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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=Berge%2C+D&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Berge%2C+D&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Berge%2C+D&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Berge%2C+D&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.10140">arXiv:2411.10140</a> <span> [<a href="https://arxiv.org/pdf/2411.10140">pdf</a>, <a href="https://arxiv.org/format/2411.10140">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"> Early Detection of Multiwavelength Blazar Variability </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Stolte%2C+H">Hermann Stolte</a>, <a href="/search/astro-ph?searchtype=author&query=Sinapius%2C+J">Jonas Sinapius</a>, <a href="/search/astro-ph?searchtype=author&query=Sadeh%2C+I">Iftach Sadeh</a>, <a href="/search/astro-ph?searchtype=author&query=Pueschel%2C+E">Elisa Pueschel</a>, <a href="/search/astro-ph?searchtype=author&query=Weidlich%2C+M">Matthias Weidlich</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">David Berge</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="2411.10140v1-abstract-short" style="display: inline;"> Blazars are a subclass of active galactic nuclei (AGNs) with relativistic jets pointing toward the observer. They are notable for their flux variability at all observed wavelengths and timescales. Together with simultaneous measurements at lower energies, the very-high-energy (VHE) emission observed during blazar flares may be used to probe the population of accelerated particles. However, optimal… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.10140v1-abstract-full').style.display = 'inline'; document.getElementById('2411.10140v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.10140v1-abstract-full" style="display: none;"> Blazars are a subclass of active galactic nuclei (AGNs) with relativistic jets pointing toward the observer. They are notable for their flux variability at all observed wavelengths and timescales. Together with simultaneous measurements at lower energies, the very-high-energy (VHE) emission observed during blazar flares may be used to probe the population of accelerated particles. However, optimally triggering observations of blazar high states can be challenging. Notable examples include identifying a flaring episode in real time and predicting VHE flaring activity based on lower energy observables. For this purpose, we have developed a novel deep learning analysis framework, based on data-driven anomaly detection techniques. It is capable of detecting various types of anomalies in real-world, multiwavelength light curves, ranging from clear high states to subtle correlations across bands. Based on unsupervised anomaly detection and clustering methods, we differentiate source variability from noisy background activity, without the need for a labeled training dataset of flaring states. The framework incorporates measurement uncertainties and is robust given data quality challenges, such as varying cadences and observational gaps. We evaluate our approach using both historical data and simulations of blazar light curves in two energy bands, corresponding to sources observable with the Fermi Large Area Telescope, and the upcoming Cherenkov Telescope Array Observatory (CTAO). In a statistical analysis, we show that our framework can reliably detect known historical flares. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.10140v1-abstract-full').style.display = 'none'; document.getElementById('2411.10140v1-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.08189">arXiv:2411.08189</a> <span> [<a href="https://arxiv.org/pdf/2411.08189">pdf</a>, <a href="https://arxiv.org/format/2411.08189">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/10.1103/PhysRevLett.133.221001">10.1103/PhysRevLett.133.221001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High-Statistics Measurement of the Cosmic-Ray Electron Spectrum with H.E.S.S </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bouyahiaoui%2C+M">M. Bouyahiaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a>, <a href="/search/astro-ph?searchtype=author&query=Bylund%2C+T">T. Bylund</a>, <a href="/search/astro-ph?searchtype=author&query=Casanova%2C+S">S. Casanova</a> , et al. (123 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="2411.08189v1-abstract-short" style="display: inline;"> Owing to their rapid cooling rate and hence loss-limited propagation distance, cosmic-ray electrons and positrons (CRe) at very high energies probe local cosmic-ray accelerators and provide constraints on exotic production mechanisms such as annihilation of dark matter particles. We present a high-statistics measurement of the spectrum of CRe candidate events from 0.3 to 40 TeV with the High Energ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.08189v1-abstract-full').style.display = 'inline'; document.getElementById('2411.08189v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.08189v1-abstract-full" style="display: none;"> Owing to their rapid cooling rate and hence loss-limited propagation distance, cosmic-ray electrons and positrons (CRe) at very high energies probe local cosmic-ray accelerators and provide constraints on exotic production mechanisms such as annihilation of dark matter particles. We present a high-statistics measurement of the spectrum of CRe candidate events from 0.3 to 40 TeV with the High Energy Stereoscopic System (H.E.S.S.), covering two orders of magnitude in energy and reaching a proton rejection power of better than $10^{4}$. The measured spectrum is well described by a broken power law, with a break around 1 TeV, where the spectral index increases from $螕_1 = 3.25$ $\pm$ 0.02 (stat) $\pm$ 0.2 (sys) to $螕_2 = 4.49$ $\pm$ 0.04 (stat) $\pm$ 0.2 (sys). Apart from the break, the spectrum is featureless. The absence of distinct signatures at multi-TeV energies imposes constraints on the presence of nearby CRe accelerators and the local CRe propagation mechanisms. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.08189v1-abstract-full').style.display = 'none'; document.getElementById('2411.08189v1-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, 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">main paper: 8 pages, 4 figures, supplemental material: 12 pages, 14 figures, accepted for publication in Physical Review Letters https://journals.aps.org/prl/</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 133, 221001 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.16219">arXiv:2407.16219</a> <span> [<a href="https://arxiv.org/pdf/2407.16219">pdf</a>, <a href="https://arxiv.org/format/2407.16219">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/ad5e67">10.3847/2041-8213/ad5e67 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Very-high-energy $纬$-ray emission from young massive star clusters in the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a>, <a href="/search/astro-ph?searchtype=author&query=Casanova%2C+S">S. Casanova</a>, <a href="/search/astro-ph?searchtype=author&query=Celic%2C+J">J. Celic</a>, <a href="/search/astro-ph?searchtype=author&query=Cerruti%2C+M">M. Cerruti</a>, <a href="/search/astro-ph?searchtype=author&query=Chand%2C+T">T. Chand</a>, <a href="/search/astro-ph?searchtype=author&query=Chandra%2C+S">S. Chandra</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+A">A. Chen</a> , et al. (107 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="2407.16219v1-abstract-short" style="display: inline;"> The Tarantula Nebula in the Large Magellanic Cloud is known for its high star formation activity. At its center lies the young massive star cluster R136, providing a significant amount of the energy that makes the nebula shine so brightly at many wavelengths. Recently, young massive star clusters have been suggested to also efficiently produce high-energy cosmic rays, potentially beyond PeV energi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.16219v1-abstract-full').style.display = 'inline'; document.getElementById('2407.16219v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.16219v1-abstract-full" style="display: none;"> The Tarantula Nebula in the Large Magellanic Cloud is known for its high star formation activity. At its center lies the young massive star cluster R136, providing a significant amount of the energy that makes the nebula shine so brightly at many wavelengths. Recently, young massive star clusters have been suggested to also efficiently produce high-energy cosmic rays, potentially beyond PeV energies. Here, we report the detection of very-high-energy $纬$-ray emission from the direction of R136 with the High Energy Stereoscopic System, achieved through a multicomponent, likelihood-based modeling of the data. This supports the hypothesis that R136 is indeed a very powerful cosmic-ray accelerator. Moreover, from the same analysis, we provide an updated measurement of the $纬$-ray emission from 30 Dor C, the only superbubble detected at TeV energies presently. The $纬$-ray luminosity above $0.5\,\mathrm{TeV}$ of both sources is $(2-3)\times 10^{35}\,\mathrm{erg}\,\mathrm{s}^{-1}$. This exceeds by more than a factor of 2 the luminosity of HESS J1646$-$458, which is associated with the most massive young star cluster in the Milky Way, Westerlund 1. Furthermore, the $纬$-ray emission from each source is extended with a significance of $>3蟽$ and a Gaussian width of about $30\,\mathrm{pc}$. For 30 Dor C, a connection between the $纬$-ray emission and the nonthermal X-ray emission appears likely. Different interpretations of the $纬$-ray signal from R136 are discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.16219v1-abstract-full').style.display = 'none'; document.getElementById('2407.16219v1-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10+11 pages, 4+6 figures. Corresponding authors: L. Mohrmann, N. Komin</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophysical Journal Letters 970, L21 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.03789">arXiv:2407.03789</a> <span> [<a href="https://arxiv.org/pdf/2407.03789">pdf</a>, <a href="https://arxiv.org/format/2407.03789">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="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Preliminary results of the Single Event Effect testing for the ULTRASAT sensors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Berlea%2C+V+D">Vlad Dumitru Berlea</a>, <a href="/search/astro-ph?searchtype=author&query=Asif%2C+A">Arooj Asif</a>, <a href="/search/astro-ph?searchtype=author&query=Barschke%2C+M+F">Merlin F. Barschke</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">David Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Crespo%2C+J+M+H">Juan Maria Haces Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Giavitto%2C+G">Gianluca Giavitto</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Shashank Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Porelli%2C+A">Andrea Porelli</a>, <a href="/search/astro-ph?searchtype=author&query=de+Simone%2C+N">Nicola de Simone</a>, <a href="/search/astro-ph?searchtype=author&query=Watson%2C+J">Jason Watson</a>, <a href="/search/astro-ph?searchtype=author&query=Worm%2C+S">Steven Worm</a>, <a href="/search/astro-ph?searchtype=author&query=Zappon%2C+F">Francesco Zappon</a>, <a href="/search/astro-ph?searchtype=author&query=Birman%2C+A">Adi Birman</a>, <a href="/search/astro-ph?searchtype=author&query=Alfassi%2C+S">Shay Alfassi</a>, <a href="/search/astro-ph?searchtype=author&query=Feningstein%2C+A">Amos Feningstein</a>, <a href="/search/astro-ph?searchtype=author&query=Waxman%2C+E">Eli Waxman</a>, <a href="/search/astro-ph?searchtype=author&query=Netzer%2C+U">Udi Netzer</a>, <a href="/search/astro-ph?searchtype=author&query=Liran%2C+T">Tuvia Liran</a>, <a href="/search/astro-ph?searchtype=author&query=Lapid%2C+O">Ofer Lapid</a>, <a href="/search/astro-ph?searchtype=author&query=Algranatti%2C+V+M">Viktor M. Algranatti</a>, <a href="/search/astro-ph?searchtype=author&query=Schvartzvald%2C+Y">Yossi Schvartzvald</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.03789v1-abstract-short" style="display: inline;"> ULTRASAT (ULtra-violet TRansient Astronomy SATellite) is a wide-angle space telescope that will perform a deep time-resolved all-sky survey in the near-ultraviolet (NUV) spectrum. The science objectives are the detection of counterparts to short-lived transient astronomical events such as gravitational wave sources and supernovae. The mission is led by the Weizmann Institute of Science and is plan… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.03789v1-abstract-full').style.display = 'inline'; document.getElementById('2407.03789v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.03789v1-abstract-full" style="display: none;"> ULTRASAT (ULtra-violet TRansient Astronomy SATellite) is a wide-angle space telescope that will perform a deep time-resolved all-sky survey in the near-ultraviolet (NUV) spectrum. The science objectives are the detection of counterparts to short-lived transient astronomical events such as gravitational wave sources and supernovae. The mission is led by the Weizmann Institute of Science and is planned for launch in 2026 in collaboration with the Israeli Space Agency and NASA. DESY will provide the UV camera, composed by the detector assembly located in the telescope focal plane and the remote electronics unit. The camera is composed out of four back-metallized CMOS Image Sensors (CIS) manufactured in the 4T, dual gain Tower process. As part of the radiation qualification of the camera, Single Event Effect (SEE) testing has been performed by irradiating the sensor with heavy ions at the RADEF, Jyvaskyla facility. Preliminary results of both Single Event Upset (SEU) and Single Event Latch-up (SEL) occurrence rate in the sensor are presented. Additionally, an in-orbit SEE rate simulation has been performed in order to gain preliminary knowledge about the expected effect of SEE on the mission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.03789v1-abstract-full').style.display = 'none'; document.getElementById('2407.03789v1-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.18167">arXiv:2406.18167</a> <span> [<a href="https://arxiv.org/pdf/2406.18167">pdf</a>, <a href="https://arxiv.org/format/2406.18167">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"> H.E.S.S. observations of the 2021 periastron passage of PSR B1259-63/LS 2883 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bouyahiaoui%2C+M">M. Bouyahiaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a>, <a href="/search/astro-ph?searchtype=author&query=Caroff%2C+S">S. Caroff</a>, <a href="/search/astro-ph?searchtype=author&query=Casanova%2C+S">S. Casanova</a> , et al. (119 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.18167v1-abstract-short" style="display: inline;"> PSR B1259-63 is a gamma-ray binary system that hosts a pulsar in an eccentric orbit, with a 3.4 year period, around an O9.5Ve star. At orbital phases close to periastron passages, the system radiates bright and variable non-thermal emission. We report on an extensive VHE observation campaign conducted with the High Energy Stereoscopic System, comprised of ~100 hours of data taken from $t_p-24$ day… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.18167v1-abstract-full').style.display = 'inline'; document.getElementById('2406.18167v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.18167v1-abstract-full" style="display: none;"> PSR B1259-63 is a gamma-ray binary system that hosts a pulsar in an eccentric orbit, with a 3.4 year period, around an O9.5Ve star. At orbital phases close to periastron passages, the system radiates bright and variable non-thermal emission. We report on an extensive VHE observation campaign conducted with the High Energy Stereoscopic System, comprised of ~100 hours of data taken from $t_p-24$ days to $t_p+127$ days around the system's 2021 periastron passage. We also present the timing and spectral analyses of the source. The VHE light curve in 2021 is consistent with the stacked light curve of all previous observations. Within the light curve, we report a VHE maximum at times coincident with the third X-ray peak first detected in the 2021 X-ray light curve. In the light curve -- although sparsely sampled in this time period -- we see no VHE enhancement during the second disc crossing. In addition, we see no correspondence to the 2021 GeV flare in the VHE light curve. The VHE spectrum obtained from the analysis of the 2021 dataset is best described by a power law of spectral index $螕= 2.65 \pm 0.04_{\text{stat}}$ $\pm 0.04_{\text{sys}}$, a value consistent with the previous H.E.S.S. observations of the source. We report spectral variability with a difference of $螖螕= 0.56 ~\pm~ 0.18_{\text{stat}}$ $~\pm~0.10_{\text{sys}}$ at 95% c.l., between sub-periods of the 2021 dataset. We also find a linear correlation between contemporaneous flux values of X-ray and TeV datasets, detected mainly after $t_p+25$ days, suggesting a change in the available energy for non-thermal radiation processes. We detect no significant correlation between GeV and TeV flux points, within the uncertainties of the measurements, from $\sim t_p-23$ days to $\sim t_p+126$ days. This suggests that the GeV and TeV emission originate from different electron populations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.18167v1-abstract-full').style.display = 'none'; document.getElementById('2406.18167v1-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 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">accepted to 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/2403.16802">arXiv:2403.16802</a> <span> [<a href="https://arxiv.org/pdf/2403.16802">pdf</a>, <a href="https://arxiv.org/format/2403.16802">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202348374">10.1051/0004-6361/202348374 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Unveiling extended gamma-ray emission around HESS J1813-178 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baktash%2C+A">A. Baktash</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+J">J. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bouyahiaoui%2C+M">M. Bouyahiaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a> , et al. (126 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.16802v1-abstract-short" style="display: inline;"> HESS J1813$-$178 is a very-high-energy $纬$-ray source spatially coincident with the young and energetic pulsar PSR J1813$-$1749 and thought to be associated with its pulsar wind nebula (PWN). Recently, evidence for extended high-energy emission in the vicinity of the pulsar has been revealed in the Fermi Large Area Telescope (LAT) data. This motivates revisiting the HESS J1813$-$178 region, taking… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.16802v1-abstract-full').style.display = 'inline'; document.getElementById('2403.16802v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.16802v1-abstract-full" style="display: none;"> HESS J1813$-$178 is a very-high-energy $纬$-ray source spatially coincident with the young and energetic pulsar PSR J1813$-$1749 and thought to be associated with its pulsar wind nebula (PWN). Recently, evidence for extended high-energy emission in the vicinity of the pulsar has been revealed in the Fermi Large Area Telescope (LAT) data. This motivates revisiting the HESS J1813$-$178 region, taking advantage of improved analysis methods and an extended data set. Using data taken by the High Energy Stereoscopic System (H.E.S.S.) experiment and the Fermi-LAT, we aim to describe the $纬$-ray emission in the region with a consistent model, to provide insights into its origin. We performed a likelihood-based analysis on 32 hours of H.E.S.S. data and 12 years of Fermi-LAT data and fit a spectro-morphological model to the combined datasets. These results allowed us to develop a physical model for the origin of the observed $纬$-ray emission in the region. In addition to the compact very-high-energy $纬$-ray emission centered on the pulsar, we find a significant yet previously undetected component along the Galactic plane. With Fermi-LAT data, we confirm extended high-energy emission consistent with the position and elongation of the extended emission observed with H.E.S.S. These results establish a consistent description of the emission in the region from GeV energies to several tens of TeV. This study suggests that HESS J1813$-$178 is associated with a $纬$-ray PWN powered by PSR J1813$-$1749. A possible origin of the extended emission component is inverse Compton emission from electrons and positrons that have escaped the confines of the pulsar and form a halo around the PWN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.16802v1-abstract-full').style.display = 'none'; document.getElementById('2403.16802v1-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13+5 pages, 13+11 figures. Accepted for publication in A&A. Corresponding authors: T.Wach, A.Mitchell, V.Joshi, P.Chamb茅ry</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 686, A149 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.12608">arXiv:2403.12608</a> <span> [<a href="https://arxiv.org/pdf/2403.12608">pdf</a>, <a href="https://arxiv.org/format/2403.12608">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/10.1051/0004-6361/202348651">10.1051/0004-6361/202348651 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectrum and extension of the inverse-Compton emission of the Crab Nebula from a combined Fermi-LAT and H.E.S.S. analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baktash%2C+A">A. Baktash</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bradascio%2C+F">F. Bradascio</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a> , et al. (137 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.12608v2-abstract-short" style="display: inline;"> The Crab Nebula is a unique laboratory for studying the acceleration of electrons and positrons through their non-thermal radiation. Observations of very-high-energy $纬$ rays from the Crab Nebula have provided important constraints for modelling its broadband emission. We present the first fully self-consistent analysis of the Crab Nebula's $纬$-ray emission between 1 GeV and $\sim$100 TeV, that is… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.12608v2-abstract-full').style.display = 'inline'; document.getElementById('2403.12608v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.12608v2-abstract-full" style="display: none;"> The Crab Nebula is a unique laboratory for studying the acceleration of electrons and positrons through their non-thermal radiation. Observations of very-high-energy $纬$ rays from the Crab Nebula have provided important constraints for modelling its broadband emission. We present the first fully self-consistent analysis of the Crab Nebula's $纬$-ray emission between 1 GeV and $\sim$100 TeV, that is, over five orders of magnitude in energy. Using the open-source software package Gammapy, we combined 11.4 yr of data from the Fermi Large Area Telescope and 80 h of High Energy Stereoscopic System (H.E.S.S.) data at the event level and provide a measurement of the spatial extension of the nebula and its energy spectrum. We find evidence for a shrinking of the nebula with increasing $纬$-ray energy. Furthermore, we fitted several phenomenological models to the measured data, finding that none of them can fully describe the spatial extension and the spectral energy distribution at the same time. Especially the extension measured at TeV energies appears too large when compared to the X-ray emission. Our measurements probe the structure of the magnetic field between the pulsar wind termination shock and the dust torus, and we conclude that the magnetic field strength decreases with increasing distance from the pulsar. We complement our study with a careful assessment of systematic uncertainties. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.12608v2-abstract-full').style.display = 'none'; document.getElementById('2403.12608v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18+6 pages, 15+2 figures. Accepted for publication in A&A. Corresponding authors: M. Meyer, L. Mohrmann, T. Unbehaun. v2: after A&A language editing</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 686, A308 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.04857">arXiv:2403.04857</a> <span> [<a href="https://arxiv.org/pdf/2403.04857">pdf</a>, <a href="https://arxiv.org/format/2403.04857">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 Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2024/07/047">10.1088/1475-7516/2024/07/047 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dark Matter Line Searches with the Cherenkov Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abhir%2C+J">J. Abhir</a>, <a href="/search/astro-ph?searchtype=author&query=Abhishek%2C+A">A. Abhishek</a>, <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre-Santaella%2C+A">A. Aguirre-Santaella</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Crespo%2C+N">N. Alvarez-Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amans%2C+J+-">J. -P. Amans</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Angel%2C+L">L. Angel</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Arnesen%2C+T+T+H">T. T. H. Arnesen</a>, <a href="/search/astro-ph?searchtype=author&query=Arrabito%2C+L">L. Arrabito</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Ascasibar%2C+Y">Y. Ascasibar</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a> , et al. (540 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.04857v2-abstract-short" style="display: inline;"> Monochromatic gamma-ray signals constitute a potential smoking gun signature for annihilating or decaying dark matter particles that could relatively easily be distinguished from astrophysical or instrumental backgrounds. We provide an updated assessment of the sensitivity of the Cherenkov Telescope Array (CTA) to such signals, based on observations of the Galactic centre region as well as of sele… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.04857v2-abstract-full').style.display = 'inline'; document.getElementById('2403.04857v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.04857v2-abstract-full" style="display: none;"> Monochromatic gamma-ray signals constitute a potential smoking gun signature for annihilating or decaying dark matter particles that could relatively easily be distinguished from astrophysical or instrumental backgrounds. We provide an updated assessment of the sensitivity of the Cherenkov Telescope Array (CTA) to such signals, based on observations of the Galactic centre region as well as of selected dwarf spheroidal galaxies. We find that current limits and detection prospects for dark matter masses above 300 GeV will be significantly improved, by up to an order of magnitude in the multi-TeV range. This demonstrates that CTA will set a new standard for gamma-ray astronomy also in this respect, as the world's largest and most sensitive high-energy gamma-ray observatory, in particular due to its exquisite energy resolution at TeV energies and the adopted observational strategy focussing on regions with large dark matter densities. Throughout our analysis, we use up-to-date instrument response functions, and we thoroughly model the effect of instrumental systematic uncertainties in our statistical treatment. We further present results for other potential signatures with sharp spectral features, e.g.~box-shaped spectra, that would likewise very clearly point to a particle dark matter origin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.04857v2-abstract-full').style.display = 'none'; document.getElementById('2403.04857v2-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">44 pages JCAP style (excluding author list and references), 19 figures; minor changes to match published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 07 (2024) 047 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.13330">arXiv:2402.13330</a> <span> [<a href="https://arxiv.org/pdf/2402.13330">pdf</a>, <a href="https://arxiv.org/format/2402.13330">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/10.1051/0004-6361/202348913">10.1051/0004-6361/202348913 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Curvature in the very-high energy gamma-ray spectrum of M87 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Bradascio%2C+F">F. Bradascio</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+T+B+C">T. Bulik C. Burger-Scheidlin</a>, <a href="/search/astro-ph?searchtype=author&query=Bylund%2C+T">T. Bylund</a>, <a href="/search/astro-ph?searchtype=author&query=Casanova%2C+S">S. Casanova</a>, <a href="/search/astro-ph?searchtype=author&query=Cecil%2C+R">R. Cecil</a>, <a href="/search/astro-ph?searchtype=author&query=Celic%2C+J">J. Celic</a>, <a href="/search/astro-ph?searchtype=author&query=Cerruti%2C+M">M. Cerruti</a> , et al. (110 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="2402.13330v3-abstract-short" style="display: inline;"> The radio galaxy M87 is a variable very-high energy (VHE) gamma-ray source, exhibiting three major flares reported in 2005, 2008, and 2010. Despite extensive studies, the origin of the VHE gamma-ray emission is yet to be understood. In this study, we investigate the VHE gamma-ray spectrum of M87 during states of high gamma-ray activity, utilizing 20.2$\,$ hours the H.E.S.S. observations. Our findi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.13330v3-abstract-full').style.display = 'inline'; document.getElementById('2402.13330v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.13330v3-abstract-full" style="display: none;"> The radio galaxy M87 is a variable very-high energy (VHE) gamma-ray source, exhibiting three major flares reported in 2005, 2008, and 2010. Despite extensive studies, the origin of the VHE gamma-ray emission is yet to be understood. In this study, we investigate the VHE gamma-ray spectrum of M87 during states of high gamma-ray activity, utilizing 20.2$\,$ hours the H.E.S.S. observations. Our findings indicate a preference for a curved spectrum, characterized by a log-parabola model with extra-galactic background light (EBL) model above 0.3$\,$TeV at the 4$蟽$ level, compared to a power-law spectrum with EBL. We investigate the degeneracy between the absorption feature and the EBL normalization and derive upper limits on EBL models mainly sensitive in the wavelength range 12.4$\,$$渭$m - 40$\,$$渭$m. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.13330v3-abstract-full').style.display = 'none'; document.getElementById('2402.13330v3-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 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">10 pages, 7 figures. Accepted for publication in A&A. Corresponding authors: Victor Barbosa Martins, Rahul Cecil, Iryna Lypova, Manuel Meyer, Perri Zilberman. Supplementary material: https://zenodo.org/records/10781524</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A, 685, A96 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.16019">arXiv:2401.16019</a> <span> [<a href="https://arxiv.org/pdf/2401.16019">pdf</a>, <a href="https://arxiv.org/format/2401.16019">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/10.1126/science.adi2048">10.1126/science.adi2048 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Acceleration and transport of relativistic electrons in the jets of the microquasar SS 433 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bouyahiaou%2C+M">M. Bouyahiaou</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhau%2C+M">M. Breuhau</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+M">A. M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a>, <a href="/search/astro-ph?searchtype=author&query=Caroff%2C+S">S. Caroff</a> , et al. (140 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.16019v1-abstract-short" style="display: inline;"> SS 433 is a microquasar, a stellar binary system with collimated relativistic jets. We observed SS 433 in gamma rays using the High Energy Stereoscopic System (H.E.S.S.), finding an energy-dependent shift in the apparent position of the gamma-ray emission of the parsec-scale jets. These observations trace the energetic electron population and indicate the gamma rays are produced by inverse-Compton… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.16019v1-abstract-full').style.display = 'inline'; document.getElementById('2401.16019v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.16019v1-abstract-full" style="display: none;"> SS 433 is a microquasar, a stellar binary system with collimated relativistic jets. We observed SS 433 in gamma rays using the High Energy Stereoscopic System (H.E.S.S.), finding an energy-dependent shift in the apparent position of the gamma-ray emission of the parsec-scale jets. These observations trace the energetic electron population and indicate the gamma rays are produced by inverse-Compton scattering. Modelling of the energy-dependent gamma-ray morphology constrains the location of particle acceleration and requires an abrupt deceleration of the jet flow. We infer the presence of shocks on either side of the binary system at distances of 25 to 30 parsecs and conclude that self-collimation of the precessing jets forms the shocks, which then efficiently accelerate electrons. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.16019v1-abstract-full').style.display = 'none'; document.getElementById('2401.16019v1-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 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">Submitted 20th Apr. 2023, published 25th January 2024 (accepted version)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Science383,402-406(2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.07071">arXiv:2401.07071</a> <span> [<a href="https://arxiv.org/pdf/2401.07071">pdf</a>, <a href="https://arxiv.org/format/2401.07071">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"> TeV flaring activity of the AGN PKS 0625-354 in November 2018 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baktash%2C+A">A. Baktash</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+J">J. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bradascio%2C+F">F. Bradascio</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A">A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a> , et al. (117 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="2401.07071v1-abstract-short" style="display: inline;"> Most $纬$-ray detected active galactic nuclei are blazars with one of their relativistic jets pointing towards the Earth. Only a few objects belong to the class of radio galaxies or misaligned blazars. Here, we investigate the nature of the object PKS 0625-354, its $纬$-ray flux and spectral variability and its broad-band spectral emission with observations from H.E.S.S., Fermi-LAT, Swift-XRT, and U… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.07071v1-abstract-full').style.display = 'inline'; document.getElementById('2401.07071v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.07071v1-abstract-full" style="display: none;"> Most $纬$-ray detected active galactic nuclei are blazars with one of their relativistic jets pointing towards the Earth. Only a few objects belong to the class of radio galaxies or misaligned blazars. Here, we investigate the nature of the object PKS 0625-354, its $纬$-ray flux and spectral variability and its broad-band spectral emission with observations from H.E.S.S., Fermi-LAT, Swift-XRT, and UVOT taken in November 2018. The H.E.S.S. light curve above 200 GeV shows an outburst in the first night of observations followed by a declining flux with a halving time scale of 5.9h. The $纬纬$-opacity constrains the upper limit of the angle between the jet and the line of sight to $\sim10^\circ$. The broad-band spectral energy distribution shows two humps and can be well fitted with a single-zone synchrotron self Compton emission model. We conclude that PKS 0625-354, as an object showing clear features of both blazars and radio galaxies, can be classified as an intermediate active galactic nuclei. Multi-wavelength studies of such intermediate objects exhibiting features of both blazars and radio galaxies are sparse but crucial for the understanding of the broad-band emission of $纬$-ray detected active galactic nuclei in general. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.07071v1-abstract-full').style.display = 'none'; document.getElementById('2401.07071v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 January, 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">9 pages, 6 figures, 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/2310.06181">arXiv:2310.06181</a> <span> [<a href="https://arxiv.org/pdf/2310.06181">pdf</a>, <a href="https://arxiv.org/format/2310.06181">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41550-023-02052-3">10.1038/s41550-023-02052-3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of a Radiation Component from the Vela Pulsar Reaching 20 Teraelectronvolts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+T+H+E+S+S">The H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bradascio%2C+F">F. Bradascio</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a> , et al. (157 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="2310.06181v1-abstract-short" style="display: inline;"> Gamma-ray observations have established energetic isolated pulsars as outstanding particle accelerators and antimatter factories in the Galaxy. There is, however, no consensus regarding the acceleration mechanisms and the radiative processes at play, nor the locations where these take place. The spectra of all observed gamma-ray pulsars to date show strong cutoffs or a break above energies of a fe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06181v1-abstract-full').style.display = 'inline'; document.getElementById('2310.06181v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.06181v1-abstract-full" style="display: none;"> Gamma-ray observations have established energetic isolated pulsars as outstanding particle accelerators and antimatter factories in the Galaxy. There is, however, no consensus regarding the acceleration mechanisms and the radiative processes at play, nor the locations where these take place. The spectra of all observed gamma-ray pulsars to date show strong cutoffs or a break above energies of a few gigaelectronvolt (GeV). Using the H.E.S.S. array of Cherenkov telescopes, we discovered a novel radiation component emerging beyond this generic GeV cutoff in the Vela pulsar's broadband spectrum. The extension of gamma-ray pulsation energies up to at least 20 teraelectronvolts (TeV) shows that Vela pulsar can accelerate particles to Lorentz factors higher than $4\times10^7$. This is an order of magnitude larger than in the case of the Crab pulsar, the only other pulsar detected in the TeV energy range. Our results challenge the state-of-the-art models for high-energy emission of pulsars while providing a new probe, i.e. the energetic multi-TeV component, for constraining the acceleration and emission processes in their extreme energy limit. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06181v1-abstract-full').style.display = 'none'; document.getElementById('2310.06181v1-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 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">38 pages, 6 figures. This preprint has not undergone peer review or any post-submission improvements or corrections. The Version of Record of this article is published in Nature Astronomy, Nat Astron (2023), and is available online at https://doi.org/10.1038/s41550-023-02052-3</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.14794">arXiv:2309.14794</a> <span> [<a href="https://arxiv.org/pdf/2309.14794">pdf</a>, <a href="https://arxiv.org/format/2309.14794">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"> TELAMON: Effelsberg Monitoring of AGN Jets with Very-High-Energy Astroparticle Emissions -- Polarization properties </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=He%C3%9Fd%C3%B6rfer%2C+J">J. He脽d枚rfer</a>, <a href="/search/astro-ph?searchtype=author&query=Kadler%2C+M">M. Kadler</a>, <a href="/search/astro-ph?searchtype=author&query=Benke%2C+P">P. Benke</a>, <a href="/search/astro-ph?searchtype=author&query=Debbrecht%2C+L">L. Debbrecht</a>, <a href="/search/astro-ph?searchtype=author&query=Eich%2C+J">J. Eich</a>, <a href="/search/astro-ph?searchtype=author&query=Eppel%2C+F">F. Eppel</a>, <a href="/search/astro-ph?searchtype=author&query=Gokus%2C+A">A. Gokus</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%A4mmerich%2C+S">S. H盲mmerich</a>, <a href="/search/astro-ph?searchtype=author&query=Kirchner%2C+D">D. Kirchner</a>, <a href="/search/astro-ph?searchtype=author&query=Paraschos%2C+G+F">G. F. Paraschos</a>, <a href="/search/astro-ph?searchtype=author&query=R%C3%B6sch%2C+F">F. R枚sch</a>, <a href="/search/astro-ph?searchtype=author&query=Schulga%2C+W">W. Schulga</a>, <a href="/search/astro-ph?searchtype=author&query=Sinapius%2C+J">J. Sinapius</a>, <a href="/search/astro-ph?searchtype=author&query=Weber%2C+P">P. Weber</a>, <a href="/search/astro-ph?searchtype=author&query=Bach%2C+U">U. Bach</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Buson%2C+S">S. Buson</a>, <a href="/search/astro-ph?searchtype=author&query=Dorner%2C+D">D. Dorner</a>, <a href="/search/astro-ph?searchtype=author&query=Edwards%2C+P+G">P. G. Edwards</a>, <a href="/search/astro-ph?searchtype=author&query=Fromm%2C+C+M">C. M. Fromm</a>, <a href="/search/astro-ph?searchtype=author&query=Giroletti%2C+M">M. Giroletti</a>, <a href="/search/astro-ph?searchtype=author&query=Hervet%2C+O">O. Hervet</a>, <a href="/search/astro-ph?searchtype=author&query=Kappes%2C+A">A. Kappes</a>, <a href="/search/astro-ph?searchtype=author&query=Koyama%2C+S">S. Koyama</a>, <a href="/search/astro-ph?searchtype=author&query=Kraus%2C+A">A. Kraus</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="2309.14794v2-abstract-short" style="display: inline;"> We present recent results of the TELAMON program, which is using the Effelsberg 100-m telescope to monitor the radio spectra of active galactic nuclei (AGN) under scrutiny in astroparticle physics, namely TeV blazars and neutrino-associated AGN. Our sample includes all known Northern TeV-emitting blazars as well as blazars positionally coincident with IceCube neutrino alerts. Polarization can give… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.14794v2-abstract-full').style.display = 'inline'; document.getElementById('2309.14794v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.14794v2-abstract-full" style="display: none;"> We present recent results of the TELAMON program, which is using the Effelsberg 100-m telescope to monitor the radio spectra of active galactic nuclei (AGN) under scrutiny in astroparticle physics, namely TeV blazars and neutrino-associated AGN. Our sample includes all known Northern TeV-emitting blazars as well as blazars positionally coincident with IceCube neutrino alerts. Polarization can give additional insight into the source properties, as the polarized emission is often found to vary on different timescales and amplitudes than the total intensity emission. Here, we present an overview of the polarization properties of the TeV-emitting TELAMON sources at four frequencies in the 20 mm and 7 mm bands. While at 7 mm roughly $82\,\%$ of all observed sources are found to be significantly polarized, for 20 mm the percentage is $\sim58\,\%$. We find that most of the sources exhibit mean fractional polarizations of $<5\%$, matching the expectations of rather low polarization levels in these sources from previous studies at lower radio frequencies. Nevertheless, we demonstrate examples of how the polarized emission can provide additional information over the total intensity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.14794v2-abstract-full').style.display = 'none'; document.getElementById('2309.14794v2-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 2 figures, Proceedings of the 38th International Cosmic Ray Conference (ICRC2023)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.13584">arXiv:2308.13584</a> <span> [<a href="https://arxiv.org/pdf/2308.13584">pdf</a>, <a href="https://arxiv.org/format/2308.13584">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/10.1051/0004-6361/202346488">10.1051/0004-6361/202346488 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gammapy: A Python package for gamma-ray astronomy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Donath%2C+A">Axel Donath</a>, <a href="/search/astro-ph?searchtype=author&query=Terrier%2C+R">R茅gis Terrier</a>, <a href="/search/astro-ph?searchtype=author&query=Remy%2C+Q">Quentin Remy</a>, <a href="/search/astro-ph?searchtype=author&query=Sinha%2C+A">Atreyee Sinha</a>, <a href="/search/astro-ph?searchtype=author&query=Nigro%2C+C">Cosimo Nigro</a>, <a href="/search/astro-ph?searchtype=author&query=Pintore%2C+F">Fabio Pintore</a>, <a href="/search/astro-ph?searchtype=author&query=Kh%C3%A9lifi%2C+B">Bruno Kh茅lifi</a>, <a href="/search/astro-ph?searchtype=author&query=Olivera-Nieto%2C+L">Laura Olivera-Nieto</a>, <a href="/search/astro-ph?searchtype=author&query=Ruiz%2C+J+E">Jose Enrique Ruiz</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%BCgge%2C+K">Kai Br眉gge</a>, <a href="/search/astro-ph?searchtype=author&query=Linhoff%2C+M">Maximilian Linhoff</a>, <a href="/search/astro-ph?searchtype=author&query=Contreras%2C+J+L">Jose Luis Contreras</a>, <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">Fabio Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Aguasca-Cabot%2C+A">Arnau Aguasca-Cabot</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">David Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharjee%2C+P">Pooja Bhattacharjee</a>, <a href="/search/astro-ph?searchtype=author&query=Buchner%2C+J">Johannes Buchner</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">Catherine Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Fidalgo%2C+D+C">David Carreto Fidalgo</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+A">Andrew Chen</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">Mathieu de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Cardoso%2C+J+V+d+M">Jos茅 Vin铆cius de Miranda Cardoso</a>, <a href="/search/astro-ph?searchtype=author&query=Deil%2C+C">Christoph Deil</a>, <a href="/search/astro-ph?searchtype=author&query=F%C3%BC%C3%9Fling%2C+M">Matthias F眉脽ling</a>, <a href="/search/astro-ph?searchtype=author&query=Funk%2C+S">Stefan Funk</a> , et al. (20 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.13584v1-abstract-short" style="display: inline;"> In this article, we present Gammapy, an open-source Python package for the analysis of astronomical $纬$-ray data, and illustrate the functionalities of its first long-term-support release, version 1.0. Built on the modern Python scientific ecosystem, Gammapy provides a uniform platform for reducing and modeling data from different $纬$-ray instruments for many analysis scenarios. Gammapy complies w… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.13584v1-abstract-full').style.display = 'inline'; document.getElementById('2308.13584v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.13584v1-abstract-full" style="display: none;"> In this article, we present Gammapy, an open-source Python package for the analysis of astronomical $纬$-ray data, and illustrate the functionalities of its first long-term-support release, version 1.0. Built on the modern Python scientific ecosystem, Gammapy provides a uniform platform for reducing and modeling data from different $纬$-ray instruments for many analysis scenarios. Gammapy complies with several well-established data conventions in high-energy astrophysics, providing serialized data products that are interoperable with other software packages. Starting from event lists and instrument response functions, Gammapy provides functionalities to reduce these data by binning them in energy and sky coordinates. Several techniques for background estimation are implemented in the package to handle the residual hadronic background affecting $纬$-ray instruments. After the data are binned, the flux and morphology of one or more $纬$-ray sources can be estimated using Poisson maximum likelihood fitting and assuming a variety of spectral, temporal, and spatial models. Estimation of flux points, likelihood profiles, and light curves is also supported. After describing the structure of the package, we show, using publicly available $纬$-ray data, the capabilities of Gammapy in multiple traditional and novel $纬$-ray analysis scenarios, such as spectral and spectro-morphological modeling and estimations of a spectral energy distribution and a light curve. Its flexibility and power are displayed in a final multi-instrument example, where datasets from different instruments, at different stages of data reduction, are simultaneously fitted with an astrophysical flux model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.13584v1-abstract-full').style.display = 'none'; document.getElementById('2308.13584v1-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 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">26 pages, 16 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 678, A157 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.01692">arXiv:2307.01692</a> <span> [<a href="https://arxiv.org/pdf/2307.01692">pdf</a>, <a href="https://arxiv.org/format/2307.01692">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/10.3847/2041-8213/ace3c0">10.3847/2041-8213/ace3c0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The vanishing of the primary emission region in PKS 1510-089 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+J">J. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernloehr%2C+K">K. Bernloehr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Boettcher%2C+M">M. Boettcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bouyahiaoui%2C+M">M. Bouyahiaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Bradascio%2C+F">F. Bradascio</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+M">A. M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a> , et al. (130 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="2307.01692v1-abstract-short" style="display: inline;"> In July 2021, PKS 1510-089 exhibited a significant flux drop in the high-energy gamma-ray (by a factor 10) and optical (by a factor 5) bands and remained in this low state throughout 2022. Similarly, the optical polarization in the source vanished, resulting in the optical spectrum being fully explained through the steady flux of the accretion disk and the broad-line region. Unlike the aforementio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.01692v1-abstract-full').style.display = 'inline'; document.getElementById('2307.01692v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.01692v1-abstract-full" style="display: none;"> In July 2021, PKS 1510-089 exhibited a significant flux drop in the high-energy gamma-ray (by a factor 10) and optical (by a factor 5) bands and remained in this low state throughout 2022. Similarly, the optical polarization in the source vanished, resulting in the optical spectrum being fully explained through the steady flux of the accretion disk and the broad-line region. Unlike the aforementioned bands, the very-high-energy gamma-ray and X-ray fluxes did not exhibit a significant flux drop from year to year. This suggests that the steady-state very-high-energy gamma-ray and X-ray fluxes originate from a different emission region than the vanished parts of the high-energy gamma-ray and optical jet fluxes. The latter component has disappeared through either a swing of the jet away from the line-of-sight or a significant drop in the photon production efficiency of the jet close to the black hole. Either change could become visible in high-resolution radio images. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.01692v1-abstract-full').style.display = 'none'; document.getElementById('2307.01692v1-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 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">18 pages, 4 figures, 6 tables; accepted for publication in ApJ Letters; corresponding authors: Joleen Barnard, Markus Boettcher, Hester Schutte, Michael Zacharias</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.17819">arXiv:2306.17819</a> <span> [<a href="https://arxiv.org/pdf/2306.17819">pdf</a>, <a href="https://arxiv.org/format/2306.17819">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"> Multiwavelength Observations of the Blazar PKS 0735+178 in Spatial and Temporal Coincidence with an Astrophysical Neutrino Candidate IceCube-211208A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C+B">C. B. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Archer%2C+A">A. Archer</a>, <a href="/search/astro-ph?searchtype=author&query=Bangale%2C+P">P. Bangale</a>, <a href="/search/astro-ph?searchtype=author&query=Bartkoske%2C+J+T">J. T. Bartkoske</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+P">P. Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Brill%2C+A">A. Brill</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Christiansen%2C+J+L">J. L. Christiansen</a>, <a href="/search/astro-ph?searchtype=author&query=Chromey%2C+A+J">A. J. Chromey</a>, <a href="/search/astro-ph?searchtype=author&query=Errando%2C+M">M. Errando</a>, <a href="/search/astro-ph?searchtype=author&query=Falcone%2C+A">A. Falcone</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+Q">Q. Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Foote%2C+G+M">G. M. Foote</a>, <a href="/search/astro-ph?searchtype=author&query=Fortson%2C+L">L. Fortson</a>, <a href="/search/astro-ph?searchtype=author&query=Furniss%2C+A">A. Furniss</a>, <a href="/search/astro-ph?searchtype=author&query=Gallagher%2C+G">G. Gallagher</a>, <a href="/search/astro-ph?searchtype=author&query=Hanlon%2C+W">W. Hanlon</a>, <a href="/search/astro-ph?searchtype=author&query=Hanna%2C+D">D. Hanna</a>, <a href="/search/astro-ph?searchtype=author&query=Hervet%2C+O">O. Hervet</a>, <a href="/search/astro-ph?searchtype=author&query=Hinrichs%2C+C+E">C. E. Hinrichs</a>, <a href="/search/astro-ph?searchtype=author&query=Hoang%2C+J">J. Hoang</a>, <a href="/search/astro-ph?searchtype=author&query=Holder%2C+J">J. Holder</a>, <a href="/search/astro-ph?searchtype=author&query=Humensky%2C+T+B">T. B. Humensky</a> , et al. (185 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.17819v1-abstract-short" style="display: inline;"> We report on multiwavelength target-of-opportunity observations of the blazar PKS 0735+178, located 2.2$^\circ$ away from the best-fit position of the IceCube neutrino event IceCube-211208A detected on December 8, 2021. The source was in a high-flux state in the optical, ultraviolet, X-ray, and GeV gamma-ray bands around the time of the neutrino event, exhibiting daily variability in the soft X-ra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.17819v1-abstract-full').style.display = 'inline'; document.getElementById('2306.17819v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.17819v1-abstract-full" style="display: none;"> We report on multiwavelength target-of-opportunity observations of the blazar PKS 0735+178, located 2.2$^\circ$ away from the best-fit position of the IceCube neutrino event IceCube-211208A detected on December 8, 2021. The source was in a high-flux state in the optical, ultraviolet, X-ray, and GeV gamma-ray bands around the time of the neutrino event, exhibiting daily variability in the soft X-ray flux. The X-ray data from Swift-XRT and NuSTAR characterize the transition between the low-energy and high-energy components of the broadband spectral energy distribution (SED), and the gamma-ray data from Fermi -LAT, VERITAS, and H.E.S.S. require a spectral cut-off near 100 GeV. Both X-ray and gamma-ray measurements provide strong constraints on the leptonic and hadronic models. We analytically explore a synchrotron self-Compton model, an external Compton model, and a lepto-hadronic model. Models that are entirely based on internal photon fields face serious difficulties in matching the observed SED. The existence of an external photon field in the source would instead explain the observed gamma-ray spectral cut-off in both leptonic and lepto-hadronic models and allow a proton jet power that marginally agrees with the Eddington limit in the lepto-hadronic model. We show a numerical lepto-hadronic model with external target photons that reproduces the observed SED and is reasonably consistent with the neutrino event despite requiring a high jet power. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.17819v1-abstract-full').style.display = 'none'; document.getElementById('2306.17819v1-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 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 3 figures, accepted by ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.15307">arXiv:2306.15307</a> <span> [<a href="https://arxiv.org/pdf/2306.15307">pdf</a>, <a href="https://arxiv.org/format/2306.15307">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="Instrumentation and Detectors">physics.ins-det</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/10.1016/j.nima.2023.168463">10.1016/j.nima.2023.168463 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Total Ionizing Dose Effects on CMOS Image Sensor for the ULTRASAT Space Mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Berlea%2C+V+D">Vlad D. Berlea</a>, <a href="/search/astro-ph?searchtype=author&query=Worm%2C+S">Steven Worm</a>, <a href="/search/astro-ph?searchtype=author&query=Kaipachery%2C+N">Nirmal Kaipachery</a>, <a href="/search/astro-ph?searchtype=author&query=Kulkarni%2C+S+R">Shrinivasrao R. Kulkarni</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+S">Shashank Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Barschke%2C+M+F">Merlin F. Barschke</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">David Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Birman%2C+A">Adi Birman</a>, <a href="/search/astro-ph?searchtype=author&query=Alfassi%2C+S">Shay Alfassi</a>, <a href="/search/astro-ph?searchtype=author&query=Fenigstein%2C+A">Amos Fenigstein</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="2306.15307v1-abstract-short" style="display: inline;"> ULTRASAT (ULtraviolet TRansient Astronomy SATellite) is a wide-angle space telescope that will perform deep time-resolved surveys in the near-ultraviolet spectrum. ULTRASAT is a space mission led by the Weizmann Institute of Science and the Israel Space Agency and is planned for launch in 2025. The camera implements backside-illuminated, stitched pixel sensors. The pixel has a dual-conversion-gain… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.15307v1-abstract-full').style.display = 'inline'; document.getElementById('2306.15307v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.15307v1-abstract-full" style="display: none;"> ULTRASAT (ULtraviolet TRansient Astronomy SATellite) is a wide-angle space telescope that will perform deep time-resolved surveys in the near-ultraviolet spectrum. ULTRASAT is a space mission led by the Weizmann Institute of Science and the Israel Space Agency and is planned for launch in 2025. The camera implements backside-illuminated, stitched pixel sensors. The pixel has a dual-conversion-gain 4T architecture, with a pitch of $9.5$ $渭m$ and is produced in a $180$ $nm$ process by Tower Semiconductor. Before the final sensor was available for testing, test sensors provided by Tower were used to gain first insights into the pixel's radiation tolerance. One of the main contributions to sensor degradation due to radiation for the ULTRASAT mission is Total Ionizing Dose (TID). TID measurements on the test sensors have been performed with a Co-60 gamma source at Helmholz Zentrum Berlin and CC-60 facility at CERN and preliminary results are presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.15307v1-abstract-full').style.display = 'none'; document.getElementById('2306.15307v1-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 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Part of the conference: Frontier Detectors for Frontier Physics: 15th Pisa Meeting on Advanced Detectors, La Biodola - Isola d'Elba Published in: Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment Available online 15 June 2023, 168463. In Press, Journal Pre-proof</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nuclear Inst. and Methods inPhysics Research, A (2023) 168463 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.15080">arXiv:2306.15080</a> <span> [<a href="https://arxiv.org/pdf/2306.15080">pdf</a>, <a href="https://arxiv.org/format/2306.15080">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Science with a small two-band UV-photometry mission I: Mission description and follow-up observations of stellar transients </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Werner%2C+N">N. Werner</a>, <a href="/search/astro-ph?searchtype=author&query=%C5%98%C3%ADpa%2C+J">J. 艠铆pa</a>, <a href="/search/astro-ph?searchtype=author&query=Th%C3%B6ne%2C+C">C. Th枚ne</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%BCnz%2C+F">F. M眉nz</a>, <a href="/search/astro-ph?searchtype=author&query=Kurf%C3%BCrst%2C+P">P. Kurf眉rst</a>, <a href="/search/astro-ph?searchtype=author&query=Jel%C3%ADnek%2C+M">M. Jel铆nek</a>, <a href="/search/astro-ph?searchtype=author&query=Hroch%2C+F">F. Hroch</a>, <a href="/search/astro-ph?searchtype=author&query=Ben%C3%A1%C4%8Dek%2C+J">J. Ben谩膷ek</a>, <a href="/search/astro-ph?searchtype=author&query=Topinka%2C+M">M. Topinka</a>, <a href="/search/astro-ph?searchtype=author&query=Lukes-Gerakopoulos%2C+G">G. Lukes-Gerakopoulos</a>, <a href="/search/astro-ph?searchtype=author&query=Zaja%C4%8Dek%2C+M">M. Zaja膷ek</a>, <a href="/search/astro-ph?searchtype=author&query=Labaj%2C+M">M. Labaj</a>, <a href="/search/astro-ph?searchtype=author&query=Pri%C5%A1egen%2C+M">M. Pri拧egen</a>, <a href="/search/astro-ph?searchtype=author&query=Krti%C4%8Dka%2C+J">J. Krti膷ka</a>, <a href="/search/astro-ph?searchtype=author&query=Merc%2C+J">J. Merc</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%A1l%2C+A">A. P谩l</a>, <a href="/search/astro-ph?searchtype=author&query=Pejcha%2C+O">O. Pejcha</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A1niel%2C+V">V. D谩niel</a>, <a href="/search/astro-ph?searchtype=author&query=Jon%2C+J">J. Jon</a>, <a href="/search/astro-ph?searchtype=author&query=%C5%A0o%C5%A1ovi%C4%8Dka%2C+R">R. 艩o拧ovi膷ka</a>, <a href="/search/astro-ph?searchtype=author&query=Grome%C5%A1%2C+J">J. Grome拧</a>, <a href="/search/astro-ph?searchtype=author&query=V%C3%A1clav%C3%ADk%2C+J">J. V谩clav铆k</a>, <a href="/search/astro-ph?searchtype=author&query=Steiger%2C+L">L. Steiger</a>, <a href="/search/astro-ph?searchtype=author&query=Segi%C5%88%C3%A1k%2C+J">J. Segi艌谩k</a>, <a href="/search/astro-ph?searchtype=author&query=Behar%2C+E">E. Behar</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="2306.15080v2-abstract-short" style="display: inline;"> This is the first in a collection of three papers introducing the science with an ultra-violet (UV) space telescope on an approximately 130~kg small satellite with a moderately fast re-pointing capability and a real-time alert communication system approved for a Czech national space mission. The mission, called Quick Ultra-Violet Kilonova surveyor - QUVIK, will provide key follow-up capabilities t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.15080v2-abstract-full').style.display = 'inline'; document.getElementById('2306.15080v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.15080v2-abstract-full" style="display: none;"> This is the first in a collection of three papers introducing the science with an ultra-violet (UV) space telescope on an approximately 130~kg small satellite with a moderately fast re-pointing capability and a real-time alert communication system approved for a Czech national space mission. The mission, called Quick Ultra-Violet Kilonova surveyor - QUVIK, will provide key follow-up capabilities to increase the discovery potential of gravitational wave observatories and future wide-field multi-wavelength surveys. The primary objective of the mission is the measurement of the UV brightness evolution of kilonovae, resulting from mergers of neutron stars, to distinguish between different explosion scenarios. The mission, which is designed to be complementary to the Ultraviolet Transient Astronomy Satellite - ULTRASAT, will also provide unique follow-up capabilities for other transients both in the near- and far-UV bands. Between the observations of transients, the satellite will target other objects described in this collection of papers, which demonstrates that a small and relatively affordable dedicated UV-space telescope can be transformative for many fields of astrophysics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.15080v2-abstract-full').style.display = 'none'; document.getElementById('2306.15080v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Space Science Reviews</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.05132">arXiv:2306.05132</a> <span> [<a href="https://arxiv.org/pdf/2306.05132">pdf</a>, <a href="https://arxiv.org/format/2306.05132">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/acd777">10.3847/2041-8213/acd777 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints on the intergalactic magnetic field using Fermi-LAT and H.E.S.S. blazar observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=S.%2C+H+E+S">H. E. S. S.</a>, <a href="/search/astro-ph?searchtype=author&query=Collaborations%2C+F">Fermi-LAT Collaborations</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Bouyahiaoui%2C+M">M. Bouyahiaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a>, <a href="/search/astro-ph?searchtype=author&query=Bylund%2C+T">T. Bylund</a>, <a href="/search/astro-ph?searchtype=author&query=Caroff%2C+S">S. Caroff</a>, <a href="/search/astro-ph?searchtype=author&query=Casanova%2C+S">S. Casanova</a>, <a href="/search/astro-ph?searchtype=author&query=Celic%2C+J">J. Celic</a>, <a href="/search/astro-ph?searchtype=author&query=Cerruti%2C+M">M. Cerruti</a>, <a href="/search/astro-ph?searchtype=author&query=Chand%2C+T">T. Chand</a>, <a href="/search/astro-ph?searchtype=author&query=Chandra%2C+S">S. Chandra</a> , et al. (113 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.05132v1-abstract-short" style="display: inline;"> Magnetic fields in galaxies and galaxy clusters are believed to be the result of the amplification of intergalactic seed fields during the formation of large-scale structures in the universe. However, the origin, strength, and morphology of this intergalactic magnetic field (IGMF) remain unknown. Lower limits on (or indirect detection of) the IGMF can be obtained from observations of high-energy g… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.05132v1-abstract-full').style.display = 'inline'; document.getElementById('2306.05132v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.05132v1-abstract-full" style="display: none;"> Magnetic fields in galaxies and galaxy clusters are believed to be the result of the amplification of intergalactic seed fields during the formation of large-scale structures in the universe. However, the origin, strength, and morphology of this intergalactic magnetic field (IGMF) remain unknown. Lower limits on (or indirect detection of) the IGMF can be obtained from observations of high-energy gamma rays from distant blazars. Gamma rays interact with the extragalactic background light to produce electron-positron pairs, which can subsequently initiate electromagnetic cascades. The $纬$-ray signature of the cascade depends on the IGMF since it deflects the pairs. Here we report on a new search for this cascade emission using a combined data set from the Fermi Large Area Telescope and the High Energy Stereoscopic System. Using state-of-the-art Monte Carlo predictions for the cascade signal, our results place a lower limit on the IGMF of $B > 7.1\times10^{-16}$ G for a coherence length of 1 Mpc even when blazar duty cycles as short as 10 yr are assumed. This improves on previous lower limits by a factor of 2. For longer duty cycles of $10^4$ ($10^7$) yr, IGMF strengths below $1.8\times10^{-14}$ G ($3.9\times10^{-14}$ G) are excluded, which rules out specific models for IGMF generation in the early universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.05132v1-abstract-full').style.display = 'none'; document.getElementById('2306.05132v1-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 7 figures, 4 tables. Accepted for publication in ApJ Letters. Auxiliary data is provided in electronic format at https://zenodo.org/record/8014311</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ Letters 2023, Volume 950, Number 2 950, L16 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.09607">arXiv:2305.09607</a> <span> [<a href="https://arxiv.org/pdf/2305.09607">pdf</a>, <a href="https://arxiv.org/format/2305.09607">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/10.1051/0004-6361/202346056">10.1051/0004-6361/202346056 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraining the cosmic-ray pressure in the inner Virgo Cluster using H.E.S.S. observations of M 87 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bradascio%2C+F">F. Bradascio</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a>, <a href="/search/astro-ph?searchtype=author&query=Bylund%2C+T">T. Bylund</a> , et al. (139 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.09607v1-abstract-short" style="display: inline;"> The origin of the gamma-ray emission from M87 is currently a matter of debate. This work aims to localize the VHE (100 GeV-100 TeV) gamma-ray emission from M87 and probe a potential extended hadronic emission component in the inner Virgo Cluster. The search for a steady and extended gamma-ray signal around M87 can constrain the cosmic-ray energy density and the pressure exerted by the cosmic rays… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.09607v1-abstract-full').style.display = 'inline'; document.getElementById('2305.09607v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.09607v1-abstract-full" style="display: none;"> The origin of the gamma-ray emission from M87 is currently a matter of debate. This work aims to localize the VHE (100 GeV-100 TeV) gamma-ray emission from M87 and probe a potential extended hadronic emission component in the inner Virgo Cluster. The search for a steady and extended gamma-ray signal around M87 can constrain the cosmic-ray energy density and the pressure exerted by the cosmic rays onto the intra-cluster medium, and allow us to investigate the role of the cosmic rays in the active galactic nucleus feedback as a heating mechanism in the Virgo Cluster. H.E.S.S. telescopes are sensitive to VHE gamma rays and have been utilized to observe M87 since 2004. We utilized a Bayesian block analysis to identify M87 emission states with H.E.S.S. observations from 2004 until 2021, dividing them into low, intermediate, and high states. Because of the causality argument, an extended ($\gtrsim$kpc) signal is allowed only in steady emission states. Hence, we fitted the morphology of the 120h low state data and found no significant gamma-ray extension. Therefore, we derived for the low state an upper limit of 58"(corresponding to $\approx$4.6kpc) in the extension of a single-component morphological model described by a rotationally symmetric 2D Gaussian model at 99.7% confidence level. Our results exclude the radio lobes ($\approx$30 kpc) as the principal component of the VHE gamma-ray emission from the low state of M87. The gamma-ray emission is compatible with a single emission region at the radio core of M87. These results, with the help of two multiple-component models, constrain the maximum cosmic-ray to thermal pressure ratio $X_{CR,max.}$$\lesssim$$0.32$ and the total energy in cosmic-ray protons (CRp) to $U_{CR}$$\lesssim$5$\times10^{58}$ erg in the inner 20kpc of the Virgo Cluster for an assumed CRp power-law distribution in momentum with spectral index $伪_{p}$=2.1. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.09607v1-abstract-full').style.display = 'none'; document.getElementById('2305.09607v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 7 figures. Accepted for publication in A&A. Corresponding authors: Victor Barbosa Martins, Stefan Ohm, Cornelia Arcaro, Natalia 呕ywucka, Mathieu de Naurois</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 675, A138 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.14482">arXiv:2304.14482</a> <span> [<a href="https://arxiv.org/pdf/2304.14482">pdf</a>, <a href="https://arxiv.org/format/2304.14482">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> ULTRASAT: A wide-field time-domain UV space telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Y. Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Waxman%2C+E">E. Waxman</a>, <a href="/search/astro-ph?searchtype=author&query=Gal-Yam%2C+A">A. Gal-Yam</a>, <a href="/search/astro-ph?searchtype=author&query=Ofek%2C+E+O">E. O. Ofek</a>, <a href="/search/astro-ph?searchtype=author&query=Ben-Ami%2C+S">S. Ben-Ami</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Kowalski%2C+M">M. Kowalski</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%BChler%2C+R">R. B眉hler</a>, <a href="/search/astro-ph?searchtype=author&query=Worm%2C+S">S. Worm</a>, <a href="/search/astro-ph?searchtype=author&query=Rhoads%2C+J+E">J. E. Rhoads</a>, <a href="/search/astro-ph?searchtype=author&query=Arcavi%2C+I">I. Arcavi</a>, <a href="/search/astro-ph?searchtype=author&query=Maoz%2C+D">D. Maoz</a>, <a href="/search/astro-ph?searchtype=author&query=Polishook%2C+D">D. Polishook</a>, <a href="/search/astro-ph?searchtype=author&query=Stone%2C+N">N. Stone</a>, <a href="/search/astro-ph?searchtype=author&query=Trakhtenbrot%2C+B">B. Trakhtenbrot</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonson%2C+O">O. Aharonson</a>, <a href="/search/astro-ph?searchtype=author&query=Birnholtz%2C+O">O. Birnholtz</a>, <a href="/search/astro-ph?searchtype=author&query=Chelouche%2C+D">D. Chelouche</a>, <a href="/search/astro-ph?searchtype=author&query=Guetta%2C+D">D. Guetta</a>, <a href="/search/astro-ph?searchtype=author&query=Hallakoun%2C+N">N. Hallakoun</a>, <a href="/search/astro-ph?searchtype=author&query=Horesh%2C+A">A. Horesh</a>, <a href="/search/astro-ph?searchtype=author&query=Kushnir%2C+D">D. Kushnir</a>, <a href="/search/astro-ph?searchtype=author&query=Mazeh%2C+T">T. Mazeh</a>, <a href="/search/astro-ph?searchtype=author&query=Nordin%2C+J">J. Nordin</a> , et al. (19 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="2304.14482v1-abstract-short" style="display: inline;"> The Ultraviolet Transient Astronomy Satellite (ULTRASAT) is scheduled to be launched to geostationary orbit in 2026. It will carry a telescope with an unprecedentedly large field of view (204 deg$^2$) and NUV (230-290nm) sensitivity (22.5 mag, 5$蟽$, at 900s). ULTRASAT will conduct the first wide-field survey of transient and variable NUV sources and will revolutionize our ability to study the hot… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.14482v1-abstract-full').style.display = 'inline'; document.getElementById('2304.14482v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.14482v1-abstract-full" style="display: none;"> The Ultraviolet Transient Astronomy Satellite (ULTRASAT) is scheduled to be launched to geostationary orbit in 2026. It will carry a telescope with an unprecedentedly large field of view (204 deg$^2$) and NUV (230-290nm) sensitivity (22.5 mag, 5$蟽$, at 900s). ULTRASAT will conduct the first wide-field survey of transient and variable NUV sources and will revolutionize our ability to study the hot transient universe: It will explore a new parameter space in energy and time-scale (months long light-curves with minutes cadence), with an extra-Galactic volume accessible for the discovery of transient sources that is $>$300 times larger than that of GALEX and comparable to that of LSST. ULTRASAT data will be transmitted to the ground in real-time, and transient alerts will be distributed to the community in $<$15 min, enabling a vigorous ground-based follow-up of ULTRASAT sources. ULTRASAT will also provide an all-sky NUV image to $>$23.5 AB mag, over 10 times deeper than the GALEX map. Two key science goals of ULTRASAT are the study of mergers of binaries involving neutron stars, and supernovae: With a large fraction ($>$50%) of the sky instantaneously accessible, fast (minutes) slewing capability and a field-of-view that covers the error ellipses expected from GW detectors beyond 2025, ULTRASAT will rapidly detect the electromagnetic emission following BNS/NS-BH mergers identified by GW detectors, and will provide continuous NUV light-curves of the events; ULTRASAT will provide early (hour) detection and continuous high (minutes) cadence NUV light curves for hundreds of core-collapse supernovae, including for rarer supernova progenitor types. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.14482v1-abstract-full').style.display = 'none'; document.getElementById('2304.14482v1-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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, 16 figures, 3 tables. Submitted to the AAS journals</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.04796">arXiv:2304.04796</a> <span> [<a href="https://arxiv.org/pdf/2304.04796">pdf</a>, <a href="https://arxiv.org/ps/2304.04796">ps</a>, <a href="https://arxiv.org/format/2304.04796">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/10.1088/1538-3873/acd8f0">10.1088/1538-3873/acd8f0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Large Array Survey Telescope -- System Overview and Performances </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ofek%2C+E+O">E. O. Ofek</a>, <a href="/search/astro-ph?searchtype=author&query=Ben-Ami%2C+S">S. Ben-Ami</a>, <a href="/search/astro-ph?searchtype=author&query=Polishook%2C+D">D. Polishook</a>, <a href="/search/astro-ph?searchtype=author&query=Segre%2C+E">E. Segre</a>, <a href="/search/astro-ph?searchtype=author&query=Blumenzweig%2C+A">A. Blumenzweig</a>, <a href="/search/astro-ph?searchtype=author&query=Strotjohann%2C+N+L">N. L. Strotjohann</a>, <a href="/search/astro-ph?searchtype=author&query=Yaron%2C+O">O. Yaron</a>, <a href="/search/astro-ph?searchtype=author&query=Shani%2C+Y+M">Y. M. Shani</a>, <a href="/search/astro-ph?searchtype=author&query=Nachshon%2C+S">S. Nachshon</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Y. Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Hershko%2C+O">O. Hershko</a>, <a href="/search/astro-ph?searchtype=author&query=Engel%2C+M">M. Engel</a>, <a href="/search/astro-ph?searchtype=author&query=Segre%2C+M">M. Segre</a>, <a href="/search/astro-ph?searchtype=author&query=Segev%2C+N">N. Segev</a>, <a href="/search/astro-ph?searchtype=author&query=Zimmerman%2C+E">E. Zimmerman</a>, <a href="/search/astro-ph?searchtype=author&query=Nir%2C+G">G. Nir</a>, <a href="/search/astro-ph?searchtype=author&query=Judkovsky%2C+Y">Y. Judkovsky</a>, <a href="/search/astro-ph?searchtype=author&query=Gal-Yam%2C+A">A. Gal-Yam</a>, <a href="/search/astro-ph?searchtype=author&query=Zackay%2C+B">B. Zackay</a>, <a href="/search/astro-ph?searchtype=author&query=Waxman%2C+E">E. Waxman</a>, <a href="/search/astro-ph?searchtype=author&query=Kushnir%2C+D">D. Kushnir</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+P">P. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Azaria%2C+R">R. Azaria</a>, <a href="/search/astro-ph?searchtype=author&query=Manulis%2C+I">I. Manulis</a>, <a href="/search/astro-ph?searchtype=author&query=Diner%2C+O">O. Diner</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="2304.04796v1-abstract-short" style="display: inline;"> The Large Array Survey Telescope (LAST) is a wide-field visible-light telescope array designed to explore the variable and transient sky with a high cadence. LAST will be composed of 48, 28-cm f/2.2 telescopes (32 already installed) equipped with full-frame backside-illuminated cooled CMOS detectors. Each telescope provides a field of view (FoV) of 7.4 deg^2 with 1.25 arcsec/pix, while the system… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.04796v1-abstract-full').style.display = 'inline'; document.getElementById('2304.04796v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.04796v1-abstract-full" style="display: none;"> The Large Array Survey Telescope (LAST) is a wide-field visible-light telescope array designed to explore the variable and transient sky with a high cadence. LAST will be composed of 48, 28-cm f/2.2 telescopes (32 already installed) equipped with full-frame backside-illuminated cooled CMOS detectors. Each telescope provides a field of view (FoV) of 7.4 deg^2 with 1.25 arcsec/pix, while the system FoV is 355 deg^2 in 2.9 Gpix. The total collecting area of LAST, with 48 telescopes, is equivalent to a 1.9-m telescope. The cost-effectiveness of the system (i.e., probed volume of space per unit time per unit cost) is about an order of magnitude higher than most existing and under-construction sky surveys. The telescopes are mounted on 12 separate mounts, each carrying four telescopes. This provides significant flexibility in operating the system. The first LAST system is under construction in the Israeli Negev Desert, with 32 telescopes already deployed. We present the system overview and performances based on the system commissioning data. The Bp 5-sigma limiting magnitude of a single 28-cm telescope is about 19.6 (21.0), in 20 s (20x20 s). Astrometric two-axes precision (rms) at the bright-end is about 60 (30)\,mas in 20\,s (20x20 s), while absolute photometric calibration, relative to GAIA, provides ~10 millimag accuracy. Relative photometric precision, in a single 20 s (320 s) image, at the bright-end measured over a time scale of about 60 min is about 3 (1) millimag. We discuss the system science goals, data pipelines, and the observatory control system in companion publications. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.04796v1-abstract-full').style.display = 'none'; document.getElementById('2304.04796v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to PASP, 15pp</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.02719">arXiv:2304.02719</a> <span> [<a href="https://arxiv.org/pdf/2304.02719">pdf</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/10.1088/1538-3873/aceb30">10.1088/1538-3873/aceb30 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Large Array Survey Telescope -- Science Goals </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ben-Ami%2C+S">S. Ben-Ami</a>, <a href="/search/astro-ph?searchtype=author&query=Ofek%2C+E+O">E. O. Ofek</a>, <a href="/search/astro-ph?searchtype=author&query=Polishook%2C+D">D. Polishook</a>, <a href="/search/astro-ph?searchtype=author&query=Franckowiak%2C+A">A. Franckowiak</a>, <a href="/search/astro-ph?searchtype=author&query=Hallakoun%2C+N">N. Hallakoun</a>, <a href="/search/astro-ph?searchtype=author&query=Segre%2C+E">E. Segre</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Y. Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Strotjohann%2C+N+L">N. L. Strotjohann</a>, <a href="/search/astro-ph?searchtype=author&query=Yaron%2C+O">O. Yaron</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonson%2C+O">O. Aharonson</a>, <a href="/search/astro-ph?searchtype=author&query=Arcavi%2C+I">I. Arcavi</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Ramazani%2C+V+F">V. Fallah Ramazani</a>, <a href="/search/astro-ph?searchtype=author&query=Gal-Yam%2C+A">A. Gal-Yam</a>, <a href="/search/astro-ph?searchtype=author&query=Garrappa%2C+S">S. Garrappa</a>, <a href="/search/astro-ph?searchtype=author&query=Hershko%2C+O">O. Hershko</a>, <a href="/search/astro-ph?searchtype=author&query=Nir%2C+G">G. Nir</a>, <a href="/search/astro-ph?searchtype=author&query=Ohm%2C+S">S. Ohm</a>, <a href="/search/astro-ph?searchtype=author&query=Rybicki%2C+K">K. Rybicki</a>, <a href="/search/astro-ph?searchtype=author&query=Segev%2C+N">N. Segev</a>, <a href="/search/astro-ph?searchtype=author&query=Shani%2C+Y+M">Y. M. Shani</a>, <a href="/search/astro-ph?searchtype=author&query=Sofer-Rimalt%2C+Y">Y. Sofer-Rimalt</a>, <a href="/search/astro-ph?searchtype=author&query=Weimann%2C+S">S. Weimann</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="2304.02719v2-abstract-short" style="display: inline;"> The Large Array Survey Telescope (LAST) is designed to survey the variable and transient sky at high temporal cadence. The array is comprised of 48 F/2.2 telescopes of 27.9cm aperture, coupled to full-frame backside-illuminated cooled CMOS detectors with $3.76$$渭$m pixels, resulting in a pixel scale of $1.25\mathrm{arcsec}$. A single telescope with a field of view of $7.4\mathrm{deg}^2$ reaches a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.02719v2-abstract-full').style.display = 'inline'; document.getElementById('2304.02719v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.02719v2-abstract-full" style="display: none;"> The Large Array Survey Telescope (LAST) is designed to survey the variable and transient sky at high temporal cadence. The array is comprised of 48 F/2.2 telescopes of 27.9cm aperture, coupled to full-frame backside-illuminated cooled CMOS detectors with $3.76$$渭$m pixels, resulting in a pixel scale of $1.25\mathrm{arcsec}$. A single telescope with a field of view of $7.4\mathrm{deg}^2$ reaches a $5蟽$ limiting magnitude of $19.6$ in $20$s. LAST 48 telescopes are mounted on 12 independent mounts -- a modular design which allows us to conduct optimized parallel surveys. Here we provide a detailed overview of the LAST survey strategy and its key scientific goals. These include the search for gravitational-wave (GW) electromagnetic counterparts with a system that can cover the uncertainty regions of the next-generation GW detectors in a single exposure, the study of planetary systems around white dwarfs, and the search for near-Earth objects. LAST is currently being commissioned, with full scientific operations expected in mid 2023. This paper is accompanied by two complementary publications in this issue, giving an overview of the system (Ofek et al. 2023a) and of the dedicated data reduction pipeline (Ofek et al. 2023b). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.02719v2-abstract-full').style.display = 'none'; document.getElementById('2304.02719v2-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> PASP 135 085002 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.02631">arXiv:2304.02631</a> <span> [<a href="https://arxiv.org/pdf/2304.02631">pdf</a>, <a href="https://arxiv.org/format/2304.02631">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/10.1051/0004-6361/202245776">10.1051/0004-6361/202245776 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detection of extended gamma-ray emission around the Geminga pulsar with H.E.S.S </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bouyahiaoui%2C+M">M. Bouyahiaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Bradascio%2C+F">F. Bradascio</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Scheidlin%2C+C+B">C. Burger Scheidlin</a>, <a href="/search/astro-ph?searchtype=author&query=Cangemi%2C+F">F. Cangemi</a> , et al. (143 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="2304.02631v1-abstract-short" style="display: inline;"> Geminga is an enigmatic radio-quiet gamma-ray pulsar located at a mere 250 pc distance from Earth. Extended very-high-energy gamma-ray emission around the pulsar was discovered by Milagro and later confirmed by HAWC, which are both water Cherenkov detector-based experiments. However, evidence for the Geminga pulsar wind nebula in gamma rays has long evaded detection by imaging atmospheric Cherenko… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.02631v1-abstract-full').style.display = 'inline'; document.getElementById('2304.02631v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.02631v1-abstract-full" style="display: none;"> Geminga is an enigmatic radio-quiet gamma-ray pulsar located at a mere 250 pc distance from Earth. Extended very-high-energy gamma-ray emission around the pulsar was discovered by Milagro and later confirmed by HAWC, which are both water Cherenkov detector-based experiments. However, evidence for the Geminga pulsar wind nebula in gamma rays has long evaded detection by imaging atmospheric Cherenkov telescopes (IACTs) despite targeted observations. The detection of gamma-ray emission on angular scales > 2 deg poses a considerable challenge for the background estimation in IACT data analysis. With recent developments in understanding the complementary background estimation techniques of water Cherenkov and atmospheric Cherenkov instruments, the H.E.S.S. IACT array can now confirm the detection of highly extended gamma-ray emission around the Geminga pulsar with a radius of at least 3 deg in the energy range 0.5-40 TeV. We find no indications for statistically significant asymmetries or energy-dependent morphology. A flux normalisation of $(2.8\pm0.7)\times10^{-12}$ cm$^{-2}$s$^{-1}$TeV$^{-1}$ at 1 TeV is obtained within a 1 deg radius region around the pulsar. To investigate the particle transport within the halo of energetic leptons around the pulsar, we fitted an electron diffusion model to the data. The normalisation of the diffusion coefficient obtained of $D_0 = 7.6^{+1.5}_{-1.2} \times 10^{27}$ cm$^2$s$^{-1}$, at an electron energy of 100 TeV, is compatible with values previously reported for the pulsar halo around Geminga, which is considerably below the Galactic average. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.02631v1-abstract-full').style.display = 'none'; document.getElementById('2304.02631v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">16 pages, 15 figures, 7 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 673, A148 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.12855">arXiv:2303.12855</a> <span> [<a href="https://arxiv.org/pdf/2303.12855">pdf</a>, <a href="https://arxiv.org/format/2303.12855">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/10.1088/1475-7516/2023/04/040">10.1088/1475-7516/2023/04/040 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for the evaporation of primordial black holes with H.E.S.S </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=collaboration%2C+H+E+S+S">H. E. S. S. collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Boettcher%2C+M">M. Boettcher</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzo%2C+R">R. Batzo</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bradascio%2C+F">F. Bradascio</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a>, <a href="/search/astro-ph?searchtype=author&query=Caro%2C+S">S. Caro</a>, <a href="/search/astro-ph?searchtype=author&query=Casanova%2C+S">S. Casanova</a>, <a href="/search/astro-ph?searchtype=author&query=Celic%2C+J">J. Celic</a> , et al. (124 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.12855v1-abstract-short" style="display: inline;"> Primordial Black Holes (PBHs) are hypothetical black holes predicted to have been formed from density fluctuations in the early Universe. PBHs with an initial mass around $10^{14}-10^{15}$g are expected to end their evaporation at present times in a burst of particles and very-high-energy (VHE) gamma rays. Those gamma rays may be detectable by the High Energy Stereoscopic System (H.E.S.S.), an arr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.12855v1-abstract-full').style.display = 'inline'; document.getElementById('2303.12855v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.12855v1-abstract-full" style="display: none;"> Primordial Black Holes (PBHs) are hypothetical black holes predicted to have been formed from density fluctuations in the early Universe. PBHs with an initial mass around $10^{14}-10^{15}$g are expected to end their evaporation at present times in a burst of particles and very-high-energy (VHE) gamma rays. Those gamma rays may be detectable by the High Energy Stereoscopic System (H.E.S.S.), an array of imaging atmospheric Cherenkov telescopes. This paper reports on the search for evaporation bursts of VHE gamma rays with H.E.S.S., ranging from 10 to 120 seconds, as expected from the final stage of PBH evaporation and using a total of 4816 hours of observations. The most constraining upper limit on the burst rate of local PBHs is $2000$ pc$^{-3}$ yr$^{-1}$ for a burst interval of 120 seconds, at the 95\% confidence level. The implication of these measurements for PBH dark matter are also discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.12855v1-abstract-full').style.display = 'none'; document.getElementById('2303.12855v1-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in JCAP, corresponding authors: F.Brun, J-F. Glicenstein, V. Marandon, T. Tavernier</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.10558">arXiv:2303.10558</a> <span> [<a href="https://arxiv.org/pdf/2303.10558">pdf</a>, <a href="https://arxiv.org/format/2303.10558">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/acc405">10.3847/2041-8213/acc405 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> H.E.S.S. follow-up observations of GRB221009A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baktash%2C+A">A. Baktash</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bouyahiaoui%2C+M">M. Bouyahiaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Bradascio%2C+F">F. Bradascio</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a> , et al. (138 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.10558v1-abstract-short" style="display: inline;"> GRB221009A is the brightest gamma-ray burst ever detected. To probe the very-high-energy (VHE, $>$\!100 GeV) emission, the High Energy Stereoscopic System (H.E.S.S.) began observations 53 hours after the triggering event, when the brightness of the moonlight no longer precluded observations. We derive differential and integral upper limits using H.E.S.S. data from the third, fourth, and ninth nigh… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.10558v1-abstract-full').style.display = 'inline'; document.getElementById('2303.10558v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.10558v1-abstract-full" style="display: none;"> GRB221009A is the brightest gamma-ray burst ever detected. To probe the very-high-energy (VHE, $>$\!100 GeV) emission, the High Energy Stereoscopic System (H.E.S.S.) began observations 53 hours after the triggering event, when the brightness of the moonlight no longer precluded observations. We derive differential and integral upper limits using H.E.S.S. data from the third, fourth, and ninth nights after the initial GRB detection, after applying atmospheric corrections. The combined observations yield an integral energy flux upper limit of $桅_\mathrm{UL}^{95\%} = 9.7 \times 10^{-12}~\mathrm{erg\,cm^{-2}\,s^{-1}}$ above $E_\mathrm{thr} = 650$ GeV. The constraints derived from the H.E.S.S. observations complement the available multiwavelength data. The radio to X-ray data are consistent with synchrotron emission from a single electron population, with the peak in the SED occurring above the X-ray band. Compared to the VHE-bright GRB190829A, the upper limits for GRB221009A imply a smaller gamma-ray to X-ray flux ratio in the afterglow. Even in the absence of a detection, the H.E.S.S. upper limits thus contribute to the multiwavelength picture of GRB221009A, effectively ruling out an IC dominated scenario. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.10558v1-abstract-full').style.display = 'none'; document.getElementById('2303.10558v1-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 4 figures. Accepted for publication in APJL. Corresponding authors: J. Damascene Mbarubucyeye, H. Ashkar, S. J. Zhu, B. Reville, F. Sch眉ssler</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.13663">arXiv:2302.13663</a> <span> [<a href="https://arxiv.org/pdf/2302.13663">pdf</a>, <a href="https://arxiv.org/format/2302.13663">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/10.1051/0004-6361/202245459">10.1051/0004-6361/202245459 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HESS J1809$-$193: a halo of escaped electrons around a pulsar wind nebula? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Borowska%2C+J">J. Borowska</a>, <a href="/search/astro-ph?searchtype=author&query=Bouyahiaoui%2C+M">M. Bouyahiaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Bradascio%2C+F">F. Bradascio</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+B">B. Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a>, <a href="/search/astro-ph?searchtype=author&query=Bylund%2C+T">T. Bylund</a>, <a href="/search/astro-ph?searchtype=author&query=Caroff%2C+S">S. Caroff</a> , et al. (130 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="2302.13663v1-abstract-short" style="display: inline;"> Context. HESS J1809$-$193 is an unassociated very-high-energy $纬$-ray source located on the Galactic plane. While it has been connected to the nebula of the energetic pulsar PSR J1809$-$1917, supernova remnants and molecular clouds present in the vicinity also constitute possible associations. Recently, the detection of $纬$-ray emission up to energies of $\sim$100 TeV with the HAWC observatory has… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.13663v1-abstract-full').style.display = 'inline'; document.getElementById('2302.13663v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.13663v1-abstract-full" style="display: none;"> Context. HESS J1809$-$193 is an unassociated very-high-energy $纬$-ray source located on the Galactic plane. While it has been connected to the nebula of the energetic pulsar PSR J1809$-$1917, supernova remnants and molecular clouds present in the vicinity also constitute possible associations. Recently, the detection of $纬$-ray emission up to energies of $\sim$100 TeV with the HAWC observatory has led to renewed interest in HESS J1809$-$193. Aims. We aim to understand the origin of the $纬$-ray emission of HESS J1809$-$193. Methods. We analysed 93.2 h of data taken on HESS J1809$-$193 above 0.27 TeV with the High Energy Stereoscopic System (H.E.S.S.), using a multi-component, three-dimensional likelihood analysis. In addition, we provide a new analysis of 12.5 yr of Fermi-LAT data above 1 GeV within the region of HESS J1809$-$193. The obtained results are interpreted in a time-dependent modelling framework. Results. For the first time, we were able to resolve the emission detected with H.E.S.S. into two components: an extended component that exhibits a spectral cut-off at $\sim$13 TeV, and a compact component that is located close to PSR J1809$-$1917 and shows no clear spectral cut-off. The Fermi-LAT analysis also revealed extended $纬$-ray emission, on scales similar to that of the extended H.E.S.S. component. Conclusions. Our modelling indicates that based on its spectrum and spatial extent, the extended H.E.S.S. component is likely caused by inverse Compton emission from old electrons that form a halo around the pulsar wind nebula. The compact component could be connected to either the pulsar wind nebula or the supernova remnant and molecular clouds. Due to its comparatively steep spectrum, modelling the Fermi-LAT emission together with the H.E.S.S. components is not straightforward. (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.13663v1-abstract-full').style.display = 'none'; document.getElementById('2302.13663v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 10 figures. Accepted for publication in A&A. Corresponding authors: Vikas Joshi, Lars Mohrmann</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 672, A103 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.09785">arXiv:2209.09785</a> <span> [<a href="https://arxiv.org/pdf/2209.09785">pdf</a>, <a href="https://arxiv.org/format/2209.09785">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/stac2686">10.1093/mnras/stac2686 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gamma-ray observations of MAXI J1820+070 during the 2018 outburst </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/astro-ph?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/astro-ph?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Baack%2C+D">D. Baack</a>, <a href="/search/astro-ph?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Baquero%2C+A">A. Baquero</a>, <a href="/search/astro-ph?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/astro-ph?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardos%2C+M">M. Bernardos</a>, <a href="/search/astro-ph?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/astro-ph?searchtype=author&query=Besenrieder%2C+J">J. Besenrieder</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharyya%2C+W">W. Bhattacharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Bigongiari%2C+C">C. Bigongiari</a> , et al. (418 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.09785v2-abstract-short" style="display: inline;"> MAXI J1820+070 is a low-mass X-ray binary with a black hole as a compact object. This binary underwent an exceptionally bright X-ray outburst from March to October 2018, showing evidence of a non-thermal particle population through its radio emission during this whole period. The combined results of 59.5 hours of observations of the MAXI J1820+070 outburst with the H.E.S.S., MAGIC and VERITAS expe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.09785v2-abstract-full').style.display = 'inline'; document.getElementById('2209.09785v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.09785v2-abstract-full" style="display: none;"> MAXI J1820+070 is a low-mass X-ray binary with a black hole as a compact object. This binary underwent an exceptionally bright X-ray outburst from March to October 2018, showing evidence of a non-thermal particle population through its radio emission during this whole period. The combined results of 59.5 hours of observations of the MAXI J1820+070 outburst with the H.E.S.S., MAGIC and VERITAS experiments at energies above 200 GeV are presented, together with Fermi-LAT data between 0.1 and 500 GeV, and multiwavelength observations from radio to X-rays. Gamma-ray emission is not detected from MAXI J1820+070, but the obtained upper limits and the multiwavelength data allow us to put meaningful constraints on the source properties under reasonable assumptions regarding the non-thermal particle population and the jet synchrotron spectrum. In particular, it is possible to show that, if a high-energy gamma-ray emitting region is present during the hard state of the source, its predicted flux should be at most a factor of 20 below the obtained Fermi-LAT upper limits, and closer to them for magnetic fields significantly below equipartition. During the state transitions, under the plausible assumption that electrons are accelerated up to ~ 500 GeV, the multiwavelength data and the gamma-ray upper limits lead consistently to the conclusion that a potential high-energy and very-high-energy gamma-ray emitting region should be located at a distance from the black hole ranging between 10^11 and 10^13 cm. Similar outbursts from low-mass X-ray binaries might be detectable in the near future with upcoming instruments such as CTA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.09785v2-abstract-full').style.display = 'none'; document.getElementById('2209.09785v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 5 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/2208.00159">arXiv:2208.00159</a> <span> [<a href="https://arxiv.org/pdf/2208.00159">pdf</a>, <a href="https://arxiv.org/format/2208.00159">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> The scientific payload of the Ultraviolet Transient Astronomy Satellite (ULTRASAT) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ben-Ami%2C+S">Sagi Ben-Ami</a>, <a href="/search/astro-ph?searchtype=author&query=Shvartzvald%2C+Y">Yossi Shvartzvald</a>, <a href="/search/astro-ph?searchtype=author&query=Waxman%2C+E">Eli Waxman</a>, <a href="/search/astro-ph?searchtype=author&query=Netzer%2C+U">Udi Netzer</a>, <a href="/search/astro-ph?searchtype=author&query=Yaniv%2C+Y">Yoram Yaniv</a>, <a href="/search/astro-ph?searchtype=author&query=Algranatti%2C+V+M">Viktor M. Algranatti</a>, <a href="/search/astro-ph?searchtype=author&query=Gal-Yam%2C+A">Avishay Gal-Yam</a>, <a href="/search/astro-ph?searchtype=author&query=Lapid%2C+O">Ofer Lapid</a>, <a href="/search/astro-ph?searchtype=author&query=Ofek%2C+E">Eran Ofek</a>, <a href="/search/astro-ph?searchtype=author&query=Topaz%2C+J">Jeremy Topaz</a>, <a href="/search/astro-ph?searchtype=author&query=Arcavi%2C+I">Iair Arcavi</a>, <a href="/search/astro-ph?searchtype=author&query=Asif%2C+A">Arooj Asif</a>, <a href="/search/astro-ph?searchtype=author&query=Azaria%2C+S">Shlomi Azaria</a>, <a href="/search/astro-ph?searchtype=author&query=Bahalul%2C+E">Eran Bahalul</a>, <a href="/search/astro-ph?searchtype=author&query=Barschke%2C+M+F">Merlin F. Barschke</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian-Querner%2C+B">Benjamin Bastian-Querner</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">David Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Berlea%2C+V+D">Vlad D. Berlea</a>, <a href="/search/astro-ph?searchtype=author&query=Buhler%2C+R">Rolf Buhler</a>, <a href="/search/astro-ph?searchtype=author&query=Dittmar%2C+L">Louise Dittmar</a>, <a href="/search/astro-ph?searchtype=author&query=Gelman%2C+A">Anatoly Gelman</a>, <a href="/search/astro-ph?searchtype=author&query=Giavitto%2C+G">Gianluca Giavitto</a>, <a href="/search/astro-ph?searchtype=author&query=Guttman%2C+O">Or Guttman</a>, <a href="/search/astro-ph?searchtype=author&query=Crespo%2C+J+M+H">Juan M. Haces Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Heilbrunn%2C+D">Daniel Heilbrunn</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="2208.00159v2-abstract-short" style="display: inline;"> The Ultraviolet Transient Astronomy Satellite (ULTRASAT) is a space-borne near UV telescope with an unprecedented large field of view (200 sq. deg.). The mission, led by the Weizmann Institute of Science and the Israel Space Agency in collaboration with DESY (Helmholtz association, Germany) and NASA (USA), is fully funded and expected to be launched to a geostationary transfer orbit in Q2/3 of 202… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.00159v2-abstract-full').style.display = 'inline'; document.getElementById('2208.00159v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.00159v2-abstract-full" style="display: none;"> The Ultraviolet Transient Astronomy Satellite (ULTRASAT) is a space-borne near UV telescope with an unprecedented large field of view (200 sq. deg.). The mission, led by the Weizmann Institute of Science and the Israel Space Agency in collaboration with DESY (Helmholtz association, Germany) and NASA (USA), is fully funded and expected to be launched to a geostationary transfer orbit in Q2/3 of 2025. With a grasp 300 times larger than GALEX, the most sensitive UV satellite to date, ULTRASAT will revolutionize our understanding of the hot transient universe, as well as of flaring galactic sources. We describe the mission payload, the optical design and the choice of materials allowing us to achieve a point spread function of ~10arcsec across the FoV, and the detector assembly. We detail the mitigation techniques implemented to suppress out-of-band flux and reduce stray light, detector properties including measured quantum efficiency of scout (prototype) detectors, and expected performance (limiting magnitude) for various objects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.00159v2-abstract-full').style.display = 'none'; document.getElementById('2208.00159v2-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 July, 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">Presented in the SPIE Astronomical Telescopes + Instrumentation 2022</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.10921">arXiv:2207.10921</a> <span> [<a href="https://arxiv.org/pdf/2207.10921">pdf</a>, <a href="https://arxiv.org/format/2207.10921">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/10.1051/0004-6361/202244323">10.1051/0004-6361/202244323 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A deep spectromorphological study of the $纬$-ray emission surrounding the young massive stellar cluster Westerlund 1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Bradascio%2C+F">F. Bradascio</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Burger-Scheidlin%2C+C">C. Burger-Scheidlin</a>, <a href="/search/astro-ph?searchtype=author&query=Cangemi%2C+F">F. Cangemi</a>, <a href="/search/astro-ph?searchtype=author&query=Caroff%2C+S">S. Caroff</a>, <a href="/search/astro-ph?searchtype=author&query=Casanova%2C+S">S. Casanova</a>, <a href="/search/astro-ph?searchtype=author&query=Cerruti%2C+M">M. Cerruti</a>, <a href="/search/astro-ph?searchtype=author&query=Chand%2C+T">T. Chand</a>, <a href="/search/astro-ph?searchtype=author&query=Chandra%2C+S">S. Chandra</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+A">A. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chibueze%2C+O">O. Chibueze</a>, <a href="/search/astro-ph?searchtype=author&query=Cristofari%2C+P">P. Cristofari</a>, <a href="/search/astro-ph?searchtype=author&query=Mbarubucyeye%2C+J+D">J. Damascene Mbarubucyeye</a>, <a href="/search/astro-ph?searchtype=author&query=Djannati-Ata%C3%AF%2C+A">A. Djannati-Ata茂</a> , et al. (134 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2207.10921v2-abstract-short" style="display: inline;"> Young massive stellar clusters are extreme environments and potentially provide the means for efficient particle acceleration. Indeed, they are increasingly considered as being responsible for a significant fraction of cosmic rays (CRs) accelerated within the Milky Way. Westerlund 1, the most massive known young stellar cluster in our Galaxy is a prime candidate for studying this hypothesis. While… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.10921v2-abstract-full').style.display = 'inline'; document.getElementById('2207.10921v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.10921v2-abstract-full" style="display: none;"> Young massive stellar clusters are extreme environments and potentially provide the means for efficient particle acceleration. Indeed, they are increasingly considered as being responsible for a significant fraction of cosmic rays (CRs) accelerated within the Milky Way. Westerlund 1, the most massive known young stellar cluster in our Galaxy is a prime candidate for studying this hypothesis. While the very-high-energy $纬$-ray source HESS J1646-458 has been detected in the vicinity of Westerlund 1 in the past, its association could not be firmly identified. We aim to identify the physical processes responsible for the $纬$-ray emission around Westerlund 1 and thus to better understand the role of massive stellar clusters in the acceleration of Galactic CRs. Using 164 hours of data recorded with the High Energy Stereoscopic System (H.E.S.S.), we carried out a deep spectromorphological study of the $纬$-ray emission of HESS J1646-458. We furthermore employed H I and CO observations of the region to infer the presence of gas that could serve as target material for interactions of accelerated CRs. We detected large-scale ($\sim 2^\circ$ diameter) $纬$-ray emission with a complex morphology, exhibiting a shell-like structure and showing no significant variation with $纬$-ray energy. The combined energy spectrum of the emission extends to several tens of TeV, and is uniform across the entire source region. We did not find a clear correlation of the $纬$-ray emission with gas clouds as identified through H I and CO observations. We conclude that, of the known objects within the region, only Westerlund 1 can explain the bulk of the $纬$-ray emission. Several CR acceleration sites and mechanisms are conceivable, and discussed in detail. (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.10921v2-abstract-full').style.display = 'none'; document.getElementById('2207.10921v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 9 figures. Corresponding authors: L. Mohrmann, S. Ohm, R. Rauth, A. Specovius. v2: corrected affiliation of M. Vecchi (still incorrect in journal version)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 666, A124 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.10471">arXiv:2207.10471</a> <span> [<a href="https://arxiv.org/pdf/2207.10471">pdf</a>, <a href="https://arxiv.org/format/2207.10471">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/10.1103/PhysRevLett.129.111101">10.1103/PhysRevLett.129.111101 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for dark matter annihilation signals in the H.E.S.S. Inner Galaxy Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Anguner%2C+E+O">E. O. Anguner</a>, <a href="/search/astro-ph?searchtype=author&query=Armand%2C+C">C. Armand</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernlohr%2C+K">K. Bernlohr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Bottcher%2C+M">M. Bottcher</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Cangemi%2C+F">F. Cangemi</a>, <a href="/search/astro-ph?searchtype=author&query=Caroff%2C+S">S. Caroff</a>, <a href="/search/astro-ph?searchtype=author&query=Cerruti%2C+M">M. Cerruti</a>, <a href="/search/astro-ph?searchtype=author&query=Chand%2C+T">T. Chand</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+A">A. Chen</a> , et al. (116 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2207.10471v1-abstract-short" style="display: inline;"> The central region of the Milky Way is one of the foremost locations to look for dark matter (DM) signatures. We report the first results on a search for DM particle annihilation signals using new observations from an unprecedented gamma-ray survey of the Galactic Center (GC) region, ${\it i.e.}$, the Inner Galaxy Survey, at very high energies ($\gtrsim$ 100 GeV) performed with the H.E.S.S. array… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.10471v1-abstract-full').style.display = 'inline'; document.getElementById('2207.10471v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.10471v1-abstract-full" style="display: none;"> The central region of the Milky Way is one of the foremost locations to look for dark matter (DM) signatures. We report the first results on a search for DM particle annihilation signals using new observations from an unprecedented gamma-ray survey of the Galactic Center (GC) region, ${\it i.e.}$, the Inner Galaxy Survey, at very high energies ($\gtrsim$ 100 GeV) performed with the H.E.S.S. array of five ground-based Cherenkov telescopes. No significant gamma-ray excess is found in the search region of the 2014-2020 dataset and a profile likelihood ratio analysis is carried out to set exclusion limits on the annihilation cross section $\langle 蟽v\rangle$. Assuming Einasto and Navarro-Frenk-White (NFW) DM density profiles at the GC, these constraints are the strongest obtained so far in the TeV DM mass range. For the Einasto profile, the constraints reach $\langle 蟽v\rangle$ values of $\rm 3.7\times10^{-26} cm^3s^{-1}$ for 1.5 TeV DM mass in the $W^+W^-$ annihilation channel, and $\rm 1.2 \times 10^{-26} cm^3s^{-1}$ for 0.7 TeV DM mass in the $蟿^+蟿^-$ annihilation channel. With the H.E.S.S. Inner Galaxy Survey, ground-based $纬$-ray observations thus probe $\langle 蟽v\rangle$ values expected from thermal-relic annihilating TeV DM particles. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.10471v1-abstract-full').style.display = 'none'; document.getElementById('2207.10471v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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 in Phys. Rev. Lett., includes Supplemental materials. 5+10 pages, 2+8 figures, 4 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 129, 111101 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.01325">arXiv:2204.01325</a> <span> [<a href="https://arxiv.org/pdf/2204.01325">pdf</a>, <a href="https://arxiv.org/format/2204.01325">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/10.1088/1475-7516/2022/08/013">10.1088/1475-7516/2022/08/013 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Introducing the MeVCube concept: a CubeSat for MeV observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lucchetta%2C+G">Giulio Lucchetta</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">Markus Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">David Berge</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%BChler%2C+R">Rolf B眉hler</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.01325v2-abstract-short" style="display: inline;"> Despite the impressive progress achieved both by X-ray and gamma-ray observatories in the last few decades, the energy range between $\sim200\;\mathrm{keV}$ and $\sim50\;\mathrm{MeV}$ remains poorly explored. COMPTEL, on-board the Compton Gamma-Ray Observatory (CGRO, $1991$-$2000$), opened the MeV gamma-ray band as a new window to astronomy, performing the first all-sky survey in the energy range… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.01325v2-abstract-full').style.display = 'inline'; document.getElementById('2204.01325v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.01325v2-abstract-full" style="display: none;"> Despite the impressive progress achieved both by X-ray and gamma-ray observatories in the last few decades, the energy range between $\sim200\;\mathrm{keV}$ and $\sim50\;\mathrm{MeV}$ remains poorly explored. COMPTEL, on-board the Compton Gamma-Ray Observatory (CGRO, $1991$-$2000$), opened the MeV gamma-ray band as a new window to astronomy, performing the first all-sky survey in the energy range from $0.75$ to $30\;\mathrm{MeV}$. More than $20$ years after the de-orbit of CGRO, no successor mission is yet operating. Over the past years many concepts have been proposed, for new observatories exploring different configurations and imaging techniques; a selection of the most recent ones includes AMEGO, ETCC, GECCO and COSI. We propose here a novel concept for a Compton telescope based on the CubeSat standard, named MeVCube, with the advantages of small cost and relatively short development time. The scientific payload is based on two layers of pixelated Cadmium-Zinc-Telluride (CdZnTe) detectors, coupled with low-power read-out electronics (ASIC, VATA450.3). The performance of the read-out electronics and CdZnTe custom designed detectors have been measured extensively at DESY. The performance of the telescope is accessed through simulations: despite a small effective area limited to a few $\mathrm{cm}^{2}$, MeVCube can reach an angular resolution of $1.5^{\circ}$ and a sensitivity comparable to the one achieved by the last generation of large-scale satellites like COMPTEL and INTEGRAL. Combined with a large field-of-view and a moderate cost, MeVCube can be a powerful instrument for transient observations and searches of electromagnetic counterparts of gravitational wave events. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.01325v2-abstract-full').style.display = 'none'; document.getElementById('2204.01325v2-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in JCAP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.00475">arXiv:2204.00475</a> <span> [<a href="https://arxiv.org/pdf/2204.00475">pdf</a>, <a href="https://arxiv.org/format/2204.00475">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/10.1088/1748-0221/17/08/P08004">10.1088/1748-0221/17/08/P08004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterization of a CdZnTe detector for a low-power CubeSat application </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lucchetta%2C+G">Giulio Lucchetta</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">Markus Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">David Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bloch%2C+I">Ingo Bloch</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%BChler%2C+R">Rolf B眉hler</a>, <a href="/search/astro-ph?searchtype=author&query=Kolanoski%2C+H">Hermann Kolanoski</a>, <a href="/search/astro-ph?searchtype=author&query=Lange%2C+W">Wolfgang Lange</a>, <a href="/search/astro-ph?searchtype=author&query=Zappon%2C+F">Francesco Zappon</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.00475v2-abstract-short" style="display: inline;"> We report spectral and imaging performance of a pixelated CdZnTe detector custom designed for the \emph{MeVCube} project: a small Compton telescope on a CubeSat platform. \emph{MeVCube} is expected to cover the energy range between $200\;\mathrm{keV}$ and $4\;\mathrm{MeV}$, with performance comparable to the last generation of larger satellites. In order to achieve this goal, an energy resolution… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.00475v2-abstract-full').style.display = 'inline'; document.getElementById('2204.00475v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.00475v2-abstract-full" style="display: none;"> We report spectral and imaging performance of a pixelated CdZnTe detector custom designed for the \emph{MeVCube} project: a small Compton telescope on a CubeSat platform. \emph{MeVCube} is expected to cover the energy range between $200\;\mathrm{keV}$ and $4\;\mathrm{MeV}$, with performance comparable to the last generation of larger satellites. In order to achieve this goal, an energy resolution of few percent in full width at half maximum (FWHM) and a $3$-D spatial resolution of few millimeters for the individual detectors are needed. The severe power constraints present in small satellites require very low power read-out electronics for the detector. Our read-out is based on the VATA450.3 ASIC developed by \emph{Ideas}, with a power consumption of only $0.25\;\mathrm{mW/channel}$, which exhibits good performance in terms of dynamic range, noise and linearity. A $2.0\;\mathrm{cm} \times 2.0\;\mathrm{cm} \times 1.5\;\mathrm{cm}$ CdZnTe detector, with a custom $8 \times 8$ pixel anode structure read-out by a VATA450.3 ASIC, has been tested. A preliminary read-out system for the cathode, based on a discrete \emph{Amptek} A250F charge sensitive pre-amplifier and a DRS4 ASIC, has been implemented. An energy resolution around $3\%$ FWHM has been measured at a gamma energy of $662\;\mathrm{keV}$; at $200\;\mathrm{keV}$ the average energy resolution is $6.5\%$, decreasing to $\lesssim 2\%$ at energies above $1\;\mathrm{MeV}$. A $3$-D spatial resolution of $\approx 2\,\mathrm{mm}$ is achieved. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.00475v2-abstract-full').style.display = 'none'; document.getElementById('2204.00475v2-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accpted for publication in JINST</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.05458">arXiv:2203.05458</a> <span> [<a href="https://arxiv.org/pdf/2203.05458">pdf</a>, <a href="https://arxiv.org/format/2203.05458">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/10.1051/0004-6361/202243092">10.1051/0004-6361/202243092 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The H.E.S.S. transients follow-up system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hoischen%2C+C">C. Hoischen</a>, <a href="/search/astro-ph?searchtype=author&query=F%C3%BC%C3%9Fling%2C+M">M. F眉脽ling</a>, <a href="/search/astro-ph?searchtype=author&query=Ohm%2C+S">S. Ohm</a>, <a href="/search/astro-ph?searchtype=author&query=Balzer%2C+A">A. Balzer</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Hofverberg%2C+P">P. Hofverberg</a>, <a href="/search/astro-ph?searchtype=author&query=Holch%2C+T+L">T. L. Holch</a>, <a href="/search/astro-ph?searchtype=author&query=Murach%2C+T">T. Murach</a>, <a href="/search/astro-ph?searchtype=author&query=Prokoph%2C+H">H. Prokoph</a>, <a href="/search/astro-ph?searchtype=author&query=Sch%C3%BCssler%2C+F">F. Sch眉ssler</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+S+J">S. J. Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Egberts%2C+K">K. Egberts</a>, <a href="/search/astro-ph?searchtype=author&query=Stegmann%2C+C">C. Stegmann</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.05458v2-abstract-short" style="display: inline;"> Observations of astrophysical transients have brought many novel discoveries and provided new insights into physical processes at work under extreme conditions in the Universe. Multi-wavelength and multi-messenger observations of variable objects require dedicated procedures and follow-up systems capable of digesting and reacting to external alerts to execute coordinated follow-up campaigns. The m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.05458v2-abstract-full').style.display = 'inline'; document.getElementById('2203.05458v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.05458v2-abstract-full" style="display: none;"> Observations of astrophysical transients have brought many novel discoveries and provided new insights into physical processes at work under extreme conditions in the Universe. Multi-wavelength and multi-messenger observations of variable objects require dedicated procedures and follow-up systems capable of digesting and reacting to external alerts to execute coordinated follow-up campaigns. The main functions of such follow-up systems are the processing, filtering, and ranking of the incoming alerts, the fully automated rapid execution of the observations according to an observation strategy tailored to the instrument, and real-time data analysis with feedback to the operators and other instruments. H.E.S.S. has been searching for transient phenomena since its inauguration in 2003. In this paper, we describe the transients follow-up system of H.E.S.S. which became operational in 2016. The system allows H.E.S.S. to conduct a more versatile, optimised, and largely autonomous transient follow-up program, combining all major functionalities in one systematic approach. We describe the design, central functionalities, and interfaces of the follow-up system in general and its three main components in detail: the Target of Opportunity (ToO) alert system, the data acquisition and central control system, and the real-time analysis. We highlight architectural decisions and features that enable fully automatic ToO follow-up and indicate key performance metrics of the sub-systems. We discuss the system's capabilities and highlight the need for a fine-tuned interplay of the different sub-systems in order to react quickly and reliably. Lessons learned from the development, integration, and operation of the follow-up system are reviewed in light of new and large science infrastructures and associated challenges in this exciting new era of inter-operable astronomy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.05458v2-abstract-full').style.display = 'none'; document.getElementById('2203.05458v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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">18 pages, 10 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 666, A119 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.08201">arXiv:2202.08201</a> <span> [<a href="https://arxiv.org/pdf/2202.08201">pdf</a>, <a href="https://arxiv.org/format/2202.08201">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/10.1126/science.abn0567">10.1126/science.abn0567 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Time-resolved hadronic particle acceleration in the recurrent Nova RS Ophiuchi </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Caroff%2C+S">S. Caroff</a>, <a href="/search/astro-ph?searchtype=author&query=Casanova%2C+S">S. Casanova</a>, <a href="/search/astro-ph?searchtype=author&query=Cerruti%2C+M">M. Cerruti</a>, <a href="/search/astro-ph?searchtype=author&query=Chand%2C+T">T. Chand</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+A">A. Chen</a> , et al. (150 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="2202.08201v2-abstract-short" style="display: inline;"> Recurrent Novae are repeating thermonuclear explosions in the outer layers of white dwarfs, due to the accretion of fresh material from a binary companion. The shock generated by ejected material slamming into the companion star's wind, accelerates particles to very-high-energies. We report very-high-energy (VHE, $\gtrsim100$\,GeV) gamma rays from the recurrent nova RS\,Ophiuchi up to a month afte… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.08201v2-abstract-full').style.display = 'inline'; document.getElementById('2202.08201v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.08201v2-abstract-full" style="display: none;"> Recurrent Novae are repeating thermonuclear explosions in the outer layers of white dwarfs, due to the accretion of fresh material from a binary companion. The shock generated by ejected material slamming into the companion star's wind, accelerates particles to very-high-energies. We report very-high-energy (VHE, $\gtrsim100$\,GeV) gamma rays from the recurrent nova RS\,Ophiuchi up to a month after its 2021 outburst, using the High Energy Stereoscopic System. The VHE emission has a similar temporal profile to lower-energy GeV emission, indicating a common origin, with a two-day delay in peak flux. These observations constrain models of time-dependent particle energization, favouring a hadronic emission scenario over the leptonic alternative. This confirms that shocks in dense winds provide favourable environments for efficient cosmic-ray acceleration to very-high-energies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.08201v2-abstract-full').style.display = 'none'; document.getElementById('2202.08201v2-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 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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">Submitted 1st Nov. 2021, first release 10th March 2022 (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/2201.05839">arXiv:2201.05839</a> <span> [<a href="https://arxiv.org/pdf/2201.05839">pdf</a>, <a href="https://arxiv.org/ps/2201.05839">ps</a>, <a href="https://arxiv.org/format/2201.05839">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 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/10.1051/0004-6361/202243096">10.1051/0004-6361/202243096 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evidence for gamma-ray emission from the remnant of Kepler's supernova based on deep H.E.S.S. observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Anguner%2C+E+O">E. O. Anguner</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernloehr%2C+K">K. Bernloehr</a>, <a href="/search/astro-ph?searchtype=author&query=Boettcher%2C+M">M. Boettcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Bylund%2C+T">T. Bylund</a>, <a href="/search/astro-ph?searchtype=author&query=Cangemi%2C+F">F. Cangemi</a>, <a href="/search/astro-ph?searchtype=author&query=Caroff%2C+S">S. Caroff</a>, <a href="/search/astro-ph?searchtype=author&query=Casanova%2C+S">S. Casanova</a>, <a href="/search/astro-ph?searchtype=author&query=Cerruti%2C+M">M. Cerruti</a>, <a href="/search/astro-ph?searchtype=author&query=Chand%2C+T">T. Chand</a> , et al. (136 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.05839v3-abstract-short" style="display: inline;"> Observations with imaging atmospheric Cherenkov telescopes (IACTs) have enhanced our knowledge of nearby supernova (SN) remnants with ages younger than 500 years by establishing Cassiopeia A and the remnant of Tycho's SN as very-high-energy (VHE) gamma-ray sources. The remnant of Kepler's SN, which is the product of the most recent naked-eye supernova in our Galaxy, is comparable in age to the oth… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.05839v3-abstract-full').style.display = 'inline'; document.getElementById('2201.05839v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.05839v3-abstract-full" style="display: none;"> Observations with imaging atmospheric Cherenkov telescopes (IACTs) have enhanced our knowledge of nearby supernova (SN) remnants with ages younger than 500 years by establishing Cassiopeia A and the remnant of Tycho's SN as very-high-energy (VHE) gamma-ray sources. The remnant of Kepler's SN, which is the product of the most recent naked-eye supernova in our Galaxy, is comparable in age to the other two, but is significantly more distant. If the gamma-ray luminosities of the remnants of Tycho's and Kepler's SNe are similar, then the latter is expected to be one of the faintest gamma-ray sources within reach of the current generation IACT arrays. Here we report evidence at a statistical level of 4.6 sigma for a VHE signal from the remnant of Kepler's SN based on deep observations by the High Energy Stereoscopic System (H.E.S.S.) with an exposure of 152 hours. The measured integral flux above an energy of 226 GeV is ~0.3% of the flux of the Crab Nebula. The spectral energy distribution (SED) reveals a gamma-ray emitting component connecting the VHE emission observed with H.E.S.S. to the emission observed at GeV energies with Fermi-LAT. The overall SED is similar to that of the remnant of Tycho's SN, possibly indicating the same non-thermal emission processes acting in both these young remnants of thermonuclear SNe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.05839v3-abstract-full').style.display = 'none'; document.getElementById('2201.05839v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in Astronomy and Astrophysics. A typo in the normalization constant in Sect. 4 was corrected</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 662, A65 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.00069">arXiv:2201.00069</a> <span> [<a href="https://arxiv.org/pdf/2201.00069">pdf</a>, <a href="https://arxiv.org/format/2201.00069">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stac1601">10.1093/mnras/stac1601 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A MeerKAT, e-MERLIN, H.E.S.S. and Swift search for persistent and transient emission associated with three localised FRBs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chibueze%2C+J+O">James O. Chibueze</a>, <a href="/search/astro-ph?searchtype=author&query=Caleb%2C+M">M. Caleb</a>, <a href="/search/astro-ph?searchtype=author&query=Spitler%2C+L">L. Spitler</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Schussler%2C+F">F. Schussler</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=Venter%2C+C">C. Venter</a>, <a href="/search/astro-ph?searchtype=author&query=Heywood%2C+I">I. Heywood</a>, <a href="/search/astro-ph?searchtype=author&query=Richards%2C+A+M+S">A. M. S. Richards</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+D+R+A">D. R. A. Williams</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">M. Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Beswick%2C+R">R. Beswick</a>, <a href="/search/astro-ph?searchtype=author&query=Bezuidenhout%2C+M+C">M. C. Bezuidenhout</a>, <a href="/search/astro-ph?searchtype=author&query=Breton%2C+R+P">R. P. Breton</a>, <a href="/search/astro-ph?searchtype=author&query=Driessen%2C+L+N">L. N. Driessen</a>, <a href="/search/astro-ph?searchtype=author&query=Jankowski%2C+F">F. Jankowski</a>, <a href="/search/astro-ph?searchtype=author&query=Keane%2C+E+F">E. F. Keane</a>, <a href="/search/astro-ph?searchtype=author&query=Malenta%2C+M">M. Malenta</a>, <a href="/search/astro-ph?searchtype=author&query=Mickaliger%2C+M">M. Mickaliger</a>, <a href="/search/astro-ph?searchtype=author&query=Morello%2C+V">V. Morello</a>, <a href="/search/astro-ph?searchtype=author&query=Qiu%2C+H">H. Qiu</a>, <a href="/search/astro-ph?searchtype=author&query=Rajwade%2C+K">K. Rajwade</a>, <a href="/search/astro-ph?searchtype=author&query=Sanidas%2C+S">S. Sanidas</a>, <a href="/search/astro-ph?searchtype=author&query=Surnis%2C+M">M. Surnis</a>, <a href="/search/astro-ph?searchtype=author&query=Scragg%2C+T+W">T. W. Scragg</a> , et al. (134 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.00069v1-abstract-short" style="display: inline;"> We report on a search for persistent radio emission from the one-off Fast Radio Burst (FRB) 20190714A, as well as from two repeating FRBs, 20190711A and 20171019A, using the MeerKAT radio telescope. For FRB 20171019A we also conducted simultaneous observations with the High Energy Stereoscopic System (H.E.S.S.) in very high energy gamma rays and searched for signals in the ultraviolet, optical, an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.00069v1-abstract-full').style.display = 'inline'; document.getElementById('2201.00069v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.00069v1-abstract-full" style="display: none;"> We report on a search for persistent radio emission from the one-off Fast Radio Burst (FRB) 20190714A, as well as from two repeating FRBs, 20190711A and 20171019A, using the MeerKAT radio telescope. For FRB 20171019A we also conducted simultaneous observations with the High Energy Stereoscopic System (H.E.S.S.) in very high energy gamma rays and searched for signals in the ultraviolet, optical, and X-ray bands. For this FRB, we obtain a UV flux upper limit of 1.39x10^-16 erg/cm^-2/s/Amstrong, X-ray limit of ~ 6.6x10^-14 erg/cm^-2/s and a limit on the very-high-energy gamma-ray flux (Phi) (E > 120 GeV) < 1.7 x 10^-12 erg/cm^-2/s. We obtain a radio upper limit of ~15 microJy/beam for persistent emission at the locations of both FRBs 20190711A and 20171019A, but detect diffuse radio emission with a peak brightness of ~53 microJy/beam associated with FRB 20190714A at z = 0.2365. This represents the first detection of the radio continuum emission potentially associated with the host (galaxy) of FRB 20190714A, and is only the third known FRB to have such an association. Given the possible association of a faint persistent source, FRB 20190714A may potentially be a repeating FRB whose age lies between that of FRB 20121102A and FRB 20180916A. A parallel search for repeat bursts from these FRBs revealed no new detections down to a fluence of 0.08 Jy ms for a 1 ms duration burst. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.00069v1-abstract-full').style.display = 'none'; document.getElementById('2201.00069v1-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 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 9 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.08307">arXiv:2112.08307</a> <span> [<a href="https://arxiv.org/pdf/2112.08307">pdf</a>, <a href="https://arxiv.org/format/2112.08307">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/ac2e04">10.3847/1538-4357/ac2e04 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> H.E.S.S. follow-up observations of Binary Black Hole Coalescence events during the second and third Gravitational Waves observing runs of Advanced LIGO and Advanced Virgo </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=collaboration%2C+H+E+S+S">H. E. S. S. collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Batzofin%2C+R">R. Batzofin</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bulik%2C+T">T. Bulik</a>, <a href="/search/astro-ph?searchtype=author&query=Bylund%2C+T">T. Bylund</a>, <a href="/search/astro-ph?searchtype=author&query=Cangemi%2C+F">F. Cangemi</a>, <a href="/search/astro-ph?searchtype=author&query=Caroff%2C+S">S. Caroff</a> , et al. (129 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2112.08307v1-abstract-short" style="display: inline;"> We report on the observations of four well-localized binary black hole (BBH) mergers by the High Energy Stereoscopic System (H.E.S.S.) during the second and third observing runs of Advanced LIGO and Advanced Virgo, O2 and O3. H.E.S.S. can observe $\mathrm{20\,deg^2}$ of the sky at a time and follows up gravitational-wave (GW) events by ``tiling'' localization regions to maximize the covered locali… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.08307v1-abstract-full').style.display = 'inline'; document.getElementById('2112.08307v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.08307v1-abstract-full" style="display: none;"> We report on the observations of four well-localized binary black hole (BBH) mergers by the High Energy Stereoscopic System (H.E.S.S.) during the second and third observing runs of Advanced LIGO and Advanced Virgo, O2 and O3. H.E.S.S. can observe $\mathrm{20\,deg^2}$ of the sky at a time and follows up gravitational-wave (GW) events by ``tiling'' localization regions to maximize the covered localization probability. During O2 and O3, H.E.S.S. observed large portions of the localization regions, between 35\% and 75\%, for four BBH mergers (GW170814, GW190512\_180714, GW190728\_064510, and S200224ca). For these four GW events, we find no significant signal from a pointlike source in any of the observations, and set upper limits on the very high energy ($>$100 GeV) $纬$-ray emission. The 1-10 TeV isotropic luminosity of these GW events is below $10^{45}$ erg s$^{-1}$ at the times of the H.E.S.S. observations, around the level of the low-luminosity GRB 190829A. Assuming no changes are made to how follow-up observations are conducted, H.E.S.S. can expect to observe over 60 GW events per year in the fourth GW observing run, O4, of which eight would be observable with minimal latency. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.08307v1-abstract-full').style.display = 'none'; document.getElementById('2112.08307v1-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ, 923, 109 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.00636">arXiv:2110.00636</a> <span> [<a href="https://arxiv.org/pdf/2110.00636">pdf</a>, <a href="https://arxiv.org/format/2110.00636">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/ac0fe1">10.3847/1538-4357/ac0fe1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searching for TeV gamma-ray emission from SGR\,1935+2154 during its 2020 X-ray and radio bursting phase </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%7Funer%2C+E+O">E. O. Anguner</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Armand%2C+C">C. Armand</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+M">M. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%7Fohr%2C+K">K. Bernlohr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%7Fottcher%2C+M">M. Bottcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a> , et al. (230 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2110.00636v1-abstract-short" style="display: inline;"> Magnetar hyperflares are the most plausible explanation for fast radio bursts (FRB) -- enigmatic powerful radio pulses with durations of several milliseconds and high brightness temperatures. The first observational evidence for this scenario was obtained in 2020 April when a FRB was detected from the direction of the Galactic magnetar and soft gamma-ray repeater SGR\,1935+2154. The FRB was preced… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.00636v1-abstract-full').style.display = 'inline'; document.getElementById('2110.00636v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.00636v1-abstract-full" style="display: none;"> Magnetar hyperflares are the most plausible explanation for fast radio bursts (FRB) -- enigmatic powerful radio pulses with durations of several milliseconds and high brightness temperatures. The first observational evidence for this scenario was obtained in 2020 April when a FRB was detected from the direction of the Galactic magnetar and soft gamma-ray repeater SGR\,1935+2154. The FRB was preceded by two gamma-ray outburst alerts by the BAT instrument aboard the Swift satellite, which triggered follow-up observations by the High Energy Stereoscopic System (H.E.S.S.). H.E.S.S. has observed SGR\,1935+2154 for 2 hr on 2020 April 28. The observations are coincident with X-ray bursts from the magnetar detected by INTEGRAL and Fermi-GBM, thus providing the first very high energy (VHE) gamma-ray observations of a magnetar in a flaring state. High-quality data acquired during these follow-up observations allow us to perform a search for short-time transients. No significant signal at energies $E>0.6$~TeV is found and upper limits on the persistent and transient emission are derived. We here present the analysis of these observations and discuss the obtained results and prospects of the H.E.S.S. follow-up program for soft gamma-ray repeaters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.00636v1-abstract-full').style.display = 'none'; document.getElementById('2110.00636v1-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 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Received 2021 June 13; accepted 2021 June 28; published 2021 September 29</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.11894">arXiv:2109.11894</a> <span> [<a href="https://arxiv.org/pdf/2109.11894">pdf</a>, <a href="https://arxiv.org/format/2109.11894">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/ac29b7">10.3847/1538-4357/ac29b7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observation of the gamma-ray binary HESS J0632+057 with the H.E.S.S., MAGIC, and VERITAS telescopes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C+B">C. B. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Brill%2C+A">A. Brill</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Capasso%2C+M">M. Capasso</a>, <a href="/search/astro-ph?searchtype=author&query=Chromey%2C+A+J">A. J. Chromey</a>, <a href="/search/astro-ph?searchtype=author&query=Errando%2C+M">M. Errando</a>, <a href="/search/astro-ph?searchtype=author&query=Falcone%2C+A">A. Falcone</a>, <a href="/search/astro-ph?searchtype=author&query=Farrell%2C+K+A">K. A. Farrell</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+Q">Q. Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Finley%2C+J+P">J P. Finley</a>, <a href="/search/astro-ph?searchtype=author&query=Foote%2C+G">G. Foote</a>, <a href="/search/astro-ph?searchtype=author&query=Fortson%2C+L">L. Fortson</a>, <a href="/search/astro-ph?searchtype=author&query=Furniss%2C+A">A. Furniss</a>, <a href="/search/astro-ph?searchtype=author&query=Gent%2C+A">A. Gent</a>, <a href="/search/astro-ph?searchtype=author&query=Gillanders%2C+G+H">G. H. Gillanders</a>, <a href="/search/astro-ph?searchtype=author&query=Giuri%2C+C">C. Giuri</a>, <a href="/search/astro-ph?searchtype=author&query=Gueta%2C+O">O. Gueta</a>, <a href="/search/astro-ph?searchtype=author&query=Hanna%2C+D">D. Hanna</a>, <a href="/search/astro-ph?searchtype=author&query=Hassan%2C+T">T. Hassan</a>, <a href="/search/astro-ph?searchtype=author&query=Hervet%2C+O">O. Hervet</a>, <a href="/search/astro-ph?searchtype=author&query=Holder%2C+J">J. Holder</a>, <a href="/search/astro-ph?searchtype=author&query=Hona%2C+B">B. Hona</a>, <a href="/search/astro-ph?searchtype=author&query=Humensky%2C+T+B">T. B. Humensky</a>, <a href="/search/astro-ph?searchtype=author&query=Jin%2C+W">W. Jin</a> , et al. (387 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="2109.11894v1-abstract-short" style="display: inline;"> The results of gamma-ray observations of the binary system HESS J0632+057 collected during 450 hours over 15 years, between 2004 and 2019, are presented. Data taken with the atmospheric Cherenkov telescopes H.E.S.S., MAGIC, and VERITAS at energies above 350 GeV were used together with observations at X-ray energies obtained with Swift-XRT, Chandra, XMM-Newton, NuSTAR, and Suzaku. Some of these obs… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.11894v1-abstract-full').style.display = 'inline'; document.getElementById('2109.11894v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.11894v1-abstract-full" style="display: none;"> The results of gamma-ray observations of the binary system HESS J0632+057 collected during 450 hours over 15 years, between 2004 and 2019, are presented. Data taken with the atmospheric Cherenkov telescopes H.E.S.S., MAGIC, and VERITAS at energies above 350 GeV were used together with observations at X-ray energies obtained with Swift-XRT, Chandra, XMM-Newton, NuSTAR, and Suzaku. Some of these observations were accompanied by measurements of the H伪 emission line. A significant detection of the modulation of the VHE gamma-ray fluxes with a period of 316.7+-4.4 days is reported, consistent with the period of 317.3+-0.7 days obtained with a refined analysis of X-ray data. The analysis of data of four orbital cycles with dense observational coverage reveals short timescale variability, with flux-decay timescales of less than 20 days at very high energies. Flux variations observed over the time scale of several years indicate orbit-to-orbit variability. The analysis confirms the previously reported correlation of X-ray and gamma-ray emission from the system at very high significance, but can not find any correlation of optical H伪 parameters with X-ray or gamma-ray energy fluxes in simultaneous observations. The key finding is that the emission of HESS J0632+057 in the X-ray and gamma-ray energy bands is highly variable on different time scales. The ratio of gamma-ray to X-ray flux shows the equality or even dominance of the gamma-ray energy range. This wealth of new data is interpreted taking into account the insufficient knowledge of the ephemeris of the system, and discussed in the context of results reported on other gamma-ray binary systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.11894v1-abstract-full').style.display = 'none'; document.getElementById('2109.11894v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 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 for publication by The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.03689">arXiv:2109.03689</a> <span> [<a href="https://arxiv.org/pdf/2109.03689">pdf</a>, <a href="https://arxiv.org/format/2109.03689">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Analysis optimisation for more than 10 TeV gamma-ray astronomy with IACTs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lypova%2C+I">Iryna Lypova</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">David Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Klepser%2C+S">Stefan Klepser</a>, <a href="/search/astro-ph?searchtype=author&query=Kostunin%2C+D">Dmitriy Kostunin</a>, <a href="/search/astro-ph?searchtype=author&query=Ohm%2C+S">Stefan Ohm</a>, <a href="/search/astro-ph?searchtype=author&query=Wagner%2C+S">Stefan Wagner</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="2109.03689v1-abstract-short" style="display: inline;"> The High Energy Stereoscopic System (H.E.S.S.) is one of the currently operating Imaging Atmospheric Cherenkov Telescopes. H.E.S.S. operates in the broad energy range from a few tens of GeV to more than 50 TeV reaching its best sensitivity around 1 TeV. In this contribution, we present an analysis technique, which is optimised for the detection at the highest energies accessible to H.E.S.S. and ai… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.03689v1-abstract-full').style.display = 'inline'; document.getElementById('2109.03689v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.03689v1-abstract-full" style="display: none;"> The High Energy Stereoscopic System (H.E.S.S.) is one of the currently operating Imaging Atmospheric Cherenkov Telescopes. H.E.S.S. operates in the broad energy range from a few tens of GeV to more than 50 TeV reaching its best sensitivity around 1 TeV. In this contribution, we present an analysis technique, which is optimised for the detection at the highest energies accessible to H.E.S.S. and aimed to improve the sensitivity above 10 TeV. It includes the employment of improved event direction reconstruction and gamma-hadron separation. For the first time, also extensive air showers with event offsets up to 4.5$^{\circ}$ from the camera centre are considered in the analysis, thereby increasing the effective Field-of-View of H.E.S.S. from 5$^{\circ}$ to 9$^{\circ}$. Key performance parameters of the new high-energy analysis are presented and its applicability demonstrated for representative hard-spectrum sources in the Milky Way. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.03689v1-abstract-full').style.display = 'none'; document.getElementById('2109.03689v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 September, 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">Proceedings of the 37th International Cosmic Ray Conference (ICRC2021)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> PoS(ICRC2021)704 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.02521">arXiv:2108.02521</a> <span> [<a href="https://arxiv.org/pdf/2108.02521">pdf</a>, <a href="https://arxiv.org/format/2108.02521">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.2593897">10.1117/12.2593897 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sensor characterization for the ULTRASAT space telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bastian-Querner%2C+B">Benjamin Bastian-Querner</a>, <a href="/search/astro-ph?searchtype=author&query=Kaipachery%2C+N">Nirmal Kaipachery</a>, <a href="/search/astro-ph?searchtype=author&query=K%C3%BCsters%2C+D">Daniel K眉sters</a>, <a href="/search/astro-ph?searchtype=author&query=Schliwinski%2C+J">Julian Schliwinski</a>, <a href="/search/astro-ph?searchtype=author&query=Alfassi%2C+S">Shay Alfassi</a>, <a href="/search/astro-ph?searchtype=author&query=Asif%2C+A">Arooj Asif</a>, <a href="/search/astro-ph?searchtype=author&query=Barschke%2C+M+F">Merlin F. Barschke</a>, <a href="/search/astro-ph?searchtype=author&query=Ben-Ami%2C+S">Sagi Ben-Ami</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">David Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Birman%2C+A">Adi Birman</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%BChler%2C+R">Rolf B眉hler</a>, <a href="/search/astro-ph?searchtype=author&query=De+Simone%2C+N">Nicola De Simone</a>, <a href="/search/astro-ph?searchtype=author&query=Fenigstein%2C+A">Amos Fenigstein</a>, <a href="/search/astro-ph?searchtype=author&query=Gal-Yam%2C+A">Avishay Gal-Yam</a>, <a href="/search/astro-ph?searchtype=author&query=Giavitto%2C+G">Gianluca Giavitto</a>, <a href="/search/astro-ph?searchtype=author&query=Crespo%2C+J+M+H">Juan M. Haces Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+D">Dmitri Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Katz%2C+O">Omer Katz</a>, <a href="/search/astro-ph?searchtype=author&query=Kowalski%2C+M">Marek Kowalski</a>, <a href="/search/astro-ph?searchtype=author&query=Kulkarni%2C+S+R">Shrinivasrao R. Kulkarni</a>, <a href="/search/astro-ph?searchtype=author&query=Lapid%2C+O">Ofer Lapid</a>, <a href="/search/astro-ph?searchtype=author&query=Liran%2C+T">Tuvia Liran</a>, <a href="/search/astro-ph?searchtype=author&query=Netzer%2C+E">Ehud Netzer</a>, <a href="/search/astro-ph?searchtype=author&query=Ofek%2C+E+O">Eran O. Ofek</a>, <a href="/search/astro-ph?searchtype=author&query=Philipp%2C+S">Sebastian Philipp</a> , et al. (9 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2108.02521v1-abstract-short" style="display: inline;"> The Ultraviolet Transient Astronomical Satellite is a scientific space mission carrying an astronomical telescope. The mission is led by the Weizmann Institute of Science in Israel and the Israel Space Agency, while the camera in the focal plane is designed and built by Deutsches Elektronen Synchrotron in Germany. Two key science goals of the mission are the detection of counterparts to gravitatio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.02521v1-abstract-full').style.display = 'inline'; document.getElementById('2108.02521v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.02521v1-abstract-full" style="display: none;"> The Ultraviolet Transient Astronomical Satellite is a scientific space mission carrying an astronomical telescope. The mission is led by the Weizmann Institute of Science in Israel and the Israel Space Agency, while the camera in the focal plane is designed and built by Deutsches Elektronen Synchrotron in Germany. Two key science goals of the mission are the detection of counterparts to gravitational wave sources and supernovae. The launch to geostationary orbit is planned for 2024. The telescope with a field-of-view of $\approx200$deg$^2$, is optimized to work in the near-ultraviolet band between $220$ and $280$nm. The focal plane array is composed of four $22.4$-megapixel, backside-illuminated CMOS sensors with a total active area of 90x90mm$^2$. Prior to sensor production, smaller test sensors have been tested to support critical design decisions for the final flight sensor. These test sensors share the design of epitaxial layer and anti-reflective coatings (ARC) with the flight sensors. Here, we present a characterization of these test sensors. Dark current and read noise are characterized as a function of the device temperature. A temperature-independent noise level is attributed to on-die infrared emission and the read-out electronics` self-heating. We utilize a high-precision photometric calibration setup to obtain the test sensors` quantum efficiency (QE) relative to PTB/NIST-calibrated transfer standards ($220$-$1100$nm), the quantum yield for $位< 300$nm, the non-linearity of the system, and the conversion gain. The uncertainties are discussed in the context of the newest results on the setup`s performance parameters. From three ARC options, Tstd, T1 and T2, the latter optimizes out-of-band rejection and peaks in the mid of the ULTRASAT operational waveband (max. QE $\approx80\%$ at $245\mathrm{nm}$). We recommend ARC option T2 for the final ULTRASAT UV sensor. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.02521v1-abstract-full').style.display = 'none'; document.getElementById('2108.02521v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.02015">arXiv:2108.02015</a> <span> [<a href="https://arxiv.org/pdf/2108.02015">pdf</a>, <a href="https://arxiv.org/format/2108.02015">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/10.1051/0004-6361/202141486">10.1051/0004-6361/202141486 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LMC N132D: A mature supernova remnant with a power-law gamma-ray spectrum extending beyond 8 TeV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Armand%2C+C">C. Armand</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+M">M. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a> , et al. (212 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2108.02015v1-abstract-short" style="display: inline;"> We analyzed 252 hours of High Energy Stereoscopic System (H.E.S.S.) observations towards the supernova remnant (SNR) LMC N132D that were accumulated between December 2004 and March 2016 during a deep survey of the Large Magellanic Cloud, adding 104 hours of observations to the previously published data set to ensure a > 5 sigma detection. To broaden the gamma-ray spectral coverage required for mod… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.02015v1-abstract-full').style.display = 'inline'; document.getElementById('2108.02015v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.02015v1-abstract-full" style="display: none;"> We analyzed 252 hours of High Energy Stereoscopic System (H.E.S.S.) observations towards the supernova remnant (SNR) LMC N132D that were accumulated between December 2004 and March 2016 during a deep survey of the Large Magellanic Cloud, adding 104 hours of observations to the previously published data set to ensure a > 5 sigma detection. To broaden the gamma-ray spectral coverage required for modeling the spectral energy distribution, an analysis of Fermi-LAT Pass 8 data was also included. We unambiguously detect N132D at very high energies (VHE) with a significance of 5.7 sigma. We report the results of a detailed analysis of its spectrum and localization based on the extended H.E.S.S. data set. The joint analysis of the extended H.E.S.S and Fermi-LAT data results in a spectral energy distribution in the energy range from 1.7 GeV to 14.8 TeV, which suggests a high luminosity of N132D at GeV and TeV energies. We set a lower limit on a gamma-ray cutoff energy of 8 TeV with a confidence level of 95%. The new gamma-ray spectrum as well as multiwavelength observations of N132D when compared to physical models suggests a hadronic origin of the VHE gamma-ray emission. SNR N132D is a VHE gamma-ray source that shows a spectrum extending to the VHE domain without a spectral cutoff at a few TeV, unlike the younger oxygen-rich SNR Cassiopeia A. The gamma-ray properties of N132D may be affected by an interaction with a nearby molecular cloud that partially lies inside the 95% confidence region of the source position. [Abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.02015v1-abstract-full').style.display = 'none'; document.getElementById('2108.02015v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 August, 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 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 655, A7 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.01493">arXiv:2108.01493</a> <span> [<a href="https://arxiv.org/pdf/2108.01493">pdf</a>, <a href="https://arxiv.org/format/2108.01493">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/10.1117/12.2594253">10.1117/12.2594253 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Design of the ULTRASAT UV camera </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Asif%2C+A">Arooj Asif</a>, <a href="/search/astro-ph?searchtype=author&query=Barschke%2C+M">Merlin Barschke</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian-Querner%2C+B">Benjamin Bastian-Querner</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">David Berge</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%BChler%2C+R">Rolf B眉hler</a>, <a href="/search/astro-ph?searchtype=author&query=De+Simone%2C+N">Nicola De Simone</a>, <a href="/search/astro-ph?searchtype=author&query=Giavitto%2C+G">Gianluca Giavitto</a>, <a href="/search/astro-ph?searchtype=author&query=Crespo%2C+J+M+H">Juan M. Haces Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Kaipachery%2C+N">Nirmal Kaipachery</a>, <a href="/search/astro-ph?searchtype=author&query=Kowalski%2C+M">Marek Kowalski</a>, <a href="/search/astro-ph?searchtype=author&query=Kulkarni%2C+S+R">Shrinivasrao R. Kulkarni</a>, <a href="/search/astro-ph?searchtype=author&query=K%C3%BCsters%2C+D">Daniel K眉sters</a>, <a href="/search/astro-ph?searchtype=author&query=Philipp%2C+S">Sebastian Philipp</a>, <a href="/search/astro-ph?searchtype=author&query=Prokoph%2C+H">Heike Prokoph</a>, <a href="/search/astro-ph?searchtype=author&query=Schliwinski%2C+J">Julian Schliwinski</a>, <a href="/search/astro-ph?searchtype=author&query=Vasilev%2C+M">Mikhail Vasilev</a>, <a href="/search/astro-ph?searchtype=author&query=Watson%2C+J+J">Jason J. Watson</a>, <a href="/search/astro-ph?searchtype=author&query=Worm%2C+S">Steven Worm</a>, <a href="/search/astro-ph?searchtype=author&query=Zappon%2C+F">Francesco Zappon</a>, <a href="/search/astro-ph?searchtype=author&query=Alfassi%2C+S">Shay Alfassi</a>, <a href="/search/astro-ph?searchtype=author&query=Ben-Ami%2C+S">Sagi Ben-Ami</a>, <a href="/search/astro-ph?searchtype=author&query=Birman%2C+A">Adi Birman</a>, <a href="/search/astro-ph?searchtype=author&query=Boggs%2C+K">Kasey Boggs</a>, <a href="/search/astro-ph?searchtype=author&query=Bredthauer%2C+G">Greg Bredthauer</a>, <a href="/search/astro-ph?searchtype=author&query=Fenigstein%2C+A">Amos Fenigstein</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="2108.01493v1-abstract-short" style="display: inline;"> The Ultraviolet Transient Astronomical Satellite (ULTRASAT) is a scientific UV space telescope that will operate in geostationary orbit. The mission, targeted to launch in 2024, is led by the Weizmann Institute of Science (WIS) in Israel and the Israel Space Agency (ISA). Deutsches Elektronen Synchrotron (DESY) in Germany is tasked with the development of the UV-sensitive camera at the heart of th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.01493v1-abstract-full').style.display = 'inline'; document.getElementById('2108.01493v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.01493v1-abstract-full" style="display: none;"> The Ultraviolet Transient Astronomical Satellite (ULTRASAT) is a scientific UV space telescope that will operate in geostationary orbit. The mission, targeted to launch in 2024, is led by the Weizmann Institute of Science (WIS) in Israel and the Israel Space Agency (ISA). Deutsches Elektronen Synchrotron (DESY) in Germany is tasked with the development of the UV-sensitive camera at the heart of the telescope. The camera's total sensitive area of ~90mm x 90mm is built up by four back-side illuminated CMOS sensors, which image a field of view of ~200 deg2. Each sensor has 22.4 megapixels. The Schmidt design of the telescope locates the detector inside the optical path, limiting the overall size of the assembly. As a result, the readout electronics is located in a remote unit outside the telescope. The short focal length of the telescope requires an accurate positioning of the sensors within +-50 mu along the optical axis, with a flatness of +-10 mu. While the telescope will be at around 295K during operations, the sensors are required to be cooled to 200K for dark current reduction. At the same time, the ability to heat the sensors to 343K is required for decontamination. In this paper, we present the preliminary design of the UV sensitive ULTRASAT camera. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.01493v1-abstract-full').style.display = 'none'; document.getElementById('2108.01493v1-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 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">"UV, X-Ray, and Gamma-Ray Space Instrumentation for Astronomy XXII", Proc. SPIE 11821, Optics and Photonics, 11821-21 (August, 2021). Contact authors Rolf Buehler (rolf.buehler@desy.de) and Merlin Barschke (merlin.barschke@desy.de)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.00383">arXiv:2108.00383</a> <span> [<a href="https://arxiv.org/pdf/2108.00383">pdf</a>, <a href="https://arxiv.org/format/2108.00383">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"> TELAMON: Effelsberg Monitoring of AGN Jets with Very-High-Energy Astroparticle Emissions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kadler%2C+M">M. Kadler</a>, <a href="/search/astro-ph?searchtype=author&query=Bach%2C+U">U. Bach</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Buson%2C+S">S. Buson</a>, <a href="/search/astro-ph?searchtype=author&query=Dorner%2C+D">D. Dorner</a>, <a href="/search/astro-ph?searchtype=author&query=Edwards%2C+P+G">P. G. Edwards</a>, <a href="/search/astro-ph?searchtype=author&query=Eppel%2C+F">F. Eppel</a>, <a href="/search/astro-ph?searchtype=author&query=Giroletti%2C+M">M. Giroletti</a>, <a href="/search/astro-ph?searchtype=author&query=Gokus%2C+A">A. Gokus</a>, <a href="/search/astro-ph?searchtype=author&query=Hervet%2C+O">O. Hervet</a>, <a href="/search/astro-ph?searchtype=author&query=He%C3%9Fd%C3%B6rfer%2C+J">J. He脽d枚rfer</a>, <a href="/search/astro-ph?searchtype=author&query=Koyama%2C+S">S. Koyama</a>, <a href="/search/astro-ph?searchtype=author&query=Kraus%2C+A">A. Kraus</a>, <a href="/search/astro-ph?searchtype=author&query=Krichbaum%2C+T+P">T. P. Krichbaum</a>, <a href="/search/astro-ph?searchtype=author&query=Lindfors%2C+E">E. Lindfors</a>, <a href="/search/astro-ph?searchtype=author&query=Mannheim%2C+K">K. Mannheim</a>, <a href="/search/astro-ph?searchtype=author&query=de+Menezes%2C+R">R. de Menezes</a>, <a href="/search/astro-ph?searchtype=author&query=Ojha%2C+R">R. Ojha</a>, <a href="/search/astro-ph?searchtype=author&query=Paraschos%2C+G+F">G. F. Paraschos</a>, <a href="/search/astro-ph?searchtype=author&query=Pueschel%2C+E">E. Pueschel</a>, <a href="/search/astro-ph?searchtype=author&query=R%C3%B6sch%2C+F">F. R枚sch</a>, <a href="/search/astro-ph?searchtype=author&query=Ros%2C+E">E. Ros</a>, <a href="/search/astro-ph?searchtype=author&query=Schleicher%2C+B">B. Schleicher</a>, <a href="/search/astro-ph?searchtype=author&query=Sinapius%2C+J">J. Sinapius</a>, <a href="/search/astro-ph?searchtype=author&query=Sitarek%2C+J">J. Sitarek</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2108.00383v1-abstract-short" style="display: inline;"> We introduce the TELAMON program, which is using the Effelsberg 100-m telescope to monitor the radio spectra of active galactic nuclei (AGN) under scrutiny in astroparticle physics, namely TeV blazars and candidate neutrino-associated AGN. Thanks to its large dish aperture and sensitive instrumentation, the Effelsberg telescope can yield radio data superior over other programs in the low flux-dens… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.00383v1-abstract-full').style.display = 'inline'; document.getElementById('2108.00383v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.00383v1-abstract-full" style="display: none;"> We introduce the TELAMON program, which is using the Effelsberg 100-m telescope to monitor the radio spectra of active galactic nuclei (AGN) under scrutiny in astroparticle physics, namely TeV blazars and candidate neutrino-associated AGN. Thanks to its large dish aperture and sensitive instrumentation, the Effelsberg telescope can yield radio data superior over other programs in the low flux-density regime down to several 10 mJy. This is a particular strength in the case of TeV-emitting blazars, which are often comparatively faint radio sources of the high-synchrotron peaked type. We perform high-cadence high-frequency observations every 2-4 weeks at multiple frequencies up to 44 GHz. This setup is well suited to trace dynamical processes in the compact parsec-scale jets of blazars related to high-energy flares or neutrino detections. Our sample currently covers about 40 sources and puts its focus on AGN with very-high-energy astroparticle emission, i.e., TeV blazars and neutrino-associated AGN. Here, we introduce the TELAMON program characteristics and present first results obtained since fall 2020. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.00383v1-abstract-full').style.display = 'none'; document.getElementById('2108.00383v1-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 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 5 figures, Proceedings of the 37th International Cosmic Ray Conference (ICRC2021). 12-23 July, 2021. Berlin, Germany. Online at https://pos.sissa.it/395/</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.01425">arXiv:2107.01425</a> <span> [<a href="https://arxiv.org/pdf/2107.01425">pdf</a>, <a href="https://arxiv.org/format/2107.01425">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/10.3847/1538-4357/abf64b">10.3847/1538-4357/abf64b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> TeV emission of Galactic plane sources with HAWC and H.E.S.S </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Armand%2C+C">C. Armand</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+M">M. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+P">P. Brun</a> , et al. (299 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="2107.01425v3-abstract-short" style="display: inline;"> The High Altitude Water Cherenkov (HAWC) observatory and the High Energy Stereoscopic System (H.E.S.S.) are two leading instruments in the ground-based very-high-energy gamma-ray domain. HAWC employs the water Cherenkov detection (WCD) technique, while H.E.S.S. is an array of Imaging Atmospheric Cherenkov Telescopes (IACTs). The two facilities therefore differ in multiple aspects, including their… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.01425v3-abstract-full').style.display = 'inline'; document.getElementById('2107.01425v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.01425v3-abstract-full" style="display: none;"> The High Altitude Water Cherenkov (HAWC) observatory and the High Energy Stereoscopic System (H.E.S.S.) are two leading instruments in the ground-based very-high-energy gamma-ray domain. HAWC employs the water Cherenkov detection (WCD) technique, while H.E.S.S. is an array of Imaging Atmospheric Cherenkov Telescopes (IACTs). The two facilities therefore differ in multiple aspects, including their observation strategy, the size of their field of view and their angular resolution, leading to different analysis approaches. Until now, it has been unclear if the results of observations by both types of instruments are consistent: several of the recently discovered HAWC sources have been followed up by IACTs, resulting in a confirmed detection only in a minority of cases. With this paper, we go further and try to resolve the tensions between previous results by performing a new analysis of the H.E.S.S. Galactic plane survey data, applying an analysis technique comparable between H.E.S.S. and HAWC. Events above 1 TeV are selected for both datasets, the point spread function of H.E.S.S. is broadened to approach that of HAWC, and a similar background estimation method is used. This is the first detailed comparison of the Galactic plane observed by both instruments. H.E.S.S. can confirm the gamma-ray emission of four HAWC sources among seven previously undetected by IACTs, while the three others have measured fluxes below the sensitivity of the H.E.S.S. dataset. Remaining differences in the overall gamma-ray flux can be explained by the systematic uncertainties. Therefore, we confirm a consistent view of the gamma-ray sky between WCD and IACT techniques. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.01425v3-abstract-full').style.display = 'none'; document.getElementById('2107.01425v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.06405">arXiv:2106.06405</a> <span> [<a href="https://arxiv.org/pdf/2106.06405">pdf</a>, <a href="https://arxiv.org/format/2106.06405">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/10.1051/0004-6361/202140962">10.1051/0004-6361/202140962 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evidence of 100 TeV $纬$-ray emission from HESS J1702-420: A new PeVatron candidate </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Armand%2C+C">C. Armand</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+M">M. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+P">P. Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Bryan%2C+M">M. Bryan</a> , et al. (211 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="2106.06405v2-abstract-short" style="display: inline;"> The identification of PeVatrons, hadronic particle accelerators reaching the knee of the cosmic ray spectrum (few $10^{15}$ eV), is crucial to understand the origin of cosmic rays in the Galaxy. We provide an update on the unidentified source HESS J1702-420, a promising PeVatron candidate. We present new observations of HESS J1702-420 made with the High Energy Stereoscopic System (H.E.S.S.), and p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.06405v2-abstract-full').style.display = 'inline'; document.getElementById('2106.06405v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.06405v2-abstract-full" style="display: none;"> The identification of PeVatrons, hadronic particle accelerators reaching the knee of the cosmic ray spectrum (few $10^{15}$ eV), is crucial to understand the origin of cosmic rays in the Galaxy. We provide an update on the unidentified source HESS J1702-420, a promising PeVatron candidate. We present new observations of HESS J1702-420 made with the High Energy Stereoscopic System (H.E.S.S.), and processed using improved analysis techniques. The analysis configuration was optimized to enhance the collection area at the highest energies. We applied a three-dimensional (3D) likelihood analysis to model the source region and adjust non thermal radiative spectral models to the $纬$-ray data. We also analyzed archival data from the Fermi Large Area Telescope (LAT) to constrain the source spectrum at $纬$-ray energies >10 GeV. We report the detection of a new source component called HESS J1702-420A, that was separated from the bulk of TeV emission at a $5.4蟽$ confidence level. The power law $纬$-ray spectrum of HESS J1702-420A extends with an index of $螕=1.53\pm0.19_\text{stat}\pm0.20_\text{sys}$ and without curvature up to the energy band 64-113 TeV, in which it was detected by H.E.S.S. at a $4.0蟽$ confidence level. This brings evidence for the source emission up to $100\,\text{TeV}$, which makes HESS J1702-420A a compelling candidate site for the presence of extremely high energy cosmic rays. Remarkably, in a hadronic scenario, the cut-off energy of the proton distribution powering HESS J1702-420A is found to be higher than 0.5 PeV at a 95% confidence level. HESS J1702-420A becomes therefore one of the most solid PeVatron candidates detected so far in H.E.S.S. data, altough a leptonic origin of its emission could not be ruled out either. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.06405v2-abstract-full').style.display = 'none'; document.getElementById('2106.06405v2-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the 2. Astrophysical processes section of 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/2106.00551">arXiv:2106.00551</a> <span> [<a href="https://arxiv.org/pdf/2106.00551">pdf</a>, <a href="https://arxiv.org/format/2106.00551">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/abff59">10.3847/1538-4357/abff59 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for dark matter annihilation signals from unidentified Fermi-LAT objects with H.E.S.S </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abdallah%2C+H">H. Abdallah</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Armand%2C+C">C. Armand</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+M">M. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brose%2C+R">R. Brose</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a> , et al. (205 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="2106.00551v2-abstract-short" style="display: inline;"> Cosmological $N$-body simulations show that Milky Way-sized galaxies harbor a population of unmerged dark matter subhalos. These subhalos could shine in gamma-rays and be eventually detected in gamma-ray surveys as unidentified sources. We performed a thorough selection among unidentified Fermi-LAT Objects (UFOs) to identify them as possible TeV-scale dark matter subhalo candidates. We search for… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.00551v2-abstract-full').style.display = 'inline'; document.getElementById('2106.00551v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.00551v2-abstract-full" style="display: none;"> Cosmological $N$-body simulations show that Milky Way-sized galaxies harbor a population of unmerged dark matter subhalos. These subhalos could shine in gamma-rays and be eventually detected in gamma-ray surveys as unidentified sources. We performed a thorough selection among unidentified Fermi-LAT Objects (UFOs) to identify them as possible TeV-scale dark matter subhalo candidates. We search for very-high-energy (E $\gtrsim$ 100 GeV) gamma-ray emissions using H.E.S.S. observations towards four selected UFOs. Since no significant very-high-energy gamma-ray emission is detected in any dataset of the four observed UFOs nor in the combined UFO dataset, strong constraints are derived on the product of the velocity-weighted annihilation cross section $\langle 蟽v \rangle$ by the $J$-factor for the dark matter models. The 95% C.L. observed upper limits derived from combined H.E.S.S. observations reach $\langle 蟽v \rangle J$ values of 3.7$\times$10$^{-5}$ and 8.1$\times$10$^{-6}$ GeV$^2$cm$^{-2}$s$^{-1}$ in the $W^+W^-$ and $蟿^+蟿^-$ channels, respectively, for a 1 TeV dark matter mass. Focusing on thermal WIMPs, the H.E.S.S. constraints restrict the $J$-factors to lie in the range 6.1$\times$10$^{19}$ - 2.0$\times$10$^{21}$ GeV$^2$cm$^{-5}$, and the masses to lie between 0.2 and 6 TeV in the $W^+W^-$ channel. For the $蟿^+蟿^-$ channel, the $J$-factors lie in the range 7.0$\times$10$^{19}$ - 7.1$\times$10$^{20}$ GeV$^2$cm$^{-5}$ and the masses lie between 0.2 and 0.5 TeV. Assuming model-dependent predictions from cosmological N-body simulations on the $J$-factor distribution for Milky Way-sized galaxies, the dark matter models with masses greater than 0.3 TeV for the UFO emissions can be ruled out at high confidence level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.00551v2-abstract-full').style.display = 'none'; document.getElementById('2106.00551v2-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 7 figures, matches accepted version in The Astrophysical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J., 918, 17 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.04325">arXiv:2105.04325</a> <span> [<a href="https://arxiv.org/pdf/2105.04325">pdf</a>, <a href="https://arxiv.org/format/2105.04325">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</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.103.102002">10.1103/PhysRevD.103.102002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for dark matter annihilation in the dwarf irregular galaxy WLM with H.E.S.S </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abdallah%2C+H">H. Abdallah</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Armand%2C+C">C. Armand</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+M">M. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Breuhaus%2C+M">M. Breuhaus</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+F">F. Brun</a> , et al. (211 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="2105.04325v1-abstract-short" style="display: inline;"> We search for an indirect signal of dark matter through very high-energy gamma rays from the Wolf-Lundmark-Melotte (WLM) dwarf irregular galaxy. The pair annihilation of dark matter particles would produce Standard Model particles in the final state such as gamma rays, which might be detected by ground-based Cherenkov telescopes. Dwarf irregular galaxies represent promising targets as they are dar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.04325v1-abstract-full').style.display = 'inline'; document.getElementById('2105.04325v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.04325v1-abstract-full" style="display: none;"> We search for an indirect signal of dark matter through very high-energy gamma rays from the Wolf-Lundmark-Melotte (WLM) dwarf irregular galaxy. The pair annihilation of dark matter particles would produce Standard Model particles in the final state such as gamma rays, which might be detected by ground-based Cherenkov telescopes. Dwarf irregular galaxies represent promising targets as they are dark matter dominated objects with well measured kinematics and small uncertainties on their dark matter distribution profiles. In 2018, the H.E.S.S. five-telescope array observed the dwarf irregular galaxy WLM for 18 hours. We present the first analysis based on data obtained from an imaging atmospheric Cherenkov telescope for this subclass of dwarf galaxy. As we do not observe any significant excess in the direction of WLM, we interpret the result in terms of constraints on the velocity-weighted cross section for dark matter pair annihilation as a function of the dark matter particle mass for various continuum channels as well as the prompt gamma-gamma emission. For the $蟿^+蟿^-$ channel the limits reach a $\langle 蟽v \rangle$ value of about $4\times 10^{-22}$ cm3s-1 for a dark matter particle mass of 1 TeV. For the prompt gamma-gamma channel, the upper limit reaches a $\langle 蟽v \rangle$ value of about $5 \times10^{-24}$ cm3s-1 for a mass of 370 GeV. These limits represent an improvement of up to a factor 200 with respect to previous results for the dwarf irregular galaxies for TeV dark matter search. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.04325v1-abstract-full').style.display = 'none'; document.getElementById('2105.04325v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 May, 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">13 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 103, 102002 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.10254">arXiv:2012.10254</a> <span> [<a href="https://arxiv.org/pdf/2012.10254">pdf</a>, <a href="https://arxiv.org/format/2012.10254">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/10.1051/0004-6361/202038949">10.1051/0004-6361/202038949 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observation of a sudden cessation of a very-high-energy gamma-ray flare in PKS 1510-089 with H.E.S.S. and MAGIC in May 2016 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+H+E+S+S">H. E. S. S. Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">F. Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Arm%2C+C">C. Arm</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baghmanyan%2C+V">V. Baghmanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+V+B">V. Barbosa Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Barnacka%2C+A">A. Barnacka</a>, <a href="/search/astro-ph?searchtype=author&query=Barnard%2C+M">M. Barnard</a>, <a href="/search/astro-ph?searchtype=author&query=Becherini%2C+Y">Y. Becherini</a>, <a href="/search/astro-ph?searchtype=author&query=Berge%2C+D">D. Berge</a>, <a href="/search/astro-ph?searchtype=author&query=Bernl%C3%B6hr%2C+K">K. Bernl枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">B. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boisson%2C+C">C. Boisson</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmont%2C+J">J. Bolmont</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoy%2C+S">S. Bonnefoy</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lavergne%2C+M+d+B">M. de Bony de Lavergne</a>, <a href="/search/astro-ph?searchtype=author&query=Bregeon%2C+J">J. Bregeon</a> , et al. (409 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="2012.10254v1-abstract-short" style="display: inline;"> The flat spectrum radio quasar (FSRQ) PKS 1510-089 is known for its complex multiwavelength behavior, and is one of only a few FSRQs detected at very high energy (VHE, $E>100\,$GeV) $纬$-rays. VHE $纬$-ray observations with H.E.S.S. and MAGIC during late May and early June 2016 resulted in the detection of an unprecedented flare, which reveals for the first time VHE $纬$-ray intranight variability in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.10254v1-abstract-full').style.display = 'inline'; document.getElementById('2012.10254v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.10254v1-abstract-full" style="display: none;"> The flat spectrum radio quasar (FSRQ) PKS 1510-089 is known for its complex multiwavelength behavior, and is one of only a few FSRQs detected at very high energy (VHE, $E>100\,$GeV) $纬$-rays. VHE $纬$-ray observations with H.E.S.S. and MAGIC during late May and early June 2016 resulted in the detection of an unprecedented flare, which reveals for the first time VHE $纬$-ray intranight variability in this source. While a common variability timescale of $1.5\,$hr is found, there is a significant deviation near the end of the flare with a timescale of $\sim 20\,$min marking the cessation of the event. The peak flux is nearly two orders of magnitude above the low-level emission. For the first time, curvature is detected in the VHE $纬$-ray spectrum of PKS 1510-089, which is fully explained through absorption by the extragalactic background light. Optical R-band observations with ATOM reveal a counterpart of the $纬$-ray flare, even though the detailed flux evolution differs from the VHE ightcurve. Interestingly, a steep flux decrease is observed at the same time as the cessation of the VHE flare. In the high energy (HE, $E>100\,$MeV) $纬$-ray band only a moderate flux increase is observed with Fermi-LAT, while the HE $纬$-ray spectrum significantly hardens up to a photon index of 1.6. A search for broad-line region (BLR) absorption features in the $纬$-ray spectrum indicates that the emission region is located outside of the BLR. Radio VLBI observations reveal a fast moving knot interacting with a standing jet feature around the time of the flare. As the standing feature is located $\sim 50\,$pc from the black hole, the emission region of the flare may have been located at a significant distance from the black hole. If this correlation is indeed true, VHE $纬$ rays have been produced far down the jet where turbulent plasma crosses a standing shock. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.10254v1-abstract-full').style.display = 'none'; document.getElementById('2012.10254v1-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 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">25 pages, 17 figures. Accepted for publication by Astronomy & Astrophysics. Corresponding authors: M. Zacharias, J. Sitarek, D. Sanchez, T. Terzic</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 648, A23 (2021) </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Berge%2C+D&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Berge%2C+D&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Berge%2C+D&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Berge%2C+D&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> </ul> </nav> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a 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