The LISA Pathfinder interferometry—hardware and system testing

Audley, H.; Danzmann, K.; Marín, A. F. García; Heinzel, Gerhard; Monsky, A.; Nofrarias, M.; Steier, Frank; Gerardi, Domenico; Gerndt, R.; Hechenblaikner, Gerald; Johann, Ulrich; Luetzow-Wentzky, Peter; Wand, Vinzenz; Antonucci, F.; Armano, M.; Auger, G.; Benedetti, M.; Binétruy, P.; Boatella, C.; Bogenstahl, J.; Bortoluzzi, D.; Bosetti, Paolo; Caleno, M.; Cavalleri, A.; Cesa, M.; Chmeissani, M.; Ciani, G.; Conchillo, A.; Congedo, G.; Cristofolini, I.; Cruise, M.; Marchi, Fabrizio De; Diaz‐Aguiló, Marc; Diepholz, I.; Dixon, G. J.; Dolesi, R.; Fauste, Jorge; Ferraioli, L.; Fertin, D.; Fichter, Walter; Fitzsimons, E.; Freschi, M.; Marirrodriga, C. García; Gesa, L.; Gibert, F.; Giardini, Domenico; Grimani, C.; Grynagier, A.; Guillaume, Bernard; Guzmán, F.; Harrison, I.; Hewitson, M.; Hollington, D.; Hough, J.; Hoyland, D.; Hueller, M.; Huesler, J.; Jeannin, Olivier; Jennrich, O.; Jetzer, Philippe; Johlander, B.; Killow, C. J.; Llamas, Xavier; Lloro, I.; Lobo, Alberto; Maarschalkerweerd, R.; Madden, S.; Mance, D.; Mateos, I.; McNamara, P. W.; Mendes, José F. G.; Mitchell, E.; Nicolini, Davide; Nicolodi, Daniele; Pedersen, Finn; Perreur-Lloyd, M.; Perreca, A.; Plagnol, E.; Prat, P.; Racca, G. D.; Raïs, B.; Ramos‐Castro, J.; Reiche, J.; Pérez, José Antonio; Robertson, D. I.; Rozemeijer, H.; Sanjuán, Jose; Schulte, M.; Shaul, D.; Stagnaro, L.; Strandmoe, S.; Sumner, T. J.; Taylor, A.; Texier, D.; Trenkel, C.; Tombolato, D.; Vitale, S.; Wanner, Gudrun; Ward, H.; Waschke, S.; Wass, Peter; Weber, William J.; Zweifel, Peter

doi:10.1088/0264-9381/28/9/094003

Cited by 40 publications

(30 citation statements)

References 15 publications

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“…The main instrument on-board LPF, the LISA Technology Package [7,8], comprises two cubic test-masses and their enclosures, and the Optical Metrology System (OMS) [9][10][11][12]. The test-masses and their surroundings form the Gravitational Reference Sensor (GRS), which consists of the vacuum enclosure and the electrode housing [13].…”

Section: Lpf Dynamicsmentioning

confidence: 99%

Calibrating the system dynamics of LISA Pathfinder

Armano¹,

Audley²,

Baird³

et al. 2018

Phys. Rev. D

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LISA Pathfinder (LPF) was a European Space Agency mission with the aim to test key technologies for future space-borne gravitational-wave observatories like LISA. The main scientific goal of LPF was to demonstrate measurements of differential acceleration between free-falling test masses at the sub-femto-g level, and to understand the residual acceleration in terms of a physical model of stray forces, and displacement readout noise. A key step towards reaching the LPF goals was the correct calibration of the dynamics of LPF, which was a three-body system composed by two testmasses enclosed in a single spacecraft, and subject to control laws for system stability. In this work, we report on the calibration procedures adopted to calculate the residual differential stray force per unit mass acting on the two test-masses in their nominal positions. The physical parameters of the adopted dynamical model are presented, together with their role on LPF performance. The analysis and results of these experiments show that the dynamics of the system was accurately modeled and the dynamical parameters were stationary throughout the mission. Finally, the impact and importance of calibrating system dynamics for future space-based gravitational wave observatories is discussed.

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Section: Lpf Dynamicsmentioning

confidence: 99%

Calibrating the system dynamics of LISA Pathfinder

Armano¹,

Audley²,

Baird³

et al. 2018

Phys. Rev. D

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“…The results for the first order and second order PGW are shown in fig. 5 in addition to the different experimental constraints [28][29][30][31][32][33][34][35][36][37] and the BBN bound [12] as outlined in the legend of the plot (the suffix number for the SKA experiment shows the constraints based on the number of years in operation). In case of scale invariance the relic of the first order PGW can have any value from ∼ 10 −16 down to the lower limit by the induced PGW of ∼ 10 −23 depending on the value of r. If r 10 −9 then the scalar induced contribution on the PGW will be dominating.…”

Section: Primordial Gravitational Waves and Experimental Constraintsmentioning

confidence: 99%

“…The spectrum of the PGW from the scale invariant first order tensor perturbations (blue dashed line) assuming the maximum value of tensor-to-scalar ratio r = 0.07 from the upper limit of Planck data [26] and the induced PGW using the observed value of scalar perturbation amplitude AR = 2.1 × 10 −9 assuming the scale invariance (green solid line), a scale dependence with ns = 0.96 (green dotted line), and ns = 1.5 (green dot-dashed line) as shown in the plot. Also, some current and future experimental constraints [28][29][30][31][32][33][34][35][36][37] and the BBN bound are shown (see the text for details). presence of non-Gaussianity in the curvature power spectrum one gets [18][19][20]…”

Section: Figmentioning

confidence: 99%

“…However, future detectors will be able to probe much smaller signatures from possible phase transitions and the PGW in the early Universe cosmology. Some of these planned GW missions are the Laser Interferometer Space Antenna (LISA) [28], the Einstein Telescope (ET) [29], the Deci-hertz Interferometer Gravitational wave Observatory (DECIGO and B-DECIGO) [30,31], the Big Bang Observatory (BBO) [32], the Square Kilometer Array (SKA) telescope [33], the North American Nanohertz Observatory for Gravitational Waves (NanoGrav) [34], and the European Pulsar Timing Array (EPTA) [35]. Moreover, LIGO can be sensitive to the predicted GW for the early Universe depending on the model [36,37].…”

Section: Introductionmentioning

confidence: 99%

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Thermal history of the early Universe and primordial gravitational waves from induced scalar perturbations

Hajkarim

Schaffner-Bielich

2020

Phys. Rev. D

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We study the induced primordial gravitational waves (GW) coming from the effect of scalar perturbation on the tensor perturbation at the second order of cosmological perturbation theory. We use the evolution of the standard model degrees of freedom with respect to temperature in the early Universe to compute the induced gravitational waves bakcground. Our result shows that the spectrum of the induced GW is affected differently by the standard model degrees of freedom than the GW coming from first order tensor perturbation. This phenomenon is due to the presence of scalar perturbations as a source for tensor perturbations and it is effective around the quark gluon deconfinement and electroweak transition. In case of considering a scalar spectral index larger than one at small scales or a non-Gaussian curvature power spectrum this effect can be observed by gravitational wave observatories.

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“…The achieved level of sensitivity to the differential acceleration of the test masses is made possible by an additional high-precision readout along their common x axis provided by a laser interferometer [16][17][18]. The measurement noise in the differential test mass position, measured above 60 mHz, is 35 fm Hz −1=2 [9].…”

mentioning

confidence: 99%

Charge-Induced Force Noise on Free-Falling Test Masses: Results from LISA Pathfinder

Armano¹,

Audley²,

Auger³

et al. 2017

Phys. Rev. Lett.

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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 freefalling 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 Hz −1=2 across the 0.1-100 mHz frequency band that is crucial to an observatory such as the Laser Interferometer Space Antenna (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 buildup due to interplanetary cosmic rays and the TM charge-to-force coupling through stray PRL 118, 171101 (2017) P H Y S I C A L R E V I E W L E T T E R S week ending 28 APRIL 20170031-9007=17=118(17)=171101 (7) 171101-1 © 2017 American Physical Society 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.

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The LISA Pathfinder interferometry—hardware and system testing

Cited by 40 publications

References 15 publications

Calibrating the system dynamics of LISA Pathfinder

Calibrating the system dynamics of LISA Pathfinder

Thermal history of the early Universe and primordial gravitational waves from induced scalar perturbations

Charge-Induced Force Noise on Free-Falling Test Masses: Results from LISA Pathfinder

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