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breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Abe%2C+S&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Abe%2C+S&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Abe%2C+S&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Abe%2C+S&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Abe%2C+S&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> <li> <a href="/search/?searchtype=author&query=Abe%2C+S&start=200" class="pagination-link " aria-label="Page 5" aria-current="page">5 </a> </li> <li> <a href="/search/?searchtype=author&query=Abe%2C+S&start=250" class="pagination-link " aria-label="Page 6" aria-current="page">6 </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/2502.18061">arXiv:2502.18061</a> <span> [<a href="https://arxiv.org/pdf/2502.18061">pdf</a>, <a href="https://arxiv.org/format/2502.18061">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Materials Science">cond-mat.mtrl-sci</span> </div> </div> <p class="title is-5 mathjax"> Deuterium retention in pre-lithiated samples and Li-D co-deposits in the DIII-D tokamak </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Morbey%2C+M">M. Morbey</a>, <a href="/search/?searchtype=author&query=Effenberg%2C+F">F. Effenberg</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Abrams%2C+T">T. Abrams</a>, <a href="/search/?searchtype=author&query=Bortolon%2C+A">A. Bortolon</a>, <a href="/search/?searchtype=author&query=Hood%2C+R">R. Hood</a>, <a href="/search/?searchtype=author&query=Losada%2C+U">U. Losada</a>, <a href="/search/?searchtype=author&query=Nagy%2C+A">A. Nagy</a>, <a href="/search/?searchtype=author&query=Ren%2C+J">J. Ren</a>, <a href="/search/?searchtype=author&query=Rudakov%2C+D+L">D. L. Rudakov</a>, <a href="/search/?searchtype=author&query=Simmonds%2C+M+J">M. J. Simmonds</a>, <a href="/search/?searchtype=author&query=Truong%2C+D">D. Truong</a>, <a href="/search/?searchtype=author&query=Morgan%2C+T+W">T. W. Morgan</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="2502.18061v1-abstract-short" style="display: inline;"> Divertor designs involving liquid lithium have been proposed as an alternative to solid designs and wall conditioning techniques. However, Li affinity with tritium poses a risk for the fuel cycle. This study investigates deuterium retention in pre-lithiated samples and Li-D co-deposits in the DIII-D tokamak, making for the first time a direct comparison between Li-D co-deposits and pre-deposited L… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.18061v1-abstract-full').style.display = 'inline'; document.getElementById('2502.18061v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.18061v1-abstract-full" style="display: none;"> Divertor designs involving liquid lithium have been proposed as an alternative to solid designs and wall conditioning techniques. However, Li affinity with tritium poses a risk for the fuel cycle. This study investigates deuterium retention in pre-lithiated samples and Li-D co-deposits in the DIII-D tokamak, making for the first time a direct comparison between Li-D co-deposits and pre-deposited Li films. Samples were exposed to H-mode plasmas in the far scrape-off layer (SOL), and Li powder was injected in-situ with the impurity powder dropper to study the uniformity of Li coatings, and the dependence of fuel retention on Li thickness. The results show that at temperatures below the melting point of lithium, deuterium retention is independent of the thickness of pre-deposited Li layers, with Li-D co-deposits being the primary factor for fuel retention. Both pre-deposited and in-situ deposited Li showed lower erosion than predicted by sputtering yield calculations. These results suggest that fuel retention in fusion reactors using lithium in the divertor will likely be dominated by co-deposits rather than in the divertor itself. If one desires to use Li to achieve flatter temperature profiles, operando Li injection is advantageous over pre-deposited Li films, at least at temperatures below the melting point of lithium. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.18061v1-abstract-full').style.display = 'none'; document.getElementById('2502.18061v1-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.17002">arXiv:2502.17002</a> <span> [<a href="https://arxiv.org/pdf/2502.17002">pdf</a>, <a href="https://arxiv.org/format/2502.17002">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 - Experiment">hep-ex</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"> Neutron multiplicity measurement in muon capture on oxygen nuclei in the Gd-loaded Super-Kamiokande detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Collaboration%2C+T+S">The Super-Kamiokande Collaboration</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Asaoka%2C+Y">Y. Asaoka</a>, <a href="/search/?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/?searchtype=author&query=Harada%2C+M">M. Harada</a>, <a href="/search/?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/?searchtype=author&query=Kaneshima%2C+R">R. Kaneshima</a>, <a href="/search/?searchtype=author&query=Kashiwagi%2C+Y">Y. Kashiwagi</a>, <a href="/search/?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/?searchtype=author&query=Noguchi%2C+Y">Y. Noguchi</a>, <a href="/search/?searchtype=author&query=Okamoto%2C+K">K. Okamoto</a> , et al. (265 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="2502.17002v1-abstract-short" style="display: inline;"> In recent neutrino detectors, neutrons produced in neutrino reactions play an important role. Muon capture on oxygen nuclei is one of the processes that produce neutrons in water Cherenkov detectors. We measured neutron multiplicity in the process using cosmic ray muons that stop in the gadolinium-loaded Super-Kamiokande detector. For this measurement, neutron detection efficiency is obtained with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.17002v1-abstract-full').style.display = 'inline'; document.getElementById('2502.17002v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.17002v1-abstract-full" style="display: none;"> In recent neutrino detectors, neutrons produced in neutrino reactions play an important role. Muon capture on oxygen nuclei is one of the processes that produce neutrons in water Cherenkov detectors. We measured neutron multiplicity in the process using cosmic ray muons that stop in the gadolinium-loaded Super-Kamiokande detector. For this measurement, neutron detection efficiency is obtained with the muon capture events followed by gamma rays to be $50.2^{+2.0}_{-2.1}\%$. By fitting the observed multiplicity considering the detection efficiency, we measure neutron multiplicity in muon capture as $P(0)=24\pm3\%$, $P(1)=70^{+3}_{-2}\%$, $P(2)=6.1\pm0.5\%$, $P(3)=0.38\pm0.09\%$. This is the first measurement of the multiplicity of neutrons associated with muon capture without neutron energy threshold. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.17002v1-abstract-full').style.display = 'none'; document.getElementById('2502.17002v1-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.03889">arXiv:2501.03889</a> <span> [<a href="https://arxiv.org/pdf/2501.03889">pdf</a>, <a href="https://arxiv.org/format/2501.03889">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"> Cosmic-ray acceleration and escape from supernova remnant W44 as probed by Fermi-LAT and MAGIC </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Abhir%2C+J">J. Abhir</a>, <a href="/search/?searchtype=author&query=Abhishek%2C+A">A. Abhishek</a>, <a href="/search/?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Babi%27c%2C+A">A. Babi'c</a>, <a href="/search/?searchtype=author&query=Baquero%2C+A">A. Baquero</a>, <a href="/search/?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/?searchtype=author&query=Batkovi%27c%2C+I">I. Batkovi'c</a>, <a href="/search/?searchtype=author&query=Bautista%2C+A">A. Bautista</a>, <a href="/search/?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/?searchtype=author&query=Gonz%27alez%2C+J+B">J. Becerra Gonz'alez</a>, <a href="/search/?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/?searchtype=author&query=Bernete%2C+J">J. Bernete</a>, <a href="/search/?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/?searchtype=author&query=Besenrieder%2C+J">J. Besenrieder</a> , et al. (196 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="2501.03889v1-abstract-short" style="display: inline;"> Context. The supernova remnant (SNR) W44 and its surroundings are a prime target for studying the acceleration of cosmic rays (CRs). Several previous studies established an extended gamma-ray emission that is set apart from the radio shell of W44. This emission is thought to originate from escaped high-energy CRs that interact with a surrounding dense molecular cloud complex. Aims. We present a de… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.03889v1-abstract-full').style.display = 'inline'; document.getElementById('2501.03889v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.03889v1-abstract-full" style="display: none;"> Context. The supernova remnant (SNR) W44 and its surroundings are a prime target for studying the acceleration of cosmic rays (CRs). Several previous studies established an extended gamma-ray emission that is set apart from the radio shell of W44. This emission is thought to originate from escaped high-energy CRs that interact with a surrounding dense molecular cloud complex. Aims. We present a detailed analysis of Fermi-LAT data with an emphasis on the spatial and spectral properties of W44 and its surroundings. We also report the results of the observations performed with the MAGIC telescopes of the northwestern region of W44. Finally, we present an interpretation model to explain the gamma-ray emission of the SNR and its surroundings. Methods. We first performed a detailed spatial analysis of 12 years of Fermi-LAT data at energies above 1 GeV, in order to exploit the better angular resolution, while we set a threshold of 100MeV for the spectral analysis. We performed a likelihood analysis of 174 hours of MAGIC data above 130 GeV using the spatial information obtained with Fermi-LAT. Results. The combined spectra of Fermi-LAT and MAGIC, extending from 100MeV to several TeV, were used to derive constraints on the escape of CRs. Using a time-dependent model to describe the particle acceleration and escape from the SNR, we show that the maximum energy of the accelerated particles has to be ' 40 GeV. However, our gamma-ray data suggest that a small number of lower-energy particles also needs to escape. We propose a novel model, the broken-shock scenario, to account for this effect and explain the gamma-ray emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.03889v1-abstract-full').style.display = 'none'; document.getElementById('2501.03889v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.03831">arXiv:2501.03831</a> <span> [<a href="https://arxiv.org/pdf/2501.03831">pdf</a>, <a href="https://arxiv.org/format/2501.03831">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"> Characterization of Markarian 421 during its most violent year: Multiwavelength variability and correlations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Abhir%2C+J">J. Abhir</a>, <a href="/search/?searchtype=author&query=Abhishek%2C+A">A. Abhishek</a>, <a href="/search/?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Baack%2C+D">D. Baack</a>, <a href="/search/?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a>, <a href="/search/?searchtype=author&query=Bautista%2C+A">A. Bautista</a>, <a href="/search/?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/?searchtype=author&query=Bernete%2C+J">J. Bernete</a>, <a href="/search/?searchtype=author&query=Berti%2C+A">A. Berti</a> , et al. (190 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="2501.03831v1-abstract-short" style="display: inline;"> Mrk 421 was in its most active state around early 2010, which led to the highest TeV gamma-ray flux ever recorded from any active galactic nuclei. We aim to characterize the multiwavelength behavior during this exceptional year for Mrk 421, and evaluate whether it is consistent with the picture derived with data from other less exceptional years. We investigated the period from November 5, 2009, (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.03831v1-abstract-full').style.display = 'inline'; document.getElementById('2501.03831v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.03831v1-abstract-full" style="display: none;"> Mrk 421 was in its most active state around early 2010, which led to the highest TeV gamma-ray flux ever recorded from any active galactic nuclei. We aim to characterize the multiwavelength behavior during this exceptional year for Mrk 421, and evaluate whether it is consistent with the picture derived with data from other less exceptional years. We investigated the period from November 5, 2009, (MJD 55140) until July 3, 2010, (MJD 55380) with extensive coverage from very-high-energy (VHE; E$\,>\,$100$\,$GeV) gamma rays to radio with MAGIC, VERITAS, Fermi-LAT, RXTE, Swift, GASP-WEBT, VLBA, and a variety of additional optical and radio telescopes. We investigated the variability and correlation behavior among different energy bands in great detail. We find the strongest variability in X-rays and VHE gamma rays, and PSDs compatible with power-law functions. We observe strong correlations between X-rays and VHE gamma rays. We also report a marginally significant positive correlation between high-energy (HE; E$\,>\,$100$\,$MeV) gamma rays and the ultraviolet band. We detected marginally significant correlations between the HE and VHE gamma rays, and between HE gamma rays and the X-ray, that disappear when the large flare in February 2010 is excluded from the correlation study. The activity of Mrk 421 also yielded the first ejection of features in the VLBA images of the jet of Mrk 421. Yet the large uncertainties in the ejection times of these radio features prevent us from firmly associating them to the specific flares recorded during the campaign. We also show that the collected multi-instrument data are consistent with a scenario where the emission is dominated by two regions, a compact and extended zone, which could be considered as a simplified implementation of an energy-stratified jet as suggested by recent IXPE observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.03831v1-abstract-full').style.display = 'none'; document.getElementById('2501.03831v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </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. Corresponding authors: Felix Schmuckermaier, David Paneque, Axel Arbet Engels</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.15836">arXiv:2412.15836</a> <span> [<a href="https://arxiv.org/pdf/2412.15836">pdf</a>, <a href="https://arxiv.org/format/2412.15836">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/10.1051/0004-6361/202451378">10.1051/0004-6361/202451378 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Time-dependent modelling of short-term variability in the TeV-blazar VER J0521+211 during the major flare in 2020 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=MAGIC+Collaboration"> MAGIC Collaboration</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Abhir%2C+J">J. Abhir</a>, <a href="/search/?searchtype=author&query=Abhishek%2C+A">A. Abhishek</a>, <a href="/search/?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Baack%2C+D">D. Baack</a>, <a href="/search/?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a>, <a href="/search/?searchtype=author&query=Bautista%2C+A">A. Bautista</a>, <a href="/search/?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/?searchtype=author&query=Bernete%2C+J">J. Bernete</a> , et al. (206 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="2412.15836v1-abstract-short" style="display: inline;"> The BL Lacertae object VER J0521+211 underwent a notable flaring episode in February 2020. A short-term monitoring campaign, led by the MAGIC (Major Atmospheric Gamma Imaging Cherenkov) collaboration, covering a wide energy range from radio to very-high-energy (VHE, 100 GeV < E < 100 TeV) gamma rays was organised to study its evolution. These observations resulted in a consistent detection of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.15836v1-abstract-full').style.display = 'inline'; document.getElementById('2412.15836v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.15836v1-abstract-full" style="display: none;"> The BL Lacertae object VER J0521+211 underwent a notable flaring episode in February 2020. A short-term monitoring campaign, led by the MAGIC (Major Atmospheric Gamma Imaging Cherenkov) collaboration, covering a wide energy range from radio to very-high-energy (VHE, 100 GeV < E < 100 TeV) gamma rays was organised to study its evolution. These observations resulted in a consistent detection of the source over six consecutive nights in the VHE gamma-ray domain. Combining these nightly observations with an extensive set of multiwavelength data made modelling of the blazar's spectral energy distribution (SED) possible during the flare. This modelling was performed with a focus on two plausible emission mechanisms: i) a leptonic two-zone synchrotron-self-Compton scenario, and ii) a lepto-hadronic one-zone scenario. Both models effectively replicated the observed SED from radio to the VHE gamma-ray band. Furthermore, by introducing a set of evolving parameters, both models were successful in reproducing the evolution of the fluxes measured in different bands throughout the observing campaign. Notably, the lepto-hadronic model predicts enhanced photon and neutrino fluxes at ultra-high energies (E > 100 TeV). While the photon component, generated via decay of neutral pions, is not directly observable as it is subject to intense pair production (and therefore extinction) through interactions with the cosmic microwave background photons, neutrino detectors (e.g. IceCube) can probe the predicted neutrino component. Finally, the analysis of the gamma-ray spectra, as observed by MAGIC and the Fermi-LAT telescopes, yielded a conservative 95\% confidence upper limit of z \leq 0.244 for the redshift of this blazar. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.15836v1-abstract-full').style.display = 'none'; document.getElementById('2412.15836v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in 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 694, A308 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.07466">arXiv:2412.07466</a> <span> [<a href="https://arxiv.org/pdf/2412.07466">pdf</a>, <a href="https://arxiv.org/format/2412.07466">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 Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.111.033006">10.1103/PhysRevD.111.033006 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Implementation and investigation of electron-nucleus scattering in the \textsc{NEUT} neutrino event generator </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">Seisho Abe</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.07466v2-abstract-short" style="display: inline;"> Understanding nuclear effects is essential for improving the sensitivity of neutrino oscillation measurements. Validating nuclear models solely through neutrino scattering data is challenging due to limited statistics and the broad energy spectrum of neutrinos. In contrast, electron scattering experiments provide abundant high-precision data with various monochromatic energies and angles. Since bo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.07466v2-abstract-full').style.display = 'inline'; document.getElementById('2412.07466v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.07466v2-abstract-full" style="display: none;"> Understanding nuclear effects is essential for improving the sensitivity of neutrino oscillation measurements. Validating nuclear models solely through neutrino scattering data is challenging due to limited statistics and the broad energy spectrum of neutrinos. In contrast, electron scattering experiments provide abundant high-precision data with various monochromatic energies and angles. Since both neutrinos and electrons interact via electroweak interactions, the same nuclear models can be applied to simulate both interactions. Thus, high-precision electron scattering data is essential for validating the nuclear models used in neutrino experiments. To enable this, the author has introduced a new electron scattering framework in the \textsc{NEUT} neutrino event generator, covering two interaction modes: quasielastic (QE) and single pion production. \textsc{NEUT} predictions of QE agree well with numerical calculations, supporting the validity of this implementation. From comparisons with \textsc{NEUT} predictions and inclusive electron scattering data, the momentum-dependent removal energy correction is derived, addressing effects beyond the plane wave impulse approximation. This correction is applied to neutrino interactions, observing significant changes in charged lepton kinematics. Notably, the reconstructed neutrino energy distribution shows a peak shift of approximately 20--30\,MeV, which is crucial for accurately measuring neutrino oscillation parameters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.07466v2-abstract-full').style.display = 'none'; document.getElementById('2412.07466v2-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 111, 033006 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.24099">arXiv:2410.24099</a> <span> [<a href="https://arxiv.org/pdf/2410.24099">pdf</a>, <a href="https://arxiv.org/format/2410.24099">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 - Experiment">hep-ex</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"> Characterization of the optical model of the T2K 3D segmented plastic scintillator detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Alekseev%2C+I">I. Alekseev</a>, <a href="/search/?searchtype=author&query=Arai%2C+T">T. Arai</a>, <a href="/search/?searchtype=author&query=Arihara%2C+T">T. Arihara</a>, <a href="/search/?searchtype=author&query=Arimoto%2C+S">S. Arimoto</a>, <a href="/search/?searchtype=author&query=Babu%2C+N">N. Babu</a>, <a href="/search/?searchtype=author&query=Baranov%2C+V">V. Baranov</a>, <a href="/search/?searchtype=author&query=Bartoszek%2C+L">L. Bartoszek</a>, <a href="/search/?searchtype=author&query=Berns%2C+L">L. Berns</a>, <a href="/search/?searchtype=author&query=Bhattacharjee%2C+S">S. Bhattacharjee</a>, <a href="/search/?searchtype=author&query=Blondel%2C+A">A. Blondel</a>, <a href="/search/?searchtype=author&query=Boikov%2C+A+V">A. V. Boikov</a>, <a href="/search/?searchtype=author&query=Buizza-Avanzini%2C+M">M. Buizza-Avanzini</a>, <a href="/search/?searchtype=author&query=Cap%C3%B3%2C+J">J. Cap贸</a>, <a href="/search/?searchtype=author&query=Cayo%2C+J">J. Cayo</a>, <a href="/search/?searchtype=author&query=Chakrani%2C+J">J. Chakrani</a>, <a href="/search/?searchtype=author&query=Chong%2C+P+S">P. S. Chong</a>, <a href="/search/?searchtype=author&query=Chvirova%2C+A">A. Chvirova</a>, <a href="/search/?searchtype=author&query=Danilov%2C+M">M. Danilov</a>, <a href="/search/?searchtype=author&query=Davis%2C+C">C. Davis</a>, <a href="/search/?searchtype=author&query=Davydov%2C+Y+I">Yu. I. Davydov</a>, <a href="/search/?searchtype=author&query=Dergacheva%2C+A">A. Dergacheva</a>, <a href="/search/?searchtype=author&query=Dokania%2C+N">N. Dokania</a>, <a href="/search/?searchtype=author&query=Douqa%2C+D">D. Douqa</a>, <a href="/search/?searchtype=author&query=Doyle%2C+T+A">T. A. Doyle</a> , et al. (106 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.24099v1-abstract-short" style="display: inline;"> The magnetised near detector (ND280) of the T2K long-baseline neutrino oscillation experiment has been recently upgraded aiming to satisfy the requirement of reducing the systematic uncertainty from measuring the neutrinonucleus interaction cross section, which is the largest systematic uncertainty in the search for leptonic charge-parity symmetry violation. A key component of the upgrade is Super… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.24099v1-abstract-full').style.display = 'inline'; document.getElementById('2410.24099v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.24099v1-abstract-full" style="display: none;"> The magnetised near detector (ND280) of the T2K long-baseline neutrino oscillation experiment has been recently upgraded aiming to satisfy the requirement of reducing the systematic uncertainty from measuring the neutrinonucleus interaction cross section, which is the largest systematic uncertainty in the search for leptonic charge-parity symmetry violation. A key component of the upgrade is SuperFGD, a 3D segmented plastic scintillator detector made of approximately 2,000,000 optically-isolated 1 cm3 cubes. It will provide a 3D image of GeV neutrino interactions by combining tracking and stopping power measurements of final state particles with sub-nanosecond time resolution. The performance of SuperFGD is characterized by the precision of its response to charged particles as well as the systematic effects that might affect the physics measurements. Hence, a detailed Geant4 based optical simulation of the SuperFGD building block, i.e. a plastic scintillating cube read out by three wavelength shifting fibers, has been developed and validated with the different datasets collected in various beam tests. In this manuscript the description of the optical model as well as the comparison with data are reported. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.24099v1-abstract-full').style.display = 'none'; document.getElementById('2410.24099v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">31 pages, 15 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/2410.23140">arXiv:2410.23140</a> <span> [<a href="https://arxiv.org/pdf/2410.23140">pdf</a>, <a href="https://arxiv.org/format/2410.23140">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"> Insights from the first flaring activity of a high-synchrotron-peaked blazar with X-ray polarization and VHE gamma rays </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=MAGIC+Collaboration"> MAGIC Collaboration</a>, <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Abhir%2C+J">J. Abhir</a>, <a href="/search/?searchtype=author&query=Abhishek%2C+A">A. Abhishek</a>, <a href="/search/?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/?searchtype=author&query=Barrios-Jim%C3%A9nez%2C+L">L. Barrios-Jim茅nez</a>, <a href="/search/?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a>, <a href="/search/?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/?searchtype=author&query=Bernete%2C+J">J. Bernete</a>, <a href="/search/?searchtype=author&query=Berti%2C+A">A. Berti</a> , et al. (229 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.23140v2-abstract-short" style="display: inline;"> We study a flaring activity of the HSP Mrk421 that was characterized from radio to very-high-energy (VHE; E $>0.1$TeV) gamma rays with MAGIC, Fermi-LAT, Swift, XMM-Newton and several optical and radio telescopes. These observations included, for the first time for a gamma-ray flare of a blazar, simultaneous X-ray polarization measurements with IXPE. We find substantial variability in both X-rays a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.23140v2-abstract-full').style.display = 'inline'; document.getElementById('2410.23140v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.23140v2-abstract-full" style="display: none;"> We study a flaring activity of the HSP Mrk421 that was characterized from radio to very-high-energy (VHE; E $>0.1$TeV) gamma rays with MAGIC, Fermi-LAT, Swift, XMM-Newton and several optical and radio telescopes. These observations included, for the first time for a gamma-ray flare of a blazar, simultaneous X-ray polarization measurements with IXPE. We find substantial variability in both X-rays and VHE gamma rays throughout the campaign, with the highest VHE flux above 0.2 TeV occurring during the IXPE observing window, and exceeding twice the flux of the Crab Nebula. However, the VHE and X-ray spectra are on average softer, and the correlation between these two bands weaker that those reported in previous flares of Mrk421. IXPE reveals an X-ray polarization degree significantly higher than that at radio and optical frequencies. The X-ray polarization angle varies by $\sim$100$^\circ$ on timescales of days, and the polarization degree changes by more than a factor 4. The highest X-ray polarization degree reaches 26%, around which a X-ray counter-clockwise hysteresis loop is measured with XMM-Newton. It suggests that the X-ray emission comes from particles close to the high-energy cutoff, hence possibly probing an extreme case of the Turbulent Extreme Multi-Zone model. We model the broadband emission with a simplified stratified jet model throughout the flare. The polarization measurements imply an electron distribution in the X-ray emitting region with a very high minimum Lorentz factor, which is expected in electron-ion plasma, as well as a variation of the emitting region size up to a factor of three during the flaring activity. We find no correlation between the fluxes and the evolution of the model parameters, which indicates a stochastic nature of the underlying physical mechanism. Such behaviour would be expected in a highly turbulent electron-ion plasma crossing a shock front. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.23140v2-abstract-full').style.display = 'none'; document.getElementById('2410.23140v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in Astronomy and Astrophysics (on January 17th 2025). Corresponding authors: Axel Arbet-Engels, Lea Heckmann, David Paneque</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.22557">arXiv:2410.22557</a> <span> [<a href="https://arxiv.org/pdf/2410.22557">pdf</a>, <a href="https://arxiv.org/format/2410.22557">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"> Multi-wavelength study of OT 081: broadband modelling of a transitional blazar </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=MAGIC+Collaboration"> MAGIC Collaboration</a>, <a href="/search/?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Baack%2C+D">D. Baack</a>, <a href="/search/?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/?searchtype=author&query=Baquero%2C+A">A. Baquero</a>, <a href="/search/?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a>, <a href="/search/?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/?searchtype=author&query=Bernardos%2C+M">M. Bernardos</a>, <a href="/search/?searchtype=author&query=Bernete%2C+J">J. Bernete</a>, <a href="/search/?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/?searchtype=author&query=Bigongiari%2C+C">C. Bigongiari</a>, <a href="/search/?searchtype=author&query=Biland%2C+A">A. Biland</a>, <a href="/search/?searchtype=author&query=Blanch%2C+O">O. Blanch</a> , et al. (250 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.22557v2-abstract-short" style="display: inline;"> OT 081 is a well-known, luminous blazar that is remarkably variable in many energy bands. We present the first broadband study of the source which includes very-high-energy (VHE, $E>$100\,GeV) $纬$-ray data taken by the MAGIC and H.E.S.S. imaging Cherenkov telescopes. The discovery of VHE $纬$-ray emission happened during a high state of $纬$-ray activity in July 2016, observed by many instruments fr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.22557v2-abstract-full').style.display = 'inline'; document.getElementById('2410.22557v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.22557v2-abstract-full" style="display: none;"> OT 081 is a well-known, luminous blazar that is remarkably variable in many energy bands. We present the first broadband study of the source which includes very-high-energy (VHE, $E>$100\,GeV) $纬$-ray data taken by the MAGIC and H.E.S.S. imaging Cherenkov telescopes. The discovery of VHE $纬$-ray emission happened during a high state of $纬$-ray activity in July 2016, observed by many instruments from radio to VHE $纬$-rays. We identify four states of activity of the source, one of which includes VHE $纬$-ray emission. Variability in the VHE domain is found on daily timescales. The intrinsic VHE spectrum can be described by a power-law with index $3.27\pm0.44_{\rm stat}\pm0.15_{\rm sys}$ (MAGIC) and $3.39\pm0.58_{\rm stat}\pm0.64_{\rm sys}$ (H.E.S.S.) in the energy range of 55--300\,GeV and 120--500\,GeV, respectively. The broadband emission cannot be sucessfully reproduced by a simple one-zone synchrotron self-Compton model. Instead, an additional external Compton component is required. We test a lepto-hadronic model that reproduces the dataset well and a proton-synchrotron dominated model that requires an extreme proton luminosity. Emission models that are able to successfully represent the data place the emitting region well outside of the Broad Line Region (BLR) to a location at which the radiative environment is dominated by the infrared thermal radiation field of the dusty torus. In the scenario described by this flaring activity, the source appears to be an FSRQ, in contrast with past categorizations. This suggests that the source can be considered to be a transitional blazar, intermediate between BL~Lac and FSRQ objects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.22557v2-abstract-full').style.display = 'none'; document.getElementById('2410.22557v2-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">v1</span> submitted 29 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted on MNRAS Corresponding authors: M. Manganaro, J. Becerra Gonz谩lez, M. Seglar-Arroyo, D. A. Sanchez</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.16042">arXiv:2410.16042</a> <span> [<a href="https://arxiv.org/pdf/2410.16042">pdf</a>, <a href="https://arxiv.org/format/2410.16042">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/10.1051/0004-6361/202450889">10.1051/0004-6361/202450889 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A new method of reconstructing images of gamma-ray telescopes applied to the LST-1 of CTAO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Project%2C+C">CTA-LST Project</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Abhishek%2C+A">A. Abhishek</a>, <a href="/search/?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Alispach%2C+C">C. Alispach</a>, <a href="/search/?searchtype=author&query=Crespo%2C+N+A">N. Alvarez Crespo</a>, <a href="/search/?searchtype=author&query=Ambrosino%2C+D">D. Ambrosino</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Arbet-Engels%2C+A">A. Arbet-Engels</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Aubert%2C+P">P. Aubert</a>, <a href="/search/?searchtype=author&query=Baktash%2C+A">A. Baktash</a>, <a href="/search/?searchtype=author&query=Balbo%2C+M">M. Balbo</a>, <a href="/search/?searchtype=author&query=Bamba%2C+A">A. Bamba</a>, <a href="/search/?searchtype=author&query=Larriva%2C+A+B">A. Baquero Larriva</a>, <a href="/search/?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/?searchtype=author&query=Jim%C3%A9nez%2C+L+B">L. Barrios Jim茅nez</a>, <a href="/search/?searchtype=author&query=Batkovic%2C+I">I. Batkovic</a> , et al. (283 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.16042v1-abstract-short" style="display: inline;"> Imaging atmospheric Cherenkov telescopes (IACTs) are used to observe very high-energy photons from the ground. Gamma rays are indirectly detected through the Cherenkov light emitted by the air showers they induce. The new generation of experiments, in particular the Cherenkov Telescope Array Observatory (CTAO), sets ambitious goals for discoveries of new gamma-ray sources and precise measurements… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.16042v1-abstract-full').style.display = 'inline'; document.getElementById('2410.16042v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.16042v1-abstract-full" style="display: none;"> Imaging atmospheric Cherenkov telescopes (IACTs) are used to observe very high-energy photons from the ground. Gamma rays are indirectly detected through the Cherenkov light emitted by the air showers they induce. The new generation of experiments, in particular the Cherenkov Telescope Array Observatory (CTAO), sets ambitious goals for discoveries of new gamma-ray sources and precise measurements of the already discovered ones. To achieve these goals, both hardware and data analysis must employ cutting-edge techniques. This also applies to the LST-1, the first IACT built for the CTAO, which is currently taking data on the Canary island of La Palma. This paper introduces a new event reconstruction technique for IACT data, aiming to improve the image reconstruction quality and the discrimination between the signal and the background from misidentified hadrons and electrons. The technique models the development of the extensive air shower signal, recorded as a waveform per pixel, seen by CTAO telescopes' cameras. Model parameters are subsequently passed to random forest regressors and classifiers to extract information on the primary particle. The new reconstruction was applied to simulated data and to data from observations of the Crab Nebula performed by the LST-1. The event reconstruction method presented here shows promising performance improvements. The angular and energy resolution, and the sensitivity, are improved by 10 to 20% over most of the energy range. At low energy, improvements reach up to 22%, 47%, and 50%, respectively. A future extension of the method to stereoscopic analysis for telescope arrays will be the next important step. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.16042v1-abstract-full').style.display = 'none'; document.getElementById('2410.16042v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted 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 691, A328 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.19633">arXiv:2409.19633</a> <span> [<a href="https://arxiv.org/pdf/2409.19633">pdf</a>, <a href="https://arxiv.org/format/2409.19633">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 - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Search for proton decay via $p\rightarrow{e^+畏}$ and $p\rightarrow{渭^+畏}$ with a 0.37 Mton-year exposure of Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Collaboration%2C+S">Super-Kamiokande Collaboration</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Taniuchi%2C+N">N. Taniuchi</a>, <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Asaoka%2C+Y">Y. Asaoka</a>, <a href="/search/?searchtype=author&query=Bronner%2C+C">C. Bronner</a>, <a href="/search/?searchtype=author&query=Harada%2C+M">M. Harada</a>, <a href="/search/?searchtype=author&query=Hayato%2C+Y">Y. Hayato</a>, <a href="/search/?searchtype=author&query=Hiraide%2C+K">K. Hiraide</a>, <a href="/search/?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/?searchtype=author&query=Ieki%2C+K">K. Ieki</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+M">M. Ikeda</a>, <a href="/search/?searchtype=author&query=Kameda%2C+J">J. Kameda</a>, <a href="/search/?searchtype=author&query=Kanemura%2C+Y">Y. Kanemura</a>, <a href="/search/?searchtype=author&query=Kaneshima%2C+R">R. Kaneshima</a>, <a href="/search/?searchtype=author&query=Kashiwagi%2C+Y">Y. Kashiwagi</a>, <a href="/search/?searchtype=author&query=Kataoka%2C+Y">Y. Kataoka</a>, <a href="/search/?searchtype=author&query=Miki%2C+S">S. Miki</a>, <a href="/search/?searchtype=author&query=Mine%2C+S">S. Mine</a>, <a href="/search/?searchtype=author&query=Miura%2C+M">M. Miura</a>, <a href="/search/?searchtype=author&query=Moriyama%2C+S">S. Moriyama</a>, <a href="/search/?searchtype=author&query=Nakahata%2C+M">M. Nakahata</a>, <a href="/search/?searchtype=author&query=Nakayama%2C+S">S. Nakayama</a>, <a href="/search/?searchtype=author&query=Noguchi%2C+Y">Y. Noguchi</a> , et al. (267 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="2409.19633v1-abstract-short" style="display: inline;"> A search for proton decay into $e^+/渭^+$ and a $畏$ meson has been performed using data from a 0.373 Mton$\cdot$year exposure (6050.3 live days) of Super-Kamiokande. Compared to previous searches this work introduces an improved model of the intranuclear $畏$ interaction cross section, resulting in a factor of two reduction in uncertainties from this source and $\sim$10\% increase in signal efficien… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.19633v1-abstract-full').style.display = 'inline'; document.getElementById('2409.19633v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.19633v1-abstract-full" style="display: none;"> A search for proton decay into $e^+/渭^+$ and a $畏$ meson has been performed using data from a 0.373 Mton$\cdot$year exposure (6050.3 live days) of Super-Kamiokande. Compared to previous searches this work introduces an improved model of the intranuclear $畏$ interaction cross section, resulting in a factor of two reduction in uncertainties from this source and $\sim$10\% increase in signal efficiency. No significant data excess was found above the expected number of atmospheric neutrino background events resulting in no indication of proton decay into either mode. Lower limits on the proton partial lifetime of $1.4\times\mathrm{10^{34}~years}$ for $p\rightarrow e^+畏$ and $7.3\times\mathrm{10^{33}~years}$ for $p\rightarrow 渭^+畏$ at the 90$\%$ C.L. were set. These limits are around 1.5 times longer than our previous study and are the most stringent to date. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.19633v1-abstract-full').style.display = 'none'; document.getElementById('2409.19633v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.18823">arXiv:2409.18823</a> <span> [<a href="https://arxiv.org/pdf/2409.18823">pdf</a>, <a href="https://arxiv.org/format/2409.18823">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"> Standardised formats and open-source analysis tools for the MAGIC telescopes data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Abhir%2C+J">J. Abhir</a>, <a href="/search/?searchtype=author&query=Abhishek%2C+A">A. Abhishek</a>, <a href="/search/?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a>, <a href="/search/?searchtype=author&query=Bautista%2C+A">A. Bautista</a>, <a href="/search/?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/?searchtype=author&query=Bernete%2C+J">J. Bernete</a>, <a href="/search/?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/?searchtype=author&query=Besenrieder%2C+J">J. Besenrieder</a> , et al. (186 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="2409.18823v2-abstract-short" style="display: inline;"> Instruments for gamma-ray astronomy at Very High Energies ($E>100\,{\rm GeV}$) have traditionally derived their scientific results through proprietary data and software. Data standardisation has become a prominent issue in this field both as a requirement for the dissemination of data from the next generation of gamma-ray observatories and as an effective solution to realise public data legacies o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.18823v2-abstract-full').style.display = 'inline'; document.getElementById('2409.18823v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.18823v2-abstract-full" style="display: none;"> Instruments for gamma-ray astronomy at Very High Energies ($E>100\,{\rm GeV}$) have traditionally derived their scientific results through proprietary data and software. Data standardisation has become a prominent issue in this field both as a requirement for the dissemination of data from the next generation of gamma-ray observatories and as an effective solution to realise public data legacies of current-generation instruments. Specifications for a standardised gamma-ray data format have been proposed as a community effort and have already been successfully adopted by several instruments. We present the first production of standardised data from the Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) telescopes. We converted $166\,{\rm h}$ of observations from different sources and validated their analysis with the open-source software Gammapy. We consider six data sets representing different scientific and technical analysis cases and compare the results obtained analysing the standardised data with open-source software against those produced with the MAGIC proprietary data and software. Aiming at a systematic production of MAGIC data in this standardised format, we also present the implementation of a database-driven pipeline automatically performing the MAGIC data reduction from the calibrated down to the standardised data level. In all the cases selected for the validation, we obtain results compatible with the MAGIC proprietary software, both for the manual and for the automatic data productions. Part of the validation data set is also made publicly available, thus representing the first large public release of MAGIC data. This effort and this first data release represent a technical milestone toward the realisation of a public MAGIC data legacy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.18823v2-abstract-full').style.display = 'none'; document.getElementById('2409.18823v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the Journal of High Energy 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/2408.02246">arXiv:2408.02246</a> <span> [<a href="https://arxiv.org/pdf/2408.02246">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Databases">cs.DB</span> </div> </div> <p class="title is-5 mathjax"> AMIDER: A Multidisciplinary Research Database and Its Application to Promote Open Science </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kozai%2C+M">Masayoshi Kozai</a>, <a href="/search/?searchtype=author&query=Tanaka%2C+Y">Yoshimasa Tanaka</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">Shuji Abe</a>, <a href="/search/?searchtype=author&query=Minamiyama%2C+Y">Yasuyuki Minamiyama</a>, <a href="/search/?searchtype=author&query=Shinbori%2C+A">Atsuki Shinbori</a>, <a href="/search/?searchtype=author&query=Kadokura%2C+A">Akira Kadokura</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.02246v3-abstract-short" style="display: inline;"> The AMIDER, Advanced Multidisciplinary Integrated-Database for Exploring new Research, is a newly developed research data catalog to demonstrate an advanced database application. AMIDER is characterized as a multidisciplinary database equipped with a user-friendly web application. Its catalog view displays diverse research data at once beyond any limitation of each individual discipline. Some usef… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.02246v3-abstract-full').style.display = 'inline'; document.getElementById('2408.02246v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.02246v3-abstract-full" style="display: none;"> The AMIDER, Advanced Multidisciplinary Integrated-Database for Exploring new Research, is a newly developed research data catalog to demonstrate an advanced database application. AMIDER is characterized as a multidisciplinary database equipped with a user-friendly web application. Its catalog view displays diverse research data at once beyond any limitation of each individual discipline. Some useful functions, such as a selectable data download, data format conversion, and display of data visual information, are also implemented. Further advanced functions, such as visualization of dataset mutual relationship, are also implemented as a preliminary trial. These characteristics and functions are expected to enhance the accessibility to individual research data, even from non-expertized users, and be helpful for collaborations among diverse scientific fields beyond individual disciplines. Multidisciplinary data management is also one of AMIDER's uniqueness, where various metadata schemas can be mapped to a uniform metadata table, and standardized and self-describing data formats are adopted. AMIDER website (https://amider.rois.ac.jp/) had been launched in April 2024. As of July 2024, over 15,000 metadata in various research fields of polar science have been registered in the database, and approximately 500 visitors are viewing the website every day on average. Expansion of the database to further multidisciplinary scientific fields, not only polar science, is planned, and advanced attempts, such as applying Natural Language Processing (NLP) to metadata, have also been considered. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.02246v3-abstract-full').style.display = 'none'; document.getElementById('2408.02246v3-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, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 4 figures, accepted for publication in Data Science 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/2407.02343">arXiv:2407.02343</a> <span> [<a href="https://arxiv.org/pdf/2407.02343">pdf</a>, <a href="https://arxiv.org/format/2407.02343">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> A detailed study of the very-high-energy Crab pulsar emission with the LST-1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Project%2C+C">CTA-LST Project</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Abhishek%2C+A">A. Abhishek</a>, <a href="/search/?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Crespo%2C+N+A">N. Alvarez Crespo</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Arbet-Engels%2C+A">A. Arbet-Engels</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Aubert%2C+P">P. Aubert</a>, <a href="/search/?searchtype=author&query=Baktash%2C+A">A. Baktash</a>, <a href="/search/?searchtype=author&query=Bamba%2C+A">A. Bamba</a>, <a href="/search/?searchtype=author&query=Larriva%2C+A+B">A. Baquero Larriva</a>, <a href="/search/?searchtype=author&query=Baroncelli%2C+L">L. Baroncelli</a>, <a href="/search/?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/?searchtype=author&query=Batkovic%2C+I">I. Batkovic</a>, <a href="/search/?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a> , et al. (272 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="2407.02343v1-abstract-short" style="display: inline;"> Context: There are currently three pulsars firmly detected by imaging atmospheric Cherenkov telescopes (IACTs), two of them reaching TeV energies, challenging models of very-high-energy (VHE) emission in pulsars. More precise observations are needed to better characterize pulsar emission at these energies. The LST-1 is the prototype of the Large-Sized Telescope, that will be part of the Cherenkov… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.02343v1-abstract-full').style.display = 'inline'; document.getElementById('2407.02343v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.02343v1-abstract-full" style="display: none;"> Context: There are currently three pulsars firmly detected by imaging atmospheric Cherenkov telescopes (IACTs), two of them reaching TeV energies, challenging models of very-high-energy (VHE) emission in pulsars. More precise observations are needed to better characterize pulsar emission at these energies. The LST-1 is the prototype of the Large-Sized Telescope, that will be part of the Cherenkov Telescope Array Observatory (CTAO). Its improved performance over previous IACTs makes it well suited for studying pulsars. Aims: To study the Crab pulsar emission with the LST-1, improving and complementing the results from other telescopes. These observations can also be used to characterize the potential of the LST-1 to study other pulsars and detect new ones. Methods: We analyzed a total of $\sim$103 hours of gamma-ray observations of the Crab pulsar conducted with the LST-1 in the period from September 2020 to January 2023. The observations were carried out at zenith angles less than 50 degrees. A new analysis of the Fermi-LAT data was also performed, including $\sim$14 years of observations. Results: The Crab pulsar phaseogram, long-term light-curve, and phase-resolved spectra are reconstructed with the LST-1 from 20 GeV to 450 GeV for P1 and up to 700 GeV for P2. The pulsed emission is detected with a significance of 15.2$蟽$. The two characteristic emission peaks of the Crab pulsar are clearly detected (>10$蟽$), as well as the so-called bridge emission (5.7$蟽$). We find that both peaks are well described by power laws, with spectral indices of $\sim$3.44 and $\sim$3.03 respectively. The joint analysis of Fermi-LAT and LST-1 data shows a good agreement between both instruments in the overlapping energy range. The detailed results obtained in the first observations of the Crab pulsar with LST-1 show the potential that CTAO will have to study this type of sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.02343v1-abstract-full').style.display = 'none'; document.getElementById('2407.02343v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 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">Accepted by 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/2406.11438">arXiv:2406.11438</a> <span> [<a href="https://arxiv.org/pdf/2406.11438">pdf</a>, <a href="https://arxiv.org/format/2406.11438">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 - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Search for Majorana Neutrinos with the Complete KamLAND-Zen Dataset </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Araki%2C+T">T. Araki</a>, <a href="/search/?searchtype=author&query=Chiba%2C+K">K. Chiba</a>, <a href="/search/?searchtype=author&query=Eda%2C+T">T. Eda</a>, <a href="/search/?searchtype=author&query=Eizuka%2C+M">M. Eizuka</a>, <a href="/search/?searchtype=author&query=Funahashi%2C+Y">Y. Funahashi</a>, <a href="/search/?searchtype=author&query=Furuto%2C+A">A. Furuto</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Goto%2C+S">S. Goto</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Marthe%2C+A">A. Marthe</a>, <a href="/search/?searchtype=author&query=Matsumoto%2C+Y">Y. Matsumoto</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Miyake%2C+H">H. Miyake</a> , et al. (48 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="2406.11438v1-abstract-short" style="display: inline;"> We present a search for neutrinoless double-beta ($0谓尾尾$) decay of $^{136}$Xe using the full KamLAND-Zen 800 dataset with 745 kg of enriched xenon, corresponding to an exposure of $2.097$ ton yr of $^{136}$Xe. This updated search benefits from a more than twofold increase in exposure, recovery of photo-sensor gain, and reduced background from muon-induced spallation of xenon. Combining with the se… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.11438v1-abstract-full').style.display = 'inline'; document.getElementById('2406.11438v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.11438v1-abstract-full" style="display: none;"> We present a search for neutrinoless double-beta ($0谓尾尾$) decay of $^{136}$Xe using the full KamLAND-Zen 800 dataset with 745 kg of enriched xenon, corresponding to an exposure of $2.097$ ton yr of $^{136}$Xe. This updated search benefits from a more than twofold increase in exposure, recovery of photo-sensor gain, and reduced background from muon-induced spallation of xenon. Combining with the search in the previous KamLAND-Zen phase, we obtain a lower limit for the $0谓尾尾$ decay half-life of $T_{1/2}^{0谓} > 3.8 \times 10^{26}$ yr at 90% C.L., a factor of 1.7 improvement over the previous limit. The corresponding upper limits on the effective Majorana neutrino mass are in the range 28-122 meV using phenomenological nuclear matrix element calculations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.11438v1-abstract-full').style.display = 'none'; document.getElementById('2406.11438v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 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">arXiv admin note: text overlap with arXiv:2203.02139</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.07140">arXiv:2406.07140</a> <span> [<a href="https://arxiv.org/pdf/2406.07140">pdf</a>, <a href="https://arxiv.org/format/2406.07140">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2024/07/044">10.1088/1475-7516/2024/07/044 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints on Lorentz invariance violation from the extraordinary Mrk 421 flare of 2014 using a novel analysis method </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=MAGIC+Collaboration"> MAGIC Collaboration</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Abhir%2C+J">J. Abhir</a>, <a href="/search/?searchtype=author&query=Abhishek%2C+A">A. Abhishek</a>, <a href="/search/?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/?searchtype=author&query=Baquero%2C+A">A. Baquero</a>, <a href="/search/?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a>, <a href="/search/?searchtype=author&query=Bautista%2C+A">A. Bautista</a>, <a href="/search/?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/?searchtype=author&query=Bernete%2C+J">J. Bernete</a> , et al. (192 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="2406.07140v1-abstract-short" style="display: inline;"> The Lorentz Invariance Violation (LIV), a proposed consequence of certain quantum gravity (QG) scenarios, could instigate an energy-dependent group velocity for ultra-relativistic particles. This energy dependence, although suppressed by the massive QG energy scale $E_\mathrm{QG}$, expected to be on the level of the Planck energy $1.22 \times 10^{19}$ GeV, is potentially detectable in astrophysica… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.07140v1-abstract-full').style.display = 'inline'; document.getElementById('2406.07140v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.07140v1-abstract-full" style="display: none;"> The Lorentz Invariance Violation (LIV), a proposed consequence of certain quantum gravity (QG) scenarios, could instigate an energy-dependent group velocity for ultra-relativistic particles. This energy dependence, although suppressed by the massive QG energy scale $E_\mathrm{QG}$, expected to be on the level of the Planck energy $1.22 \times 10^{19}$ GeV, is potentially detectable in astrophysical observations. In this scenario, the cosmological distances traversed by photons act as an amplifier for this effect. By leveraging the observation of a remarkable flare from the blazar Mrk\,421, recorded at energies above 100 GeV by the MAGIC telescopes on the night of April 25 to 26, 2014, we look for time delays scaling linearly and quadratically with the photon energies. Using for the first time in LIV studies a binned-likelihood approach we set constraints on the QG energy scale. For the linear scenario, we set $95\%$ lower limits $E_\mathrm{QG}>2.7\times10^{17}$ GeV for the subluminal case and $E_\mathrm{QG}> 3.6 \times10^{17}$ GeV for the superluminal case. For the quadratic scenario, the $95\%$ lower limits for the subluminal and superluminal cases are $E_\mathrm{QG}>2.6 \times10^{10}$ GeV and $E_\mathrm{QG}>2.5\times10^{10}$ GeV, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.07140v1-abstract-full').style.display = 'none'; document.getElementById('2406.07140v1-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 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">Journal ref:</span> Journal of Cosmology and Astroparticle Physics 07 p.044 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.12488">arXiv:2405.12488</a> <span> [<a href="https://arxiv.org/pdf/2405.12488">pdf</a>, <a href="https://arxiv.org/format/2405.12488">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 - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> First joint oscillation analysis of Super-Kamiokande atmospheric and T2K accelerator neutrino data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Super-Kamiokande"> Super-Kamiokande</a>, <a href="/search/?searchtype=author&query=collaborations%2C+T">T2K collaborations</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Akhlaq%2C+N">N. Akhlaq</a>, <a href="/search/?searchtype=author&query=Akutsu%2C+R">R. Akutsu</a>, <a href="/search/?searchtype=author&query=Alarakia-Charles%2C+H">H. Alarakia-Charles</a>, <a href="/search/?searchtype=author&query=Ali%2C+A">A. Ali</a>, <a href="/search/?searchtype=author&query=Hakim%2C+Y+I+A">Y. I. Alj Hakim</a>, <a href="/search/?searchtype=author&query=Monsalve%2C+S+A">S. Alonso Monsalve</a>, <a href="/search/?searchtype=author&query=Amanai%2C+S">S. Amanai</a>, <a href="/search/?searchtype=author&query=Andreopoulos%2C+C">C. Andreopoulos</a>, <a href="/search/?searchtype=author&query=Anthony%2C+L+H+V">L. H. V. Anthony</a>, <a href="/search/?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/?searchtype=author&query=Aoki%2C+S">S. Aoki</a>, <a href="/search/?searchtype=author&query=Apte%2C+K+A">K. A. Apte</a>, <a href="/search/?searchtype=author&query=Arai%2C+T">T. Arai</a>, <a href="/search/?searchtype=author&query=Arihara%2C+T">T. Arihara</a>, <a href="/search/?searchtype=author&query=Arimoto%2C+S">S. Arimoto</a>, <a href="/search/?searchtype=author&query=Asada%2C+Y">Y. Asada</a>, <a href="/search/?searchtype=author&query=Asaka%2C+R">R. Asaka</a>, <a href="/search/?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/?searchtype=author&query=Atkin%2C+E+T">E. T. Atkin</a>, <a href="/search/?searchtype=author&query=Babu%2C+N">N. Babu</a> , et al. (524 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="2405.12488v2-abstract-short" style="display: inline;"> The Super-Kamiokande and T2K collaborations present a joint measurement of neutrino oscillation parameters from their atmospheric and beam neutrino data. It uses a common interaction model for events overlapping in neutrino energy and correlated detector systematic uncertainties between the two datasets, which are found to be compatible. Using 3244.4 days of atmospheric data and a beam exposure of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.12488v2-abstract-full').style.display = 'inline'; document.getElementById('2405.12488v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.12488v2-abstract-full" style="display: none;"> The Super-Kamiokande and T2K collaborations present a joint measurement of neutrino oscillation parameters from their atmospheric and beam neutrino data. It uses a common interaction model for events overlapping in neutrino energy and correlated detector systematic uncertainties between the two datasets, which are found to be compatible. Using 3244.4 days of atmospheric data and a beam exposure of $19.7(16.3) \times 10^{20}$ protons on target in (anti)neutrino mode, the analysis finds a 1.9$蟽$ exclusion of CP-conservation (defined as $J_{CP}=0$) and a preference for the normal mass ordering. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.12488v2-abstract-full').style.display = 'none'; document.getElementById('2405.12488v2-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 4 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/2405.02974">arXiv:2405.02974</a> <span> [<a href="https://arxiv.org/pdf/2405.02974">pdf</a>, <a href="https://arxiv.org/format/2405.02974">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Materials Science">cond-mat.mtrl-sci</span> </div> </div> <p class="title is-5 mathjax"> Importance of Gas Heating in Capacitively Coupled Radiofrequency Plasma-assisted Synthesis of Carbon Nanomaterials </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Nikhar%2C+T">Tanvi Nikhar</a>, <a href="/search/?searchtype=author&query=Basu%2C+S">Sankhadeep Basu</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">Shota Abe</a>, <a href="/search/?searchtype=author&query=Yatom%2C+S">Shurik Yatom</a>, <a href="/search/?searchtype=author&query=Raitses%2C+Y">Yevgeny Raitses</a>, <a href="/search/?searchtype=author&query=Anthony%2C+R">Rebecca Anthony</a>, <a href="/search/?searchtype=author&query=Baryshev%2C+S+V">Sergey V. Baryshev</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.02974v1-abstract-short" style="display: inline;"> In pursuit of diamond nanoparticles, a capacitively-coupled radio frequency (CCRF) flow-through plasma reactor was operated with methane argon gas mixtures. Signatures of the final product obtained microscopically and spectroscopically indicated that the product was an amorphous form of graphite. This result was consistent irrespective of combinations of the macroscopic reactor settings. To explai… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.02974v1-abstract-full').style.display = 'inline'; document.getElementById('2405.02974v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.02974v1-abstract-full" style="display: none;"> In pursuit of diamond nanoparticles, a capacitively-coupled radio frequency (CCRF) flow-through plasma reactor was operated with methane argon gas mixtures. Signatures of the final product obtained microscopically and spectroscopically indicated that the product was an amorphous form of graphite. This result was consistent irrespective of combinations of the macroscopic reactor settings. To explain the observed synthesis output, measurements of C2 and gas properties were carried out by laser-induced fluorescence and optical emission spectroscopy. Strikingly, the results indicated a strong gas temperature gradient of 100 K per mm from the center of the reactor to the wall. Based on additional plasma imaging, a model of hot constricted region (filamentation region) was then formulated. It illustrated that, while the hot constricted region was present, the bulk of the gas was not hot enough to facilitate diamond sp3 formation: characterized by much lower reaction rates, when compared to sp2, sp3 formation kinetics are expected to become exponentially slow. This result was further confirmed by experiments under identical conditions but with a H2/CH4 mixture, where no output material was detected: if graphitic sp2 formation was expected as the main output material from the methane feedstock, atomic hydrogen would then be expected to etch it away in situ, such that the net production of that sp2-hybridized solid material is nearly a zero. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.02974v1-abstract-full').style.display = 'none'; document.getElementById('2405.02974v1-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.17623">arXiv:2404.17623</a> <span> [<a href="https://arxiv.org/pdf/2404.17623">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <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/10.1051/0004-6361/202450497">10.1051/0004-6361/202450497 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Broadband Multi-wavelength Properties of M87 during the 2018 EHT Campaign including a Very High Energy Flaring Episode </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Algaba%2C+J+C">J. C. Algaba</a>, <a href="/search/?searchtype=author&query=Balokovic%2C+M">M. Balokovic</a>, <a href="/search/?searchtype=author&query=Chandra%2C+S">S. Chandra</a>, <a href="/search/?searchtype=author&query=Cheong%2C+W+Y">W. Y. Cheong</a>, <a href="/search/?searchtype=author&query=Cui%2C+Y+Z">Y. Z. Cui</a>, <a href="/search/?searchtype=author&query=D%27Ammando%2C+F">F. D'Ammando</a>, <a href="/search/?searchtype=author&query=Falcone%2C+A+D">A. D. Falcone</a>, <a href="/search/?searchtype=author&query=Ford%2C+N+M">N. M. Ford</a>, <a href="/search/?searchtype=author&query=Giroletti%2C+M">M. Giroletti</a>, <a href="/search/?searchtype=author&query=Goddi%2C+C">C. Goddi</a>, <a href="/search/?searchtype=author&query=Gurwell%2C+M+A">M. A. Gurwell</a>, <a href="/search/?searchtype=author&query=Hada%2C+K">K. Hada</a>, <a href="/search/?searchtype=author&query=Haggard%2C+D">D. Haggard</a>, <a href="/search/?searchtype=author&query=Jorstad%2C+S">S. Jorstad</a>, <a href="/search/?searchtype=author&query=Kaur%2C+A">A. Kaur</a>, <a href="/search/?searchtype=author&query=Kawashima%2C+T">T. Kawashima</a>, <a href="/search/?searchtype=author&query=Kerby%2C+S">S. Kerby</a>, <a href="/search/?searchtype=author&query=Kim%2C+J+Y">J. Y. Kim</a>, <a href="/search/?searchtype=author&query=Kino%2C+M">M. Kino</a>, <a href="/search/?searchtype=author&query=Kravchenko%2C+E+V">E. V. Kravchenko</a>, <a href="/search/?searchtype=author&query=Lee%2C+S+S">S. S. Lee</a>, <a href="/search/?searchtype=author&query=Lu%2C+R+S">R. S. Lu</a>, <a href="/search/?searchtype=author&query=Markoff%2C+S">S. Markoff</a>, <a href="/search/?searchtype=author&query=Michail%2C+J">J. Michail</a>, <a href="/search/?searchtype=author&query=Neilsen%2C+J">J. Neilsen</a> , et al. (721 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="2404.17623v3-abstract-short" style="display: inline;"> The nearby elliptical galaxy M87 contains one of the only two supermassive black holes whose emission surrounding the event horizon has been imaged by the Event Horizon Telescope (EHT). In 2018, more than two dozen multi-wavelength (MWL) facilities (from radio to gamma-ray energies) took part in the second M87 EHT campaign. The goal of this extensive MWL campaign was to better understand the physi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.17623v3-abstract-full').style.display = 'inline'; document.getElementById('2404.17623v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.17623v3-abstract-full" style="display: none;"> The nearby elliptical galaxy M87 contains one of the only two supermassive black holes whose emission surrounding the event horizon has been imaged by the Event Horizon Telescope (EHT). In 2018, more than two dozen multi-wavelength (MWL) facilities (from radio to gamma-ray energies) took part in the second M87 EHT campaign. The goal of this extensive MWL campaign was to better understand the physics of the accreting black hole M87*, the relationship between the inflow and inner jets, and the high-energy particle acceleration. Understanding the complex astrophysics is also a necessary first step towards performing further tests of general relativity. The MWL campaign took place in April 2018, overlapping with the EHT M87* observations. We present a new, contemporaneous spectral energy distribution (SED) ranging from radio to very high energy (VHE) gamma-rays, as well as details of the individual observations and light curves. We also conduct phenomenological modelling to investigate the basic source properties. We present the first VHE gamma-ray flare from M87 detected since 2010. The flux above 350 GeV has more than doubled within a period of about 36 hours. We find that the X-ray flux is enhanced by about a factor of two compared to 2017, while the radio and millimetre core fluxes are consistent between 2017 and 2018. We detect evidence for a monotonically increasing jet position angle that corresponds to variations in the bright spot of the EHT image. Our results show the value of continued MWL monitoring together with precision imaging for addressing the origins of high-energy particle acceleration. While we cannot currently pinpoint the precise location where such acceleration takes place, the new VHE gamma-ray flare already presents a challenge to simple one-zone leptonic emission model approaches, and emphasises the need for combined image and spectral modelling. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.17623v3-abstract-full').style.display = 'none'; document.getElementById('2404.17623v3-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">46 pages, 23 figures, accepted by Astronomy & Astrophysics on August. 29, 2024</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 692, A140 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.09920">arXiv:2404.09920</a> <span> [<a href="https://arxiv.org/pdf/2404.09920">pdf</a>, <a href="https://arxiv.org/format/2404.09920">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 - Experiment">hep-ex</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="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/10.3847/1538-4357/ad5fee">10.3847/1538-4357/ad5fee <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Combined Pre-Supernova Alert System with Kamland and Super-Kamiokande </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=KamLAND"> KamLAND</a>, <a href="/search/?searchtype=author&query=Collaborations%2C+S">Super-Kamiokande Collaborations</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">Seisho Abe</a>, <a href="/search/?searchtype=author&query=Eizuka%2C+M">Minori Eizuka</a>, <a href="/search/?searchtype=author&query=Futagi%2C+S">Sawako Futagi</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">Azusa Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Yoshihito Gando</a>, <a href="/search/?searchtype=author&query=Goto%2C+S">Shun Goto</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">Takahiko Hachiya</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">Kazumi Hata</a>, <a href="/search/?searchtype=author&query=Ichimura%2C+K">Koichi Ichimura</a>, <a href="/search/?searchtype=author&query=Ieki%2C+S">Sei Ieki</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">Haruo Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">Kunio Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">Koji Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Yuto Kamei</a>, <a href="/search/?searchtype=author&query=Kawada%2C+N">Nanami Kawada</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Yasuhiro Kishimoto</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">Masayuki Koga</a>, <a href="/search/?searchtype=author&query=Kurasawa%2C+M">Maho Kurasawa</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">Tadao Mitsui</a>, <a href="/search/?searchtype=author&query=Miyake%2C+H">Haruhiko Miyake</a>, <a href="/search/?searchtype=author&query=Morita%2C+D">Daisuke Morita</a>, <a href="/search/?searchtype=author&query=Nakahata%2C+T">Takeshi Nakahata</a> , et al. (290 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="2404.09920v3-abstract-short" style="display: inline;"> Preceding a core-collapse supernova, various processes produce an increasing amount of neutrinos of all flavors characterized by mounting energies from the interior of massive stars. Among them, the electron antineutrinos are potentially detectable by terrestrial neutrino experiments such as KamLAND and Super-Kamiokande via inverse beta decay interactions. Once these pre-supernova neutrinos are ob… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.09920v3-abstract-full').style.display = 'inline'; document.getElementById('2404.09920v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.09920v3-abstract-full" style="display: none;"> Preceding a core-collapse supernova, various processes produce an increasing amount of neutrinos of all flavors characterized by mounting energies from the interior of massive stars. Among them, the electron antineutrinos are potentially detectable by terrestrial neutrino experiments such as KamLAND and Super-Kamiokande via inverse beta decay interactions. Once these pre-supernova neutrinos are observed, an early warning of the upcoming core-collapse supernova can be provided. In light of this, KamLAND and Super-Kamiokande, both located in the Kamioka mine in Japan, have been monitoring pre-supernova neutrinos since 2015 and 2021, respectively. Recently, we performed a joint study between KamLAND and Super-Kamiokande on pre-supernova neutrino detection. A pre-supernova alert system combining the KamLAND detector and the Super-Kamiokande detector was developed and put into operation, which can provide a supernova alert to the astrophysics community. Fully leveraging the complementary properties of these two detectors, the combined alert is expected to resolve a pre-supernova neutrino signal from a 15 M$_{\odot}$ star within 510 pc of the Earth, at a significance level corresponding to a false alarm rate of no more than 1 per century. For a Betelgeuse-like model with optimistic parameters, it can provide early warnings up to 12 hours in advance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.09920v3-abstract-full').style.display = 'none'; document.getElementById('2404.09920v3-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Resubmitted to ApJ. 22 pages, 16 figures, for more information about the combined pre-supernova alert system, see https://www.lowbg.org/presnalarm/</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.19965">arXiv:2403.19965</a> <span> [<a href="https://arxiv.org/pdf/2403.19965">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> </div> <p class="title is-5 mathjax"> Muon Nuclear Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Niikura%2C+M">Megumi Niikura</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">Shinichiro Abe</a>, <a href="/search/?searchtype=author&query=Kawase%2C+S">Shoichiro Kawase</a>, <a href="/search/?searchtype=author&query=Matsuzaki%2C+T">Teiichiro Matsuzaki</a>, <a href="/search/?searchtype=author&query=Minato%2C+F">Futoshi Minato</a>, <a href="/search/?searchtype=author&query=Mizuno%2C+R">Rurie Mizuno</a>, <a href="/search/?searchtype=author&query=Watanabe%2C+Y">Yukinobu Watanabe</a>, <a href="/search/?searchtype=author&query=Yamaguchi%2C+Y">Yuji Yamaguchi</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.19965v1-abstract-short" style="display: inline;"> We plan to develop a new nuclear database for muon-induced nuclear reactions (muon nuclear data). The database will consist of (1) energies and intensities of the muonic X rays, (2) lifetimes of the muonic atom, (3) production branching ratio of the residual nuclei by muon capture, (4) emission probabilities of the particles after muon capture, and (5) energy spectra of the emitted particles after… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.19965v1-abstract-full').style.display = 'inline'; document.getElementById('2403.19965v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.19965v1-abstract-full" style="display: none;"> We plan to develop a new nuclear database for muon-induced nuclear reactions (muon nuclear data). The database will consist of (1) energies and intensities of the muonic X rays, (2) lifetimes of the muonic atom, (3) production branching ratio of the residual nuclei by muon capture, (4) emission probabilities of the particles after muon capture, and (5) energy spectra of the emitted particles after muon capture. In this paper, we review the present status and current investigations for the muon nuclear data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.19965v1-abstract-full').style.display = 'none'; document.getElementById('2403.19965v1-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, 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">Proceedings for Joint Symposium on Nuclear Data and PHITS in 2023, in print (JAEA-Conf series)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.04857">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/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Abhir%2C+J">J. Abhir</a>, <a href="/search/?searchtype=author&query=Abhishek%2C+A">A. Abhishek</a>, <a href="/search/?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Aguirre-Santaella%2C+A">A. Aguirre-Santaella</a>, <a href="/search/?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/?searchtype=author&query=Alvarez-Crespo%2C+N">N. Alvarez-Crespo</a>, <a href="/search/?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/?searchtype=author&query=Amans%2C+J+-">J. -P. Amans</a>, <a href="/search/?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/?searchtype=author&query=Angel%2C+L">L. Angel</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Arnesen%2C+T+T+H">T. T. H. Arnesen</a>, <a href="/search/?searchtype=author&query=Arrabito%2C+L">L. Arrabito</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Ascasibar%2C+Y">Y. Ascasibar</a>, <a href="/search/?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/?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/2403.02159">arXiv:2403.02159</a> <span> [<a href="https://arxiv.org/pdf/2403.02159">pdf</a>, <a href="https://arxiv.org/format/2403.02159">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/stae649">10.1093/mnras/stae649 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The variability patterns of the TeV blazar PG 1553+113 from a decade of MAGIC and multi-band observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=MAGIC+Collaboration"> MAGIC Collaboration</a>, <a href="/search/?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Abhir%2C+J">J. Abhir</a>, <a href="/search/?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Baack%2C+D">D. Baack</a>, <a href="/search/?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/?searchtype=author&query=Baquero%2C+A">A. Baquero</a>, <a href="/search/?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a>, <a href="/search/?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/?searchtype=author&query=Bernete%2C+J">J. Bernete</a>, <a href="/search/?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/?searchtype=author&query=Besenrieder%2C+J">J. Besenrieder</a>, <a href="/search/?searchtype=author&query=Bigongiari%2C+C">C. Bigongiari</a> , et al. (242 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="2403.02159v1-abstract-short" style="display: inline;"> PG 1553+113 is one of the few blazars with a convincing quasi-periodic emission in the gamma-ray band. The source is also a very high-energy (VHE; >100 GeV) gamma-ray emitter. To better understand its properties and identify the underlying physical processes driving its variability, the MAGIC Collaboration initiated a multiyear, multiwavelength monitoring campaign in 2015 involving the OVRO 40-m a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.02159v1-abstract-full').style.display = 'inline'; document.getElementById('2403.02159v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.02159v1-abstract-full" style="display: none;"> PG 1553+113 is one of the few blazars with a convincing quasi-periodic emission in the gamma-ray band. The source is also a very high-energy (VHE; >100 GeV) gamma-ray emitter. To better understand its properties and identify the underlying physical processes driving its variability, the MAGIC Collaboration initiated a multiyear, multiwavelength monitoring campaign in 2015 involving the OVRO 40-m and Medicina radio telescopes, REM, KVA, and the MAGIC telescopes, Swift and Fermi satellites, and the WEBT network. The analysis presented in this paper uses data until 2017 and focuses on the characterization of the variability. The gamma-ray data show a (hint of a) periodic signal compatible with literature, but the X-ray and VHE gamma-ray data do not show statistical evidence for a periodic signal. In other bands, the data are compatible with the gamma-ray period, but with a relatively high p-value. The complex connection between the low and high-energy emission and the non-monochromatic modulation and changes in flux suggests that a simple one-zone model is unable to explain all the variability. Instead, a model including a periodic component along with multiple emission zones is required. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.02159v1-abstract-full').style.display = 'none'; document.getElementById('2403.02159v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Monthly Notices of the Royal Astronomical Society. 19 pages, 9 figures. Corresponding authors: Elisa Prandini, Antonio Stamerra, Talvikki Hovatta</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.04755">arXiv:2402.04755</a> <span> [<a href="https://arxiv.org/pdf/2402.04755">pdf</a>, <a href="https://arxiv.org/format/2402.04755">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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stae697">10.1093/mnras/stae697 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Performance and first measurements of the MAGIC Stellar Intensity Interferometer </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=MAGIC+Collaboration"> MAGIC Collaboration</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Abhir%2C+J">J. Abhir</a>, <a href="/search/?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/?searchtype=author&query=Baquero%2C+A">A. Baquero</a>, <a href="/search/?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a>, <a href="/search/?searchtype=author&query=Bautista%2C+A">A. Bautista</a>, <a href="/search/?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/?searchtype=author&query=Bernardos%2C+M">M. Bernardos</a>, <a href="/search/?searchtype=author&query=Bernete%2C+J">J. Bernete</a>, <a href="/search/?searchtype=author&query=Berti%2C+A">A. Berti</a> , et al. (195 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="2402.04755v1-abstract-short" style="display: inline;"> In recent years, a new generation of optical intensity interferometers has emerged, leveraging the existing infrastructure of Imaging Atmospheric Cherenkov Telescopes (IACTs). The MAGIC telescopes host the MAGIC-SII system (Stellar Intensity Interferometer), implemented to investigate the feasibility and potential of this technique on IACTs. After the first successful measurements in 2019, the sys… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.04755v1-abstract-full').style.display = 'inline'; document.getElementById('2402.04755v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.04755v1-abstract-full" style="display: none;"> In recent years, a new generation of optical intensity interferometers has emerged, leveraging the existing infrastructure of Imaging Atmospheric Cherenkov Telescopes (IACTs). The MAGIC telescopes host the MAGIC-SII system (Stellar Intensity Interferometer), implemented to investigate the feasibility and potential of this technique on IACTs. After the first successful measurements in 2019, the system was upgraded and now features a real-time, dead-time-free, 4-channel, GPU-based correlator. These hardware modifications allow seamless transitions between MAGIC's standard very-high-energy gamma-ray observations and optical interferometry measurements within seconds. We establish the feasibility and potential of employing IACTs as competitive optical Intensity Interferometers with minimal hardware adjustments. The measurement of a total of 22 stellar diameters are reported, 9 corresponding to reference stars with previous comparable measurements, and 13 with no prior measurements. A prospective implementation involving telescopes from the forthcoming Cherenkov Telescope Array Observatory's northern hemisphere array, such as the first prototype of its Large-Sized Telescopes, LST-1, is technically viable. This integration would significantly enhance the sensitivity of the current system and broaden the UV-plane coverage. This advancement would enable the system to achieve competitive sensitivity with the current generation of long-baseline optical interferometers over blue wavelengths. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.04755v1-abstract-full').style.display = 'none'; document.getElementById('2402.04755v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 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">18 pages, 13 figures, submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.08560">arXiv:2401.08560</a> <span> [<a href="https://arxiv.org/pdf/2401.08560">pdf</a>, <a href="https://arxiv.org/format/2401.08560">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"> Insights into the broad-band emission of the TeV blazar Mrk 501 during the first X-ray polarization measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Abhir%2C+J">J. Abhir</a>, <a href="/search/?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/?searchtype=author&query=Baquero%2C+A">A. Baquero</a>, <a href="/search/?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a>, <a href="/search/?searchtype=author&query=Bautista%2C+A">A. Bautista</a>, <a href="/search/?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/?searchtype=author&query=Bernardos%2C+M">M. Bernardos</a>, <a href="/search/?searchtype=author&query=Bernete%2C+J">J. Bernete</a>, <a href="/search/?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/?searchtype=author&query=Besenrieder%2C+J">J. Besenrieder</a> , et al. (239 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="2401.08560v1-abstract-short" style="display: inline;"> We present the first multi-wavelength study of Mrk 501 including very-high-energy (VHE) gamma-ray observations simultaneous to X-ray polarization measurements from the Imaging X-ray Polarimetry Explorer (IXPE). We use radio-to-VHE data from a multi-wavelength campaign organized between 2022-03-01 and 2022-07-19. The observations were performed by MAGIC, Fermi-LAT, NuSTAR, Swift (XRT and UVOT), and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.08560v1-abstract-full').style.display = 'inline'; document.getElementById('2401.08560v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.08560v1-abstract-full" style="display: none;"> We present the first multi-wavelength study of Mrk 501 including very-high-energy (VHE) gamma-ray observations simultaneous to X-ray polarization measurements from the Imaging X-ray Polarimetry Explorer (IXPE). We use radio-to-VHE data from a multi-wavelength campaign organized between 2022-03-01 and 2022-07-19. The observations were performed by MAGIC, Fermi-LAT, NuSTAR, Swift (XRT and UVOT), and several instruments covering the optical and radio bands. During the IXPE pointings, the VHE state is close to the average behavior with a 0.2-1 TeV flux of 20%-50% the emission of the Crab Nebula. Despite the average VHE activity, an extreme X-ray behavior is measured for the first two IXPE pointings in March 2022 with a synchrotron peak frequency >1 keV. For the third IXPE pointing in July 2022, the synchrotron peak shifts towards lower energies and the optical/X-ray polarization degrees drop. The X-ray polarization is systematically higher than at lower energies, suggesting an energy-stratification of the jet. While during the IXPE epochs the polarization angle in the X-ray, optical and radio bands align well, we find a clear discrepancy in the optical and radio polarization angles in the middle of the campaign. We model the broad-band spectra simultaneous to the IXPE pointings assuming a compact zone dominating in the X-rays and VHE, and an extended zone stretching further downstream the jet dominating the emission at lower energies. NuSTAR data allow us to precisely constrain the synchrotron peak and therefore the underlying electron distribution. The change between the different states observed in the three IXPE pointings can be explained by a change of magnetization and/or emission region size, which directly connects the shift of the synchrotron peak to lower energies with the drop in polarization degree. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.08560v1-abstract-full').style.display = 'none'; document.getElementById('2401.08560v1-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy & Astrophysics. 19 pages, 9 figures. Corresponding authors: Lea Heckmann, Axel Arbet Engels, David Paneque</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.07798">arXiv:2401.07798</a> <span> [<a href="https://arxiv.org/pdf/2401.07798">pdf</a>, <a href="https://arxiv.org/format/2401.07798">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.dark.2024.101425">10.1016/j.dark.2024.101425 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints on axion-like particles with the Perseus Galaxy Cluster with MAGIC </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=MAGIC+Collaboration"> MAGIC Collaboration</a>, <a href="/search/?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Abhir%2C+J">J. Abhir</a>, <a href="/search/?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Baack%2C+D">D. Baack</a>, <a href="/search/?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/?searchtype=author&query=Baquero%2C+A">A. Baquero</a>, <a href="/search/?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a>, <a href="/search/?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/?searchtype=author&query=Bernete%2C+J">J. Bernete</a>, <a href="/search/?searchtype=author&query=Berti%2C+A">A. Berti</a> , et al. (189 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="2401.07798v1-abstract-short" style="display: inline;"> Axion-like particles (ALPs) are pseudo-Nambu-Goldstone bosons that emerge in various theories beyond the standard model. These particles can interact with high-energy photons in external magnetic fields, influencing the observed gamma-ray spectrum. This study analyzes 41.3 hrs of observational data from the Perseus Galaxy Cluster collected with the MAGIC telescopes. We focused on the spectra the r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.07798v1-abstract-full').style.display = 'inline'; document.getElementById('2401.07798v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.07798v1-abstract-full" style="display: none;"> Axion-like particles (ALPs) are pseudo-Nambu-Goldstone bosons that emerge in various theories beyond the standard model. These particles can interact with high-energy photons in external magnetic fields, influencing the observed gamma-ray spectrum. This study analyzes 41.3 hrs of observational data from the Perseus Galaxy Cluster collected with the MAGIC telescopes. We focused on the spectra the radio galaxy in the center of the cluster: NGC 1275. By modeling the magnetic field surrounding this target, we searched for spectral indications of ALP presence. Despite finding no statistical evidence of ALP signatures, we were able to exclude ALP models in the sub-micro electronvolt range. Our analysis improved upon previous work by calculating the full likelihood and statistical coverage for all considered models across the parameter space. Consequently, we achieved the most stringent limits to date for ALP masses around 50 neV, with cross sections down to $g_{a纬} = 3 \times 10^{-12}$ GeV$^{-1}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.07798v1-abstract-full').style.display = 'none'; document.getElementById('2401.07798v1-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 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">25 pages, 10 figures, accepted for publication in Physics of the Dark Universe</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.06525">arXiv:2401.06525</a> <span> [<a href="https://arxiv.org/pdf/2401.06525">pdf</a>, <a href="https://arxiv.org/format/2401.06525">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/10.1016/j.astropartphys.2023.102891">10.1016/j.astropartphys.2023.102891 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> EUSO-SPB1 Mission and Science </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Collaboration%2C+J">JEM-EUSO Collaboration</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Abdellaoui%2C+G">G. Abdellaoui</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Adams.%2C+J+H">J. H. Adams. Jr.</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Alonso%2C+G">G. Alonso</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Attallah%2C+R">R. Attallah</a>, <a href="/search/?searchtype=author&query=Attoui%2C+H">H. Attoui</a>, <a href="/search/?searchtype=author&query=Pernas%2C+M+A">M. Ave Pernas</a>, <a href="/search/?searchtype=author&query=Bachmann%2C+R">R. Bachmann</a>, <a href="/search/?searchtype=author&query=Bacholle%2C+S">S. Bacholle</a>, <a href="/search/?searchtype=author&query=Bagheri%2C+M">M. Bagheri</a>, <a href="/search/?searchtype=author&query=Bakiri%2C+M">M. Bakiri</a>, <a href="/search/?searchtype=author&query=Bal%C3%A1z%2C+J">J. Bal谩z</a>, <a href="/search/?searchtype=author&query=Barghini%2C+D">D. Barghini</a>, <a href="/search/?searchtype=author&query=Bartocci%2C+S">S. Bartocci</a>, <a href="/search/?searchtype=author&query=Battisti%2C+M">M. Battisti</a>, <a href="/search/?searchtype=author&query=Bayer%2C+J">J. Bayer</a>, <a href="/search/?searchtype=author&query=Beldjilali%2C+B">B. Beldjilali</a>, <a href="/search/?searchtype=author&query=Belenguer%2C+T">T. Belenguer</a> , et al. (271 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="2401.06525v1-abstract-short" style="display: inline;"> The Extreme Universe Space Observatory on a Super Pressure Balloon 1 (EUSO-SPB1) was launched in 2017 April from Wanaka, New Zealand. The plan of this mission of opportunity on a NASA super pressure balloon test flight was to circle the southern hemisphere. The primary scientific goal was to make the first observations of ultra-high-energy cosmic-ray extensive air showers (EASs) by looking down on… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.06525v1-abstract-full').style.display = 'inline'; document.getElementById('2401.06525v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.06525v1-abstract-full" style="display: none;"> The Extreme Universe Space Observatory on a Super Pressure Balloon 1 (EUSO-SPB1) was launched in 2017 April from Wanaka, New Zealand. The plan of this mission of opportunity on a NASA super pressure balloon test flight was to circle the southern hemisphere. The primary scientific goal was to make the first observations of ultra-high-energy cosmic-ray extensive air showers (EASs) by looking down on the atmosphere with an ultraviolet (UV) fluorescence telescope from suborbital altitude (33~km). After 12~days and 4~hours aloft, the flight was terminated prematurely in the Pacific Ocean. Before the flight, the instrument was tested extensively in the West Desert of Utah, USA, with UV point sources and lasers. The test results indicated that the instrument had sensitivity to EASs of approximately 3 EeV. Simulations of the telescope system, telescope on time, and realized flight trajectory predicted an observation of about 1 event assuming clear sky conditions. The effects of high clouds were estimated to reduce this value by approximately a factor of 2. A manual search and a machine-learning-based search did not find any EAS signals in these data. Here we review the EUSO-SPB1 instrument and flight and the EAS search. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.06525v1-abstract-full').style.display = 'none'; document.getElementById('2401.06525v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <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, 19 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astropart Phys 154 (2024) 102891 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.04559">arXiv:2401.04559</a> <span> [<a href="https://arxiv.org/pdf/2401.04559">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Disordered Systems and Neural Networks">cond-mat.dis-nn</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Biological Physics">physics.bio-ph</span> </div> </div> <p class="title is-5 mathjax"> Information bath and learning processes along geodesics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Barua%2C+A">Arnab Barua</a>, <a href="/search/?searchtype=author&query=Hatzikirou%2C+H">Haralampos Hatzikirou</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">Sumiyoshi Abe</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.04559v1-abstract-short" style="display: inline;"> Learning is a fundamental characteristic of living systems, enabling them to comprehend their environments and make informed decisions. These decision-making processes are inherently influenced by available information about their surroundings and specific objectives. An intriguing perspective is that each process could be optimal under a given set of conditions. Here, a geometric method is introd… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.04559v1-abstract-full').style.display = 'inline'; document.getElementById('2401.04559v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.04559v1-abstract-full" style="display: none;"> Learning is a fundamental characteristic of living systems, enabling them to comprehend their environments and make informed decisions. These decision-making processes are inherently influenced by available information about their surroundings and specific objectives. An intriguing perspective is that each process could be optimal under a given set of conditions. Here, a geometric method is introduced for analytically exploring such a perspective. The probability distribution describing the state of the composite system of the environment, termed the information bath, and a decision-maker is discussed on the basis of the entropic concept. This enables one to study the system in analogy with thermodynamics. Learning processes are expressed as the changes of parameters contained in the distribution. For a geometric interpretation of the processes, the manifold endowed with the Fisher-Rao metric as the Riemannian metric is considered. This framework allows one to conceptualize the optimality of each process as a state change along a geodesic curve on the manifold, which is referred to here as geodesic learning. Then, the bivariate Gaussian model is presented for illustrating this approach, and its rigorous solution is obtained. There, the correspondence between learning and cooling is made manifest. Evolution of the entropy is evaluated for geodesic learning. The findings are then interpreted in the context of adaptation. Geodesic learning plays a role of the case of reference and may give novel insights into the mechanics of learning in living systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.04559v1-abstract-full').style.display = 'none'; document.getElementById('2401.04559v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, no 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/2312.10732">arXiv:2312.10732</a> <span> [<a href="https://arxiv.org/pdf/2312.10732">pdf</a>, <a href="https://arxiv.org/format/2312.10732">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> First characterization of the emission behavior of Mrk421 from radio to VHE gamma rays with simultaneous X-ray polarization measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Abhir%2C+J">J. Abhir</a>, <a href="/search/?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/?searchtype=author&query=Baquero%2C+A">A. Baquero</a>, <a href="/search/?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a>, <a href="/search/?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/?searchtype=author&query=Bernete%2C+J">J. Bernete</a>, <a href="/search/?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/?searchtype=author&query=Besenrieder%2C+J">J. Besenrieder</a>, <a href="/search/?searchtype=author&query=Bigongiari%2C+C">C. Bigongiari</a>, <a href="/search/?searchtype=author&query=Biland%2C+A">A. Biland</a> , et al. (229 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.10732v1-abstract-short" style="display: inline;"> We perform the first broadband study of Mrk421 from radio to TeV gamma rays with simultaneous measurements of the X-ray polarization from IXPE. The data were collected within an extensive multiwavelength campaign organized between May and June 2022 using MAGIC, Fermi-LAT, NuSTAR, XMM-Newton, Swift, and several optical and radio telescopes to complement IXPE. During the IXPE exposures, the measured… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.10732v1-abstract-full').style.display = 'inline'; document.getElementById('2312.10732v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.10732v1-abstract-full" style="display: none;"> We perform the first broadband study of Mrk421 from radio to TeV gamma rays with simultaneous measurements of the X-ray polarization from IXPE. The data were collected within an extensive multiwavelength campaign organized between May and June 2022 using MAGIC, Fermi-LAT, NuSTAR, XMM-Newton, Swift, and several optical and radio telescopes to complement IXPE. During the IXPE exposures, the measured 0.2-1 TeV flux is close to the quiescent state and ranges from 25% to 50% of the Crab Nebula without intra-night variability. Throughout the campaign, the VHE and X-ray emission are positively correlated at a $4蟽$ significance level. The IXPE measurements unveil a X-ray polarization degree that is a factor of 2-5 higher than in the optical/radio bands; that implies an energy-stratified jet in which the VHE photons are emitted co-spatially with the X-rays, in the vicinity of a shock front. The June 2022 observations exhibit a rotation of the X-ray polarization angle. Despite no simultaneous VHE coverage being available during a large fraction of the swing, the Swift-XRT monitoring unveils an X-ray flux increase with a clear spectral hardening. It suggests that flares in high synchrotron peaked blazars can be accompanied by a polarization angle rotation, as observed in some flat spectrum radio quasars. Finally, during the polarization angle rotation, NuSTAR data reveal two contiguous spectral hysteresis loops in opposite directions (clockwise and counter-clockwise), implying important changes in the particle acceleration efficiency on $\sim$hour timescales. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.10732v1-abstract-full').style.display = 'none'; document.getElementById('2312.10732v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy & Astrophysics. 29 pages, 22 figures. Corresponding authors: Axel Arbet Engels, Felix Schmuckermaier, David Paneque</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.08204">arXiv:2312.08204</a> <span>  </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"> JEM-EUSO Collaboration contributions to the 38th International Cosmic Ray Conference </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Adams%2C+J+H">J. H. Adams Jr.</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Alldredge%2C+P">P. Alldredge</a>, <a href="/search/?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/?searchtype=author&query=Bagheri%2C+M">M. Bagheri</a>, <a href="/search/?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/?searchtype=author&query=Barghini%2C+D">D. Barghini</a>, <a href="/search/?searchtype=author&query=Battisti%2C+M">M. Battisti</a>, <a href="/search/?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/?searchtype=author&query=Belov%2C+A+A">A. A. Belov</a>, <a href="/search/?searchtype=author&query=Bertaina%2C+M">M. Bertaina</a>, <a href="/search/?searchtype=author&query=Bertone%2C+P+F">P. F. Bertone</a>, <a href="/search/?searchtype=author&query=Bianciotto%2C+M">M. Bianciotto</a>, <a href="/search/?searchtype=author&query=Bisconti%2C+F">F. Bisconti</a>, <a href="/search/?searchtype=author&query=Blaksley%2C+C">C. Blaksley</a>, <a href="/search/?searchtype=author&query=Blin-Bondil%2C+S">S. Blin-Bondil</a>, <a href="/search/?searchtype=author&query=Bolmgren%2C+K">K. Bolmgren</a>, <a href="/search/?searchtype=author&query=Briz%2C+S">S. Briz</a>, <a href="/search/?searchtype=author&query=Burton%2C+J">J. Burton</a>, <a href="/search/?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/?searchtype=author&query=Cambi%C3%A8%2C+G">G. Cambi猫</a> , et al. (133 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.08204v1-abstract-short" style="display: inline;"> This is a collection of papers presented by the JEM-EUSO Collaboration at the 38th International Cosmic Ray Conference (Nagoya, Japan, July 26-August 3, 2023) </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.08204v1-abstract-full" style="display: none;"> This is a collection of papers presented by the JEM-EUSO Collaboration at the 38th International Cosmic Ray Conference (Nagoya, Japan, July 26-August 3, 2023) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.08204v1-abstract-full').style.display = 'none'; document.getElementById('2312.08204v1-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.01583">arXiv:2312.01583</a> <span> [<a href="https://arxiv.org/pdf/2312.01583">pdf</a>, <a href="https://arxiv.org/format/2312.01583">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Robotics">cs.RO</span> </div> </div> <p class="title is-5 mathjax"> Efficient Collision Detection Oriented Motion Primitives for Path Planning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=DallaLibera%2C+F">Fabio DallaLibera</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">Shinya Abe</a>, <a href="/search/?searchtype=author&query=Ando%2C+T">Takeshi Ando</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.01583v2-abstract-short" style="display: inline;"> Mobile robots in dynamic environments require fast planning, especially when onboard computational resources are limited. While classic potential field based algorithms may suffice in simple scenarios, in most cases algorithms able to escape local minima are necessary. Configuration-space search algorithms have proven to provide a good trade-off between quality of the solutions and search time. Li… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.01583v2-abstract-full').style.display = 'inline'; document.getElementById('2312.01583v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.01583v2-abstract-full" style="display: none;"> Mobile robots in dynamic environments require fast planning, especially when onboard computational resources are limited. While classic potential field based algorithms may suffice in simple scenarios, in most cases algorithms able to escape local minima are necessary. Configuration-space search algorithms have proven to provide a good trade-off between quality of the solutions and search time. Literature presents a wide variety of approaches that speed up this search by reducing the number of edges that need to be inspected. Much less attention was instead given to reducing the time necessary to evaluate the cost of a single edge. This paper addresses this point by associating edges to motion primitives that prioritize fast collision detection. We show how biarcs can be used as motion primitives that enable fast collision detection, while still providing smooth, tangent continuous paths. The proposed approach does not assume a disc shaped hitbox, making it appealing for all robots with very different width and length or for differential drive robots with active wheels located far from the robot's center. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.01583v2-abstract-full').style.display = 'none'; document.getElementById('2312.01583v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.12656">arXiv:2311.12656</a> <span> [<a href="https://arxiv.org/pdf/2311.12656">pdf</a>, <a href="https://arxiv.org/format/2311.12656">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 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/10.1140/epjc/s10052-023-12090-w">10.1140/epjc/s10052-023-12090-w <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Developments and results in the context of the JEM-EUSO program obtained with the ESAF Simulation and Analysis Framework </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Adams%2C+J+H">J. H. Adams Jr.</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Alldredge%2C+P">P. Alldredge</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/?searchtype=author&query=Barghini%2C+D">D. Barghini</a>, <a href="/search/?searchtype=author&query=Battisti%2C+M">M. Battisti</a>, <a href="/search/?searchtype=author&query=Bayer%2C+J">J. Bayer</a>, <a href="/search/?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/?searchtype=author&query=Belov%2C+A+A">A. A. Belov</a>, <a href="/search/?searchtype=author&query=Bertaina%2C+M">M. Bertaina</a>, <a href="/search/?searchtype=author&query=Bertone%2C+P+F">P. F. Bertone</a>, <a href="/search/?searchtype=author&query=Bianciotto%2C+M">M. Bianciotto</a>, <a href="/search/?searchtype=author&query=Biermann%2C+P+L">P. L. Biermann</a>, <a href="/search/?searchtype=author&query=Bisconti%2C+F">F. Bisconti</a>, <a href="/search/?searchtype=author&query=Blaksley%2C+C">C. Blaksley</a>, <a href="/search/?searchtype=author&query=Blin-Bondil%2C+S">S. Blin-Bondil</a>, <a href="/search/?searchtype=author&query=Bobik%2C+P">P. Bobik</a>, <a href="/search/?searchtype=author&query=Bolmgren%2C+K">K. Bolmgren</a>, <a href="/search/?searchtype=author&query=Briz%2C+S">S. Briz</a>, <a href="/search/?searchtype=author&query=Burton%2C+J">J. Burton</a>, <a href="/search/?searchtype=author&query=Cafagna%2C+F">F. Cafagna</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="2311.12656v1-abstract-short" style="display: inline;"> JEM--EUSO is an international program for the development of space-based Ultra-High Energy Cosmic Ray observatories. The program consists of a series of missions which are either under development or in the data analysis phase. All instruments are based on a wide-field-of-view telescope, which operates in the near-UV range, designed to detect the fluorescence light emitted by extensive air showers… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.12656v1-abstract-full').style.display = 'inline'; document.getElementById('2311.12656v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.12656v1-abstract-full" style="display: none;"> JEM--EUSO is an international program for the development of space-based Ultra-High Energy Cosmic Ray observatories. The program consists of a series of missions which are either under development or in the data analysis phase. All instruments are based on a wide-field-of-view telescope, which operates in the near-UV range, designed to detect the fluorescence light emitted by extensive air showers in the atmosphere. We describe the simulation software ESAFin the framework of the JEM--EUSO program and explain the physical assumptions used. We present here the implementation of the JEM--EUSO, POEMMA, K--EUSO, TUS, Mini--EUSO, EUSO--SPB1 and EUSO--TA configurations in ESAF. For the first time ESAF simulation outputs are compared with experimental data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.12656v1-abstract-full').style.display = 'none'; document.getElementById('2311.12656v1-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 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C 83, 1028 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.09676">arXiv:2311.09676</a> <span> [<a href="https://arxiv.org/pdf/2311.09676">pdf</a>, <a href="https://arxiv.org/format/2311.09676">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 - Experiment">hep-ex</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.physletb.2024.138846">10.1016/j.physletb.2024.138846 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Charged Excited States of Dark Matter with KamLAND-Zen </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=collaboration%2C+K">KamLAND-Zen collaboration</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Eizuka%2C+M">M. Eizuka</a>, <a href="/search/?searchtype=author&query=Futagi%2C+S">S. Futagi</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Goto%2C+S">S. Goto</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Kurasawa%2C+M">M. Kurasawa</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Miyake%2C+H">H. Miyake</a>, <a href="/search/?searchtype=author&query=Morita%2C+D">D. Morita</a>, <a href="/search/?searchtype=author&query=Nakahata%2C+T">T. Nakahata</a> , et al. (44 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.09676v2-abstract-short" style="display: inline;"> Particle dark matter could belong to a multiplet that includes an electrically charged state. WIMP dark matter ($蠂^{0}$) accompanied by a negatively charged excited state ($蠂^{-}$) with a small mass difference (e.g. $<$ 20 MeV) can form a bound-state with a nucleus such as xenon. This bound-state formation is rare and the released energy is $\mathcal{O}(1-10$) MeV depending on the nucleus, making… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.09676v2-abstract-full').style.display = 'inline'; document.getElementById('2311.09676v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.09676v2-abstract-full" style="display: none;"> Particle dark matter could belong to a multiplet that includes an electrically charged state. WIMP dark matter ($蠂^{0}$) accompanied by a negatively charged excited state ($蠂^{-}$) with a small mass difference (e.g. $<$ 20 MeV) can form a bound-state with a nucleus such as xenon. This bound-state formation is rare and the released energy is $\mathcal{O}(1-10$) MeV depending on the nucleus, making large liquid scintillator detectors suitable for detection. We searched for bound-state formation events with xenon in two experimental phases of the KamLAND-Zen experiment, a xenon-doped liquid scintillator detector. No statistically significant events were observed. For a benchmark parameter set of WIMP mass $m_{蠂^{0}} = 1$ TeV and mass difference $螖m = 17$ MeV, we set the most stringent upper limits on the recombination cross section times velocity $\langle蟽v\rangle$ and the decay-width of $蠂^{-}$ to $9.2 \times 10^{-30}$ ${\rm cm^3/s}$ and $8.7 \times 10^{-14}$ GeV, respectively at 90% confidence level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.09676v2-abstract-full').style.display = 'none'; document.getElementById('2311.09676v2-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Lett. B 855 (2024) 138846 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.10394">arXiv:2310.10394</a> <span> [<a href="https://arxiv.org/pdf/2310.10394">pdf</a>, <a href="https://arxiv.org/format/2310.10394">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 Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.109.036009">10.1103/PhysRevD.109.036009 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Nuclear deexcitation simulator for neutrino interactions and nucleon decays of $^{12}\text{C}$ and $^{16}\text{O}$ based on TALYS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">Seisho Abe</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.10394v2-abstract-short" style="display: inline;"> Nuclear deexcitation associated with neutrino interactions and nucleon decays has a significant impact on a recent key observable for neutrino detectors: neutron multiplicity. However, most existing neutrino Monte Carlo event generators do not consider this process. For a comprehensive prediction of the neutron multiplicity, a nuclear deexcitation simulator based on TALYS named NucDeEx is develope… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.10394v2-abstract-full').style.display = 'inline'; document.getElementById('2310.10394v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.10394v2-abstract-full" style="display: none;"> Nuclear deexcitation associated with neutrino interactions and nucleon decays has a significant impact on a recent key observable for neutrino detectors: neutron multiplicity. However, most existing neutrino Monte Carlo event generators do not consider this process. For a comprehensive prediction of the neutron multiplicity, a nuclear deexcitation simulator based on TALYS named NucDeEx is developed. NucDeEx can be used for neutrino interactions and nucleon decayes for $^{12}\text{C}$ and $^{16}\text{O}$. The author provides the NucDeEx codes and sample codes for applying the NucDeex to widely-used neutrino Monte Carlo event generators, NEUT, NuWro, and GENIE. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.10394v2-abstract-full').style.display = 'none'; document.getElementById('2310.10394v2-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 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">Journal ref:</span> Phys. Rev. D 109, 036009 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.07413">arXiv:2310.07413</a> <span> [<a href="https://arxiv.org/pdf/2310.07413">pdf</a>, <a href="https://arxiv.org/format/2310.07413">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"> Chasing Gravitational Waves with the Cherenkov Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Green%2C+J+G">Jarred Gershon Green</a>, <a href="/search/?searchtype=author&query=Carosi%2C+A">Alessandro Carosi</a>, <a href="/search/?searchtype=author&query=Nava%2C+L">Lara Nava</a>, <a href="/search/?searchtype=author&query=Patricelli%2C+B">Barbara Patricelli</a>, <a href="/search/?searchtype=author&query=Sch%C3%BCssler%2C+F">Fabian Sch眉ssler</a>, <a href="/search/?searchtype=author&query=Seglar-Arroyo%2C+M">Monica Seglar-Arroyo</a>, <a href="/search/?searchtype=author&query=Consortium%2C+C">Cta Consortium</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Abe%2C+K">Kazuki Abe</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">Shotaro Abe</a>, <a href="/search/?searchtype=author&query=Acharyya%2C+A">Atreya Acharyya</a>, <a href="/search/?searchtype=author&query=Adam%2C+R">Remi Adam</a>, <a href="/search/?searchtype=author&query=Aguasca-Cabot%2C+A">Arnau Aguasca-Cabot</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">Ivan Agudo</a>, <a href="/search/?searchtype=author&query=Alfaro%2C+J">Jorge Alfaro</a>, <a href="/search/?searchtype=author&query=Alvarez-Crespo%2C+N">Nuria Alvarez-Crespo</a>, <a href="/search/?searchtype=author&query=Batista%2C+R+A">Rafael Alves Batista</a>, <a href="/search/?searchtype=author&query=Amans%2C+J">Jean-Philippe Amans</a>, <a href="/search/?searchtype=author&query=Amato%2C+E">Elena Amato</a>, <a href="/search/?searchtype=author&query=Ambrosino%2C+F">Filippo Ambrosino</a>, <a href="/search/?searchtype=author&query=Ang%C3%BCner%2C+E+O">Ekrem Oguzhan Ang眉ner</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">Lucio Angelo Antonelli</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">Carla Aramo</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">Cornelia Arcaro</a>, <a href="/search/?searchtype=author&query=Arrabito%2C+L">Luisa Arrabito</a> , et al. (545 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="2310.07413v3-abstract-short" style="display: inline;"> The detection of gravitational waves from a binary neutron star merger by Advanced LIGO and Advanced Virgo (GW170817), along with the discovery of the electromagnetic counterparts of this gravitational wave event, ushered in a new era of multimessenger astronomy, providing the first direct evidence that BNS mergers are progenitors of short gamma-ray bursts (GRBs). Such events may also produce very… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.07413v3-abstract-full').style.display = 'inline'; document.getElementById('2310.07413v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.07413v3-abstract-full" style="display: none;"> The detection of gravitational waves from a binary neutron star merger by Advanced LIGO and Advanced Virgo (GW170817), along with the discovery of the electromagnetic counterparts of this gravitational wave event, ushered in a new era of multimessenger astronomy, providing the first direct evidence that BNS mergers are progenitors of short gamma-ray bursts (GRBs). Such events may also produce very-high-energy (VHE, > 100GeV) photons which have yet to be detected in coincidence with a gravitational wave signal. The Cherenkov Telescope Array (CTA) is a next-generation VHE observatory which aims to be indispensable in this search, with an unparalleled sensitivity and ability to slew anywhere on the sky within a few tens of seconds. New observing modes and follow-up strategies are being developed for CTA to rapidly cover localization areas of gravitational wave events that are typically larger than the CTA field of view. This work will evaluate and provide estimations on the expected number of of gravitational wave events that will be observable with CTA, considering both on- and off-axis emission. In addition, we will present and discuss the prospects of potential follow-up strategies with CTA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.07413v3-abstract-full').style.display = 'none'; document.getElementById('2310.07413v3-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 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">Presented at the 38th International Cosmic Ray Conference (ICRC 2023), 2023 (arXiv:2309.08219)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> CTA-ICRC/2023/30 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.06473">arXiv:2310.06473</a> <span> [<a href="https://arxiv.org/pdf/2310.06473">pdf</a>, <a href="https://arxiv.org/format/2310.06473">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/stad2958">10.1093/mnras/stad2958 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MAGIC detection of GRB 201216C at $z=1.1$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Baack%2C+D">D. Baack</a>, <a href="/search/?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/?searchtype=author&query=Baquero%2C+A">A. Baquero</a>, <a href="/search/?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a>, <a href="/search/?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/?searchtype=author&query=Bernete%2C+J">J. Bernete</a>, <a href="/search/?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/?searchtype=author&query=Besenrieder%2C+J">J. Besenrieder</a>, <a href="/search/?searchtype=author&query=Bigongiari%2C+C">C. Bigongiari</a> , et al. (195 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="2310.06473v1-abstract-short" style="display: inline;"> Gamma-ray bursts (GRBs) are explosive transient events occurring at cosmological distances, releasing a large amount of energy as electromagnetic radiation over several energy bands. We report the detection of the long GRB~201216C by the MAGIC telescopes. The source is located at $z=1.1$ and thus it is the farthest one detected at very high energies. The emission above \SI{70}{\GeV} of GRB~201216C… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06473v1-abstract-full').style.display = 'inline'; document.getElementById('2310.06473v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.06473v1-abstract-full" style="display: none;"> Gamma-ray bursts (GRBs) are explosive transient events occurring at cosmological distances, releasing a large amount of energy as electromagnetic radiation over several energy bands. We report the detection of the long GRB~201216C by the MAGIC telescopes. The source is located at $z=1.1$ and thus it is the farthest one detected at very high energies. The emission above \SI{70}{\GeV} of GRB~201216C is modelled together with multi-wavelength data within a synchrotron and synchrotron-self Compton (SSC) scenario. We find that SSC can explain the broadband data well from the optical to the very-high-energy band. For the late-time radio data, a different component is needed to account for the observed emission. Differently from previous GRBs detected in the very-high-energy range, the model for GRB~201216C strongly favors a wind-like medium. The model parameters have values similar to those found in past studies of the afterglows of GRBs detected up to GeV energies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06473v1-abstract-full').style.display = 'none'; document.getElementById('2310.06473v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 October, 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">13 pages, 6 figures, 2 tables. Accepted for publication in Monthly Notices of the Royal Astronomical Society</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Monthly Notices of the Royal Astronomical Society, Volume 527, Issue 3, January 2024, Pages 5856-5867 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.03922">arXiv:2310.03922</a> <span> [<a href="https://arxiv.org/pdf/2310.03922">pdf</a>, <a href="https://arxiv.org/format/2310.03922">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/10.1051/0004-6361/202347845">10.1051/0004-6361/202347845 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multi-year characterisation of the broad-band emission from the intermittent extreme BL Lac 1ES~2344+514 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Baack%2C+D">D. Baack</a>, <a href="/search/?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/?searchtype=author&query=Baquero%2C+A">A. Baquero</a>, <a href="/search/?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a>, <a href="/search/?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/?searchtype=author&query=Bernete%2C+J">J. Bernete</a>, <a href="/search/?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/?searchtype=author&query=Besenrieder%2C+J">J. Besenrieder</a>, <a href="/search/?searchtype=author&query=Bigongiari%2C+C">C. Bigongiari</a>, <a href="/search/?searchtype=author&query=Biland%2C+A">A. Biland</a>, <a href="/search/?searchtype=author&query=Blanch%2C+O">O. Blanch</a> , et al. (210 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="2310.03922v1-abstract-short" style="display: inline;"> The BL Lac 1ES 2344+514 is known for temporary extreme properties (e.g., a shift of the synchrotron SED peak energy $谓_{synch,p}$ above 1keV). While those extreme states were so far observed only during high flux levels, additional multi-year observing campaigns are required to achieve a coherent picture. Here, we report the longest investigation of the source from radio to VHE performed so far, f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.03922v1-abstract-full').style.display = 'inline'; document.getElementById('2310.03922v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.03922v1-abstract-full" style="display: none;"> The BL Lac 1ES 2344+514 is known for temporary extreme properties (e.g., a shift of the synchrotron SED peak energy $谓_{synch,p}$ above 1keV). While those extreme states were so far observed only during high flux levels, additional multi-year observing campaigns are required to achieve a coherent picture. Here, we report the longest investigation of the source from radio to VHE performed so far, focusing on a systematic characterisation of the intermittent extreme states. While our results confirm that 1ES 2344+514 typically exhibits $谓_{synch,p}>$1keV during elevated flux periods, we also find periods where the extreme state coincides with low flux activity. A strong spectral variability thus happens in the quiescent state, and is likely caused by an increase of the electron acceleration efficiency without a change in the electron injection luminosity. We also report a strong X-ray flare (among the brightest for 1ES 2344+514) without a significant shift of $谓_{synch,p}$. During this particular flare, the X-ray spectrum is among the softest of the campaign. It unveils complexity in the spectral evolution, where the common harder-when-brighter trend observed in BL Lacs is violated. During a low and hard X-ray state, we find an excess of the UV flux with respect to an extrapolation of the X-ray spectrum to lower energies. This UV excess implies that at least two regions contribute significantly to the infrared/optical/ultraviolet/X-ray emission. Using the simultaneous MAGIC, XMM-Newton, NuSTAR, and AstroSat observations, we argue that a region possibly associated with the 10 GHz radio core may explain such an excess. Finally, we investigate a VHE flare, showing an absence of simultaneous variability in the 0.3-2keV band. Using a time-dependent leptonic modelling, we show that this behaviour, in contradiction to single-zone scenarios, can instead be explained by a two-component model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.03922v1-abstract-full').style.display = 'none'; document.getElementById('2310.03922v1-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 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">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 682, A114 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.03307">arXiv:2310.03307</a> <span> [<a href="https://arxiv.org/pdf/2310.03307">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1021/acs.jpca.3c06841">10.1021/acs.jpca.3c06841 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Kinetic Modeling Analysis of Ar Addition to Atmospheric Pressure N2-H2 Plasma for Plasma-Assisted Catalytic Synthesis of NH3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lin%2C+Z">Zihan Lin</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">Shota Abe</a>, <a href="/search/?searchtype=author&query=Chen%2C+Z">Zhe Chen</a>, <a href="/search/?searchtype=author&query=Jaiswal%2C+S">Surabhi Jaiswal</a>, <a href="/search/?searchtype=author&query=Koel%2C+B+E">Bruce E. Koel</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.03307v1-abstract-short" style="display: inline;"> Zero-dimensional kinetic modeling of atmospheric pressure Ar-N2-H2 nonthermal plasma was carried out to gain mechanistic insights into ammonia formation during plasma-assisted catalysis of ammonia synthesis. The kinetic model was developed for a coaxial dielectric barrier discharge (DBD) quartz wool-packed bed reactor operating at near room temperature using a kHz-frequency plasma source. With 30%… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.03307v1-abstract-full').style.display = 'inline'; document.getElementById('2310.03307v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.03307v1-abstract-full" style="display: none;"> Zero-dimensional kinetic modeling of atmospheric pressure Ar-N2-H2 nonthermal plasma was carried out to gain mechanistic insights into ammonia formation during plasma-assisted catalysis of ammonia synthesis. The kinetic model was developed for a coaxial dielectric barrier discharge (DBD) quartz wool-packed bed reactor operating at near room temperature using a kHz-frequency plasma source. With 30% Ar mixed in a 1:1 N2-H2 plasma at 760 Torr, we find that NH3 production is dominated by Eley-Rideal (E-R) surface reactions, which heavily involve surface NHx species derived from N and H radicals in the gas phase, while the influence of excited N2 molecules is negligible. This is contrary to the commonly proposed mechanism that excited N2 molecules created by Penning excitation of N2 by Ar (4s) and Ar(4p) plays a significant role in assisting NH3 formation. Our model shows that the enhanced NH3 formation upon Ar dilution is unlikely due to the interactions between Ar and H species, as excited Ar atoms have a weak effect on H radical formation through H2 dissociation compared to electrons. We find that excited Ar atoms contribute to 28% of the N radical production in the gas phase via N2 dissociation, while the rest is dominated by electron-impact dissociation. Furthermore, Ar species play a negligible role in the product NH3 dissociation. N2 conversion sensitivity analyses were carried out for electron density (ne) and reduced electric field (E/N), and contributions from Ar to gas-phase N radical production were quantified. The model can provide guidance on potential reasons for observing enhanced NH3 formation upon Ar dilution in N2-H2 plasmas beyond changes to the discharge characteristics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.03307v1-abstract-full').style.display = 'none'; document.getElementById('2310.03307v1-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 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">5 figures, 3 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.01954">arXiv:2310.01954</a> <span> [<a href="https://arxiv.org/pdf/2310.01954">pdf</a>, <a href="https://arxiv.org/format/2310.01954">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/10.1051/0004-6361/202346927">10.1051/0004-6361/202346927 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Performance of the joint LST-1 and MAGIC observations evaluated with Crab Nebula data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Crespo%2C+N+A">N. Alvarez Crespo</a>, <a href="/search/?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Arbet-Engels%2C+A">A. Arbet-Engels</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Aubert%2C+P">P. Aubert</a>, <a href="/search/?searchtype=author&query=Baack%2C+D">D. Baack</a>, <a href="/search/?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/?searchtype=author&query=Baktash%2C+A">A. Baktash</a>, <a href="/search/?searchtype=author&query=Bamba%2C+A">A. Bamba</a>, <a href="/search/?searchtype=author&query=Larriva%2C+A+B">A. Baquero Larriva</a>, <a href="/search/?searchtype=author&query=Baroncelli%2C+L">L. Baroncelli</a>, <a href="/search/?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a> , et al. (344 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="2310.01954v1-abstract-short" style="display: inline;"> Aims. LST-1, the prototype of the Large-Sized Telescope for the upcoming Cherenkov Telescope Array Observatory, is concluding its commissioning in Observatorio del Roque de los Muchachos on the island of La Palma. The proximity of LST-1 (Large-Sized Telescope 1) to the two MAGIC (Major Atmospheric Gamma Imaging Cherenkov) telescopes permits observations of the same gamma-ray events with both syste… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.01954v1-abstract-full').style.display = 'inline'; document.getElementById('2310.01954v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.01954v1-abstract-full" style="display: none;"> Aims. LST-1, the prototype of the Large-Sized Telescope for the upcoming Cherenkov Telescope Array Observatory, is concluding its commissioning in Observatorio del Roque de los Muchachos on the island of La Palma. The proximity of LST-1 (Large-Sized Telescope 1) to the two MAGIC (Major Atmospheric Gamma Imaging Cherenkov) telescopes permits observations of the same gamma-ray events with both systems. Methods. We describe the joint LST-1+MAGIC analysis pipeline and use simultaneous Crab Nebula observations and Monte Carlo simulations to assess the performance of the three-telescope system. The addition of the LST-1 telescope allows the recovery of events in which one of the MAGIC images is too dim to survive analysis quality cuts. Results. Thanks to the resulting increase in the collection area and stronger background rejection, we find a significant improvement in sensitivity, allowing the detection of 30% weaker fluxes in the energy range between 200 GeV and 3 TeV. The spectrum of the Crab Nebula, reconstructed in the energy range ~60 GeV to ~10 TeV, is in agreement with previous measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.01954v1-abstract-full').style.display = 'none'; document.getElementById('2310.01954v1-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 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">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 680, A66 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.03712">arXiv:2309.03712</a> <span> [<a href="https://arxiv.org/pdf/2309.03712">pdf</a>, <a href="https://arxiv.org/format/2309.03712">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2024/10/004">10.1088/1475-7516/2024/10/004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Prospects for $纬$-ray observations of the Perseus galaxy cluster with the Cherenkov Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Consortium%2C+T+C+T+A">The Cherenkov Telescope Array Consortium</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Aguirre-Santaella%2C+A">A. Aguirre-Santaella</a>, <a href="/search/?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/?searchtype=author&query=Alvarez-Crespo%2C+N">N. Alvarez-Crespo</a>, <a href="/search/?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/?searchtype=author&query=Amans%2C+J+-">J. -P. Amans</a>, <a href="/search/?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Araya%2C+M">M. Araya</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Arrabito%2C+L">L. Arrabito</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Ascas%C3%ADbar%2C+Y">Y. Ascas铆bar</a>, <a href="/search/?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a> , et al. (542 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="2309.03712v1-abstract-short" style="display: inline;"> Galaxy clusters are expected to be dark matter (DM) reservoirs and storage rooms for the cosmic-ray protons (CRp) that accumulate along the cluster's formation history. Accordingly, they are excellent targets to search for signals of DM annihilation and decay at gamma-ray energies and are predicted to be sources of large-scale gamma-ray emission due to hadronic interactions in the intracluster med… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03712v1-abstract-full').style.display = 'inline'; document.getElementById('2309.03712v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.03712v1-abstract-full" style="display: none;"> Galaxy clusters are expected to be dark matter (DM) reservoirs and storage rooms for the cosmic-ray protons (CRp) that accumulate along the cluster's formation history. Accordingly, they are excellent targets to search for signals of DM annihilation and decay at gamma-ray energies and are predicted to be sources of large-scale gamma-ray emission due to hadronic interactions in the intracluster medium. We estimate the sensitivity of the Cherenkov Telescope Array (CTA) to detect diffuse gamma-ray emission from the Perseus galaxy cluster. We perform a detailed spatial and spectral modelling of the expected signal for the DM and the CRp components. For each, we compute the expected CTA sensitivity. The observing strategy of Perseus is also discussed. In the absence of a diffuse signal (non-detection), CTA should constrain the CRp to thermal energy ratio within the radius $R_{500}$ down to about $X_{500}<3\times 10^{-3}$, for a spatial CRp distribution that follows the thermal gas and a CRp spectral index $伪_{\rm CRp}=2.3$. Under the optimistic assumption of a pure hadronic origin of the Perseus radio mini-halo and depending on the assumed magnetic field profile, CTA should measure $伪_{\rm CRp}$ down to about $螖伪_{\rm CRp}\simeq 0.1$ and the CRp spatial distribution with 10% precision. Regarding DM, CTA should improve the current ground-based gamma-ray DM limits from clusters observations on the velocity-averaged annihilation cross-section by a factor of up to $\sim 5$, depending on the modelling of DM halo substructure. In the case of decay of DM particles, CTA will explore a new region of the parameter space, reaching models with $蟿_蠂>10^{27}$s for DM masses above 1 TeV. These constraints will provide unprecedented sensitivity to the physics of both CRp acceleration and transport at cluster scale and to TeV DM particle models, especially in the decay scenario. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03712v1-abstract-full').style.display = 'none'; document.getElementById('2309.03712v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">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">93 pages (including author list, appendix and references), 143 figures. Submitted to JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP10(2024)004 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.16358">arXiv:2308.16358</a> <span> [<a href="https://arxiv.org/pdf/2308.16358">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Materials Science">cond-mat.mtrl-sci</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.jnucmat.2024.154942">10.1016/j.jnucmat.2024.154942 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Investigation of W-SiC compositionally graded films as a divertor material </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lin%2C+Z">Zihan Lin</a>, <a href="/search/?searchtype=author&query=Monton%2C+C">Carlos Monton</a>, <a href="/search/?searchtype=author&query=Bringuier%2C+S">Stefan Bringuier</a>, <a href="/search/?searchtype=author&query=Sinclair%2C+G">Gregory Sinclair</a>, <a href="/search/?searchtype=author&query=Cheng%2C+G">Guangming Cheng</a>, <a href="/search/?searchtype=author&query=Marin%2C+E">Eduardo Marin</a>, <a href="/search/?searchtype=author&query=Bergstrom%2C+Z">Zachary Bergstrom</a>, <a href="/search/?searchtype=author&query=Rudakov%2C+D">Dmitry Rudakov</a>, <a href="/search/?searchtype=author&query=Popovi%C4%87%2C+%C5%BD">沤ana Popovi膰</a>, <a href="/search/?searchtype=author&query=Losada%2C+U">Ulises Losada</a>, <a href="/search/?searchtype=author&query=Bykov%2C+I">Igor Bykov</a>, <a href="/search/?searchtype=author&query=Ostrowski%2C+E+T">Evan T. Ostrowski</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">Shota Abe</a>, <a href="/search/?searchtype=author&query=Yao%2C+N">Nan Yao</a>, <a href="/search/?searchtype=author&query=Koel%2C+B+E">Bruce E. Koel</a>, <a href="/search/?searchtype=author&query=Abrams%2C+T">Tyler Abrams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.16358v2-abstract-short" style="display: inline;"> W-SiC composite material is a promising plasma-facing material candidate alternative to pure W due to the low neutron activation, low impurity radiation, and low tritium diffusivity of SiC while leveraging the high erosion resistance of the W armor. Additionally, W and SiC have high thermomechanical compatibility given their similar thermal expansion rates. The present study addresses the synthesi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.16358v2-abstract-full').style.display = 'inline'; document.getElementById('2308.16358v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.16358v2-abstract-full" style="display: none;"> W-SiC composite material is a promising plasma-facing material candidate alternative to pure W due to the low neutron activation, low impurity radiation, and low tritium diffusivity of SiC while leveraging the high erosion resistance of the W armor. Additionally, W and SiC have high thermomechanical compatibility given their similar thermal expansion rates. The present study addresses the synthesis and performance of compositionally graded W-SiC films fabricated by pulsed-DC magnetron sputtering. Compositional gradients were characterized using transmission electron microscopy (TEM) and energy-dispersive X-ray spectroscopy (EDS), and crystallographic information was obtained using electron diffraction and X-ray diffraction (XRD). Samples were exposed to L-mode deuterium plasma discharges in the DIII-D tokamak using the Divertor Material Evaluation System (DiMES). Post-mortem characterizations were performed using scanning electron microscopy (SEM) and XRD. Electron diffraction and XRD showed that the compositionally graded W-SiC films were composed of polycrystalline W and amorphous SiC with amorphous W+SiC interlayers. No macroscopic delamination or microstructural changes were observed under mild exposure conditions. This study serves as a preliminary examination of W-SiC compositionally graded composites as a potential candidate divertor material in future tokamak devices. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.16358v2-abstract-full').style.display = 'none'; document.getElementById('2308.16358v2-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 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">Published in Journal of Nuclear Materials</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> J. Nucl. Mater. 592 (2024) 154942 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.01537">arXiv:2307.01537</a> <span> [<a href="https://arxiv.org/pdf/2307.01537">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Geophysics">physics.geo-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Statistical Mechanics">cond-mat.stat-mech</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/10.3390/e25070989">10.3390/e25070989 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Aftershocks and fluctuating diffusivity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">Sumiyoshi Abe</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+N">Norikazu Suzuki</a>, <a href="/search/?searchtype=author&query=Tayurskii%2C+D+A">Dmitrii A. Tayurskii</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="2307.01537v1-abstract-short" style="display: inline;"> The Omori-Utsu law shows the temporal power-law-like decrease of the frequency of earthquake aftershocks and, interestingly, is found in a variety of complex systems/phenomena exhibiting catastrophes. Now, it may be interpreted as a characteristic response of such systems to large events. Here, hierarchical dynamics with the fast and slow degrees of freedom is studied on the basis of the Fokker-Pl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.01537v1-abstract-full').style.display = 'inline'; document.getElementById('2307.01537v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.01537v1-abstract-full" style="display: none;"> The Omori-Utsu law shows the temporal power-law-like decrease of the frequency of earthquake aftershocks and, interestingly, is found in a variety of complex systems/phenomena exhibiting catastrophes. Now, it may be interpreted as a characteristic response of such systems to large events. Here, hierarchical dynamics with the fast and slow degrees of freedom is studied on the basis of the Fokker-Planck theory for the load-state distribution to formulate the law as a relaxation process, in which diffusion coefficient in the space of the load state is treated as a fluctuating slow variable. The evolution equation reduced from the full Fokker-Planck equation and its Green's function are analyzed for the subdynamics governing the load state as the fast degree of freedom. It is shown that the subsystem has the temporal translational invariance in the logarithmic time, not in the conventional time, and consequently the aging phenomenon appears. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.01537v1-abstract-full').style.display = 'none'; document.getElementById('2307.01537v1-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">25 pages, no figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Entropy 25, 989 (2023). open access </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.01526">arXiv:2307.01526</a> <span> [<a href="https://arxiv.org/pdf/2307.01526">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Geophysics">physics.geo-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Statistical Mechanics">cond-mat.stat-mech</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s11600-023-01102-8">10.1007/s11600-023-01102-8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Scaling and memory in seismological phenomena </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">Sumiyoshi Abe</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+N">Norikazu Suzuki</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="2307.01526v1-abstract-short" style="display: inline;"> The concept of memory is of central importance for characterizing complex systems and phenomena. Presence of long-term memories indicates how their dynamics can be less sensitive to initial conditions compared to the chaotic cases. On the other hand, it is empirically known that the Feller-Pareto distribution, which decays as the power law i.e. the scale-invariant nature, frequently appears as a s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.01526v1-abstract-full').style.display = 'inline'; document.getElementById('2307.01526v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.01526v1-abstract-full" style="display: none;"> The concept of memory is of central importance for characterizing complex systems and phenomena. Presence of long-term memories indicates how their dynamics can be less sensitive to initial conditions compared to the chaotic cases. On the other hand, it is empirically known that the Feller-Pareto distribution, which decays as the power law i.e. the scale-invariant nature, frequently appears as a statistical law generated by the dynamics of complex systems. However, it is generally not a simple task to determine if a system obeying such a power law possesses a high degree of complexity with a long-term memory. Here, a new method is proposed for characterization of memory. In particular, a scaling relation to be satisfied by any memoryless dynamics generating the Feller-Pareto power-law distribution is presented. Then, the method is applied to the real data of energies released by a series of earthquakes and acceleration of ground motion due to a strong earthquake. It is shown in this way that the sequence of the released energy in seismicity is memoryless in the event time, whereas that of acceleration is memoryful in the sampling time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.01526v1-abstract-full').style.display = 'none'; document.getElementById('2307.01526v1-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">22 pages, 4 figures, 2 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Acta Geophysica (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.12960">arXiv:2306.12960</a> <span> [<a href="https://arxiv.org/pdf/2306.12960">pdf</a>, <a href="https://arxiv.org/ps/2306.12960">ps</a>, <a href="https://arxiv.org/format/2306.12960">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ace89d">10.3847/1538-4357/ace89d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observations of the Crab Nebula and Pulsar with the Large-Sized Telescope Prototype of the Cherenkov Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Project%2C+C">CTA-LST Project</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Crespo%2C+N+A">N. Alvarez Crespo</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Arbet-Engels%2C+A">A. Arbet-Engels</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Aubert%2C+P">P. Aubert</a>, <a href="/search/?searchtype=author&query=Baktash%2C+A">A. Baktash</a>, <a href="/search/?searchtype=author&query=Bamba%2C+A">A. Bamba</a>, <a href="/search/?searchtype=author&query=Larriva%2C+A+B">A. Baquero Larriva</a>, <a href="/search/?searchtype=author&query=Baroncelli%2C+L">L. Baroncelli</a>, <a href="/search/?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/?searchtype=author&query=Batkovic%2C+I">I. Batkovic</a>, <a href="/search/?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a> , et al. (267 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="2306.12960v3-abstract-short" style="display: inline;"> CTA (Cherenkov Telescope Array) is the next generation ground-based observatory for gamma-ray astronomy at very-high energies. The Large-Sized Telescope prototype (LST-1) is located at the Northern site of CTA, on the Canary Island of La Palma. LSTs are designed to provide optimal performance in the lowest part of the energy range covered by CTA, down to $\simeq 20$ GeV. LST-1 started performing a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.12960v3-abstract-full').style.display = 'inline'; document.getElementById('2306.12960v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.12960v3-abstract-full" style="display: none;"> CTA (Cherenkov Telescope Array) is the next generation ground-based observatory for gamma-ray astronomy at very-high energies. The Large-Sized Telescope prototype (LST-1) is located at the Northern site of CTA, on the Canary Island of La Palma. LSTs are designed to provide optimal performance in the lowest part of the energy range covered by CTA, down to $\simeq 20$ GeV. LST-1 started performing astronomical observations in November 2019, during its commissioning phase, and it has been taking data since then. We present the first LST-1 observations of the Crab Nebula, the standard candle of very-high energy gamma-ray astronomy, and use them, together with simulations, to assess the basic performance parameters of the telescope. The data sample consists of around 36 hours of observations at low zenith angles collected between November 2020 and March 2022. LST-1 has reached the expected performance during its commissioning period - only a minor adjustment of the preexisting simulations was needed to match the telescope behavior. The energy threshold at trigger level is estimated to be around 20 GeV, rising to $\simeq 30$ GeV after data analysis. Performance parameters depend strongly on energy, and on the strength of the gamma-ray selection cuts in the analysis: angular resolution ranges from 0.12 to 0.40 degrees, and energy resolution from 15 to 50%. Flux sensitivity is around 1.1% of the Crab Nebula flux above 250 GeV for a 50-h observation (12% for 30 minutes). The spectral energy distribution (in the 0.03 - 30 TeV range) and the light curve obtained for the Crab Nebula agree with previous measurements, considering statistical and systematic uncertainties. A clear periodic signal is also detected from the pulsar at the center of the Nebula. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.12960v3-abstract-full').style.display = 'none'; document.getElementById('2306.12960v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 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 in ApJ. v3: updated author list and acknowledgements, fixed typos and other minor issues</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2023 ApJ 956 80 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.03923">arXiv:2304.03923</a> <span> [<a href="https://arxiv.org/pdf/2304.03923">pdf</a>, <a href="https://arxiv.org/ps/2304.03923">ps</a>, <a href="https://arxiv.org/format/2304.03923">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Materials Science">cond-mat.mtrl-sci</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/10.1088/1741-4326/acee98">10.1088/1741-4326/acee98 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> In-situ coating of silicon-rich films on tokamak plasma-facing components with real-time Si material injection </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Effenberg%2C+F">Florian Effenberg</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">Shota Abe</a>, <a href="/search/?searchtype=author&query=Sinclair%2C+G">Gregory Sinclair</a>, <a href="/search/?searchtype=author&query=Abrams%2C+T">Tyler Abrams</a>, <a href="/search/?searchtype=author&query=Bortolon%2C+A">Alessandro Bortolon</a>, <a href="/search/?searchtype=author&query=Wampler%2C+W+R">William R. Wampler</a>, <a href="/search/?searchtype=author&query=Laggner%2C+F+M">Florian M. Laggner</a>, <a href="/search/?searchtype=author&query=Rudakov%2C+D+L">Dmitry L. Rudakov</a>, <a href="/search/?searchtype=author&query=Bykov%2C+I">Igor Bykov</a>, <a href="/search/?searchtype=author&query=Lasnier%2C+C+J">Charles J. Lasnier</a>, <a href="/search/?searchtype=author&query=Mauzey%2C+D">David Mauzey</a>, <a href="/search/?searchtype=author&query=Nagy%2C+A">Alexander Nagy</a>, <a href="/search/?searchtype=author&query=Nazikian%2C+R">Raffi Nazikian</a>, <a href="/search/?searchtype=author&query=Scotti%2C+F">Filippo Scotti</a>, <a href="/search/?searchtype=author&query=Wang%2C+H">Huiqian Wang</a>, <a href="/search/?searchtype=author&query=Wilcox%2C+R+S">Robert S. Wilcox</a>, <a href="/search/?searchtype=author&query=Team%2C+t+D">the DIII-D Team</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="2304.03923v3-abstract-short" style="display: inline;"> Experiments have been conducted in the DIII-D tokamak to explore the in-situ growth of silicon-rich layers as a potential technique for real-time replenishment of surface coatings on plasma-facing components (PFCs) during steady-state long-pulse reactor operation. Silicon (Si) pellets of 1 mm diameter were injected into low- and high-confinement (L-mode and H-mode) plasma discharges with densities… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.03923v3-abstract-full').style.display = 'inline'; document.getElementById('2304.03923v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.03923v3-abstract-full" style="display: none;"> Experiments have been conducted in the DIII-D tokamak to explore the in-situ growth of silicon-rich layers as a potential technique for real-time replenishment of surface coatings on plasma-facing components (PFCs) during steady-state long-pulse reactor operation. Silicon (Si) pellets of 1 mm diameter were injected into low- and high-confinement (L-mode and H-mode) plasma discharges with densities ranging from $3.9-7.5\times10^{19}$ m$^{-3}$ and input powers ranging from $5.5-9$ MW. The small Si pellets were delivered with the impurity granule injector (IGI) at frequencies ranging from 4-16 Hz corresponding to mass flow rates of $5-19$ mg/s ($1-4.2\times10^{20}$ Si/s) at cumulative amounts of up to 34 mg of Si per five-second discharge. Graphite samples were exposed to the scrape-off layer and private flux region plasmas through the divertor material evaluation system (DiMES) to evaluate the Si deposition on the divertor targets. The Si II emission at the sample correlates with silicon injection and suggests net surface Si-deposition in measurable amounts. Post-mortem analysis showed Si-rich coatings containing silicon oxides, of which SiO$_2$ is the dominant component. No evidence of SiC was found, which is attributed to low divertor surface temperatures. The in-situ and ex-situ analysis found that Si-rich coatings of at least $0.4-1.2$ nm thickness have been deposited at $0.4-0.7$ nm/s. The technique is estimated to coat a surface area of at least 0.94 m$^2$ on the outer divertor. These results demonstrate the potential of using real-time material injection to form Si-enriched layers on divertor PFCs during reactor operation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.03923v3-abstract-full').style.display = 'none'; document.getElementById('2304.03923v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 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">Florian Effenberg et al 2023 Nucl. Fusion in press https://doi.org/10.1088/1741-4326/acee98</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nucl. Fusion 63 106004 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.09307">arXiv:2301.09307</a> <span> [<a href="https://arxiv.org/pdf/2301.09307">pdf</a>, <a href="https://arxiv.org/format/2301.09307">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 - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</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"> Measurement of cosmic-ray muon spallation products in a xenon-loaded liquid scintillator with KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Collaboration%2C+K">KamLAND-Zen Collaboration</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/?searchtype=author&query=Eizuka%2C+M">M. Eizuka</a>, <a href="/search/?searchtype=author&query=Futagi%2C+S">S. Futagi</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Kurasawa%2C+M">M. Kurasawa</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Miyake%2C+H">H. Miyake</a> , et al. (42 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.09307v1-abstract-short" style="display: inline;"> Cosmic-ray muons produce various radioisotopes when passing through material. These spallation products can be backgrounds for rare event searches such as in solar neutrino, double-beta decay, and dark matter search experiments. The KamLAND-Zen experiment searches for neutrinoless double-beta decay in 745kg of xenon dissolved in liquid scintillator. The experiment includes dead-time-free electroni… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.09307v1-abstract-full').style.display = 'inline'; document.getElementById('2301.09307v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.09307v1-abstract-full" style="display: none;"> Cosmic-ray muons produce various radioisotopes when passing through material. These spallation products can be backgrounds for rare event searches such as in solar neutrino, double-beta decay, and dark matter search experiments. The KamLAND-Zen experiment searches for neutrinoless double-beta decay in 745kg of xenon dissolved in liquid scintillator. The experiment includes dead-time-free electronics with a high efficiency for detecting muon-induced neutrons. The production yields of different radioisotopes are measured with a combination of delayed coincidence techniques, newly developed muon reconstruction and xenon spallation identification methods. The observed xenon spallation products are consistent with results from the FLUKA and Geant4 simulation codes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.09307v1-abstract-full').style.display = 'none'; document.getElementById('2301.09307v1-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 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.10527">arXiv:2212.10527</a> <span> [<a href="https://arxiv.org/pdf/2212.10527">pdf</a>, <a href="https://arxiv.org/format/2212.10527">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.130.061002">10.1103/PhysRevLett.130.061002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Gamma-ray Spectral Lines from Dark Matter Annihilation up to 100 TeV towards the Galactic Center with MAGIC </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=MAGIC+Collaboration"> MAGIC Collaboration</a>, <a href="/search/?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Baack%2C+D">D. Baack</a>, <a href="/search/?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/?searchtype=author&query=Baquero%2C+A">A. Baquero</a>, <a href="/search/?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a>, <a href="/search/?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/?searchtype=author&query=Bernardos%2C+M">M. Bernardos</a>, <a href="/search/?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/?searchtype=author&query=Besenrieder%2C+J">J. Besenrieder</a>, <a href="/search/?searchtype=author&query=Bhattacharyya%2C+W">W. Bhattacharyya</a> , et al. (188 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.10527v1-abstract-short" style="display: inline;"> Line-like features in TeV $纬$-rays constitute a ''smoking gun'' for TeV-scale particle dark matter and new physics. Probing the Galactic Center region with ground-based Cherenkov telescopes enables the search for TeV spectral features in immediate association with a dense dark matter reservoir at a sensitivity out of reach for satellite $纬$-ray detectors, and direct detection and collider experime… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.10527v1-abstract-full').style.display = 'inline'; document.getElementById('2212.10527v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.10527v1-abstract-full" style="display: none;"> Line-like features in TeV $纬$-rays constitute a ''smoking gun'' for TeV-scale particle dark matter and new physics. Probing the Galactic Center region with ground-based Cherenkov telescopes enables the search for TeV spectral features in immediate association with a dense dark matter reservoir at a sensitivity out of reach for satellite $纬$-ray detectors, and direct detection and collider experiments. We report on 223 hours of observations of the Galactic Center region with the MAGIC stereoscopic telescope system reaching $纬$-ray energies up to 100 TeV. We improved the sensitivity to spectral lines at high energies using large-zenith-angle observations and a novel background modeling method within a maximum-likelihood analysis in the energy domain. No line-like spectral feature is found in our analysis. Therefore, we constrain the cross section for dark matter annihilation into two photons to $\langle 蟽v \rangle \lesssim 5 \times 10^{-28}\,\mathrm{cm^3\,s^{-1}}$ at 1 TeV and $\langle 蟽v \rangle \lesssim 1 \times 10^{-25}\,\mathrm{cm^3\,s^{-1}}$ at 100 TeV, achieving the best limits to date for a dark matter mass above 20 TeV and a cuspy dark matter profile at the Galactic Center. Finally, we use the derived limits for both cuspy and cored dark matter profiles to constrain supersymmetric wino models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.10527v1-abstract-full').style.display = 'none'; document.getElementById('2212.10527v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in Phys. Rev. Lett., includes Supplemental materials. 9+4 pages, 3+3 figures, 3 tables. Corresponding authors: T. Inada, D. Kerszberg, M. H眉tten</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> KEK-TH-2487, KEK-Cosmo-0307 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.15321">arXiv:2211.15321</a> <span> [<a href="https://arxiv.org/pdf/2211.15321">pdf</a>, <a href="https://arxiv.org/format/2211.15321">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/10.1051/0004-6361/202244931">10.1051/0004-6361/202244931 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MAGIC observations provide compelling evidence of the hadronic multi-TeV emission from the putative PeVatron SNR G106.3+2.7 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=MAGIC+Collaboration"> MAGIC Collaboration</a>, <a href="/search/?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Baack%2C+D">D. Baack</a>, <a href="/search/?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/?searchtype=author&query=Baquero%2C+A">A. Baquero</a>, <a href="/search/?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a>, <a href="/search/?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/?searchtype=author&query=Bernardos%2C+M">M. Bernardos</a>, <a href="/search/?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/?searchtype=author&query=Besenrieder%2C+J">J. Besenrieder</a> , et al. (192 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="2211.15321v1-abstract-short" style="display: inline;"> The SNR G106.3+2.7, detected at 1--100 TeV energies by different $纬$-ray facilities, is one of the most promising PeVatron candidates. This SNR has a cometary shape which can be divided into a head and a tail region with different physical conditions. However, it is not identified in which region the 100 TeV emission is produced due to the limited position accuracy and/or angular resolution of exi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.15321v1-abstract-full').style.display = 'inline'; document.getElementById('2211.15321v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.15321v1-abstract-full" style="display: none;"> The SNR G106.3+2.7, detected at 1--100 TeV energies by different $纬$-ray facilities, is one of the most promising PeVatron candidates. This SNR has a cometary shape which can be divided into a head and a tail region with different physical conditions. However, it is not identified in which region the 100 TeV emission is produced due to the limited position accuracy and/or angular resolution of existing observational data. Additionally, it remains unclear whether the origin of the $纬$-ray emission is leptonic or hadronic. With the better angular resolution provided by these new MAGIC data compared to earlier $纬$-ray datasets, we aim to reveal the acceleration site of PeV particles and the emission mechanism by resolving the SNR G106.3+2.7 with 0.1$^\circ$ resolution at TeV energies. We detected extended $纬$-ray emission spatially coincident with the radio continuum emission at the head and tail of SNR G106.3+2.7. The fact that we detected a significant $纬$-ray emission with energies above 6.0 TeV from the tail region only suggests that the emissions above 10 TeV, detected with air shower experiments (Milagro, HAWC, Tibet AS$纬$ and LHAASO), are emitted only from the SNR tail. Under this assumption, the multi-wavelength spectrum of the head region can be explained with either hadronic or leptonic models, while the leptonic model for the tail region is in contradiction with the emission above 10 TeV and X-rays. In contrast, the hadronic model could reproduce the observed spectrum at the tail by assuming a proton spectrum with a cutoff energy of $\sim 1$ PeV for the tail region. Such a high energy emission in this middle-aged SNR (4--10 kyr) can be explained by considering the scenario that protons escaping from the SNR in the past interact with surrounding dense gases at present. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.15321v1-abstract-full').style.display = 'none'; document.getElementById('2211.15321v1-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 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 7 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 671, A12 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.13911">arXiv:2211.13911</a> <span> [<a href="https://arxiv.org/pdf/2211.13911">pdf</a>, <a href="https://arxiv.org/format/2211.13911">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 - 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.107.072006">10.1103/PhysRevD.107.072006 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First measurement of the strange axial coupling constant using neutral-current quasielastic interactions of atmospheric neutrinos at KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=KamLAND+Collaboration"> KamLAND Collaboration</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Asami%2C+S">S. Asami</a>, <a href="/search/?searchtype=author&query=Eizuka%2C+M">M. Eizuka</a>, <a href="/search/?searchtype=author&query=Futagi%2C+S">S. Futagi</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Gima%2C+T">T. Gima</a>, <a href="/search/?searchtype=author&query=Goto%2C+A">A. Goto</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/?searchtype=author&query=Ichimura%2C+K">K. Ichimura</a>, <a href="/search/?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/?searchtype=author&query=Kawada%2C+N">N. Kawada</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Kurasawa%2C+M">M. Kurasawa</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Miyake%2C+H">H. Miyake</a>, <a href="/search/?searchtype=author&query=Nakahata%2C+T">T. Nakahata</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a> , et al. (39 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="2211.13911v2-abstract-short" style="display: inline;"> We report a measurement of the strange axial coupling constant $g_A^s$ using atmospheric neutrino data at KamLAND. This constant is a component of the axial form factor of the neutral-current quasielastic (NCQE) interaction. The value of $g_A^s$ significantly changes the ratio of proton and neutron NCQE cross sections. KamLAND is suitable for measuring NCQE interactions as it can detect nucleon re… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.13911v2-abstract-full').style.display = 'inline'; document.getElementById('2211.13911v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.13911v2-abstract-full" style="display: none;"> We report a measurement of the strange axial coupling constant $g_A^s$ using atmospheric neutrino data at KamLAND. This constant is a component of the axial form factor of the neutral-current quasielastic (NCQE) interaction. The value of $g_A^s$ significantly changes the ratio of proton and neutron NCQE cross sections. KamLAND is suitable for measuring NCQE interactions as it can detect nucleon recoils with low-energy thresholds and measure neutron multiplicity with high efficiency. KamLAND data, including the information on neutron multiplicity associated with the NCQE interactions, makes it possible to measure $g_A^s$ with a suppressed dependence on the axial mass $M_A$, which has not yet been determined. For a comprehensive prediction of the neutron emission associated with neutrino interactions, we establish a simulation of particle emission via nuclear deexcitation of $^{12}$C, a process not considered in existing neutrino Monte Carlo event generators. Energy spectrum fitting for each neutron multiplicity gives $g_A^s =-0.14^{+0.25}_{-0.26}$, which is the most stringent limit obtained using NCQE interactions without $M_A$ constraints. The two-body current contribution considered in this analysis relies on a theoretically effective model and electron scattering experiments and requires future verification by direct measurements and future model improvement. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.13911v2-abstract-full').style.display = 'none'; document.getElementById('2211.13911v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 107,072006 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.02547">arXiv:2210.02547</a> <span> [<a href="https://arxiv.org/pdf/2210.02547">pdf</a>, <a href="https://arxiv.org/format/2210.02547">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/10.3847/1538-4365/acc181">10.3847/1538-4365/acc181 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multi-messenger characterization of Mrk 501 during historically low X-ray and $纬$-ray activity </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=MAGIC+collaboration"> MAGIC collaboration</a>, <a href="/search/?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Baack%2C+D">D. Baack</a>, <a href="/search/?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/?searchtype=author&query=Baquero%2C+A">A. Baquero</a>, <a href="/search/?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a>, <a href="/search/?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/?searchtype=author&query=Bernardos%2C+M">M. Bernardos</a>, <a href="/search/?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/?searchtype=author&query=Besenrieder%2C+J">J. Besenrieder</a> , et al. (300 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="2210.02547v3-abstract-short" style="display: inline;"> We study the broadband emission of Mrk 501 using multi-wavelength observations from 2017 to 2020 performed with a multitude of instruments, involving, among others, MAGIC, Fermi-LAT, NuSTAR, Swift, GASP-WEBT, and OVRO. Mrk 501 showed an extremely low broadband activity, which may help to unravel its baseline emission. Nonetheless, significant flux variations are detected at all wavebands, with the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.02547v3-abstract-full').style.display = 'inline'; document.getElementById('2210.02547v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.02547v3-abstract-full" style="display: none;"> We study the broadband emission of Mrk 501 using multi-wavelength observations from 2017 to 2020 performed with a multitude of instruments, involving, among others, MAGIC, Fermi-LAT, NuSTAR, Swift, GASP-WEBT, and OVRO. Mrk 501 showed an extremely low broadband activity, which may help to unravel its baseline emission. Nonetheless, significant flux variations are detected at all wavebands, with the highest occurring at X-rays and very-high-energy (VHE) $纬$-rays. A significant correlation ($>$3$蟽$) between X-rays and VHE $纬$-rays is measured, supporting leptonic scenarios to explain the variable parts of the emission, also during low activity. This is further supported when we extend our data from 2008 to 2020, and identify, for the first time, significant correlations between Swift-XRT and Fermi-LAT. We additionally find correlations between high-energy $纬$-rays and radio, with the radio lagging by more than 100 days, placing the $纬$-ray emission zone upstream of the radio-bright regions in the jet. Furthermore, Mrk 501 showed a historically low activity in X-rays and VHE $纬$-rays from mid-2017 to mid-2019 with a stable VHE flux ($>$0.2 TeV) of 5% the emission of the Crab Nebula. The broadband spectral energy distribution (SED) of this 2-year-long low-state, the potential baseline emission of Mrk 501, can be characterized with one-zone leptonic models, and with (lepto)-hadronic models fulfilling neutrino flux constraints from IceCube. We explore the time evolution of the SED towards the low-state, revealing that the stable baseline emission may be ascribed to a standing shock, and the variable emission to an additional expanding or traveling shock. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.02547v3-abstract-full').style.display = 'none'; document.getElementById('2210.02547v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">55 pages, 30 figures, 14 tables, accepted by APJS. Corresponding authors are L. Heckmann, D. Paneque, S. Gasparyan, M. Cerruti, and N. Sahakyan</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJS 266 37 (2023) </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=Abe%2C+S&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Abe%2C+S&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Abe%2C+S&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Abe%2C+S&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Abe%2C+S&start=150" class="pagination-link " aria-label="Page 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