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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/2312.16668">arXiv:2312.16668</a> <span> [<a href="https://arxiv.org/pdf/2312.16668">pdf</a>, <a href="https://arxiv.org/format/2312.16668">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Axion Dark Matter eXperiment: Run 1A Analysis Details </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Boutan%2C+C">C. Boutan</a>, <a href="/search/physics?searchtype=author&query=LaRoque%2C+B+H">B. H. LaRoque</a>, <a href="/search/physics?searchtype=author&query=Lentz%2C+E">E. Lentz</a>, <a href="/search/physics?searchtype=author&query=Oblath%2C+N+S">N. S. Oblath</a>, <a href="/search/physics?searchtype=author&query=Taubman%2C+M+S">M. S. Taubman</a>, <a href="/search/physics?searchtype=author&query=Tedeschi%2C+J">J. Tedeschi</a>, <a href="/search/physics?searchtype=author&query=Yang%2C+J">J. Yang</a>, <a href="/search/physics?searchtype=author&query=Jones%2C+A+M">A. M. Jones</a>, <a href="/search/physics?searchtype=author&query=Braine%2C+T">T. Braine</a>, <a href="/search/physics?searchtype=author&query=Crisosto%2C+N">N. Crisosto</a>, <a href="/search/physics?searchtype=author&query=Rosenberg%2C+L+J">L. J Rosenberg</a>, <a href="/search/physics?searchtype=author&query=Rybka%2C+G">G. Rybka</a>, <a href="/search/physics?searchtype=author&query=Will%2C+D">D. Will</a>, <a href="/search/physics?searchtype=author&query=Zhang%2C+D">D. Zhang</a>, <a href="/search/physics?searchtype=author&query=Kimes%2C+S">S. Kimes</a>, <a href="/search/physics?searchtype=author&query=Ottens%2C+R">R. Ottens</a>, <a href="/search/physics?searchtype=author&query=Bartram%2C+C">C. Bartram</a>, <a href="/search/physics?searchtype=author&query=Bowring%2C+D">D. Bowring</a>, <a href="/search/physics?searchtype=author&query=Cervantes%2C+R">R. Cervantes</a>, <a href="/search/physics?searchtype=author&query=Chou%2C+A+S">A. S. Chou</a>, <a href="/search/physics?searchtype=author&query=Knirck%2C+S">S. Knirck</a>, <a href="/search/physics?searchtype=author&query=Mitchell%2C+D+V">D. V. Mitchell</a>, <a href="/search/physics?searchtype=author&query=Sonnenschein%2C+A">A. Sonnenschein</a>, <a href="/search/physics?searchtype=author&query=Wester%2C+W">W. Wester</a>, <a href="/search/physics?searchtype=author&query=Khatiwada%2C+R">R. Khatiwada</a> , et al. (28 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.16668v1-abstract-short" style="display: inline;"> The ADMX collaboration gathered data for its Run 1A axion dark matter search from January to June 2017, scanning with an axion haloscope over the frequency range 645-680 MHz (2.66-2.81 ueV in axion mass) at DFSZ sensitivity. The resulting axion search found no axion-like signals comprising all the dark matter in the form of a virialized galactic halo over the entire frequency range, implying lower… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.16668v1-abstract-full').style.display = 'inline'; document.getElementById('2312.16668v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.16668v1-abstract-full" style="display: none;"> The ADMX collaboration gathered data for its Run 1A axion dark matter search from January to June 2017, scanning with an axion haloscope over the frequency range 645-680 MHz (2.66-2.81 ueV in axion mass) at DFSZ sensitivity. The resulting axion search found no axion-like signals comprising all the dark matter in the form of a virialized galactic halo over the entire frequency range, implying lower bound exclusion limits at or below DFSZ coupling at the 90% confidence level. This paper presents expanded details of the axion search analysis of Run 1A, including review of relevant experimental systems, data-taking operations, preparation and interpretation of raw data, axion search methodology, candidate handling, and final axion limits. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.16668v1-abstract-full').style.display = 'none'; document.getElementById('2312.16668v1-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 19 figures, accepted for publication in PRD</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.07116">arXiv:2303.07116</a> <span> [<a href="https://arxiv.org/pdf/2303.07116">pdf</a>, <a href="https://arxiv.org/ps/2303.07116">ps</a>, <a href="https://arxiv.org/format/2303.07116">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Low Frequency (100-600 MHz) Searches with Axion Cavity Haloscopes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Chakrabarty%2C+S">S. Chakrabarty</a>, <a href="/search/physics?searchtype=author&query=Gleason%2C+J+R">J. R. Gleason</a>, <a href="/search/physics?searchtype=author&query=Han%2C+Y">Y. Han</a>, <a href="/search/physics?searchtype=author&query=Hipp%2C+A+T">A. T. Hipp</a>, <a href="/search/physics?searchtype=author&query=Solano%2C+M">M. Solano</a>, <a href="/search/physics?searchtype=author&query=Sikivie%2C+P">P. Sikivie</a>, <a href="/search/physics?searchtype=author&query=Sullivan%2C+N+S">N. S. Sullivan</a>, <a href="/search/physics?searchtype=author&query=Tanner%2C+D+B">D. B. Tanner</a>, <a href="/search/physics?searchtype=author&query=Goryachev%2C+M">M. Goryachev</a>, <a href="/search/physics?searchtype=author&query=Hartman%2C+E">E. Hartman</a>, <a href="/search/physics?searchtype=author&query=McAllister%2C+B+T">B. T. McAllister</a>, <a href="/search/physics?searchtype=author&query=Quiskamp%2C+A">A. Quiskamp</a>, <a href="/search/physics?searchtype=author&query=Thomson%2C+C">C. Thomson</a>, <a href="/search/physics?searchtype=author&query=Tobar%2C+M+E">M. E. Tobar</a>, <a href="/search/physics?searchtype=author&query=Awida%2C+M+H">M. H. Awida</a>, <a href="/search/physics?searchtype=author&query=Chou%2C+A+S">A. S. Chou</a>, <a href="/search/physics?searchtype=author&query=Hollister%2C+M">M. Hollister</a>, <a href="/search/physics?searchtype=author&query=Knirck%2C+S">S. Knirck</a>, <a href="/search/physics?searchtype=author&query=Sonnenschein%2C+A">A. Sonnenschein</a>, <a href="/search/physics?searchtype=author&query=Wester%2C+W">W. Wester</a>, <a href="/search/physics?searchtype=author&query=Braine%2C+T">T. Braine</a>, <a href="/search/physics?searchtype=author&query=Guzzetti%2C+M">M. Guzzetti</a>, <a href="/search/physics?searchtype=author&query=Hanretty%2C+C">C. Hanretty</a>, <a href="/search/physics?searchtype=author&query=Leum%2C+G">G. Leum</a>, <a href="/search/physics?searchtype=author&query=Rosenberg%2C+L+J">L. J Rosenberg</a> , et al. (22 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="2303.07116v2-abstract-short" style="display: inline;"> We investigate reentrant and dielectric loaded cavities for the purpose of extending the range of axion cavity haloscopes to lower masses, below the range where the Axion Dark Matter eXperiment (ADMX) has already searched. Reentrant and dielectric loaded cavities were simulated numerically to calculate and optimize their form factors and quality factors. A prototype reentrant cavity was built and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.07116v2-abstract-full').style.display = 'inline'; document.getElementById('2303.07116v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.07116v2-abstract-full" style="display: none;"> We investigate reentrant and dielectric loaded cavities for the purpose of extending the range of axion cavity haloscopes to lower masses, below the range where the Axion Dark Matter eXperiment (ADMX) has already searched. Reentrant and dielectric loaded cavities were simulated numerically to calculate and optimize their form factors and quality factors. A prototype reentrant cavity was built and its measured properties were compared with the simulations. We estimate the sensitivity of axion dark matter searches using reentrant and dielectric loaded cavities inserted in the existing ADMX magnet at the University of Washington and a large magnet being installed at Fermilab. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.07116v2-abstract-full').style.display = 'none'; document.getElementById('2303.07116v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 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">33 pages, 24 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.06096">arXiv:2110.06096</a> <span> [<a href="https://arxiv.org/pdf/2110.06096">pdf</a>, <a href="https://arxiv.org/format/2110.06096">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/10.1103/PhysRevLett.127.261803">10.1103/PhysRevLett.127.261803 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for "Invisible" Axion Dark Matter in the $3.3\text{-}4.2~渭$eV Mass Range </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=ADMX+Collaboration"> ADMX Collaboration</a>, <a href="/search/physics?searchtype=author&query=Bartram%2C+C">C. Bartram</a>, <a href="/search/physics?searchtype=author&query=Braine%2C+T">T. Braine</a>, <a href="/search/physics?searchtype=author&query=Burns%2C+E">E. Burns</a>, <a href="/search/physics?searchtype=author&query=Cervantes%2C+R">R. Cervantes</a>, <a href="/search/physics?searchtype=author&query=Crisosto%2C+N">N. Crisosto</a>, <a href="/search/physics?searchtype=author&query=Du%2C+N">N. Du</a>, <a href="/search/physics?searchtype=author&query=Korandla%2C+H">H. Korandla</a>, <a href="/search/physics?searchtype=author&query=Leum%2C+G">G. Leum</a>, <a href="/search/physics?searchtype=author&query=Mohapatra%2C+P">P. Mohapatra</a>, <a href="/search/physics?searchtype=author&query=Nitta%2C+T">T. Nitta</a>, <a href="/search/physics?searchtype=author&query=Rosenberg%2C+L+J">L. J Rosenberg</a>, <a href="/search/physics?searchtype=author&query=Rybka%2C+G">G. Rybka</a>, <a href="/search/physics?searchtype=author&query=Yang%2C+J">J. Yang</a>, <a href="/search/physics?searchtype=author&query=Clarke%2C+J">John Clarke</a>, <a href="/search/physics?searchtype=author&query=Siddiqi%2C+I">I. Siddiqi</a>, <a href="/search/physics?searchtype=author&query=Agrawal%2C+A">A. Agrawal</a>, <a href="/search/physics?searchtype=author&query=Dixit%2C+A+V">A. V. Dixit</a>, <a href="/search/physics?searchtype=author&query=Awida%2C+M+H">M. H. Awida</a>, <a href="/search/physics?searchtype=author&query=Chou%2C+A+S">A. S. Chou</a>, <a href="/search/physics?searchtype=author&query=Hollister%2C+M">M. Hollister</a>, <a href="/search/physics?searchtype=author&query=Knirck%2C+S">S. Knirck</a>, <a href="/search/physics?searchtype=author&query=Sonnenschein%2C+A">A. Sonnenschein</a>, <a href="/search/physics?searchtype=author&query=Wester%2C+W">W. Wester</a>, <a href="/search/physics?searchtype=author&query=Gleason%2C+J+R">J. R. Gleason</a> , et al. (27 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2110.06096v3-abstract-short" style="display: inline;"> We report the results from a haloscope search for axion dark matter in the $3.3\text{-}4.2~渭$eV mass range. This search excludes the axion-photon coupling predicted by one of the benchmark models of "invisible" axion dark matter, the KSVZ model. This sensitivity is achieved using a large-volume cavity, a superconducting magnet, an ultra low noise Josephson parametric amplifier, and sub-Kelvin temp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.06096v3-abstract-full').style.display = 'inline'; document.getElementById('2110.06096v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.06096v3-abstract-full" style="display: none;"> We report the results from a haloscope search for axion dark matter in the $3.3\text{-}4.2~渭$eV mass range. This search excludes the axion-photon coupling predicted by one of the benchmark models of "invisible" axion dark matter, the KSVZ model. This sensitivity is achieved using a large-volume cavity, a superconducting magnet, an ultra low noise Josephson parametric amplifier, and sub-Kelvin temperatures. The validity of our detection procedure is ensured by injecting and detecting blind synthetic axion signals. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.06096v3-abstract-full').style.display = 'none'; document.getElementById('2110.06096v3-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 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 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">6 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 127, 261803 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.08545">arXiv:2107.08545</a> <span> [<a href="https://arxiv.org/pdf/2107.08545">pdf</a>, <a href="https://arxiv.org/format/2107.08545">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div 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/s00190-022-01659-0">10.1007/s00190-022-01659-0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Simplified Gravitational Reference Sensor for Satellite Geodesy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Alvarez%2C+A+D">Anthony Davila Alvarez</a>, <a href="/search/physics?searchtype=author&query=Knudtson%2C+A">Aaron Knudtson</a>, <a href="/search/physics?searchtype=author&query=Patel%2C+U">Unmil Patel</a>, <a href="/search/physics?searchtype=author&query=Gleason%2C+J">Joseph Gleason</a>, <a href="/search/physics?searchtype=author&query=Hollis%2C+H">Harold Hollis</a>, <a href="/search/physics?searchtype=author&query=Sanjuan%2C+J">Jose Sanjuan</a>, <a href="/search/physics?searchtype=author&query=Doughty%2C+N">Neil Doughty</a>, <a href="/search/physics?searchtype=author&query=McDaniel%2C+G">Glenn McDaniel</a>, <a href="/search/physics?searchtype=author&query=Lee%2C+J">Jennifer Lee</a>, <a href="/search/physics?searchtype=author&query=Leitch%2C+J">James Leitch</a>, <a href="/search/physics?searchtype=author&query=Bennett%2C+S">Stephen Bennett</a>, <a href="/search/physics?searchtype=author&query=Bevilacqua%2C+R">Riccardo Bevilacqua</a>, <a href="/search/physics?searchtype=author&query=Mueller%2C+G">Guido Mueller</a>, <a href="/search/physics?searchtype=author&query=Spero%2C+R">Robert Spero</a>, <a href="/search/physics?searchtype=author&query=Ware%2C+B">Brent Ware</a>, <a href="/search/physics?searchtype=author&query=Wass%2C+P">Peter Wass</a>, <a href="/search/physics?searchtype=author&query=Wiese%2C+D">David Wiese</a>, <a href="/search/physics?searchtype=author&query=Ziemer%2C+J">John Ziemer</a>, <a href="/search/physics?searchtype=author&query=Conklin%2C+J+W">John W. Conklin</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="2107.08545v4-abstract-short" style="display: inline;"> We describe a Simplified Gravitational Reference Sensor (S-GRS), an ultra-precise inertial sensor for future Earth geodesy missions. These sensors are used to measure or compensate for all non-gravitational accelerations of the host spacecraft so that they can be removed in the data analysis to recover spacecraft motion due to Earth's gravity field, which is the main science observable. Low-low sa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.08545v4-abstract-full').style.display = 'inline'; document.getElementById('2107.08545v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.08545v4-abstract-full" style="display: none;"> We describe a Simplified Gravitational Reference Sensor (S-GRS), an ultra-precise inertial sensor for future Earth geodesy missions. These sensors are used to measure or compensate for all non-gravitational accelerations of the host spacecraft so that they can be removed in the data analysis to recover spacecraft motion due to Earth's gravity field, which is the main science observable. Low-low satellite-to-satellite tracking missions like GRACE-FO that utilize laser ranging interferometers are technologically limited by the acceleration noise performance of their electrostatic accelerometers, in addition to temporal aliasing associated with Earth's dynamic gravity field. The S-GRS is estimated to be at least 40 times more sensitive than the GRACE accelerometers and more than 500 times more sensitive if operated on a drag-compensated platform. The improved performance is enabled by increasing the mass of the sensor's test mass, increasing the gap between the test mass and its electrode housing, removing the small grounding wire used in the GRACE accelerometers and replacing them with a UV LED-based charge management system. This level of improvement allows future missions to fully take advantage of the sensitivity of the GRACE-FO laser Ranging Interferometer in the gravity recovery analysis. The S-GRS concept is a simplified version of the flight-proven LISA Pathfinder GRS. Our performance estimates are based on models vetted during the LISA Pathfinder flight and the expected Earth orbiting spacecraft environment based on flight data from GRACE-FO. The relatively low volume, mass, and a power consumption enables use of the S-GRS on ESPA-class microsatellites, reducing launch costs or enabling larger numbers of satellite pairs to be utilized to improve the temporal resolution of Earth gravity field maps. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.08545v4-abstract-full').style.display = 'none'; document.getElementById('2107.08545v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Corrected typos, clarified some sentences, and added references</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.02334">arXiv:2010.02334</a> <span> [<a href="https://arxiv.org/pdf/2010.02334">pdf</a>, <a href="https://arxiv.org/format/2010.02334">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Optics">physics.optics</span> </div> </div> <p class="title is-5 mathjax"> The heterodyne sensing system for the ALPS II search for sub-eV weakly interacting particles </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Hallal%2C+A">Ayman Hallal</a>, <a href="/search/physics?searchtype=author&query=Messineo%2C+G">Giuseppe Messineo</a>, <a href="/search/physics?searchtype=author&query=Ortiz%2C+M+D">Mauricio Diaz Ortiz</a>, <a href="/search/physics?searchtype=author&query=Gleason%2C+J">Joseph Gleason</a>, <a href="/search/physics?searchtype=author&query=Hollis%2C+H">Harold Hollis</a>, <a href="/search/physics?searchtype=author&query=Tanner%2C+D+B">D. B. Tanner</a>, <a href="/search/physics?searchtype=author&query=Mueller%2C+G">Guido Mueller</a>, <a href="/search/physics?searchtype=author&query=Spector%2C+A">Aaron Spector</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="2010.02334v3-abstract-short" style="display: inline;"> ALPS II, the Any Light Particle Search, is a second-generation Light Shining through a Wall experiment that hunts for axion-like particles. The experiment is currently transitioning from the design and construction phase to the commissioning phase, with science runs expected to start in 2021. ALPS II plans to use two different sensing schemes to confirm the potential detection of axion-like partic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.02334v3-abstract-full').style.display = 'inline'; document.getElementById('2010.02334v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.02334v3-abstract-full" style="display: none;"> ALPS II, the Any Light Particle Search, is a second-generation Light Shining through a Wall experiment that hunts for axion-like particles. The experiment is currently transitioning from the design and construction phase to the commissioning phase, with science runs expected to start in 2021. ALPS II plans to use two different sensing schemes to confirm the potential detection of axion-like particles or to verify an upper limit on their coupling strength to two photons of $g_{a纬纬}\leq2\times10^{-11}\text{GeV}^{-1}$. This paper discusses a heterodyne sensing scheme (HET) which will be the first scheme deployed to detect the regenerated light. It presents critical details of the optical layout, the length and alignment sensing scheme, design features to minimize spurious signals from stray light, as well as several control and veto channels specific to HET which are needed to commission and operate the instrument and to calibrate the detector sensitivity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.02334v3-abstract-full').style.display = 'none'; document.getElementById('2010.02334v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 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">12 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> DESY 20-164 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.00169">arXiv:2010.00169</a> <span> [<a href="https://arxiv.org/pdf/2010.00169">pdf</a>, <a href="https://arxiv.org/format/2010.00169">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Quantum Physics">quant-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/10.1063/5.0037857">10.1063/5.0037857 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Axion Dark Matter eXperiment: Detailed Design and Operations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Khatiwada%2C+R">R. Khatiwada</a>, <a href="/search/physics?searchtype=author&query=Bowring%2C+D">D. Bowring</a>, <a href="/search/physics?searchtype=author&query=Chou%2C+A+S">A. S. Chou</a>, <a href="/search/physics?searchtype=author&query=Sonnenschein%2C+A">A. Sonnenschein</a>, <a href="/search/physics?searchtype=author&query=Wester%2C+W">W. Wester</a>, <a href="/search/physics?searchtype=author&query=Mitchell%2C+D+V">D. V. Mitchell</a>, <a href="/search/physics?searchtype=author&query=Braine%2C+T">T. Braine</a>, <a href="/search/physics?searchtype=author&query=Bartram%2C+C">C. Bartram</a>, <a href="/search/physics?searchtype=author&query=Cervantes%2C+R">R. Cervantes</a>, <a href="/search/physics?searchtype=author&query=Crisosto%2C+N">N. Crisosto</a>, <a href="/search/physics?searchtype=author&query=Du%2C+N">N. Du</a>, <a href="/search/physics?searchtype=author&query=Kimes%2C+S">S. Kimes</a>, <a href="/search/physics?searchtype=author&query=Rosenberg%2C+L+J">L. J Rosenberg</a>, <a href="/search/physics?searchtype=author&query=Rybka%2C+G">G. Rybka</a>, <a href="/search/physics?searchtype=author&query=Yang%2C+J">J. Yang</a>, <a href="/search/physics?searchtype=author&query=Will%2C+D">D. Will</a>, <a href="/search/physics?searchtype=author&query=Carosi%2C+G">G. Carosi</a>, <a href="/search/physics?searchtype=author&query=Woollett%2C+N">N. Woollett</a>, <a href="/search/physics?searchtype=author&query=Durham%2C+S">S. Durham</a>, <a href="/search/physics?searchtype=author&query=Duffy%2C+L+D">L. D. Duffy</a>, <a href="/search/physics?searchtype=author&query=Bradley%2C+R">R. Bradley</a>, <a href="/search/physics?searchtype=author&query=Boutan%2C+C">C. Boutan</a>, <a href="/search/physics?searchtype=author&query=Jones%2C+M">M. Jones</a>, <a href="/search/physics?searchtype=author&query=LaRoque%2C+B+H">B. H. LaRoque</a>, <a href="/search/physics?searchtype=author&query=Oblath%2C+N+S">N. S. Oblath</a> , et al. (26 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="2010.00169v1-abstract-short" style="display: inline;"> Axion Dark Matter eXperiment (ADMX) ultra low noise haloscope technology has enabled the successful completion of two science runs (1A and 1B) that looked for dark matter axions in the $2.66$ to $3.1$ $渭$eV mass range with Dine-Fischler-Srednicki-Zhitnisky (DFSZ) sensitivity Ref. [1,2]. Therefore, it is the most sensitive axion search experiment to date in this mass range. We discuss the technolog… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.00169v1-abstract-full').style.display = 'inline'; document.getElementById('2010.00169v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.00169v1-abstract-full" style="display: none;"> Axion Dark Matter eXperiment (ADMX) ultra low noise haloscope technology has enabled the successful completion of two science runs (1A and 1B) that looked for dark matter axions in the $2.66$ to $3.1$ $渭$eV mass range with Dine-Fischler-Srednicki-Zhitnisky (DFSZ) sensitivity Ref. [1,2]. Therefore, it is the most sensitive axion search experiment to date in this mass range. We discuss the technological advances made in the last several years to achieve this sensitivity, which includes the implementation of components, such as state-of-the-art quantum limited amplifiers and a dilution refrigerator. Furthermore, we demonstrate the use of a frequency tunable Microstrip Superconducting Quantum Interference Device (SQUID) Amplifier (MSA), in Run 1A, and a Josephson Parametric Amplifier (JPA), in Run 1B, along with novel analysis tools that characterize the system noise temperature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.00169v1-abstract-full').style.display = 'none'; document.getElementById('2010.00169v1-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 September, 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">23 pages, 28 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-20-331-AD-E-QIS </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.14294">arXiv:2009.14294</a> <span> [<a href="https://arxiv.org/pdf/2009.14294">pdf</a>, <a href="https://arxiv.org/format/2009.14294">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Optics">physics.optics</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Design of the ALPS II Optical System </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Ortiz%2C+M+D">M. Diaz Ortiz</a>, <a href="/search/physics?searchtype=author&query=Gleason%2C+J">J. Gleason</a>, <a href="/search/physics?searchtype=author&query=Grote%2C+H">H. Grote</a>, <a href="/search/physics?searchtype=author&query=Hallal%2C+A">A. Hallal</a>, <a href="/search/physics?searchtype=author&query=Hartman%2C+M+T">M. T. Hartman</a>, <a href="/search/physics?searchtype=author&query=Hollis%2C+H">H. Hollis</a>, <a href="/search/physics?searchtype=author&query=Isleif%2C+K+S">K. S. Isleif</a>, <a href="/search/physics?searchtype=author&query=James%2C+A">A. James</a>, <a href="/search/physics?searchtype=author&query=Karan%2C+K">K. Karan</a>, <a href="/search/physics?searchtype=author&query=Kozlowski%2C+T">T. Kozlowski</a>, <a href="/search/physics?searchtype=author&query=Lindner%2C+A">A. Lindner</a>, <a href="/search/physics?searchtype=author&query=Messineo%2C+G">G. Messineo</a>, <a href="/search/physics?searchtype=author&query=Mueller%2C+G">G. Mueller</a>, <a href="/search/physics?searchtype=author&query=Poeld%2C+J+H">J. H. Poeld</a>, <a href="/search/physics?searchtype=author&query=Smith%2C+R+C+G">R. C. G. Smith</a>, <a href="/search/physics?searchtype=author&query=Spector%2C+A+D">A. D. Spector</a>, <a href="/search/physics?searchtype=author&query=Tanner%2C+D+B">D. B. Tanner</a>, <a href="/search/physics?searchtype=author&query=Wei%2C+L+-">L. -W. Wei</a>, <a href="/search/physics?searchtype=author&query=Willke%2C+B">B. Willke</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="2009.14294v4-abstract-short" style="display: inline;"> The Any Light Particle Search II (ALPS II) is an experiment currently being built at DESY in Hamburg, Germany, that will use a light-shining-through-a-wall (LSW) approach to search for axion-like particles. ALPS II represents a significant step forward for these types of experiments as it will use 24 superconducting dipole magnets, along with dual, high-finesse, 122 m long optical cavities. This p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.14294v4-abstract-full').style.display = 'inline'; document.getElementById('2009.14294v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.14294v4-abstract-full" style="display: none;"> The Any Light Particle Search II (ALPS II) is an experiment currently being built at DESY in Hamburg, Germany, that will use a light-shining-through-a-wall (LSW) approach to search for axion-like particles. ALPS II represents a significant step forward for these types of experiments as it will use 24 superconducting dipole magnets, along with dual, high-finesse, 122 m long optical cavities. This paper gives the first comprehensive recipe for the realization of the idea, proposed over 30 years ago, to use optical cavities before and after the wall to increase the power of the regenerated photon signal. The experiment is designed to achieve a sensitivity to the coupling between axion-like particles and photons down to g=2e-11 1/GeV for masses below 0.1 meV, more than three orders of magnitude beyond the sensitivity of previous laboratory experiments. The layout and main components that define ALPS II are discussed along with plans for reaching design sensitivity. An accompanying paper (Hallal, et al [1]) offers a more in-depth description of the heterodyne detection scheme, the first of two independent detection systems that will be implemented in ALPS II. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.14294v4-abstract-full').style.display = 'none'; document.getElementById('2009.14294v4-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 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> DESY 20-158 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1910.08638">arXiv:1910.08638</a> <span> [<a href="https://arxiv.org/pdf/1910.08638">pdf</a>, <a href="https://arxiv.org/format/1910.08638">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/10.1103/PhysRevLett.124.101303">10.1103/PhysRevLett.124.101303 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Extended Search for the Invisible Axion with the Axion Dark Matter Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Braine%2C+T">T. Braine</a>, <a href="/search/physics?searchtype=author&query=Cervantes%2C+R">R. Cervantes</a>, <a href="/search/physics?searchtype=author&query=Crisosto%2C+N">N. Crisosto</a>, <a href="/search/physics?searchtype=author&query=Du%2C+N">N. Du</a>, <a href="/search/physics?searchtype=author&query=Kimes%2C+S">S. Kimes</a>, <a href="/search/physics?searchtype=author&query=Rosenberg%2C+L+J">L. J Rosenberg</a>, <a href="/search/physics?searchtype=author&query=Rybka%2C+G">G. Rybka</a>, <a href="/search/physics?searchtype=author&query=Yang%2C+J">J. Yang</a>, <a href="/search/physics?searchtype=author&query=Bowring%2C+D">D. Bowring</a>, <a href="/search/physics?searchtype=author&query=Chou%2C+A+S">A. S. Chou</a>, <a href="/search/physics?searchtype=author&query=Khatiwada%2C+R">R. Khatiwada</a>, <a href="/search/physics?searchtype=author&query=Sonnenschein%2C+A">A. Sonnenschein</a>, <a href="/search/physics?searchtype=author&query=Wester%2C+W">W. Wester</a>, <a href="/search/physics?searchtype=author&query=Carosi%2C+G">G. Carosi</a>, <a href="/search/physics?searchtype=author&query=Woollett%2C+N">N. Woollett</a>, <a href="/search/physics?searchtype=author&query=Duffy%2C+L+D">L. D. Duffy</a>, <a href="/search/physics?searchtype=author&query=Bradley%2C+R">R. Bradley</a>, <a href="/search/physics?searchtype=author&query=Boutan%2C+C">C. Boutan</a>, <a href="/search/physics?searchtype=author&query=Jones%2C+M">M. Jones</a>, <a href="/search/physics?searchtype=author&query=LaRoque%2C+B+H">B. H. LaRoque</a>, <a href="/search/physics?searchtype=author&query=Oblath%2C+N+S">N. S. Oblath</a>, <a href="/search/physics?searchtype=author&query=Taubman%2C+M+S">M. S. Taubman</a>, <a href="/search/physics?searchtype=author&query=Clarke%2C+J">J. Clarke</a>, <a href="/search/physics?searchtype=author&query=Dove%2C+A">A. Dove</a>, <a href="/search/physics?searchtype=author&query=Eddins%2C+A">A. Eddins</a> , et al. (17 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="1910.08638v3-abstract-short" style="display: inline;"> This paper reports on a cavity haloscope search for dark matter axions in the galactic halo in the mass range $2.81$-$3.31$ $渭eV$. This search excludes the full range of axion-photon coupling values predicted in benchmark models of the invisible axion that solve the strong CP problem of quantum chromodynamics, and marks the first time a haloscope search has been able to search for axions at mode c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.08638v3-abstract-full').style.display = 'inline'; document.getElementById('1910.08638v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.08638v3-abstract-full" style="display: none;"> This paper reports on a cavity haloscope search for dark matter axions in the galactic halo in the mass range $2.81$-$3.31$ $渭eV$. This search excludes the full range of axion-photon coupling values predicted in benchmark models of the invisible axion that solve the strong CP problem of quantum chromodynamics, and marks the first time a haloscope search has been able to search for axions at mode crossings using an alternate cavity configuration. Unprecedented sensitivity in this higher mass range is achieved by deploying an ultra low-noise Josephson parametric amplifier as the first stage signal amplifier. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.08638v3-abstract-full').style.display = 'none'; document.getElementById('1910.08638v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 124, 101303 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1901.00920">arXiv:1901.00920</a> <span> [<a href="https://arxiv.org/pdf/1901.00920">pdf</a>, <a href="https://arxiv.org/format/1901.00920">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/10.1103/PhysRevLett.121.261302">10.1103/PhysRevLett.121.261302 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Piezoelectrically Tuned Multimode Cavity Search for Axion Dark Matter </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Boutan%2C+C">C. Boutan</a>, <a href="/search/physics?searchtype=author&query=Jones%2C+M">M. Jones</a>, <a href="/search/physics?searchtype=author&query=LaRoque%2C+B+H">B. H. LaRoque</a>, <a href="/search/physics?searchtype=author&query=Oblath%2C+N+S">N. S. Oblath</a>, <a href="/search/physics?searchtype=author&query=Cervantes%2C+R">R. Cervantes</a>, <a href="/search/physics?searchtype=author&query=Du%2C+N">N. Du</a>, <a href="/search/physics?searchtype=author&query=Force%2C+N">N. Force</a>, <a href="/search/physics?searchtype=author&query=Kimes%2C+S">S. Kimes</a>, <a href="/search/physics?searchtype=author&query=Ottens%2C+R">R. Ottens</a>, <a href="/search/physics?searchtype=author&query=Rosenberg%2C+L+J">L. J. Rosenberg</a>, <a href="/search/physics?searchtype=author&query=Rybka%2C+G">G. Rybka</a>, <a href="/search/physics?searchtype=author&query=Yang%2C+J">J. Yang</a>, <a href="/search/physics?searchtype=author&query=Carosi%2C+G">G. Carosi</a>, <a href="/search/physics?searchtype=author&query=Woollett%2C+N">N. Woollett</a>, <a href="/search/physics?searchtype=author&query=Bowring%2C+D">D. Bowring</a>, <a href="/search/physics?searchtype=author&query=Chou%2C+A+S">A. S. Chou</a>, <a href="/search/physics?searchtype=author&query=Khatiwada%2C+R">R. Khatiwada</a>, <a href="/search/physics?searchtype=author&query=Sonnenschein%2C+A">A. Sonnenschein</a>, <a href="/search/physics?searchtype=author&query=Wester%2C+W">W. Wester</a>, <a href="/search/physics?searchtype=author&query=Bradley%2C+R">R. Bradley</a>, <a href="/search/physics?searchtype=author&query=Daw%2C+E+J">E. J. Daw</a>, <a href="/search/physics?searchtype=author&query=Agrawal%2C+A">A. Agrawal</a>, <a href="/search/physics?searchtype=author&query=Dixit%2C+A+V">A. V. Dixit</a>, <a href="/search/physics?searchtype=author&query=Clarke%2C+J">J. Clarke</a>, <a href="/search/physics?searchtype=author&query=O%27Kelley%2C+S+R">S. R. O'Kelley</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="1901.00920v1-abstract-short" style="display: inline;"> The $渭$eV axion is a well-motivated extension to the standard model. The Axion Dark Matter eXperiment (ADMX) collaboration seeks to discover this particle by looking for the resonant conversion of dark-matter axions to microwave photons in a strong magnetic field. In this Letter, we report results from a pathfinder experiment, the ADMX "Sidecar," which is designed to pave the way for future, highe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.00920v1-abstract-full').style.display = 'inline'; document.getElementById('1901.00920v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.00920v1-abstract-full" style="display: none;"> The $渭$eV axion is a well-motivated extension to the standard model. The Axion Dark Matter eXperiment (ADMX) collaboration seeks to discover this particle by looking for the resonant conversion of dark-matter axions to microwave photons in a strong magnetic field. In this Letter, we report results from a pathfinder experiment, the ADMX "Sidecar," which is designed to pave the way for future, higher mass, searches. This testbed experiment lives inside of and operates in tandem with the main ADMX experiment. The Sidecar experiment excludes masses in three widely spaced frequency ranges (4202-4249, 5086-5799, and 7173-7203 MHz). In addition, Sidecar demonstrates the successful use of a piezoelectric actuator for cavity tuning. Finally, this publication is the first to report data measured using both the TM$_{010}$ and TM$_{020}$ modes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.00920v1-abstract-full').style.display = 'none'; document.getElementById('1901.00920v1-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 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">7 Pages, 4 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 121 (2018) 261302 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1804.05750">arXiv:1804.05750</a> <span> [<a href="https://arxiv.org/pdf/1804.05750">pdf</a>, <a href="https://arxiv.org/format/1804.05750">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/10.1103/PhysRevLett.120.151301">10.1103/PhysRevLett.120.151301 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Search for Invisible Axion Dark Matter with the Axion Dark Matter Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Du%2C+N">N. Du</a>, <a href="/search/physics?searchtype=author&query=Force%2C+N">N. Force</a>, <a href="/search/physics?searchtype=author&query=Khatiwada%2C+R">R. Khatiwada</a>, <a href="/search/physics?searchtype=author&query=Lentz%2C+E">E. Lentz</a>, <a href="/search/physics?searchtype=author&query=Ottens%2C+R">R. Ottens</a>, <a href="/search/physics?searchtype=author&query=Rosenberg%2C+L+J">L. J Rosenberg</a>, <a href="/search/physics?searchtype=author&query=Rybka%2C+G">G. Rybka</a>, <a href="/search/physics?searchtype=author&query=Carosi%2C+G">G. Carosi</a>, <a href="/search/physics?searchtype=author&query=Woolett%2C+N">N. Woolett</a>, <a href="/search/physics?searchtype=author&query=Bowring%2C+D">D. Bowring</a>, <a href="/search/physics?searchtype=author&query=Chou%2C+A+S">A. S. Chou</a>, <a href="/search/physics?searchtype=author&query=Sonnenschein%2C+A">A. Sonnenschein</a>, <a href="/search/physics?searchtype=author&query=Wester%2C+W">W. Wester</a>, <a href="/search/physics?searchtype=author&query=Boutan%2C+C">C. Boutan</a>, <a href="/search/physics?searchtype=author&query=Oblath%2C+N+S">N. S. Oblath</a>, <a href="/search/physics?searchtype=author&query=Bradley%2C+R">R. Bradley</a>, <a href="/search/physics?searchtype=author&query=Daw%2C+E+J">E. J. Daw</a>, <a href="/search/physics?searchtype=author&query=Dixit%2C+A+V">A. V. Dixit</a>, <a href="/search/physics?searchtype=author&query=Clarke%2C+J">J. Clarke</a>, <a href="/search/physics?searchtype=author&query=O%27Kelley%2C+S+R">S. R. O'Kelley</a>, <a href="/search/physics?searchtype=author&query=Crisosto%2C+N">N. Crisosto</a>, <a href="/search/physics?searchtype=author&query=Gleason%2C+J+R">J. R. Gleason</a>, <a href="/search/physics?searchtype=author&query=Jois%2C+S">S. Jois</a>, <a href="/search/physics?searchtype=author&query=Sikivie%2C+P">P. Sikivie</a>, <a href="/search/physics?searchtype=author&query=Stern%2C+I">I. Stern</a> , et al. (3 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="1804.05750v2-abstract-short" style="display: inline;"> This Letter reports results from a haloscope search for dark matter axions with masses between 2.66 and 2.81 $渭$eV. The search excludes the range of axion-photon couplings predicted by plausible models of the invisible axion. This unprecedented sensitivity is achieved by operating a large-volume haloscope at sub-kelvin temperatures, thereby reducing thermal noise as well as the excess noise from t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.05750v2-abstract-full').style.display = 'inline'; document.getElementById('1804.05750v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1804.05750v2-abstract-full" style="display: none;"> This Letter reports results from a haloscope search for dark matter axions with masses between 2.66 and 2.81 $渭$eV. The search excludes the range of axion-photon couplings predicted by plausible models of the invisible axion. This unprecedented sensitivity is achieved by operating a large-volume haloscope at sub-kelvin temperatures, thereby reducing thermal noise as well as the excess noise from the ultra-low-noise SQUID amplifier used for the signal power readout. Ongoing searches will provide nearly definitive tests of the invisible axion model over a wide range of axion masses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.05750v2-abstract-full').style.display = 'none'; document.getElementById('1804.05750v2-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 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">5 pages, 4 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 120, 151301 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1608.05055">arXiv:1608.05055</a> <span> [<a href="https://arxiv.org/pdf/1608.05055">pdf</a>, <a href="https://arxiv.org/format/1608.05055">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/10.1063/1.4967303">10.1063/1.4967303 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Advanced LIGO Photon Calibrators </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Karki%2C+S">S. Karki</a>, <a href="/search/physics?searchtype=author&query=Tuyenbayev%2C+D">D. Tuyenbayev</a>, <a href="/search/physics?searchtype=author&query=Kandhasamy%2C+S">S. Kandhasamy</a>, <a href="/search/physics?searchtype=author&query=Abbott%2C+B+P">B. P. Abbott</a>, <a href="/search/physics?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/physics?searchtype=author&query=Anders%2C+E+H">E. H. Anders</a>, <a href="/search/physics?searchtype=author&query=Berliner%2C+J">J. Berliner</a>, <a href="/search/physics?searchtype=author&query=Betzwieser%2C+J">J. Betzwieser</a>, <a href="/search/physics?searchtype=author&query=Daveloza%2C+H+P">H. P. Daveloza</a>, <a href="/search/physics?searchtype=author&query=Cahillane%2C+C">C. Cahillane</a>, <a href="/search/physics?searchtype=author&query=Canete%2C+L">L. Canete</a>, <a href="/search/physics?searchtype=author&query=Conley%2C+C">C. Conley</a>, <a href="/search/physics?searchtype=author&query=Gleason%2C+J+R">J. R. Gleason</a>, <a href="/search/physics?searchtype=author&query=Goetz%2C+E">E. Goetz</a>, <a href="/search/physics?searchtype=author&query=Kissel%2C+J+S">J. S. Kissel</a>, <a href="/search/physics?searchtype=author&query=Izumi%2C+K">K. Izumi</a>, <a href="/search/physics?searchtype=author&query=Mendell%2C+G">G. Mendell</a>, <a href="/search/physics?searchtype=author&query=Quetschke%2C+V">V. Quetschke</a>, <a href="/search/physics?searchtype=author&query=Rodruck%2C+M">M. Rodruck</a>, <a href="/search/physics?searchtype=author&query=Sachdev%2C+S">S. Sachdev</a>, <a href="/search/physics?searchtype=author&query=Sadecki%2C+T">T. Sadecki</a>, <a href="/search/physics?searchtype=author&query=Schwinberg%2C+P+B">P. B. Schwinberg</a>, <a href="/search/physics?searchtype=author&query=Sottile%2C+A">A. Sottile</a>, <a href="/search/physics?searchtype=author&query=Wade%2C+M">M. Wade</a>, <a href="/search/physics?searchtype=author&query=Weinstein%2C+A+J">A. J. Weinstein</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="1608.05055v1-abstract-short" style="display: inline;"> The two interferometers of the Laser Interferometry Gravitaional-wave Observatory (LIGO) recently detected gravitational waves from the mergers of binary black hole systems. Accurate calibration of the output of these detectors was crucial for the observation of these events, and the extraction of parameters of the sources. The principal tools used to calibrate the responses of the second-generati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.05055v1-abstract-full').style.display = 'inline'; document.getElementById('1608.05055v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1608.05055v1-abstract-full" style="display: none;"> The two interferometers of the Laser Interferometry Gravitaional-wave Observatory (LIGO) recently detected gravitational waves from the mergers of binary black hole systems. Accurate calibration of the output of these detectors was crucial for the observation of these events, and the extraction of parameters of the sources. The principal tools used to calibrate the responses of the second-generation (Advanced) LIGO detectors to gravitational waves are systems based on radiation pressure and referred to as Photon Calibrators. These systems, which were completely redesigned for Advanced LIGO, include several significant upgrades that enable them to meet the calibration requirements of second-generation gravitational wave detectors in the new era of gravitational-wave astronomy. We report on the design, implementation, and operation of these Advanced LIGO Photon Calibrators that are currently providing fiducial displacements on the order of $10^{-18}$ m/$\sqrt{\textrm{Hz}}$ with accuracy and precision of better than 1 %. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.05055v1-abstract-full').style.display = 'none'; document.getElementById('1608.05055v1-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 August, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">14 pages, 19 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1606.09159">arXiv:1606.09159</a> <span> [<a href="https://arxiv.org/pdf/1606.09159">pdf</a>, <a href="https://arxiv.org/format/1606.09159">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div 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/10.1063/1.4967716">10.1063/1.4967716 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Small optic suspensions for Advanced LIGO input optics and other precision optical experiments </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Ciani%2C+G">G. Ciani</a>, <a href="/search/physics?searchtype=author&query=Arain%2C+M+A">M. A. Arain</a>, <a href="/search/physics?searchtype=author&query=Aston%2C+S+M">S. M. Aston</a>, <a href="/search/physics?searchtype=author&query=Feldbaum%2C+D">D. Feldbaum</a>, <a href="/search/physics?searchtype=author&query=Fulda%2C+P">P. Fulda</a>, <a href="/search/physics?searchtype=author&query=Gleason%2C+J">J. Gleason</a>, <a href="/search/physics?searchtype=author&query=Heintze%2C+M">M. Heintze</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+R+M">R. M. Martin</a>, <a href="/search/physics?searchtype=author&query=Mueller%2C+C+L">C. L. Mueller</a>, <a href="/search/physics?searchtype=author&query=Kumar%2C+D+M+N">D. M. Nanda Kumar</a>, <a href="/search/physics?searchtype=author&query=Pele%2C+A">A. Pele</a>, <a href="/search/physics?searchtype=author&query=Reitze%2C+D+H">D. H. Reitze</a>, <a href="/search/physics?searchtype=author&query=Sainathan%2C+P">P. Sainathan</a>, <a href="/search/physics?searchtype=author&query=Tanner%2C+D+B">D. B. Tanner</a>, <a href="/search/physics?searchtype=author&query=Williams%2C+L+F">L. F. Williams</a>, <a href="/search/physics?searchtype=author&query=Mueller%2C+G">G. Mueller</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="1606.09159v1-abstract-short" style="display: inline;"> We report on the design and performance of small optic suspensions developed to suppress seismic motion of out-of-cavity optics in the Input Optics subsystem of the Advanced LIGO interferometric gravitational wave detector. These compact single stage suspensions provide isolation in all six degrees of freedom of the optic, local sensing and actuation in three of them, and passive damping for the o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.09159v1-abstract-full').style.display = 'inline'; document.getElementById('1606.09159v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1606.09159v1-abstract-full" style="display: none;"> We report on the design and performance of small optic suspensions developed to suppress seismic motion of out-of-cavity optics in the Input Optics subsystem of the Advanced LIGO interferometric gravitational wave detector. These compact single stage suspensions provide isolation in all six degrees of freedom of the optic, local sensing and actuation in three of them, and passive damping for the other three. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.09159v1-abstract-full').style.display = 'none'; document.getElementById('1606.09159v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 June, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P1600178 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1604.00439">arXiv:1604.00439</a> <span> [<a href="https://arxiv.org/pdf/1604.00439">pdf</a>, <a href="https://arxiv.org/format/1604.00439">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/10.1103/PhysRevD.93.112004">10.1103/PhysRevD.93.112004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Sensitivity of the Advanced LIGO Detectors at the Beginning of Gravitational Wave Astronomy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Martynov%2C+D+V">D. V. Martynov</a>, <a href="/search/physics?searchtype=author&query=Hall%2C+E+D">E. D. Hall</a>, <a href="/search/physics?searchtype=author&query=Abbott%2C+B+P">B. P. Abbott</a>, <a href="/search/physics?searchtype=author&query=Abbott%2C+R">R. Abbott</a>, <a href="/search/physics?searchtype=author&query=Abbott%2C+T+D">T. D. Abbott</a>, <a href="/search/physics?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/physics?searchtype=author&query=Adhikari%2C+R+X">R. X. Adhikari</a>, <a href="/search/physics?searchtype=author&query=Anderson%2C+R+A">R. A. Anderson</a>, <a href="/search/physics?searchtype=author&query=Anderson%2C+S+B">S. B. Anderson</a>, <a href="/search/physics?searchtype=author&query=Arai%2C+K">K. Arai</a>, <a href="/search/physics?searchtype=author&query=Arain%2C+M+A">M. A. Arain</a>, <a href="/search/physics?searchtype=author&query=Aston%2C+S+M">S. M. Aston</a>, <a href="/search/physics?searchtype=author&query=Austin%2C+L">L. Austin</a>, <a href="/search/physics?searchtype=author&query=Ballmer%2C+S+W">S. W. Ballmer</a>, <a href="/search/physics?searchtype=author&query=Barbet%2C+M">M. Barbet</a>, <a href="/search/physics?searchtype=author&query=Barker%2C+D">D. Barker</a>, <a href="/search/physics?searchtype=author&query=Barr%2C+B">B. Barr</a>, <a href="/search/physics?searchtype=author&query=Barsotti%2C+L">L. Barsotti</a>, <a href="/search/physics?searchtype=author&query=Bartlett%2C+J">J. Bartlett</a>, <a href="/search/physics?searchtype=author&query=Barton%2C+M+A">M. A. Barton</a>, <a href="/search/physics?searchtype=author&query=Bartos%2C+I">I. Bartos</a>, <a href="/search/physics?searchtype=author&query=Batch%2C+J+C">J. C. Batch</a>, <a href="/search/physics?searchtype=author&query=Bell%2C+A+S">A. S. Bell</a>, <a href="/search/physics?searchtype=author&query=Belopolski%2C+I">I. Belopolski</a>, <a href="/search/physics?searchtype=author&query=Bergman%2C+J">J. Bergman</a> , et al. (239 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1604.00439v3-abstract-short" style="display: inline;"> The Laser Interferometer Gravitational Wave Observatory (LIGO) consists of two widely separated 4 km laser interferometers designed to detect gravitational waves from distant astrophysical sources in the frequency range from 10 Hz to 10 kHz. The first observation run of the Advanced LIGO detectors started in September 2015 and ended in January 2016. A strain sensitivity of better than… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.00439v3-abstract-full').style.display = 'inline'; document.getElementById('1604.00439v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1604.00439v3-abstract-full" style="display: none;"> The Laser Interferometer Gravitational Wave Observatory (LIGO) consists of two widely separated 4 km laser interferometers designed to detect gravitational waves from distant astrophysical sources in the frequency range from 10 Hz to 10 kHz. The first observation run of the Advanced LIGO detectors started in September 2015 and ended in January 2016. A strain sensitivity of better than $10^{-23}/\sqrt{\text{Hz}}$ was achieved around 100 Hz. Understanding both the fundamental and the technical noise sources was critical for increasing the observable volume in the universe. The average distance at which coalescing binary black hole systems with individual masses of 30 $M_\odot$ could be detected was 1.3 Gpc. Similarly, the range for binary neutron star inspirals was about 75 Mpc. With respect to the initial detectors, the observable volume of Universe increased respectively by a factor 69 and 43. These improvements allowed Advanced LIGO to detect the gravitational wave signal from the binary black hole coalescence, known as GW150914. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.00439v3-abstract-full').style.display = 'none'; document.getElementById('1604.00439v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 93, 112004 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1601.05442">arXiv:1601.05442</a> <span> [<a href="https://arxiv.org/pdf/1601.05442">pdf</a>, <a href="https://arxiv.org/format/1601.05442">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1063/1.4936974">10.1063/1.4936974 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Advanced LIGO Input Optics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Mueller%2C+C">Chris Mueller</a>, <a href="/search/physics?searchtype=author&query=Arain%2C+M">Muzammil Arain</a>, <a href="/search/physics?searchtype=author&query=Ciani%2C+G">Giacomo Ciani</a>, <a href="/search/physics?searchtype=author&query=DeRosa%2C+R">Ryan DeRosa</a>, <a href="/search/physics?searchtype=author&query=Effler%2C+A">Anamaria Effler</a>, <a href="/search/physics?searchtype=author&query=Feldbaum%2C+D">David Feldbaum</a>, <a href="/search/physics?searchtype=author&query=Frolov%2C+V">Valery Frolov</a>, <a href="/search/physics?searchtype=author&query=Fulda%2C+P">Paul Fulda</a>, <a href="/search/physics?searchtype=author&query=Gleason%2C+J">Joseph Gleason</a>, <a href="/search/physics?searchtype=author&query=Heintze%2C+M">Matthew Heintze</a>, <a href="/search/physics?searchtype=author&query=King%2C+E">Eleanor King</a>, <a href="/search/physics?searchtype=author&query=Kokeyama%2C+K">Keiko Kokeyama</a>, <a href="/search/physics?searchtype=author&query=Korth%2C+W">William Korth</a>, <a href="/search/physics?searchtype=author&query=Martin%2C+R">Rodica Martin</a>, <a href="/search/physics?searchtype=author&query=Mullavey%2C+A">Adam Mullavey</a>, <a href="/search/physics?searchtype=author&query=Poeld%2C+J">Jan Poeld</a>, <a href="/search/physics?searchtype=author&query=Quetschke%2C+V">Volker Quetschke</a>, <a href="/search/physics?searchtype=author&query=Reitze%2C+D">David Reitze</a>, <a href="/search/physics?searchtype=author&query=Tanner%2C+D">David Tanner</a>, <a href="/search/physics?searchtype=author&query=Williams%2C+L">Luke Williams</a>, <a href="/search/physics?searchtype=author&query=Mueller%2C+G">Guido Mueller</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="1601.05442v1-abstract-short" style="display: inline;"> The Advanced LIGO gravitational wave detectors are nearing their design sensitivity and should begin taking meaningful astrophysical data in the fall of 2015. These resonant optical interferometers will have unprecedented sensitivity to the strains caused by passing gravitational waves. The input optics play a significant part in allowing these devices to reach such sensitivities. Residing between… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1601.05442v1-abstract-full').style.display = 'inline'; document.getElementById('1601.05442v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1601.05442v1-abstract-full" style="display: none;"> The Advanced LIGO gravitational wave detectors are nearing their design sensitivity and should begin taking meaningful astrophysical data in the fall of 2015. These resonant optical interferometers will have unprecedented sensitivity to the strains caused by passing gravitational waves. The input optics play a significant part in allowing these devices to reach such sensitivities. Residing between the pre-stabilized laser and the main interferometer, the input optics is tasked with preparing the laser beam for interferometry at the sub-attometer level while operating at continuous wave input power levels ranging from 100 mW to 150 W. These extreme operating conditions required every major component to be custom designed. These designs draw heavily on the experience and understanding gained during the operation of Initial LIGO and Enhanced LIGO. In this article we report on how the components of the input optics were designed to meet their stringent requirements and present measurements showing how well they have lived up to their design. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1601.05442v1-abstract-full').style.display = 'none'; document.getElementById('1601.05442v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 January, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2016. </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div 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