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</div> <div class="control"> <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/2411.13402">arXiv:2411.13402</a> <span> [<a href="https://arxiv.org/pdf/2411.13402">pdf</a>, <a href="https://arxiv.org/format/2411.13402">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</span> </div> </div> <p class="title is-5 mathjax"> Extraction of gravitational wave signals from LISA data in the presence of artifacts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Castelli%2C+E">Eleonora Castelli</a>, <a href="/search/astro-ph?searchtype=author&query=Baghi%2C+Q">Quentin Baghi</a>, <a href="/search/astro-ph?searchtype=author&query=Baker%2C+J+G">John G. Baker</a>, <a href="/search/astro-ph?searchtype=author&query=Slutsky%2C+J">Jacob Slutsky</a>, <a href="/search/astro-ph?searchtype=author&query=Bobin%2C+J">J茅r么me Bobin</a>, <a href="/search/astro-ph?searchtype=author&query=Karnesis%2C+N">Nikolaos Karnesis</a>, <a href="/search/astro-ph?searchtype=author&query=Petiteau%2C+A">Antoine Petiteau</a>, <a href="/search/astro-ph?searchtype=author&query=Sauter%2C+O">Orion Sauter</a>, <a href="/search/astro-ph?searchtype=author&query=Wass%2C+P">Peter Wass</a>, <a href="/search/astro-ph?searchtype=author&query=Weber%2C+W+J">William J. Weber</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.13402v2-abstract-short" style="display: inline;"> The Laser Interferometer Space Antenna (LISA) mission is being developed by ESA with NASA participation. As it has recently passed the Mission Adoption milestone, models of the instruments and noise performance are becoming more detailed, and likewise prototype data analyses must as well. Assumptions such as Gaussianity, stationarity, and data continuity are unrealistic, and must be replaced with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.13402v2-abstract-full').style.display = 'inline'; document.getElementById('2411.13402v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.13402v2-abstract-full" style="display: none;"> The Laser Interferometer Space Antenna (LISA) mission is being developed by ESA with NASA participation. As it has recently passed the Mission Adoption milestone, models of the instruments and noise performance are becoming more detailed, and likewise prototype data analyses must as well. Assumptions such as Gaussianity, stationarity, and data continuity are unrealistic, and must be replaced with physically motivated data simulations, and data analysis methods adapted to accommodate such likely imperfections. To this end, the LISA Data Challenges have produced datasets featuring time-varying and unequal constellation armlength, and measurement artifacts including data interruptions and instrumental transients. In this work, we assess the impact of these data artifacts on the inference of Galactic Binary and Massive Black Hole properties. Our analysis shows that the treatment of noise transients and gaps is necessary for effective parameter estimation, as they substantially corrupt the analysis if unmitigated. We find that straightforward mitigation techniques can significantly if imperfectly suppress artifacts. For the Galactic Binaries, mitigation of glitches was essentially total, while mitigations of the data gaps increased parameter uncertainty by approximately 10%. For the Massive Black Hole binaries the particularly pernicious glitches resulted in a 30% uncertainty increase after mitigations, while the data gaps can increase parameter uncertainty by up to several times. Critically, this underlines the importance of early detection of transient gravitational waves to ensure they are protected from planned data interruptions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.13402v2-abstract-full').style.display = 'none'; document.getElementById('2411.13402v2-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 15 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.05852">arXiv:2407.05852</a> <span> [<a href="https://arxiv.org/pdf/2407.05852">pdf</a>, <a href="https://arxiv.org/format/2407.05852">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/10.1103/PhysRevD.110.063005">10.1103/PhysRevD.110.063005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Tilt-to-length coupling in LISA Pathfinder: long-term stability </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Armano%2C+M">M Armano</a>, <a href="/search/astro-ph?searchtype=author&query=Audley%2C+H">H Audley</a>, <a href="/search/astro-ph?searchtype=author&query=Baird%2C+J">J Baird</a>, <a href="/search/astro-ph?searchtype=author&query=Binetruy%2C+P">P Binetruy</a>, <a href="/search/astro-ph?searchtype=author&query=Born%2C+M">M Born</a>, <a href="/search/astro-ph?searchtype=author&query=Bortoluzzi%2C+D">D Bortoluzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Castelli%2C+E">E Castelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cavalleri%2C+A">A Cavalleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cesarini%2C+A">A Cesarini</a>, <a href="/search/astro-ph?searchtype=author&query=Cruise%2C+A+M">A M Cruise</a>, <a href="/search/astro-ph?searchtype=author&query=Danzmann%2C+K">K Danzmann</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+M+d+D">M de Deus Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Diepholz%2C+I">I Diepholz</a>, <a href="/search/astro-ph?searchtype=author&query=Dixon%2C+G">G Dixon</a>, <a href="/search/astro-ph?searchtype=author&query=Dolesi%2C+R">R Dolesi</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraioli%2C+L">L Ferraioli</a>, <a href="/search/astro-ph?searchtype=author&query=Ferroni%2C+V">V Ferroni</a>, <a href="/search/astro-ph?searchtype=author&query=Fitzsimons%2C+E+D">E D Fitzsimons</a>, <a href="/search/astro-ph?searchtype=author&query=Freschi%2C+M">M Freschi</a>, <a href="/search/astro-ph?searchtype=author&query=Gesa%2C+L">L Gesa</a>, <a href="/search/astro-ph?searchtype=author&query=Giardini%2C+D">D Giardini</a>, <a href="/search/astro-ph?searchtype=author&query=Gibert%2C+F">F Gibert</a>, <a href="/search/astro-ph?searchtype=author&query=Giusteri%2C+R">R Giusteri</a>, <a href="/search/astro-ph?searchtype=author&query=Grimani%2C+C">C Grimani</a>, <a href="/search/astro-ph?searchtype=author&query=Grzymisch%2C+J">J Grzymisch</a> , et al. (53 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.05852v1-abstract-short" style="display: inline;"> The tilt-to-length coupling during the LISA Pathfinder mission has been numerically and analytically modeled for particular timespans. In this work, we investigate the long-term stability of the coupling coefficients of this noise. We show that they drifted slowly (by 1\,$渭$m/rad and 6$\times10^{-6}$ in 100 days) and strongly correlated to temperature changes within the satellite (8\,$渭$m/rad/K an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.05852v1-abstract-full').style.display = 'inline'; document.getElementById('2407.05852v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.05852v1-abstract-full" style="display: none;"> The tilt-to-length coupling during the LISA Pathfinder mission has been numerically and analytically modeled for particular timespans. In this work, we investigate the long-term stability of the coupling coefficients of this noise. We show that they drifted slowly (by 1\,$渭$m/rad and 6$\times10^{-6}$ in 100 days) and strongly correlated to temperature changes within the satellite (8\,$渭$m/rad/K and 30$\times10^{-6}$/K). Based on analytical TTL coupling models, we attribute the temperature-driven coupling changes to rotations of the test masses and small distortions in the optical setup. Particularly, we show that LISA Pathfinder's optical baseplate was bent during the cooldown experiment, which started in late 2016 and lasted several months. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.05852v1-abstract-full').style.display = 'none'; document.getElementById('2407.05852v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.04431">arXiv:2407.04431</a> <span> [<a href="https://arxiv.org/pdf/2407.04431">pdf</a>, <a href="https://arxiv.org/format/2407.04431">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="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.111.042007">10.1103/PhysRevD.111.042007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Precision measurements of the magnetic parameters of LISA Pathfinder test masses </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Armano%2C+M">M Armano</a>, <a href="/search/astro-ph?searchtype=author&query=Audley%2C+H">H Audley</a>, <a href="/search/astro-ph?searchtype=author&query=Baird%2C+J">J Baird</a>, <a href="/search/astro-ph?searchtype=author&query=Binetruy%2C+P">P Binetruy</a>, <a href="/search/astro-ph?searchtype=author&query=Born%2C+M">M Born</a>, <a href="/search/astro-ph?searchtype=author&query=Bortoluzzi%2C+D">D Bortoluzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Castelli%2C+E">E Castelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cavalleri%2C+A">A Cavalleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cesarini%2C+A">A Cesarini</a>, <a href="/search/astro-ph?searchtype=author&query=Cruise%2C+A+M">A M Cruise</a>, <a href="/search/astro-ph?searchtype=author&query=Danzmann%2C+K">K Danzmann</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+M+D+D">M De Deus Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Diepholz%2C+I">I Diepholz</a>, <a href="/search/astro-ph?searchtype=author&query=Dixon%2C+G">G Dixon</a>, <a href="/search/astro-ph?searchtype=author&query=Dolesi%2C+R">R Dolesi</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraioli%2C+L">L Ferraioli</a>, <a href="/search/astro-ph?searchtype=author&query=Ferroni%2C+V">V Ferroni</a>, <a href="/search/astro-ph?searchtype=author&query=Fitzsimons%2C+E+D">E D Fitzsimons</a>, <a href="/search/astro-ph?searchtype=author&query=Freschi%2C+M">M Freschi</a>, <a href="/search/astro-ph?searchtype=author&query=Gesa%2C+L">L Gesa</a>, <a href="/search/astro-ph?searchtype=author&query=Giardini%2C+D">D Giardini</a>, <a href="/search/astro-ph?searchtype=author&query=Gibert%2C+F">F Gibert</a>, <a href="/search/astro-ph?searchtype=author&query=Giusteri%2C+R">R Giusteri</a>, <a href="/search/astro-ph?searchtype=author&query=Grimani%2C+C">C Grimani</a>, <a href="/search/astro-ph?searchtype=author&query=Grzymisch%2C+J">J Grzymisch</a> , et al. (54 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.04431v2-abstract-short" style="display: inline;"> A precise characterization of the magnetic properties of LISA Pathfinder free falling test-masses is of special interest for future gravitational wave observatory in space. Magnetic forces have an important impact on the instrument sensitivity in the low frequency regime below the millihertz. In this paper we report on the magnetic injection experiments performed throughout LISA Pathfinder operati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04431v2-abstract-full').style.display = 'inline'; document.getElementById('2407.04431v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.04431v2-abstract-full" style="display: none;"> A precise characterization of the magnetic properties of LISA Pathfinder free falling test-masses is of special interest for future gravitational wave observatory in space. Magnetic forces have an important impact on the instrument sensitivity in the low frequency regime below the millihertz. In this paper we report on the magnetic injection experiments performed throughout LISA Pathfinder operations. We show how these experiments allowed a high precision estimate of the instrument magnetic parameters. The remanent magnetic moment was found to have a modulus of $(0.245\pm0.081)\,\rm{nAm}^2$, the x-component of the background magnetic field within the test masses position was measured to be $(414 \pm 74)$ nT and its gradient had a value of $(-7.4\pm 2.1)\,渭$T/m. Finally, we also measured the test mass magnetic susceptibility to be $(-3.35\pm0.15)\times$10$^{-5}$ in the low frequency regime. All results are in agreement with on-ground estimates. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04431v2-abstract-full').style.display = 'none'; document.getElementById('2407.04431v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.04427">arXiv:2407.04427</a> <span> [<a href="https://arxiv.org/pdf/2407.04427">pdf</a>, <a href="https://arxiv.org/format/2407.04427">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="General Relativity and Quantum Cosmology">gr-qc</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.134.071401">10.1103/PhysRevLett.134.071401 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Magnetic-induced force noise in LISA Pathfinder free-falling test masses </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Armano%2C+M">M Armano</a>, <a href="/search/astro-ph?searchtype=author&query=Audley%2C+H">H Audley</a>, <a href="/search/astro-ph?searchtype=author&query=Baird%2C+J">J Baird</a>, <a href="/search/astro-ph?searchtype=author&query=Binetruy%2C+P">P Binetruy</a>, <a href="/search/astro-ph?searchtype=author&query=Born%2C+M">M Born</a>, <a href="/search/astro-ph?searchtype=author&query=Bortoluzzi%2C+D">D Bortoluzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Castelli%2C+E">E Castelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cavalleri%2C+A">A Cavalleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cesarini%2C+A">A Cesarini</a>, <a href="/search/astro-ph?searchtype=author&query=Cruise%2C+A+M">A M Cruise</a>, <a href="/search/astro-ph?searchtype=author&query=Danzmann%2C+K">K Danzmann</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+M+D+D">M De Deus Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Diepholz%2C+I">I Diepholz</a>, <a href="/search/astro-ph?searchtype=author&query=Dixon%2C+G">G Dixon</a>, <a href="/search/astro-ph?searchtype=author&query=Dolesi%2C+R">R Dolesi</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraioli%2C+L">L Ferraioli</a>, <a href="/search/astro-ph?searchtype=author&query=Ferroni%2C+V">V Ferroni</a>, <a href="/search/astro-ph?searchtype=author&query=Fitzsimons%2C+E+D">E D Fitzsimons</a>, <a href="/search/astro-ph?searchtype=author&query=Freschi%2C+M">M Freschi</a>, <a href="/search/astro-ph?searchtype=author&query=Gesa%2C+L">L Gesa</a>, <a href="/search/astro-ph?searchtype=author&query=Giardini%2C+D">D Giardini</a>, <a href="/search/astro-ph?searchtype=author&query=Gibert%2C+F">F Gibert</a>, <a href="/search/astro-ph?searchtype=author&query=Giusteri%2C+R">R Giusteri</a>, <a href="/search/astro-ph?searchtype=author&query=Grimani%2C+C">C Grimani</a>, <a href="/search/astro-ph?searchtype=author&query=Grzymisch%2C+J">J Grzymisch</a> , et al. (54 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.04427v2-abstract-short" style="display: inline;"> LISA Pathfinder was a mission designed to test key technologies required for gravitational wave detection in space. Magnetically driven forces play a key role in the instrument sensitivity in the low-frequency regime, which corresponds to the measurement band of interest for future space-borne gravitational wave observatories. Magnetic-induced forces couple to the test mass motion, introducing a c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04427v2-abstract-full').style.display = 'inline'; document.getElementById('2407.04427v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.04427v2-abstract-full" style="display: none;"> LISA Pathfinder was a mission designed to test key technologies required for gravitational wave detection in space. Magnetically driven forces play a key role in the instrument sensitivity in the low-frequency regime, which corresponds to the measurement band of interest for future space-borne gravitational wave observatories. Magnetic-induced forces couple to the test mass motion, introducing a contribution to the relative acceleration noise between the free falling test masses. In this Letter we present the first complete estimate of this term of the instrument performance model. Our results set the magnetic-induced acceleration noise during the February 2017 noise run of $\rm 0.25_{-0.08}^{+0.15}\,fm\,s^{-2}/\sqrt{Hz}$ at 1 mHz and $\rm 1.01_{-0.24}^{+0.73}\, fm\,s^{-2}/\sqrt{Hz}$ at 0.1 mHz. We also discuss how the non-stationarities of the interplanetary magnetic field can affect these values during extreme space weather conditions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04427v2-abstract-full').style.display = 'none'; document.getElementById('2407.04427v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.05207">arXiv:2405.05207</a> <span> [<a href="https://arxiv.org/pdf/2405.05207">pdf</a>, <a href="https://arxiv.org/format/2405.05207">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/10.1103/PhysRevD.110.042004">10.1103/PhysRevD.110.042004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> In-depth analysis of LISA Pathfinder performance results: Time evolution, noise projection, physical models, and implications for LISA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Armano%2C+M">M. Armano</a>, <a href="/search/astro-ph?searchtype=author&query=Audley%2C+H">H. Audley</a>, <a href="/search/astro-ph?searchtype=author&query=Baird%2C+J">J. Baird</a>, <a href="/search/astro-ph?searchtype=author&query=Binetruy%2C+P">P. Binetruy</a>, <a href="/search/astro-ph?searchtype=author&query=Born%2C+M">M. Born</a>, <a href="/search/astro-ph?searchtype=author&query=Bortoluzzi%2C+D">D. Bortoluzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Castelli%2C+E">E. Castelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cavalleri%2C+A">A. Cavalleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cesarini%2C+A">A. Cesarini</a>, <a href="/search/astro-ph?searchtype=author&query=Chiavegato%2C+V">V. Chiavegato</a>, <a href="/search/astro-ph?searchtype=author&query=Cruise%2C+A+M">A. M. Cruise</a>, <a href="/search/astro-ph?searchtype=author&query=Bosco%2C+D+D">D. Dal Bosco</a>, <a href="/search/astro-ph?searchtype=author&query=Danzmann%2C+K">K. Danzmann</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+M+D+D">M. De Deus Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Diepholz%2C+I">I. Diepholz</a>, <a href="/search/astro-ph?searchtype=author&query=Dixon%2C+G">G. Dixon</a>, <a href="/search/astro-ph?searchtype=author&query=Dolesi%2C+R">R. Dolesi</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraioli%2C+L">L. Ferraioli</a>, <a href="/search/astro-ph?searchtype=author&query=Ferroni%2C+V">V. Ferroni</a>, <a href="/search/astro-ph?searchtype=author&query=Fitzsimons%2C+E+D">E. D. Fitzsimons</a>, <a href="/search/astro-ph?searchtype=author&query=Freschi%2C+M">M. Freschi</a>, <a href="/search/astro-ph?searchtype=author&query=Gesa%2C+L">L. Gesa</a>, <a href="/search/astro-ph?searchtype=author&query=Giardini%2C+D">D. Giardini</a>, <a href="/search/astro-ph?searchtype=author&query=Gibert%2C+F">F. Gibert</a>, <a href="/search/astro-ph?searchtype=author&query=Giusteri%2C+R">R. Giusteri</a> , et al. (55 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.05207v3-abstract-short" style="display: inline;"> We present an in-depth analysis of the LISA Pathfinder differential acceleration performance over the entire course of its science operations, spanning approximately 500 days. We find that: 1) the evolution of the Brownian noise that dominates the acceleration amplitude spectral density (ASD), for frequencies $f\gtrsim 1\,\text{mHz}$, is consistent with the decaying pressure due to the outgassing… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.05207v3-abstract-full').style.display = 'inline'; document.getElementById('2405.05207v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.05207v3-abstract-full" style="display: none;"> We present an in-depth analysis of the LISA Pathfinder differential acceleration performance over the entire course of its science operations, spanning approximately 500 days. We find that: 1) the evolution of the Brownian noise that dominates the acceleration amplitude spectral density (ASD), for frequencies $f\gtrsim 1\,\text{mHz}$, is consistent with the decaying pressure due to the outgassing of a single gaseous species. 2) between $f=36\,渭\text{Hz}$ and $1\,\text{mHz}$, the acceleration ASD shows a $1/f$ tail in excess of the Brownian noise of almost constant amplitude, with $\simeq 20\%$ fluctuations over a period of a few days, with no particular time pattern over the course of the mission; 3) at the lowest considered frequency of $f=18\,渭\text{Hz}$, the ASD significantly deviates from the $1/f$ behavior, because of temperature fluctuations that appear to modulate a quasi-static pressure gradient, sustained by the asymmetries of the outgassing pattern. We also present the results of a projection of the observed acceleration noise on the potential sources for which we had either a direct correlation measurement, or a quantitative estimate from dedicated experiments. These sources account for approximately $40\%$ of the noise power in the $1/f$ tail. Finally, we analyze the possible sources of the remaining unexplained fraction, and identify the possible measures that may be taken to keep those under control in LISA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.05207v3-abstract-full').style.display = 'none'; document.getElementById('2405.05207v3-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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">Journal ref:</span> Phys. Rev. D 110, 042004 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.07571">arXiv:2402.07571</a> <span> [<a href="https://arxiv.org/pdf/2402.07571">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> </div> <p class="title is-5 mathjax"> LISA Definition Study Report </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Colpi%2C+M">Monica Colpi</a>, <a href="/search/astro-ph?searchtype=author&query=Danzmann%2C+K">Karsten Danzmann</a>, <a href="/search/astro-ph?searchtype=author&query=Hewitson%2C+M">Martin Hewitson</a>, <a href="/search/astro-ph?searchtype=author&query=Holley-Bockelmann%2C+K">Kelly Holley-Bockelmann</a>, <a href="/search/astro-ph?searchtype=author&query=Jetzer%2C+P">Philippe Jetzer</a>, <a href="/search/astro-ph?searchtype=author&query=Nelemans%2C+G">Gijs Nelemans</a>, <a href="/search/astro-ph?searchtype=author&query=Petiteau%2C+A">Antoine Petiteau</a>, <a href="/search/astro-ph?searchtype=author&query=Shoemaker%2C+D">David Shoemaker</a>, <a href="/search/astro-ph?searchtype=author&query=Sopuerta%2C+C">Carlos Sopuerta</a>, <a href="/search/astro-ph?searchtype=author&query=Stebbins%2C+R">Robin Stebbins</a>, <a href="/search/astro-ph?searchtype=author&query=Tanvir%2C+N">Nial Tanvir</a>, <a href="/search/astro-ph?searchtype=author&query=Ward%2C+H">Henry Ward</a>, <a href="/search/astro-ph?searchtype=author&query=Weber%2C+W+J">William Joseph Weber</a>, <a href="/search/astro-ph?searchtype=author&query=Thorpe%2C+I">Ira Thorpe</a>, <a href="/search/astro-ph?searchtype=author&query=Daurskikh%2C+A">Anna Daurskikh</a>, <a href="/search/astro-ph?searchtype=author&query=Deep%2C+A">Atul Deep</a>, <a href="/search/astro-ph?searchtype=author&query=N%C3%BA%C3%B1ez%2C+I+F">Ignacio Fern谩ndez N煤帽ez</a>, <a href="/search/astro-ph?searchtype=author&query=Marirrodriga%2C+C+G">C茅sar Garc铆a Marirrodriga</a>, <a href="/search/astro-ph?searchtype=author&query=Gehler%2C+M">Martin Gehler</a>, <a href="/search/astro-ph?searchtype=author&query=Halain%2C+J">Jean-Philippe Halain</a>, <a href="/search/astro-ph?searchtype=author&query=Jennrich%2C+O">Oliver Jennrich</a>, <a href="/search/astro-ph?searchtype=author&query=Lammers%2C+U">Uwe Lammers</a>, <a href="/search/astro-ph?searchtype=author&query=Larra%C3%B1aga%2C+J">Jonan Larra帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Lieser%2C+M">Maike Lieser</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%BCtzgendorf%2C+N">Nora L眉tzgendorf</a> , et al. (86 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.07571v1-abstract-short" style="display: inline;"> The Laser Interferometer Space Antenna (LISA) is the first scientific endeavour to detect and study gravitational waves from space. LISA will survey the sky for Gravitational Waves in the 0.1 mHz to 1 Hz frequency band which will enable the study of a vast number of objects ranging from Galactic binaries and stellar mass black holes in the Milky Way, to distant massive black-hole mergers and the e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.07571v1-abstract-full').style.display = 'inline'; document.getElementById('2402.07571v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.07571v1-abstract-full" style="display: none;"> The Laser Interferometer Space Antenna (LISA) is the first scientific endeavour to detect and study gravitational waves from space. LISA will survey the sky for Gravitational Waves in the 0.1 mHz to 1 Hz frequency band which will enable the study of a vast number of objects ranging from Galactic binaries and stellar mass black holes in the Milky Way, to distant massive black-hole mergers and the expansion of the Universe. This definition study report, or Red Book, presents a summary of the very large body of work that has been undertaken on the LISA mission over the LISA definition phase. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.07571v1-abstract-full').style.display = 'none'; document.getElementById('2402.07571v1-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">155 pages, with executive summary and table of contents</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.00884">arXiv:2401.00884</a> <span> [<a href="https://arxiv.org/pdf/2401.00884">pdf</a>, <a href="https://arxiv.org/format/2401.00884">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="General Relativity and Quantum Cosmology">gr-qc</span> </div> </div> <p class="title is-5 mathjax"> NanoNewton electrostatic force actuators for femtoNewton-sensitive measurements: system performance test in the LISA Pathfinder mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Armano%2C+M">M Armano</a>, <a href="/search/astro-ph?searchtype=author&query=Audley%2C+H">H Audley</a>, <a href="/search/astro-ph?searchtype=author&query=Baird%2C+J">J Baird</a>, <a href="/search/astro-ph?searchtype=author&query=Bassan%2C+M">M Bassan</a>, <a href="/search/astro-ph?searchtype=author&query=Binetruy%2C+P">P Binetruy</a>, <a href="/search/astro-ph?searchtype=author&query=Born%2C+M">M Born</a>, <a href="/search/astro-ph?searchtype=author&query=Bortoluzzi%2C+D">D Bortoluzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Castelli%2C+E">E Castelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cavalleri%2C+A">A Cavalleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cesarini%2C+A">A Cesarini</a>, <a href="/search/astro-ph?searchtype=author&query=Chiavegato%2C+V">V Chiavegato</a>, <a href="/search/astro-ph?searchtype=author&query=Cruise%2C+A+M">A M Cruise</a>, <a href="/search/astro-ph?searchtype=author&query=Bosco%2C+D+D">D Dal Bosco</a>, <a href="/search/astro-ph?searchtype=author&query=Danzmann%2C+K">K Danzmann</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+M+D+D">M De Deus Silva</a>, <a href="/search/astro-ph?searchtype=author&query=De+Rosa%2C+R">R De Rosa</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Fiore%2C+L">L Di Fiore</a>, <a href="/search/astro-ph?searchtype=author&query=Diepholz%2C+I">I Diepholz</a>, <a href="/search/astro-ph?searchtype=author&query=Dixon%2C+G">G Dixon</a>, <a href="/search/astro-ph?searchtype=author&query=Dolesi%2C+R">R Dolesi</a>, <a href="/search/astro-ph?searchtype=author&query=Ferroni%2C+L+F+V">L Ferraioli V Ferroni</a>, <a href="/search/astro-ph?searchtype=author&query=Fitzsimons%2C+E+D">E D Fitzsimons</a>, <a href="/search/astro-ph?searchtype=author&query=Freschi%2C+M">M Freschi</a>, <a href="/search/astro-ph?searchtype=author&query=Gesa%2C+L">L Gesa</a>, <a href="/search/astro-ph?searchtype=author&query=Giardini%2C+D">D Giardini</a> , et al. (65 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.00884v1-abstract-short" style="display: inline;"> Electrostatic force actuation is a key component of the system of geodesic reference test masses (TM) for the LISA orbiting gravitational wave observatory and in particular for performance at low frequencies, below 1 mHz, where the observatory sensitivity is limited by stray force noise. The system needs to apply forces of order 10$^{-9}$ N while limiting fluctuations in the measurement band to le… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.00884v1-abstract-full').style.display = 'inline'; document.getElementById('2401.00884v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.00884v1-abstract-full" style="display: none;"> Electrostatic force actuation is a key component of the system of geodesic reference test masses (TM) for the LISA orbiting gravitational wave observatory and in particular for performance at low frequencies, below 1 mHz, where the observatory sensitivity is limited by stray force noise. The system needs to apply forces of order 10$^{-9}$ N while limiting fluctuations in the measurement band to levels approaching 10$^{-15}$ N/Hz$^{1/2}$. We present here the LISA actuation system design, based on audio-frequency voltage carrier signals, and results of its in-flight performance test with the LISA Pathfinder test mission. In LISA, TM force actuation is used to align the otherwise free-falling TM to the spacecraft-mounted optical metrology system, without any forcing along the critical gravitational wave-sensitive interferometry axes. In LISA Pathfinder, on the other hand, the actuation was used also to stabilize the TM along the critical $x$ axis joining the two TM, with the commanded actuation force entering directly into the mission's main differential acceleration science observable. The mission allowed demonstration of the full compatibility of the electrostatic actuation system with the LISA observatory requirements, including dedicated measurement campaigns to amplify, isolate, and quantify the two main force noise contributions from the actuation system, from actuator gain noise and from low frequency ``in band'' voltage fluctuations. These campaigns have shown actuation force noise to be a relevant, but not dominant, noise source in LISA Pathfinder and have allowed performance projections for the conditions expected in the LISA mission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.00884v1-abstract-full').style.display = 'none'; document.getElementById('2401.00884v1-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, 2023; <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/2308.02398">arXiv:2308.02398</a> <span> [<a href="https://arxiv.org/pdf/2308.02398">pdf</a>, <a href="https://arxiv.org/format/2308.02398">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/10.1103/PhysRevD.108.102003">10.1103/PhysRevD.108.102003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Tilt-to-length coupling in LISA Pathfinder: a data analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Armano%2C+M">M Armano</a>, <a href="/search/astro-ph?searchtype=author&query=Audley%2C+H">H Audley</a>, <a href="/search/astro-ph?searchtype=author&query=Baird%2C+J">J Baird</a>, <a href="/search/astro-ph?searchtype=author&query=Binetruy%2C+P">P Binetruy</a>, <a href="/search/astro-ph?searchtype=author&query=Born%2C+M">M Born</a>, <a href="/search/astro-ph?searchtype=author&query=Bortoluzzi%2C+D">D Bortoluzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Castelli%2C+E">E Castelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cavalleri%2C+A">A Cavalleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cesarini%2C+A">A Cesarini</a>, <a href="/search/astro-ph?searchtype=author&query=Cruise%2C+A+M">A M Cruise</a>, <a href="/search/astro-ph?searchtype=author&query=Danzmann%2C+K">K Danzmann</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+M+d+D">M de Deus Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Diepholz%2C+I">I Diepholz</a>, <a href="/search/astro-ph?searchtype=author&query=Dixon%2C+G">G Dixon</a>, <a href="/search/astro-ph?searchtype=author&query=Dolesi%2C+R">R Dolesi</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraioli%2C+L">L Ferraioli</a>, <a href="/search/astro-ph?searchtype=author&query=Ferroni%2C+V">V Ferroni</a>, <a href="/search/astro-ph?searchtype=author&query=Fitzsimons%2C+E+D">E D Fitzsimons</a>, <a href="/search/astro-ph?searchtype=author&query=Freschi%2C+M">M Freschi</a>, <a href="/search/astro-ph?searchtype=author&query=Gesa%2C+L">L Gesa</a>, <a href="/search/astro-ph?searchtype=author&query=Giardini%2C+D">D Giardini</a>, <a href="/search/astro-ph?searchtype=author&query=Gibert%2C+F">F Gibert</a>, <a href="/search/astro-ph?searchtype=author&query=Giusteri%2C+R">R Giusteri</a>, <a href="/search/astro-ph?searchtype=author&query=Grimani%2C+C">C Grimani</a>, <a href="/search/astro-ph?searchtype=author&query=Grzymisch%2C+J">J Grzymisch</a> , et al. (54 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.02398v1-abstract-short" style="display: inline;"> We present a study of the tilt-to-length coupling noise during the LISA Pathfinder mission and how it depended on the system's alignment. Tilt-to-length coupling noise is the unwanted coupling of angular and lateral spacecraft or test mass motion into the primary interferometric displacement readout. It was one of the major noise sources in the LISA Pathfinder mission and is likewise expected to b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.02398v1-abstract-full').style.display = 'inline'; document.getElementById('2308.02398v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.02398v1-abstract-full" style="display: none;"> We present a study of the tilt-to-length coupling noise during the LISA Pathfinder mission and how it depended on the system's alignment. Tilt-to-length coupling noise is the unwanted coupling of angular and lateral spacecraft or test mass motion into the primary interferometric displacement readout. It was one of the major noise sources in the LISA Pathfinder mission and is likewise expected to be a primary noise source in LISA. We demonstrate here that a recently derived and published analytical model describes the dependency of the LISA Pathfinder tilt-to-length coupling noise on the alignment of the two freely falling test masses. This was verified with the data taken before and after the realignments performed in March (engineering days) and June 2016, and during a two-day experiment in February 2017 (long cross-talk experiment). The latter was performed with the explicit goal of testing the tilt-to-length coupling noise dependency on the test mass alignment. Using the analytical model, we show that all realignments performed during the mission were only partially successful and explain the reasons why. In addition to the analytical model, we computed another physical tilt-to-length coupling model via a minimising routine making use of the long cross-talk experiment data. A similar approach could prove useful for the LISA mission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.02398v1-abstract-full').style.display = 'none'; document.getElementById('2308.02398v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.09309">arXiv:2211.09309</a> <span> [<a href="https://arxiv.org/pdf/2211.09309">pdf</a>, <a href="https://arxiv.org/format/2211.09309">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/10.1103/PhysRevD.107.062007">10.1103/PhysRevD.107.062007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Charging of free-falling test masses in orbit due to cosmic rays: results from LISA Pathfinder </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=LISA+Pathfinder+Collaboration"> LISA Pathfinder Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Armano%2C+M">M. Armano</a>, <a href="/search/astro-ph?searchtype=author&query=Audley%2C+H">H. Audley</a>, <a href="/search/astro-ph?searchtype=author&query=Baird%2C+J">J. Baird</a>, <a href="/search/astro-ph?searchtype=author&query=Binetruy%2C+P">P. Binetruy</a>, <a href="/search/astro-ph?searchtype=author&query=Born%2C+M">M. Born</a>, <a href="/search/astro-ph?searchtype=author&query=Bortoluzzi%2C+D">D. Bortoluzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Castelli%2C+E">E. Castelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cesarini%2C+A+C+A">A. Cavalleri A. Cesarini</a>, <a href="/search/astro-ph?searchtype=author&query=Cruise%2C+A+M">A. M Cruise</a>, <a href="/search/astro-ph?searchtype=author&query=Danzmann%2C+K">K. Danzmann</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+M+d+D">M. de Deus Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Diepholz%2C+I">I. Diepholz</a>, <a href="/search/astro-ph?searchtype=author&query=Dixon%2C+G">G. Dixon</a>, <a href="/search/astro-ph?searchtype=author&query=Dolesi%2C+R">R. Dolesi</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraioli%2C+L">L. Ferraioli</a>, <a href="/search/astro-ph?searchtype=author&query=Ferroni%2C+V">V. Ferroni</a>, <a href="/search/astro-ph?searchtype=author&query=Fitzsimons%2C+E+D">E. D. Fitzsimons</a>, <a href="/search/astro-ph?searchtype=author&query=Freschi%2C+M">M. Freschi</a>, <a href="/search/astro-ph?searchtype=author&query=Gesa%2C+L">L. Gesa</a>, <a href="/search/astro-ph?searchtype=author&query=Giardini%2C+D">D. Giardini</a>, <a href="/search/astro-ph?searchtype=author&query=Gibert%2C+F">F. Gibert</a>, <a href="/search/astro-ph?searchtype=author&query=Giusteri%2C+R">R. Giusteri</a>, <a href="/search/astro-ph?searchtype=author&query=Grimani%2C+C">C. Grimani</a>, <a href="/search/astro-ph?searchtype=author&query=Grzymisch%2C+J">J. Grzymisch</a> , et al. (50 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.09309v2-abstract-short" style="display: inline;"> A comprehensive summary of the measurements made to characterize test mass charging due to the space environment during the LISA Pathfinder mission is presented. Measurements of the residual charge of the test mass after release by the grabbing and positioning mechanism, show that the initial charge of the test masses was negative after all releases, leaving the test mass with a potential in the r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.09309v2-abstract-full').style.display = 'inline'; document.getElementById('2211.09309v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.09309v2-abstract-full" style="display: none;"> A comprehensive summary of the measurements made to characterize test mass charging due to the space environment during the LISA Pathfinder mission is presented. Measurements of the residual charge of the test mass after release by the grabbing and positioning mechanism, show that the initial charge of the test masses was negative after all releases, leaving the test mass with a potential in the range $-12$ mV to $-512$ mV. Variations in the neutral test mass charging rate between $21.7$ e s$^{-1}$ and $30.7$ e s$^{-1}$ were observed over the course of the 17-month science operations produced by cosmic ray flux changes including a Forbush decrease associated with a small solar energetic particle event. A dependence of the cosmic ray charging rate on the test mass potential between $-30.2$ e s$^{-1}$ V$^{-1}$ and $-40.3$ e s$^{-1}$ V$^{-1}$ was observed and this is attributed to a contribution to charging from low-energy electrons emitted from the gold surfaces of the gravitational reference sensor. Data from the on-board particle detector show a reliable correlation with the charging rate and with other environmental monitors of the cosmic ray flux. This correlation is exploited to extrapolate test mass charging rates to a 20-year period giving useful insight into the expected range of charging rate that may be observed in the LISA mission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.09309v2-abstract-full').style.display = 'none'; document.getElementById('2211.09309v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 10 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 107, 062007 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.07490">arXiv:2112.07490</a> <span> [<a href="https://arxiv.org/pdf/2112.07490">pdf</a>, <a href="https://arxiv.org/format/2112.07490">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</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/10.1103/PhysRevD.105.042002">10.1103/PhysRevD.105.042002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detection and characterization of instrumental transients in LISA Pathfinder and their projection to LISA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Baghi%2C+Q">Quentin Baghi</a>, <a href="/search/astro-ph?searchtype=author&query=Korsakova%2C+N">Natalia Korsakova</a>, <a href="/search/astro-ph?searchtype=author&query=Slutsky%2C+J">Jacob Slutsky</a>, <a href="/search/astro-ph?searchtype=author&query=Castelli%2C+E">Eleonora Castelli</a>, <a href="/search/astro-ph?searchtype=author&query=Karnesis%2C+N">Nikolaos Karnesis</a>, <a href="/search/astro-ph?searchtype=author&query=Bayle%2C+J">Jean-Baptiste Bayle</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="2112.07490v1-abstract-short" style="display: inline;"> The LISA Pathfinder (LPF) mission succeeded outstandingly in demonstrating key technological aspects of future space-borne gravitational-wave detectors, such as the Laser Interferometer Space Antenna (LISA). Specifically, LPF demonstrated with unprecedented sensitivity the measurement of the relative acceleration of two free-falling cubic test masses. Although most disruptive non-gravitational for… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.07490v1-abstract-full').style.display = 'inline'; document.getElementById('2112.07490v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.07490v1-abstract-full" style="display: none;"> The LISA Pathfinder (LPF) mission succeeded outstandingly in demonstrating key technological aspects of future space-borne gravitational-wave detectors, such as the Laser Interferometer Space Antenna (LISA). Specifically, LPF demonstrated with unprecedented sensitivity the measurement of the relative acceleration of two free-falling cubic test masses. Although most disruptive non-gravitational forces have been identified and their effects mitigated through a series of calibration processes, some faint transient signals of yet unexplained origin remain in the measurements. If they appear in the LISA data, these perturbations (also called glitches) could skew the characterization of gravitational-wave sources or even be confused with gravitational-wave bursts. For the first time, we provide a comprehensive census of LPF transient events. Our analysis is based on a phenomenological shapelet model allowing us to derive simple statistics about the physical features of the glitch population. We then implement a generator of synthetic glitches designed to be used for subsequent LISA studies, and perform a preliminary evaluation of the effect of the glitches on future LISA data analyses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.07490v1-abstract-full').style.display = 'none'; document.getElementById('2112.07490v1-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 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 12 figures, to be submitted to 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/2005.03423">arXiv:2005.03423</a> <span> [<a href="https://arxiv.org/pdf/2005.03423">pdf</a>, <a href="https://arxiv.org/format/2005.03423">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/10.1093/mnras/staa830">10.1093/mnras/staa830 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spacecraft and interplanetary contributions to the magnetic environment on-board LISA Pathfinder </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Armano%2C+M">M. Armano</a>, <a href="/search/astro-ph?searchtype=author&query=Audley%2C+H">H. Audley</a>, <a href="/search/astro-ph?searchtype=author&query=Baird%2C+J">J. Baird</a>, <a href="/search/astro-ph?searchtype=author&query=Binetruy%2C+P">P. Binetruy</a>, <a href="/search/astro-ph?searchtype=author&query=Born%2C+M">M. Born</a>, <a href="/search/astro-ph?searchtype=author&query=Bortoluzzi%2C+D">D. Bortoluzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Castelli%2C+E">E. Castelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cavalleri%2C+A">A. Cavalleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cesarini%2C+A">A. Cesarini</a>, <a href="/search/astro-ph?searchtype=author&query=Cruise%2C+A+M">A. M. Cruise</a>, <a href="/search/astro-ph?searchtype=author&query=Danzmann%2C+K">K. Danzmann</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+M+d+D">M. de Deus Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Diepholz%2C+I">I. Diepholz</a>, <a href="/search/astro-ph?searchtype=author&query=Dixon%2C+G">G. Dixon</a>, <a href="/search/astro-ph?searchtype=author&query=Dolesi%2C+R">R. Dolesi</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraioli%2C+L">L. Ferraioli</a>, <a href="/search/astro-ph?searchtype=author&query=Ferroni%2C+V">V. Ferroni</a>, <a href="/search/astro-ph?searchtype=author&query=Fitzsimons%2C+E+D">E. D. Fitzsimons</a>, <a href="/search/astro-ph?searchtype=author&query=Freschi%2C+M">M. Freschi</a>, <a href="/search/astro-ph?searchtype=author&query=Gesa%2C+L">L. Gesa</a>, <a href="/search/astro-ph?searchtype=author&query=Gibert%2C+F">F. Gibert</a>, <a href="/search/astro-ph?searchtype=author&query=Giardini%2C+D">D. Giardini</a>, <a href="/search/astro-ph?searchtype=author&query=Giusteri%2C+R">R. Giusteri</a>, <a href="/search/astro-ph?searchtype=author&query=Grimani%2C+C">C. Grimani</a>, <a href="/search/astro-ph?searchtype=author&query=Grzymisch%2C+J">J. Grzymisch</a> , et al. (57 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="2005.03423v1-abstract-short" style="display: inline;"> LISA Pathfinder (LPF) has been a space-based mission designed to test new technologies that will be required for a gravitational wave observatory in space. Magnetically driven forces play a key role in the instrument sensitivity in the low-frequency regime (mHz and below), the measurement band of interest for a space-based observatory. The magnetic field can couple to the magnetic susceptibility a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.03423v1-abstract-full').style.display = 'inline'; document.getElementById('2005.03423v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.03423v1-abstract-full" style="display: none;"> LISA Pathfinder (LPF) has been a space-based mission designed to test new technologies that will be required for a gravitational wave observatory in space. Magnetically driven forces play a key role in the instrument sensitivity in the low-frequency regime (mHz and below), the measurement band of interest for a space-based observatory. The magnetic field can couple to the magnetic susceptibility and remanent magnetic moment from the test masses and disturb them from their geodesic movement. LISA Pathfinder carried on-board a dedicated magnetic measurement subsystem with noise levels of 10 $ \rm nT \ Hz^{-1/2}$ from 1 Hz down to 1 mHz. In this paper we report on the magnetic measurements throughout LISA Pathfinder operations. We characterise the magnetic environment within the spacecraft, study the time evolution of the magnetic field and its stability down to 20 $渭$Hz, where we measure values around 200 $ \rm nT \ Hz^{-1/2}$ and identify two different frequency regimes, one related to the interplanetary magnetic field and the other to the magnetic field originating inside the spacecraft. Finally, we characterise the non-stationary component of the fluctuations of the magnetic field below the mHz and relate them to the dynamics of the solar wind. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.03423v1-abstract-full').style.display = 'none'; document.getElementById('2005.03423v1-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 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">16 pages, 17 figures. MNRAS LaTeX style file version 3.0</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Monthly Notices of the Royal Astronomical Society, 2020, 494.2: 3014-3027 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1908.11584">arXiv:1908.11584</a> <span> [<a href="https://arxiv.org/pdf/1908.11584">pdf</a>, <a href="https://arxiv.org/format/1908.11584">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</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/10.1103/PhysRevLett.123.111101">10.1103/PhysRevLett.123.111101 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LISA Pathfinder Performance Confirmed in an Open-Loop Configuration: Results from the Free-Fall Actuation Mode </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Armano%2C+M">M. Armano</a>, <a href="/search/astro-ph?searchtype=author&query=Audley%2C+H">H. Audley</a>, <a href="/search/astro-ph?searchtype=author&query=Baird%2C+J">J. Baird</a>, <a href="/search/astro-ph?searchtype=author&query=Binetruy%2C+P">P. Binetruy</a>, <a href="/search/astro-ph?searchtype=author&query=Born%2C+M">M. Born</a>, <a href="/search/astro-ph?searchtype=author&query=Bortoluzzi%2C+D">D. Bortoluzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Castelli%2C+E">E. Castelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cavalleri%2C+A">A. Cavalleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cesarini%2C+A">A. Cesarini</a>, <a href="/search/astro-ph?searchtype=author&query=Cruise%2C+A+M">A. M. Cruise</a>, <a href="/search/astro-ph?searchtype=author&query=Danzmann%2C+K">K. Danzmann</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+M+d+D">M. de Deus Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Diepholz%2C+I">I. Diepholz</a>, <a href="/search/astro-ph?searchtype=author&query=Dixon%2C+G">G. Dixon</a>, <a href="/search/astro-ph?searchtype=author&query=Dolesi%2C+R">R. Dolesi</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraioli%2C+L">L. Ferraioli</a>, <a href="/search/astro-ph?searchtype=author&query=Ferroni%2C+V">V. Ferroni</a>, <a href="/search/astro-ph?searchtype=author&query=Fitzsimons%2C+E+D">E. D. Fitzsimons</a>, <a href="/search/astro-ph?searchtype=author&query=Freschi%2C+M">M. Freschi</a>, <a href="/search/astro-ph?searchtype=author&query=Gesa%2C+L">L. Gesa</a>, <a href="/search/astro-ph?searchtype=author&query=Gibert%2C+F">F. Gibert</a>, <a href="/search/astro-ph?searchtype=author&query=Giardini%2C+D">D. Giardini</a>, <a href="/search/astro-ph?searchtype=author&query=Giusteri%2C+R">R. Giusteri</a>, <a href="/search/astro-ph?searchtype=author&query=Grimani%2C+C">C. Grimani</a>, <a href="/search/astro-ph?searchtype=author&query=Grzymisch%2C+J">J. Grzymisch</a> , et al. (53 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="1908.11584v1-abstract-short" style="display: inline;"> We report on the results of the LISA Pathfinder (LPF) free-fall mode experiment, in which the control force needed to compensate the quasistatic differential force acting on two test masses is applied intermittently as a series of "impulse" forces lasting a few seconds and separated by roughly 350 s periods of true free fall. This represents an alternative to the normal LPF mode of operation in wh… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.11584v1-abstract-full').style.display = 'inline'; document.getElementById('1908.11584v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.11584v1-abstract-full" style="display: none;"> We report on the results of the LISA Pathfinder (LPF) free-fall mode experiment, in which the control force needed to compensate the quasistatic differential force acting on two test masses is applied intermittently as a series of "impulse" forces lasting a few seconds and separated by roughly 350 s periods of true free fall. This represents an alternative to the normal LPF mode of operation in which this balancing force is applied continuously, with the advantage that the acceleration noise during free fall is measured in the absence of the actuation force, thus eliminating associated noise and force calibration errors. The differential acceleration noise measurement presented here with the free-fall mode agrees with noise measured with the continuous actuation scheme, representing an important and independent confirmation of the LPF result. An additional measurement with larger actuation forces also shows that the technique can be used to eliminate actuation noise when this is a dominant factor. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.11584v1-abstract-full').style.display = 'none'; document.getElementById('1908.11584v1-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 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2019. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1905.09060">arXiv:1905.09060</a> <span> [<a href="https://arxiv.org/pdf/1905.09060">pdf</a>, <a href="https://arxiv.org/format/1905.09060">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="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stz1017">10.1093/mnras/stz1017 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Temperature stability in the sub-milliHertz band with LISA Pathfinder </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Armano%2C+M">M. Armano</a>, <a href="/search/astro-ph?searchtype=author&query=Audley%2C+H">H. Audley</a>, <a href="/search/astro-ph?searchtype=author&query=Baird%2C+J">J. Baird</a>, <a href="/search/astro-ph?searchtype=author&query=Binetruy%2C+P">P. Binetruy</a>, <a href="/search/astro-ph?searchtype=author&query=Born%2C+M">M. Born</a>, <a href="/search/astro-ph?searchtype=author&query=Bortoluzzi%2C+D">D. Bortoluzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Castelli%2C+E">E. Castelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cavalleri%2C+A">A. Cavalleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cesarini%2C+A">A. Cesarini</a>, <a href="/search/astro-ph?searchtype=author&query=Cruise%2C+A+M">A. M. Cruise</a>, <a href="/search/astro-ph?searchtype=author&query=Danzmann%2C+K">K. Danzmann</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+M+d+D">M. de Deus Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Diepholz%2C+I">I. Diepholz</a>, <a href="/search/astro-ph?searchtype=author&query=Dixon%2C+G">G. Dixon</a>, <a href="/search/astro-ph?searchtype=author&query=Dolesi%2C+R">R. Dolesi</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraioli%2C+L">L. Ferraioli</a>, <a href="/search/astro-ph?searchtype=author&query=Ferroni%2C+V">V. Ferroni</a>, <a href="/search/astro-ph?searchtype=author&query=Fitzsimons%2C+E+D">E. D. Fitzsimons</a>, <a href="/search/astro-ph?searchtype=author&query=Freschi%2C+M">M. Freschi</a>, <a href="/search/astro-ph?searchtype=author&query=Gesa%2C+L">L. Gesa</a>, <a href="/search/astro-ph?searchtype=author&query=Gibert%2C+F">F. Gibert</a>, <a href="/search/astro-ph?searchtype=author&query=Giardini%2C+D">D. Giardini</a>, <a href="/search/astro-ph?searchtype=author&query=Giusteri%2C+R">R. Giusteri</a>, <a href="/search/astro-ph?searchtype=author&query=Grimani%2C+C">C. Grimani</a>, <a href="/search/astro-ph?searchtype=author&query=Grzymisch%2C+J">J. Grzymisch</a> , et al. (57 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="1905.09060v1-abstract-short" style="display: inline;"> LISA Pathfinder (LPF) was a technology pioneering mission designed to test key technologies required for gravitational wave detection in space. In the low frequency regime (milli-Hertz and below), where space-based gravitational wave observatories will operate, temperature fluctuations play a crucial role since they can couple into the interferometric measurement and the test masses' free-fall acc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.09060v1-abstract-full').style.display = 'inline'; document.getElementById('1905.09060v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1905.09060v1-abstract-full" style="display: none;"> LISA Pathfinder (LPF) was a technology pioneering mission designed to test key technologies required for gravitational wave detection in space. In the low frequency regime (milli-Hertz and below), where space-based gravitational wave observatories will operate, temperature fluctuations play a crucial role since they can couple into the interferometric measurement and the test masses' free-fall accuracy in many ways. A dedicated temperature measurement subsystem, with noise levels in 10$\,渭$K$\,$Hz$^{-1/2}$ down to $1\,$mHz was part of the diagnostics unit on board LPF. In this paper we report on the temperature measurements throughout mission operations, characterize the thermal environment, estimate transfer functions between different locations and report temperature stability (and its time evolution) at frequencies as low as 10$\,渭$Hz, where typically values around $1\,$K$\,$Hz$^{-1/2}$ were measured. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.09060v1-abstract-full').style.display = 'none'; document.getElementById('1905.09060v1-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 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">13 pages, 16 figures. MNRAS LaTeX style file version 3.0</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Mon.Not.Roy.Astron.Soc 486 (2019) no.3, 3368-3379 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.04694">arXiv:1904.04694</a> <span> [<a href="https://arxiv.org/pdf/1904.04694">pdf</a>, <a href="https://arxiv.org/ps/1904.04694">ps</a>, <a href="https://arxiv.org/format/1904.04694">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ab0c99">10.3847/1538-4357/ab0c99 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Forbush decreases and $<$ 2-day GCR flux non-recurrent variations studied with LISA Pathfinder </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Grimani%2C+C">C. Grimani</a>, <a href="/search/astro-ph?searchtype=author&query=Armano%2C+M">M. Armano</a>, <a href="/search/astro-ph?searchtype=author&query=Audley%2C+H">H. Audley</a>, <a href="/search/astro-ph?searchtype=author&query=Baird%2C+J">J. Baird</a>, <a href="/search/astro-ph?searchtype=author&query=Benella%2C+S">S. Benella</a>, <a href="/search/astro-ph?searchtype=author&query=Binetruy%2C+P">P. Binetruy</a>, <a href="/search/astro-ph?searchtype=author&query=Born%2C+M">M. Born</a>, <a href="/search/astro-ph?searchtype=author&query=Bortoluzzi%2C+D">D. Bortoluzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Castelli%2C+E">E. Castelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cavalleri%2C+A">A. Cavalleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cesarini%2C+A">A. Cesarini</a>, <a href="/search/astro-ph?searchtype=author&query=Cruise%2C+A+M">A. M. Cruise</a>, <a href="/search/astro-ph?searchtype=author&query=Danzmann%2C+K">K. Danzmann</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+M+d+D">M. de Deus Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Diepholz%2C+I">I. Diepholz</a>, <a href="/search/astro-ph?searchtype=author&query=Dixon%2C+G">G. Dixon</a>, <a href="/search/astro-ph?searchtype=author&query=Dolesi%2C+R">R. Dolesi</a>, <a href="/search/astro-ph?searchtype=author&query=Fabi%2C+M">M. Fabi</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraioli%2C+L">L. Ferraioli</a>, <a href="/search/astro-ph?searchtype=author&query=Ferroni%2C+V">V. Ferroni</a>, <a href="/search/astro-ph?searchtype=author&query=Finetti%2C+N">N. Finetti</a>, <a href="/search/astro-ph?searchtype=author&query=Fitzsimons%2C+E+D">E. D. Fitzsimons</a>, <a href="/search/astro-ph?searchtype=author&query=Freschi%2C+M">M. Freschi</a>, <a href="/search/astro-ph?searchtype=author&query=Gesa%2C+L">L. Gesa</a>, <a href="/search/astro-ph?searchtype=author&query=Gibert%2C+F">F. Gibert</a> , et al. (60 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="1904.04694v1-abstract-short" style="display: inline;"> Non-recurrent short term variations of the galactic cosmic-ray (GCR) flux above 70 MeV n$^{-1}$ were observed between 2016 February 18 and 2017 July 3 aboard the European Space Agency LISA Pathfinder (LPF) mission orbiting around the Lagrange point L1 at 1.5$\times$10$^6$ km from Earth. The energy dependence of three Forbush decreases (FDs) is studied and reported here. A comparison of these obser… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.04694v1-abstract-full').style.display = 'inline'; document.getElementById('1904.04694v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.04694v1-abstract-full" style="display: none;"> Non-recurrent short term variations of the galactic cosmic-ray (GCR) flux above 70 MeV n$^{-1}$ were observed between 2016 February 18 and 2017 July 3 aboard the European Space Agency LISA Pathfinder (LPF) mission orbiting around the Lagrange point L1 at 1.5$\times$10$^6$ km from Earth. The energy dependence of three Forbush decreases (FDs) is studied and reported here. A comparison of these observations with others carried out in space down to the energy of a few tens of MeV n$^{-1}$ shows that the same GCR flux parameterization applies to events of different intensity during the main phase. FD observations in L1 with LPF and geomagnetic storm occurrence is also presented. Finally, the characteristics of GCR flux non-recurrent variations (peaks and depressions) of duration $<$ 2 days and their association with interplanetary structures are investigated. It is found that, most likely, plasma compression regions between subsequent corotating high-speed streams cause peaks, while heliospheric current sheet crossing cause the majority of the depressions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.04694v1-abstract-full').style.display = 'none'; document.getElementById('1904.04694v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 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">Journal ref:</span> M. Armano et al 2019 ApJ 874 167 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1903.08924">arXiv:1903.08924</a> <span> [<a href="https://arxiv.org/pdf/1903.08924">pdf</a>, <a href="https://arxiv.org/format/1903.08924">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"> LISA Pathfinder </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Armano%2C+M">Michele Armano</a>, <a href="/search/astro-ph?searchtype=author&query=Audley%2C+H">Heather Audley</a>, <a href="/search/astro-ph?searchtype=author&query=Baird%2C+J">Jonathon Baird</a>, <a href="/search/astro-ph?searchtype=author&query=Binetruy%2C+P">Pierre Binetruy</a>, <a href="/search/astro-ph?searchtype=author&query=Born%2C+M">Michael Born</a>, <a href="/search/astro-ph?searchtype=author&query=Bortoluzzi%2C+D">Daniele Bortoluzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Castelli%2C+E">Eleanora Castelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cavalleri%2C+A">Antonella Cavalleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cesarini%2C+A">Andrea Cesarini</a>, <a href="/search/astro-ph?searchtype=author&query=Cruise%2C+M">Mike Cruise</a>, <a href="/search/astro-ph?searchtype=author&query=Danzmann%2C+K">Karsten Danzmann</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+M+d+D">Marcus de Deus Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Diepholz%2C+I">Ingo Diepholz</a>, <a href="/search/astro-ph?searchtype=author&query=Dixon%2C+G">George Dixon</a>, <a href="/search/astro-ph?searchtype=author&query=Dolesi%2C+R">Rita Dolesi</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraioli%2C+L">Luigi Ferraioli</a>, <a href="/search/astro-ph?searchtype=author&query=Ferroni%2C+V">Valerio Ferroni</a>, <a href="/search/astro-ph?searchtype=author&query=Fitzsimons%2C+E">Ewan Fitzsimons</a>, <a href="/search/astro-ph?searchtype=author&query=Freschi%2C+M">Mario Freschi</a>, <a href="/search/astro-ph?searchtype=author&query=Gesa%2C+L">Luis Gesa</a>, <a href="/search/astro-ph?searchtype=author&query=Gibert%2C+F">Ferran Gibert</a>, <a href="/search/astro-ph?searchtype=author&query=Giardini%2C+D">Domenico Giardini</a>, <a href="/search/astro-ph?searchtype=author&query=Giusteri%2C+R">Roberta Giusteri</a>, <a href="/search/astro-ph?searchtype=author&query=Grimani%2C+C">Catia Grimani</a>, <a href="/search/astro-ph?searchtype=author&query=Grzymisch%2C+J">Jonathan Grzymisch</a> , et al. (53 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="1903.08924v1-abstract-short" style="display: inline;"> Since the 2017 Nobel Prize in Physics was awarded for the observation of gravitational waves, it is fair to say that the epoch of gravitational wave astronomy (GWs) has begun. However, a number of interesting sources of GWs can only be observed from space. To demonstrate the feasibility of the Laser Interferometer Space Antenna (LISA), a future gravitational wave observatory in space, the LISA Pat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.08924v1-abstract-full').style.display = 'inline'; document.getElementById('1903.08924v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.08924v1-abstract-full" style="display: none;"> Since the 2017 Nobel Prize in Physics was awarded for the observation of gravitational waves, it is fair to say that the epoch of gravitational wave astronomy (GWs) has begun. However, a number of interesting sources of GWs can only be observed from space. To demonstrate the feasibility of the Laser Interferometer Space Antenna (LISA), a future gravitational wave observatory in space, the LISA Pathfinder satellite was launched on December, 3rd 2015. Measurements of the spurious forces accelerating an otherwise free-falling test mass, and detailed investigations of the individual subsystems needed to achieve the free-fall, have been conducted throughout the mission. This overview article starts with the purpose and aim of the mission, explains satellite hardware and mission operations and ends with a summary of selected important results and an outlook towards LISA. From the LISA Pathfinder experience, we can conclude that the proposed LISA mission is feasible. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.08924v1-abstract-full').style.display = 'none'; document.getElementById('1903.08924v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">Preprint of an article submitted for consideration in Lepton-Photon 2017 conference proceedings 漏2019 copyright World Scientific Publishing Company</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1812.05491">arXiv:1812.05491</a> <span> [<a href="https://arxiv.org/pdf/1812.05491">pdf</a>, <a href="https://arxiv.org/format/1812.05491">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/10.1103/PhysRevD.99.082001">10.1103/PhysRevD.99.082001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LISA Pathfinder Platform Stability and Drag-free Performance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Armano%2C+M">Michele Armano</a>, <a href="/search/astro-ph?searchtype=author&query=Audley%2C+H">Heather Audley</a>, <a href="/search/astro-ph?searchtype=author&query=Baird%2C+J">Jonathon Baird</a>, <a href="/search/astro-ph?searchtype=author&query=Binetruy%2C+P">Pierre Binetruy</a>, <a href="/search/astro-ph?searchtype=author&query=Born%2C+M">Michael Born</a>, <a href="/search/astro-ph?searchtype=author&query=Bortoluzzi%2C+D">Daniele Bortoluzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Castelli%2C+E">Eleanora Castelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cavalleri%2C+A">Antonella Cavalleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cesarini%2C+A">Andrea Cesarini</a>, <a href="/search/astro-ph?searchtype=author&query=Cruise%2C+M">Mike Cruise</a>, <a href="/search/astro-ph?searchtype=author&query=Danzmann%2C+K">Karsten Danzmann</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+M+d+D">Marcus de Deus Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Diepholz%2C+I">Igo Diepholz</a>, <a href="/search/astro-ph?searchtype=author&query=Dixon%2C+G">George Dixon</a>, <a href="/search/astro-ph?searchtype=author&query=Dolesi%2C+R">Rita Dolesi</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraioli%2C+L">Luigi Ferraioli</a>, <a href="/search/astro-ph?searchtype=author&query=Ferroni%2C+V">Valerio Ferroni</a>, <a href="/search/astro-ph?searchtype=author&query=Fitzsimons%2C+E">Ewan Fitzsimons</a>, <a href="/search/astro-ph?searchtype=author&query=Freschi%2C+M">Mario Freschi</a>, <a href="/search/astro-ph?searchtype=author&query=Gesa%2C+L">Luis Gesa</a>, <a href="/search/astro-ph?searchtype=author&query=Gibert%2C+F">Ferran Gibert</a>, <a href="/search/astro-ph?searchtype=author&query=Giardini%2C+D">Domenico Giardini</a>, <a href="/search/astro-ph?searchtype=author&query=Giusteri%2C+R">Roberta Giusteri</a>, <a href="/search/astro-ph?searchtype=author&query=Grimani%2C+C">Catia Grimani</a>, <a href="/search/astro-ph?searchtype=author&query=Grzymisch%2C+J">Jonathan Grzymisch</a> , et al. (53 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="1812.05491v1-abstract-short" style="display: inline;"> The science operations of the LISA Pathfinder mission has demonstrated the feasibility of sub-femto-g free-fall of macroscopic test masses necessary to build a LISA-like gravitational wave observatory in space. While the main focus of interest, i.e. the optical axis or the $x$-axis, has been extensively studied, it is also of interest to evaluate the stability of the spacecraft with respect to all… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.05491v1-abstract-full').style.display = 'inline'; document.getElementById('1812.05491v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1812.05491v1-abstract-full" style="display: none;"> The science operations of the LISA Pathfinder mission has demonstrated the feasibility of sub-femto-g free-fall of macroscopic test masses necessary to build a LISA-like gravitational wave observatory in space. While the main focus of interest, i.e. the optical axis or the $x$-axis, has been extensively studied, it is also of interest to evaluate the stability of the spacecraft with respect to all the other degrees of freedom. The current paper is dedicated to such a study, with a focus set on an exhaustive and quantitative evaluation of the imperfections and dynamical effects that impact the stability with respect to its local geodesic. A model of the complete closed-loop system provides a comprehensive understanding of each part of the in-loop coordinates spectra. As will be presented, this model gives very good agreements with LISA Pathfinder flight data. It allows one to identify the physical noise source at the origin and the physical phenomena underlying the couplings. From this, the performances of the stability of the spacecraft, with respect to its geodesic, are extracted as a function of frequency. Close to $1 mHz$, the stability of the spacecraft on the $X_{SC}$, $Y_{SC}$ and $Z_{SC}$ degrees of freedom is shown to be of the order of $5.0\ 10^{-15} m\ s^{-2}/\sqrt{Hz}$ for X and $4.0 \ 10^{-14} m\ s^{-2}/\sqrt{Hz}$ for Y and Z. For the angular degrees of freedom, the values are of the order $3\ 10^{-12} rad\ s^{-2}/\sqrt{Hz}$ for $螛_{SC}$ and $3\ 10^{-13} rad\ s^{-2}/\sqrt{Hz}$ for $H_{SC}$ and $桅_{SC}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.05491v1-abstract-full').style.display = 'none'; document.getElementById('1812.05491v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 December, 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">16 pages, 10 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 99, 082001 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1809.08969">arXiv:1809.08969</a> <span> [<a href="https://arxiv.org/pdf/1809.08969">pdf</a>, <a href="https://arxiv.org/format/1809.08969">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/10.1103/PhysRevD.98.102005">10.1103/PhysRevD.98.102005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Experimental results from the ST7 mission on LISA Pathfinder </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+G">G Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+J">J Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+M">M Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Aveni%2C+G">G Aveni</a>, <a href="/search/astro-ph?searchtype=author&query=Bame%2C+D">D Bame</a>, <a href="/search/astro-ph?searchtype=author&query=Barela%2C+P">P Barela</a>, <a href="/search/astro-ph?searchtype=author&query=Blackman%2C+K">K Blackman</a>, <a href="/search/astro-ph?searchtype=author&query=Carmain%2C+A">A Carmain</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+L">L Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cherng%2C+M">M Cherng</a>, <a href="/search/astro-ph?searchtype=author&query=Clark%2C+S">S Clark</a>, <a href="/search/astro-ph?searchtype=author&query=Connally%2C+M">M Connally</a>, <a href="/search/astro-ph?searchtype=author&query=Connolly%2C+W">W Connolly</a>, <a href="/search/astro-ph?searchtype=author&query=Conroy%2C+D">D Conroy</a>, <a href="/search/astro-ph?searchtype=author&query=Cooper%2C+M">M Cooper</a>, <a href="/search/astro-ph?searchtype=author&query=Cutler%2C+C">C Cutler</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Agostino%2C+J">J D'Agostino</a>, <a href="/search/astro-ph?searchtype=author&query=Demmons%2C+N">N Demmons</a>, <a href="/search/astro-ph?searchtype=author&query=Dorantes%2C+E">E Dorantes</a>, <a href="/search/astro-ph?searchtype=author&query=Dunn%2C+C">C Dunn</a>, <a href="/search/astro-ph?searchtype=author&query=Duran%2C+M">M Duran</a>, <a href="/search/astro-ph?searchtype=author&query=Ehrbar%2C+E">E Ehrbar</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+J">J Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandez%2C+J">J Fernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Franklin%2C+G">G Franklin</a> , et al. (123 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1809.08969v2-abstract-short" style="display: inline;"> The Space Technology 7 Disturbance Reduction System (ST7-DRS) is a NASA technology demonstration payload that operated from January 2016 through July of 2017 on the European Space Agency's LISA Pathfinder spacecraft. The joint goal of the NASA and ESA missions was to validate key technologies for a future space-based gravitational wave observatory targeting the source-rich milliHertz band. The two… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.08969v2-abstract-full').style.display = 'inline'; document.getElementById('1809.08969v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1809.08969v2-abstract-full" style="display: none;"> The Space Technology 7 Disturbance Reduction System (ST7-DRS) is a NASA technology demonstration payload that operated from January 2016 through July of 2017 on the European Space Agency's LISA Pathfinder spacecraft. The joint goal of the NASA and ESA missions was to validate key technologies for a future space-based gravitational wave observatory targeting the source-rich milliHertz band. The two primary components of ST7-DRS are a micropropulsion system based on colloidal micro-Newton thrusters (CMNTs) and a control system that simultaneously controls the attitude and position of the spacecraft and the two free-flying test masses (TMs). This paper presents our main experimental results and summarizes the overall the performance of the CMNTs and control laws. We find that the CMNT performance to be consistent with pre-flight predictions, with a measured system thrust noise on the order of $100\,\textrm{nN}/\sqrt{\textrm{Hz}}$ in the $1\,\textrm{mHz}\leq f \leq 30\,\textrm{mHz}$ band. The control system maintained the TM-spacecraft separation with an RMS error of less than 2$\,$nm and a noise spectral density of less than $3\,\textrm{nm}/\sqrt{\textrm{Hz}}$ in the same band. Thruster calibration measurements yield thrust values consistent with the performance model and ground-based thrust-stand measurements, to within a few percent. We also report a differential acceleration noise between the two test masses with a spectral density of roughly $3\,\textrm{fm}/\textrm{s}^2/\sqrt{\textrm{Hz}}$ in the $1\,\textrm{mHz}\leq f \leq 30\,\textrm{mHz}$ band, slightly less than twice as large as the best performance reported with the baseline LISA Pathfinder configuration and below the current requirements for the Laser Interferometer Space Antenna (LISA) mission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.08969v2-abstract-full').style.display = 'none'; document.getElementById('1809.08969v2-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 October, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 September, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 98, 102005 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1806.08581">arXiv:1806.08581</a> <span> [<a href="https://arxiv.org/pdf/1806.08581">pdf</a>, <a href="https://arxiv.org/format/1806.08581">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/10.1103/PhysRevD.97.122002">10.1103/PhysRevD.97.122002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Calibrating the system dynamics of LISA Pathfinder </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Armano%2C+M">M. Armano</a>, <a href="/search/astro-ph?searchtype=author&query=Audley%2C+H">H. Audley</a>, <a href="/search/astro-ph?searchtype=author&query=Baird%2C+J">J. Baird</a>, <a href="/search/astro-ph?searchtype=author&query=Binetruy%2C+P">P. Binetruy</a>, <a href="/search/astro-ph?searchtype=author&query=Born%2C+M">M. Born</a>, <a href="/search/astro-ph?searchtype=author&query=Bortoluzzi%2C+D">D. Bortoluzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Castelli%2C+E">E. Castelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cavalleri%2C+A">A. Cavalleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cesarini%2C+A">A. Cesarini</a>, <a href="/search/astro-ph?searchtype=author&query=Cruise%2C+A+M">A. M. Cruise</a>, <a href="/search/astro-ph?searchtype=author&query=Danzmann%2C+K">K. Danzmann</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+M+d+D">M. de Deus Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Diepholz%2C+I">I. Diepholz</a>, <a href="/search/astro-ph?searchtype=author&query=Dixon%2C+G">G. Dixon</a>, <a href="/search/astro-ph?searchtype=author&query=Dolesi%2C+R">R. Dolesi</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraioli%2C+L">L. Ferraioli</a>, <a href="/search/astro-ph?searchtype=author&query=Ferroni%2C+V">V. Ferroni</a>, <a href="/search/astro-ph?searchtype=author&query=Fitzsimons%2C+E+D">E. D. Fitzsimons</a>, <a href="/search/astro-ph?searchtype=author&query=Freschi%2C+M">M. Freschi</a>, <a href="/search/astro-ph?searchtype=author&query=Gesa%2C+L">L. Gesa</a>, <a href="/search/astro-ph?searchtype=author&query=Gibert%2C+F">F. Gibert</a>, <a href="/search/astro-ph?searchtype=author&query=Giardini%2C+D">D. Giardini</a>, <a href="/search/astro-ph?searchtype=author&query=Giusteri%2C+R">R. Giusteri</a>, <a href="/search/astro-ph?searchtype=author&query=Grimani%2C+C">C. Grimani</a>, <a href="/search/astro-ph?searchtype=author&query=Grzymisch%2C+J">J. Grzymisch</a> , et al. (53 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="1806.08581v1-abstract-short" style="display: inline;"> LISA Pathfinder (LPF) was a European Space Agency mission with the aim to test key technologies for future space-borne gravitational-wave observatories like LISA. The main scientific goal of LPF was to demonstrate measurements of differential acceleration between free-falling test masses at the sub-femto-g level, and to understand the residual acceleration in terms of a physical model of stray for… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.08581v1-abstract-full').style.display = 'inline'; document.getElementById('1806.08581v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1806.08581v1-abstract-full" style="display: none;"> LISA Pathfinder (LPF) was a European Space Agency mission with the aim to test key technologies for future space-borne gravitational-wave observatories like LISA. The main scientific goal of LPF was to demonstrate measurements of differential acceleration between free-falling test masses at the sub-femto-g level, and to understand the residual acceleration in terms of a physical model of stray forces, and displacement readout noise. A key step toward reaching the LPF goals was the correct calibration of the dynamics of LPF, which was a three-body system composed by two test-masses enclosed in a single spacecraft, and subject to control laws for system stability. In this work, we report on the calibration procedures adopted to calculate the residual differential stray force per unit mass acting on the two test-masses in their nominal positions. The physical parameters of the adopted dynamical model are presented, together with their role on LPF performance. The analysis and results of these experiments show that the dynamics of the system was accurately modeled and the dynamical parameters were stationary throughout the mission. Finally, the impact and importance of calibrating system dynamics for future space-based gravitational wave observatories is discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.08581v1-abstract-full').style.display = 'none'; document.getElementById('1806.08581v1-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 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 97, 122002 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1711.07427">arXiv:1711.07427</a> <span> [<a href="https://arxiv.org/pdf/1711.07427">pdf</a>, <a href="https://arxiv.org/format/1711.07427">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.2018.01.006">10.1016/j.astropartphys.2018.01.006 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measuring the Galactic Cosmic Ray Flux with the LISA Pathfinder Radiation Monitor </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Armano%2C+M">M Armano</a>, <a href="/search/astro-ph?searchtype=author&query=Audley%2C+H">H Audley</a>, <a href="/search/astro-ph?searchtype=author&query=Baird%2C+J">J Baird</a>, <a href="/search/astro-ph?searchtype=author&query=Binetruy%2C+P">P Binetruy</a>, <a href="/search/astro-ph?searchtype=author&query=Born%2C+M">M Born</a>, <a href="/search/astro-ph?searchtype=author&query=Bortoluzzi%2C+D">D Bortoluzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Castelli%2C+E">E Castelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cavalleri%2C+A">A Cavalleri</a>, <a href="/search/astro-ph?searchtype=author&query=Cesarini%2C+A">A Cesarini</a>, <a href="/search/astro-ph?searchtype=author&query=Cruise%2C+M">M Cruise</a>, <a href="/search/astro-ph?searchtype=author&query=Danzmann%2C+K">K Danzmann</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+M+d+D">M de Deus Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Diepholz%2C+I">I Diepholz</a>, <a href="/search/astro-ph?searchtype=author&query=Dixon%2C+G">G Dixon</a>, <a href="/search/astro-ph?searchtype=author&query=Dolesi%2C+R">R Dolesi</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraioli%2C+L">L Ferraioli</a>, <a href="/search/astro-ph?searchtype=author&query=Ferroni%2C+V">V Ferroni</a>, <a href="/search/astro-ph?searchtype=author&query=Finetti%2C+N">N Finetti</a>, <a href="/search/astro-ph?searchtype=author&query=Fitzsimons%2C+E+D">E D Fitzsimons</a>, <a href="/search/astro-ph?searchtype=author&query=Freschi%2C+M">M Freschi</a>, <a href="/search/astro-ph?searchtype=author&query=Gesa%2C+L">L Gesa</a>, <a href="/search/astro-ph?searchtype=author&query=Gibert%2C+F">F Gibert</a>, <a href="/search/astro-ph?searchtype=author&query=Giardini%2C+D">D Giardini</a>, <a href="/search/astro-ph?searchtype=author&query=Giusteri%2C+R">R Giusteri</a>, <a href="/search/astro-ph?searchtype=author&query=Grimani%2C+C">C Grimani</a> , et al. (54 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="1711.07427v2-abstract-short" style="display: inline;"> Test mass charging caused by cosmic rays will be a significant source of acceleration noise for space-based gravitational wave detectors like LISA. Operating between December 2015 and July 2017, the technology demonstration mission LISA Pathfinder included a bespoke monitor to help characterise the relationship between test mass charging and the local radiation environment. The radiation monitor m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.07427v2-abstract-full').style.display = 'inline'; document.getElementById('1711.07427v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1711.07427v2-abstract-full" style="display: none;"> Test mass charging caused by cosmic rays will be a significant source of acceleration noise for space-based gravitational wave detectors like LISA. Operating between December 2015 and July 2017, the technology demonstration mission LISA Pathfinder included a bespoke monitor to help characterise the relationship between test mass charging and the local radiation environment. The radiation monitor made in situ measurements of the cosmic ray flux while also providing information about its energy spectrum. We describe the monitor and present measurements which show a gradual 40% increase in count rate coinciding with the declining phase of the solar cycle. Modulations of up to 10% were also observed with periods of 13 and 26 days that are associated with co-rotating interaction regions and heliospheric current sheet crossings. These variations in the flux above the monitor detection threshold (approximately 70 MeV) are shown to be coherent with measurements made by the IREM monitor on-board the Earth orbiting INTEGRAL spacecraft. Finally we use the measured deposited energy spectra, in combination with a GEANT4 model, to estimate the galactic cosmic ray differential energy spectrum over the course of the mission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.07427v2-abstract-full').style.display = 'none'; document.getElementById('1711.07427v2-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, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 November, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2017. </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 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