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class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2503.03692">arXiv:2503.03692</a> <span> [<a href="https://arxiv.org/pdf/2503.03692">pdf</a>, <a href="https://arxiv.org/format/2503.03692">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 Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Atmospheric and Oceanic Physics">physics.ao-ph</span> </div> </div> <p class="title is-5 mathjax"> Capturing methane in a barn environment: the CH4 Livestock Emission (CH4rLiE) project </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Angiulli%2C+F+A">Francesco Alessandro Angiulli</a>, <a href="/search/?searchtype=author&query=Aim%C3%A8%2C+C">Chiara Aim猫</a>, <a href="/search/?searchtype=author&query=Arena%2C+M+C">Maria Cristina Arena</a>, <a href="/search/?searchtype=author&query=Biagini%2C+D">Davide Biagini</a>, <a href="/search/?searchtype=author&query=Braghieri%2C+A">Alessandro Braghieri</a>, <a href="/search/?searchtype=author&query=Brunoldi%2C+M">Matteo Brunoldi</a>, <a href="/search/?searchtype=author&query=Calzaferri%2C+S">Simone Calzaferri</a>, <a href="/search/?searchtype=author&query=Dinuccio%2C+E">Elio Dinuccio</a>, <a href="/search/?searchtype=author&query=Dondi%2C+D">Daniele Dondi</a>, <a href="/search/?searchtype=author&query=Finco%2C+L">Linda Finco</a>, <a href="/search/?searchtype=author&query=Guida%2C+R">Roberto Guida</a>, <a href="/search/?searchtype=author&query=Kameswaran%2C+N+K">Nithish Kumar Kameswaran</a>, <a href="/search/?searchtype=author&query=Mandelli%2C+B">Beatrice Mandelli</a>, <a href="/search/?searchtype=author&query=Montagna%2C+P">Paolo Montagna</a>, <a href="/search/?searchtype=author&query=Riccardi%2C+C">Cristina Riccardi</a>, <a href="/search/?searchtype=author&query=Salvini%2C+P">Paola Salvini</a>, <a href="/search/?searchtype=author&query=Tamigio%2C+A">Alessandro Tamigio</a>, <a href="/search/?searchtype=author&query=Vai%2C+I">Ilaria Vai</a>, <a href="/search/?searchtype=author&query=Vadivel%2C+D">Dhanalakshmi Vadivel</a>, <a href="/search/?searchtype=author&query=Verna%2C+R">Riccardo Verna</a>, <a href="/search/?searchtype=author&query=Vitulo%2C+P">Paolo Vitulo</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="2503.03692v1-abstract-short" style="display: inline;"> The CH4 Livestock Emission (CH4rLiE) project aims at developing a prototype for methane emissions capture in a barn environment. Methane has a higher global warming potential (GWP) with respect to CO2, and methane emissions of human origin contribute about 23% to global warming. Emissions from livestock farms play a non-negligible role, as a single cow is capable of emitting about 110 kg of methan… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2503.03692v1-abstract-full').style.display = 'inline'; document.getElementById('2503.03692v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2503.03692v1-abstract-full" style="display: none;"> The CH4 Livestock Emission (CH4rLiE) project aims at developing a prototype for methane emissions capture in a barn environment. Methane has a higher global warming potential (GWP) with respect to CO2, and methane emissions of human origin contribute about 23% to global warming. Emissions from livestock farms play a non-negligible role, as a single cow is capable of emitting about 110 kg of methane in a year. Several projects have tried to mitigate the problem by intervening on animal feed: CH4rLiE, in contrast, proposes to act on the methane already produced and diffused in the air, using a specially developed recovery system. The idea arose from the expertise acquired in the Large Hadron Collider experiments at CERN, where special gas recuperation systems are being developed to extract CF4 from gaseous detectors' exhausted gas mixture. The project focuses on the study of gas adsorption by porous materials and on the development of a prototype system for methane capture, which will be installed in a real barn. This study is being supported by an initial phase of gas diffusion simulations and by a campaign of measurements of gas concentrations in different barn areas. CH4rLiE will also provide an opportunity to explore, for the first time, the feasibility of methane recovery from the farm environment without affecting the animals' feeding or living conditions. The social benefits are extremely interesting both in terms of developing and implementing low-impact farming production processes, but also in terms of recycling expensive or environmentally unfriendly gasses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2503.03692v1-abstract-full').style.display = 'none'; document.getElementById('2503.03692v1-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, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2025. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.03254">arXiv:2411.03254</a> <span> [<a href="https://arxiv.org/pdf/2411.03254">pdf</a>, <a href="https://arxiv.org/format/2411.03254">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.3014300">10.1117/12.3014300 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Computation of the Fresnel diffraction of starshades based on a polygonal approximation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Prunet%2C+S">Simon Prunet</a>, <a href="/search/?searchtype=author&query=Aime%2C+C">Claude Aime</a>, <a href="/search/?searchtype=author&query=Ferrari%2C+A">Andr茅 Ferrari</a>, <a href="/search/?searchtype=author&query=Theys%2C+C">C茅line Theys</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.03254v1-abstract-short" style="display: inline;"> The design of starshades, i.e. external occulters for stellar coronography, relies on the fast and precise computation of their associated diffraction patterns of incoming plane waves in the telescope aperture plane. We present here a method based on a polygonal approximation of the occulter's shape, that allows fast computation of their diffraction patterns in the Fresnel approximation, without a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.03254v1-abstract-full').style.display = 'inline'; document.getElementById('2411.03254v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.03254v1-abstract-full" style="display: none;"> The design of starshades, i.e. external occulters for stellar coronography, relies on the fast and precise computation of their associated diffraction patterns of incoming plane waves in the telescope aperture plane. We present here a method based on a polygonal approximation of the occulter's shape, that allows fast computation of their diffraction patterns in the Fresnel approximation, without aliasing artefacts. It is competitive with respect to methods based on direct 2D Fourier transforms, or Boundary Diffraction Wave algorithms. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.03254v1-abstract-full').style.display = 'none'; document.getElementById('2411.03254v1-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 4 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proceedings Volume 13092, Space Telescopes and Instrumentation 2024: Optical, Infrared, and Millimeter Wave </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.03144">arXiv:2411.03144</a> <span> [<a href="https://arxiv.org/pdf/2411.03144">pdf</a>, <a href="https://arxiv.org/format/2411.03144">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.3013679">10.1117/12.3013679 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A comparison of solar and stellar coronagraphs that make use of external occulters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Aime%2C+C">Claude Aime</a>, <a href="/search/?searchtype=author&query=Theys%2C+C">C茅line Theys</a>, <a href="/search/?searchtype=author&query=Prunet%2C+S">Simon Prunet</a>, <a href="/search/?searchtype=author&query=Ferrari%2C+A">Andr茅 Ferrari</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.03144v1-abstract-short" style="display: inline;"> Solar and stellar externally occulted coronagraphs share similar concepts, but are actually very different because of geometric characteristics. Solar occulters were first developed with a simple geometric model of diffraction perpendicular to the occulter edges. We apply this mere approach to starshades, and introduce a simple shifted circular integral of the occulter which allows to illustrate t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.03144v1-abstract-full').style.display = 'inline'; document.getElementById('2411.03144v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.03144v1-abstract-full" style="display: none;"> Solar and stellar externally occulted coronagraphs share similar concepts, but are actually very different because of geometric characteristics. Solar occulters were first developed with a simple geometric model of diffraction perpendicular to the occulter edges. We apply this mere approach to starshades, and introduce a simple shifted circular integral of the occulter which allows to illustrate the influence of the number of petals on the extent of the deep central dark zone. We illustrate the reasons for the presence of an internal coronagraph in the solar case and its absence in the exoplanet case. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.03144v1-abstract-full').style.display = 'none'; document.getElementById('2411.03144v1-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 10 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proceedings Volume 13092, Space Telescopes and Instrumentation 2024: Optical, Infrared, and Millimeter Wave </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.02966">arXiv:2411.02966</a> <span> [<a href="https://arxiv.org/pdf/2411.02966">pdf</a>, <a href="https://arxiv.org/format/2411.02966">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Accelerator Physics">physics.acc-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/10.5281/zenodo.13970100">10.5281/zenodo.13970100 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MuCol Milestone Report No. 5: Preliminary Parameters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Accettura%2C+C">Carlotta Accettura</a>, <a href="/search/?searchtype=author&query=Adrian%2C+S">Simon Adrian</a>, <a href="/search/?searchtype=author&query=Agarwal%2C+R">Rohit Agarwal</a>, <a href="/search/?searchtype=author&query=Ahdida%2C+C">Claudia Ahdida</a>, <a href="/search/?searchtype=author&query=Aim%C3%A9%2C+C">Chiara Aim茅</a>, <a href="/search/?searchtype=author&query=Aksoy%2C+A">Avni Aksoy</a>, <a href="/search/?searchtype=author&query=Alberghi%2C+G+L">Gian Luigi Alberghi</a>, <a href="/search/?searchtype=author&query=Alden%2C+S">Siobhan Alden</a>, <a href="/search/?searchtype=author&query=Alfonso%2C+L">Luca Alfonso</a>, <a href="/search/?searchtype=author&query=Amapane%2C+N">Nicola Amapane</a>, <a href="/search/?searchtype=author&query=Amorim%2C+D">David Amorim</a>, <a href="/search/?searchtype=author&query=Andreetto%2C+P">Paolo Andreetto</a>, <a href="/search/?searchtype=author&query=Anulli%2C+F">Fabio Anulli</a>, <a href="/search/?searchtype=author&query=Appleby%2C+R">Rob Appleby</a>, <a href="/search/?searchtype=author&query=Apresyan%2C+A">Artur Apresyan</a>, <a href="/search/?searchtype=author&query=Asadi%2C+P">Pouya Asadi</a>, <a href="/search/?searchtype=author&query=Mahmoud%2C+M+A">Mohammed Attia Mahmoud</a>, <a href="/search/?searchtype=author&query=Auchmann%2C+B">Bernhard Auchmann</a>, <a href="/search/?searchtype=author&query=Back%2C+J">John Back</a>, <a href="/search/?searchtype=author&query=Badea%2C+A">Anthony Badea</a>, <a href="/search/?searchtype=author&query=Bae%2C+K+J">Kyu Jung Bae</a>, <a href="/search/?searchtype=author&query=Bahng%2C+E+J">E. J. Bahng</a>, <a href="/search/?searchtype=author&query=Balconi%2C+L">Lorenzo Balconi</a>, <a href="/search/?searchtype=author&query=Balli%2C+F">Fabrice Balli</a>, <a href="/search/?searchtype=author&query=Bandiera%2C+L">Laura Bandiera</a> , et al. (369 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.02966v1-abstract-short" style="display: inline;"> This document is comprised of a collection of updated preliminary parameters for the key parts of the muon collider. The updated preliminary parameters follow on from the October 2023 Tentative Parameters Report. Particular attention has been given to regions of the facility that are believed to hold greater technical uncertainty in their design and that have a strong impact on the cost and power… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.02966v1-abstract-full').style.display = 'inline'; document.getElementById('2411.02966v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.02966v1-abstract-full" style="display: none;"> This document is comprised of a collection of updated preliminary parameters for the key parts of the muon collider. The updated preliminary parameters follow on from the October 2023 Tentative Parameters Report. Particular attention has been given to regions of the facility that are believed to hold greater technical uncertainty in their design and that have a strong impact on the cost and power consumption of the facility. The data is collected from a collaborative spreadsheet and transferred to overleaf. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.02966v1-abstract-full').style.display = 'none'; document.getElementById('2411.02966v1-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.12450">arXiv:2407.12450</a> <span> [<a href="https://arxiv.org/pdf/2407.12450">pdf</a>, <a href="https://arxiv.org/format/2407.12450">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Accelerator Physics">physics.acc-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Interim report for the International Muon Collider Collaboration (IMCC) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Accettura%2C+C">C. Accettura</a>, <a href="/search/?searchtype=author&query=Adrian%2C+S">S. Adrian</a>, <a href="/search/?searchtype=author&query=Agarwal%2C+R">R. Agarwal</a>, <a href="/search/?searchtype=author&query=Ahdida%2C+C">C. Ahdida</a>, <a href="/search/?searchtype=author&query=Aim%C3%A9%2C+C">C. Aim茅</a>, <a href="/search/?searchtype=author&query=Aksoy%2C+A">A. Aksoy</a>, <a href="/search/?searchtype=author&query=Alberghi%2C+G+L">G. L. Alberghi</a>, <a href="/search/?searchtype=author&query=Alden%2C+S">S. Alden</a>, <a href="/search/?searchtype=author&query=Amapane%2C+N">N. Amapane</a>, <a href="/search/?searchtype=author&query=Amorim%2C+D">D. Amorim</a>, <a href="/search/?searchtype=author&query=Andreetto%2C+P">P. Andreetto</a>, <a href="/search/?searchtype=author&query=Anulli%2C+F">F. Anulli</a>, <a href="/search/?searchtype=author&query=Appleby%2C+R">R. Appleby</a>, <a href="/search/?searchtype=author&query=Apresyan%2C+A">A. Apresyan</a>, <a href="/search/?searchtype=author&query=Asadi%2C+P">P. Asadi</a>, <a href="/search/?searchtype=author&query=Mahmoud%2C+M+A">M. Attia Mahmoud</a>, <a href="/search/?searchtype=author&query=Auchmann%2C+B">B. Auchmann</a>, <a href="/search/?searchtype=author&query=Back%2C+J">J. Back</a>, <a href="/search/?searchtype=author&query=Badea%2C+A">A. Badea</a>, <a href="/search/?searchtype=author&query=Bae%2C+K+J">K. J. Bae</a>, <a href="/search/?searchtype=author&query=Bahng%2C+E+J">E. J. Bahng</a>, <a href="/search/?searchtype=author&query=Balconi%2C+L">L. Balconi</a>, <a href="/search/?searchtype=author&query=Balli%2C+F">F. Balli</a>, <a href="/search/?searchtype=author&query=Bandiera%2C+L">L. Bandiera</a>, <a href="/search/?searchtype=author&query=Barbagallo%2C+C">C. Barbagallo</a> , et al. (362 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="2407.12450v2-abstract-short" style="display: inline;"> The International Muon Collider Collaboration (IMCC) [1] was established in 2020 following the recommendations of the European Strategy for Particle Physics (ESPP) and the implementation of the European Strategy for Particle Physics-Accelerator R&D Roadmap by the Laboratory Directors Group [2], hereinafter referred to as the the European LDG roadmap. The Muon Collider Study (MuC) covers the accele… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.12450v2-abstract-full').style.display = 'inline'; document.getElementById('2407.12450v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.12450v2-abstract-full" style="display: none;"> The International Muon Collider Collaboration (IMCC) [1] was established in 2020 following the recommendations of the European Strategy for Particle Physics (ESPP) and the implementation of the European Strategy for Particle Physics-Accelerator R&D Roadmap by the Laboratory Directors Group [2], hereinafter referred to as the the European LDG roadmap. The Muon Collider Study (MuC) covers the accelerator complex, detectors and physics for a future muon collider. In 2023, European Commission support was obtained for a design study of a muon collider (MuCol) [3]. This project started on 1st March 2023, with work-packages aligned with the overall muon collider studies. In preparation of and during the 2021-22 U.S. Snowmass process, the muon collider project parameters, technical studies and physics performance studies were performed and presented in great detail. Recently, the P5 panel [4] in the U.S. recommended a muon collider R&D, proposed to join the IMCC and envisages that the U.S. should prepare to host a muon collider, calling this their "muon shot". In the past, the U.S. Muon Accelerator Programme (MAP) [5] has been instrumental in studies of concepts and technologies for a muon collider. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.12450v2-abstract-full').style.display = 'none'; document.getElementById('2407.12450v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 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">This document summarises the International Muon Collider Collaboration (IMCC) progress and status of the Muon Collider R&D programme</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.08533">arXiv:2303.08533</a> <span> [<a href="https://arxiv.org/pdf/2303.08533">pdf</a>, <a href="https://arxiv.org/format/2303.08533">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Accelerator Physics">physics.acc-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="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Towards a Muon Collider </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Accettura%2C+C">Carlotta Accettura</a>, <a href="/search/?searchtype=author&query=Adams%2C+D">Dean Adams</a>, <a href="/search/?searchtype=author&query=Agarwal%2C+R">Rohit Agarwal</a>, <a href="/search/?searchtype=author&query=Ahdida%2C+C">Claudia Ahdida</a>, <a href="/search/?searchtype=author&query=Aim%C3%A8%2C+C">Chiara Aim猫</a>, <a href="/search/?searchtype=author&query=Amapane%2C+N">Nicola Amapane</a>, <a href="/search/?searchtype=author&query=Amorim%2C+D">David Amorim</a>, <a href="/search/?searchtype=author&query=Andreetto%2C+P">Paolo Andreetto</a>, <a href="/search/?searchtype=author&query=Anulli%2C+F">Fabio Anulli</a>, <a href="/search/?searchtype=author&query=Appleby%2C+R">Robert Appleby</a>, <a href="/search/?searchtype=author&query=Apresyan%2C+A">Artur Apresyan</a>, <a href="/search/?searchtype=author&query=Apyan%2C+A">Aram Apyan</a>, <a href="/search/?searchtype=author&query=Arsenyev%2C+S">Sergey Arsenyev</a>, <a href="/search/?searchtype=author&query=Asadi%2C+P">Pouya Asadi</a>, <a href="/search/?searchtype=author&query=Mahmoud%2C+M+A">Mohammed Attia Mahmoud</a>, <a href="/search/?searchtype=author&query=Azatov%2C+A">Aleksandr Azatov</a>, <a href="/search/?searchtype=author&query=Back%2C+J">John Back</a>, <a href="/search/?searchtype=author&query=Balconi%2C+L">Lorenzo Balconi</a>, <a href="/search/?searchtype=author&query=Bandiera%2C+L">Laura Bandiera</a>, <a href="/search/?searchtype=author&query=Barlow%2C+R">Roger Barlow</a>, <a href="/search/?searchtype=author&query=Bartosik%2C+N">Nazar Bartosik</a>, <a href="/search/?searchtype=author&query=Barzi%2C+E">Emanuela Barzi</a>, <a href="/search/?searchtype=author&query=Batsch%2C+F">Fabian Batsch</a>, <a href="/search/?searchtype=author&query=Bauce%2C+M">Matteo Bauce</a>, <a href="/search/?searchtype=author&query=Berg%2C+J+S">J. Scott Berg</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="2303.08533v2-abstract-short" style="display: inline;"> A muon collider would enable the big jump ahead in energy reach that is needed for a fruitful exploration of fundamental interactions. The challenges of producing muon collisions at high luminosity and 10 TeV centre of mass energy are being investigated by the recently-formed International Muon Collider Collaboration. This Review summarises the status and the recent advances on muon colliders desi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.08533v2-abstract-full').style.display = 'inline'; document.getElementById('2303.08533v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.08533v2-abstract-full" style="display: none;"> A muon collider would enable the big jump ahead in energy reach that is needed for a fruitful exploration of fundamental interactions. The challenges of producing muon collisions at high luminosity and 10 TeV centre of mass energy are being investigated by the recently-formed International Muon Collider Collaboration. This Review summarises the status and the recent advances on muon colliders design, physics and detector studies. The aim is to provide a global perspective of the field and to outline directions for future work. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.08533v2-abstract-full').style.display = 'none'; document.getElementById('2303.08533v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">118 pages, 103 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.01318">arXiv:2209.01318</a> <span> [<a href="https://arxiv.org/pdf/2209.01318">pdf</a>, <a href="https://arxiv.org/format/2209.01318">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 Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Muon Collider Forum Report </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Black%2C+K+M">K. M. Black</a>, <a href="/search/?searchtype=author&query=Jindariani%2C+S">S. Jindariani</a>, <a href="/search/?searchtype=author&query=Li%2C+D">D. Li</a>, <a href="/search/?searchtype=author&query=Maltoni%2C+F">F. Maltoni</a>, <a href="/search/?searchtype=author&query=Meade%2C+P">P. Meade</a>, <a href="/search/?searchtype=author&query=Stratakis%2C+D">D. Stratakis</a>, <a href="/search/?searchtype=author&query=Acosta%2C+D">D. Acosta</a>, <a href="/search/?searchtype=author&query=Agarwal%2C+R">R. Agarwal</a>, <a href="/search/?searchtype=author&query=Agashe%2C+K">K. Agashe</a>, <a href="/search/?searchtype=author&query=Aime%2C+C">C. Aime</a>, <a href="/search/?searchtype=author&query=Ally%2C+D">D. Ally</a>, <a href="/search/?searchtype=author&query=Apresyan%2C+A">A. Apresyan</a>, <a href="/search/?searchtype=author&query=Apyan%2C+A">A. Apyan</a>, <a href="/search/?searchtype=author&query=Asadi%2C+P">P. Asadi</a>, <a href="/search/?searchtype=author&query=Athanasakos%2C+D">D. Athanasakos</a>, <a href="/search/?searchtype=author&query=Bao%2C+Y">Y. Bao</a>, <a href="/search/?searchtype=author&query=Barzi%2C+E">E. Barzi</a>, <a href="/search/?searchtype=author&query=Bartosik%2C+N">N. Bartosik</a>, <a href="/search/?searchtype=author&query=Bauerdick%2C+L+A+T">L. A. T. Bauerdick</a>, <a href="/search/?searchtype=author&query=Beacham%2C+J">J. Beacham</a>, <a href="/search/?searchtype=author&query=Belomestnykh%2C+S">S. Belomestnykh</a>, <a href="/search/?searchtype=author&query=Berg%2C+J+S">J. S. Berg</a>, <a href="/search/?searchtype=author&query=Berryhill%2C+J">J. Berryhill</a>, <a href="/search/?searchtype=author&query=Bertolin%2C+A">A. Bertolin</a>, <a href="/search/?searchtype=author&query=Bhat%2C+P+C">P. C. Bhat</a> , et al. (160 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.01318v3-abstract-short" style="display: inline;"> A multi-TeV muon collider offers a spectacular opportunity in the direct exploration of the energy frontier. Offering a combination of unprecedented energy collisions in a comparatively clean leptonic environment, a high energy muon collider has the unique potential to provide both precision measurements and the highest energy reach in one machine that cannot be paralleled by any currently availab… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.01318v3-abstract-full').style.display = 'inline'; document.getElementById('2209.01318v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.01318v3-abstract-full" style="display: none;"> A multi-TeV muon collider offers a spectacular opportunity in the direct exploration of the energy frontier. Offering a combination of unprecedented energy collisions in a comparatively clean leptonic environment, a high energy muon collider has the unique potential to provide both precision measurements and the highest energy reach in one machine that cannot be paralleled by any currently available technology. The topic generated a lot of excitement in Snowmass meetings and continues to attract a large number of supporters, including many from the early career community. In light of this very strong interest within the US particle physics community, Snowmass Energy, Theory and Accelerator Frontiers created a cross-frontier Muon Collider Forum in November of 2020. The Forum has been meeting on a monthly basis and organized several topical workshops dedicated to physics, accelerator technology, and detector R&D. Findings of the Forum are summarized in this report. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.01318v3-abstract-full').style.display = 'none'; document.getElementById('2209.01318v3-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.12037">arXiv:2203.12037</a> <span> [<a href="https://arxiv.org/pdf/2203.12037">pdf</a>, <a href="https://arxiv.org/format/2203.12037">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 Detectors">physics.ins-det</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/10.1016/j.nima.2022.166716">10.1016/j.nima.2022.166716 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Quality Control of Mass-Produced GEM Detectors for the CMS GE1/1 Muon Upgrade </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abbas%2C+M">M. Abbas</a>, <a href="/search/?searchtype=author&query=Abbrescia%2C+M">M. Abbrescia</a>, <a href="/search/?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/?searchtype=author&query=Abdelalim%2C+A">A. Abdelalim</a>, <a href="/search/?searchtype=author&query=AbuZeid%2C+S">S. AbuZeid</a>, <a href="/search/?searchtype=author&query=Agapitos%2C+A">A. Agapitos</a>, <a href="/search/?searchtype=author&query=Ahmad%2C+A">A. Ahmad</a>, <a href="/search/?searchtype=author&query=Ahmed%2C+A">A. Ahmed</a>, <a href="/search/?searchtype=author&query=Ahmed%2C+W">W. Ahmed</a>, <a href="/search/?searchtype=author&query=Aim%C3%A8%2C+C">C. Aim猫</a>, <a href="/search/?searchtype=author&query=Aruta%2C+C">C. Aruta</a>, <a href="/search/?searchtype=author&query=Asghar%2C+I">I. Asghar</a>, <a href="/search/?searchtype=author&query=Aspell%2C+P">P. Aspell</a>, <a href="/search/?searchtype=author&query=Avila%2C+C">C. Avila</a>, <a href="/search/?searchtype=author&query=Babbar%2C+J">J. Babbar</a>, <a href="/search/?searchtype=author&query=Ban%2C+Y">Y. Ban</a>, <a href="/search/?searchtype=author&query=Band%2C+R">R. Band</a>, <a href="/search/?searchtype=author&query=Bansal%2C+S">S. Bansal</a>, <a href="/search/?searchtype=author&query=Benussi%2C+L">L. Benussi</a>, <a href="/search/?searchtype=author&query=Beyrouthy%2C+T">T. Beyrouthy</a>, <a href="/search/?searchtype=author&query=Bhatnagar%2C+V">V. Bhatnagar</a>, <a href="/search/?searchtype=author&query=Bianco%2C+M">M. Bianco</a>, <a href="/search/?searchtype=author&query=Bianco%2C+S">S. Bianco</a>, <a href="/search/?searchtype=author&query=Black%2C+K">K. Black</a>, <a href="/search/?searchtype=author&query=Borgonovi%2C+L">L. Borgonovi</a> , et al. (157 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.12037v1-abstract-short" style="display: inline;"> The series of upgrades to the Large Hadron Collider, culminating in the High Luminosity Large Hadron Collider, will enable a significant expansion of the physics program of the CMS experiment. However, the accelerator upgrades will also make the experimental conditions more challenging, with implications for detector operations, triggering, and data analysis. The luminosity of the proton-proton co… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.12037v1-abstract-full').style.display = 'inline'; document.getElementById('2203.12037v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.12037v1-abstract-full" style="display: none;"> The series of upgrades to the Large Hadron Collider, culminating in the High Luminosity Large Hadron Collider, will enable a significant expansion of the physics program of the CMS experiment. However, the accelerator upgrades will also make the experimental conditions more challenging, with implications for detector operations, triggering, and data analysis. The luminosity of the proton-proton collisions is expected to exceed $2-3\times10^{34}$~cm$^{-2}$s$^{-1}$ for Run 3 (starting in 2022), and it will be at least $5\times10^{34}$~cm$^{-2}$s$^{-1}$ when the High Luminosity Large Hadron Collider is completed for Run 4. These conditions will affect muon triggering, identification, and measurement, which are critical capabilities of the experiment. To address these challenges, additional muon detectors are being installed in the CMS endcaps, based on Gas Electron Multiplier technology. For this purpose, 161 large triple-Gas Electron Multiplier detectors have been constructed and tested. Installation of these devices began in 2019 with the GE1/1 station and will be followed by two additional stations, GE2/1 and ME0, to be installed in 2023 and 2026, respectively. The assembly and quality control of the GE1/1 detectors were distributed across several production sites around the world. We motivate and discuss the quality control procedures that were developed to standardize the performance of the detectors, and we present the final results of the production. Out of 161 detectors produced, 156 detectors passed all tests, and 144 detectors are now installed in the CMS experiment. The various visual inspections, gas tightness tests, intrinsic noise rate characterizations, and effective gas gain and response uniformity tests allowed the project to achieve this high success rate. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.12037v1-abstract-full').style.display = 'none'; document.getElementById('2203.12037v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">45 pages, 39 figures, submitted to Nuclear Instruments and Methods in Physics Research Section 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/2203.08033">arXiv:2203.08033</a> <span> [<a href="https://arxiv.org/pdf/2203.08033">pdf</a>, <a href="https://arxiv.org/format/2203.08033">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Accelerator Physics">physics.acc-ph</span> </div> </div> <p class="title is-5 mathjax"> A Muon Collider Facility for Physics Discovery </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Stratakis%2C+D">D. Stratakis</a>, <a href="/search/?searchtype=author&query=Mokhov%2C+N">N. Mokhov</a>, <a href="/search/?searchtype=author&query=Palmer%2C+M">M. Palmer</a>, <a href="/search/?searchtype=author&query=Pastrone%2C+N">N. Pastrone</a>, <a href="/search/?searchtype=author&query=Raubenheimer%2C+T">T. Raubenheimer</a>, <a href="/search/?searchtype=author&query=Rogers%2C+C">C. Rogers</a>, <a href="/search/?searchtype=author&query=Schulte%2C+D">D. Schulte</a>, <a href="/search/?searchtype=author&query=Shiltsev%2C+V">V. Shiltsev</a>, <a href="/search/?searchtype=author&query=Tang%2C+J">J. Tang</a>, <a href="/search/?searchtype=author&query=Yamamoto%2C+A">A. Yamamoto</a>, <a href="/search/?searchtype=author&query=Aim%C3%A8%2C+C">C. Aim猫</a>, <a href="/search/?searchtype=author&query=Mahmoud%2C+M+A">M. A. Mahmoud</a>, <a href="/search/?searchtype=author&query=Bartosik%2C+N">N. Bartosik</a>, <a href="/search/?searchtype=author&query=Barzi%2C+E">E. Barzi</a>, <a href="/search/?searchtype=author&query=Bersani%2C+A">A. Bersani</a>, <a href="/search/?searchtype=author&query=Bertolin%2C+A">A. Bertolin</a>, <a href="/search/?searchtype=author&query=Bonesini%2C+M">M. Bonesini</a>, <a href="/search/?searchtype=author&query=Caiffi%2C+B">B. Caiffi</a>, <a href="/search/?searchtype=author&query=Casarsa%2C+M">M. Casarsa</a>, <a href="/search/?searchtype=author&query=Catanesi%2C+M+G">M. G. Catanesi</a>, <a href="/search/?searchtype=author&query=Cerri%2C+A">A. Cerri</a>, <a href="/search/?searchtype=author&query=Curatolo%2C+C">C. Curatolo</a>, <a href="/search/?searchtype=author&query=Dam%2C+M">M. Dam</a>, <a href="/search/?searchtype=author&query=Damerau%2C+H">H. Damerau</a>, <a href="/search/?searchtype=author&query=De+Matteis%2C+E">E. De Matteis</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="2203.08033v1-abstract-short" style="display: inline;"> Muon colliders provide a unique route to deliver high energy collisions that enable discovery searches and precision measurements to extend our understanding of the fundamental laws of physics. The muon collider design aims to deliver physics reach at the highest energies with costs, power consumption and on a time scale that may prove favorable relative to other proposed facilities. In this conte… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.08033v1-abstract-full').style.display = 'inline'; document.getElementById('2203.08033v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.08033v1-abstract-full" style="display: none;"> Muon colliders provide a unique route to deliver high energy collisions that enable discovery searches and precision measurements to extend our understanding of the fundamental laws of physics. The muon collider design aims to deliver physics reach at the highest energies with costs, power consumption and on a time scale that may prove favorable relative to other proposed facilities. In this context, a new international collaboration has formed to further extend the design concepts and performance studies of such a machine. This effort is focused on delivering the elements of a $\sim$10 TeV center of mass (CM) energy design to explore the physics energy frontier. The path to such a machine may pass through lower energy options. Currently a 3 TeV CM stage is considered. Other energy stages could also be explored, e.g. an s-channel Higgs Factory operating at 125 GeV CM. We describe the status of the R&D and design effort towards such a machine and lay out a plan to bring these concepts to maturity as a tool for the high energy physics community. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.08033v1-abstract-full').style.display = 'none'; document.getElementById('2203.08033v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 3 figures. arXiv admin note: text overlap with arXiv:2201.07895</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.07964">arXiv:2203.07964</a> <span> [<a href="https://arxiv.org/pdf/2203.07964">pdf</a>, <a href="https://arxiv.org/format/2203.07964">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 Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Simulated Detector Performance at the Muon Collider </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bartosik%2C+N">Nazar Bartosik</a>, <a href="/search/?searchtype=author&query=Krizka%2C+K">Karol Krizka</a>, <a href="/search/?searchtype=author&query=Griso%2C+S+P">Simone Pagan Griso</a>, <a href="/search/?searchtype=author&query=Aim%C3%A8%2C+C">Chiara Aim猫</a>, <a href="/search/?searchtype=author&query=Apyan%2C+A">Aram Apyan</a>, <a href="/search/?searchtype=author&query=Mahmoud%2C+M+A">Mohammed Attia Mahmoud</a>, <a href="/search/?searchtype=author&query=Bertolin%2C+A">Alessandro Bertolin</a>, <a href="/search/?searchtype=author&query=Braghieri%2C+A">Alessandro Braghieri</a>, <a href="/search/?searchtype=author&query=Buonincontri%2C+L">Laura Buonincontri</a>, <a href="/search/?searchtype=author&query=Calzaferri%2C+S">Simone Calzaferri</a>, <a href="/search/?searchtype=author&query=Casarsa%2C+M">Massimo Casarsa</a>, <a href="/search/?searchtype=author&query=Castelli%2C+L">Luca Castelli</a>, <a href="/search/?searchtype=author&query=Catanesi%2C+M+G">Maria Gabriella Catanesi</a>, <a href="/search/?searchtype=author&query=Celiberto%2C+F+G">Francesco Giovanni Celiberto</a>, <a href="/search/?searchtype=author&query=Cerri%2C+A">Alessandro Cerri</a>, <a href="/search/?searchtype=author&query=Chachamis%2C+G">Grigorios Chachamis</a>, <a href="/search/?searchtype=author&query=Colaleo%2C+A">Anna Colaleo</a>, <a href="/search/?searchtype=author&query=Curatolo%2C+C">Camilla Curatolo</a>, <a href="/search/?searchtype=author&query=Da+Molin%2C+G">Giacomo Da Molin</a>, <a href="/search/?searchtype=author&query=Dasu%2C+S">Sridhara Dasu</a>, <a href="/search/?searchtype=author&query=Desinov%2C+D">Dmitri Desinov</a>, <a href="/search/?searchtype=author&query=Denizli%2C+H">Haluk Denizli</a>, <a href="/search/?searchtype=author&query=Di+Micco%2C+B">Biagio Di Micco</a>, <a href="/search/?searchtype=author&query=Dorigo%2C+T">Tommaso Dorigo</a>, <a href="/search/?searchtype=author&query=Errico%2C+F">Filippo Errico</a> , et al. (46 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.07964v2-abstract-short" style="display: inline;"> In this paper we report on the current status of studies on the expected performance for a detector designed to operate in a muon collider environment. Beam-induced backgrounds (BIB) represent the main challenge in the design of the detector and the event reconstruction algorithms. The current detector design aims to show that satisfactory performance can be achieved, while further optimizations a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07964v2-abstract-full').style.display = 'inline'; document.getElementById('2203.07964v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.07964v2-abstract-full" style="display: none;"> In this paper we report on the current status of studies on the expected performance for a detector designed to operate in a muon collider environment. Beam-induced backgrounds (BIB) represent the main challenge in the design of the detector and the event reconstruction algorithms. The current detector design aims to show that satisfactory performance can be achieved, while further optimizations are expected to significantly improve the overall performance. We present the characterization of the expected beam-induced background, describe the detector design and software used for detailed event simulations taking into account BIB effects. The expected performance of charged-particle reconstruction, jets, electrons, photons and muons is discussed, including an initial study on heavy-flavor jet tagging. A simple method to measure the delivered luminosity is also described. Overall, the proposed design and reconstruction algorithms can successfully reconstruct the high transverse-momentum objects needed to carry out a broad physics program. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07964v2-abstract-full').style.display = 'none'; document.getElementById('2203.07964v2-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 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">contribution to Snowmass 2021</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.07261">arXiv:2203.07261</a> <span> [<a href="https://arxiv.org/pdf/2203.07261">pdf</a>, <a href="https://arxiv.org/format/2203.07261">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> </div> </div> <p class="title is-5 mathjax"> The physics case of a 3 TeV muon collider stage </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=De+Blas%2C+J">Jorge De Blas</a>, <a href="/search/?searchtype=author&query=Buttazzo%2C+D">Dario Buttazzo</a>, <a href="/search/?searchtype=author&query=Capdevilla%2C+R">Rodolfo Capdevilla</a>, <a href="/search/?searchtype=author&query=Curtin%2C+D">David Curtin</a>, <a href="/search/?searchtype=author&query=Franceschini%2C+R">Roberto Franceschini</a>, <a href="/search/?searchtype=author&query=Maltoni%2C+F">Fabio Maltoni</a>, <a href="/search/?searchtype=author&query=Meade%2C+P">Patrick Meade</a>, <a href="/search/?searchtype=author&query=Meloni%2C+F">Federico Meloni</a>, <a href="/search/?searchtype=author&query=Su%2C+S">Shufang Su</a>, <a href="/search/?searchtype=author&query=Vryonidou%2C+E">Eleni Vryonidou</a>, <a href="/search/?searchtype=author&query=Wulzer%2C+A">Andrea Wulzer</a>, <a href="/search/?searchtype=author&query=Aim%C3%A8%2C+C">Chiara Aim猫</a>, <a href="/search/?searchtype=author&query=Apyan%2C+A">Aram Apyan</a>, <a href="/search/?searchtype=author&query=Asadi%2C+P">Pouya Asadi</a>, <a href="/search/?searchtype=author&query=Mahmoud%2C+M+A">Mohammed Attia Mahmoud</a>, <a href="/search/?searchtype=author&query=Azatov%2C+A">Aleksandr Azatov</a>, <a href="/search/?searchtype=author&query=Bartosik%2C+N">Nazar Bartosik</a>, <a href="/search/?searchtype=author&query=Bertolin%2C+A">Alessandro Bertolin</a>, <a href="/search/?searchtype=author&query=Bottaro%2C+S">Salvatore Bottaro</a>, <a href="/search/?searchtype=author&query=Buonincontri%2C+L">Laura Buonincontri</a>, <a href="/search/?searchtype=author&query=Casarsa%2C+M">Massimo Casarsa</a>, <a href="/search/?searchtype=author&query=Castelli%2C+L">Luca Castelli</a>, <a href="/search/?searchtype=author&query=Catanesi%2C+M+G">Maria Gabriella Catanesi</a>, <a href="/search/?searchtype=author&query=Celiberto%2C+F+G">Francesco Giovanni Celiberto</a>, <a href="/search/?searchtype=author&query=Cerri%2C+A">Alessandro Cerri</a> , et al. (109 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.07261v2-abstract-short" style="display: inline;"> In the path towards a muon collider with center of mass energy of 10 TeV or more, a stage at 3 TeV emerges as an appealing option. Reviewing the physics potential of such muon collider is the main purpose of this document. In order to outline the progression of the physics performances across the stages, a few sensitivity projections for higher energy are also presented. There are many opportuniti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07261v2-abstract-full').style.display = 'inline'; document.getElementById('2203.07261v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.07261v2-abstract-full" style="display: none;"> In the path towards a muon collider with center of mass energy of 10 TeV or more, a stage at 3 TeV emerges as an appealing option. Reviewing the physics potential of such muon collider is the main purpose of this document. In order to outline the progression of the physics performances across the stages, a few sensitivity projections for higher energy are also presented. There are many opportunities for probing new physics at a 3 TeV muon collider. Some of them are in common with the extensively documented physics case of the CLIC 3 TeV energy stage, and include measuring the Higgs trilinear coupling and testing the possible composite nature of the Higgs boson and of the top quark at the 20 TeV scale. Other opportunities are unique of a 3 TeV muon collider, and stem from the fact that muons are collided rather than electrons. This is exemplified by studying the potential to explore the microscopic origin of the current $g$-2 and $B$-physics anomalies, which are both related with muons. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07261v2-abstract-full').style.display = 'none'; document.getElementById('2203.07261v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">73 pages, 28 figures; Contribution to Snowmass 2021</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.07256">arXiv:2203.07256</a> <span> [<a href="https://arxiv.org/pdf/2203.07256">pdf</a>, <a href="https://arxiv.org/format/2203.07256">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> </div> </div> <p class="title is-5 mathjax"> Muon Collider Physics Summary </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Aim%C3%A8%2C+C">Chiara Aim猫</a>, <a href="/search/?searchtype=author&query=Apyan%2C+A">Aram Apyan</a>, <a href="/search/?searchtype=author&query=Mahmoud%2C+M+A">Mohammed Attia Mahmoud</a>, <a href="/search/?searchtype=author&query=Bartosik%2C+N">Nazar Bartosik</a>, <a href="/search/?searchtype=author&query=Bertolin%2C+A">Alessandro Bertolin</a>, <a href="/search/?searchtype=author&query=Bonesini%2C+M">Maurizio Bonesini</a>, <a href="/search/?searchtype=author&query=Bottaro%2C+S">Salvatore Bottaro</a>, <a href="/search/?searchtype=author&query=Buttazzo%2C+D">Dario Buttazzo</a>, <a href="/search/?searchtype=author&query=Capdevilla%2C+R">Rodolfo Capdevilla</a>, <a href="/search/?searchtype=author&query=Casarsa%2C+M">Massimo Casarsa</a>, <a href="/search/?searchtype=author&query=Castelli%2C+L">Luca Castelli</a>, <a href="/search/?searchtype=author&query=Catanesi%2C+M+G">Maria Gabriella Catanesi</a>, <a href="/search/?searchtype=author&query=Celiberto%2C+F+G">Francesco Giovanni Celiberto</a>, <a href="/search/?searchtype=author&query=Cerri%2C+A">Alessandro Cerri</a>, <a href="/search/?searchtype=author&query=Cesarotti%2C+C">Cari Cesarotti</a>, <a href="/search/?searchtype=author&query=Chachamis%2C+G">Grigorios Chachamis</a>, <a href="/search/?searchtype=author&query=Chen%2C+S">Siyu Chen</a>, <a href="/search/?searchtype=author&query=Chien%2C+Y">Yang-Ting Chien</a>, <a href="/search/?searchtype=author&query=Chiesa%2C+M">Mauro Chiesa</a>, <a href="/search/?searchtype=author&query=Collazuol%2C+G">Gianmaria Collazuol</a>, <a href="/search/?searchtype=author&query=Costa%2C+M">Marco Costa</a>, <a href="/search/?searchtype=author&query=Craig%2C+N">Nathaniel Craig</a>, <a href="/search/?searchtype=author&query=Curtin%2C+D">David Curtin</a>, <a href="/search/?searchtype=author&query=Dasu%2C+S">Sridhara Dasu</a>, <a href="/search/?searchtype=author&query=De+Blas%2C+J">Jorge De Blas</a> , et al. (100 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.07256v2-abstract-short" style="display: inline;"> The perspective of designing muon colliders with high energy and luminosity, which is being investigated by the International Muon Collider Collaboration, has triggered a growing interest in their physics reach. We present a concise summary of the muon colliders potential to explore new physics, leveraging on the unique possibility of combining high available energy with very precise measurements. </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.07256v2-abstract-full" style="display: none;"> The perspective of designing muon colliders with high energy and luminosity, which is being investigated by the International Muon Collider Collaboration, has triggered a growing interest in their physics reach. We present a concise summary of the muon colliders potential to explore new physics, leveraging on the unique possibility of combining high available energy with very precise measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07256v2-abstract-full').style.display = 'none'; document.getElementById('2203.07256v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 7 figures; Contribution to Snowmass 2021</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.07224">arXiv:2203.07224</a> <span> [<a href="https://arxiv.org/pdf/2203.07224">pdf</a>, <a href="https://arxiv.org/format/2203.07224">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 Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Promising Technologies and R&D Directions for the Future Muon Collider Detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Jindariani%2C+S">Sergo Jindariani</a>, <a href="/search/?searchtype=author&query=Meloni%2C+F">Federico Meloni</a>, <a href="/search/?searchtype=author&query=Pastrone%2C+N">Nadia Pastrone</a>, <a href="/search/?searchtype=author&query=Aim%C3%A8%2C+C">Chiara Aim猫</a>, <a href="/search/?searchtype=author&query=Bartosik%2C+N">Nazar Bartosik</a>, <a href="/search/?searchtype=author&query=Barzi%2C+E">Emanuela Barzi</a>, <a href="/search/?searchtype=author&query=Bertolin%2C+A">Alessandro Bertolin</a>, <a href="/search/?searchtype=author&query=Braghieri%2C+A">Alessandro Braghieri</a>, <a href="/search/?searchtype=author&query=Buonincontri%2C+L">Laura Buonincontri</a>, <a href="/search/?searchtype=author&query=Calzaferri%2C+S">Simone Calzaferri</a>, <a href="/search/?searchtype=author&query=Casarsa%2C+M">Massimo Casarsa</a>, <a href="/search/?searchtype=author&query=Catanesi%2C+M+G">Maria Gabriella Catanesi</a>, <a href="/search/?searchtype=author&query=Cerri%2C+A">Alessandro Cerri</a>, <a href="/search/?searchtype=author&query=Chachamis%2C+G">Grigorios Chachamis</a>, <a href="/search/?searchtype=author&query=Colaleo%2C+A">Anna Colaleo</a>, <a href="/search/?searchtype=author&query=Curatolo%2C+C">Camilla Curatolo</a>, <a href="/search/?searchtype=author&query=Da+Molin%2C+G">Giacomo Da Molin</a>, <a href="/search/?searchtype=author&query=Delahaye%2C+J">Jean-Pierre Delahaye</a>, <a href="/search/?searchtype=author&query=Di+Micco%2C+B">Biagio Di Micco</a>, <a href="/search/?searchtype=author&query=Dorigo%2C+T">Tommaso Dorigo</a>, <a href="/search/?searchtype=author&query=Errico%2C+F">Filippo Errico</a>, <a href="/search/?searchtype=author&query=Fiorina%2C+D">Davide Fiorina</a>, <a href="/search/?searchtype=author&query=Gianelle%2C+A">Alessio Gianelle</a>, <a href="/search/?searchtype=author&query=Giraldin%2C+C">Carlo Giraldin</a>, <a href="/search/?searchtype=author&query=Hauptman%2C+J">John Hauptman</a> , et al. (36 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.07224v1-abstract-short" style="display: inline;"> Among the post-LHC generation of particle accelerators, the muon collider represents a unique machine with capability to provide very high energy leptonic collisions and to open the path to a vast and mostly unexplored physics programme. However, on the experimental side, such great physics potential is accompanied by unprecedented technological challenges, due to the fact that muons are unstable… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07224v1-abstract-full').style.display = 'inline'; document.getElementById('2203.07224v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.07224v1-abstract-full" style="display: none;"> Among the post-LHC generation of particle accelerators, the muon collider represents a unique machine with capability to provide very high energy leptonic collisions and to open the path to a vast and mostly unexplored physics programme. However, on the experimental side, such great physics potential is accompanied by unprecedented technological challenges, due to the fact that muons are unstable particles. Their decay products interact with the machine elements and produce an intense flux of background particles that eventually reach the detector and may degrade its performance. In this paper, we present technologies that have a potential to match the challenging specifications of a muon collider detector and outline a path forward for the future R&D efforts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07224v1-abstract-full').style.display = 'none'; document.getElementById('2203.07224v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Contribution to Snowmass 2021, 27 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/2203.06525">arXiv:2203.06525</a> <span> [<a href="https://arxiv.org/pdf/2203.06525">pdf</a>, <a href="https://arxiv.org/format/2203.06525">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 Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> MPGDs for tracking and Muon detection at future high energy physics colliders </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Black%2C+K">K. Black</a>, <a href="/search/?searchtype=author&query=Colaleo%2C+A">A. Colaleo</a>, <a href="/search/?searchtype=author&query=Aim%C3%A8%2C+C">C. Aim猫</a>, <a href="/search/?searchtype=author&query=Alviggi%2C+M">M. Alviggi</a>, <a href="/search/?searchtype=author&query=Aruta%2C+C">C. Aruta</a>, <a href="/search/?searchtype=author&query=Bianco%2C+M">M. Bianco</a>, <a href="/search/?searchtype=author&query=Balossino%2C+I">I. Balossino</a>, <a href="/search/?searchtype=author&query=Bencivenni%2C+G">G. Bencivenni</a>, <a href="/search/?searchtype=author&query=Bertani%2C+M">M. Bertani</a>, <a href="/search/?searchtype=author&query=Braghieri%2C+A">A. Braghieri</a>, <a href="/search/?searchtype=author&query=Cafaro%2C+V">V. Cafaro</a>, <a href="/search/?searchtype=author&query=Calzaferri%2C+S">S. Calzaferri</a>, <a href="/search/?searchtype=author&query=Camerlingo%2C+M+T">M. T. Camerlingo</a>, <a href="/search/?searchtype=author&query=Canale%2C+V">V. Canale</a>, <a href="/search/?searchtype=author&query=Cibinetto%2C+G">G. Cibinetto</a>, <a href="/search/?searchtype=author&query=Corbetta%2C+M">M. Corbetta</a>, <a href="/search/?searchtype=author&query=D%27Amico%2C+V">V. D'Amico</a>, <a href="/search/?searchtype=author&query=De+Lucia%2C+E">E. De Lucia</a>, <a href="/search/?searchtype=author&query=Della+Pietra%2C+M">M. Della Pietra</a>, <a href="/search/?searchtype=author&query=Di+Donato%2C+C">C. Di Donato</a>, <a href="/search/?searchtype=author&query=Di+Nardo%2C+R">R. Di Nardo</a>, <a href="/search/?searchtype=author&query=Domenici%2C+D">D. Domenici</a>, <a href="/search/?searchtype=author&query=Errico%2C+F">F. Errico</a>, <a href="/search/?searchtype=author&query=Everaerts%2C+P">P. Everaerts</a>, <a href="/search/?searchtype=author&query=Fallavollita%2C+F">F. Fallavollita</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="2203.06525v1-abstract-short" style="display: inline;"> In the next years, the energy and intensity frontiers of the experimental Particle Physics will be pushed forward with the upgrade of existing accelerators (LHC at CERN) and the envisaged construction of new machines at energy scales up to hundreds TeV or with unprecedented intensity (FCC-hh, FCC-ee, ILC, Muon Collider). Large size, cost-effective, high-efficiency detection systems in high backgro… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.06525v1-abstract-full').style.display = 'inline'; document.getElementById('2203.06525v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.06525v1-abstract-full" style="display: none;"> In the next years, the energy and intensity frontiers of the experimental Particle Physics will be pushed forward with the upgrade of existing accelerators (LHC at CERN) and the envisaged construction of new machines at energy scales up to hundreds TeV or with unprecedented intensity (FCC-hh, FCC-ee, ILC, Muon Collider). Large size, cost-effective, high-efficiency detection systems in high background environments are required in order to accomplish the physics program. MPGDs offer a diversity of technologies that allow them to meet the required performance challenges at future facilities thanks to the specific advantages that each technology provides. MPGDs allow stable operation, with environmentally friendly gas mixtures, at very high background particle flux with high detection efficiency and excellent spatial resolution. These features make MPGD one of the primary choices as precise muon tracking and trigger system in general-purpose detectors at future HEP colliders. In addition, the low material budget and the flexibility of the base material make MPGDs suitable for the development of very light, full cylindrical fine tracking inner trackers at lepton colliders. On-going R&Ds aim at pushing the detector performance at the limits of each technology. We are working in continuing to consolidate the construction and stable operation of large-size detectors, able to cope with large particle fluxes. In this white paper, we describe some of the most prominent MPGD technologies, their performance measurements, the challenges faced in the most recent applications, and the areas of improvement towards efficient tracking and Muon detection at future high energy physics colliders. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.06525v1-abstract-full').style.display = 'none'; document.getElementById('2203.06525v1-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 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Contribution to Snowmass 2021</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.05489">arXiv:2108.05489</a> <span> [<a href="https://arxiv.org/pdf/2108.05489">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Human-Computer Interaction">cs.HC</span> </div> </div> <p class="title is-5 mathjax"> Advancing Data for Street-level Flood Vulnerability: Extraction of Variables from Google Street View in Quito, Ecuador </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Velez%2C+R">Raychell Velez</a>, <a href="/search/?searchtype=author&query=Calderon%2C+D">Diana Calderon</a>, <a href="/search/?searchtype=author&query=Carey%2C+L">Lauren Carey</a>, <a href="/search/?searchtype=author&query=Aime%2C+C">Christopher Aime</a>, <a href="/search/?searchtype=author&query=Hultquist%2C+C">Carolynne Hultquist</a>, <a href="/search/?searchtype=author&query=Yetman%2C+G">Greg Yetman</a>, <a href="/search/?searchtype=author&query=Kruczkiewicz%2C+A">Andrew Kruczkiewicz</a>, <a href="/search/?searchtype=author&query=Gorokhovich%2C+Y">Yuri Gorokhovich</a>, <a href="/search/?searchtype=author&query=Chen%2C+R+S">Robert S. Chen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2108.05489v1-abstract-short" style="display: inline;"> Data relevant to flood vulnerability is minimal and infrequently collected, if at all, for much of the world. This makes it difficult to highlight areas for humanitarian aid, monitor changes, and support communities in need. It would be time consuming and resource intensive to do an exhaustive study for multiple flood relevant vulnerability variables using a field survey. We use a mixed methods ap… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.05489v1-abstract-full').style.display = 'inline'; document.getElementById('2108.05489v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.05489v1-abstract-full" style="display: none;"> Data relevant to flood vulnerability is minimal and infrequently collected, if at all, for much of the world. This makes it difficult to highlight areas for humanitarian aid, monitor changes, and support communities in need. It would be time consuming and resource intensive to do an exhaustive study for multiple flood relevant vulnerability variables using a field survey. We use a mixed methods approach to develop a survey on variables of interest and utilize an open-source crowdsourcing technique to remotely collect data with a human-machine interface using high-resolution satellite images and Google Street View. This paper focuses on Quito, Ecuador as a case study, but the methodology can be quickly replicated to produce labelled training data in other areas. The overall project goal is to build training datasets that in the future will allow us to automate the mapping of flood vulnerability for urban areas in geographic regions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.05489v1-abstract-full').style.display = 'none'; document.getElementById('2108.05489v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 5 figures, ACM KDD Workshop on Data-Driven Humanitarian Mapping 2021</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">ACM Class:</span> J.2.5 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.09364">arXiv:2107.09364</a> <span> [<a href="https://arxiv.org/pdf/2107.09364">pdf</a>, <a href="https://arxiv.org/format/2107.09364">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 Detectors">physics.ins-det</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/10.1088/1748-0221/16/11/P11014">10.1088/1748-0221/16/11/P11014 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Performance of a Triple-GEM Demonstrator in $pp$ Collisions at the CMS Detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abbas%2C+M">M. Abbas</a>, <a href="/search/?searchtype=author&query=Abbrescia%2C+M">M. Abbrescia</a>, <a href="/search/?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/?searchtype=author&query=Abdelalim%2C+A">A. Abdelalim</a>, <a href="/search/?searchtype=author&query=AbuZeid%2C+S">S. AbuZeid</a>, <a href="/search/?searchtype=author&query=Agapitos%2C+A">A. Agapitos</a>, <a href="/search/?searchtype=author&query=Ahmad%2C+A">A. Ahmad</a>, <a href="/search/?searchtype=author&query=Ahmed%2C+A">A. Ahmed</a>, <a href="/search/?searchtype=author&query=Ahmed%2C+W">W. Ahmed</a>, <a href="/search/?searchtype=author&query=Aim%C3%A8%2C+C">C. Aim猫</a>, <a href="/search/?searchtype=author&query=Aruta%2C+C">C. Aruta</a>, <a href="/search/?searchtype=author&query=Asghar%2C+I">I. Asghar</a>, <a href="/search/?searchtype=author&query=Aspell%2C+P">P. Aspell</a>, <a href="/search/?searchtype=author&query=Avila%2C+C">C. Avila</a>, <a href="/search/?searchtype=author&query=Babbar%2C+J">J. Babbar</a>, <a href="/search/?searchtype=author&query=Ban%2C+Y">Y. Ban</a>, <a href="/search/?searchtype=author&query=Band%2C+R">R. Band</a>, <a href="/search/?searchtype=author&query=Bansal%2C+S">S. Bansal</a>, <a href="/search/?searchtype=author&query=Benussi%2C+L">L. Benussi</a>, <a href="/search/?searchtype=author&query=Bhatnagar%2C+V">V. Bhatnagar</a>, <a href="/search/?searchtype=author&query=Bianco%2C+M">M. Bianco</a>, <a href="/search/?searchtype=author&query=Bianco%2C+S">S. Bianco</a>, <a href="/search/?searchtype=author&query=Black%2C+K">K. Black</a>, <a href="/search/?searchtype=author&query=Borgonovi%2C+L">L. Borgonovi</a>, <a href="/search/?searchtype=author&query=Bouhali%2C+O">O. Bouhali</a> , et al. (156 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2107.09364v2-abstract-short" style="display: inline;"> After the Phase-2 high-luminosity upgrade to the Large Hadron Collider (LHC), the collision rate and therefore the background rate will significantly increase, particularly in the high $畏$ region. To improve both the tracking and triggering of muons, the Compact Muon Solenoid (CMS) Collaboration plans to install triple-layer Gas Electron Multiplier (GEM) detectors in the CMS muon endcaps. Demonstr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.09364v2-abstract-full').style.display = 'inline'; document.getElementById('2107.09364v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.09364v2-abstract-full" style="display: none;"> After the Phase-2 high-luminosity upgrade to the Large Hadron Collider (LHC), the collision rate and therefore the background rate will significantly increase, particularly in the high $畏$ region. To improve both the tracking and triggering of muons, the Compact Muon Solenoid (CMS) Collaboration plans to install triple-layer Gas Electron Multiplier (GEM) detectors in the CMS muon endcaps. Demonstrator GEM detectors were installed in CMS during 2017 to gain operational experience and perform a preliminary investigation of detector performance. We present the results of triple-GEM detector performance studies performed in situ during normal CMS and LHC operations in 2018. The distribution of cluster size and the efficiency to reconstruct high $p_T$ muons in proton--proton collisions are presented as well as the measurement of the environmental background rate to produce hits in the GEM detector. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.09364v2-abstract-full').style.display = 'none'; document.getElementById('2107.09364v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 5 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.03621">arXiv:2107.03621</a> <span> [<a href="https://arxiv.org/pdf/2107.03621">pdf</a>, <a href="https://arxiv.org/format/2107.03621">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 Detectors">physics.ins-det</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/10.1088/1748-0221/16/12/P12026">10.1088/1748-0221/16/12/P12026 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Modeling the triple-GEM detector response to background particles for the CMS Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abbas%2C+M">M. Abbas</a>, <a href="/search/?searchtype=author&query=Abbrescia%2C+M">M. Abbrescia</a>, <a href="/search/?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/?searchtype=author&query=Abdelalim%2C+A">A. Abdelalim</a>, <a href="/search/?searchtype=author&query=AbuZeid%2C+S">S. AbuZeid</a>, <a href="/search/?searchtype=author&query=Agapitos%2C+A">A. Agapitos</a>, <a href="/search/?searchtype=author&query=Ahmad%2C+A">A. Ahmad</a>, <a href="/search/?searchtype=author&query=Ahmed%2C+A">A. Ahmed</a>, <a href="/search/?searchtype=author&query=Ahmed%2C+W">W. Ahmed</a>, <a href="/search/?searchtype=author&query=Aim%C3%A8%2C+C">C. Aim猫</a>, <a href="/search/?searchtype=author&query=Aruta%2C+C">C. Aruta</a>, <a href="/search/?searchtype=author&query=Asghar%2C+I">I. Asghar</a>, <a href="/search/?searchtype=author&query=Aspell%2C+P">P. Aspell</a>, <a href="/search/?searchtype=author&query=Avila%2C+C">C. Avila</a>, <a href="/search/?searchtype=author&query=Azhgirey%2C+I">I. Azhgirey</a>, <a href="/search/?searchtype=author&query=Babbar%2C+J">J. Babbar</a>, <a href="/search/?searchtype=author&query=Ban%2C+Y">Y. Ban</a>, <a href="/search/?searchtype=author&query=Band%2C+R">R. Band</a>, <a href="/search/?searchtype=author&query=Bansal%2C+S">S. Bansal</a>, <a href="/search/?searchtype=author&query=Benussi%2C+L">L. Benussi</a>, <a href="/search/?searchtype=author&query=Bhatnagar%2C+V">V. Bhatnagar</a>, <a href="/search/?searchtype=author&query=Bianco%2C+M">M. Bianco</a>, <a href="/search/?searchtype=author&query=Bianco%2C+S">S. Bianco</a>, <a href="/search/?searchtype=author&query=Black%2C+K">K. Black</a>, <a href="/search/?searchtype=author&query=Borgonovi%2C+L">L. Borgonovi</a> , et al. (164 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2107.03621v1-abstract-short" style="display: inline;"> An estimate of environmental background hit rate on triple-GEM chambers is performed using Monte Carlo (MC) simulation and compared to data taken by test chambers installed in the CMS experiment (GE1/1) during Run-2 at the Large Hadron Collider (LHC). The hit rate is measured using data collected with proton-proton collisions at 13 TeV and a luminosity of 1.5$\times10^{34}$ cm$^{-2}$ s$^{-1}$. The… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.03621v1-abstract-full').style.display = 'inline'; document.getElementById('2107.03621v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.03621v1-abstract-full" style="display: none;"> An estimate of environmental background hit rate on triple-GEM chambers is performed using Monte Carlo (MC) simulation and compared to data taken by test chambers installed in the CMS experiment (GE1/1) during Run-2 at the Large Hadron Collider (LHC). The hit rate is measured using data collected with proton-proton collisions at 13 TeV and a luminosity of 1.5$\times10^{34}$ cm$^{-2}$ s$^{-1}$. The simulation framework uses a combination of the FLUKA and Geant4 packages to obtain the hit rate. FLUKA provides the radiation environment around the GE1/1 chambers, which is comprised of the particle flux with momentum direction and energy spectra ranging from $10^{-11}$ to $10^{4}$ MeV for neutrons, $10^{-3}$ to $10^{4}$ MeV for $纬$'s, $10^{-2}$ to $10^{4}$ MeV for $e^{\pm}$, and $10^{-1}$ to $10^{4}$ MeV for charged hadrons. Geant4 provides an estimate of detector response (sensitivity) based on an accurate description of detector geometry, material composition and interaction of particles with the various detector layers. The MC simulated hit rate is estimated as a function of the perpendicular distance from the beam line and agrees with data within the assigned uncertainties of 10-14.5%. This simulation framework can be used to obtain a reliable estimate of background rates expected at the High Luminosity LHC. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.03621v1-abstract-full').style.display = 'none'; document.getElementById('2107.03621v1-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 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 9 figures, 6 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/2009.09505">arXiv:2009.09505</a> <span> [<a href="https://arxiv.org/pdf/2009.09505">pdf</a>, <a href="https://arxiv.org/format/2009.09505">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 Detectors">physics.ins-det</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/10.1088/1748-0221/15/12/P12019">10.1088/1748-0221/15/12/P12019 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Interstrip Capacitances of the Readout Board used in Large Triple-GEM Detectors for the CMS Muon Upgrade </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abbas%2C+M">M. Abbas</a>, <a href="/search/?searchtype=author&query=Abbrescia%2C+M">M. Abbrescia</a>, <a href="/search/?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/?searchtype=author&query=Abdelalim%2C+A">A. Abdelalim</a>, <a href="/search/?searchtype=author&query=AbuZeid%2C+S">S. AbuZeid</a>, <a href="/search/?searchtype=author&query=Agapitos%2C+A">A. Agapitos</a>, <a href="/search/?searchtype=author&query=Ahmad%2C+A">A. Ahmad</a>, <a href="/search/?searchtype=author&query=Ahmed%2C+A">A. Ahmed</a>, <a href="/search/?searchtype=author&query=Ahmed%2C+W">W. Ahmed</a>, <a href="/search/?searchtype=author&query=Aim%C3%A8%2C+C">C. Aim猫</a>, <a href="/search/?searchtype=author&query=Aruta%2C+C">C. Aruta</a>, <a href="/search/?searchtype=author&query=Asghar%2C+I">I. Asghar</a>, <a href="/search/?searchtype=author&query=Aspell%2C+P">P. Aspell</a>, <a href="/search/?searchtype=author&query=Avila%2C+C">C. Avila</a>, <a href="/search/?searchtype=author&query=Babbar%2C+J">J. Babbar</a>, <a href="/search/?searchtype=author&query=Ban%2C+Y">Y. Ban</a>, <a href="/search/?searchtype=author&query=Band%2C+R">R. Band</a>, <a href="/search/?searchtype=author&query=Bansal%2C+S">S. Bansal</a>, <a href="/search/?searchtype=author&query=Benussi%2C+L">L. Benussi</a>, <a href="/search/?searchtype=author&query=Bhatnagar%2C+V">V. Bhatnagar</a>, <a href="/search/?searchtype=author&query=Bianco%2C+M">M. Bianco</a>, <a href="/search/?searchtype=author&query=Bianco%2C+S">S. Bianco</a>, <a href="/search/?searchtype=author&query=Black%2C+K">K. Black</a>, <a href="/search/?searchtype=author&query=Borgonovi%2C+L">L. Borgonovi</a>, <a href="/search/?searchtype=author&query=Bouhali%2C+O">O. Bouhali</a> , et al. (156 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="2009.09505v1-abstract-short" style="display: inline;"> We present analytical calculations, Finite Element Analysis modeling, and physical measurements of the interstrip capacitances for different potential strip geometries and dimensions of the readout boards for the GE2/1 triple-Gas Electron Multiplier detector in the CMS muon system upgrade. The main goal of the study is to find configurations that minimize the interstrip capacitances and consequent… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.09505v1-abstract-full').style.display = 'inline'; document.getElementById('2009.09505v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.09505v1-abstract-full" style="display: none;"> We present analytical calculations, Finite Element Analysis modeling, and physical measurements of the interstrip capacitances for different potential strip geometries and dimensions of the readout boards for the GE2/1 triple-Gas Electron Multiplier detector in the CMS muon system upgrade. The main goal of the study is to find configurations that minimize the interstrip capacitances and consequently maximize the signal-to-noise ratio for the detector. We find agreement at the 1.5--4.8% level between the two methods of calculations and on the average at the 17% level between calculations and measurements. A configuration with halved strip lengths and doubled strip widths results in a measured 27--29% reduction over the original configuration while leaving the total number of strips unchanged. We have now adopted this design modification for all eight module types of the GE2/1 detector and will produce the final detector with this new strip design. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.09505v1-abstract-full').style.display = 'none'; document.getElementById('2009.09505v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2020 JINST 15 P12019 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.10437">arXiv:2001.10437</a> <span> [<a href="https://arxiv.org/pdf/2001.10437">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Neurons and Cognition">q-bio.NC</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"> Differentiation of neural-type cells on multi-scale ordered collagen-silica bionanocomposites </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Debons%2C+N">Nicolas Debons</a>, <a href="/search/?searchtype=author&query=Dems%2C+D">Dounia Dems</a>, <a href="/search/?searchtype=author&query=H%C3%A9lary%2C+C">Christophe H茅lary</a>, <a href="/search/?searchtype=author&query=Grill%2C+S+L">Sylvain Le Grill</a>, <a href="/search/?searchtype=author&query=Picaut%2C+L">Lise Picaut</a>, <a href="/search/?searchtype=author&query=Renaud%2C+F">Flore Renaud</a>, <a href="/search/?searchtype=author&query=Delsuc%2C+N">Nicolas Delsuc</a>, <a href="/search/?searchtype=author&query=Schanne-Klein%2C+M">Marie-Claire Schanne-Klein</a>, <a href="/search/?searchtype=author&query=Coradin%2C+T">Thibaud Coradin</a>, <a href="/search/?searchtype=author&query=Aim%C3%A9%2C+C">Carole Aim茅</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="2001.10437v1-abstract-short" style="display: inline;"> Cells respond to biophysical and biochemical signals. We developed a composite filament from collagen and silica particles modified to interact with collagen and/or present a laminin epitope (IKVAV) crucial for cell-matrix adhesion and signal transduction. This combines scaffolding and signaling and shows that local tuning of collagen organization enhances cell differentiation. </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.10437v1-abstract-full" style="display: none;"> Cells respond to biophysical and biochemical signals. We developed a composite filament from collagen and silica particles modified to interact with collagen and/or present a laminin epitope (IKVAV) crucial for cell-matrix adhesion and signal transduction. This combines scaffolding and signaling and shows that local tuning of collagen organization enhances cell differentiation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.10437v1-abstract-full').style.display = 'none'; document.getElementById('2001.10437v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Biomaterials Science, Royal Society of Chemistry (RSC), 2020 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1811.09648">arXiv:1811.09648</a> <span> [<a href="https://arxiv.org/pdf/1811.09648">pdf</a>, <a href="https://arxiv.org/format/1811.09648">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/aas:1997215">10.1051/aas:1997215 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Imaging binary stars by the cross-correlation technique </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Aristidi%2C+E">Eric Aristidi</a>, <a href="/search/?searchtype=author&query=Carbillet%2C+M">Marcel Carbillet</a>, <a href="/search/?searchtype=author&query=Lyon%2C+J">Jean-F茅lix Lyon</a>, <a href="/search/?searchtype=author&query=Aime%2C+C">Claude Aime</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1811.09648v1-abstract-short" style="display: inline;"> We present in this paper a technique for imaging binary stars from speckle data. This technique is based upon the computation of the cross-correlation between the speckle frames and their square. This may be considered as a simple, easy to implement, complementary computation to the autocorrelation function of Labeyrie's technique for a rapid determination of the position angle of binary systems.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.09648v1-abstract-full').style.display = 'inline'; document.getElementById('1811.09648v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1811.09648v1-abstract-full" style="display: none;"> We present in this paper a technique for imaging binary stars from speckle data. This technique is based upon the computation of the cross-correlation between the speckle frames and their square. This may be considered as a simple, easy to implement, complementary computation to the autocorrelation function of Labeyrie's technique for a rapid determination of the position angle of binary systems. Angular separation, absolute position angle and relative photometry of binary stars can be derived from this technique. We show an application to the bright double star zeta Sge observed at the 2m Telescope Bernard Lyot. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.09648v1-abstract-full').style.display = 'none'; document.getElementById('1811.09648v1-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 November, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A & A Supplement series, Vol. 125, October 1997, p.139-148 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1407.6654">arXiv:1407.6654</a> <span> [<a href="https://arxiv.org/pdf/1407.6654">pdf</a>, <a href="https://arxiv.org/format/1407.6654">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201423680">10.1051/0004-6361/201423680 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Optimization of starshades: focal plane versus pupil plane </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Flamary%2C+R">R茅mi Flamary</a>, <a href="/search/?searchtype=author&query=Aime%2C+C">Claude Aime</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="1407.6654v1-abstract-short" style="display: inline;"> We search for the best possible transmission for an external occulter coronagraph that is dedicated to the direct observation of terrestrial exoplanets. We show that better observation conditions are obtained when the flux in the focal plane is minimized in the zone in which the exoplanet is observed, instead of the total flux received by the telescope. We describe the transmission of the occulter… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.6654v1-abstract-full').style.display = 'inline'; document.getElementById('1407.6654v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1407.6654v1-abstract-full" style="display: none;"> We search for the best possible transmission for an external occulter coronagraph that is dedicated to the direct observation of terrestrial exoplanets. We show that better observation conditions are obtained when the flux in the focal plane is minimized in the zone in which the exoplanet is observed, instead of the total flux received by the telescope. We describe the transmission of the occulter as a sum of basis functions. For each element of the basis, we numerically computed the Fresnel diffraction at the aperture of the telescope and the complex amplitude at its focus. The basis functions are circular disks that are linearly apodized over a few centimeters (truncated cones). We complemented the numerical calculation of the Fresnel diffraction for these functions by a comparison with pure circular discs (cylinder) for which an analytical expression, based on a decomposition in Lommel series, is available. The technique of deriving the optimal transmission for a given spectral bandwidth is a classical regularized quadratic minimization of intensities, but linear optimizations can be used as well. Minimizing the integrated intensity on the aperture of the telescope or for selected regions of the focal plane leads to slightly different transmissions for the occulter. For the focal plane optimization, the resulting residual intensity is concentrated behind the geometrical image of the occulter, in a blind region for the observation of an exoplanet, and the level of background residual starlight becomes very low outside this image. Finally, we provide a tolerance analysis for the alignment of the occulter to the telescope which also favors the focal plane optimization.This means that telescope offsets of a few decimeters do not strongly reduce the efficiency of the occulter. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.6654v1-abstract-full').style.display = 'none'; document.getElementById('1407.6654v1-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 July, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 569, A28 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0911.2936">arXiv:0911.2936</a> <span> [<a href="https://arxiv.org/pdf/0911.2936">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Exoplanet Characterization and the Search for Life </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kasting%2C+J">J. Kasting</a>, <a href="/search/?searchtype=author&query=Traub%2C+W">W. Traub</a>, <a href="/search/?searchtype=author&query=Roberge%2C+A">A. Roberge</a>, <a href="/search/?searchtype=author&query=Leger%2C+A">A. Leger</a>, <a href="/search/?searchtype=author&query=Schwartz%2C+A">A. Schwartz</a>, <a href="/search/?searchtype=author&query=Wooten%2C+A">A. Wooten</a>, <a href="/search/?searchtype=author&query=Vosteen%2C+A">A. Vosteen</a>, <a href="/search/?searchtype=author&query=Lo%2C+A">A. Lo</a>, <a href="/search/?searchtype=author&query=Brack%2C+A">A. Brack</a>, <a href="/search/?searchtype=author&query=Tanner%2C+A">A. Tanner</a>, <a href="/search/?searchtype=author&query=Coustenis%2C+A">A. Coustenis</a>, <a href="/search/?searchtype=author&query=Lane%2C+B">B. Lane</a>, <a href="/search/?searchtype=author&query=Oppenheimer%2C+B">B. Oppenheimer</a>, <a href="/search/?searchtype=author&query=Mennesson%2C+B">B. Mennesson</a>, <a href="/search/?searchtype=author&query=Lopez%2C+B">B. Lopez</a>, <a href="/search/?searchtype=author&query=Grillmair%2C+C">C. Grillmair</a>, <a href="/search/?searchtype=author&query=Beichman%2C+C">C. Beichman</a>, <a href="/search/?searchtype=author&query=Cockell%2C+C">C. Cockell</a>, <a href="/search/?searchtype=author&query=Hanot%2C+C">C. Hanot</a>, <a href="/search/?searchtype=author&query=McCarthy%2C+C">C. McCarthy</a>, <a href="/search/?searchtype=author&query=Stark%2C+C">C. Stark</a>, <a href="/search/?searchtype=author&query=Marois%2C+C">C. Marois</a>, <a href="/search/?searchtype=author&query=Aime%2C+C">C. Aime</a>, <a href="/search/?searchtype=author&query=Angerhausen%2C+D">D. Angerhausen</a>, <a href="/search/?searchtype=author&query=Montes%2C+D">D. Montes</a> , et al. (97 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="0911.2936v1-abstract-short" style="display: inline;"> Over 300 extrasolar planets (exoplanets) have been detected orbiting nearby stars. We now hope to conduct a census of all planets around nearby stars and to characterize their atmospheres and surfaces with spectroscopy. Rocky planets within their star's habitable zones have the highest priority, as these have the potential to harbor life. Our science goal is to find and characterize all nearby e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0911.2936v1-abstract-full').style.display = 'inline'; document.getElementById('0911.2936v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0911.2936v1-abstract-full" style="display: none;"> Over 300 extrasolar planets (exoplanets) have been detected orbiting nearby stars. We now hope to conduct a census of all planets around nearby stars and to characterize their atmospheres and surfaces with spectroscopy. Rocky planets within their star's habitable zones have the highest priority, as these have the potential to harbor life. Our science goal is to find and characterize all nearby exoplanets; this requires that we measure the mass, orbit, and spectroscopic signature of each one at visible and infrared wavelengths. The techniques for doing this are at hand today. Within the decade we could answer long-standing questions about the evolution and nature of other planetary systems, and we could search for clues as to whether life exists elsewhere in our galactic neighborhood. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0911.2936v1-abstract-full').style.display = 'none'; document.getElementById('0911.2936v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 November, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 2 figures, submitted to Astro2010 Decadal Review</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0706.1739">arXiv:0706.1739</a> <span> [<a href="https://arxiv.org/pdf/0706.1739">pdf</a>, <a href="https://arxiv.org/ps/0706.1739">ps</a>, <a href="https://arxiv.org/format/0706.1739">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-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/10.1086/520913">10.1086/520913 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Speckle noise and dynamic range in coronagraphic images </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Soummer%2C+R">R茅mi Soummer</a>, <a href="/search/?searchtype=author&query=Ferrari%2C+A">Andr茅 Ferrari</a>, <a href="/search/?searchtype=author&query=Aime%2C+C">Claude Aime</a>, <a href="/search/?searchtype=author&query=Jolissaint%2C+L">Laurent Jolissaint</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="0706.1739v1-abstract-short" style="display: inline;"> This paper is concerned with the theoretical properties of high contrast coronagraphic images in the context of exoplanet searches. We derive and analyze the statistical properties of the residual starlight in coronagraphic images, and describe the effect of a coronagraph on the speckle and photon noise. Current observations with coronagraphic instruments have shown that the main limitations to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0706.1739v1-abstract-full').style.display = 'inline'; document.getElementById('0706.1739v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0706.1739v1-abstract-full" style="display: none;"> This paper is concerned with the theoretical properties of high contrast coronagraphic images in the context of exoplanet searches. We derive and analyze the statistical properties of the residual starlight in coronagraphic images, and describe the effect of a coronagraph on the speckle and photon noise. Current observations with coronagraphic instruments have shown that the main limitations to high contrast imaging are due to residual quasi-static speckles. We tackle this problem in this paper, and propose a generalization of our statistical model to include the description of static, quasi-static and fast residual atmospheric speckles. The results provide insight into the effects on the dynamic range of wavefront control, coronagraphy, active speckle reduction, and differential speckle calibration. The study is focused on ground-based imaging with extreme adaptive optics, but the approach is general enough to be applicable to space, with different parameters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0706.1739v1-abstract-full').style.display = 'none'; document.getElementById('0706.1739v1-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 June, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2007. </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, 18 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/astro-ph/0703655">arXiv:astro-ph/0703655</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0703655">pdf</a>, <a href="https://arxiv.org/format/astro-ph/0703655">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-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.crhy.2007.05.008">10.1016/j.crhy.2007.05.008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Introduction to stellar coronagraphy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ferrari%2C+A">A. Ferrari</a>, <a href="/search/?searchtype=author&query=Soummer%2C+R">R. Soummer</a>, <a href="/search/?searchtype=author&query=Aime%2C+C">C. Aime</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="astro-ph/0703655v4-abstract-short" style="display: inline;"> This paper gives a simple and original presentation of various coronagraphs inherited from the Lyot coronagraph. We first present the Lyot and Roddier phase mask coronagraphs and study their properties as a function of the focal mask size. We show that the Roddier phase mask can be used to produce an apodization for the star. Optimal coronagraphy can be obtained from two main approaches, using p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0703655v4-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0703655v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0703655v4-abstract-full" style="display: none;"> This paper gives a simple and original presentation of various coronagraphs inherited from the Lyot coronagraph. We first present the Lyot and Roddier phase mask coronagraphs and study their properties as a function of the focal mask size. We show that the Roddier phase mask can be used to produce an apodization for the star. Optimal coronagraphy can be obtained from two main approaches, using prolate spheroidal pupil apodization and a finite-size focal mask, or using a clear aperture and an infinite mask of variable transmission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0703655v4-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0703655v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 October, 2008; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 March, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2007. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ComptesRendusPhysique8:277-287,2007 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0306419">arXiv:astro-ph/0306419</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0306419">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0306419">ps</a>, <a href="https://arxiv.org/format/astro-ph/0306419">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-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/10.1051/0004-6361:20031111">10.1051/0004-6361:20031111 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ringing effects reduction by improved deconvolution algorithm Application to A370 CFHT image of gravitational arcs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Roche%2C+M">Muriel Roche</a>, <a href="/search/?searchtype=author&query=Bracco%2C+C">Christian Bracco</a>, <a href="/search/?searchtype=author&query=Aime%2C+C">Claude Aime</a>, <a href="/search/?searchtype=author&query=Lanteri%2C+H">Henri Lanteri</a>, <a href="/search/?searchtype=author&query=Mellier%2C+Y">Yannick Mellier</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="astro-ph/0306419v1-abstract-short" style="display: inline;"> We develop a self-consistent automatic procedure to restore informations from astronomical observations. It relies on both a new deconvolution algorithm called LBCA (Lower Bound Constraint Algorithm) and the use of the Wiener filter. In order to explore its scientific potential for strong and weak gravitational lensing, we process a CFHT image of the galaxies cluster Abell 370 which exhibits spe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0306419v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0306419v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0306419v1-abstract-full" style="display: none;"> We develop a self-consistent automatic procedure to restore informations from astronomical observations. It relies on both a new deconvolution algorithm called LBCA (Lower Bound Constraint Algorithm) and the use of the Wiener filter. In order to explore its scientific potential for strong and weak gravitational lensing, we process a CFHT image of the galaxies cluster Abell 370 which exhibits spectacular strong gravitational lensing effects. A high quality restoration is here of particular interest to map the dark matter within the cluster. We show that the LBCA turns out specially efficient to reduce ringing effects introduced by classical deconvolution algorithms in images with a high background. The method allows us to make a blind detection of the radial arc and to recover morphological properties similar to thoseobserved from HST data. We also show that the Wiener filter is suitable to stop the iterative process before noise amplification, using only the unrestored data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0306419v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0306419v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 June, 2003; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2003. </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">A&A in press 9 pages 9 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0009198">arXiv:astro-ph/0009198</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0009198">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0009198">ps</a>, <a href="https://arxiv.org/format/astro-ph/0009198">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-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/10.1051/aas:2000227">10.1051/aas:2000227 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Adaptive optics imaging of P Cygni in Halpha </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Chesneau%2C+O">O. Chesneau</a>, <a href="/search/?searchtype=author&query=Roche%2C+M">M. Roche</a>, <a href="/search/?searchtype=author&query=Boccaletti%2C+A">A. Boccaletti</a>, <a href="/search/?searchtype=author&query=Abe%2C+L">L. Abe</a>, <a href="/search/?searchtype=author&query=Moutou%2C+C">C. Moutou</a>, <a href="/search/?searchtype=author&query=Charbonnier%2C+F">F. Charbonnier</a>, <a href="/search/?searchtype=author&query=Aime%2C+C">C. Aime</a>, <a href="/search/?searchtype=author&query=Lanteri%2C+H">H. Lanteri</a>, <a href="/search/?searchtype=author&query=Vakili%2C+F">F. Vakili</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="astro-ph/0009198v1-abstract-short" style="display: inline;"> We obtained Halpha diffraction limited data of the LBV star P Cyg using the ONERA Adaptive Optics (AO) facility BOA at the OHP 1.52m telescope on October 1997. Taking P Cyg and the reference star 59 Cyg AO long exposures we find that P Cyg clearly exhibits a large and diffuse intensity distribution compared to the 59 Cyg's point-like source. A deconvolution of P Cyg using 59 Cyg as the Point Spr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0009198v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0009198v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0009198v1-abstract-full" style="display: none;"> We obtained Halpha diffraction limited data of the LBV star P Cyg using the ONERA Adaptive Optics (AO) facility BOA at the OHP 1.52m telescope on October 1997. Taking P Cyg and the reference star 59 Cyg AO long exposures we find that P Cyg clearly exhibits a large and diffuse intensity distribution compared to the 59 Cyg's point-like source. A deconvolution of P Cyg using 59 Cyg as the Point Spread Function was performed by means of the Richardson-Lucy algorithm. P Cyg clearly appears as an unresolved star surrounded by a clumped envelope. The reconstructed image of P Cyg is compared to similar spatial resolution maps obtained from radio aperture synthesis imaging. We put independent constraints on the physics of P Cyg which agree well with radio results. We discuss future possibilities to constrain the wind structure of P Cyg by using multi-resolution imaging, coronagraphy and long baseline interferometry to trace back its evolutionary status. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0009198v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0009198v1-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 September, 2000; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2000. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 19 Encapsulated Postscript figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astron. & Astrophys. Suppl. Ser., 144, 523-532 (2000) </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

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