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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/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/2211.09987">arXiv:2211.09987</a> <span> [<a href="https://arxiv.org/pdf/2211.09987">pdf</a>, <a href="https://arxiv.org/format/2211.09987">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.107.022010">10.1103/PhysRevD.107.022010 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Simulating the charging of isolated free-falling masses from TeV to eV energies: detailed comparison with LISA Pathfinder results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wass%2C+P+J">P. J. Wass</a>, <a href="/search/astro-ph?searchtype=author&query=Sumner%2C+T+J">T. J. Sumner</a>, <a href="/search/astro-ph?searchtype=author&query=Ara%C3%BAjo%2C+H+M">H. M Ara煤jo</a>, <a href="/search/astro-ph?searchtype=author&query=Hollington%2C+D">D. Hollington</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="2211.09987v2-abstract-short" style="display: inline;"> A model is presented that explains the charging rate of the LISA Pathfinder test masses by the interplanetary cosmic ray environment. The model incorporates particle-tracking from TeV to eV energies using a combination of GEANT4 and a custom low-energy particle generation and tracking code. The electrostatic environment of the test mass is simulated allowing for a comparison of the test-mass charg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.09987v2-abstract-full').style.display = 'inline'; document.getElementById('2211.09987v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.09987v2-abstract-full" style="display: none;"> A model is presented that explains the charging rate of the LISA Pathfinder test masses by the interplanetary cosmic ray environment. The model incorporates particle-tracking from TeV to eV energies using a combination of GEANT4 and a custom low-energy particle generation and tracking code. The electrostatic environment of the test mass is simulated allowing for a comparison of the test-mass charging-rate dependence on local electric fields with observations made in orbit. The model is able to reproduce the observed charging behavior with good accuracy using gold surface properties compatible with literature values. The results of the model confirm that a significant fraction of the net charging current is caused by a population of low-energy ($\sim$eV) electrons produced by electron- and ion-induced kinetic emission from the test mass and surrounding metal surfaces. Assuming a gold work function of 4.2 eV, the unbalanced flow of these electrons to and from the unbiased test mass contributes $\sim$10% of the overall test mass charging rate. Their contribution to the charging-current shot noise is disproportionately higher and it adds $\sim$40% to the overall predicted noise. However, even with this increased noise contribution the overall charging-current noise is still only 40% of that measured in-orbit, and this remains an unsolved issue. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.09987v2-abstract-full').style.display = 'none'; document.getElementById('2211.09987v2-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 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">20 pages, 10 figures. Accepted by Physical Review D</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, 022010 (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/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/2005.00917">arXiv:2005.00917</a> <span> [<a href="https://arxiv.org/pdf/2005.00917">pdf</a>, <a href="https://arxiv.org/format/2005.00917">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.102.042002">10.1103/PhysRevD.102.042002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Numerical Modeling and Experimental Demonstration of Pulsed Charge Control for the Space Inertial Sensor used in LISA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Inchausp%C3%A9%2C+H">Henri Inchausp茅</a>, <a href="/search/astro-ph?searchtype=author&query=Olatunde%2C+T">Taiwo Olatunde</a>, <a href="/search/astro-ph?searchtype=author&query=Apple%2C+S">Stephen Apple</a>, <a href="/search/astro-ph?searchtype=author&query=Parry%2C+S">Samantha Parry</a>, <a href="/search/astro-ph?searchtype=author&query=Letson%2C+B">Ben Letson</a>, <a href="/search/astro-ph?searchtype=author&query=Turetta%2C+N">Nicholas Turetta</a>, <a href="/search/astro-ph?searchtype=author&query=Mueller%2C+G">Guido Mueller</a>, <a href="/search/astro-ph?searchtype=author&query=Wass%2C+P+J">Peter J Wass</a>, <a href="/search/astro-ph?searchtype=author&query=Conklin%2C+J+W">John W Conklin</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2005.00917v1-abstract-short" style="display: inline;"> Electrostatic charge control of isolated free-falling test masses is a key enabling technology for space-based gravitational missions. Contact-free electrostatic charge control can be achieved using photoelectron emission from metal surfaces under illumination with deep UV light. A contact-free method minimizes force disturbances that can perturb measurements or interrupt science operations. In th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.00917v1-abstract-full').style.display = 'inline'; document.getElementById('2005.00917v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.00917v1-abstract-full" style="display: none;"> Electrostatic charge control of isolated free-falling test masses is a key enabling technology for space-based gravitational missions. Contact-free electrostatic charge control can be achieved using photoelectron emission from metal surfaces under illumination with deep UV light. A contact-free method minimizes force disturbances that can perturb measurements or interrupt science operations. In this paper we present charge control experiments using a gravitational reference sensor geometry relevant to the Laser Interferometer Space Antenna (LISA) gravitational wave observatory in a torsion pendulum apparatus. We use a UV LED light source to control the test mass potential, taking advantage of their high bandwidth to phase-lock the light output to 100kHz electric fields used for capacitive position sensing of the test mass. We demonstrate charge-rate and test mass potential control by adjustment of the phase of the light with respect to the electric field. We present a simple physics-based model of the discharging process which explains our experimental results in terms of the UV light distribution in the sensor, surface work functions and quantum yields. A robust fitting method is used to determine the best-fit physical parameters of the model that describe the system <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.00917v1-abstract-full').style.display = 'none'; document.getElementById('2005.00917v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 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">Journal ref:</span> Phys. Rev. D 102, 042002 (2020) </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/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/1702.04633">arXiv:1702.04633</a> <span> [<a href="https://arxiv.org/pdf/1702.04633">pdf</a>, <a href="https://arxiv.org/ps/1702.04633">ps</a>, <a href="https://arxiv.org/format/1702.04633">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/PhysRevLett.118.171101">10.1103/PhysRevLett.118.171101 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Charge-induced force-noise on free-falling test masses: results from 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=Auger%2C+G">G. Auger</a>, <a href="/search/astro-ph?searchtype=author&query=Baird%2C+J+T">J. T. 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=Brandt%2C+N">N. Brandt</a>, <a href="/search/astro-ph?searchtype=author&query=Bursi%2C+A">A. Bursi</a>, <a href="/search/astro-ph?searchtype=author&query=Caleno%2C+M">M. Caleno</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=Dolesi%2C+R">R. Dolesi</a>, <a href="/search/astro-ph?searchtype=author&query=Dunbar%2C+N">N. Dunbar</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=Flatscher%2C+R">R. Flatscher</a>, <a href="/search/astro-ph?searchtype=author&query=Freschi%2C+M">M. Freschi</a>, <a href="/search/astro-ph?searchtype=author&query=Gallegos%2C+J">J. Gallegos</a>, <a href="/search/astro-ph?searchtype=author&query=Marirrodriga%2C+C+G">C. Garc铆a Marirrodriga</a> , et al. (69 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="1702.04633v1-abstract-short" style="display: inline;"> We report on electrostatic measurements made on board the European Space Agency mission LISA Pathfinder. Detailed measurements of the charge-induced electrostatic forces exerted on free-falling test masses (TMs) inside the capacitive gravitational reference sensor are the first made in a relevant environment for a space-based gravitational wave detector. Employing a combination of charge control a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1702.04633v1-abstract-full').style.display = 'inline'; document.getElementById('1702.04633v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1702.04633v1-abstract-full" style="display: none;"> We report on electrostatic measurements made on board the European Space Agency mission LISA Pathfinder. Detailed measurements of the charge-induced electrostatic forces exerted on free-falling test masses (TMs) inside the capacitive gravitational reference sensor are the first made in a relevant environment for a space-based gravitational wave detector. Employing a combination of charge control and electric-field compensation, we show that the level of charge-induced acceleration noise on a single TM can be maintained at a level close to 1.0 fm/s^2/sqrt(Hz) across the 0.1-100 mHz frequency band that is crucial to an observatory such as LISA. Using dedicated measurements that detect these effects in the differential acceleration between the two test masses, we resolve the stochastic nature of the TM charge build up due to interplanetary cosmic rays and the TM charge-to-force coupling through stray electric fields in the sensor. All our measurements are in good agreement with predictions based on a relatively simple electrostatic model of the LISA Pathfinder instrument. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1702.04633v1-abstract-full').style.display = 'none'; document.getElementById('1702.04633v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 February, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 Pages, 3 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 118, 171101 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1508.00812">arXiv:1508.00812</a> <span> [<a href="https://arxiv.org/pdf/1508.00812">pdf</a>, <a href="https://arxiv.org/format/1508.00812">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0264-9381/32/23/235020">10.1088/0264-9381/32/23/235020 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterising and Testing Deep UV LEDs for Use in Space Applications </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hollington%2C+D">D. Hollington</a>, <a href="/search/astro-ph?searchtype=author&query=Baird%2C+J+T">J. T. Baird</a>, <a href="/search/astro-ph?searchtype=author&query=Sumner%2C+T+J">T. J. Sumner</a>, <a href="/search/astro-ph?searchtype=author&query=Wass%2C+P+J">P. J. Wass</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1508.00812v1-abstract-short" style="display: inline;"> Deep ultraviolet (DUV) light sources are used to neutralise isolated test masses in highly sensitive space-based gravitational experiments. An example is the LISA Pathfinder charge management system, which uses low-pressure mercury lamps. A future gravitational-wave observatory such as eLISA will use UV light-emitting diodes (UV LEDs), which offer numerous advantages over traditional discharge lam… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.00812v1-abstract-full').style.display = 'inline'; document.getElementById('1508.00812v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1508.00812v1-abstract-full" style="display: none;"> Deep ultraviolet (DUV) light sources are used to neutralise isolated test masses in highly sensitive space-based gravitational experiments. An example is the LISA Pathfinder charge management system, which uses low-pressure mercury lamps. A future gravitational-wave observatory such as eLISA will use UV light-emitting diodes (UV LEDs), which offer numerous advantages over traditional discharge lamps. Such devices have limited space heritage but are are now available from a number of commercial suppliers. Here we report on a test campaign that was carried out to quantify the general properties of three types of commercially available UV LEDs and demonstrate their suitability for use in space. Testing included general electrical and UV output measurements, spectral stability, pulsed performance, temperature dependence as well as thermal vacuum, radiation and vibration survivability. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.00812v1-abstract-full').style.display = 'none'; document.getElementById('1508.00812v1-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, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2015. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1108.3254">arXiv:1108.3254</a> <span> [<a href="https://arxiv.org/pdf/1108.3254">pdf</a>, <a href="https://arxiv.org/ps/1108.3254">ps</a>, <a href="https://arxiv.org/format/1108.3254">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="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.84.063007">10.1103/PhysRevD.84.063007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Brownian force noise from molecular collisions and the sensitivity of advanced gravitational wave observatories </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dolesi%2C+R">R. Dolesi</a>, <a href="/search/astro-ph?searchtype=author&query=Hueller%2C+M">M. Hueller</a>, <a href="/search/astro-ph?searchtype=author&query=Nicolodi%2C+D">D. Nicolodi</a>, <a href="/search/astro-ph?searchtype=author&query=Tombolato%2C+D">D. Tombolato</a>, <a href="/search/astro-ph?searchtype=author&query=Vitale%2C+S">S. Vitale</a>, <a href="/search/astro-ph?searchtype=author&query=Wass%2C+P+J">P. J. Wass</a>, <a href="/search/astro-ph?searchtype=author&query=Weber%2C+W+J">W. J. Weber</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+M">M. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Fritschel%2C+P">P. Fritschel</a>, <a href="/search/astro-ph?searchtype=author&query=Weiss%2C+R">R. Weiss</a>, <a href="/search/astro-ph?searchtype=author&query=Gundlach%2C+J+H">J. H. Gundlach</a>, <a href="/search/astro-ph?searchtype=author&query=Hagedorn%2C+C+A">C. A. Hagedorn</a>, <a href="/search/astro-ph?searchtype=author&query=Schlamminger%2C+S">S. Schlamminger</a>, <a href="/search/astro-ph?searchtype=author&query=Ciani%2C+G">G. Ciani</a>, <a href="/search/astro-ph?searchtype=author&query=Cavalleri%2C+A">A. Cavalleri</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="1108.3254v2-abstract-short" style="display: inline;"> We present an analysis of Brownian force noise from residual gas damping of reference test masses as a fundamental sensitivity limit in small force experiments. The resulting acceleration noise increases significantly when the distance of the test mass to the surrounding experimental apparatus is smaller than the dimension of the test mass itself. For the Advanced LIGO interferometric gravitationa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1108.3254v2-abstract-full').style.display = 'inline'; document.getElementById('1108.3254v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1108.3254v2-abstract-full" style="display: none;"> We present an analysis of Brownian force noise from residual gas damping of reference test masses as a fundamental sensitivity limit in small force experiments. The resulting acceleration noise increases significantly when the distance of the test mass to the surrounding experimental apparatus is smaller than the dimension of the test mass itself. For the Advanced LIGO interferometric gravitational wave observatory, where the relevant test mass is a suspended 340 mm diameter cylindrical end mirror, the force noise power is increased by roughly a factor 40 by the presence of a similarly shaped reaction mass at a nominal separation of 5 mm. The force noise, of order 20 fN\rthz\ for $2 \times 10^{-6}$ Pa of residual H$_2$ gas, rivals quantum optical fluctuations as the dominant noise source between 10 and 30 Hz. We present here a numerical and analytical analysis for the gas damping force noise for Advanced LIGO, backed up by experimental evidence from several recent measurements. Finally, we discuss the impact of residual gas damping on the gravitational wave sensitivity and possible mitigation strategies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1108.3254v2-abstract-full').style.display = 'none'; document.getElementById('1108.3254v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 September, 2011; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 August, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2011. </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 with 9 figures (fixed typos found in proofs)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Physical Review D 84, 063007 (2011) </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 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