a>, <a href="/search/astro-ph?searchtype=author&query=Merryfield%2C+M">M. Merryfield</a>, <a href="/search/astro-ph?searchtype=author&query=Michilli%2C+D">D. Michilli</a>, <a href="/search/astro-ph?searchtype=author&query=M%7F%C3%BCnchmeyer%2C+M">M. M眉nchmeyer</a>, <a href="/search/astro-ph?searchtype=author&query=Ng%2C+C">C. Ng</a>, <a href="/search/astro-ph?searchtype=author&query=Patel%2C+C">C. Patel</a>, <a href="/search/astro-ph?searchtype=author&query=Pearlman%2C+A+B">A. B. Pearlman</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">E. Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Pleunis%2C+Z">Z. Pleunis</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2107.10858v2-abstract-short" style="display: inline;"> We present a Monte Carlo-based population synthesis study of fast radio burst (FRB) dispersion and scattering focusing on the first catalog of sources detected with the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst (CHIME/FRB) project. We simulate intrinsic properties and propagation effects for a variety of FRB population models and compare the simulated distributions of dispers… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.10858v2-abstract-full').style.display = 'inline'; document.getElementById('2107.10858v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.10858v2-abstract-full" style="display: none;"> We present a Monte Carlo-based population synthesis study of fast radio burst (FRB) dispersion and scattering focusing on the first catalog of sources detected with the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst (CHIME/FRB) project. We simulate intrinsic properties and propagation effects for a variety of FRB population models and compare the simulated distributions of dispersion measures (DMs) and scattering timescales with the corresponding distributions from the CHIME/FRB catalog. Our simulations confirm the results of previous population studies, which suggested that the interstellar medium of the host galaxy alone (simulated based on the NE2001 model) cannot explain the observed scattering timescales of FRBs. We therefore consider additional sources of scattering, namely, the circumgalactic medium (CGM) of intervening galaxies and the circumburst medium whose properties are modeled based on typical Galactic plane environments. We find that a population of FRBs with scattering contributed by these media is marginally consistent with the CHIME/FRB catalog. In this scenario, our simulations favor a population of FRBs offset from their galaxy centers over a population which is distributed along the spiral arms. However, if the models proposing the CGM as a source of intense scattering are incorrect, then we conclude that FRBs may inhabit environments with more extreme properties than those inferred for pulsars in the Milky Way. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.10858v2-abstract-full').style.display = 'none'; document.getElementById('2107.10858v2-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 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in 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/2107.10113">arXiv:2107.10113</a> <span> [<a href="https://arxiv.org/pdf/2107.10113">pdf</a>, <a href="https://arxiv.org/format/2107.10113">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s00159-022-00139-w">10.1007/s00159-022-00139-w <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Fast radio bursts at the dawn of the 2020s </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">E. Petroff</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=Lorimer%2C+D+R">D. R. Lorimer</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2107.10113v2-abstract-short" style="display: inline;"> Since the discovery of the first fast radio burst (FRB) in 2007, and their confirmation as an abundant extragalactic population in 2013, the study of these sources has expanded at an incredible rate. In our 2019 review on the subject we presented a growing, but still mysterious, population of FRBs -- 60 unique sources, 2 repeating FRBs, and only 1 identified host galaxy. However, in only a few sho… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.10113v2-abstract-full').style.display = 'inline'; document.getElementById('2107.10113v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.10113v2-abstract-full" style="display: none;"> Since the discovery of the first fast radio burst (FRB) in 2007, and their confirmation as an abundant extragalactic population in 2013, the study of these sources has expanded at an incredible rate. In our 2019 review on the subject we presented a growing, but still mysterious, population of FRBs -- 60 unique sources, 2 repeating FRBs, and only 1 identified host galaxy. However, in only a few short years new observations and discoveries have given us a wealth of information about these sources. The total FRB population now stands at over 600 published sources, 24 repeaters, and 19 host galaxies. Higher time resolution data, sustained monitoring, and precision localisations have given us insight into repeaters, host galaxies, burst morphology, source activity, progenitor models, and the use of FRBs as cosmological probes. The recent detection of a bright FRB-like burst from the Galactic magnetar SGR~1935+2154 provides an important link between FRBs and magnetars. There also continue to be surprising discoveries, like periodic modulation of activity from repeaters and the localisation of one FRB source to a relatively nearby globular cluster associated with the M81 galaxy. In this review, we summarise the exciting observational results from the past few years. We also highlight their impact on our understanding of the FRB population and proposed progenitor models. We build on the introduction to FRBs in our earlier review, update our readers on recent results, and discuss interesting avenues for exploration as the field enters a new regime where hundreds to thousands of new FRBs will be discovered and reported each year. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.10113v2-abstract-full').style.display = 'none'; document.getElementById('2107.10113v2-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Invited review article for The Astronomy and Astrophysics Review. Resubmission with community feedback; thank you for your comments</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.08463">arXiv:2107.08463</a> <span> [<a href="https://arxiv.org/pdf/2107.08463">pdf</a>, <a href="https://arxiv.org/format/2107.08463">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/s41586-022-04841-8">10.1038/s41586-022-04841-8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sub-second periodicity in a fast radio burst </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+T+C">The CHIME/FRB Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+B+C">Bridget C. Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Bandura%2C+K">Kevin Bandura</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">Mohit Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+P+J">P. J. Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Brar%2C+C">Charanjot Brar</a>, <a href="/search/astro-ph?searchtype=author&query=Breitman%2C+D">Daniela Breitman</a>, <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">Tomas Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Chatterjee%2C+S">Shami Chatterjee</a>, <a href="/search/astro-ph?searchtype=author&query=Chawla%2C+P">Pragya Chawla</a>, <a href="/search/astro-ph?searchtype=author&query=Cliche%2C+J">Jean-Fran莽ois Cliche</a>, <a href="/search/astro-ph?searchtype=author&query=Cubranic%2C+D">Davor Cubranic</a>, <a href="/search/astro-ph?searchtype=author&query=Curtin%2C+A+P">Alice P. Curtin</a>, <a href="/search/astro-ph?searchtype=author&query=Deng%2C+M">Meiling Deng</a>, <a href="/search/astro-ph?searchtype=author&query=Dobbs%2C+M">Matt Dobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+F+A">Fengqiu Adam Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Fonseca%2C+E">Emmanuel Fonseca</a>, <a href="/search/astro-ph?searchtype=author&query=Gaensler%2C+B+M">B. M. Gaensler</a>, <a href="/search/astro-ph?searchtype=author&query=Giri%2C+U">Utkarsh Giri</a>, <a href="/search/astro-ph?searchtype=author&query=Good%2C+D+C">Deborah C. Good</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+A+S">Alex S. Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Josephy%2C+A">Alexander Josephy</a>, <a href="/search/astro-ph?searchtype=author&query=Kaczmarek%2C+J+F">J. F. Kaczmarek</a>, <a href="/search/astro-ph?searchtype=author&query=Kader%2C+Z">Zarif Kader</a>, <a href="/search/astro-ph?searchtype=author&query=Kania%2C+J">Joseph Kania</a> , et al. (37 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2107.08463v2-abstract-short" style="display: inline;"> Fast radio bursts (FRBs) are millisecond-duration flashes of radio waves that are visible at distances of billions of light-years. The nature of their progenitors and their emission mechanism remain open astrophysical questions. Here we report the detection of the multi-component FRB 20191221A and the identification of a periodic separation of 216.8(1) ms between its components with a significance… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.08463v2-abstract-full').style.display = 'inline'; document.getElementById('2107.08463v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.08463v2-abstract-full" style="display: none;"> Fast radio bursts (FRBs) are millisecond-duration flashes of radio waves that are visible at distances of billions of light-years. The nature of their progenitors and their emission mechanism remain open astrophysical questions. Here we report the detection of the multi-component FRB 20191221A and the identification of a periodic separation of 216.8(1) ms between its components with a significance of 6.5 sigmas. The long (~3 s) duration and nine or more components forming the pulse profile make this source an outlier in the FRB population. Such short periodicity provides strong evidence for a neutron-star origin of the event. Moreover, our detection favours emission arising from the neutron-star magnetosphere, as opposed to emission regions located further away from the star, as predicted by some models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.08463v2-abstract-full').style.display = 'none'; document.getElementById('2107.08463v2-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 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Updated to conform to the accepted version</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.04354">arXiv:2106.04354</a> <span> [<a href="https://arxiv.org/pdf/2106.04354">pdf</a>, <a href="https://arxiv.org/format/2106.04354">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/ac1dab">10.3847/1538-4357/ac1dab <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CHIME/FRB Catalog 1 results: statistical cross-correlations with large-scale structure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rafiei-Ravandi%2C+M">Masoud Rafiei-Ravandi</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+K+M">Kendrick M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+D">Dongzi Li</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K+W">Kiyoshi W. Masui</a>, <a href="/search/astro-ph?searchtype=author&query=Josephy%2C+A">Alexander Josephy</a>, <a href="/search/astro-ph?searchtype=author&query=Dobbs%2C+M">Matt Dobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Lang%2C+D">Dustin Lang</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">Mohit Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Patel%2C+C">Chitrang Patel</a>, <a href="/search/astro-ph?searchtype=author&query=Bandura%2C+K">Kevin Bandura</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+S">Sabrina Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+P+J">P. J. Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Brar%2C+C">Charanjot Brar</a>, <a href="/search/astro-ph?searchtype=author&query=Breitman%2C+D">Daniela Breitman</a>, <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">Tomas Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Chawla%2C+P">Pragya Chawla</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+F+A">Fengqiu Adam Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Fonseca%2C+E">Emmanuel Fonseca</a>, <a href="/search/astro-ph?searchtype=author&query=Gaensler%2C+B+M">B. M. Gaensler</a>, <a href="/search/astro-ph?searchtype=author&query=Giri%2C+U">Utkarsh Giri</a>, <a href="/search/astro-ph?searchtype=author&query=Good%2C+D+C">Deborah C. Good</a>, <a href="/search/astro-ph?searchtype=author&query=Halpern%2C+M">Mark Halpern</a>, <a href="/search/astro-ph?searchtype=author&query=Kaczmarek%2C+J">Jane Kaczmarek</a>, <a href="/search/astro-ph?searchtype=author&query=Kaspi%2C+V+M">Victoria M. Kaspi</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">Calvin Leung</a> , et al. (16 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.04354v2-abstract-short" style="display: inline;"> The CHIME/FRB Project has recently released its first catalog of fast radio bursts (FRBs), containing 492 unique sources. We present results from angular cross-correlations of CHIME/FRB sources with galaxy catalogs. We find a statistically significant ($p$-value $\sim 10^{-4}$, accounting for look-elsewhere factors) cross-correlation between CHIME FRBs and galaxies in the redshift range… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.04354v2-abstract-full').style.display = 'inline'; document.getElementById('2106.04354v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.04354v2-abstract-full" style="display: none;"> The CHIME/FRB Project has recently released its first catalog of fast radio bursts (FRBs), containing 492 unique sources. We present results from angular cross-correlations of CHIME/FRB sources with galaxy catalogs. We find a statistically significant ($p$-value $\sim 10^{-4}$, accounting for look-elsewhere factors) cross-correlation between CHIME FRBs and galaxies in the redshift range $0.3 \lesssim z \lesssim 0.5$, in three photometric galaxy surveys: WISE$\times$SCOS, DESI-BGS, and DESI-LRG. The level of cross-correlation is consistent with an order-one fraction of the CHIME FRBs being in the same dark matter halos as survey galaxies in this redshift range. We find statistical evidence for a population of FRBs with large host dispersion measure ($\sim 400$ pc cm$^{-3}$), and show that this can plausibly arise from gas in large halos ($M \sim 10^{14} M_\odot$), for FRBs near the halo center ($r \lesssim 100$ kpc). These results will improve in future CHIME/FRB catalogs, with more FRBs and better angular resolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.04354v2-abstract-full').style.display = 'none'; document.getElementById('2106.04354v2-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 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 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">26 pages, 16 figures, published in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.04352">arXiv:2106.04352</a> <span> [<a href="https://arxiv.org/pdf/2106.04352">pdf</a>, <a href="https://arxiv.org/format/2106.04352">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.3847/1538-4365/ac33ab">10.3847/1538-4365/ac33ab <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The First CHIME/FRB Fast Radio Burst Catalog </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+T+C">The CHIME/FRB Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+B+C">Bridget C. Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Bandura%2C+K">Kevin Bandura</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+S">Sabrina Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">Mohit Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Boyce%2C+M+M">Michelle M. Boyce</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+P+J">P. J. Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Brar%2C+C">Charanjot Brar</a>, <a href="/search/astro-ph?searchtype=author&query=Breitman%2C+D">Daniela Breitman</a>, <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">Tomas Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Chawla%2C+P">Pragya Chawla</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+T">Tianyue Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cliche%2C+J+-">J. -F. Cliche</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+A">Amanda Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Cubranic%2C+D">Davor Cubranic</a>, <a href="/search/astro-ph?searchtype=author&query=Curtin%2C+A+P">Alice P. Curtin</a>, <a href="/search/astro-ph?searchtype=author&query=Deng%2C+M">Meiling Deng</a>, <a href="/search/astro-ph?searchtype=author&query=Dobbs%2C+M">Matt Dobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Fengqiu"> Fengqiu</a>, <a href="/search/astro-ph?searchtype=author&query=Dong"> Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Eadie%2C+G">Gwendolyn Eadie</a>, <a href="/search/astro-ph?searchtype=author&query=Fandino%2C+M">Mateus Fandino</a>, <a href="/search/astro-ph?searchtype=author&query=Fonseca%2C+E">Emmanuel Fonseca</a> , et al. (52 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="2106.04352v3-abstract-short" style="display: inline;"> We present a catalog of 536 fast radio bursts (FRBs) detected by the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst (CHIME/FRB) Project between 400 and 800 MHz from 2018 July 25 to 2019 July 1, including 62 bursts from 18 previously reported repeating sources. The catalog represents the first large sample, including bursts from repeaters and non-repeaters, observed in a single sur… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.04352v3-abstract-full').style.display = 'inline'; document.getElementById('2106.04352v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.04352v3-abstract-full" style="display: none;"> We present a catalog of 536 fast radio bursts (FRBs) detected by the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst (CHIME/FRB) Project between 400 and 800 MHz from 2018 July 25 to 2019 July 1, including 62 bursts from 18 previously reported repeating sources. The catalog represents the first large sample, including bursts from repeaters and non-repeaters, observed in a single survey with uniform selection effects. This facilitates comparative and absolute studies of the FRB population. We show that repeaters and apparent non-repeaters have sky locations and dispersion measures (DMs) that are consistent with being drawn from the same distribution. However, bursts from repeating sources differ from apparent non-repeaters in intrinsic temporal width and spectral bandwidth. Through injection of simulated events into our detection pipeline, we perform an absolute calibration of selection effects to account for systematic biases. We find evidence for a population of FRBs - comprising a large fraction of the overall population - with a scattering time at 600 MHz in excess of 10 ms, of which only a small fraction are observed by CHIME/FRB. We infer a power-law index for the cumulative fluence distribution of $伪=-1.40\pm0.11(\textrm{stat.})^{+0.06}_{-0.09}(\textrm{sys.})$, consistent with the $-3/2$ expectation for a non-evolving population in Euclidean space. We find $伪$ is steeper for high-DM events and shallower for low-DM events, which is what would be expected when DM is correlated with distance. We infer a sky rate of $[525\pm30(\textrm{stat.})^{+140}_{-130}({\textrm{sys.}})]/\textrm{sky}/\textrm{day}$ above a fluence of 5 Jy ms at 600 MHz, with scattering time at $600$ MHz under 10 ms, and DM above 100 pc cm$^{-3}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.04352v3-abstract-full').style.display = 'none'; document.getElementById('2106.04352v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 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">67 pages, 27 figures, 5 tables. Published in ApJS and updated with changes reflected in an erratum (affecting the sky rate). Extended figures and data at https://www.chime-frb.ca/catalog</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.11446">arXiv:2105.11446</a> <span> [<a href="https://arxiv.org/pdf/2105.11446">pdf</a>, <a href="https://arxiv.org/format/2105.11446">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"> Burst timescales and luminosities link young pulsars and fast radio bursts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nimmo%2C+K">K. Nimmo</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=Kirsten%2C+F">F. Kirsten</a>, <a href="/search/astro-ph?searchtype=author&query=Keimpema%2C+A">A. Keimpema</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=Snelders%2C+M+P">M. P. Snelders</a>, <a href="/search/astro-ph?searchtype=author&query=Hewitt%2C+D+M">D. M. Hewitt</a>, <a href="/search/astro-ph?searchtype=author&query=Karuppusamy%2C+R">R. Karuppusamy</a>, <a href="/search/astro-ph?searchtype=author&query=Archibald%2C+A+M">A. M. Archibald</a>, <a href="/search/astro-ph?searchtype=author&query=Bezukovs%2C+V">V. Bezukovs</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">M. Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Blaauw%2C+R">R. Blaauw</a>, <a href="/search/astro-ph?searchtype=author&query=Buttaccio%2C+S+T">S. T. Buttaccio</a>, <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">T. Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Conway%2C+J+E">J. E. Conway</a>, <a href="/search/astro-ph?searchtype=author&query=Corongiu%2C+A">A. Corongiu</a>, <a href="/search/astro-ph?searchtype=author&query=Feiler%2C+R">R. Feiler</a>, <a href="/search/astro-ph?searchtype=author&query=Fonseca%2C+E">E. Fonseca</a>, <a href="/search/astro-ph?searchtype=author&query=Forssen%2C+O">O. Forssen</a>, <a href="/search/astro-ph?searchtype=author&query=Gawronski%2C+M">M. Gawronski</a>, <a href="/search/astro-ph?searchtype=author&query=Giroletti%2C+M">M. Giroletti</a>, <a href="/search/astro-ph?searchtype=author&query=Kharinov%2C+M+A">M. A. Kharinov</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">C. Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Lindqvist%2C+M">M. Lindqvist</a>, <a href="/search/astro-ph?searchtype=author&query=Maccaferri%2C+G">G. Maccaferri</a> , et al. (23 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2105.11446v2-abstract-short" style="display: inline;"> Fast radio bursts (FRBs) are extragalactic radio flashes of unknown physical origin. Their high luminosities and short durations require extreme energy densities, like those found in the vicinity of neutron stars and black holes. Studying the burst intensities and polarimetric properties on a wide range of timescales, from milliseconds down to nanoseconds, is key to understanding the emission mech… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.11446v2-abstract-full').style.display = 'inline'; document.getElementById('2105.11446v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.11446v2-abstract-full" style="display: none;"> Fast radio bursts (FRBs) are extragalactic radio flashes of unknown physical origin. Their high luminosities and short durations require extreme energy densities, like those found in the vicinity of neutron stars and black holes. Studying the burst intensities and polarimetric properties on a wide range of timescales, from milliseconds down to nanoseconds, is key to understanding the emission mechanism. However, high-time-resolution studies of FRBs are limited by their unpredictable activity levels, available instrumentation and temporal broadening in the intervening ionised medium. Here we show that the repeating FRB 20200120E can produce isolated shots of emission as short as about 60 nanoseconds in duration, with brightness temperatures as high as $3\times 10^{41}$ K (excluding relativistic effects), comparable to `nano-shots' from the Crab pulsar. Comparing both the range of timescales and luminosities, we find that FRB 20200120E observationally bridges the gap between known Galactic young pulsars and magnetars, and the much more distant extragalactic FRBs. This suggests a common magnetically powered emission mechanism spanning many orders of magnitude in timescale and luminosity. In this work, we probe a relatively unexplored region of the short-duration transient phase space; we highlight that there likely exists a population of ultra-fast radio transients at nanosecond to microsecond timescales, which current FRB searches are insensitive to. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.11446v2-abstract-full').style.display = 'none'; document.getElementById('2105.11446v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted. Comments welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.11445">arXiv:2105.11445</a> <span> [<a href="https://arxiv.org/pdf/2105.11445">pdf</a>, <a href="https://arxiv.org/format/2105.11445">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41586-021-04354-w">10.1038/s41586-021-04354-w <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A repeating fast radio burst source in a globular cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kirsten%2C+F">F. Kirsten</a>, <a href="/search/astro-ph?searchtype=author&query=Marcote%2C+B">B. Marcote</a>, <a href="/search/astro-ph?searchtype=author&query=Nimmo%2C+K">K. Nimmo</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=Bhardwaj%2C+M">M. Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Tendulkar%2C+S+P">S. P. Tendulkar</a>, <a href="/search/astro-ph?searchtype=author&query=Keimpema%2C+A">A. Keimpema</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+J">J. Yang</a>, <a href="/search/astro-ph?searchtype=author&query=Snelders%2C+M+P">M. P. Snelders</a>, <a href="/search/astro-ph?searchtype=author&query=Scholz%2C+P">P. Scholz</a>, <a href="/search/astro-ph?searchtype=author&query=Pearlman%2C+A+B">A. B. Pearlman</a>, <a href="/search/astro-ph?searchtype=author&query=Law%2C+C+J">C. J. Law</a>, <a href="/search/astro-ph?searchtype=author&query=Peters%2C+W+M">W. M. Peters</a>, <a href="/search/astro-ph?searchtype=author&query=Giroletti%2C+M">M. Giroletti</a>, <a href="/search/astro-ph?searchtype=author&query=Paragi%2C+Z">Z. Paragi</a>, <a href="/search/astro-ph?searchtype=author&query=Bassa%2C+C">C. Bassa</a>, <a href="/search/astro-ph?searchtype=author&query=Hewitt%2C+D+M">D. M. Hewitt</a>, <a href="/search/astro-ph?searchtype=author&query=Bach%2C+U">U. Bach</a>, <a href="/search/astro-ph?searchtype=author&query=Bezrukovs%2C+V">V. Bezrukovs</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Buttaccio%2C+S+T">S. T. Buttaccio</a>, <a href="/search/astro-ph?searchtype=author&query=Conway%2C+J+E">J. E. Conway</a>, <a href="/search/astro-ph?searchtype=author&query=Corongiu%2C+A">A. Corongiu</a>, <a href="/search/astro-ph?searchtype=author&query=Feiler%2C+R">R. Feiler</a>, <a href="/search/astro-ph?searchtype=author&query=Forss%C3%A9n%2C+O">O. Forss茅n</a> , et al. (41 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2105.11445v2-abstract-short" style="display: inline;"> Fast radio bursts (FRBs) are exceptionally luminous flashes of unknown physical origin, reaching us from other galaxies (Petroff et al. 2019). Most FRBs have only ever been seen once, while others flash repeatedly, though sporadically (Spitler et al. 2016, CHIME/FRB Collaboration et al. 2021). Many models invoke magnetically powered neutron stars (magnetars) as the engines producing FRB emission (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.11445v2-abstract-full').style.display = 'inline'; document.getElementById('2105.11445v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.11445v2-abstract-full" style="display: none;"> Fast radio bursts (FRBs) are exceptionally luminous flashes of unknown physical origin, reaching us from other galaxies (Petroff et al. 2019). Most FRBs have only ever been seen once, while others flash repeatedly, though sporadically (Spitler et al. 2016, CHIME/FRB Collaboration et al. 2021). Many models invoke magnetically powered neutron stars (magnetars) as the engines producing FRB emission (Margalit & Metzger 2018, CHIME/FRB Collaboration et al. 2020). Recently, CHIME/FRB announced the discovery (Bhardwaj et al. 2021) of the repeating FRB 20200120E, coming from the direction of the nearby grand design spiral galaxy M81. Four potential counterparts at other observing wavelengths were identified (Bhardwaj et al. 2021) but no definitive association with these sources, or M81, could be made. Here we report an extremely precise localisation of FRB 20200120E, which allows us to associate it with a globular cluster (GC) in the M81 galactic system and to place it ~2pc offset from the optical center of light of the GC. This confirms (Bhardwaj et al. 2021) that FRB 20200120E is 40 times closer than any other known extragalactic FRB. Because such GCs host old stellar populations, this association strongly challenges FRB models that invoke young magnetars formed in a core-collapse supernova as powering FRB emission. We propose, instead, that FRB 20200120E is a highly magnetised neutron star formed via either accretion-induced collapse of a white dwarf or via merger of compact stars in a binary system (Margalit et al. 2019). Alternative scenarios involving compact binary systems, efficiently formed inside globular clusters, could also be responsible for the observed bursts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.11445v2-abstract-full').style.display = 'none'; document.getElementById('2105.11445v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted. Comments welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.11680">arXiv:2104.11680</a> <span> [<a href="https://arxiv.org/pdf/2104.11680">pdf</a>, <a href="https://arxiv.org/format/2104.11680">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/abe70d">10.3847/1538-4357/abe70d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Location of Young Pulsar PSR J0837$-$2454: Galactic Halo or Local Supernova Remnant? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pol%2C+N">Nihan Pol</a>, <a href="/search/astro-ph?searchtype=author&query=Burke-Spolaor%2C+S">Sarah Burke-Spolaor</a>, <a href="/search/astro-ph?searchtype=author&query=Hurley-Walker%2C+N">Natasha Hurley-Walker</a>, <a href="/search/astro-ph?searchtype=author&query=Blumer%2C+H">Harsha Blumer</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+S">Simon Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Keith%2C+M">Michael Keith</a>, <a href="/search/astro-ph?searchtype=author&query=Keane%2C+E+F">Evan F. Keane</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">Marta Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">Andrea Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">Emily Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Bhat%2C+N+D+R">N. D. Ramesh Bhat</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="2104.11680v1-abstract-short" style="display: inline;"> We present the discovery and timing of the young (age $\sim 28.6$ kyr) pulsar PSR J0837$-$2454. Based on its high latitude ($b = 9.8^{\circ}$) and dispersion measure (DM $ = 143$~pc~cm$^{-3}$), the pulsar appears to be at a $z$-height of $>$1 kpc above the Galactic plane, but near the edge of our Galaxy. This is many times the observed scale height of the canonical pulsar population, which suggest… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.11680v1-abstract-full').style.display = 'inline'; document.getElementById('2104.11680v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.11680v1-abstract-full" style="display: none;"> We present the discovery and timing of the young (age $\sim 28.6$ kyr) pulsar PSR J0837$-$2454. Based on its high latitude ($b = 9.8^{\circ}$) and dispersion measure (DM $ = 143$~pc~cm$^{-3}$), the pulsar appears to be at a $z$-height of $>$1 kpc above the Galactic plane, but near the edge of our Galaxy. This is many times the observed scale height of the canonical pulsar population, which suggests this pulsar may have been born far out of the plane. If accurate, the young age and high $z$-height imply that this is the first pulsar known to be born from a runaway O/B star. In follow-up imaging with the Australia Telescope Compact Array (ATCA), we detect the pulsar with a flux density $S_{1400} = 0.18 \pm 0.05$ mJy. We do not detect an obvious supernova remnant around the pulsar in our ATCA data, but we detect a co-located, low-surface-brightness region of $\sim$1.5$^\circ$ extent in archival Galactic and Extragalactic All-sky MWA Survey data. We also detect co-located H$伪$ emission from the Southern H$伪$ Sky Survey Atlas. Distance estimates based on these two detections come out to $\sim$0.9 kpc and $\sim$0.2 kpc respectively, both of which are much smaller than the distance predicted by the NE2001 model ($6.3$ kpc) and YMW model ($>25$ kpc) and place the pulsar much closer to the plane of the Galaxy. If the pulsar/remnant association holds, this result also highlights the inherent difficulty in the classification of transients as "Galactic" (pulsar) or "extragalactic" (fast radio burst) toward the Galactic anti-center based solely on the modeled Galactic electron contribution to a detection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.11680v1-abstract-full').style.display = 'none'; document.getElementById('2104.11680v1-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 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">Published in ApJ. 12 pages, 9 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/2012.08348">arXiv:2012.08348</a> <span> [<a href="https://arxiv.org/pdf/2012.08348">pdf</a>, <a href="https://arxiv.org/format/2012.08348">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/s41586-021-03724-8">10.1038/s41586-021-03724-8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Chromatic periodic activity down to 120 MHz in a Fast Radio Burst </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pastor-Marazuela%2C+I">In茅s Pastor-Marazuela</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">Liam Connor</a>, <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+J">Joeri van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=Maan%2C+Y">Yogesh Maan</a>, <a href="/search/astro-ph?searchtype=author&query=ter+Veen%2C+S">Sander ter Veen</a>, <a href="/search/astro-ph?searchtype=author&query=Bilous%2C+A">Anna Bilous</a>, <a href="/search/astro-ph?searchtype=author&query=Oostrum%2C+L">Leon Oostrum</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">Emily Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Straal%2C+S">Samayra Straal</a>, <a href="/search/astro-ph?searchtype=author&query=Vohl%2C+D">Dany Vohl</a>, <a href="/search/astro-ph?searchtype=author&query=Attema%2C+J">Jisk Attema</a>, <a href="/search/astro-ph?searchtype=author&query=Boersma%2C+O+M">Oliver M. Boersma</a>, <a href="/search/astro-ph?searchtype=author&query=Kooistra%2C+E">Eric Kooistra</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Schuur%2C+D">Daniel van der Schuur</a>, <a href="/search/astro-ph?searchtype=author&query=Sclocco%2C+A">Alessio Sclocco</a>, <a href="/search/astro-ph?searchtype=author&query=Smits%2C+R">Roy Smits</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">Elizabeth A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">Bj枚rn Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">Willem J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Coolen%2C+A+H+W+M">Arthur H. W. M. Coolen</a>, <a href="/search/astro-ph?searchtype=author&query=Damstra%2C+S">Sieds Damstra</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9nes%2C+H">Helga D茅nes</a>, <a href="/search/astro-ph?searchtype=author&query=Hess%2C+K+M">Kelley M. Hess</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Hulst%2C+T">Thijs van der Hulst</a>, <a href="/search/astro-ph?searchtype=author&query=Hut%2C+B">Boudewijn Hut</a> , et al. (12 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.08348v1-abstract-short" style="display: inline;"> Fast radio bursts (FRBs) are extragalactic astrophysical transients whose brightness requires emitters that are highly energetic, yet compact enough to produce the short, millisecond-duration bursts. FRBs have thus far been detected between 300 MHz and 8 GHz, but lower-frequency emission has remained elusive. A subset of FRBs is known to repeat, and one of those sources, FRB 20180916B, does so wit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.08348v1-abstract-full').style.display = 'inline'; document.getElementById('2012.08348v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.08348v1-abstract-full" style="display: none;"> Fast radio bursts (FRBs) are extragalactic astrophysical transients whose brightness requires emitters that are highly energetic, yet compact enough to produce the short, millisecond-duration bursts. FRBs have thus far been detected between 300 MHz and 8 GHz, but lower-frequency emission has remained elusive. A subset of FRBs is known to repeat, and one of those sources, FRB 20180916B, does so with a 16.3 day activity period. Using simultaneous Apertif and LOFAR data, we show that FRB 20180916B emits down to 120 MHz, and that its activity window is both narrower and earlier at higher frequencies. Binary wind interaction models predict a narrower periodic activity window at lower frequencies, which is the opposite of our observations. Our detections establish that low-frequency FRB emission can escape the local medium. For bursts of the same fluence, FRB 20180916B is more active below 200 MHz than at 1.4 GHz. Combining our results with previous upper-limits on the all-sky FRB rate at 150 MHz, we find that there are 3-450 FRBs/sky/day above 50 Jy ms at 90% confidence. We are able to rule out the scenario in which companion winds cause FRB periodicity. We also demonstrate that some FRBs live in clean environments that do not absorb or scatter low-frequency radiation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.08348v1-abstract-full').style.display = 'none'; document.getElementById('2012.08348v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">50 pages, 14 figures, 3 tables, submitted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.02460">arXiv:2012.02460</a> <span> [<a href="https://arxiv.org/pdf/2012.02460">pdf</a>, <a href="https://arxiv.org/format/2012.02460">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/10.1051/0004-6361/202039626">10.1051/0004-6361/202039626 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Synthesizing the repeating FRB population using frbpoppy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gardenier%2C+D+W">D. W. Gardenier</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">L. Connor</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=Oostrum%2C+L+C">L. C. Oostrum</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">E. Petroff</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.02460v1-abstract-short" style="display: inline;"> The observed Fast Radio Burst (FRB) population can be divided into one-off and repeating FRB sources. Either this division is a true dichotomy of the underlying sources, or selection effects and low activity prohibit us from observing repeat pulses from all constituents making up the FRB source population. We attempt to break this degeneracy through FRB population synthesis. With that aim we exten… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02460v1-abstract-full').style.display = 'inline'; document.getElementById('2012.02460v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.02460v1-abstract-full" style="display: none;"> The observed Fast Radio Burst (FRB) population can be divided into one-off and repeating FRB sources. Either this division is a true dichotomy of the underlying sources, or selection effects and low activity prohibit us from observing repeat pulses from all constituents making up the FRB source population. We attempt to break this degeneracy through FRB population synthesis. With that aim we extend frbpoppy, which earlier only handled one-off FRBs, to also simulate repeaters. We next model the Canadian Hydrogen Intensity Mapping Experiment FRB survey (CHIME/FRB). Using this implementation, we investigate the impact of luminosity functions on the observed dispersion measure (DM) and distance distributions of both repeating and one-off FRBs. We show that for a single, intrinsically repeating source population with a steep luminosity function, selection effects should shape the DM distributions of one-off and repeating FRB sources differently. This difference is not yet observed. We next show how the repeater fraction over time can help in determining the repetition rate of an intrinsic source population. We simulate this fraction for CHIME/FRB, and show that a source population comprised solely of repeating FRBs can describe CHIME/FRB observations with the use of a flat luminosity function. From the outcome of these two methods we thus conclude that all FRBs originate from a single and mostly uniform population of varying repeaters. Within this population, the luminosity function cannot be steep, and there must be minor differences in physical or behaviour parameters that correlate with repeat rate. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.02460v1-abstract-full').style.display = 'none'; document.getElementById('2012.02460v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 6 figures, submitted to 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 647, A30 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.04550">arXiv:2006.04550</a> <span> [<a href="https://arxiv.org/pdf/2006.04550">pdf</a>, <a href="https://arxiv.org/format/2006.04550">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> A Demonstration of Extremely Low Latency $纬$-ray, X-Ray & UV Follow-Up of a Millisecond Radio Transient </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tohuvavohu%2C+A">Aaron Tohuvavohu</a>, <a href="/search/astro-ph?searchtype=author&query=Law%2C+C+J">Casey J. Law</a>, <a href="/search/astro-ph?searchtype=author&query=Kennea%2C+J+A">Jamie A. Kennea</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">Elizabeth A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Aggarwal%2C+K">Kshitij Aggarwal</a>, <a href="/search/astro-ph?searchtype=author&query=Bower%2C+G">Geoffrey Bower</a>, <a href="/search/astro-ph?searchtype=author&query=Burke-Spolaor%2C+S">Sarah Burke-Spolaor</a>, <a href="/search/astro-ph?searchtype=author&query=Butler%2C+B+J">Bryan J. Butler</a>, <a href="/search/astro-ph?searchtype=author&query=Cannon%2C+J+M">John M. Cannon</a>, <a href="/search/astro-ph?searchtype=author&query=Cenko%2C+S+B">S. Bradley Cenko</a>, <a href="/search/astro-ph?searchtype=author&query=DeLaunay%2C+J">James DeLaunay</a>, <a href="/search/astro-ph?searchtype=author&query=Demorest%2C+P">Paul Demorest</a>, <a href="/search/astro-ph?searchtype=author&query=Drout%2C+M+R">Maria R. Drout</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+P+A">Philip A. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschauer%2C+A+S">Alec S. Hirschauer</a>, <a href="/search/astro-ph?searchtype=author&query=Lazio%2C+T+J+W">T. J. W. Lazio</a>, <a href="/search/astro-ph?searchtype=author&query=Linford%2C+J">Justin Linford</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+F+E">Francis E. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=McQuinn%2C+K">K. McQuinn</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">Emily Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Skillman%2C+E+D">Evan D. Skillman</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2006.04550v1-abstract-short" style="display: inline;"> We report results of a novel high-energy follow-up observation of a potential Fast Radio Burst. The radio burst was detected by VLA/realfast and followed-up by the Neil Gehrels Swift Observatory in very low latency utilizing new operational capabilities of Swift (arXiv:2005.01751), with pointed soft X-ray and UV observations beginning at T0+32 minutes, and hard X-ray/gamma-ray event data saved aro… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.04550v1-abstract-full').style.display = 'inline'; document.getElementById('2006.04550v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.04550v1-abstract-full" style="display: none;"> We report results of a novel high-energy follow-up observation of a potential Fast Radio Burst. The radio burst was detected by VLA/realfast and followed-up by the Neil Gehrels Swift Observatory in very low latency utilizing new operational capabilities of Swift (arXiv:2005.01751), with pointed soft X-ray and UV observations beginning at T0+32 minutes, and hard X-ray/gamma-ray event data saved around T0. These observations are $>10$x faster than previous X-ray/UV follow-up of any radio transient to date. No emission is seen coincident with the FRB candidate at T0, with a 0.2s fluence $5蟽$ upper limit of $1.35\times10^{-8}$ erg cm$^{-2}$ (14-195 keV) for a SGR 1935+2154-like flare, nor at T0+32 minutes down to $3蟽$ upper limits of 22.18 AB mag in UVOT u band, and $3.33\times10^{-13}$ erg cm$^{-2}$ s$^{-1}$ from 0.3-10 keV for the 2 ks observation. The candidate FRB alone is not significant enough to be considered astrophysical, so this note serves as a technical demonstration. These new Swift operational capabilities will allow future FRB detections to be followed up with Swift at even lower latencies than demonstrated here: 15-20 minutes should be regularly achievable, and 5-10 minutes occasionally achievable. We encourage FRB detecting facilities to release alerts in low latency to enable this science. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.04550v1-abstract-full').style.display = 'none'; document.getElementById('2006.04550v1-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 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Technical note and capability update for the community. We encourage low latency FRB alerts from relevant facilities to enable this science</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.01399">arXiv:2002.01399</a> <span> [<a href="https://arxiv.org/pdf/2002.01399">pdf</a>, <a href="https://arxiv.org/format/2002.01399">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/staa3009">10.1093/mnras/staa3009 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A bright, high rotation-measure FRB that skewers the M33 halo </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">Liam Connor</a>, <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+J">Joeri van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=Oostrum%2C+L+C">L. C. Oostrum</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">E. Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Maan%2C+Y">Yogesh Maan</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">E. A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Attema%2C+J+J">J. J. Attema</a>, <a href="/search/astro-ph?searchtype=author&query=Bast%2C+J+E">J. E. Bast</a>, <a href="/search/astro-ph?searchtype=author&query=Boersma%2C+O+M">O. M. Boersma</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9nes%2C+H">H. D茅nes</a>, <a href="/search/astro-ph?searchtype=author&query=Gardenier%2C+D+W">D. W. Gardenier</a>, <a href="/search/astro-ph?searchtype=author&query=Hargreaves%2C+J+E">J. E. Hargreaves</a>, <a href="/search/astro-ph?searchtype=author&query=Kooistra%2C+E">E. Kooistra</a>, <a href="/search/astro-ph?searchtype=author&query=Pastor-Marazuela%2C+I">I. Pastor-Marazuela</a>, <a href="/search/astro-ph?searchtype=author&query=Schulz%2C+R">R. Schulz</a>, <a href="/search/astro-ph?searchtype=author&query=Sclocco%2C+A">A. Sclocco</a>, <a href="/search/astro-ph?searchtype=author&query=Smits%2C+R">R. Smits</a>, <a href="/search/astro-ph?searchtype=author&query=Straal%2C+S+M">S. M. Straal</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Schuur%2C+D">D. van der Schuur</a>, <a href="/search/astro-ph?searchtype=author&query=Vohl%2C+D">Dany Vohl</a>, <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">B. Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=van+Cappellen%2C+W+A">W. A. van Cappellen</a>, <a href="/search/astro-ph?searchtype=author&query=Coolen%2C+A+H+W+M">A. H. W. M. Coolen</a>, <a href="/search/astro-ph?searchtype=author&query=Damstra%2C+S">S. Damstra</a> , et al. (15 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2002.01399v2-abstract-short" style="display: inline;"> We report the detection of a bright fast radio burst, FRB\,191108, with Apertif on the Westerbork Synthesis Radio Telescope (WSRT). The interferometer allows us to localise the FRB to a narrow $5\arcsec\times7\arcmin$ ellipse by employing both multibeam information within the Apertif phased-array feed (PAF) beam pattern, and across different tied-array beams. The resulting sight line passes close… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.01399v2-abstract-full').style.display = 'inline'; document.getElementById('2002.01399v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.01399v2-abstract-full" style="display: none;"> We report the detection of a bright fast radio burst, FRB\,191108, with Apertif on the Westerbork Synthesis Radio Telescope (WSRT). The interferometer allows us to localise the FRB to a narrow $5\arcsec\times7\arcmin$ ellipse by employing both multibeam information within the Apertif phased-array feed (PAF) beam pattern, and across different tied-array beams. The resulting sight line passes close to Local Group galaxy M33, with an impact parameter of only 18\,kpc with respect to the core. It also traverses the much larger circumgalactic medium of M31, the Andromeda Galaxy. We find that the shared plasma of the Local Group galaxies could contribute $\sim$10\% of its dispersion measure of 588\,pc\,cm$^{-3}$. FRB\,191108 has a Faraday rotation measure of +474\,$\pm\,3$\,rad\,m$^{-2}$, which is too large to be explained by either the Milky Way or the intergalactic medium. Based on the more moderate RMs of other extragalactic sources that traverse the halo of M33, we conclude that the dense magnetised plasma resides in the host galaxy. The FRB exhibits frequency structure on two scales, one that is consistent with quenched Galactic scintillation and broader spectral structure with $螖谓\approx40$\,MHz. If the latter is due to scattering in the shared M33/M31 CGM, our results constrain the Local Group plasma environment. We found no accompanying persistent radio sources in the Apertif imaging survey data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.01399v2-abstract-full').style.display = 'none'; document.getElementById('2002.01399v2-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 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2020. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.01823">arXiv:2001.01823</a> <span> [<a href="https://arxiv.org/pdf/2001.01823">pdf</a>, <a href="https://arxiv.org/ps/2001.01823">ps</a>, <a href="https://arxiv.org/format/2001.01823">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/staa039">10.1093/mnras/staa039 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The High Time Resolution Universe Pulsar Survey -- XVI. Discovery and timing of 40 pulsars from the southern Galactic plane </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+A+D">A. D. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Balakrishnan%2C+V">V. Balakrishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Bassa%2C+C+G">C. G. Bassa</a>, <a href="/search/astro-ph?searchtype=author&query=Bates%2C+S">S. Bates</a>, <a href="/search/astro-ph?searchtype=author&query=Bhandari%2C+S">S. Bhandari</a>, <a href="/search/astro-ph?searchtype=author&query=Bhat%2C+N+D+R">N. D. R. Bhat</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Burke-Spolaor%2C+S">S. Burke-Spolaor</a>, <a href="/search/astro-ph?searchtype=author&query=Flynn%2C+C+M+L">C. M. L. Flynn</a>, <a href="/search/astro-ph?searchtype=author&query=Jameson%2C+A">A. Jameson</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+S">S. Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Keith%2C+M+J">M. J. Keith</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Levin%2C+L">L. Levin</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=Ng%2C+C">C. Ng</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">E. Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</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=Stappers%2C+B+W">B. W. Stappers</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=Tiburzi%2C+C">C. Tiburzi</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2001.01823v1-abstract-short" style="display: inline;"> We present the results of processing an additional 44% of the High Time Resolution Universe South Low Latitude (HTRU-S LowLat) pulsar survey, the most sensitive blind pulsar survey of the southern Galactic plane to date. Our partially-coherent segmented acceleration search pipeline is designed to enable the discovery of pulsars in short, highly-accelerated orbits, while our 72-min integration leng… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.01823v1-abstract-full').style.display = 'inline'; document.getElementById('2001.01823v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.01823v1-abstract-full" style="display: none;"> We present the results of processing an additional 44% of the High Time Resolution Universe South Low Latitude (HTRU-S LowLat) pulsar survey, the most sensitive blind pulsar survey of the southern Galactic plane to date. Our partially-coherent segmented acceleration search pipeline is designed to enable the discovery of pulsars in short, highly-accelerated orbits, while our 72-min integration lengths will allow us to discover pulsars at the lower end of the pulsar luminosity distribution. We report the discovery of 40 pulsars, including three millisecond pulsar-white dwarf binary systems (PSRs J1537-5312, J1547-5709 and J1618-4624), a black-widow binary system (PSR J1745-23) and a candidate black-widow binary system (PSR J1727-2951), a glitching pulsar (PSR J1706-4434), an eclipsing binary pulsar with a 1.5-yr orbital period (PSR J1653-45), and a pair of long spin-period binary pulsars which display either nulling or intermittent behaviour (PSRs J1812-15 and J1831-04). We show that the total population of 100 pulsars discovered in the HTRU-S LowLat survey to date represents both an older and lower-luminosity population, and indicates that we have yet to reach the bottom of the luminosity distribution function. We present evaluations of the performance of our search technique and of the overall yield of the survey, considering the 94% of the survey which we have processed to date. We show that our pulsar yield falls below earlier predictions by approximately 25% (especially in the case of millisecond pulsars), and discuss explanations for this discrepancy as well as future adaptations in RFI mitigation and searching techniques which may address these shortfalls. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.01823v1-abstract-full').style.display = 'none'; document.getElementById('2001.01823v1-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 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 9 figures, 13 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/1912.12217">arXiv:1912.12217</a> <span> [<a href="https://arxiv.org/pdf/1912.12217">pdf</a>, <a href="https://arxiv.org/format/1912.12217">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/10.1051/0004-6361/201937422">10.1051/0004-6361/201937422 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Repeating fast radio bursts with WSRT/Apertif </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Oostrum%2C+L+C">L. C. Oostrum</a>, <a href="/search/astro-ph?searchtype=author&query=Maan%2C+Y">Y. Maan</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=Connor%2C+L">L. Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">E. Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Attema%2C+J+J">J. J. Attema</a>, <a href="/search/astro-ph?searchtype=author&query=Bast%2C+J+E">J. E. Bast</a>, <a href="/search/astro-ph?searchtype=author&query=Gardenier%2C+D+W">D. W. Gardenier</a>, <a href="/search/astro-ph?searchtype=author&query=Hargreaves%2C+J+E">J. E. Hargreaves</a>, <a href="/search/astro-ph?searchtype=author&query=Kooistra%2C+E">E. Kooistra</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Schuur%2C+D">D. van der Schuur</a>, <a href="/search/astro-ph?searchtype=author&query=Sclocco%2C+A">A. Sclocco</a>, <a href="/search/astro-ph?searchtype=author&query=Smits%2C+R">R. Smits</a>, <a href="/search/astro-ph?searchtype=author&query=Straal%2C+S+M">S. M. Straal</a>, <a href="/search/astro-ph?searchtype=author&query=ter+Veen%2C+S">S. ter Veen</a>, <a href="/search/astro-ph?searchtype=author&query=Vohl%2C+D">D. Vohl</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">E. A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">B. Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Brink%2C+R+H+v+d">R. H. van den Brink</a>, <a href="/search/astro-ph?searchtype=author&query=van+Cappellen%2C+W+A">W. A. van Cappellen</a>, <a href="/search/astro-ph?searchtype=author&query=Coolen%2C+A+H+W+M">A. H. W. M. Coolen</a>, <a href="/search/astro-ph?searchtype=author&query=Damstra%2C+S">S. Damstra</a>, <a href="/search/astro-ph?searchtype=author&query=van+Diepen%2C+G+N+J">G. N. J. van Diepen</a>, <a href="/search/astro-ph?searchtype=author&query=Frank%2C+B+S">B. S. Frank</a> , et al. (18 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1912.12217v2-abstract-short" style="display: inline;"> Repeating fast radio bursts (FRBs) present excellent opportunities to identify FRB progenitors and host environments, as well as decipher the underlying emission mechanism. Detailed studies of repeating FRBs might also hold clues to the origin of FRBs as a population. We aim to detect the first two repeating FRBs: FRB 121102 (R1) and FRB 180814.J0422+73 (R2), and characterise their repeat statisti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.12217v2-abstract-full').style.display = 'inline'; document.getElementById('1912.12217v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1912.12217v2-abstract-full" style="display: none;"> Repeating fast radio bursts (FRBs) present excellent opportunities to identify FRB progenitors and host environments, as well as decipher the underlying emission mechanism. Detailed studies of repeating FRBs might also hold clues to the origin of FRBs as a population. We aim to detect the first two repeating FRBs: FRB 121102 (R1) and FRB 180814.J0422+73 (R2), and characterise their repeat statistics. We also want to significantly improve the sky localisation of R2. We use the Westerbork Synthesis Radio Telescope to conduct extensive follow-up of these two repeating FRBs. The new phased-array feed system, Apertif, allows covering the entire sky position uncertainty of R2 with fine spatial resolution in one pointing. We characterise the energy distribution and the clustering of detected R1 bursts. We detected 30 bursts from R1. Our measurements indicate a dispersion measure of 563.5(2) pc cm$^{-3}$, suggesting a significant increase in DM over the past few years. We place an upper limit of 8% on the linear polarisation fraction of the brightest burst. We did not detect any bursts from R2. A single power-law might not fit the R1 burst energy distribution across the full energy range or widely separated detections. Our observations provide improved constraints on the clustering of R1 bursts. Our stringent upper limits on the linear polarisation fraction imply a significant depolarisation, either intrinsic to the emission mechanism or caused by the intervening medium, at 1400 MHz that is not observed at higher frequencies. The non-detection of any bursts from R2 implies either a highly clustered nature of the bursts, a steep spectral index, or a combination of both. Alternatively, R2 has turned off completely, either permanently or for an extended period of time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.12217v2-abstract-full').style.display = 'none'; document.getElementById('1912.12217v2-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 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 7 figures, submitted to 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 635, A61 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1910.08365">arXiv:1910.08365</a> <span> [<a href="https://arxiv.org/pdf/1910.08365">pdf</a>, <a href="https://arxiv.org/format/1910.08365">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/10.1051/0004-6361/201936404">10.1051/0004-6361/201936404 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Synthesizing the intrinsic FRB population using frbpoppy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gardenier%2C+D+W">D. W. Gardenier</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=Connor%2C+L">L. Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">E. Petroff</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1910.08365v1-abstract-short" style="display: inline;"> Fast Radio Bursts (FRBs) are radio transients of an unknown origin. Naturally, we are curious as to their nature. Enough FRBs have been detected for a statistical approach to parts of this challenge to be feasible. To understand the crucial link between detected FRBs and the underlying FRB source classes we perform FRB population synthesis, to determine how the underlying population behaves. The P… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.08365v1-abstract-full').style.display = 'inline'; document.getElementById('1910.08365v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.08365v1-abstract-full" style="display: none;"> Fast Radio Bursts (FRBs) are radio transients of an unknown origin. Naturally, we are curious as to their nature. Enough FRBs have been detected for a statistical approach to parts of this challenge to be feasible. To understand the crucial link between detected FRBs and the underlying FRB source classes we perform FRB population synthesis, to determine how the underlying population behaves. The Python package we developed for this synthesis, frbpoppy, is open source and freely available. Our goal is to determine the current best fit FRB population model. Our secondary aim is to provide an easy-to-use tool for simulating and understanding FRB detections. It can compare surveys, or inform us of the intrinsic FRB population. frbpoppy simulates intrinsic FRB populations and the surveys that find them, to produce virtual observed populations. These resulting populations can then be compared with real data, allowing constrains to be placed on underlying physics and selection effects. We are able to replicate real Parkes and ASKAP FRB surveys, in terms of both detection rates and distributions observed. We also show the effect of beam patterns on the observed dispersion measure (DM) distributions. We compare four types of source models. The "Complex" model, featuring a range of luminosities, pulse widths and spectral indices, reproduces current detections best. Using frbpoppy, an open-source FRB population synthesis package, we explain current FRB detections and offer a first glimpse of what the true population must be. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.08365v1-abstract-full').style.display = 'none'; document.getElementById('1910.08365v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 9 figures, 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 632, A125 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1905.03080">arXiv:1905.03080</a> <span> [<a href="https://arxiv.org/pdf/1905.03080">pdf</a>, <a href="https://arxiv.org/format/1905.03080">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/stz1352">10.1093/mnras/stz1352 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Polarization studies of Rotating Radio Transients </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Caleb%2C+M">M. Caleb</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=Keane%2C+E+F">E. F. Keane</a>, <a href="/search/astro-ph?searchtype=author&query=Jameson%2C+A">A. Jameson</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Flynn%2C+C">C. Flynn</a>, <a href="/search/astro-ph?searchtype=author&query=Ilie%2C+C+D">C. D. Ilie</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">E. Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Rogers%2C+A">A. Rogers</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">B. W. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Krishnan%2C+V+V">V. Venkatraman Krishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Weltevrede%2C+P">P. Weltevrede</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1905.03080v2-abstract-short" style="display: inline;"> We study the polarization properties of 22 known rotating radio transients (RRATs) with the 64-m Parkes radio telescope and present the Faraday rotation measures (RMs) for the 17 with linearly polarized flux exceeding the off-pulse noise by 3$蟽$. Each RM was estimated using a brute-force search over trial RMs that spanned the maximum measurable range $\pm1.18 \times 10^5 \, \mathrm{rad \, m^2}$ (i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.03080v2-abstract-full').style.display = 'inline'; document.getElementById('1905.03080v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1905.03080v2-abstract-full" style="display: none;"> We study the polarization properties of 22 known rotating radio transients (RRATs) with the 64-m Parkes radio telescope and present the Faraday rotation measures (RMs) for the 17 with linearly polarized flux exceeding the off-pulse noise by 3$蟽$. Each RM was estimated using a brute-force search over trial RMs that spanned the maximum measurable range $\pm1.18 \times 10^5 \, \mathrm{rad \, m^2}$ (in steps of 1 $\mathrm{rad \, m^2}$), followed by an iterative refinement algorithm. The measured RRAT RMs are in the range |RM| $\sim 1$ to $\sim 950$ rad m$^{-2}$ with an average linear polarization fraction of $\sim 40$ per cent. Individual single pulses are observed to be up to 100 per cent linearly polarized. The RMs of the RRATs and the corresponding inferred average magnetic fields (parallel to the line-of-sight and weighted by the free electron density) are observed to be consistent with the Galactic plane pulsar population. Faraday rotation analyses are typically performed on accumulated pulsar data, for which hundreds to thousands of pulses have been integrated, rather than on individual pulses. Therefore, we verified the iterative refinement algorithm by performing Monte Carlo simulations of artificial single pulses over a wide range of S/N and RM. At and above a S/N of 17 in linearly polarized flux, the iterative refinement recovers the simulated RM value 100 per cent of the time with a typical mean uncertainty of $\sim5$ rad m$^{-2}$. The method described and validated here has also been successfully used to determine reliable RMs of several fast radio bursts (FRBs) discovered at Parkes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.03080v2-abstract-full').style.display = 'none'; document.getElementById('1905.03080v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to MNRAS, 10 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/1904.07947">arXiv:1904.07947</a> <span> [<a href="https://arxiv.org/pdf/1904.07947">pdf</a>, <a href="https://arxiv.org/format/1904.07947">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s00159-019-0116-6">10.1007/s00159-019-0116-6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Fast Radio Bursts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">E. Petroff</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=Lorimer%2C+D+R">D. R. Lorimer</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1904.07947v1-abstract-short" style="display: inline;"> The discovery of radio pulsars over a half century ago was a seminal moment in astronomy. It demonstrated the existence of neutron stars, gave a powerful observational tool to study them, and has allowed us to probe strong gravity, dense matter, and the interstellar medium. More recently, pulsar surveys have led to the serendipitous discovery of fast radio bursts (FRBs). While FRBs appear similar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.07947v1-abstract-full').style.display = 'inline'; document.getElementById('1904.07947v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.07947v1-abstract-full" style="display: none;"> The discovery of radio pulsars over a half century ago was a seminal moment in astronomy. It demonstrated the existence of neutron stars, gave a powerful observational tool to study them, and has allowed us to probe strong gravity, dense matter, and the interstellar medium. More recently, pulsar surveys have led to the serendipitous discovery of fast radio bursts (FRBs). While FRBs appear similar to the individual pulses from pulsars, their large dispersive delays suggest that they originate from far outside the Milky Way and hence are many orders-of-magnitude more luminous. While most FRBs appear to be one-off, perhaps cataclysmic events, two sources are now known to repeat and thus clearly have a longer-lived central engine. Beyond understanding how they are created, there is also the prospect of using FRBs -- as with pulsars -- to probe the extremes of the Universe as well as the otherwise invisible intervening medium. Such studies will be aided by the high implied all-sky event rate: there is a detectable FRB roughly once every minute occurring somewhere on the sky. The fact that less than a hundred FRB sources have been discovered in the last decade is largely due to the small fields-of-view of current radio telescopes. A new generation of wide-field instruments is now coming online, however, and these will be capable of detecting multiple FRBs per day. We are thus on the brink of further breakthroughs in the short-duration radio transient phase space, which will be critical for differentiating between the many proposed theories for the origin of FRBs. In this review, we give an observational and theoretical introduction at a level that is accessible to astronomers entering the field. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.07947v1-abstract-full').style.display = 'none'; document.getElementById('1904.07947v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Invited review article for The Astronomy and Astrophysics Review</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1903.11083">arXiv:1903.11083</a> <span> [<a href="https://arxiv.org/pdf/1903.11083">pdf</a>, <a href="https://arxiv.org/format/1903.11083">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/stz3381">10.1093/mnras/stz3381 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing the extragalactic fast transient sky at minute timescales with DECam </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Andreoni%2C+I">Igor Andreoni</a>, <a href="/search/astro-ph?searchtype=author&query=Cooke%2C+J">Jeffrey Cooke</a>, <a href="/search/astro-ph?searchtype=author&query=Webb%2C+S">Sara Webb</a>, <a href="/search/astro-ph?searchtype=author&query=Rest%2C+A">Armin Rest</a>, <a href="/search/astro-ph?searchtype=author&query=Pritchard%2C+T+A">Tyler A. Pritchard</a>, <a href="/search/astro-ph?searchtype=author&query=Caleb%2C+M">Manisha Caleb</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+S">Seo-Won Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Farah%2C+W">Wael Farah</a>, <a href="/search/astro-ph?searchtype=author&query=Lien%2C+A">Amy Lien</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%B6ller%2C+A">Anais M枚ller</a>, <a href="/search/astro-ph?searchtype=author&query=Ravasio%2C+M+E">Maria Edvige Ravasio</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">Timothy M. C. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Bhandari%2C+S">Shivani Bhandari</a>, <a href="/search/astro-ph?searchtype=author&query=Cucchiara%2C+A">Antonino Cucchiara</a>, <a href="/search/astro-ph?searchtype=author&query=Flynn%2C+C+M">Christopher M. Flynn</a>, <a href="/search/astro-ph?searchtype=author&query=Jankowski%2C+F">Fabian Jankowski</a>, <a href="/search/astro-ph?searchtype=author&query=Keane%2C+E+F">Evan F. Keane</a>, <a href="/search/astro-ph?searchtype=author&query=Moriya%2C+T+J">Takashi J. Moriya</a>, <a href="/search/astro-ph?searchtype=author&query=Onken%2C+C">Christopher Onken</a>, <a href="/search/astro-ph?searchtype=author&query=Parthasarathy%2C+A">Aditya Parthasarathy</a>, <a href="/search/astro-ph?searchtype=author&query=Price%2C+D+C">Daniel C. Price</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">Emily Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Ryder%2C+S">Stuart Ryder</a>, <a href="/search/astro-ph?searchtype=author&query=Vohl%2C+D">Dany Vohl</a>, <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+C">Christian Wolf</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="1903.11083v2-abstract-short" style="display: inline;"> Searches for optical transients are usually performed with a cadence of days to weeks, optimised for supernova discovery. The optical fast transient sky is still largely unexplored, with only a few surveys to date having placed meaningful constraints on the detection of extragalactic transients evolving at sub-hour timescales. Here, we present the results of deep searches for dim, minute-timescale… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.11083v2-abstract-full').style.display = 'inline'; document.getElementById('1903.11083v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.11083v2-abstract-full" style="display: none;"> Searches for optical transients are usually performed with a cadence of days to weeks, optimised for supernova discovery. The optical fast transient sky is still largely unexplored, with only a few surveys to date having placed meaningful constraints on the detection of extragalactic transients evolving at sub-hour timescales. Here, we present the results of deep searches for dim, minute-timescale extragalactic fast transients using the Dark Energy Camera, a core facility of our all-wavelength and all-messenger Deeper, Wider, Faster programme. We used continuous 20s exposures to systematically probe timescales down to 1.17 minutes at magnitude limits $g > 23$ (AB), detecting hundreds of transient and variable sources. Nine candidates passed our strict criteria on duration and non-stellarity, all of which could be classified as flare stars based on deep multi-band imaging. Searches for fast radio burst and gamma-ray counterparts during simultaneous multi-facility observations yielded no counterparts to the optical transients. Also, no long-term variability was detected with pre-imaging and follow-up observations using the SkyMapper optical telescope. We place upper limits for minute-timescale fast optical transient rates for a range of depths and timescales. Finally, we demonstrate that optical $g$-band light curve behaviour alone cannot discriminate between confirmed extragalactic fast transients such as prompt GRB flashes and Galactic stellar flares. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.11083v2-abstract-full').style.display = 'none'; document.getElementById('1903.11083v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Monthly Notices of the Royal Astronomical Society (2020), Volume 491, Issue 4, p.5852-5866 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1902.06731">arXiv:1902.06731</a> <span> [<a href="https://arxiv.org/pdf/1902.06731">pdf</a>, <a href="https://arxiv.org/format/1902.06731">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ab1aad">10.3847/2041-8213/ab1aad <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Resolving the decades-long transient FIRST J141918.9+394036: an orphan long gamma-ray burst or a young magnetar nebula? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marcote%2C+B">B. Marcote</a>, <a href="/search/astro-ph?searchtype=author&query=Nimmo%2C+K">K. Nimmo</a>, <a href="/search/astro-ph?searchtype=author&query=Salafia%2C+O+S">O. S. Salafia</a>, <a href="/search/astro-ph?searchtype=author&query=Paragi%2C+Z">Z. Paragi</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=Petroff%2C+E">E. Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Karuppusamy%2C+R">R. Karuppusamy</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="1902.06731v2-abstract-short" style="display: inline;"> Ofek (2017) identified FIRST J141918.9+394036 (hereafter FIRST J1419+3940) as a radio source sharing similar properties and host galaxy type to the compact, persistent radio source associated with the first known repeating fast radio burst, FRB 121102. Law et al. (2018) showed that FIRST J1419+3940 is a transient source decaying in brightness over the last few decades. One possible interpretation… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.06731v2-abstract-full').style.display = 'inline'; document.getElementById('1902.06731v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1902.06731v2-abstract-full" style="display: none;"> Ofek (2017) identified FIRST J141918.9+394036 (hereafter FIRST J1419+3940) as a radio source sharing similar properties and host galaxy type to the compact, persistent radio source associated with the first known repeating fast radio burst, FRB 121102. Law et al. (2018) showed that FIRST J1419+3940 is a transient source decaying in brightness over the last few decades. One possible interpretation is that FIRST J1419+3940 is a nearby analogue to FRB 121102 and that the radio emission represents a young magnetar nebula (as several scenarios assume for FRB 121102). Another interpretation is that FIRST J1419+3940 is the afterglow of an `orphan' long gamma-ray burst (GRB). The environment is similar to where most such events are produced. To distinguish between these hypotheses, we conducted radio observations using the European VLBI Network at 1.6 GHz to spatially resolve the emission and to search for millisecond-duration radio bursts. We detect FIRST J1419+3940 as a compact radio source with a flux density of $620 \pm 20\ \mathrm{渭Jy}$ (on 2018 September 18) and a source size of $3.9 \pm 0.7\ \mathrm{mas}$ (i.e. $1.6 \pm 0.3\ \mathrm{pc}$ given the angular diameter distance of $83\ \mathrm{Mpc}$). These results confirm that the radio emission is non-thermal and imply an average expansion velocity of $(0.10 \pm 0.02)c$. Contemporaneous high-time-resolution observations using the 100-m Effelsberg telescope detected no millisecond-duration bursts of astrophysical origin. The source properties and lack of short-duration bursts are consistent with a GRB jet expansion, whereas they disfavor a magnetar birth nebula. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.06731v2-abstract-full').style.display = 'none'; document.getElementById('1902.06731v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 February, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 4 figures, 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/1902.05571">arXiv:1902.05571</a> <span> [<a href="https://arxiv.org/pdf/1902.05571">pdf</a>, <a href="https://arxiv.org/ps/1902.05571">ps</a>, <a href="https://arxiv.org/format/1902.05571">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/stz401">10.1093/mnras/stz401 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The High Time Resolution Universe Pulsar Survey -- XV: completion of the intermediate latitude survey with the discovery and timing of 25 further pulsars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B">B. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Bates%2C+S">S. Bates</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=Burke-Spolaor%2C+S">S. Burke-Spolaor</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+A+D">A. D. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Eatough%2C+R+P">R. P. Eatough</a>, <a href="/search/astro-ph?searchtype=author&query=Flynn%2C+C+M+L">C. M. L. Flynn</a>, <a href="/search/astro-ph?searchtype=author&query=Jameson%2C+A">A. Jameson</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+S">S. Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Keith%2C+M+J">M. J. Keith</a>, <a href="/search/astro-ph?searchtype=author&query=Keane%2C+E+F">E. F. Keane</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Levin%2C+L">L. Levin</a>, <a href="/search/astro-ph?searchtype=author&query=Ng%2C+C">C. Ng</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">E. Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</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=Tiburzi%2C+C">C. Tiburzi</a>, <a href="/search/astro-ph?searchtype=author&query=Bondonneau%2C+L">L. Bondonneau</a>, <a href="/search/astro-ph?searchtype=author&query=Lyne%2C+A+G">A. G. Lyne</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="1902.05571v1-abstract-short" style="display: inline;"> We report on the latest six pulsars discovered through our standard pipeline in the intermediate-latitude region (|b| < 15 deg) of the Parkes High Time Resolution Universe Survey (HTRU). We also present timing solutions for the new discoveries and for 19 further pulsars for which only discovery parameters were previously published. Highlights of the presented sample include the isolated millisecon… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.05571v1-abstract-full').style.display = 'inline'; document.getElementById('1902.05571v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1902.05571v1-abstract-full" style="display: none;"> We report on the latest six pulsars discovered through our standard pipeline in the intermediate-latitude region (|b| < 15 deg) of the Parkes High Time Resolution Universe Survey (HTRU). We also present timing solutions for the new discoveries and for 19 further pulsars for which only discovery parameters were previously published. Highlights of the presented sample include the isolated millisecond pulsar J1826-2415, the long-period binary pulsar J1837-0822 in a mildly eccentric 98-day orbit with a > 0.27 M_sun companion, and the nulling pulsar J1638-4233, detected only 10% of the time. Other interesting objects are PSR J1757-1500, exhibiting sporadic mode changes, and PSR J1635-2616 showing one glitch over 6 years. The new discoveries bring the total count of HTRU intermediate-latitude pulsars to 113, 25% of which are recycled pulsars. This is the higest ratio of recycled over ordinary pulsars discoveries of all recent pulsar surveys in this region of the sky. Among HTRU recycled pulsars, four are isolated objects. Comparing the characteristics of Galactic fully-recycled isolated MSPs with those of eclipsing binaries ('spiders'), from which the former are believed to have formed, we highlight a discrepancy in their spatial distribution. This may reflect a difference in the natal kick, hence, possibly, a different formation path. On the other hand, however, isolated fully-recycled MSPs spin periods are, on average, longer than those of spiders, in line with what one would expect, from simple magnetic-dipole spin-down, if the former were indeed evolved from the latter. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.05571v1-abstract-full').style.display = 'none'; document.getElementById('1902.05571v1-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, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS; 12 pages, 9 figures, 7 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/1901.07412">arXiv:1901.07412</a> <span> [<a href="https://arxiv.org/pdf/1901.07412">pdf</a>, <a href="https://arxiv.org/format/1901.07412">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/stz958">10.1093/mnras/stz958 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Fast Radio Burst with frequency-dependent polarization detected during Breakthrough Listen observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Price%2C+D+C">D. C. Price</a>, <a href="/search/astro-ph?searchtype=author&query=Foster%2C+G">G. Foster</a>, <a href="/search/astro-ph?searchtype=author&query=Geyer%2C+M">M. Geyer</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=Gajjar%2C+V">V. Gajjar</a>, <a href="/search/astro-ph?searchtype=author&query=Hellbourg%2C+G">G. Hellbourg</a>, <a href="/search/astro-ph?searchtype=author&query=Karastergiou%2C+A">A. Karastergiou</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=Siemion%2C+A+P+V">A. P. V. Siemion</a>, <a href="/search/astro-ph?searchtype=author&query=Arcavi%2C+I">I. Arcavi</a>, <a href="/search/astro-ph?searchtype=author&query=Bhat%2C+R">R. Bhat</a>, <a href="/search/astro-ph?searchtype=author&query=Caleb%2C+M">M. Caleb</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+S">S-W. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Croft%2C+S">S. Croft</a>, <a href="/search/astro-ph?searchtype=author&query=DeBoer%2C+D">D. DeBoer</a>, <a href="/search/astro-ph?searchtype=author&query=de+Pater%2C+I">I. de Pater</a>, <a href="/search/astro-ph?searchtype=author&query=Drew%2C+J">J. Drew</a>, <a href="/search/astro-ph?searchtype=author&query=Enriquez%2C+J+E">J. E. Enriquez</a>, <a href="/search/astro-ph?searchtype=author&query=Farah%2C+W">W. Farah</a>, <a href="/search/astro-ph?searchtype=author&query=Gizani%2C+N">N. Gizani</a>, <a href="/search/astro-ph?searchtype=author&query=Green%2C+J+A">J. A. Green</a>, <a href="/search/astro-ph?searchtype=author&query=Isaacson%2C+H">H. Isaacson</a>, <a href="/search/astro-ph?searchtype=author&query=Hickish%2C+J">J. Hickish</a>, <a href="/search/astro-ph?searchtype=author&query=Jameson%2C+A">A. Jameson</a>, <a href="/search/astro-ph?searchtype=author&query=Lebofsky%2C+M">M. Lebofsky</a> , et al. (8 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1901.07412v1-abstract-short" style="display: inline;"> Here, we report on the detection and verification of Fast Radio Burst FRB 180301, which occurred on UTC 2018 March 1 during the Breakthrough Listen observations with the Parkes telescope. Full-polarization voltage data of the detection were captured--a first for non-repeating FRBs--allowing for coherent de-dispersion and additional verification tests. The coherently de-dispersed dynamic spectrum o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.07412v1-abstract-full').style.display = 'inline'; document.getElementById('1901.07412v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.07412v1-abstract-full" style="display: none;"> Here, we report on the detection and verification of Fast Radio Burst FRB 180301, which occurred on UTC 2018 March 1 during the Breakthrough Listen observations with the Parkes telescope. Full-polarization voltage data of the detection were captured--a first for non-repeating FRBs--allowing for coherent de-dispersion and additional verification tests. The coherently de-dispersed dynamic spectrum of FRB 180301 shows complex, polarized frequency structure over a small fractional bandwidth. As FRB 180301 was detected close to the geosynchronous satellite band during a time of known 1-2 GHz satellite transmissions, we consider whether the burst was due to radio interference emitted or reflected from an orbiting object. Based on the preponderance of our verification tests, we find that FRB 180301 is likely of astrophysical origin, but caution that anthropogenic sources cannot conclusively be ruled out. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.07412v1-abstract-full').style.display = 'none'; document.getElementById('1901.07412v1-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 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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/1811.10748">arXiv:1811.10748</a> <span> [<a href="https://arxiv.org/pdf/1811.10748">pdf</a>, <a href="https://arxiv.org/format/1811.10748">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ab13ae">10.3847/2041-8213/ab13ae <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> FRB 121102 Bursts Show Complex Time-Frequency Structure </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Spitler%2C+L+G">L. G. Spitler</a>, <a href="/search/astro-ph?searchtype=author&query=Seymour%2C+A+D">A. D. Seymour</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=Michilli%2C+D">D. Michilli</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=Gourdji%2C+K">K. Gourdji</a>, <a href="/search/astro-ph?searchtype=author&query=Archibald%2C+A+M">A. M. Archibald</a>, <a href="/search/astro-ph?searchtype=author&query=Bassa%2C+C+G">C. G. Bassa</a>, <a href="/search/astro-ph?searchtype=author&query=Bower%2C+G+C">G. C. Bower</a>, <a href="/search/astro-ph?searchtype=author&query=Chatterjee%2C+S">S. Chatterjee</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">L. Connor</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=Gajjar%2C+V">V. Gajjar</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=Keimpema%2C+A">A. Keimpema</a>, <a href="/search/astro-ph?searchtype=author&query=Law%2C+C+J">C. J. Law</a>, <a href="/search/astro-ph?searchtype=author&query=Marcote%2C+B">B. Marcote</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=Paragi%2C+Z">Z. Paragi</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">E. Petroff</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=Scholz%2C+P">P. Scholz</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">B. W. Stappers</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1811.10748v1-abstract-short" style="display: inline;"> FRB 121102 is the only known repeating fast radio burst source. Here we analyze a wide-frequency-range (1-8 GHz) sample of high-signal-to-noise, coherently dedispersed bursts detected using the Arecibo and Green Bank telescopes. These bursts reveal complex time-frequency structures that include sub-bursts with finite bandwidths. The frequency-dependent burst structure complicates the determination… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.10748v1-abstract-full').style.display = 'inline'; document.getElementById('1811.10748v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1811.10748v1-abstract-full" style="display: none;"> FRB 121102 is the only known repeating fast radio burst source. Here we analyze a wide-frequency-range (1-8 GHz) sample of high-signal-to-noise, coherently dedispersed bursts detected using the Arecibo and Green Bank telescopes. These bursts reveal complex time-frequency structures that include sub-bursts with finite bandwidths. The frequency-dependent burst structure complicates the determination of a dispersion measure (DM); we argue that it is appropriate to use a DM metric that maximizes frequency-averaged pulse structure, as opposed to peak signal-to-noise, and find DM = 560.57 +/- 0.07 pc/cc at MJD 57644. After correcting for dispersive delay, we find that the sub-bursts have characteristic frequencies that typically drift lower at later times in the total burst envelope. In the 1.1-1.7 GHz band, the ~ 0.5-1-ms sub-bursts have typical bandwidths ranging from 100-400 MHz, and a characteristic drift rate of ~ 200 MHz/ms towards lower frequencies. At higher radio frequencies, the sub-burst bandwidths and drift rate are larger, on average. While these features could be intrinsic to the burst emission mechanism, they could also be imparted by propagation effects in the medium local to the source. Comparison of the burst DMs with previous values in the literature suggests an increase of Delta(DM) ~ 1-3 pc/cc in 4 years, though this could be a stochastic variation as opposed to a secular trend. This implies changes in the local medium or an additional source of frequency-dependent delay. Overall, the results are consistent with previously proposed scenarios in which FRB 121102 is embedded in a dense nebula. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.10748v1-abstract-full').style.display = 'none'; document.getElementById('1811.10748v1-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 November, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to ApJ; comments welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1811.04929">arXiv:1811.04929</a> <span> [<a href="https://arxiv.org/pdf/1811.04929">pdf</a>, <a href="https://arxiv.org/format/1811.04929">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/sty3328">10.1093/mnras/sty3328 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The High Time Resolution Universe survey XIV: Discovery of 23 pulsars through GPU-accelerated reprocessing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Morello%2C+V">V. Morello</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=Cooper%2C+S">S. Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Bates%2C+S">S. Bates</a>, <a href="/search/astro-ph?searchtype=author&query=Bhat%2C+N+D+R">N. D. R. Bhat</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Burke-Spolaor%2C+S">S. Burke-Spolaor</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+A+D">A. D. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Eatough%2C+R+P">R. P. Eatough</a>, <a href="/search/astro-ph?searchtype=author&query=Flynn%2C+C+M+L">C. M. L. Flynn</a>, <a href="/search/astro-ph?searchtype=author&query=Jameson%2C+A">A. Jameson</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+S">S. Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Keith%2C+M+J">M. J. Keith</a>, <a href="/search/astro-ph?searchtype=author&query=Keane%2C+E+F">E. F. Keane</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Levin%2C+L">L. Levin</a>, <a href="/search/astro-ph?searchtype=author&query=Ng%2C+C">C. Ng</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">E. Petroff</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=van+Straten%2C+W">W. van Straten</a>, <a href="/search/astro-ph?searchtype=author&query=Tiburzi%2C+C">C. Tiburzi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1811.04929v1-abstract-short" style="display: inline;"> We have performed a new search for radio pulsars in archival data of the intermediate and high Galactic latitude parts of the Southern High Time Resolution Universe pulsar survey. This is the first time the entire dataset has been searched for binary pulsars, an achievement enabled by GPU-accelerated dedispersion and periodicity search codes nearly 50 times faster than the previously used pipeline… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.04929v1-abstract-full').style.display = 'inline'; document.getElementById('1811.04929v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1811.04929v1-abstract-full" style="display: none;"> We have performed a new search for radio pulsars in archival data of the intermediate and high Galactic latitude parts of the Southern High Time Resolution Universe pulsar survey. This is the first time the entire dataset has been searched for binary pulsars, an achievement enabled by GPU-accelerated dedispersion and periodicity search codes nearly 50 times faster than the previously used pipeline. Candidate selection was handled entirely by a Machine Learning algorithm, allowing for the assessment of 17.6 million candidates in a few person-days. We have also introduced an outlier detection algorithm for efficient radio-frequency interference (RFI) mitigation on folded data, a new approach that enabled the discovery of pulsars previously masked by RFI. We discuss implications for future searches, particularly the importance of expanding work on RFI mitigation to improve survey completeness. In total we discovered 23 previously unknown sources, including 6 millisecond pulsars and at least 4 pulsars in binary systems. We also found an elusive but credible redback candidate that we have yet to confirm. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.04929v1-abstract-full').style.display = 'none'; document.getElementById('1811.04929v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 November, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS, 14 pages, 5 figures, 10 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/1810.10773">arXiv:1810.10773</a> <span> [<a href="https://arxiv.org/pdf/1810.10773">pdf</a>, <a href="https://arxiv.org/format/1810.10773">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/sty2909">10.1093/mnras/sty2909 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A fast radio burst with a low dispersion measure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">E. Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Oostrum%2C+L+C">L. C. Oostrum</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B+W">B. W. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Bates%2C+S">S. Bates</a>, <a href="/search/astro-ph?searchtype=author&query=Bhandari%2C+S">S. Bhandari</a>, <a href="/search/astro-ph?searchtype=author&query=Bhat%2C+N+D+R">N. D. R. Bhat</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Burke-Spolaor%2C+S">S. Burke-Spolaor</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+A+D">A. D. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Champion%2C+D+J">D. J. Champion</a>, <a href="/search/astro-ph?searchtype=author&query=Eatough%2C+R+P">R. P. Eatough</a>, <a href="/search/astro-ph?searchtype=author&query=Flynn%2C+C+M+L">C. M. L. Flynn</a>, <a href="/search/astro-ph?searchtype=author&query=Jameson%2C+A">A. Jameson</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+S">S. Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Keane%2C+E+F">E. F. Keane</a>, <a href="/search/astro-ph?searchtype=author&query=Keith%2C+M+J">M. J. Keith</a>, <a href="/search/astro-ph?searchtype=author&query=Levin%2C+L">L. Levin</a>, <a href="/search/astro-ph?searchtype=author&query=Morello%2C+V">V. Morello</a>, <a href="/search/astro-ph?searchtype=author&query=Ng%2C+C">C. Ng</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Ravi%2C+V">V. Ravi</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=Thornton%2C+D">D. Thornton</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1810.10773v1-abstract-short" style="display: inline;"> Fast radio bursts (FRBs) are millisecond pulses of radio emission of seemingly extragalactic origin. More than 50 FRBs have now been detected, with only one seen to repeat. Here we present a new FRB discovery, FRB 110214, which was detected in the high latitude portion of the High Time Resolution Universe South survey at the Parkes telescope. FRB 110214 has one of the lowest dispersion measures of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.10773v1-abstract-full').style.display = 'inline'; document.getElementById('1810.10773v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1810.10773v1-abstract-full" style="display: none;"> Fast radio bursts (FRBs) are millisecond pulses of radio emission of seemingly extragalactic origin. More than 50 FRBs have now been detected, with only one seen to repeat. Here we present a new FRB discovery, FRB 110214, which was detected in the high latitude portion of the High Time Resolution Universe South survey at the Parkes telescope. FRB 110214 has one of the lowest dispersion measures of any known FRB (DM = 168.9$\pm$0.5 pc cm$^{-3}$), and was detected in two beams of the Parkes multi-beam receiver. A triangulation of the burst origin on the sky identified three possible regions in the beam pattern where it may have originated, all in sidelobes of the primary detection beam. Depending on the true location of the burst the intrinsic fluence is estimated to fall in the range of 50 -- 2000 Jy ms, making FRB 110214 one of the highest-fluence FRBs detected with the Parkes telescope. No repeating pulses were seen in almost 100 hours of follow-up observations with the Parkes telescope down to a limiting fluence of 0.3 Jy ms for a 2-ms pulse. Similar low-DM, ultra-bright FRBs may be detected in telescope sidelobes in the future, making careful modeling of multi-beam instrument beam patterns of utmost importance for upcoming FRB surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.10773v1-abstract-full').style.display = 'none'; document.getElementById('1810.10773v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 October, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 3 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/1808.03400">arXiv:1808.03400</a> <span> [<a href="https://arxiv.org/pdf/1808.03400">pdf</a>, <a href="https://arxiv.org/ps/1808.03400">ps</a>, <a href="https://arxiv.org/format/1808.03400">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/pasj/psy101">10.1093/pasj/psy101 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Optical follow-up observation of Fast Radio Burst 151230 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Tominaga%2C+N">Nozomu Tominaga</a>, <a href="/search/astro-ph?searchtype=author&query=Niino%2C+Y">Yuu Niino</a>, <a href="/search/astro-ph?searchtype=author&query=Totani%2C+T">Tomonori Totani</a>, <a href="/search/astro-ph?searchtype=author&query=Yasuda%2C+N">Naoki Yasuda</a>, <a href="/search/astro-ph?searchtype=author&query=Furusawa%2C+H">Hisanori Furusawa</a>, <a href="/search/astro-ph?searchtype=author&query=Tanaka%2C+M">Masayuki Tanaka</a>, <a href="/search/astro-ph?searchtype=author&query=Bhandari%2C+S">Shivani Bhandari</a>, <a href="/search/astro-ph?searchtype=author&query=Dodson%2C+R">Richard Dodson</a>, <a href="/search/astro-ph?searchtype=author&query=Keane%2C+E">Evan Keane</a>, <a href="/search/astro-ph?searchtype=author&query=Morokuma%2C+T">Tomoki Morokuma</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">Emily Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">Andrea Possenti</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1808.03400v1-abstract-short" style="display: inline;"> The origin of fast radio bursts (FRBs), bright millisecond radio transients, is still somewhat of a mystery. Several theoretical models expect that the FRB accompanies an optical afterglow (e.g., Totani 2013; Kashiyama et al. 2013). In order to investigate the origin of FRBs, we perform $gri$-band follow-up observations of FRB~151230 (estimated $z \lesssim 0.8$) with Subaru/Hyper Suprime-Cam at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.03400v1-abstract-full').style.display = 'inline'; document.getElementById('1808.03400v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.03400v1-abstract-full" style="display: none;"> The origin of fast radio bursts (FRBs), bright millisecond radio transients, is still somewhat of a mystery. Several theoretical models expect that the FRB accompanies an optical afterglow (e.g., Totani 2013; Kashiyama et al. 2013). In order to investigate the origin of FRBs, we perform $gri$-band follow-up observations of FRB~151230 (estimated $z \lesssim 0.8$) with Subaru/Hyper Suprime-Cam at $8$, $11$, and $14$~days after discovery. The follow-up observation reaches a $50\%$ completeness magnitude of $26.5$~mag for point sources, which is the deepest optical follow-up of FRBs to date. We find $13$ counterpart candidates with variabilities during the observation. We investigate their properties with multicolor and multi-wavelength observations and archival catalogs. Two candidates are excluded by the non-detection of FRB~151230 in the other radio feed horns that operated simultaneously to the detection, as well as the inconsistency between the photometric redshift and that derived from the dispersion measure of FRB~151230. Eight further candidates are consistent with optical variability seen in AGNs. Two more candidates are well fitted with transient templates (Type IIn supernovae), and the final candidate is poorly fitted with all of our transient templates and is located off-center of an extended source. It can only be reproduced with rapid transients with a faint peak and rapid decline and the probability of chance coincidence is $\sim3.6\%$. We also find that none of our candidates are consistent with Type Ia supernovae, which rules out the association of Type Ia supernovae to FRB~151230 at $z\leq0.6$ and limits the dispersion measure of the host galaxy to $\lesssim300$~pc~cm$^{-3}$ in a Type Ia supernova scenario. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.03400v1-abstract-full').style.display = 'none'; document.getElementById('1808.03400v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 11 figures. Accepted for publication in PASJ (Publications of the Astronomical Society of Japan)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1804.09178">arXiv:1804.09178</a> <span> [<a href="https://arxiv.org/pdf/1804.09178">pdf</a>, <a href="https://arxiv.org/format/1804.09178">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/sty1137">10.1093/mnras/sty1137 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The SUrvey for Pulsars and Extragalactic Radio Bursts III: Polarization properties of FRBs 160102 & 151230 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Caleb%2C+M">M. Caleb</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=van+Straten%2C+W">W. van Straten</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Macquart%2C+J+P">J. P. Macquart</a>, <a href="/search/astro-ph?searchtype=author&query=Bailes%2C+M">M. Bailes</a>, <a href="/search/astro-ph?searchtype=author&query=Barr%2C+E+D">E. D. Barr</a>, <a href="/search/astro-ph?searchtype=author&query=Bhat%2C+N+D+R">N. D. R. Bhat</a>, <a href="/search/astro-ph?searchtype=author&query=Bhandari%2C+S">S. Bhandari</a>, <a href="/search/astro-ph?searchtype=author&query=Burgay%2C+M">M. Burgay</a>, <a href="/search/astro-ph?searchtype=author&query=Farah%2C+W">W. Farah</a>, <a href="/search/astro-ph?searchtype=author&query=Jameson%2C+A">A. Jameson</a>, <a href="/search/astro-ph?searchtype=author&query=Jankowski%2C+F">F. Jankowski</a>, <a href="/search/astro-ph?searchtype=author&query=Johnston%2C+S">S. Johnston</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">E. Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Possenti%2C+A">A. Possenti</a>, <a href="/search/astro-ph?searchtype=author&query=Stappers%2C+B">B. Stappers</a>, <a href="/search/astro-ph?searchtype=author&query=Tiburzi%2C+C">C. Tiburzi</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="1804.09178v2-abstract-short" style="display: inline;"> We report on the polarization properties of two fast radio bursts (FRBs): 151230 and 160102 discovered in the SUrvey for Pulsars and Extragalactic Radio Bursts (SUPERB) at the Parkes radio telescope. FRB 151230 is observed to be 6 $\pm$ 11% circularly polarized and 35 $\pm$ 13 % linearly polarized with a rotation measure (RM) consistent with zero. Conversely, FRB 160102 is observed to have a circu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.09178v2-abstract-full').style.display = 'inline'; document.getElementById('1804.09178v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1804.09178v2-abstract-full" style="display: none;"> We report on the polarization properties of two fast radio bursts (FRBs): 151230 and 160102 discovered in the SUrvey for Pulsars and Extragalactic Radio Bursts (SUPERB) at the Parkes radio telescope. FRB 151230 is observed to be 6 $\pm$ 11% circularly polarized and 35 $\pm$ 13 % linearly polarized with a rotation measure (RM) consistent with zero. Conversely, FRB 160102 is observed to have a circular polarization fraction of 30 $\pm$ 11 %, linear polarization fraction of 84 $\pm$ 15 % for RM = -221(6) rad m$^{-2}$ and the highest measured DM (2596.1 $\pm$ 0.3 pc cm$^{-3}$) for an FRB to date. We examine possible progenitor models for FRB 160102 in extragalactic, non-cosmological and cosmological scenarios. After accounting for the Galactic foreground contribution, we estimate the intrinsic RM to be -256(9) rad m$^{-2}$ in the low-redshift case and $\sim 2.4 \times 10^{2}$ rad m$^{-2}$ in the high-redshift case. We assess the relative likeliness of these scenarios and how each can be tested. We also place constraints on the scattering measure and study the impact of scattering on the signal's polarization position angle. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.09178v2-abstract-full').style.display = 'none'; document.getElementById('1804.09178v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 7 figures, accepted for publication in MNRAS</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" 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