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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/2411.14191">arXiv:2411.14191</a> <span> [<a href="https://arxiv.org/pdf/2411.14191">pdf</a>, <a href="https://arxiv.org/format/2411.14191">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"> Post-processing subtraction of tilt-to-length noise in LISA in the presence of gravitational wave signals </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+M">Marie-Sophie Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Paczkowski%2C+S">Sarah Paczkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Hewitson%2C+M">Martin Hewitson</a>, <a href="/search/astro-ph?searchtype=author&query=Heinzel%2C+G">Gerhard Heinzel</a>, <a href="/search/astro-ph?searchtype=author&query=Wanner%2C+G">Gudrun Wanner</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="2411.14191v3-abstract-short" style="display: inline;"> The Laser Interferometer Space Antenna (LISA) will be the first space-based gravitational wave (GW) observatory. It will measure gravitational wave signals in the frequency regime from 0.1 mHz to 1 Hz. The success of these measurements will depend on the suppression of the various instrument noises. One important noise source in LISA will be tilt-to-length (TTL) coupling. Here, it is understood as… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.14191v3-abstract-full').style.display = 'inline'; document.getElementById('2411.14191v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.14191v3-abstract-full" style="display: none;"> The Laser Interferometer Space Antenna (LISA) will be the first space-based gravitational wave (GW) observatory. It will measure gravitational wave signals in the frequency regime from 0.1 mHz to 1 Hz. The success of these measurements will depend on the suppression of the various instrument noises. One important noise source in LISA will be tilt-to-length (TTL) coupling. Here, it is understood as the coupling of angular jitter, predominantly from the spacecraft, into the interferometric length readout. The current plan is to subtract this noise in-flight in post-processing as part of a noise minimization strategy. It is crucial to distinguish TTL coupling well from the GW signals in the same readout to ensure that the noise will be properly modeled. Furthermore, it is important that the subtraction of TTL noise will not degrade the GW signals. In the present manuscript, we show on simulated LISA data and for four different GW signal types that the GW responses have little effect on the quality of the TTL coupling fit and subtraction. Also, the GW signal characteristics were not altered by the TTL coupling subtraction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.14191v3-abstract-full').style.display = 'none'; document.getElementById('2411.14191v3-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.10409">arXiv:2411.10409</a> <span> [<a href="https://arxiv.org/pdf/2411.10409">pdf</a>, <a href="https://arxiv.org/format/2411.10409">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Design of Dedicated Tilt-to-Length Calibration Maneuvers for LISA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wegener%2C+H">Henry Wegener</a>, <a href="/search/astro-ph?searchtype=author&query=Paczkowski%2C+S">Sarah Paczkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+M">Marie-Sophie Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Hewitson%2C+M">Martin Hewitson</a>, <a href="/search/astro-ph?searchtype=author&query=Heinzel%2C+G">Gerhard Heinzel</a>, <a href="/search/astro-ph?searchtype=author&query=Wanner%2C+G">Gudrun Wanner</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="2411.10409v1-abstract-short" style="display: inline;"> Tilts of certain elements within a laser interferometer can undesirably couple into measurements as a form of noise, known as tilt-to-length (TTL) coupling. This TTL coupling is anticipated to be one of the primary noise sources in the Laser Interferometer Space Antenna (LISA) mission, after Time Delay Interferometry (TDI) is applied. Despite the careful interferometer design and calibration on th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.10409v1-abstract-full').style.display = 'inline'; document.getElementById('2411.10409v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.10409v1-abstract-full" style="display: none;"> Tilts of certain elements within a laser interferometer can undesirably couple into measurements as a form of noise, known as tilt-to-length (TTL) coupling. This TTL coupling is anticipated to be one of the primary noise sources in the Laser Interferometer Space Antenna (LISA) mission, after Time Delay Interferometry (TDI) is applied. Despite the careful interferometer design and calibration on the ground, TTL is likely to require in-flight mitigation through post-processing subtraction to achieve the necessary sensitivity. Past research has demonstrated TTL subtraction in simulations through the estimation of 24 linear coupling coefficients using a noise minimization approach. This paper investigates an approach based on performing rotation maneuvers for estimating coupling coefficients with low uncertainties. In this study, we evaluate the feasibility and optimal configurations of such maneuvers to identify the most efficient solutions. We assess the efficacy of TTL calibration maneuvers by modulating either the spacecraft attitude or the Moving Optical Sub-Assembly (MOSA) yaw angle. We found that sinusoidal signals with amplitudes of around 30 nrad and frequencies near 43 mHz are practical and nearly optimal choices for such modulations. Employing different frequencies generates uncorrelated signals, allowing for multiple maneuvers to be executed simultaneously. Our simulations enable us to estimate the TTL coefficients with precision below 15 um/rad (1-sigma, in free space) after a total maneuver time of 20 minutes. The results are compared to the estimation uncertainties that can be achieved without using maneuvers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.10409v1-abstract-full').style.display = 'none'; document.getElementById('2411.10409v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.16475">arXiv:2410.16475</a> <span> [<a href="https://arxiv.org/pdf/2410.16475">pdf</a>, <a href="https://arxiv.org/format/2410.16475">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/10.1088/1361-6382/ada866">10.1088/1361-6382/ada866 <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 -- Uncertainty and Biases </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+M">Marie-Sophie Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Marmor%2C+J">Joshua Marmor</a>, <a href="/search/astro-ph?searchtype=author&query=George%2C+D">Daniel George</a>, <a href="/search/astro-ph?searchtype=author&query=Paczkowski%2C+S">Sarah Paczkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Sanjuan%2C+J">Jose Sanjuan</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="2410.16475v3-abstract-short" style="display: inline;"> The coupling of the angular jitter of the spacecraft and their sub-assemblies with the optical bench and the telescope into the interferometric length readout will be a major noise source in the LISA mission. We refer to this noise as tilt-to-length (TTL) coupling. It will be reduced directly by realignments, and the residual noise will then be subtracted in post-processing. The success of these m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.16475v3-abstract-full').style.display = 'inline'; document.getElementById('2410.16475v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.16475v3-abstract-full" style="display: none;"> The coupling of the angular jitter of the spacecraft and their sub-assemblies with the optical bench and the telescope into the interferometric length readout will be a major noise source in the LISA mission. We refer to this noise as tilt-to-length (TTL) coupling. It will be reduced directly by realignments, and the residual noise will then be subtracted in post-processing. The success of these mitigation strategies depends on an accurate computation of the TTL coupling coefficients. We present here a thorough analysis of the accuracy of the coefficient estimation under different jitter characteristics, angular readout noise levels, and gravitational wave sources. We analyze in which cases the estimates degrade using two estimators, the common least squares estimator and the instrumental variables estimator. Our investigations show that angular readout noise leads to a systematic bias of the least squares estimator, depending on the TTL coupling coefficients, jitter and readout noise level, while the instrumental variable estimator converges to an unbiased result as the data set length increases. We present an equation that predicts the estimation bias of the least squares method due to angular readout noise. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.16475v3-abstract-full').style.display = 'none'; document.getElementById('2410.16475v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.05852">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> <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> <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/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/2305.03667">arXiv:2305.03667</a> <span> [<a href="https://arxiv.org/pdf/2305.03667">pdf</a>, <a href="https://arxiv.org/format/2305.03667">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.108.022008">10.1103/PhysRevD.108.022008 <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: analytical modelling </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+M">Marie-Sophie Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Wanner%2C+G">Gudrun Wanner</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="2305.03667v1-abstract-short" style="display: inline;"> Tilt-to-length coupling was the limiting noise source in LISA Pathfinder between 20 and 200 mHz before subtraction in post-processing. To prevent the adding of sensing noise to the data by the subtraction process, the success of this strategy depended on a previous direct noise reduction by test mass alignment. The exact dependency of the level of tilt-to-length coupling on the set-points of LISA… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.03667v1-abstract-full').style.display = 'inline'; document.getElementById('2305.03667v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.03667v1-abstract-full" style="display: none;"> Tilt-to-length coupling was the limiting noise source in LISA Pathfinder between 20 and 200 mHz before subtraction in post-processing. To prevent the adding of sensing noise to the data by the subtraction process, the success of this strategy depended on a previous direct noise reduction by test mass alignment. The exact dependency of the level of tilt-to-length coupling on the set-points of LISA Pathfinder's test masses was not understood until the end of the mission. Here, we present, for the first time, an analytical tilt-to-length coupling model that describes the coupling noise changes due to the realignments. We report on the different mechanisms, namely the lever arm and piston effect as well as the coupling due to transmissive components, and how they contribute to the full coupling. Further, we show that a pure geometric model would not have been sufficient to describe the coupling in LISA Pathfinder. Therefore, we model also the non-geometric tilt-to-length noise contributions. For the resulting coupling coefficients of the full model, we compute the expected error bars based on the known individual error sources. Also, we validated the analytical model against numerical simulations. A detailed study and thorough understanding of this noise are the basis for a successful analysis of the LISA Pathfinder data with respect to tilt-to-length coupling. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.03667v1-abstract-full').style.display = 'none'; document.getElementById('2305.03667v1-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 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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/2207.06278">arXiv:2207.06278</a> <span> [<a href="https://arxiv.org/pdf/2207.06278">pdf</a>, <a href="https://arxiv.org/format/2207.06278">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Optics">physics.optics</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1088/2040-8986/acc3ac">10.1088/2040-8986/acc3ac <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Non-geometric tilt-to-length coupling in precision interferometry: mechanisms and analytical descriptions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+M">Marie-Sophie Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Schuster%2C+S">S枚nke Schuster</a>, <a href="/search/astro-ph?searchtype=author&query=Heinzel%2C+G">Gerhard Heinzel</a>, <a href="/search/astro-ph?searchtype=author&query=Wanner%2C+G">Gudrun Wanner</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="2207.06278v3-abstract-short" style="display: inline;"> This paper is the second in a set of two investigating tilt-to-length (TTL) coupling. TTL describes the cross-coupling of angular or translational jitter into an interferometric phase signal and is an important noise source in precision interferometers, including space gravitational wave detectors like LISA. We discussed in 10.1088/2040-8986/ac675e the TTL coupling effects originating from optical… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.06278v3-abstract-full').style.display = 'inline'; document.getElementById('2207.06278v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.06278v3-abstract-full" style="display: none;"> This paper is the second in a set of two investigating tilt-to-length (TTL) coupling. TTL describes the cross-coupling of angular or translational jitter into an interferometric phase signal and is an important noise source in precision interferometers, including space gravitational wave detectors like LISA. We discussed in 10.1088/2040-8986/ac675e the TTL coupling effects originating from optical path length changes, i.e. geometric TTL coupling. Within this work, we focus on the wavefront and detector geometry dependent TTL coupling, called non-geometric TTL coupling, in the case of two interfering fundamental Gaussian beams. We characterise the coupling originating from the properties of the interfering beams, i.e. their absolute and relative angle at the detector, their relative offset and the individual beam parameters. Furthermore, we discuss the dependency of the TTL coupling on the geometry of the detecting photodiode. Wherever possible, we provide analytical expressions for the expected TTL coupling effects. We investigate the non-geometric coupling effects originating from beam walk due to the angular or translational jitter of a mirror or a receiving system. These effects are directly compared with the corresponding detected optical path length changes in 10.1088/2040-8986/ac675e. Both together provide the total interferometric readout. We discuss in which cases the geometric and non-geometric TTL effects cancel one-another. Additionally, we list linear TTL contributions that can be used to counteract other TTL effects. Altogether, our results provide key knowledge to minimise the total TTL coupling noise in experiments by design or realignment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.06278v3-abstract-full').style.display = 'none'; document.getElementById('2207.06278v3-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 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.06943">arXiv:2201.06943</a> <span> [<a href="https://arxiv.org/pdf/2201.06943">pdf</a>, <a href="https://arxiv.org/format/2201.06943">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Optics">physics.optics</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/10.1088/2040-8986/ac675e">10.1088/2040-8986/ac675e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Geometric tilt-to-length coupling in precision interferometry: mechanisms and analytical descriptions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+M">Marie-Sophie Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Schuster%2C+S">S枚nke Schuster</a>, <a href="/search/astro-ph?searchtype=author&query=Wanner%2C+G">Gudrun Wanner</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.06943v2-abstract-short" style="display: inline;"> Tilt-to-length coupling is a technical term for the cross-coupling of angular or lateral jitter into an interferometric phase signal. It is an important noise source in precision interferometers and originates either from changes in the optical path lengths or from wavefront and clipping effects. Within this paper, we focus on geometric TTL coupling and categorize it into a number of different mec… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.06943v2-abstract-full').style.display = 'inline'; document.getElementById('2201.06943v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.06943v2-abstract-full" style="display: none;"> Tilt-to-length coupling is a technical term for the cross-coupling of angular or lateral jitter into an interferometric phase signal. It is an important noise source in precision interferometers and originates either from changes in the optical path lengths or from wavefront and clipping effects. Within this paper, we focus on geometric TTL coupling and categorize it into a number of different mechanisms for which we give analytic expressions. We then show that this geometric description is not always sufficient to predict the TTL coupling noise within an interferometer. We, therefore, discuss how understanding the geometric effects allows TTL noise reduction already by smart design choices. Additionally, they can be used to counteract the total measured TTL noise in a system. The presented content applies to a large variety of precision interferometers, including space gravitational wave detectors like LISA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.06943v2-abstract-full').style.display = 'none'; document.getElementById('2201.06943v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.10443">arXiv:2012.10443</a> <span> [<a href="https://arxiv.org/pdf/2012.10443">pdf</a>, <a href="https://arxiv.org/format/2012.10443">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="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/10.1088/1361-6382/abf441">10.1088/1361-6382/abf441 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LION :Laser Interferometer On the mooN </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Amaro-Seoane%2C+P">Pau Amaro-Seoane</a>, <a href="/search/astro-ph?searchtype=author&query=Bischof%2C+L">Lea Bischof</a>, <a href="/search/astro-ph?searchtype=author&query=Carter%2C+J+J">Jonathan J. Carter</a>, <a href="/search/astro-ph?searchtype=author&query=Hartig%2C+M">Marie-Sophie Hartig</a>, <a href="/search/astro-ph?searchtype=author&query=Wilken%2C+D">Dennis Wilken</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.10443v1-abstract-short" style="display: inline;"> Gravitational wave astronomy has now left its infancy and has become an important tool for probing the most violent phenomena in our universe. The LIGO/Virgo-KAGRA collaboration operates ground based detectors which cover the frequency band from 10 Hz to the kHz regime, meanwhile the pulsar timing array and the soon to launch LISA mission will cover frequencies below 0.1 Hz, leaving a gap in detec… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.10443v1-abstract-full').style.display = 'inline'; document.getElementById('2012.10443v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.10443v1-abstract-full" style="display: none;"> Gravitational wave astronomy has now left its infancy and has become an important tool for probing the most violent phenomena in our universe. The LIGO/Virgo-KAGRA collaboration operates ground based detectors which cover the frequency band from 10 Hz to the kHz regime, meanwhile the pulsar timing array and the soon to launch LISA mission will cover frequencies below 0.1 Hz, leaving a gap in detectable gravitational wave frequencies. Here we show how a Laser Interferometer On the mooN (LION) gravitational wave detector would be sensitive to frequencies from sub Hz to kHz. We find that the sensitivity curve is such that LION can measure compact binaries with masses between 10 and 100M at cosmological distances, with redshifts as high as z= 100 and beyond, depending on the spin and the mass ratio of the binaries. LION can detect binaries of compact objects with higher-masses, with very large signal-to-noise ratios, help us tounderstand how supermassive black holes got their colossal masses on the cosmological landscape, and it can observe in detail intermediate-mass ratio inspirals at distances as large as at least 100 Gpc. Compact binaries that never reach the LIGO/Virgo sensitivity band can spend significantamounts of time in the LION band, while sources present in the LISA band can be picked up by the detector and observed until their final merger. Since LION covers the deci-Hertz regime with such large signal-to-noise ratios, it truly achieves the dream of multi messenger astronomy <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.10443v1-abstract-full').style.display = 'none'; document.getElementById('2012.10443v1-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> 18 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to Journal, Open for comments</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> </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 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