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start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.08630">arXiv:2411.08630</a> <span> [<a href="https://arxiv.org/pdf/2411.08630">pdf</a>, <a href="https://arxiv.org/format/2411.08630">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41586-024-07879-y">10.1038/s41586-024-07879-y <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Black hole jets on the scale of the Cosmic Web </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Oei%2C+M+S+S+L">Martijn S. S. L. Oei</a>, <a href="/search/?searchtype=author&query=Hardcastle%2C+M+J">Martin J. Hardcastle</a>, <a href="/search/?searchtype=author&query=Timmerman%2C+R">Roland Timmerman</a>, <a href="/search/?searchtype=author&query=Gast%2C+A+R+D+J+G+I+B">Aivin R. D. J. G. I. B. Gast</a>, <a href="/search/?searchtype=author&query=Botteon%2C+A">Andrea Botteon</a>, <a href="/search/?searchtype=author&query=Rodriguez%2C+A+C">Antonio C. Rodriguez</a>, <a href="/search/?searchtype=author&query=Stern%2C+D">Daniel Stern</a>, <a href="/search/?searchtype=author&query=Rivera%2C+G+C">Gabriela Calistro Rivera</a>, <a href="/search/?searchtype=author&query=van+Weeren%2C+R+J">Reinout J. van Weeren</a>, <a href="/search/?searchtype=author&query=R%C3%B6ttgering%2C+H+J+A">Huub J. A. R枚ttgering</a>, <a href="/search/?searchtype=author&query=Intema%2C+H+T">Huib T. Intema</a>, <a href="/search/?searchtype=author&query=de+Gasperin%2C+F">Francesco de Gasperin</a>, <a href="/search/?searchtype=author&query=Djorgovski%2C+S+G">S. G. Djorgovski</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.08630v1-abstract-short" style="display: inline;"> Jets launched by supermassive black holes transport relativistic leptons, magnetic fields, and atomic nuclei from the centres of galaxies to their outskirts and beyond. These outflows embody the most energetic pathway by which galaxies respond to their Cosmic Web environment. Studying black hole feedback is an astrophysical frontier, providing insights on star formation, galaxy cluster stability,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.08630v1-abstract-full').style.display = 'inline'; document.getElementById('2411.08630v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.08630v1-abstract-full" style="display: none;"> Jets launched by supermassive black holes transport relativistic leptons, magnetic fields, and atomic nuclei from the centres of galaxies to their outskirts and beyond. These outflows embody the most energetic pathway by which galaxies respond to their Cosmic Web environment. Studying black hole feedback is an astrophysical frontier, providing insights on star formation, galaxy cluster stability, and the origin of cosmic rays, magnetism, and heavy elements throughout the Universe. This feedback's cosmological importance is ultimately bounded by the reach of black hole jets, and could be sweeping if jets travel far at early epochs. Here we present the joint LOFAR-uGMRT-Keck discovery of a black hole jet pair extending over $7$ megaparsecs -- the largest galaxy-made structure ever found. The outflow, seen $7.5$ gigayears into the past, spans two-thirds of a typical cosmic void radius, thus penetrating voids at ${\sim}95\%$ probability. This system demonstrates that jets can avoid destruction by magnetohydrodynamical instabilities over cosmological distances, even at epochs when the Universe was 15 to 7 times denser than it is today. Whereas previous record-breaking outflows were powered by radiatively inefficient active galactic nuclei, this outflow is powered by a radiatively efficient active galactic nucleus, a type common at early epochs. If, as implied, a population of early void-penetrating outflows existed, then black hole jets could have overwritten the fields from primordial magnetogenesis. This outflow shows that energy transport from supermassive black holes operates on scales of the Cosmic Web and raises the possibility that cosmic rays and magnetism in the intergalactic medium have a non-local, cross-void origin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.08630v1-abstract-full').style.display = 'none'; document.getElementById('2411.08630v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">30 pages, 10 figures, 1 table, published in Nature. This arXiv version pre-dates the peer review process</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature, 2024, Volume 633, Issue 8030, Pages 537--541 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.17776">arXiv:2404.17776</a> <span> [<a href="https://arxiv.org/pdf/2404.17776">pdf</a>, <a href="https://arxiv.org/format/2404.17776">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202347115">10.1051/0004-6361/202347115 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Luminous giants populate the dense Cosmic Web: The radio luminosity-environmental density relation for radio galaxies in action </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Oei%2C+M+S+S+L">Martijn S. S. L. Oei</a>, <a href="/search/?searchtype=author&query=van+Weeren%2C+R+J">Reinout J. van Weeren</a>, <a href="/search/?searchtype=author&query=Hardcastle%2C+M+J">Martin J. Hardcastle</a>, <a href="/search/?searchtype=author&query=Gast%2C+A+R+D+J+G+I+B">Aivin R. D. J. G. I. B. Gast</a>, <a href="/search/?searchtype=author&query=Leclercq%2C+F">Florent Leclercq</a>, <a href="/search/?searchtype=author&query=R%C3%B6ttgering%2C+H+J+A">Huub J. A. R枚ttgering</a>, <a href="/search/?searchtype=author&query=Dabhade%2C+P">Pratik Dabhade</a>, <a href="/search/?searchtype=author&query=Shimwell%2C+T+W">Tim W. Shimwell</a>, <a href="/search/?searchtype=author&query=Botteon%2C+A">Andrea Botteon</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="2404.17776v1-abstract-short" style="display: inline;"> Giant radio galaxies (GRGs, giant RGs, or giants) are megaparsec-scale, jet-driven outflows from accretion disks of supermassive black holes, and represent the most extreme pathway by which galaxies can impact the Cosmic Web around them. A long-standing but unresolved question is why giants are so much larger than other radio galaxies. It has been proposed that, in addition to having higher jet po… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.17776v1-abstract-full').style.display = 'inline'; document.getElementById('2404.17776v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.17776v1-abstract-full" style="display: none;"> Giant radio galaxies (GRGs, giant RGs, or giants) are megaparsec-scale, jet-driven outflows from accretion disks of supermassive black holes, and represent the most extreme pathway by which galaxies can impact the Cosmic Web around them. A long-standing but unresolved question is why giants are so much larger than other radio galaxies. It has been proposed that, in addition to having higher jet powers than most RGs, giants might live in especially low-density Cosmic Web environments. In this work, we aim to test this hypothesis by pinpointing Local Universe giants and other RGs in physically principled, Bayesian large-scale structure reconstructions. More specifically, we localised a LOFAR Two-metre Sky Survey (LoTSS) DR2-dominated sample of luminous ($l_谓(谓= 150\ \mathrm{MHz}) \geq 10^{24}\ \mathrm{W\ Hz^{-1}}$) giants and a control sample of LoTSS DR1 RGs, both with spectroscopic redshifts up to $z_\mathrm{max} = 0.16$, in the BORG SDSS Cosmic Web reconstructions. We measured the Cosmic Web density for each RG; for the control sample, we then quantified the relation between RG radio luminosity and Cosmic Web density. With the BORG SDSS tidal tensor, we also measured for each RG whether the gravitational dynamics of its Cosmic Web environment resemble those of clusters, filaments, sheets, or voids. Luminous giants populate large-scale environments that tend to be denser than those of general RGs. This shows that -- at least at high jet powers -- low-density environments are no prerequisite for giant growth. This result is corroborated by gravitational dynamics classification and a cluster catalogue crossmatching analysis. This work presents more than a thousand inferred megaparsec-scale densities around radio galaxies. Our findings are consistent with the view that giants are regular, rather than mechanistically special, members of the radio galaxy population. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.17776v1-abstract-full').style.display = 'none'; document.getElementById('2404.17776v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 21 figures, 4 tables, accepted for publication in Astronomy & Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.10234">arXiv:2210.10234</a> <span> [<a href="https://arxiv.org/pdf/2210.10234">pdf</a>, <a href="https://arxiv.org/format/2210.10234">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243572">10.1051/0004-6361/202243572 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measuring the giant radio galaxy length distribution with the LoTSS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Oei%2C+M+S+S+L">Martijn S. S. L. Oei</a>, <a href="/search/?searchtype=author&query=van+Weeren%2C+R+J">Reinout J. van Weeren</a>, <a href="/search/?searchtype=author&query=Gast%2C+A+R+D+J+G+I+B">Aivin R. D. J. G. I. B. Gast</a>, <a href="/search/?searchtype=author&query=Botteon%2C+A">Andrea Botteon</a>, <a href="/search/?searchtype=author&query=Hardcastle%2C+M+J">Martin J. Hardcastle</a>, <a href="/search/?searchtype=author&query=Dabhade%2C+P">Pratik Dabhade</a>, <a href="/search/?searchtype=author&query=Shimwell%2C+T+W">Tim W. Shimwell</a>, <a href="/search/?searchtype=author&query=R%C3%B6ttgering%2C+H+J+A">Huub J. A. R枚ttgering</a>, <a href="/search/?searchtype=author&query=Drabent%2C+A">Alexander Drabent</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.10234v2-abstract-short" style="display: inline;"> Radio galaxies are luminous structures created by the jets of supermassive black holes, and consist of atomic nuclei, relativistic electrons, and magnetic fields. In exceptional cases, radio galaxies attain cosmological, megaparsec extents - and thus turn into giants. Giants embody the most extreme known mechanism through which galaxies can impact the Cosmic Web around them. The triggers of giant… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.10234v2-abstract-full').style.display = 'inline'; document.getElementById('2210.10234v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.10234v2-abstract-full" style="display: none;"> Radio galaxies are luminous structures created by the jets of supermassive black holes, and consist of atomic nuclei, relativistic electrons, and magnetic fields. In exceptional cases, radio galaxies attain cosmological, megaparsec extents - and thus turn into giants. Giants embody the most extreme known mechanism through which galaxies can impact the Cosmic Web around them. The triggers of giant growth remain a mystery. Excitingly, new sensitive low-frequency sky surveys hold promise to change this situation. In this work, we perform a precision measurement of the distribution of giant growth's central dynamical quantity: total length. We first construct a statistical geometric framework for radio galaxies that is both rigorous and practical. We then search the LOFAR Two-metre Sky Survey for giants, discovering 2060 previously unknown specimina: more than have been found in all preceding literature combined. Spectacular discoveries include the longest giant hosted by an elliptical galaxy, the longest giant hosted by a spiral galaxy, and 13 giants with an angular length larger than that of the full Moon. By combining theory and observations - and carefully forward modelling selection effects - we infer that giant radio galaxy lengths are well described by a Pareto distribution with tail index $-3.5 \pm 0.5$. This finding is a new observational constraint for models and simulations of radio galaxy growth. In addition, for the first time, we determine the comoving number density of giants, $5 \pm 2\ (100\ \mathrm{Mpc})^{-3}$, and the volume-filling fraction of giant radio galaxy lobes in clusters and filaments, $5\substack{+8\\-2}\cdot 10^{-6}$. We conclude that giants are truly rare - not only from an observational perspective, but also from a cosmological one. At any moment in time, most clusters and filaments - the building blocks of the modern Cosmic Web - do not harbour giants. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.10234v2-abstract-full').style.display = 'none'; document.getElementById('2210.10234v2-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 18 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">41 pages, 28 figures, 5 tables, published 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 672, A163 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.05427">arXiv:2202.05427</a> <span> [<a href="https://arxiv.org/pdf/2202.05427">pdf</a>, <a href="https://arxiv.org/format/2202.05427">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202142778">10.1051/0004-6361/202142778 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The discovery of a radio galaxy of at least 5 Mpc </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Oei%2C+M+S+S+L">Martijn S. S. L. Oei</a>, <a href="/search/?searchtype=author&query=van+Weeren%2C+R+J">Reinout J. van Weeren</a>, <a href="/search/?searchtype=author&query=Hardcastle%2C+M+J">Martin J. Hardcastle</a>, <a href="/search/?searchtype=author&query=Botteon%2C+A">Andrea Botteon</a>, <a href="/search/?searchtype=author&query=Shimwell%2C+T+W">Tim W. Shimwell</a>, <a href="/search/?searchtype=author&query=Dabhade%2C+P">Pratik Dabhade</a>, <a href="/search/?searchtype=author&query=Gast%2C+A+R+D+J+G+I+B">Aivin R. D. J. G. I. B. Gast</a>, <a href="/search/?searchtype=author&query=R%C3%B6ttgering%2C+H+J+A">Huub J. A. R枚ttgering</a>, <a href="/search/?searchtype=author&query=Br%C3%BCggen%2C+M">Marcus Br眉ggen</a>, <a href="/search/?searchtype=author&query=Tasse%2C+C">Cyril Tasse</a>, <a href="/search/?searchtype=author&query=Williams%2C+W+L">Wendy L. Williams</a>, <a href="/search/?searchtype=author&query=Shulevski%2C+A">Aleksandar Shulevski</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2202.05427v1-abstract-short" style="display: inline;"> We discover what is in projection the largest known structure of galactic origin: a giant radio galaxy with a projected proper length of $4.99 \pm 0.04\ \mathrm{Mpc}$. The source, named Alcyoneus, was first identified in low-resolution LOFAR Two-metre Sky Survey images from which angularly compact sources had been removed. Being an extreme example in its class, Alcyoneus could shed light on the ma… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.05427v1-abstract-full').style.display = 'inline'; document.getElementById('2202.05427v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.05427v1-abstract-full" style="display: none;"> We discover what is in projection the largest known structure of galactic origin: a giant radio galaxy with a projected proper length of $4.99 \pm 0.04\ \mathrm{Mpc}$. The source, named Alcyoneus, was first identified in low-resolution LOFAR Two-metre Sky Survey images from which angularly compact sources had been removed. Being an extreme example in its class, Alcyoneus could shed light on the main mechanisms that drive radio galaxy growth. We find that - beyond geometry - Alcyoneus and its host galaxy appear suspiciously ordinary: the total low-frequency luminosity density, stellar mass and supermassive black hole mass are all lower than, though similar to, those of the medial giant radio galaxy (percentiles $45 \pm 3\%$, $25 \pm 9 \%$ and $23 \pm 11 \%$, respectively). The source resides in a filament of the Cosmic Web, with which it might have significant thermodynamic interaction. At $5 \cdot 10^{-16}\ \mathrm{Pa}$, the pressures in the lobes are the lowest hitherto found, and Alcyoneus therefore represents one of the most promising radio galaxies yet to probe the warm-hot intergalactic medium. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.05427v1-abstract-full').style.display = 'none'; document.getElementById('2202.05427v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 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">18 pages, 14 figures, 3 tables, accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 660, A2 (2022) </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 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