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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.05058">arXiv:2405.05058</a> <span> [<a href="https://arxiv.org/pdf/2405.05058">pdf</a>, <a href="https://arxiv.org/format/2405.05058">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Quality assurance of actuators for the Medium-Sized Telescopes of the Cherenkov Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Salzmann%2C+H">Heiko Salzmann</a>, <a href="/search/astro-ph?searchtype=author&query=Dick%2C+J">J眉rgen Dick</a>, <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">Sebastian Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%BChlhofer%2C+G">Gerd P眉hlhofer</a>, <a href="/search/astro-ph?searchtype=author&query=Renner%2C+S">Siegbert Renner</a>, <a href="/search/astro-ph?searchtype=author&query=Santangelo%2C+A">Andrea Santangelo</a>, <a href="/search/astro-ph?searchtype=author&query=Project%2C+C+M">CTA MST Project</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.05058v1-abstract-short" style="display: inline;"> The Cherenkov Telescope Array (CTA) is a future ground-based observatory for gamma-ray astronomy providing unparalleled sensitivity in the energy range from 20 GeV up to 300 TeV. CTA will consist of telescopes with three different sizes. The Medium-Sized Telescopes (MSTs) will have 12 m reflectors with a tessellated mirror design of 86 mirror facets each. Each mirror facet is mounted on the mirror… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.05058v1-abstract-full').style.display = 'inline'; document.getElementById('2405.05058v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.05058v1-abstract-full" style="display: none;"> The Cherenkov Telescope Array (CTA) is a future ground-based observatory for gamma-ray astronomy providing unparalleled sensitivity in the energy range from 20 GeV up to 300 TeV. CTA will consist of telescopes with three different sizes. The Medium-Sized Telescopes (MSTs) will have 12 m reflectors with a tessellated mirror design of 86 mirror facets each. Each mirror facet is mounted on the mirror support structure with two actuators that are adjustable in length to align the mirrors, and a freely rotating fixpoint. Image resolution and pointing accuracy constraints impose limits on the backlash and deformation of the actuators and the fixpoint under various weight and wind loads. In this contribution, the test stand to measure the backlash and deformation behaviour of actuators and fixpoints is described and the measurement procedure is explained. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.05058v1-abstract-full').style.display = 'none'; document.getElementById('2405.05058v1-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 5 figures. Accepted as Proceeding of the 7th Heidelberg International Symposium on High-Energy Gamma-Ray Astronomy (Gamma2022)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> PoS Gamma2022 228 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.04857">arXiv:2403.04857</a> <span> [<a href="https://arxiv.org/pdf/2403.04857">pdf</a>, <a href="https://arxiv.org/format/2403.04857">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2024/07/047">10.1088/1475-7516/2024/07/047 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dark Matter Line Searches with the Cherenkov Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abhir%2C+J">J. Abhir</a>, <a href="/search/astro-ph?searchtype=author&query=Abhishek%2C+A">A. Abhishek</a>, <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre-Santaella%2C+A">A. Aguirre-Santaella</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Crespo%2C+N">N. Alvarez-Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amans%2C+J+-">J. -P. Amans</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Angel%2C+L">L. Angel</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Arnesen%2C+T+T+H">T. T. H. Arnesen</a>, <a href="/search/astro-ph?searchtype=author&query=Arrabito%2C+L">L. Arrabito</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Ascasibar%2C+Y">Y. Ascasibar</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a> , et al. (540 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.04857v2-abstract-short" style="display: inline;"> Monochromatic gamma-ray signals constitute a potential smoking gun signature for annihilating or decaying dark matter particles that could relatively easily be distinguished from astrophysical or instrumental backgrounds. We provide an updated assessment of the sensitivity of the Cherenkov Telescope Array (CTA) to such signals, based on observations of the Galactic centre region as well as of sele… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.04857v2-abstract-full').style.display = 'inline'; document.getElementById('2403.04857v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.04857v2-abstract-full" style="display: none;"> Monochromatic gamma-ray signals constitute a potential smoking gun signature for annihilating or decaying dark matter particles that could relatively easily be distinguished from astrophysical or instrumental backgrounds. We provide an updated assessment of the sensitivity of the Cherenkov Telescope Array (CTA) to such signals, based on observations of the Galactic centre region as well as of selected dwarf spheroidal galaxies. We find that current limits and detection prospects for dark matter masses above 300 GeV will be significantly improved, by up to an order of magnitude in the multi-TeV range. This demonstrates that CTA will set a new standard for gamma-ray astronomy also in this respect, as the world's largest and most sensitive high-energy gamma-ray observatory, in particular due to its exquisite energy resolution at TeV energies and the adopted observational strategy focussing on regions with large dark matter densities. Throughout our analysis, we use up-to-date instrument response functions, and we thoroughly model the effect of instrumental systematic uncertainties in our statistical treatment. We further present results for other potential signatures with sharp spectral features, e.g.~box-shaped spectra, that would likewise very clearly point to a particle dark matter origin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.04857v2-abstract-full').style.display = 'none'; document.getElementById('2403.04857v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">44 pages JCAP style (excluding author list and references), 19 figures; minor changes to match published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 07 (2024) 047 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.17301">arXiv:2401.17301</a> <span> [<a href="https://arxiv.org/pdf/2401.17301">pdf</a>, <a href="https://arxiv.org/format/2401.17301">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Using SRG/eROSITA to estimate soft proton fluxes at the ATHENA detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Perinati%2C+E">E. Perinati</a>, <a href="/search/astro-ph?searchtype=author&query=Freyberg%2C+M">M. Freyberg</a>, <a href="/search/astro-ph?searchtype=author&query=Yeung%2C+M+C+H">M. C. H. Yeung</a>, <a href="/search/astro-ph?searchtype=author&query=Pommranz%2C+C">C. Pommranz</a>, <a href="/search/astro-ph?searchtype=author&query=Hess%2C+B">B. Hess</a>, <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">S. Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=Tenzer%2C+C">C. Tenzer</a>, <a href="/search/astro-ph?searchtype=author&query=Santangelo%2C+A">A. Santangelo</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.17301v1-abstract-short" style="display: inline;"> Context: Environmental soft protons have affected the performance of the X-ray detectors on board Chandra and XMM-Newton, and they pose a threat for future high energy astrophysics missions with larger aperture, such as ATHENA. Aims: We aim at estimating soft proton fluxes at the ATHENA detectors independently of any modelisation of the external fluxes in the space environment.We analysed the ba… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17301v1-abstract-full').style.display = 'inline'; document.getElementById('2401.17301v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.17301v1-abstract-full" style="display: none;"> Context: Environmental soft protons have affected the performance of the X-ray detectors on board Chandra and XMM-Newton, and they pose a threat for future high energy astrophysics missions with larger aperture, such as ATHENA. Aims: We aim at estimating soft proton fluxes at the ATHENA detectors independently of any modelisation of the external fluxes in the space environment.We analysed the background data measured by eROSITA on board SRG, and with the help of simulations we defined a range of values for the potential count-rate of quiet-time soft protons focused through the mirror shells. We used it to derive an estimate of soft proton fluxes at the ATHENA detectors, assuming ATHENA in the same L2-orbit as SRG. Results: The scaling, based on the computed proton transmission yields of the optics and optical/thermal filters of eROSITA and ATHENA, indicates that the soft proton induced WFI and X-IFU backgrounds could be expected close to the requirement. Conclusions: No soft proton fluxes detrimental to the observations have been suffered by eROSITA during its all-sky survey in orbit around L2. Regardless of where ATHENA will be placed (L1 or L2), our analysis suggests that increasing somewhat the thickness of the WFI optical blocking filter, e.g. by 30%, would help to reduce the soft proton flux onto the detector, in case the planned magnetic diverters perform worse than expected due to soft proton neutralisation at the mirror level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17301v1-abstract-full').style.display = 'none'; document.getElementById('2401.17301v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.07413">arXiv:2310.07413</a> <span> [<a href="https://arxiv.org/pdf/2310.07413">pdf</a>, <a href="https://arxiv.org/format/2310.07413">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Chasing Gravitational Waves with the Cherenkov Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Green%2C+J+G">Jarred Gershon Green</a>, <a href="/search/astro-ph?searchtype=author&query=Carosi%2C+A">Alessandro Carosi</a>, <a href="/search/astro-ph?searchtype=author&query=Nava%2C+L">Lara Nava</a>, <a href="/search/astro-ph?searchtype=author&query=Patricelli%2C+B">Barbara Patricelli</a>, <a href="/search/astro-ph?searchtype=author&query=Sch%C3%BCssler%2C+F">Fabian Sch眉ssler</a>, <a href="/search/astro-ph?searchtype=author&query=Seglar-Arroyo%2C+M">Monica Seglar-Arroyo</a>, <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+C">Cta Consortium</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+K">Kazuki Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+S">Shotaro Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">Atreya Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">Remi Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Aguasca-Cabot%2C+A">Arnau Aguasca-Cabot</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">Ivan Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">Jorge Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Crespo%2C+N">Nuria Alvarez-Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">Rafael Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amans%2C+J">Jean-Philippe Amans</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">Elena Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosino%2C+F">Filippo Ambrosino</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">Ekrem Oguzhan Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">Lucio Angelo Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">Carla Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">Cornelia Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Arrabito%2C+L">Luisa Arrabito</a> , et al. (545 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.07413v3-abstract-short" style="display: inline;"> The detection of gravitational waves from a binary neutron star merger by Advanced LIGO and Advanced Virgo (GW170817), along with the discovery of the electromagnetic counterparts of this gravitational wave event, ushered in a new era of multimessenger astronomy, providing the first direct evidence that BNS mergers are progenitors of short gamma-ray bursts (GRBs). Such events may also produce very… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.07413v3-abstract-full').style.display = 'inline'; document.getElementById('2310.07413v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.07413v3-abstract-full" style="display: none;"> The detection of gravitational waves from a binary neutron star merger by Advanced LIGO and Advanced Virgo (GW170817), along with the discovery of the electromagnetic counterparts of this gravitational wave event, ushered in a new era of multimessenger astronomy, providing the first direct evidence that BNS mergers are progenitors of short gamma-ray bursts (GRBs). Such events may also produce very-high-energy (VHE, > 100GeV) photons which have yet to be detected in coincidence with a gravitational wave signal. The Cherenkov Telescope Array (CTA) is a next-generation VHE observatory which aims to be indispensable in this search, with an unparalleled sensitivity and ability to slew anywhere on the sky within a few tens of seconds. New observing modes and follow-up strategies are being developed for CTA to rapidly cover localization areas of gravitational wave events that are typically larger than the CTA field of view. This work will evaluate and provide estimations on the expected number of of gravitational wave events that will be observable with CTA, considering both on- and off-axis emission. In addition, we will present and discuss the prospects of potential follow-up strategies with CTA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.07413v3-abstract-full').style.display = 'none'; document.getElementById('2310.07413v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Presented at the 38th International Cosmic Ray Conference (ICRC 2023), 2023 (arXiv:2309.08219)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> CTA-ICRC/2023/30 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.03712">arXiv:2309.03712</a> <span> [<a href="https://arxiv.org/pdf/2309.03712">pdf</a>, <a href="https://arxiv.org/format/2309.03712">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2024/10/004">10.1088/1475-7516/2024/10/004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Prospects for $纬$-ray observations of the Perseus galaxy cluster with the Cherenkov Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+T+C+T+A">The Cherenkov Telescope Array Consortium</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre-Santaella%2C+A">A. Aguirre-Santaella</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Crespo%2C+N">N. Alvarez-Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amans%2C+J+-">J. -P. Amans</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Araya%2C+M">M. Araya</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Arrabito%2C+L">L. Arrabito</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Ascas%C3%ADbar%2C+Y">Y. Ascas铆bar</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a> , et al. (542 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.03712v1-abstract-short" style="display: inline;"> Galaxy clusters are expected to be dark matter (DM) reservoirs and storage rooms for the cosmic-ray protons (CRp) that accumulate along the cluster's formation history. Accordingly, they are excellent targets to search for signals of DM annihilation and decay at gamma-ray energies and are predicted to be sources of large-scale gamma-ray emission due to hadronic interactions in the intracluster med… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03712v1-abstract-full').style.display = 'inline'; document.getElementById('2309.03712v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.03712v1-abstract-full" style="display: none;"> Galaxy clusters are expected to be dark matter (DM) reservoirs and storage rooms for the cosmic-ray protons (CRp) that accumulate along the cluster's formation history. Accordingly, they are excellent targets to search for signals of DM annihilation and decay at gamma-ray energies and are predicted to be sources of large-scale gamma-ray emission due to hadronic interactions in the intracluster medium. We estimate the sensitivity of the Cherenkov Telescope Array (CTA) to detect diffuse gamma-ray emission from the Perseus galaxy cluster. We perform a detailed spatial and spectral modelling of the expected signal for the DM and the CRp components. For each, we compute the expected CTA sensitivity. The observing strategy of Perseus is also discussed. In the absence of a diffuse signal (non-detection), CTA should constrain the CRp to thermal energy ratio within the radius $R_{500}$ down to about $X_{500}<3\times 10^{-3}$, for a spatial CRp distribution that follows the thermal gas and a CRp spectral index $伪_{\rm CRp}=2.3$. Under the optimistic assumption of a pure hadronic origin of the Perseus radio mini-halo and depending on the assumed magnetic field profile, CTA should measure $伪_{\rm CRp}$ down to about $螖伪_{\rm CRp}\simeq 0.1$ and the CRp spatial distribution with 10% precision. Regarding DM, CTA should improve the current ground-based gamma-ray DM limits from clusters observations on the velocity-averaged annihilation cross-section by a factor of up to $\sim 5$, depending on the modelling of DM halo substructure. In the case of decay of DM particles, CTA will explore a new region of the parameter space, reaching models with $蟿_蠂>10^{27}$s for DM masses above 1 TeV. These constraints will provide unprecedented sensitivity to the physics of both CRp acceleration and transport at cluster scale and to TeV DM particle models, especially in the decay scenario. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03712v1-abstract-full').style.display = 'none'; document.getElementById('2309.03712v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">93 pages (including author list, appendix and references), 143 figures. Submitted to JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP10(2024)004 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.15007">arXiv:2303.15007</a> <span> [<a href="https://arxiv.org/pdf/2303.15007">pdf</a>, <a href="https://arxiv.org/format/2303.15007">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.astropartphys.2023.102850">10.1016/j.astropartphys.2023.102850 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sensitivity of the Cherenkov Telescope Array to spectral signatures of hadronic PeVatrons with application to Galactic Supernova Remnants </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+T+C+T+A">The Cherenkov Telescope Array Consortium</a>, <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre-Santaella%2C+A">A. Aguirre-Santaella</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Crespo%2C+N+%C3%81">N. 脕lvarez Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amati%2C+L">L. Amati</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Ascasibar%2C+Y">Y. Ascasibar</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baktash%2C+A">A. Baktash</a>, <a href="/search/astro-ph?searchtype=author&query=Balazs%2C+C">C. Balazs</a>, <a href="/search/astro-ph?searchtype=author&query=Balbo%2C+M">M. Balbo</a> , et al. (334 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="2303.15007v1-abstract-short" style="display: inline;"> The local Cosmic Ray (CR) energy spectrum exhibits a spectral softening at energies around 3~PeV. Sources which are capable of accelerating hadrons to such energies are called hadronic PeVatrons. However, hadronic PeVatrons have not yet been firmly identified within the Galaxy. Several source classes, including Galactic Supernova Remnants (SNRs), have been proposed as PeVatron candidates. The pote… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15007v1-abstract-full').style.display = 'inline'; document.getElementById('2303.15007v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.15007v1-abstract-full" style="display: none;"> The local Cosmic Ray (CR) energy spectrum exhibits a spectral softening at energies around 3~PeV. Sources which are capable of accelerating hadrons to such energies are called hadronic PeVatrons. However, hadronic PeVatrons have not yet been firmly identified within the Galaxy. Several source classes, including Galactic Supernova Remnants (SNRs), have been proposed as PeVatron candidates. The potential to search for hadronic PeVatrons with the Cherenkov Telescope Array (CTA) is assessed. The focus is on the usage of very high energy $纬$-ray spectral signatures for the identification of PeVatrons. Assuming that SNRs can accelerate CRs up to knee energies, the number of Galactic SNRs which can be identified as PeVatrons with CTA is estimated within a model for the evolution of SNRs. Additionally, the potential of a follow-up observation strategy under moonlight conditions for PeVatron searches is investigated. Statistical methods for the identification of PeVatrons are introduced, and realistic Monte--Carlo simulations of the response of the CTA observatory to the emission spectra from hadronic PeVatrons are performed. Based on simulations of a simplified model for the evolution for SNRs, the detection of a $纬$-ray signal from in average 9 Galactic PeVatron SNRs is expected to result from the scan of the Galactic plane with CTA after 10 hours of exposure. CTA is also shown to have excellent potential to confirm these sources as PeVatrons in deep observations with $\mathcal{O}(100)$ hours of exposure per source. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15007v1-abstract-full').style.display = 'none'; document.getElementById('2303.15007v1-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 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">34 pages, 16 figures, Accepted for publication in Astroparticle Physics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.10883">arXiv:2210.10883</a> <span> [<a href="https://arxiv.org/pdf/2210.10883">pdf</a>, <a href="https://arxiv.org/format/2210.10883">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/10.1007/978-981-16-4544-0_16-1">10.1007/978-981-16-4544-0_16-1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Proportional counters and microchannel plates </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">Sebastian Diebold</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.10883v2-abstract-short" style="display: inline;"> Developed right at the beginning of the space age in the 1940s, the proportional counter was the first detector used in X-ray astronomy and stayed its workhorse for almost four decades. Although the principle of such a detector seems to be rather simple, over time it underwent considerable performance improvements and the lifetime under orbital conditions was extended tremendously. Particularly th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.10883v2-abstract-full').style.display = 'inline'; document.getElementById('2210.10883v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.10883v2-abstract-full" style="display: none;"> Developed right at the beginning of the space age in the 1940s, the proportional counter was the first detector used in X-ray astronomy and stayed its workhorse for almost four decades. Although the principle of such a detector seems to be rather simple, over time it underwent considerable performance improvements and the lifetime under orbital conditions was extended tremendously. Particularly the invention of position-sensitive proportional counters provided new and sophisticated methods to discriminate background and thus enabled observations of much weaker sources. A leap forward in position resolution was achieved with the advent of microchannel plate (MCP) detectors in the 1970s. In contrary to gas filled detectors, they provide no considerable energy resolution but feature spatial resolutions reaching down to a few tens of micrometers, fitting ideally the angular resolution of the novel grazing incidence imaging X-ray telescopes upcoming at that time. Even today, both types of detectors are still relevant in space-based astronomy. However, in case of MCPs new developments focus on the far and extreme ultraviolet wavelength range, while the Chandra X-ray observatory is most likely the last mission applying this technology for X-rays. In contrast, compact detectors with gas electron multiplier (GEM) foils and micropattern readout are currently under heavy development for the soft X-ray range, since they allow for the first time to measure polarization in X-rays over a broad energy range. This chapter presents the principles of proportional counters and MCP detectors, highlights the respective performance characteristics, and summarizes their most important applications in X-ray astronomy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.10883v2-abstract-full').style.display = 'none'; document.getElementById('2210.10883v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">36 pages, 11 figures, invited chapter for "Handbook of X-ray and Gamma-ray Astrophysics" (Eds. C. Bambi and A. Santangelo, Springer Singapore, expected in 2023)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.08103">arXiv:2201.08103</a> <span> [<a href="https://arxiv.org/pdf/2201.08103">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/1.JATIS.8.1.014005">10.1117/1.JATIS.8.1.014005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Mirror production for the Cherenkov telescopes of the ASTRI Mini-Array and of the MST project for the Cherenkov Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=La+Palombara%2C+N">N. La Palombara</a>, <a href="/search/astro-ph?searchtype=author&query=Sironi%2C+G">G. Sironi</a>, <a href="/search/astro-ph?searchtype=author&query=Giro%2C+E">E. Giro</a>, <a href="/search/astro-ph?searchtype=author&query=Scuderi%2C+S">S. Scuderi</a>, <a href="/search/astro-ph?searchtype=author&query=Canestrari%2C+R">R. Canestrari</a>, <a href="/search/astro-ph?searchtype=author&query=Iovenitti%2C+S">S. Iovenitti</a>, <a href="/search/astro-ph?searchtype=author&query=Garczarczyk%2C+M">M. Garczarczyk</a>, <a href="/search/astro-ph?searchtype=author&query=Krause%2C+M">M. Krause</a>, <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">S. Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=Millul%2C+R">R. Millul</a>, <a href="/search/astro-ph?searchtype=author&query=Marioni%2C+F">F. Marioni</a>, <a href="/search/astro-ph?searchtype=author&query=Missaglia%2C+N">N. Missaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Redaelli%2C+M">M. Redaelli</a>, <a href="/search/astro-ph?searchtype=author&query=Valsecchi%2C+G">G. Valsecchi</a>, <a href="/search/astro-ph?searchtype=author&query=Zocchi%2C+F">F. Zocchi</a>, <a href="/search/astro-ph?searchtype=author&query=Zanoni%2C+A">A. Zanoni</a>, <a href="/search/astro-ph?searchtype=author&query=Pareschi%2C+G">G. Pareschi</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="2201.08103v2-abstract-short" style="display: inline;"> The Cherenkov Telescope Array (CTA) is the next ground-based $纬$-ray observatory in the TeV $纬$-ray spectral region operating with the Imaging Atmospheric Cherenkov Technique. It is based on almost 70 telescopes of different class diameters - LST, MST and SST of 23, 12, and 4 m, respectively - to be installed in two sites in the two hemispheres (at La Palma, Canary Islands, and near Paranal, Chile… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.08103v2-abstract-full').style.display = 'inline'; document.getElementById('2201.08103v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.08103v2-abstract-full" style="display: none;"> The Cherenkov Telescope Array (CTA) is the next ground-based $纬$-ray observatory in the TeV $纬$-ray spectral region operating with the Imaging Atmospheric Cherenkov Technique. It is based on almost 70 telescopes of different class diameters - LST, MST and SST of 23, 12, and 4 m, respectively - to be installed in two sites in the two hemispheres (at La Palma, Canary Islands, and near Paranal, Chile). Several thousands of reflecting mirror tiles larger than 1 m$^2$ will be produced for realizing the segmented primary mirrors of a so large number of telescopes. Almost in parallel, the ASTRI Mini-Array (MA) is being implemented in Tenerife (Canary Islands), composed of nine 4 m diameter dual-mirror Cherenkov telescopes (very similar to the SSTs). We completed the mirror production for all nine telescopes of the ASTRI MA and two MST telescopes (400 segments in total) using the cold glass slumping replication technology. The results related to the quality achieved with a so large-scale production are presented, also discussing the adopted testing methods and approaches. They will be very useful for the adoption and optimization of the quality assurance process for the huge production (almost 3000 m$^2$ of reflecting surface) of the MST and SST CTA telescopes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.08103v2-abstract-full').style.display = 'none'; document.getElementById('2201.08103v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the SPIE Journal of Astronomical Telescopes, Instruments, and Systems (JATIS); 29 pages, 17 figures, 4 tables, quite a lot of stress, infinite patience. Published online on February 3, 2022 at http://dx.doi.org/10.1117/1.JATIS.8.1.014005</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.04122">arXiv:2110.04122</a> <span> [<a href="https://arxiv.org/pdf/2110.04122">pdf</a>, <a href="https://arxiv.org/format/2110.04122">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s10686-021-09806-9">10.1007/s10686-021-09806-9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Scattering efficiencies measurements of soft protons at grazing incidence from an Athena Silicon Pore Optics sample </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Amato%2C+R">R. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">S. Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=Guzman%2C+A">A. Guzman</a>, <a href="/search/astro-ph?searchtype=author&query=Perinati%2C+E">E. Perinati</a>, <a href="/search/astro-ph?searchtype=author&query=Tenzer%2C+C">C. Tenzer</a>, <a href="/search/astro-ph?searchtype=author&query=Santangelo%2C+A">A. Santangelo</a>, <a href="/search/astro-ph?searchtype=author&query=Mineo%2C+T">T. Mineo</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="2110.04122v1-abstract-short" style="display: inline;"> Soft protons are a potential threat for X-ray missions using grazing incidence optics, as once focused onto the detectors they can contribute to increase the background and possibly induce radiation damage as well. The assessment of these undesired effects is especially relevant for the future ESA X-ray mission Athena, due to its large collecting area. To prevent degradation of the instrumental pe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.04122v1-abstract-full').style.display = 'inline'; document.getElementById('2110.04122v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.04122v1-abstract-full" style="display: none;"> Soft protons are a potential threat for X-ray missions using grazing incidence optics, as once focused onto the detectors they can contribute to increase the background and possibly induce radiation damage as well. The assessment of these undesired effects is especially relevant for the future ESA X-ray mission Athena, due to its large collecting area. To prevent degradation of the instrumental performance, which ultimately could compromise some of the scientific goals of the mission, the adoption of ad-hoc magnetic diverters is envisaged. Dedicated laboratory measurements are fundamental to understand the mechanisms of proton forward scattering, validate the application of the existing physical models to the Athena case and support the design of the diverters. In this paper we report on scattering efficiency measurements of soft protons impinging at grazing incidence onto a Silicon Pore Optics sample, conducted in the framework of the EXACRAD project. Measurements were taken at two different energies, ~470 keV and ~170 keV, and at four different scattering angles between 0.6 deg and 1.2 deg. The results are generally consistent with previous measurements conducted on eROSITA mirror samples, and as expected the peak of the scattering efficiency is found around the angle of specular reflection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.04122v1-abstract-full').style.display = 'none'; document.getElementById('2110.04122v1-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 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 11 figures; accepted for publication on Experimental Astronomy</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.03046">arXiv:2108.03046</a> <span> [<a href="https://arxiv.org/pdf/2108.03046">pdf</a>, <a href="https://arxiv.org/format/2108.03046">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/10.22323/1.395.0743">10.22323/1.395.0743 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Performance of the New FlashCam-based Camera in the 28\,m Telescope of H.E.S.S </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bi%2C+B">Baiyang Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Barcelo%2C+M">Miquel Barcelo</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+C">Christian Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Benkhali%2C+F+A">Faical Ait Benkhali</a>, <a href="/search/astro-ph?searchtype=author&query=Catalano%2C+J">Jacqueline Catalano</a>, <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">Sebastian Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=F%C3%B6hr%2C+C">Christian F枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Funk%2C+S">Stefan Funk</a>, <a href="/search/astro-ph?searchtype=author&query=Giavitto%2C+G">Gianluca Giavitto</a>, <a href="/search/astro-ph?searchtype=author&query=Hermann%2C+G">German Hermann</a>, <a href="/search/astro-ph?searchtype=author&query=Hinton%2C+J">Jim Hinton</a>, <a href="/search/astro-ph?searchtype=author&query=Jung-Richardt%2C+I">Ira Jung-Richardt</a>, <a href="/search/astro-ph?searchtype=author&query=Kalekin%2C+O">Oleg Kalekin</a>, <a href="/search/astro-ph?searchtype=author&query=Kankanyan%2C+R">Ruben Kankanyan</a>, <a href="/search/astro-ph?searchtype=author&query=Kihm%2C+T">Thomas Kihm</a>, <a href="/search/astro-ph?searchtype=author&query=Leuschner%2C+F">Fabian Leuschner</a>, <a href="/search/astro-ph?searchtype=author&query=Pfeifer%2C+M">Marc Pfeifer</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%BChlhofer%2C+G">Gerd P眉hlhofer</a>, <a href="/search/astro-ph?searchtype=author&query=Reimer%2C+O">Olaf Reimer</a>, <a href="/search/astro-ph?searchtype=author&query=Sailer%2C+S">Simon Sailer</a>, <a href="/search/astro-ph?searchtype=author&query=Salzmann%2C+H">Heiko Salzmann</a>, <a href="/search/astro-ph?searchtype=author&query=Santangelo%2C+A">Andrea Santangelo</a>, <a href="/search/astro-ph?searchtype=author&query=Steinmassl%2C+S">Simon Steinmassl</a>, <a href="/search/astro-ph?searchtype=author&query=Schanz%2C+T">Thomas Schanz</a>, <a href="/search/astro-ph?searchtype=author&query=Tenzer%2C+C">Chris Tenzer</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2108.03046v1-abstract-short" style="display: inline;"> In October 2019, the central 28 m telescope of the H.E.S.S. experiment has been upgraded with a new camera. The camera is based on the FlashCam design which has been developed in view of a possible future implementation in the Medium-Sized Telescopes of the Cherenkov Telescope Array (CTA), with emphasis on cost and performance optimization and on reliability. The fully digital design of the trigge… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.03046v1-abstract-full').style.display = 'inline'; document.getElementById('2108.03046v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.03046v1-abstract-full" style="display: none;"> In October 2019, the central 28 m telescope of the H.E.S.S. experiment has been upgraded with a new camera. The camera is based on the FlashCam design which has been developed in view of a possible future implementation in the Medium-Sized Telescopes of the Cherenkov Telescope Array (CTA), with emphasis on cost and performance optimization and on reliability. The fully digital design of the trigger and readout system makes it possible to operate the camera at high event rates and to precisely adjust and understand the trigger system. The novel design of the front-end electronics achieves a dynamic range of over 3,000 photoelectrons with only one electronics readout circuit per pixel. Here we report on the performance parameters of the camera obtained during the first year of operation in the field, including operational stability and optimization of calibration algorithms. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.03046v1-abstract-full').style.display = 'none'; document.getElementById('2108.03046v1-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 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">Proceedings of the 37th International Cosmic Ray Conference (ICRC 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/2012.14215">arXiv:2012.14215</a> <span> [<a href="https://arxiv.org/pdf/2012.14215">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Status of the STUDIO UV balloon mission and platform </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pahler%2C+A">A. Pahler</a>, <a href="/search/astro-ph?searchtype=author&query=%C3%85ngermann%2C+M">M. 脜ngermann</a>, <a href="/search/astro-ph?searchtype=author&query=Barnstedt%2C+J">J. Barnstedt</a>, <a href="/search/astro-ph?searchtype=author&query=Bougueroua%2C+S">S. Bougueroua</a>, <a href="/search/astro-ph?searchtype=author&query=Colin%2C+A">A. Colin</a>, <a href="/search/astro-ph?searchtype=author&query=Conti%2C+L">L. Conti</a>, <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">S. Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=Duffard%2C+R">R. Duffard</a>, <a href="/search/astro-ph?searchtype=author&query=Emberger%2C+M">M. Emberger</a>, <a href="/search/astro-ph?searchtype=author&query=Hanke%2C+L">L. Hanke</a>, <a href="/search/astro-ph?searchtype=author&query=Kalkuhl%2C+C">C. Kalkuhl</a>, <a href="/search/astro-ph?searchtype=author&query=Kappelmann%2C+N">N. Kappelmann</a>, <a href="/search/astro-ph?searchtype=author&query=Keilig%2C+T">T. Keilig</a>, <a href="/search/astro-ph?searchtype=author&query=Klinkner%2C+S">S. Klinkner</a>, <a href="/search/astro-ph?searchtype=author&query=Krabbe%2C+A">A. Krabbe</a>, <a href="/search/astro-ph?searchtype=author&query=Janson%2C+O">O. Janson</a>, <a href="/search/astro-ph?searchtype=author&query=Lengowski%2C+M">M. Lengowski</a>, <a href="/search/astro-ph?searchtype=author&query=Lockowandt%2C+C">C. Lockowandt</a>, <a href="/search/astro-ph?searchtype=author&query=Maier%2C+P">P. Maier</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%BCller%2C+T">T. M眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Rauch%2C+T">T. Rauch</a>, <a href="/search/astro-ph?searchtype=author&query=Schanz%2C+T">T. Schanz</a>, <a href="/search/astro-ph?searchtype=author&query=Stelzer%2C+B">B. Stelzer</a>, <a href="/search/astro-ph?searchtype=author&query=Taheran%2C+M">M. Taheran</a>, <a href="/search/astro-ph?searchtype=author&query=Vaerneus%2C+A">A. Vaerneus</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.14215v1-abstract-short" style="display: inline;"> Stratospheric balloons offer accessible and affordable platforms for observations in atmosphere-constrained wavelength ranges. At the same time, they can serve as an effective step for technology demonstration towards future space applications of instruments and other hardware. The Stratospheric UV Demonstrator of an Imaging Observatory (STUDIO) is a balloon-borne platform and mission carrying an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.14215v1-abstract-full').style.display = 'inline'; document.getElementById('2012.14215v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.14215v1-abstract-full" style="display: none;"> Stratospheric balloons offer accessible and affordable platforms for observations in atmosphere-constrained wavelength ranges. At the same time, they can serve as an effective step for technology demonstration towards future space applications of instruments and other hardware. The Stratospheric UV Demonstrator of an Imaging Observatory (STUDIO) is a balloon-borne platform and mission carrying an imaging micro-channel plate (MCP) detector on a 0.5 m aperture telescope. STUDIO is currently planned to fly during the summer turnaround conditions over Esrange, Sweden, in the 2022 season. For details on the ultraviolet (UV) detector, see the contribution of Conti et al. to this symposium. The scientific goal of the mission is to survey for variable hot compact stars and flaring M-dwarf stars within the galactic plane. At the same time, the mission acts as a demonstrator for a versatile and scalable astronomical balloon platform as well as for the aforementioned MCP instrument. The gondola is designed to allow the use of different instruments or telescopes. Furthermore, it is designed to serve for several, also longer, flights, which are envisioned under the European Stratospheric Balloon Observatory (ESBO) initiative. In this paper, we present the design and current status of manufacturing and testing of the STUDIO platform. We furthermore present the current plans for the flight and observations from Esrange. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.14215v1-abstract-full').style.display = 'none'; document.getElementById('2012.14215v1-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 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Proc. SPIE Conf., Astronomical Telescopes and Instrumentation, 14-18 December 2020</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.12548">arXiv:2012.12548</a> <span> [<a href="https://arxiv.org/pdf/2012.12548">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Microchannel-Plate Detector Development for Ultraviolet Missions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Conti%2C+L">Lauro Conti</a>, <a href="/search/astro-ph?searchtype=author&query=Barnstedt%2C+J">J眉rgen Barnstedt</a>, <a href="/search/astro-ph?searchtype=author&query=Buntrock%2C+S">Sebastian Buntrock</a>, <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">Sebastian Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=Hanke%2C+L">Lars Hanke</a>, <a href="/search/astro-ph?searchtype=author&query=Kalkuhl%2C+C">Christoph Kalkuhl</a>, <a href="/search/astro-ph?searchtype=author&query=Kappelmann%2C+N">Norbert Kappelmann</a>, <a href="/search/astro-ph?searchtype=author&query=Kaufmann%2C+T">Thomas Kaufmann</a>, <a href="/search/astro-ph?searchtype=author&query=Rauch%2C+T">Thomas Rauch</a>, <a href="/search/astro-ph?searchtype=author&query=Stelzer%2C+B">Beate Stelzer</a>, <a href="/search/astro-ph?searchtype=author&query=Schanz%2C+T">Thomas Schanz</a>, <a href="/search/astro-ph?searchtype=author&query=Werner%2C+K">Klaus Werner</a>, <a href="/search/astro-ph?searchtype=author&query=Elsener%2C+H">Hans-Rudolf Elsener</a>, <a href="/search/astro-ph?searchtype=author&query=Bougueroua%2C+S">Sarah Bougueroua</a>, <a href="/search/astro-ph?searchtype=author&query=Keilig%2C+T">Thomas Keilig</a>, <a href="/search/astro-ph?searchtype=author&query=Krabbe%2C+A">Alfred Krabbe</a>, <a href="/search/astro-ph?searchtype=author&query=Maier%2C+P">Philipp Maier</a>, <a href="/search/astro-ph?searchtype=author&query=Pahler%2C+A">Andreas Pahler</a>, <a href="/search/astro-ph?searchtype=author&query=Taheran%2C+M">Mahsa Taheran</a>, <a href="/search/astro-ph?searchtype=author&query=Wolf%2C+J">J眉rgen Wolf</a>, <a href="/search/astro-ph?searchtype=author&query=Meyer%2C+K">Kevin Meyer</a>, <a href="/search/astro-ph?searchtype=author&query=Schaadt%2C+D+M">Daniel M. Schaadt</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.12548v1-abstract-short" style="display: inline;"> The Institute for Astronomy and Astrophysics in T眉bingen (IAAT) has a long-term experience in developing and building space-qualified imaging and photon counting microchannel-plate (MCP) detectors, which are sensitive in the ultraviolet wavelength range. Our goal is to achieve high quantum efficiency and spatial resolution, while maintaining solar blindness and low-noise characteristics. Our flexi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.12548v1-abstract-full').style.display = 'inline'; document.getElementById('2012.12548v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.12548v1-abstract-full" style="display: none;"> The Institute for Astronomy and Astrophysics in T眉bingen (IAAT) has a long-term experience in developing and building space-qualified imaging and photon counting microchannel-plate (MCP) detectors, which are sensitive in the ultraviolet wavelength range. Our goal is to achieve high quantum efficiency and spatial resolution, while maintaining solar blindness and low-noise characteristics. Our flexible detector design is currently tailored to the specific needs of three missions: For the ESBO DS (European Stratospheric Balloon Observatory Design Study) we provide a sealed detector to the STUDIO instrument (Stratospheric Ultraviolet Demonstrator of an Imaging Observatory), a 50 cm telescope with a UV imager for operation at an altitude of 37-41 km. In collaboration with the Indian Institute of Astrophysics we plan a space mission with a CubeSat-sized far-ultraviolet spectroscopic imaging instrument, featuring an open version of our detector. A Chinese mission, led by the Purple Mountain Observatory, comprises a multi-channel imager using open and sealed detector versions. Our MCP detector has a cesium activated p-doped gallium-nitride photocathode. Other photocathode materials like cesium-telluride or potassium-bromide could be used as an alternative. For the sealed version, the photocathode is operated in semi-transparent mode on a MgF$_2$ window with a cut-off wavelength of about 118 nm. For missions requiring sensitivity below this cut-off, we are planning an open version. We employ a coplanar cross-strip anode and advanced low-power readout electronics with a 128-channel charge-amplifier chip. This publication focuses on the progress concerning the main development challenges: the optimization of the photocathode parameters and the sophisticated detector electronics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.12548v1-abstract-full').style.display = 'none'; document.getElementById('2012.12548v1-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 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Proc. SPIE Conf., Astronomical Telescopes and Instrumentation, 14-18 December 2020</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.07384">arXiv:2012.07384</a> <span> [<a href="https://arxiv.org/pdf/2012.07384">pdf</a>, <a href="https://arxiv.org/format/2012.07384">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Mapping Diffuse Emission in Lyman UV band </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ji%2C+L">Li Ji</a>, <a href="/search/astro-ph?searchtype=author&query=Lou%2C+Z">Zheng Lou</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+J">Jinlong Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Qiu%2C+K">Keqiang Qiu</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+S">Shuangying Li</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+W">Wei Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Yan%2C+S">Shuping Yan</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+S">Shuinai Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Qian%2C+Y">Yuan Qian</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+S">Sen Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Werner%2C+K">Klaus Werner</a>, <a href="/search/astro-ph?searchtype=author&query=Fang%2C+T">Taotao Fang</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+T">Tinggui Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Barnstedt%2C+J">J眉rgen Barnstedt</a>, <a href="/search/astro-ph?searchtype=author&query=Buntrock%2C+S">Sebastian Buntrock</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+M">Mingsheng Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W">Wen Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Conti%2C+L">Lauro Conti</a>, <a href="/search/astro-ph?searchtype=author&query=Deng%2C+L">Lei Deng</a>, <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">Sebastian Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=Fu%2C+S">Shaojun Fu</a>, <a href="/search/astro-ph?searchtype=author&query=Guo%2C+J">Jianhua Guo</a>, <a href="/search/astro-ph?searchtype=author&query=Hanke%2C+L">Lars Hanke</a>, <a href="/search/astro-ph?searchtype=author&query=Hong%2C+Y">Yilin Hong</a>, <a href="/search/astro-ph?searchtype=author&query=Kalkuhl%2C+C">Christoph Kalkuhl</a> , et al. (16 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.07384v2-abstract-short" style="display: inline;"> The CAFE (Census of warm-hot intergalactic medium, Accretion, and Feedback Explorer) and LyRIC (Lyman UV Radiation from Interstellar medium and Circum-galactic medium) have been proposed to the space agencies in China respectively. CAFE was first proposed in 2015 as a joint scientific CAS-ESA small space mission. LyRIC was proposed in 2019 as an independent external payload operating on the Chines… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.07384v2-abstract-full').style.display = 'inline'; document.getElementById('2012.07384v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.07384v2-abstract-full" style="display: none;"> The CAFE (Census of warm-hot intergalactic medium, Accretion, and Feedback Explorer) and LyRIC (Lyman UV Radiation from Interstellar medium and Circum-galactic medium) have been proposed to the space agencies in China respectively. CAFE was first proposed in 2015 as a joint scientific CAS-ESA small space mission. LyRIC was proposed in 2019 as an independent external payload operating on the Chinese Space Station. Both missions are dedicated to mapping the Lyman UV emission (ionized oxygen (O VI) resonance lines at 103.2 and 103.8 nm, and Lyman series) for the diffuse sources in our Galaxy and the circum-galactic mediums of the nearby galaxies. We present the primary science objectives, mission concepts, the enabling technologies, as well as the current status. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.07384v2-abstract-full').style.display = 'none'; document.getElementById('2012.07384v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 6 figures, SPIE Astronomical Telescopes + Instrumentation 2020 conference Paper No. 11444-4</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.01349">arXiv:2010.01349</a> <span> [<a href="https://arxiv.org/pdf/2010.01349">pdf</a>, <a href="https://arxiv.org/format/2010.01349">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2021/02/048">10.1088/1475-7516/2021/02/048 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sensitivity of the Cherenkov Telescope Array for probing cosmology and fundamental physics with gamma-ray propagation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+T+C+T+A">The Cherenkov Telescope Array Consortium</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+H">H. Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre-Santaella%2C+A">A. Aguirre-Santaella</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alispach%2C+C">C. Alispach</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=B%2C+R+A">R. Alves B</a>, <a href="/search/astro-ph?searchtype=author&query=Amati%2C+L">L. Amati</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Araudo%2C+A">A. Araudo</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arrabito%2C+L">L. Arrabito</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Ascas%C3%ADbar%2C+Y">Y. Ascas铆bar</a>, <a href="/search/astro-ph?searchtype=author&query=Ashley%2C+M">M. Ashley</a> , et al. (474 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="2010.01349v2-abstract-short" style="display: inline;"> The Cherenkov Telescope Array (CTA), the new-generation ground-based observatory for $纬$-ray astronomy, provides unique capabilities to address significant open questions in astrophysics, cosmology, and fundamental physics. We study some of the salient areas of $纬$-ray cosmology that can be explored as part of the Key Science Projects of CTA, through simulated observations of active galactic nucle… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.01349v2-abstract-full').style.display = 'inline'; document.getElementById('2010.01349v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.01349v2-abstract-full" style="display: none;"> The Cherenkov Telescope Array (CTA), the new-generation ground-based observatory for $纬$-ray astronomy, provides unique capabilities to address significant open questions in astrophysics, cosmology, and fundamental physics. We study some of the salient areas of $纬$-ray cosmology that can be explored as part of the Key Science Projects of CTA, through simulated observations of active galactic nuclei (AGN) and of their relativistic jets. Observations of AGN with CTA will enable a measurement of $纬$-ray absorption on the extragalactic background light with a statistical uncertainty below 15% up to a redshift $z=2$ and to constrain or detect $纬$-ray halos up to intergalactic-magnetic-field strengths of at least 0.3pG. Extragalactic observations with CTA also show promising potential to probe physics beyond the Standard Model. The best limits on Lorentz invariance violation from $纬$-ray astronomy will be improved by a factor of at least two to three. CTA will also probe the parameter space in which axion-like particles could constitute a significant fraction, if not all, of dark matter. We conclude on the synergies between CTA and other upcoming facilities that will foster the growth of $纬$-ray cosmology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.01349v2-abstract-full').style.display = 'none'; document.getElementById('2010.01349v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">71 pages (including affiliations and references), 13 figures, 6 tables. Accepted in JCAP; matches published version. Corresponding authors: Jonathan Biteau, Julien Lefaucheur, Humberto Martinez-Huerta, Manuel Meyer, Santiago Pita, Ievgen Vovk</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 02 (2021) 048 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.16129">arXiv:2007.16129</a> <span> [<a href="https://arxiv.org/pdf/2007.16129">pdf</a>, <a href="https://arxiv.org/format/2007.16129">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2021/01/057">10.1088/1475-7516/2021/01/057 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sensitivity of the Cherenkov Telescope Array to a dark matter signal from the Galactic centre </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+T+C+T+A">The Cherenkov Telescope Array Consortium</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre-Santaella%2C+A">A. Aguirre-Santaella</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alispach%2C+C">C. Alispach</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amati%2C+L">L. Amati</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Araudo%2C+A">A. Araudo</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Ascas%C3%ADbar%2C+Y">Y. Ascas铆bar</a>, <a href="/search/astro-ph?searchtype=author&query=Ashley%2C+M">M. Ashley</a>, <a href="/search/astro-ph?searchtype=author&query=Balazs%2C+C">C. Balazs</a>, <a href="/search/astro-ph?searchtype=author&query=Ballester%2C+O">O. Ballester</a> , et al. (427 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="2007.16129v2-abstract-short" style="display: inline;"> We provide an updated assessment of the power of the Cherenkov Telescope Array (CTA) to search for thermally produced dark matter at the TeV scale, via the associated gamma-ray signal from pair-annihilating dark matter particles in the region around the Galactic centre. We find that CTA will open a new window of discovery potential, significantly extending the range of robustly testable models giv… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.16129v2-abstract-full').style.display = 'inline'; document.getElementById('2007.16129v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.16129v2-abstract-full" style="display: none;"> We provide an updated assessment of the power of the Cherenkov Telescope Array (CTA) to search for thermally produced dark matter at the TeV scale, via the associated gamma-ray signal from pair-annihilating dark matter particles in the region around the Galactic centre. We find that CTA will open a new window of discovery potential, significantly extending the range of robustly testable models given a standard cuspy profile of the dark matter density distribution. Importantly, even for a cored profile, the projected sensitivity of CTA will be sufficient to probe various well-motivated models of thermally produced dark matter at the TeV scale. This is due to CTA's unprecedented sensitivity, angular and energy resolutions, and the planned observational strategy. The survey of the inner Galaxy will cover a much larger region than corresponding previous observational campaigns with imaging atmospheric Cherenkov telescopes. CTA will map with unprecedented precision the large-scale diffuse emission in high-energy gamma rays, constituting a background for dark matter searches for which we adopt state-of-the-art models based on current data. Throughout our analysis, we use up-to-date event reconstruction Monte Carlo tools developed by the CTA consortium, and pay special attention to quantifying the level of instrumental systematic uncertainties, as well as background template systematic errors, required to probe thermally produced dark matter at these energies. "Full likelihood tables complementing our analysis are provided here [ https://doi.org/10.5281/zenodo.4057987 ]" <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.16129v2-abstract-full').style.display = 'none'; document.getElementById('2007.16129v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">68 pages (including references) and 26 figures; text identical to the version published in JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP01(2021)057 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2003.07295">arXiv:2003.07295</a> <span> [<a href="https://arxiv.org/pdf/2003.07295">pdf</a>, <a href="https://arxiv.org/format/2003.07295">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/10.1007/s10686-020-09657-w">10.1007/s10686-020-09657-w <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Soft proton scattering at grazing incidence from X-ray mirrors: analysis of experimental data in the framework of the non-elastic approximation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Amato%2C+R">R. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Mineo%2C+T">T. Mineo</a>, <a href="/search/astro-ph?searchtype=author&query=D%27A%C3%AC%2C+A">A. D'A矛</a>, <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">S. Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=Fioretti%2C+V">V. Fioretti</a>, <a href="/search/astro-ph?searchtype=author&query=Guzman%2C+A">A. Guzman</a>, <a href="/search/astro-ph?searchtype=author&query=Lotti%2C+S">S. Lotti</a>, <a href="/search/astro-ph?searchtype=author&query=Macculi%2C+C">C. Macculi</a>, <a href="/search/astro-ph?searchtype=author&query=Molendi%2C+S">S. Molendi</a>, <a href="/search/astro-ph?searchtype=author&query=Perinati%2C+E">E. Perinati</a>, <a href="/search/astro-ph?searchtype=author&query=Tenzer%2C+C">C. Tenzer</a>, <a href="/search/astro-ph?searchtype=author&query=Santangelo%2C+A">A. Santangelo</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="2003.07295v1-abstract-short" style="display: inline;"> Astronomical X-ray observatories with grazing incidence optics face the problem of pseudo-focusing of low energy protons from the mirrors towards the focal plane. Those protons constitute a variable, unpredictable component of the non X-ray background that strongly affects astronomical observations and a correct estimation of their flux at the focal plane is then essential. For this reason, we inv… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.07295v1-abstract-full').style.display = 'inline'; document.getElementById('2003.07295v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.07295v1-abstract-full" style="display: none;"> Astronomical X-ray observatories with grazing incidence optics face the problem of pseudo-focusing of low energy protons from the mirrors towards the focal plane. Those protons constitute a variable, unpredictable component of the non X-ray background that strongly affects astronomical observations and a correct estimation of their flux at the focal plane is then essential. For this reason, we investigate how they are scattered from the mirror surfaces when impacting with grazing angles. We compare the non-elastic model of reflectivity of particles at grazing incidence proposed by Remizovich et al. (1980) with the few available experimental measurements of proton scattering from X-ray mirrors. We develop a semi-empirical analytical model based on the fit of those experimental data with the Remizovich solution. We conclude that the scattering probability weakly depends on the energy of the impinging protons and that the relative energy losses are necessary to correctly model the data. The model we propose assumes no dependence on the incident energy and can be implemented in particle transport simulation codes to generate, for instance, proton response matrices for specific X-ray missions. Further laboratory measurements at lower energies and on other mirror samples, such as ATHENA Silicon Pore Optics, will improve the resolution of the model and will allow us to build the proper proton response matrices for a wider sample of X-ray observatories. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.07295v1-abstract-full').style.display = 'none'; document.getElementById('2003.07295v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2020. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1907.09220">arXiv:1907.09220</a> <span> [<a href="https://arxiv.org/pdf/1907.09220">pdf</a>, <a href="https://arxiv.org/format/1907.09220">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/10.1016/j.nima.2018.08.104">10.1016/j.nima.2018.08.104 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Trigger performance verification of the FlashCam prototype camera </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sailer%2C+S">S. Sailer</a>, <a href="/search/astro-ph?searchtype=author&query=Werner%2C+F">F. Werner</a>, <a href="/search/astro-ph?searchtype=author&query=Hermann%2C+G">G. Hermann</a>, <a href="/search/astro-ph?searchtype=author&query=Barcelo%2C+M">M. Barcelo</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+C">C. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Bernhard%2C+S">S. Bernhard</a>, <a href="/search/astro-ph?searchtype=author&query=Biegger%2C+M">M. Biegger</a>, <a href="/search/astro-ph?searchtype=author&query=Canelli%2C+F">F. Canelli</a>, <a href="/search/astro-ph?searchtype=author&query=Capasso%2C+M">M. Capasso</a>, <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">S. Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=Eisenkolb%2C+F">F. Eisenkolb</a>, <a href="/search/astro-ph?searchtype=author&query=Eschbach%2C+S">S. Eschbach</a>, <a href="/search/astro-ph?searchtype=author&query=Florin%2C+D">D. Florin</a>, <a href="/search/astro-ph?searchtype=author&query=F%C3%B6hr%2C+C">C. F枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Funk%2C+S">S. Funk</a>, <a href="/search/astro-ph?searchtype=author&query=Gadola%2C+A">A. Gadola</a>, <a href="/search/astro-ph?searchtype=author&query=Garrecht%2C+F">F. Garrecht</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+I">I. Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Kalekin%2C+O">O. Kalekin</a>, <a href="/search/astro-ph?searchtype=author&query=Kalkuhl%2C+C">C. Kalkuhl</a>, <a href="/search/astro-ph?searchtype=author&query=Kihm%2C+T">T. Kihm</a>, <a href="/search/astro-ph?searchtype=author&query=Lahmann%2C+R">R. Lahmann</a>, <a href="/search/astro-ph?searchtype=author&query=Pfeifer%2C+M">M. Pfeifer</a>, <a href="/search/astro-ph?searchtype=author&query=Principe%2C+G">G. Principe</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%BChlhofer%2C+G">G. P眉hlhofer</a> , et al. (11 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1907.09220v1-abstract-short" style="display: inline;"> FlashCam is a camera proposed for the medium-sized telescopes of the Cherenkov Telescope Array (CTA). We compare camera trigger rates obtained from measurements with the camera prototype in the laboratory and Monte-Carlo simulations, when scanning the parameter space of the fully-digital trigger logic and the intensity of a continuous light source mimicking the night sky background (NSB) during on… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.09220v1-abstract-full').style.display = 'inline'; document.getElementById('1907.09220v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1907.09220v1-abstract-full" style="display: none;"> FlashCam is a camera proposed for the medium-sized telescopes of the Cherenkov Telescope Array (CTA). We compare camera trigger rates obtained from measurements with the camera prototype in the laboratory and Monte-Carlo simulations, when scanning the parameter space of the fully-digital trigger logic and the intensity of a continuous light source mimicking the night sky background (NSB) during on-site operation. The comparisons of the measured data results to the Monte-Carlo simulations are used to verify the FlashCam trigger logic and the expected trigger performance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.09220v1-abstract-full').style.display = 'none'; document.getElementById('1907.09220v1-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 July, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14th Pisa Meeting on Advanced Detectors</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, Volume 936, 2019, Pages 392-393, ISSN 0168-9002 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.01426">arXiv:1904.01426</a> <span> [<a href="https://arxiv.org/pdf/1904.01426">pdf</a>, <a href="https://arxiv.org/format/1904.01426">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/10.1016/j.astropartphys.2019.04.001">10.1016/j.astropartphys.2019.04.001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Monte Carlo studies for the optimisation of the Cherenkov Telescope Array layout </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alispach%2C+C">C. Alispach</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amans%2C+J+-">J. -P. Amans</a>, <a href="/search/astro-ph?searchtype=author&query=Amati%2C+L">L. Amati</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arrabito%2C+L">L. Arrabito</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a>, <a href="/search/astro-ph?searchtype=author&query=Balazs%2C+C">C. Balazs</a>, <a href="/search/astro-ph?searchtype=author&query=Balbo%2C+M">M. Balbo</a>, <a href="/search/astro-ph?searchtype=author&query=Balmaverde%2C+B">B. Balmaverde</a>, <a href="/search/astro-ph?searchtype=author&query=Barai%2C+P">P. Barai</a>, <a href="/search/astro-ph?searchtype=author&query=Barbano%2C+A">A. Barbano</a>, <a href="/search/astro-ph?searchtype=author&query=Barkov%2C+M">M. Barkov</a> , et al. (445 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="1904.01426v1-abstract-short" style="display: inline;"> The Cherenkov Telescope Array (CTA) is the major next-generation observatory for ground-based very-high-energy gamma-ray astronomy. It will improve the sensitivity of current ground-based instruments by a factor of five to twenty, depending on the energy, greatly improving both their angular and energy resolutions over four decades in energy (from 20 GeV to 300 TeV). This achievement will be possi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.01426v1-abstract-full').style.display = 'inline'; document.getElementById('1904.01426v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.01426v1-abstract-full" style="display: none;"> The Cherenkov Telescope Array (CTA) is the major next-generation observatory for ground-based very-high-energy gamma-ray astronomy. It will improve the sensitivity of current ground-based instruments by a factor of five to twenty, depending on the energy, greatly improving both their angular and energy resolutions over four decades in energy (from 20 GeV to 300 TeV). This achievement will be possible by using tens of imaging Cherenkov telescopes of three successive sizes. They will be arranged into two arrays, one per hemisphere, located on the La Palma island (Spain) and in Paranal (Chile). We present here the optimised and final telescope arrays for both CTA sites, as well as their foreseen performance, resulting from the analysis of three different large-scale Monte Carlo productions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.01426v1-abstract-full').style.display = 'none'; document.getElementById('1904.01426v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">48 pages, 16 figures, accepted for publication in Astroparticle Physics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1812.04020">arXiv:1812.04020</a> <span> [<a href="https://arxiv.org/pdf/1812.04020">pdf</a>, <a href="https://arxiv.org/format/1812.04020">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s11433-018-9309-2">10.1007/s11433-018-9309-2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The enhanced X-ray Timing and Polarimetry mission - eXTP </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+S">ShuangNan Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Santangelo%2C+A">Andrea Santangelo</a>, <a href="/search/astro-ph?searchtype=author&query=Feroci%2C+M">Marco Feroci</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+Y">YuPeng Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+F">FangJun Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Y">Yong Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+H">Hua Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+S">Shu Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Brandt%2C+S">S酶ren Brandt</a>, <a href="/search/astro-ph?searchtype=author&query=Hernanz%2C+M">Margarita Hernanz</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+L">Luca Baldini</a>, <a href="/search/astro-ph?searchtype=author&query=Bozzo%2C+E">Enrico Bozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Campana%2C+R">Riccardo Campana</a>, <a href="/search/astro-ph?searchtype=author&query=De+Rosa%2C+A">Alessandra De Rosa</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+Y">YongWei Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Evangelista%2C+Y">Yuri Evangelista</a>, <a href="/search/astro-ph?searchtype=author&query=Karas%2C+V">Vladimir Karas</a>, <a href="/search/astro-ph?searchtype=author&query=Meidinger%2C+N">Norbert Meidinger</a>, <a href="/search/astro-ph?searchtype=author&query=Meuris%2C+A">Aline Meuris</a>, <a href="/search/astro-ph?searchtype=author&query=Nandra%2C+K">Kirpal Nandra</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+T">Teng Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Pareschi%2C+G">Giovanni Pareschi</a>, <a href="/search/astro-ph?searchtype=author&query=Orleanski%2C+P">Piotr Orleanski</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+Q">QiuShi Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Schanne%2C+S">Stephane Schanne</a> , et al. (125 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="1812.04020v1-abstract-short" style="display: inline;"> In this paper we present the enhanced X-ray Timing and Polarimetry mission - eXTP. eXTP is a space science mission designed to study fundamental physics under extreme conditions of density, gravity and magnetism. The mission aims at determining the equation of state of matter at supra-nuclear density, measuring effects of QED, and understanding the dynamics of matter in strong-field gravity. In ad… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.04020v1-abstract-full').style.display = 'inline'; document.getElementById('1812.04020v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1812.04020v1-abstract-full" style="display: none;"> In this paper we present the enhanced X-ray Timing and Polarimetry mission - eXTP. eXTP is a space science mission designed to study fundamental physics under extreme conditions of density, gravity and magnetism. The mission aims at determining the equation of state of matter at supra-nuclear density, measuring effects of QED, and understanding the dynamics of matter in strong-field gravity. In addition to investigating fundamental physics, eXTP will be a very powerful observatory for astrophysics that will provide observations of unprecedented quality on a variety of galactic and extragalactic objects. In particular, its wide field monitoring capabilities will be highly instrumental to detect the electro-magnetic counterparts of gravitational wave sources. The paper provides a detailed description of: (1) the technological and technical aspects, and the expected performance of the instruments of the scientific payload; (2) the elements and functions of the mission, from the spacecraft to the ground segment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.04020v1-abstract-full').style.display = 'none'; document.getElementById('1812.04020v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 December, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication on Sci. China Phys. Mech. Astron. (2019)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1807.11269">arXiv:1807.11269</a> <span> [<a href="https://arxiv.org/pdf/1807.11269">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.2312466">10.1117/12.2312466 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Large Area Detector onboard the eXTP mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Feroci%2C+M">Marco Feroci</a>, <a href="/search/astro-ph?searchtype=author&query=Ahangarianabhari%2C+M">Mahdi Ahangarianabhari</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">Giovanni Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosino%2C+F">Filippo Ambrosino</a>, <a href="/search/astro-ph?searchtype=author&query=Argan%2C+A">Andrea Argan</a>, <a href="/search/astro-ph?searchtype=author&query=Barbera%2C+M">Marco Barbera</a>, <a href="/search/astro-ph?searchtype=author&query=Bayer%2C+J">Joerg Bayer</a>, <a href="/search/astro-ph?searchtype=author&query=Bellutti%2C+P">Pierluigi Bellutti</a>, <a href="/search/astro-ph?searchtype=author&query=Bertucci%2C+B">Bruna Bertucci</a>, <a href="/search/astro-ph?searchtype=author&query=Bertuccio%2C+G">Giuseppe Bertuccio</a>, <a href="/search/astro-ph?searchtype=author&query=Borghi%2C+G">Giacomo Borghi</a>, <a href="/search/astro-ph?searchtype=author&query=Bozzo%2C+E">Enrico Bozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Cadoux%2C+F">Franck Cadoux</a>, <a href="/search/astro-ph?searchtype=author&query=Campana%2C+R">Riccardo Campana</a>, <a href="/search/astro-ph?searchtype=author&query=Ceraudo%2C+F">Francesco Ceraudo</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+T">Tianxiang Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cirrincione%2C+D">Daniela Cirrincione</a>, <a href="/search/astro-ph?searchtype=author&query=De+Rosa%2C+A">Alessandra De Rosa</a>, <a href="/search/astro-ph?searchtype=author&query=Del+Monte%2C+E">Ettore Del Monte</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Cosimo%2C+S">Sergio Di Cosimo</a>, <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">Sebastian Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=Evangelista%2C+Y">Yuri Evangelista</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+Q">Qingmei Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Favre%2C+Y">Yannick Favre</a>, <a href="/search/astro-ph?searchtype=author&query=Ficorella%2C+F">Francesco Ficorella</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="1807.11269v1-abstract-short" style="display: inline;"> The eXTP (enhanced X-ray Timing and Polarimetry) mission is a major project of the Chinese Academy of Sciences (CAS) and China National Space Administration (CNSA) currently performing an extended phase A study and proposed for a launch by 2025 in a low-earth orbit. The eXTP scientific payload envisages a suite of instruments (Spectroscopy Focusing Array, Polarimetry Focusing Array, Large Area Det… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.11269v1-abstract-full').style.display = 'inline'; document.getElementById('1807.11269v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1807.11269v1-abstract-full" style="display: none;"> The eXTP (enhanced X-ray Timing and Polarimetry) mission is a major project of the Chinese Academy of Sciences (CAS) and China National Space Administration (CNSA) currently performing an extended phase A study and proposed for a launch by 2025 in a low-earth orbit. The eXTP scientific payload envisages a suite of instruments (Spectroscopy Focusing Array, Polarimetry Focusing Array, Large Area Detector and Wide Field Monitor) offering unprecedented simultaneous wide-band X-ray spectral, timing and polarimetry sensitivity. A large European consortium is contributing to the eXTP study and it is expected to provide key hardware elements, including a Large Area Detector (LAD). The LAD instrument for eXTP is based on the design originally proposed for the LOFT mission within the ESA context. The eXTP/LAD envisages a deployed 3.4 m2 effective area in the 2-30 keV energy range, achieved through the technology of the large-area Silicon Drift Detectors - offering a spectral resolution of up to 200 eV FWHM at 6 keV - and of capillary plate collimators - limiting the field of view to about 1 degree. In this paper we provide an overview of the LAD instrument design, including new elements with respect to the earlier LOFT configuration. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.11269v1-abstract-full').style.display = 'none'; document.getElementById('1807.11269v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Paper presented at SPIE Space Telescopes and Instrumentation 2018</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proc. of SPIE Vol. 10699, 106991C - Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray, edited by Jan-Willem A. den Herder, Shouleh Nikzad, Kazuhiro Nakazawa </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1709.07997">arXiv:1709.07997</a> <span> [<a href="https://arxiv.org/pdf/1709.07997">pdf</a>, <a href="https://arxiv.org/format/1709.07997">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <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/10.1142/10986">10.1142/10986 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Science with the Cherenkov Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+T+C+T+A">The Cherenkov Telescope Array Consortium</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Acharya%2C+B+S">B. S. Acharya</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alispach%2C+C">C. Alispach</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amans%2C+J+-">J. -P. Amans</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Antolini%2C+E">E. Antolini</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Araya%2C+M">M. Araya</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arrabito%2C+L">L. Arrabito</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Ashley%2C+M">M. Ashley</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Balazs%2C+C">C. Balazs</a>, <a href="/search/astro-ph?searchtype=author&query=Balbo%2C+M">M. Balbo</a>, <a href="/search/astro-ph?searchtype=author&query=Ballester%2C+O">O. Ballester</a> , et al. (558 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="1709.07997v2-abstract-short" style="display: inline;"> The Cherenkov Telescope Array, CTA, will be the major global observatory for very high energy gamma-ray astronomy over the next decade and beyond. The scientific potential of CTA is extremely broad: from understanding the role of relativistic cosmic particles to the search for dark matter. CTA is an explorer of the extreme universe, probing environments from the immediate neighbourhood of black ho… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.07997v2-abstract-full').style.display = 'inline'; document.getElementById('1709.07997v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1709.07997v2-abstract-full" style="display: none;"> The Cherenkov Telescope Array, CTA, will be the major global observatory for very high energy gamma-ray astronomy over the next decade and beyond. The scientific potential of CTA is extremely broad: from understanding the role of relativistic cosmic particles to the search for dark matter. CTA is an explorer of the extreme universe, probing environments from the immediate neighbourhood of black holes to cosmic voids on the largest scales. Covering a huge range in photon energy from 20 GeV to 300 TeV, CTA will improve on all aspects of performance with respect to current instruments. The observatory will operate arrays on sites in both hemispheres to provide full sky coverage and will hence maximize the potential for the rarest phenomena such as very nearby supernovae, gamma-ray bursts or gravitational wave transients. With 99 telescopes on the southern site and 19 telescopes on the northern site, flexible operation will be possible, with sub-arrays available for specific tasks. CTA will have important synergies with many of the new generation of major astronomical and astroparticle observatories. Multi-wavelength and multi-messenger approaches combining CTA data with those from other instruments will lead to a deeper understanding of the broad-band non-thermal properties of target sources. The CTA Observatory will be operated as an open, proposal-driven observatory, with all data available on a public archive after a pre-defined proprietary period. Scientists from institutions worldwide have combined together to form the CTA Consortium. This Consortium has prepared a proposal for a Core Programme of highly motivated observations. The programme, encompassing approximately 40% of the available observing time over the first ten years of CTA operation, is made up of individual Key Science Projects (KSPs), which are presented in this document. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.07997v2-abstract-full').style.display = 'none'; document.getElementById('1709.07997v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 September, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2017. </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">213 pages, including references and glossary. Version 2: credits and references updated, some figures updated, and author list updated</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1709.03483">arXiv:1709.03483</a> <span>  </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Cherenkov Telescope Array Contributions to the 35th International Cosmic Ray Conference (ICRC2017) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Acharya%2C+B+S">B. S. Acharya</a>, <a href="/search/astro-ph?searchtype=author&query=Portella%2C+V+A">V. Ac铆n Portella</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Alberdi%2C+A">A. Alberdi</a>, <a href="/search/astro-ph?searchtype=author&query=Alcubierre%2C+M">M. Alcubierre</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alispach%2C+C">C. Alispach</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amans%2C+J+-">J. -P. Amans</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrogi%2C+L">L. Ambrogi</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Anduze%2C+M">M. Anduze</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Antolini%2C+E">E. Antolini</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Antonuccio%2C+V">V. Antonuccio</a> , et al. (1117 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="1709.03483v5-abstract-short" style="display: inline;"> List of contributions from the Cherenkov Telescope Array Consortium presented at the 35th International Cosmic Ray Conference, July 12-20 2017, Busan, Korea. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1709.03483v5-abstract-full" style="display: none;"> List of contributions from the Cherenkov Telescope Array Consortium presented at the 35th International Cosmic Ray Conference, July 12-20 2017, Busan, Korea. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.03483v5-abstract-full').style.display = 'none'; document.getElementById('1709.03483v5-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 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 September, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2017. </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">Index of Cherenkov Telescope Array conference proceedings at the ICRC2017, Busan, Korea</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1612.09528">arXiv:1612.09528</a> <span> [<a href="https://arxiv.org/pdf/1612.09528">pdf</a>, <a href="https://arxiv.org/format/1612.09528">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nima.2016.12.056">10.1016/j.nima.2016.12.056 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Performance Verification of the FlashCam Prototype Camera for the Cherenkov Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Werner%2C+F">F. Werner</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+C">C. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Bernhard%2C+S">S. Bernhard</a>, <a href="/search/astro-ph?searchtype=author&query=Capasso%2C+M">M. Capasso</a>, <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">S. Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=Eisenkolb%2C+F">F. Eisenkolb</a>, <a href="/search/astro-ph?searchtype=author&query=Eschbach%2C+S">S. Eschbach</a>, <a href="/search/astro-ph?searchtype=author&query=Florin%2C+D">D. Florin</a>, <a href="/search/astro-ph?searchtype=author&query=F%C3%B6hr%2C+C">C. F枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Funk%2C+S">S. Funk</a>, <a href="/search/astro-ph?searchtype=author&query=Gadola%2C+A">A. Gadola</a>, <a href="/search/astro-ph?searchtype=author&query=Garrecht%2C+F">F. Garrecht</a>, <a href="/search/astro-ph?searchtype=author&query=Hermann%2C+G">G. Hermann</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+I">I. Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Kalekin%2C+O">O. Kalekin</a>, <a href="/search/astro-ph?searchtype=author&query=Kalkuhl%2C+C">C. Kalkuhl</a>, <a href="/search/astro-ph?searchtype=author&query=Kasperek%2C+J">J. Kasperek</a>, <a href="/search/astro-ph?searchtype=author&query=Kihm%2C+T">T. Kihm</a>, <a href="/search/astro-ph?searchtype=author&query=Lahmann%2C+R">R. Lahmann</a>, <a href="/search/astro-ph?searchtype=author&query=Marszalek%2C+A">A. Marszalek</a>, <a href="/search/astro-ph?searchtype=author&query=Pfeifer%2C+M">M. Pfeifer</a>, <a href="/search/astro-ph?searchtype=author&query=Principe%2C+G">G. Principe</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%BChlhofer%2C+G">G. P眉hlhofer</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%BCrckhauer%2C+S">S. P眉rckhauer</a>, <a href="/search/astro-ph?searchtype=author&query=Rajda%2C+P+J">P. J. Rajda</a> , et al. (10 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="1612.09528v1-abstract-short" style="display: inline;"> The Cherenkov Telescope Array (CTA) is a future gamma-ray observatory that is planned to significantly improve upon the sensitivity and precision of the current generation of Cherenkov telescopes. The observatory will consist of several dozens of telescopes with different sizes and equipped with different types of cameras. Of these, the FlashCam camera system is the first to implement a fully digi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.09528v1-abstract-full').style.display = 'inline'; document.getElementById('1612.09528v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1612.09528v1-abstract-full" style="display: none;"> The Cherenkov Telescope Array (CTA) is a future gamma-ray observatory that is planned to significantly improve upon the sensitivity and precision of the current generation of Cherenkov telescopes. The observatory will consist of several dozens of telescopes with different sizes and equipped with different types of cameras. Of these, the FlashCam camera system is the first to implement a fully digital signal processing chain which allows for a traceable, configurable trigger scheme and flexible signal reconstruction. As of autumn 2016, a prototype FlashCam camera for the medium-sized telescopes of CTA nears completion. First results of the ongoing system tests demonstrate that the signal chain and the readout system surpass CTA requirements. The stability of the system is shown using long-term temperature cycling. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.09528v1-abstract-full').style.display = 'none'; document.getElementById('1612.09528v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 December, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 13 figures, Proceedings of the 9th International Workshop on Ring Imaging Cherenkov Detectors (RICH 2016), Lake Bled, Slovenia</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1610.05151">arXiv:1610.05151</a> <span>  </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Contributions of the Cherenkov Telescope Array (CTA) to the 6th International Symposium on High-Energy Gamma-Ray Astronomy (Gamma 2016) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+T+C">The CTA Consortium</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abchiche%2C+A">A. Abchiche</a>, <a href="/search/astro-ph?searchtype=author&query=Abeysekara%2C+U">U. Abeysekara</a>, <a href="/search/astro-ph?searchtype=author&query=Abril%2C+%C3%93">脫. Abril</a>, <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Acharya%2C+B+S">B. S. Acharya</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agnetta%2C+G">G. Agnetta</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Akhperjanian%2C+A">A. Akhperjanian</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alcubierre%2C+M">M. Alcubierre</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Allafort%2C+A+J">A. J. Allafort</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Amans%2C+J+-">J. -P. Amans</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrogi%2C+L">L. Ambrogi</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Anduze%2C+M">M. Anduze</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a> , et al. (1387 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="1610.05151v1-abstract-short" style="display: inline;"> List of contributions from the Cherenkov Telescope Array (CTA) Consortium presented at the 6th International Symposium on High-Energy Gamma-Ray Astronomy (Gamma 2016), July 11-15, 2016, in Heidelberg, Germany. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1610.05151v1-abstract-full" style="display: none;"> List of contributions from the Cherenkov Telescope Array (CTA) Consortium presented at the 6th International Symposium on High-Energy Gamma-Ray Astronomy (Gamma 2016), July 11-15, 2016, in Heidelberg, Germany. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.05151v1-abstract-full').style.display = 'none'; document.getElementById('1610.05151v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2016. </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">Index of CTA conference proceedings for the Gamma 2016, Heidelberg, Germany</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1610.04392">arXiv:1610.04392</a> <span> [<a href="https://arxiv.org/pdf/1610.04392">pdf</a>, <a href="https://arxiv.org/format/1610.04392">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1063/1.4969036">10.1063/1.4969036 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An Efficient Test Facility For The Cherenkov Telescope Array FlashCam Readout Electronics Production </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Eisenkolb%2C+F">F. Eisenkolb</a>, <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">S. Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=Kalkuhl%2C+C">C. Kalkuhl</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%BChlhofer%2C+G">G. P眉hlhofer</a>, <a href="/search/astro-ph?searchtype=author&query=Santangelo%2C+A">A. Santangelo</a>, <a href="/search/astro-ph?searchtype=author&query=Schanz%2C+T">T. Schanz</a>, <a href="/search/astro-ph?searchtype=author&query=Tenzer%2C+C">C. Tenzer</a>, <a href="/search/astro-ph?searchtype=author&query=team%2C+t+F">the FlashCam team</a>, <a href="/search/astro-ph?searchtype=author&query=consortium%2C+t+C">the CTA consortium</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="1610.04392v1-abstract-short" style="display: inline;"> The Cherenkov Telescope Array (CTA) is the planned next-generation instrument for ground-based gamma-ray astronomy, currently under preparation by a world-wide consortium. The FlashCam group is preparing a photomultiplier-based camera for the Medium Size Telescopes of CTA, with a fully digital Readout System (ROS). For the forthcoming mass production of a substantial number of cameras, efficient t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.04392v1-abstract-full').style.display = 'inline'; document.getElementById('1610.04392v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1610.04392v1-abstract-full" style="display: none;"> The Cherenkov Telescope Array (CTA) is the planned next-generation instrument for ground-based gamma-ray astronomy, currently under preparation by a world-wide consortium. The FlashCam group is preparing a photomultiplier-based camera for the Medium Size Telescopes of CTA, with a fully digital Readout System (ROS). For the forthcoming mass production of a substantial number of cameras, efficient test routines for all components are currently under development. We report here on a test facility for the ROS components. A test setup and routines have been developed and an early version of that setup has successfully been used to test a significant fraction of the ROS for the FlashCam camera prototype in January 2016. The test setup with its components and interface, as well as first results, are presented here. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.04392v1-abstract-full').style.display = 'none'; document.getElementById('1610.04392v1-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 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2016. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1610.01363">arXiv:1610.01363</a> <span> [<a href="https://arxiv.org/pdf/1610.01363">pdf</a>, <a href="https://arxiv.org/format/1610.01363">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/10.1063/1.4969035">10.1063/1.4969035 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Actuator Development at IAAT for the Cherenkov Telescope Array Medium Size Telescopes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">S. Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=Dick%2C+J">J. Dick</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%BChlhofer%2C+G">G. P眉hlhofer</a>, <a href="/search/astro-ph?searchtype=author&query=Renner%2C+S">S. Renner</a>, <a href="/search/astro-ph?searchtype=author&query=Santangelo%2C+A">A. Santangelo</a>, <a href="/search/astro-ph?searchtype=author&query=Schanz%2C+T">T. Schanz</a>, <a href="/search/astro-ph?searchtype=author&query=Tenzer%2C+C">C. Tenzer</a>, <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+t+C">the CTA Consortium</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="1610.01363v1-abstract-short" style="display: inline;"> The Cherenkov Telescope Array (CTA) will be the future observatory for TeV gamma-ray astronomy. In order to increase the sensitivity and to extend the energy coverage beyond the capabilities of current facilities, its design concept features telescopes of three different size classes. Based on the experience from H.E.S.S. phase II, the Institute for Astronomy and Astrophysics T眉bingen (IAAT) devel… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.01363v1-abstract-full').style.display = 'inline'; document.getElementById('1610.01363v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1610.01363v1-abstract-full" style="display: none;"> The Cherenkov Telescope Array (CTA) will be the future observatory for TeV gamma-ray astronomy. In order to increase the sensitivity and to extend the energy coverage beyond the capabilities of current facilities, its design concept features telescopes of three different size classes. Based on the experience from H.E.S.S. phase II, the Institute for Astronomy and Astrophysics T眉bingen (IAAT) develops actuators for the mirror control system of the CTA Medium Size Telescopes (MSTs). The goals of this effort are durability, high precision, and mechanical stability under all environmental conditions. Up to now, several revisions were developed and the corresponding prototypes were extensively tested. In this contribution our latest design revision proposed for the CTA MSTs are presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.01363v1-abstract-full').style.display = 'none'; document.getElementById('1610.01363v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2016. </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 the 6th International Symposium on High Energy Gamma-Ray Astronomy (Gamma2016), July 11-15, 2016, Heidelberg, Germany. To be published in the AIP Conference Proceedings</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1607.08823">arXiv:1607.08823</a> <span> [<a href="https://arxiv.org/pdf/1607.08823">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.2232034">10.1117/12.2232034 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> eXTP -- enhanced X-ray Timing and Polarimetry Mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+S+N">S. N. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Feroci%2C+M">M. Feroci</a>, <a href="/search/astro-ph?searchtype=author&query=Santangelo%2C+A">A. Santangelo</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+Y+W">Y. W. Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+H">H. Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Lu%2C+F+J">F. J. Lu</a>, <a href="/search/astro-ph?searchtype=author&query=Nandra%2C+K">K. Nandra</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Z+S">Z. S. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+S">S. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Bozzo%2C+E">E. Bozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Brandt%2C+S">S. Brandt</a>, <a href="/search/astro-ph?searchtype=author&query=De+Rosa%2C+A">A. De Rosa</a>, <a href="/search/astro-ph?searchtype=author&query=Gou%2C+L+J">L. J. Gou</a>, <a href="/search/astro-ph?searchtype=author&query=Hernanz%2C+M">M. Hernanz</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Klis%2C+M">M. van der Klis</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+X+D">X. D. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+Y">Y. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Orleanski%2C+P">P. Orleanski</a>, <a href="/search/astro-ph?searchtype=author&query=Pareschi%2C+G">G. Pareschi</a>, <a href="/search/astro-ph?searchtype=author&query=Pohl%2C+M">M. Pohl</a>, <a href="/search/astro-ph?searchtype=author&query=Poutanen%2C+J">J. Poutanen</a>, <a href="/search/astro-ph?searchtype=author&query=Qu%2C+J+L">J. L. Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Schanne%2C+S">S. Schanne</a>, <a href="/search/astro-ph?searchtype=author&query=Stella%2C+L">L. Stella</a>, <a href="/search/astro-ph?searchtype=author&query=Uttley%2C+P">P. Uttley</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="1607.08823v1-abstract-short" style="display: inline;"> eXTP is a science mission designed to study the state of matter under extreme conditions of density, gravity and magnetism. Primary targets include isolated and binary neutron stars, strong magnetic field systems like magnetars, and stellar-mass and supermassive black holes. The mission carries a unique and unprecedented suite of state-of-the-art scientific instruments enabling for the first time… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.08823v1-abstract-full').style.display = 'inline'; document.getElementById('1607.08823v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1607.08823v1-abstract-full" style="display: none;"> eXTP is a science mission designed to study the state of matter under extreme conditions of density, gravity and magnetism. Primary targets include isolated and binary neutron stars, strong magnetic field systems like magnetars, and stellar-mass and supermassive black holes. The mission carries a unique and unprecedented suite of state-of-the-art scientific instruments enabling for the first time ever the simultaneous spectral-timing-polarimetry studies of cosmic sources in the energy range from 0.5-30 keV (and beyond). Key elements of the payload are: the Spectroscopic Focusing Array (SFA) - a set of 11 X-ray optics for a total effective area of about 0.9 m^2 and 0.6 m^2 at 2 keV and 6 keV respectively, equipped with Silicon Drift Detectors offering <180 eV spectral resolution; the Large Area Detector (LAD) - a deployable set of 640 Silicon Drift Detectors, for a total effective area of about 3.4 m^2, between 6 and 10 keV, and spectral resolution <250 eV; the Polarimetry Focusing Array (PFA) - a set of 2 X-ray telescope, for a total effective area of 250 cm^2 at 2 keV, equipped with imaging gas pixel photoelectric polarimeters; the Wide Field Monitor (WFM) - a set of 3 coded mask wide field units, equipped with position-sensitive Silicon Drift Detectors, each covering a 90 degrees x 90 degrees FoV. The eXTP international consortium includes mostly major institutions of the Chinese Academy of Sciences and Universities in China, as well as major institutions in several European countries and the United States. The predecessor of eXTP, the XTP mission concept, has been selected and funded as one of the so-called background missions in the Strategic Priority Space Science Program of the Chinese Academy of Sciences since 2011. The strong European participation has significantly enhanced the scientific capabilities of eXTP. The planned launch date of the mission is earlier than 2025. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.08823v1-abstract-full').style.display = 'none'; document.getElementById('1607.08823v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 July, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2016. </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, 16 figures. Oral talk presented at SPIE Astronomical Telescopes and Instrumentation, June 26 to July 1, 2016, Edingurgh, UK</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Science China Physics, Mechanics & Astronomy, 2019, Volume 62, Issue 2, article id. 29502, 25 pp </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1509.02434">arXiv:1509.02434</a> <span> [<a href="https://arxiv.org/pdf/1509.02434">pdf</a>, <a href="https://arxiv.org/format/1509.02434">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> FlashCam: a fully-digital camera for the medium-sized telescopes of the Cherenkov Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=P%C3%BChlhofer%2C+G">G. P眉hlhofer</a>, <a href="/search/astro-ph?searchtype=author&query=Bauer%2C+C">C. Bauer</a>, <a href="/search/astro-ph?searchtype=author&query=Bernhard%2C+S">S. Bernhard</a>, <a href="/search/astro-ph?searchtype=author&query=Capasso%2C+M">M. Capasso</a>, <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">S. Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=Eisenkolb%2C+F">F. Eisenkolb</a>, <a href="/search/astro-ph?searchtype=author&query=Florin%2C+D">D. Florin</a>, <a href="/search/astro-ph?searchtype=author&query=F%C3%B6hr%2C+C">C. F枚hr</a>, <a href="/search/astro-ph?searchtype=author&query=Funk%2C+S">S. Funk</a>, <a href="/search/astro-ph?searchtype=author&query=Gadola%2C+A">A. Gadola</a>, <a href="/search/astro-ph?searchtype=author&query=Garrecht%2C+F">F. Garrecht</a>, <a href="/search/astro-ph?searchtype=author&query=Hermann%2C+G">G. Hermann</a>, <a href="/search/astro-ph?searchtype=author&query=Jung%2C+I">I. Jung</a>, <a href="/search/astro-ph?searchtype=author&query=Kalekin%2C+O">O. Kalekin</a>, <a href="/search/astro-ph?searchtype=author&query=Kalkuhl%2C+C">C. Kalkuhl</a>, <a href="/search/astro-ph?searchtype=author&query=Kasperek%2C+J">J. Kasperek</a>, <a href="/search/astro-ph?searchtype=author&query=Kihm%2C+T">T. Kihm</a>, <a href="/search/astro-ph?searchtype=author&query=Lahmann%2C+R">R. Lahmann</a>, <a href="/search/astro-ph?searchtype=author&query=Manalaysay%2C+A">A. Manalaysay</a>, <a href="/search/astro-ph?searchtype=author&query=Marszalek%2C+A">A. Marszalek</a>, <a href="/search/astro-ph?searchtype=author&query=Pfeifer%2C+M">M. Pfeifer</a>, <a href="/search/astro-ph?searchtype=author&query=Rajda%2C+P+J">P. J. Rajda</a>, <a href="/search/astro-ph?searchtype=author&query=Reimer%2C+O">O. Reimer</a>, <a href="/search/astro-ph?searchtype=author&query=Santangelo%2C+A">A. Santangelo</a>, <a href="/search/astro-ph?searchtype=author&query=Schanz%2C+T">T. Schanz</a> , et al. (9 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1509.02434v1-abstract-short" style="display: inline;"> The FlashCam group is currently preparing photomultiplier-tube based cameras proposed for the medium-sized telescopes (MST) of the Cherenkov Telescope Array (CTA). The cameras are designed around the FlashCam readout concept which is the first fully-digital readout system for Cherenkov cameras, based on commercial FADCs and FPGAs as key components for the front-end electronics modules and a high p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.02434v1-abstract-full').style.display = 'inline'; document.getElementById('1509.02434v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1509.02434v1-abstract-full" style="display: none;"> The FlashCam group is currently preparing photomultiplier-tube based cameras proposed for the medium-sized telescopes (MST) of the Cherenkov Telescope Array (CTA). The cameras are designed around the FlashCam readout concept which is the first fully-digital readout system for Cherenkov cameras, based on commercial FADCs and FPGAs as key components for the front-end electronics modules and a high performance camera server as back-end. This contribution describes the progress of the full-scale FlashCam camera prototype currently under construction, as well as performance results also obtained with earlier demonstrator setups. Plans towards the production and implementation of FlashCams on site are also briefly presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.02434v1-abstract-full').style.display = 'none'; document.getElementById('1509.02434v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2015. </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, 6 figures. In Proceedings of the 34th International Cosmic Ray Conference (ICRC2015), The Hague, The Netherlands. All CTA contributions at arXiv:1508.05894</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1508.06177">arXiv:1508.06177</a> <span> [<a href="https://arxiv.org/pdf/1508.06177">pdf</a>, <a href="https://arxiv.org/format/1508.06177">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Recent developments for the testing of Cherenkov Telescope Array mirrors and actuators in T眉bingen </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dick%2C+J">J. Dick</a>, <a href="/search/astro-ph?searchtype=author&query=Bonardi%2C+A">A. Bonardi</a>, <a href="/search/astro-ph?searchtype=author&query=Bressel%2C+S">S. Bressel</a>, <a href="/search/astro-ph?searchtype=author&query=Capasso%2C+M">M. Capasso</a>, <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">S. Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=Eisenkolb%2C+F">F. Eisenkolb</a>, <a href="/search/astro-ph?searchtype=author&query=Gottschall%2C+D">D. Gottschall</a>, <a href="/search/astro-ph?searchtype=author&query=Kendziorra%2C+E">E. Kendziorra</a>, <a href="/search/astro-ph?searchtype=author&query=P%C3%BChlhofer%2C+G">G. P眉hlhofer</a>, <a href="/search/astro-ph?searchtype=author&query=Renner%2C+S">S. Renner</a>, <a href="/search/astro-ph?searchtype=author&query=Santangelo%2C+A">A. Santangelo</a>, <a href="/search/astro-ph?searchtype=author&query=Schanz%2C+T">T. Schanz</a>, <a href="/search/astro-ph?searchtype=author&query=Tenzer%2C+C">C. Tenzer</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="1508.06177v1-abstract-short" style="display: inline;"> The Cherenkov Telescope Array (CTA) is the next generation Cherenkov telescope facility. It will consist of a large number of segmented-mirror telescopes of three different diameters, placed in two locations, one in the northern and one in the southern hemisphere, thus covering the whole sky. The total number of mirror tiles will be on the order of 10,000, corresponding to a reflective area of ~10… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.06177v1-abstract-full').style.display = 'inline'; document.getElementById('1508.06177v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1508.06177v1-abstract-full" style="display: none;"> The Cherenkov Telescope Array (CTA) is the next generation Cherenkov telescope facility. It will consist of a large number of segmented-mirror telescopes of three different diameters, placed in two locations, one in the northern and one in the southern hemisphere, thus covering the whole sky. The total number of mirror tiles will be on the order of 10,000, corresponding to a reflective area of ~10^4 m^2. The Institute for Astronomy and Astrophysics in T眉bingen (IAAT) is currently developing mirror control alignment mechanics, electronics, and software optimized for the medium sized telescopes. In addition, IAAT is participating in the CTA mirror prototype testing. In this paper we present the status of the current developments, the main results of recent tests, and plans for the production phase of the mirror control system. We also briefly present the T眉bingen facility for mirror testing. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.06177v1-abstract-full').style.display = 'none'; document.getElementById('1508.06177v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 August, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2015. </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">In Proceedings of the 34th International Cosmic Ray Conference (ICRC2015), The Hague, The Netherlands. All CTA contributions at arXiv:1508.05894</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1508.05894">arXiv:1508.05894</a> <span>  </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> CTA Contributions to the 34th International Cosmic Ray Conference (ICRC2015) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+T+C">The CTA Consortium</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abchiche%2C+A">A. Abchiche</a>, <a href="/search/astro-ph?searchtype=author&query=Abeysekara%2C+U">U. Abeysekara</a>, <a href="/search/astro-ph?searchtype=author&query=Abril%2C+%C3%93">脫. Abril</a>, <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Acharya%2C+B+S">B. S. Acharya</a>, <a href="/search/astro-ph?searchtype=author&query=Actis%2C+M">M. Actis</a>, <a href="/search/astro-ph?searchtype=author&query=Agnetta%2C+G">G. Agnetta</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/astro-ph?searchtype=author&query=Akhperjanian%2C+A">A. Akhperjanian</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alcubierre%2C+M">M. Alcubierre</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Aliu%2C+E">E. Aliu</a>, <a href="/search/astro-ph?searchtype=author&query=Allafort%2C+A+J">A. J. Allafort</a>, <a href="/search/astro-ph?searchtype=author&query=Allan%2C+D">D. Allan</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Amans%2C+J+-">J. -P. Amans</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrogi%2C+L">L. Ambrogi</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a> , et al. (1290 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="1508.05894v2-abstract-short" style="display: inline;"> List of contributions from the CTA Consortium presented at the 34th International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, The Netherlands. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1508.05894v2-abstract-full" style="display: none;"> List of contributions from the CTA Consortium presented at the 34th International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, The Netherlands. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.05894v2-abstract-full').style.display = 'none'; document.getElementById('1508.05894v2-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 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 August, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2015. </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">Index of CTA conference proceedings at the ICRC2015, The Hague (The Netherlands). v1: placeholder with no arXiv links yet, to be replaced once individual contributions have been all submitted; v2: final with arXiv links to all CTA contributions and full author list</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1504.01024">arXiv:1504.01024</a> <span> [<a href="https://arxiv.org/pdf/1504.01024">pdf</a>, <a href="https://arxiv.org/format/1504.01024">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s10686-015-9451-4">10.1007/s10686-015-9451-4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Soft Proton Scattering Efficiency Measurements on X-Ray Mirror Shells </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">S. Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=Tenzer%2C+C">C. Tenzer</a>, <a href="/search/astro-ph?searchtype=author&query=Perinati%2C+E">E. Perinati</a>, <a href="/search/astro-ph?searchtype=author&query=Santangelo%2C+A">A. Santangelo</a>, <a href="/search/astro-ph?searchtype=author&query=Freyberg%2C+M">M. Freyberg</a>, <a href="/search/astro-ph?searchtype=author&query=Friedrich%2C+P">P. Friedrich</a>, <a href="/search/astro-ph?searchtype=author&query=Jochum%2C+J">J. Jochum</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="1504.01024v1-abstract-short" style="display: inline;"> In-orbit experience has shown that soft protons are funneled more efficiently through focusing Wolter-type optics of X-ray observatories than simulations predicted. These protons can degrade the performance of solid-state X-ray detectors and contribute to the instrumental background. Since laboratory measurements of the scattering process are rare, an experiment for grazing angles has been set up… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.01024v1-abstract-full').style.display = 'inline'; document.getElementById('1504.01024v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1504.01024v1-abstract-full" style="display: none;"> In-orbit experience has shown that soft protons are funneled more efficiently through focusing Wolter-type optics of X-ray observatories than simulations predicted. These protons can degrade the performance of solid-state X-ray detectors and contribute to the instrumental background. Since laboratory measurements of the scattering process are rare, an experiment for grazing angles has been set up at the accelerator facility of the University of T眉bingen. Systematic measurements at incidence angles ranging from 0.3掳 to 1.2掳 with proton energies around 250 keV, 500 keV, and 1 MeV have been carried out. Parts of spare mirror shells of the eROSITA (extended ROentgen Survey with an Imaging Telescope Array) instrument have been used as scattering targets. This publication comprises a detailed description of the setup, the calibration and normalization methods, and the scattering efficiency and energy loss results. A comparison of the results with a theoretical scattering description and with simulations is included as well. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.01024v1-abstract-full').style.display = 'none'; document.getElementById('1504.01024v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 April, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2015. </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, 19 figures; accepted for publication in Experimental Astronomy</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1408.6548">arXiv:1408.6548</a> <span> [<a href="https://arxiv.org/pdf/1408.6548">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.2055747">10.1117/12.2055747 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radiation tests of the Silicon Drift Detectors for LOFT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Del+Monte%2C+E">E. Del Monte</a>, <a href="/search/astro-ph?searchtype=author&query=Azzarello%2C+P">P. Azzarello</a>, <a href="/search/astro-ph?searchtype=author&query=Bozzo%2C+E">E. Bozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Bugiel%2C+S">S. Bugiel</a>, <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">S. Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=Evangelista%2C+Y">Y. Evangelista</a>, <a href="/search/astro-ph?searchtype=author&query=Kendziorra%2C+E">E. Kendziorra</a>, <a href="/search/astro-ph?searchtype=author&query=Muleri%2C+F">F. Muleri</a>, <a href="/search/astro-ph?searchtype=author&query=Perinati%2C+E">E. Perinati</a>, <a href="/search/astro-ph?searchtype=author&query=Rachevski%2C+A">A. Rachevski</a>, <a href="/search/astro-ph?searchtype=author&query=Zampa%2C+G">G. Zampa</a>, <a href="/search/astro-ph?searchtype=author&query=Zampa%2C+N">N. Zampa</a>, <a href="/search/astro-ph?searchtype=author&query=Feroci%2C+M">M. Feroci</a>, <a href="/search/astro-ph?searchtype=author&query=Pohl%2C+M">M. Pohl</a>, <a href="/search/astro-ph?searchtype=author&query=Santangelo%2C+A">A. Santangelo</a>, <a href="/search/astro-ph?searchtype=author&query=Vacchi%2C+A">A. Vacchi</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="1408.6548v1-abstract-short" style="display: inline;"> During the three years long assessment phase of the LOFT mission, candidate to the M3 launch opportunity of the ESA Cosmic Vision programme, we estimated and measured the radiation damage of the silicon drift detectors (SDDs) of the satellite instrumentation. In particular, we irradiated the detectors with protons (of 0.8 and 11 MeV energy) to study the increment of leakage current and the variati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.6548v1-abstract-full').style.display = 'inline'; document.getElementById('1408.6548v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1408.6548v1-abstract-full" style="display: none;"> During the three years long assessment phase of the LOFT mission, candidate to the M3 launch opportunity of the ESA Cosmic Vision programme, we estimated and measured the radiation damage of the silicon drift detectors (SDDs) of the satellite instrumentation. In particular, we irradiated the detectors with protons (of 0.8 and 11 MeV energy) to study the increment of leakage current and the variation of the charge collection efficiency produced by the displacement damage, and we "bombarded" the detectors with hypervelocity dust grains to measure the effect of the debris impacts. In this paper we describe the measurements and discuss the results in the context of the LOFT mission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.6548v1-abstract-full').style.display = 'none'; document.getElementById('1408.6548v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2014. </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">Proc. SPIE 9144, Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray, 914464</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1408.6535">arXiv:1408.6535</a> <span> [<a href="https://arxiv.org/pdf/1408.6535">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.2054943">10.1117/12.2054943 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hyper-velocity impact test and simulation of a double-wall shield concept for the Wide Field Monitor aboard LOFT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Perinati%2C+E">E. Perinati</a>, <a href="/search/astro-ph?searchtype=author&query=Rott%2C+M">M. Rott</a>, <a href="/search/astro-ph?searchtype=author&query=Santangelo%2C+A">A. Santangelo</a>, <a href="/search/astro-ph?searchtype=author&query=Suchy%2C+S">S. Suchy</a>, <a href="/search/astro-ph?searchtype=author&query=Tenzer%2C+C">C. Tenzer</a>, <a href="/search/astro-ph?searchtype=author&query=Del+Monte%2C+E">E. Del Monte</a>, <a href="/search/astro-ph?searchtype=author&query=Herder%2C+J+-+d">J. -W. den Herder</a>, <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">S. Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=Feroci%2C+M">M. Feroci</a>, <a href="/search/astro-ph?searchtype=author&query=Rachevski%2C+A">A. Rachevski</a>, <a href="/search/astro-ph?searchtype=author&query=Vacchi%2C+A">A. Vacchi</a>, <a href="/search/astro-ph?searchtype=author&query=Zampa%2C+G">G. Zampa</a>, <a href="/search/astro-ph?searchtype=author&query=Zampa%2C+N">N. Zampa</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="1408.6535v1-abstract-short" style="display: inline;"> The space mission LOFT (Large Observatory For X-ray Timing) was selected in 2011 by ESA as one of the candidates for the M3 launch opportunity. LOFT is equipped with two instruments, the Large Area Detector (LAD) and the Wide Field Monitor (WFM), based on Silicon Drift Detectors (SDDs). In orbit, they would be exposed to hyper-velocity impacts by environmental dust particles, which might alter the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.6535v1-abstract-full').style.display = 'inline'; document.getElementById('1408.6535v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1408.6535v1-abstract-full" style="display: none;"> The space mission LOFT (Large Observatory For X-ray Timing) was selected in 2011 by ESA as one of the candidates for the M3 launch opportunity. LOFT is equipped with two instruments, the Large Area Detector (LAD) and the Wide Field Monitor (WFM), based on Silicon Drift Detectors (SDDs). In orbit, they would be exposed to hyper-velocity impacts by environmental dust particles, which might alter the surface properties of the SDDs. In order to assess the risk posed by these events, we performed simulations in ESABASE2 and laboratory tests. Tests on SDD prototypes aimed at verifying to what extent the structural damages produced by impacts affect the SDD functionality have been performed at the Van de Graaff dust accelerator at the Max Planck Institute for Nuclear Physics (MPIK) in Heidelberg. For the WFM, where we expect a rate of risky impacts notably higher than for the LAD, we designed, simulated and successfully tested at the plasma accelerator at the Technical University in Munich (TUM) a double-wall shielding configuration based on thin foils of Kapton and Polypropylene. In this paper we summarize all the assessment, focussing on the experimental test campaign at TUM. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.6535v1-abstract-full').style.display = 'none'; document.getElementById('1408.6535v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2014. </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">Proc. SPIE 9144, Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray, 914465</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1408.6526">arXiv:1408.6526</a> <span> [<a href="https://arxiv.org/pdf/1408.6526">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.2055913">10.1117/12.2055913 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Large Observatory For x-ray Timing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Feroci%2C+M">M. Feroci</a>, <a href="/search/astro-ph?searchtype=author&query=Herder%2C+J+W+d">J. W. den Herder</a>, <a href="/search/astro-ph?searchtype=author&query=Bozzo%2C+E">E. Bozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Barret%2C+D">D. Barret</a>, <a href="/search/astro-ph?searchtype=author&query=Brandt%2C+S">S. Brandt</a>, <a href="/search/astro-ph?searchtype=author&query=Hernanz%2C+M">M. Hernanz</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Klis%2C+M">M. van der Klis</a>, <a href="/search/astro-ph?searchtype=author&query=Pohl%2C+M">M. Pohl</a>, <a href="/search/astro-ph?searchtype=author&query=Santangelo%2C+A">A. Santangelo</a>, <a href="/search/astro-ph?searchtype=author&query=Stella%2C+L">L. Stella</a>, <a href="/search/astro-ph?searchtype=author&query=Watts%2C+A">A. Watts</a>, <a href="/search/astro-ph?searchtype=author&query=Wilms%2C+J">J. Wilms</a>, <a href="/search/astro-ph?searchtype=author&query=Zane%2C+S">S. Zane</a>, <a href="/search/astro-ph?searchtype=author&query=Ahangarianabhari%2C+M">M. Ahangarianabhari</a>, <a href="/search/astro-ph?searchtype=author&query=Albertus%2C+C">C. Albertus</a>, <a href="/search/astro-ph?searchtype=author&query=Alford%2C+M">M. Alford</a>, <a href="/search/astro-ph?searchtype=author&query=Alpar%2C+A">A. Alpar</a>, <a href="/search/astro-ph?searchtype=author&query=Altamirano%2C+D">D. Altamirano</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+L">L. Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Amati%2C+L">L. Amati</a>, <a href="/search/astro-ph?searchtype=author&query=Amoros%2C+C">C. Amoros</a>, <a href="/search/astro-ph?searchtype=author&query=Andersson%2C+N">N. Andersson</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+A">A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Argan%2C+A">A. Argan</a>, <a href="/search/astro-ph?searchtype=author&query=Artigue%2C+R">R. Artigue</a> , et al. (320 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="1408.6526v2-abstract-short" style="display: inline;"> The Large Observatory For x-ray Timing (LOFT) was studied within ESA M3 Cosmic Vision framework and participated in the final down-selection for a launch slot in 2022-2024. Thanks to the unprecedented combination of effective area and spectral resolution of its main instrument, LOFT will study the behaviour of matter under extreme conditions, such as the strong gravitational field in the innermost… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.6526v2-abstract-full').style.display = 'inline'; document.getElementById('1408.6526v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1408.6526v2-abstract-full" style="display: none;"> The Large Observatory For x-ray Timing (LOFT) was studied within ESA M3 Cosmic Vision framework and participated in the final down-selection for a launch slot in 2022-2024. Thanks to the unprecedented combination of effective area and spectral resolution of its main instrument, LOFT will study the behaviour of matter under extreme conditions, such as the strong gravitational field in the innermost regions of accretion flows close to black holes and neutron stars, and the supra-nuclear densities in the interior of neutron stars. The science payload is based on a Large Area Detector (LAD, 10 m 2 effective area, 2-30 keV, 240 eV spectral resolution, 1 deg collimated field of view) and a WideField Monitor (WFM, 2-50 keV, 4 steradian field of view, 1 arcmin source location accuracy, 300 eV spectral resolution). The WFM is equipped with an on-board system for bright events (e.g. GRB) localization. The trigger time and position of these events are broadcast to the ground within 30 s from discovery. In this paper we present the status of the mission at the end of its Phase A study. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.6526v2-abstract-full').style.display = 'none'; document.getElementById('1408.6526v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2014. </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">Proc. SPIE 9144, Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray, 91442T</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1405.5466">arXiv:1405.5466</a> <span> [<a href="https://arxiv.org/pdf/1405.5466">pdf</a>, <a href="https://arxiv.org/ps/1405.5466">ps</a>, <a href="https://arxiv.org/format/1405.5466">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/9/07/P07016">10.1088/1748-0221/9/07/P07016 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the effect of Non Ionising Energy Losses on the leakage current of Silicon Drift Detector prototypes for the LOFT satellite </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Del+Monte%2C+E">E. Del Monte</a>, <a href="/search/astro-ph?searchtype=author&query=Rachevski%2C+A">A. Rachevski</a>, <a href="/search/astro-ph?searchtype=author&query=Zampa%2C+G">G. Zampa</a>, <a href="/search/astro-ph?searchtype=author&query=Zampa%2C+N">N. Zampa</a>, <a href="/search/astro-ph?searchtype=author&query=Azzarello%2C+P">P. Azzarello</a>, <a href="/search/astro-ph?searchtype=author&query=Bozzo%2C+E">E. Bozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Campana%2C+R">R. Campana</a>, <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">S. Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=Evangelista%2C+Y">Y. Evangelista</a>, <a href="/search/astro-ph?searchtype=author&query=Perinati%2C+E">E. Perinati</a>, <a href="/search/astro-ph?searchtype=author&query=Feroci%2C+M">M. Feroci</a>, <a href="/search/astro-ph?searchtype=author&query=Pohl%2C+M">M. Pohl</a>, <a href="/search/astro-ph?searchtype=author&query=Vacchi%2C+A">A. Vacchi</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="1405.5466v3-abstract-short" style="display: inline;"> The silicon drift detectors are at the basis of the instrumentation aboard the Large Observatory For x-ray Timing (LOFT) satellite mission, which underwent a three year assessment phase within the "Cosmic Vision 2015 - 2025" long-term science plan of the European Space Agency. Silicon detectors are especially sensitive to the displacement damage, produced by the non ionising energy losses of charg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.5466v3-abstract-full').style.display = 'inline'; document.getElementById('1405.5466v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1405.5466v3-abstract-full" style="display: none;"> The silicon drift detectors are at the basis of the instrumentation aboard the Large Observatory For x-ray Timing (LOFT) satellite mission, which underwent a three year assessment phase within the "Cosmic Vision 2015 - 2025" long-term science plan of the European Space Agency. Silicon detectors are especially sensitive to the displacement damage, produced by the non ionising energy losses of charged and neutral particles, leading to an increase of the device leakage current and thus worsening the spectral resolution. During the LOFT assessment phase, we irradiated two silicon drift detectors with a proton beam at the Proton Irradiation Facility in the accelerator of the Paul Scherrer Institute and we measured the increase in leakage current. In this paper we report the results of the irradiation and we discuss the impact of the radiation damage on the LOFT scientific performance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.5466v3-abstract-full').style.display = 'none'; document.getElementById('1405.5466v3-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 June, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 May, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2014. </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, 2 tables. Accepted for publication by Journal of Instrumentation (JINST)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Instrumentation, Volume 9, July 2014 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1307.4204">arXiv:1307.4204</a> <span> [<a href="https://arxiv.org/pdf/1307.4204">pdf</a>, <a href="https://arxiv.org/format/1307.4204">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nima.2013.04.049">10.1016/j.nima.2013.04.049 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A setup for soft proton irradiation of X-ray detectors for future astronomical space missions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">Sebastian Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=Azzarello%2C+P">Philipp Azzarello</a>, <a href="/search/astro-ph?searchtype=author&query=Del+Monte%2C+E">Ettore Del Monte</a>, <a href="/search/astro-ph?searchtype=author&query=Feroci%2C+M">Marco Feroci</a>, <a href="/search/astro-ph?searchtype=author&query=Jochum%2C+J">Josef Jochum</a>, <a href="/search/astro-ph?searchtype=author&query=Kendziorra%2C+E">Eckhard Kendziorra</a>, <a href="/search/astro-ph?searchtype=author&query=Perinati%2C+E">Emanuele Perinati</a>, <a href="/search/astro-ph?searchtype=author&query=Rachevski%2C+A">Alexandre Rachevski</a>, <a href="/search/astro-ph?searchtype=author&query=Santangelo%2C+A">Andrea Santangelo</a>, <a href="/search/astro-ph?searchtype=author&query=Tenzer%2C+C">Christoph Tenzer</a>, <a href="/search/astro-ph?searchtype=author&query=Vacchi%2C+A">Andrea Vacchi</a>, <a href="/search/astro-ph?searchtype=author&query=Zampa%2C+G">Gianluigi Zampa</a>, <a href="/search/astro-ph?searchtype=author&query=Zampa%2C+N">Nicola Zampa</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="1307.4204v1-abstract-short" style="display: inline;"> Protons that are trapped in the Earth's magnetic field are one of the main threats to astronomical X-ray observatories. Soft protons, in the range from tens of keV up to a few MeV, impinging on silicon X-ray detectors can lead to a significant degradation of the detector performance. Especially in low earth orbits an enhancement of the soft proton flux has been found. A setup to irradiate detector… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.4204v1-abstract-full').style.display = 'inline'; document.getElementById('1307.4204v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1307.4204v1-abstract-full" style="display: none;"> Protons that are trapped in the Earth's magnetic field are one of the main threats to astronomical X-ray observatories. Soft protons, in the range from tens of keV up to a few MeV, impinging on silicon X-ray detectors can lead to a significant degradation of the detector performance. Especially in low earth orbits an enhancement of the soft proton flux has been found. A setup to irradiate detectors with soft protons has been constructed at the Van-de-Graaff accelerator of the Physikalisches Institut of the University of T眉bingen. Key advantages are a high flux uniformity over a large area, to enable irradiations of large detectors, and a monitoring system for the applied fluence, the beam uniformity, and the spectrum, that allows testing of detector prototypes in early development phases, when readout electronics are not yet available. Two irradiation campaigns have been performed so far with this setup. The irradiated detectors are silicon drift detectors, designated for the use on-board the LOFT space mission. This paper gives a description of the experimental setup and the associated monitoring system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.4204v1-abstract-full').style.display = 'none'; document.getElementById('1307.4204v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 July, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 10 figures, 4 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nuclear Instruments and Methods in Physics Research Section A, Volume 721 (2013), Pages 65-72 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1209.3094">arXiv:1209.3094</a> <span> [<a href="https://arxiv.org/pdf/1209.3094">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.926118">10.1117/12.926118 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Accelerator experiments with soft protons and hyper-velocity dust particles: application to ongoing projects of future X-ray missions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Perinati%2C+E">E. Perinati</a>, <a href="/search/astro-ph?searchtype=author&query=Diebold%2C+S">S. Diebold</a>, <a href="/search/astro-ph?searchtype=author&query=Kendziorra%2C+E">E. Kendziorra</a>, <a href="/search/astro-ph?searchtype=author&query=Santangelo%2C+A">A. Santangelo</a>, <a href="/search/astro-ph?searchtype=author&query=Tenzer%2C+C">C. Tenzer</a>, <a href="/search/astro-ph?searchtype=author&query=Jochum%2C+J">J. Jochum</a>, <a href="/search/astro-ph?searchtype=author&query=Bugiel%2C+S">S. Bugiel</a>, <a href="/search/astro-ph?searchtype=author&query=Srama%2C+R">R. Srama</a>, <a href="/search/astro-ph?searchtype=author&query=Del+Monte%2C+E">E. Del Monte</a>, <a href="/search/astro-ph?searchtype=author&query=Feroci%2C+M">M. Feroci</a>, <a href="/search/astro-ph?searchtype=author&query=Rubini%2C+A">A. Rubini</a>, <a href="/search/astro-ph?searchtype=author&query=Rachevski%2C+A">A. Rachevski</a>, <a href="/search/astro-ph?searchtype=author&query=Zampa%2C+G">G. Zampa</a>, <a href="/search/astro-ph?searchtype=author&query=Zampa%2C+N">N. Zampa</a>, <a href="/search/astro-ph?searchtype=author&query=Rashevskaya%2C+I">I. Rashevskaya</a>, <a href="/search/astro-ph?searchtype=author&query=Vacchi%2C+A">A. Vacchi</a>, <a href="/search/astro-ph?searchtype=author&query=Azzarello%2C+P">P. Azzarello</a>, <a href="/search/astro-ph?searchtype=author&query=Bozzo%2C+E">E. Bozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Herder%2C+J+-+d">J. -W. den Herder</a>, <a href="/search/astro-ph?searchtype=author&query=Zane%2C+S">S. Zane</a>, <a href="/search/astro-ph?searchtype=author&query=Brandt%2C+S">S. Brandt</a>, <a href="/search/astro-ph?searchtype=author&query=Hernanz%2C+M">M. Hernanz</a>, <a href="/search/astro-ph?searchtype=author&query=Leutenegger%2C+M+A">M. A. Leutenegger</a>, <a href="/search/astro-ph?searchtype=author&query=Kelley%2C+R+L">R. L. Kelley</a>, <a href="/search/astro-ph?searchtype=author&query=Kilbourne%2C+C+A">C. A. Kilbourne</a> , et al. (9 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1209.3094v1-abstract-short" style="display: inline;"> We report on our activities, currently in progress, aimed at performing accelerator experiments with soft protons and hyper-velocity dust particles. They include tests of different types of X-ray detectors and related components (such as filters) and measurements of scattering of soft protons and hyper-velocity dust particles off X-ray mirror shells. These activities have been identified as a goal… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1209.3094v1-abstract-full').style.display = 'inline'; document.getElementById('1209.3094v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1209.3094v1-abstract-full" style="display: none;"> We report on our activities, currently in progress, aimed at performing accelerator experiments with soft protons and hyper-velocity dust particles. They include tests of different types of X-ray detectors and related components (such as filters) and measurements of scattering of soft protons and hyper-velocity dust particles off X-ray mirror shells. These activities have been identified as a goal in the context of a number of ongoing space projects in order to assess the risk posed by environmental radiation and dust and qualify the adopted instrumentation with respect to possible damage or performance degradation. In this paper we focus on tests for the Silicon Drift Detectors (SDDs) used aboard the LOFT space mission. We use the Van de Graaff accelerators at the University of T眉bingen and at the Max Planck Institute for Nuclear Physics (MPIK) in Heidelberg, for soft proton and hyper-velocity dust tests respectively. We present the experimental set-up adopted to perform the tests, status of the activities and some very preliminary results achieved at present time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1209.3094v1-abstract-full').style.display = 'none'; document.getElementById('1209.3094v1-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 September, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Proceedings of SPIE, Vol. 8443, Paper No. 8443-24, 2012</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1209.1497">arXiv:1209.1497</a> <span> [<a href="https://arxiv.org/pdf/1209.1497">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.926310">10.1117/12.926310 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LOFT: the Large Observatory For X-ray Timing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Feroci%2C+M">M. Feroci</a>, <a href="/search/astro-ph?searchtype=author&query=Herder%2C+J+W+d">J. W. den Herder</a>, <a href="/search/astro-ph?searchtype=author&query=Bozzo%2C+E">E. Bozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Barret%2C+D">D. Barret</a>, <a href="/search/astro-ph?searchtype=author&query=Brandt%2C+S">S. Brandt</a>, <a href="/search/astro-ph?searchtype=author&query=Hernanz%2C+M">M. Hernanz</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Klis%2C+M">M. van der Klis</a>, <a href="/search/astro-ph?searchtype=author&query=Pohl%2C+M">M. Pohl</a>, <a href="/search/astro-ph?searchtype=author&query=Santangelo%2C+A">A. Santangelo</a>, <a href="/search/astro-ph?searchtype=author&query=Stella%2C+L">L. Stella</a>, <a href="/search/astro-ph?searchtype=author&query=Watts%2C+A">A. Watts</a>, <a href="/search/astro-ph?searchtype=author&query=Wilms%2C+J">J. Wilms</a>, <a href="/search/astro-ph?searchtype=author&query=Zane%2C+S">S. Zane</a>, <a href="/search/astro-ph?searchtype=author&query=Ahangarianabhari%2C+M">M. Ahangarianabhari</a>, <a href="/search/astro-ph?searchtype=author&query=Alpar%2C+A">A. Alpar</a>, <a href="/search/astro-ph?searchtype=author&query=Altamirano%2C+D">D. Altamirano</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+L">L. Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Amati%2C+L">L. Amati</a>, <a href="/search/astro-ph?searchtype=author&query=Amoros%2C+C">C. Amoros</a>, <a href="/search/astro-ph?searchtype=author&query=Andersson%2C+N">N. Andersson</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+A">A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Argan%2C+A">A. Argan</a>, <a href="/search/astro-ph?searchtype=author&query=Artigue%2C+R">R. Artigue</a>, <a href="/search/astro-ph?searchtype=author&query=Azzarello%2C+P">P. Azzarello</a>, <a href="/search/astro-ph?searchtype=author&query=Baldazzi%2C+G">G. Baldazzi</a> , et al. (223 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="1209.1497v1-abstract-short" style="display: inline;"> The LOFT mission concept is one of four candidates selected by ESA for the M3 launch opportunity as Medium Size missions of the Cosmic Vision programme. The launch window is currently planned for between 2022 and 2024. LOFT is designed to exploit the diagnostics of rapid X-ray flux and spectral variability that directly probe the motion of matter down to distances very close to black holes and neu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1209.1497v1-abstract-full').style.display = 'inline'; document.getElementById('1209.1497v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1209.1497v1-abstract-full" style="display: none;"> The LOFT mission concept is one of four candidates selected by ESA for the M3 launch opportunity as Medium Size missions of the Cosmic Vision programme. The launch window is currently planned for between 2022 and 2024. LOFT is designed to exploit the diagnostics of rapid X-ray flux and spectral variability that directly probe the motion of matter down to distances very close to black holes and neutron stars, as well as the physical state of ultra-dense matter. These primary science goals will be addressed by a payload composed of a Large Area Detector (LAD) and a Wide Field Monitor (WFM). The LAD is a collimated (<1 degree field of view) experiment operating in the energy range 2-50 keV, with a 10 m^2 peak effective area and an energy resolution of 260 eV at 6 keV. The WFM will operate in the same energy range as the LAD, enabling simultaneous monitoring of a few-steradian wide field of view, with an angular resolution of <5 arcmin. The LAD and WFM experiments will allow us to investigate variability from submillisecond QPO's to year-long transient outbursts. In this paper we report the current status of the project. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1209.1497v1-abstract-full').style.display = 'none'; document.getElementById('1209.1497v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 September, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Proceedings of SPIE, Vol. 8443, Paper No. 8443-85, 2012</span> </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" 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