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Journal articles on the topic 'Laser Interferometer Space Antenna'

Author: Grafiati

Published: 4 June 2021

Last updated: 4 February 2022

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1

Zhan, Ming-Sheng, Jin Wang, Wei-Tou Ni, Dong-Feng Gao, Gang Wang, Ling-Xiang He, Run-Bing Li, et al. "ZAIGA: Zhaoshan long-baseline atom interferometer gravitation antenna." International Journal of Modern Physics D 29, no. 04 (July 2, 2019): 1940005. http://dx.doi.org/10.1142/s0218271819400054.

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The Zhaoshan long-baseline Atom Interferometer Gravitation Antenna (ZAIGA) is a new type of underground laser-linked interferometer facility, and is currently under construction. It is in the 200-m-on-average underground of a mountain named Zhaoshan which is about 80[Formula: see text]km southeast to Wuhan. ZAIGA will be equipped with long-baseline atom interferometers, high-precision atom clocks, and large-scale gyros. ZAIGA facility will take an equilateral triangle configuration with two 1-km-apart atom interferometers in each arm, a 300-m vertical tunnel with atom fountain and atom clocks mounted, and a tracking-and-ranging 1-km-arm-length prototype with lattice optical clocks linked by locked lasers. The ZAIGA facility will be used for experimental research on gravitation and related problems including gravitational wave detection, high-precision test of the equivalence principle of micro-particles, clock-based gravitational red-shift measurement, rotation measurement and gravitomagnetic effect.

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2

Shaddock, D. A. "An Overview of the Laser Interferometer Space Antenna." Publications of the Astronomical Society of Australia 26, no. 2 (2009): 128–32. http://dx.doi.org/10.1071/as08059.

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AbstractThe Laser Interferometer Space Antenna (LISA) will detect gravitational waves with frequencies from 0.1 mHz to 1 Hz. This article provides a brief overview of LISA's science goals followed by a tutorial of the LISA measurement concept.

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3

Zhao, Ya, Zhi Wang, Yupeng Li, Chao Fang, Heshan Liu, and Huilong Gao. "Method to Remove Tilt-to-Length Coupling Caused by Interference of Flat-Top Beam and Gaussian Beam." Applied Sciences 9, no. 19 (October 1, 2019): 4112. http://dx.doi.org/10.3390/app9194112.

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We discuss the tilt-to-length (TTL) coupling noise caused by interference between a flat-top beam and a Gaussian beam. Several physical models are presented to research the effects of non-diffracted and diffracted beams on TTL noise. A special case that can remove TTL coupling noise is discovered and is verified via both theoretical analysis and numerical simulations. The proposed case could provide desirable suggestions for the construction of high-precision interferometers such as the Laser Interferometer Space Antenna (LISA), Taiji program, or other interferometry systems.

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4

Liu, He-Shan, Zi-Ren Luo, and Wei Sha. "In-orbit performance of the laser interferometer of Taiji-1 experimental satellite." International Journal of Modern Physics A 36, no. 11n12 (February 22, 2021): 2140004. http://dx.doi.org/10.1142/s0217751x21400042.

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Taiji-1, which is the first experimental satellite for space gravitational wave detection in China, relies on key technologies which include the laser interferometer, the gravitational reference sensor (GRS), the micro-thruster and the satellite platform. Similarly to the Laser Interferometer Space Antenna (LISA) pathfinder, except for the science interferometer, the optical bench (OB) of Taiji-1 contains reference and test mass (TM) interferometers. Limited by the lower mechanical strength of the carrier rocket and by the orbit environment, the OB of Taiji-1 is made of invar steel and fused silica, and it is aimed to achieve a sensitivity of the order of 100[Formula: see text]pm/[Formula: see text]. The experimental results from in-orbit tests of Taiji-1 demonstrate that the interferometer can reach a sensitivity of 30[Formula: see text]pm/[Formula: see text] in the frequency range of 0.01–10[Formula: see text]Hz, which satisfies the requirements of Taiji-1 mission.

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5

Maghami, Peiman G., and T. Tupper Hyde. "Laser interferometer space antenna dynamics and controls model." Classical and Quantum Gravity 20, no. 10 (April 29, 2003): S273—S282. http://dx.doi.org/10.1088/0264-9381/20/10/330.

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6

Christensen, Nelson. "Lasers and Optics for the Laser Interferometer Space Antenna (LISA)." EPJ Web of Conferences 243 (2020): 08001. http://dx.doi.org/10.1051/epjconf/202024308001.

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7

Wang, Zhi, Tao Yu, Ya Zhao, Ziren Luo, Wei Sha, Chao Fang, Yukun Wang, et al. "Research on Telescope TTL Coupling Noise in Intersatellite Laser Interferometry." Photonic Sensors 10, no. 3 (November 29, 2019): 265–74. http://dx.doi.org/10.1007/s13320-019-0574-5.

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AbstractThe detection mission of gravitational waves in space is that the accuracy of the long-baseline intersatellite laser interferometry on the million-kilometer order needs to reach the order of $$8 \rm{pm}/\sqrt{\rm{Hz}}$$8pm/Hz. Among all noise sources that affect the interferometry accuracy, tilt-to-length (TTL) coupling noise is the second largest source of noise after shot noise. This paper focuses on studying the contribution of TTL coupling noise of the telescope system in the intersatellite scientific interferometer. By referring to the laser interferometer space antenna (LISA)’s noise budget, TTL coupling noise is required to be within ±25μm/rad (±300μrad). Therefore, this paper focuses on studying both the mechanism of TTL coupling noise due to the noise sources of the telescope and the method of suppressing the TTL noise, which can lay a foundation for noise distribution and the development of engineering prototypes in subsequent tasks.

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8

Escudero Sanz, Isabel, Astrid Heske, and Jeffrey C. Livas. "A telescope for LISA – the Laser Interferometer Space Antenna." Advanced Optical Technologies 7, no. 6 (December 19, 2018): 395–400. http://dx.doi.org/10.1515/aot-2018-0044.

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Abstract Gravitational waves are a prediction of Einstein’s general relativity theory. In autumn 2017, the Laser Interferometer Gravitational-Wave Observatory (LIGO; https://www.ligo.caltech.edu/) experiment reported the first detection of gravitational waves in addition to electromagnetic radiation from the collision of two neutron stars. This marks the first time that a cosmic event has been viewed in both gravitational waves and light and opens the door to a new type of astronomical observatory based on gravitational waves. The gravitational wave spectrum covers a broad span of frequencies and requires both space- and ground-based observatories to cover the full range. Space-based gravitational wave observatories, such as the proposed Laser Interferometer Space Antenna (LISA), operate at frequencies between 0.1 mHz and 1 Hz and complement the frequency range of 30–1000 Hz accessible by ground-based gravitational wave observatories, such as LIGO. A rich array of high-energy astrophysical sources is expected in the LISA measurement band. LISA was selected in 2017 as the third large mission of the Cosmic Vision program of the European Space Agency. The National Aeronautics and Space Administration will collaborate on both the scientific and technical aspects of this mission. This paper addresses the design of the optical telescope as an essential component of LISA’s long-distance interferometric measurement system.

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9

Xia, Yan, GuangYu Li, Gerhard Heinzel, Albrecht Rüdiger, and YongJie Luo. "Orbit design for the Laser Interferometer Space Antenna (LISA)." Science China Physics, Mechanics and Astronomy 53, no. 1 (January 2010): 179–86. http://dx.doi.org/10.1007/s11433-010-0100-7.

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10

Maghami, P. G., T. T. Hyde, and J. Kim. "An acquisition control for the laser interferometer space antenna." Classical and Quantum Gravity 22, no. 10 (April 28, 2005): S421—S428. http://dx.doi.org/10.1088/0264-9381/22/10/038.

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11

Danzmann, Karsten, and the LISA study team. "LISA: laser interferometer space antenna for gravitational wave measurements." Classical and Quantum Gravity 13, no. 11A (November 1, 1996): A247—A250. http://dx.doi.org/10.1088/0264-9381/13/11a/033.

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12

Smetana, Adam. "Background for gravitational wave signal at LISA from refractive index of solar wind plasma." Monthly Notices of the Royal Astronomical Society: Letters 499, no. 1 (September 16, 2020): L77—L81. http://dx.doi.org/10.1093/mnrasl/slaa155.

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ABSTRACT A strong indication is presented that the space-based gravitational antennas, in particular the Laser Interferometer Space Antenna (LISA) concept introduced in 2017 in response to the ESA call for L3 mission concepts, are going to be sensitive to a strong background signal interfering with the prospected signal of gravitational waves. The false signal is due to variations in the electron number density of the solar wind, causing variations in the refractive index of plasma flowing through interplanetary space. As countermeasures, two solutions are proposed. The first solution is to deploy enough solar wind detectors to the LISA mission to allow for reliable knowledge of the solar wind background. The second solution is to equip the LISA interferometer with a second laser beam with a distinct wavelength to allow cancelling of the background solar wind signal from the interferometric data.

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13

Hechler, F., and W. M. Folkner. "Mission analysis for the Laser Interferometer Space Antenna (LISA) mission." Advances in Space Research 32, no. 7 (October 2003): 1277–82. http://dx.doi.org/10.1016/s0273-1177(03)90332-2.

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14

Grimani, Catia. "Clues from 4U 0142+61 on supernova fallback disc formation and precession." Monthly Notices of the Royal Astronomical Society 507, no. 1 (July 21, 2021): 261–66. http://dx.doi.org/10.1093/mnras/stab2078.

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ABSTRACT The Nuclear Spectroscopic Telescope Array (NuSTAR) experiment detected a hard X-ray emission (10–70 keV) with a period of 8.68917 s and a pulse-phase modulation at 55 ks, or half this value, from the anomalous X-ray pulsar (AXP) 4U 0142+61. It is shown here that this evidence is naturally explained by the precession of a Keplerian supernova fallback disc surrounding this AXP. It is also found that the precession of discs formed around young neutron stars at distances larger than those considered in the past, may constitute almost neglected sources of gravitational waves with frequencies belonging to the sensitivity bands of the future space interferometers: Laser Interferometer Space Antenna (LISA), Advanced Laser Interferometer Antenna (ALIA), DECi-hertz Interferometer Gravitational wave Observatory (DECIGO), and Big Bang Observer (BBO). In this work, the gravitational wave emission from precessing fallback discs possibly formed around young pulsars such as Crab in a region extending beyond 8 × 107 m from the pulsar surface is estimated. It is also evaluated the role that infrared radiation emission from circumpulsar discs may play in contributing to inverse Compton scattering of TeV energy positrons and electrons. Extensive observational campaigns of disc formation around young and middle-aged pulsars may also contribute to solve the long-standing problem of a pulsar origin for the excess of positrons in cosmic rays observed near the Earth above 7 GeV. In the near future the James Webb Space Telescope, with unprecedented near- and mid-infrared observation capabilities, may provide direct evidence of a large sample of supernova fallback discs.

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15

Ni, Wei-Tou. "Gravitational wave detection in space." International Journal of Modern Physics D 25, no. 14 (December 2016): 1630001. http://dx.doi.org/10.1142/s0218271816300019.

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Gravitational Wave (GW) detection in space is aimed at low frequency band (100[Formula: see text]nHz–100[Formula: see text]mHz) and middle frequency band (100[Formula: see text]mHz–10[Formula: see text]Hz). The science goals are the detection of GWs from (i) Supermassive Black Holes; (ii) Extreme-Mass-Ratio Black Hole Inspirals; (iii) Intermediate-Mass Black Holes; (iv) Galactic Compact Binaries and (v) Relic GW Background. In this paper, we present an overview on the sensitivity, orbit design, basic orbit configuration, angular resolution, orbit optimization, deployment, time-delay interferometry (TDI) and payload concept of the current proposed GW detectors in space under study. The detector proposals under study have arm length ranging from 1000[Formula: see text]km to [Formula: see text][Formula: see text]km (8.6[Formula: see text]AU) including (a) Solar orbiting detectors — (ASTROD Astrodynamical Space Test of Relativity using Optical Devices (ASTROD-GW) optimized for GW detection), Big Bang Observer (BBO), DECi-hertz Interferometer GW Observatory (DECIGO), evolved LISA (e-LISA), Laser Interferometer Space Antenna (LISA), other LISA-type detectors such as ALIA, TAIJI etc. (in Earthlike solar orbits), and Super-ASTROD (in Jupiterlike solar orbits); and (b) Earth orbiting detectors — ASTROD-EM/LAGRANGE, GADFLI/GEOGRAWI/g-LISA, OMEGA and TIANQIN.

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16

Danielski, C., V. Korol, N. Tamanini, and E. M. Rossi. "Circumbinary exoplanets and brown dwarfs with the Laser Interferometer Space Antenna." Astronomy & Astrophysics 632 (December 2019): A113. http://dx.doi.org/10.1051/0004-6361/201936729.

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Aims. We explore the prospects for the detection of giant circumbinary exoplanets and brown dwarfs (BDs) orbiting Galactic double white dwarfs (DWDs) binaries with the Laser Interferometer Space Antenna (LISA). Methods. By assuming an occurrence rate of 50%, motivated by white dwarf pollution observations, we built a Galactic synthetic population of P-type giant exoplanets and BDs orbiting DWDs. We carried this out by injecting different sub-stellar populations, with various mass and orbital separation characteristics, into the DWD population used in the LISA mission proposal. We then performed a Fisher matrix analysis to measure how many of these three-body systems show a periodic Doppler-shifted gravitational wave perturbation detectable by LISA. Results. We report the number of circumbinary planets (CBPs) and BDs that can be detected by LISA for various combinations of mass and semi-major axis distributions. We identify pessimistic and optimistic scenarios corresponding, respectively, to 3 and 83 (14 and 2218) detections of CBPs (BDs), observed during the length of the nominal LISA mission. These detections are distributed all over the Galaxy following the underlying DWD distribution, and they are biased towards DWDs with higher LISA signal-to-noise ratio and shorter orbital period. Finally, we show that if LISA were to be extended for four more years, the number of systems detected will be more than doubled in both the optimistic and pessimistic scenarios. Conclusions. Our results present promising prospects for the detection of post-main sequence exoplanets and BDs, showing that gravitational waves can prove the existence of these populations over the totality of the Milky Way. Detections by LISA will deepen our knowledge on the life of exoplanets subsequent to the most extreme evolution phases of their hosts, clarifying whether new phases of planetary formation take place later in the life of the stars. Such a method is strongly complementary to electromagnetic studies within the solar region and opens a window into the investigation of planets and BDs everywhere in the entire Galaxy, and possibly even in nearby galaxies in the Local Group.

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Wong, Kaze W. K., Vishal Baibhav, and Emanuele Berti. "Binary radial velocity measurements with space-based gravitational-wave detectors." Monthly Notices of the Royal Astronomical Society 488, no. 4 (July 30, 2019): 5665–70. http://dx.doi.org/10.1093/mnras/stz2077.

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ABSTRACT Unlike traditional electromagnetic measurements, gravitational-wave observations are not affected by crowding and extinction. For this reason, compact object binaries orbiting around a massive black hole can be used as probes of the inner environment of the black hole in regions inaccessible to traditional astronomical measurements. The orbit of the binary’s barycentre around the massive black hole will cause a Doppler shift in the gravitational waveform, which is in principle measurable by future space-based gravitational-wave interferometers, such as the Laser Interferometer Space Antenna (LISA). We investigate the conditions under which these Doppler shifts are observable by LISA. Our results imply that Doppler shift observations can be used to study the central region of globular clusters in the Milky Way, as well the central environment of extragalactic massive black holes.

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18

Mukherjee, Suvodip, Benjamin D. Wandelt, and Joseph Silk. "Probing the theory of gravity with gravitational lensing of gravitational waves and galaxy surveys." Monthly Notices of the Royal Astronomical Society 494, no. 2 (March 28, 2020): 1956–70. http://dx.doi.org/10.1093/mnras/staa827.

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ABSTRACT The cross-correlation of gravitational wave strain with upcoming galaxy surveys probes theories of gravity in a new way. This method enables testing the theory of gravity by combining the effects from both gravitational lensing of gravitational waves and the propagation of gravitational waves in space–time. We find that within 10 yr the combination of the Advanced LIGO (Laser Interferometer Gravitational-Wave Observatory) and VIRGO (Virgo interferometer) detector networks with planned galaxy surveys should detect weak gravitational lensing of gravitational waves in the low-redshift Universe (z < 0.5). With the next-generation gravitational wave experiments such as Voyager, LISA (Laser Interferometer Space Antenna), Cosmic Explorer, and the Einstein Telescope, we can extend this test of the theory of gravity to larger redshifts by exploiting the synergies between electromagnetic wave and gravitational wave probes.

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19

Tinto, M., D. DeBra, S. Buchman, and S. Tilley. "gLISA: geosynchronous laser interferometer space antenna concepts with off-the-shelf satellites." Review of Scientific Instruments 86, no. 1 (January 2015): 014501. http://dx.doi.org/10.1063/1.4904862.

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20

Touboul, Pierre, Manuel Rodrigues, and George M. Le Clerc. "The inertial reference sensor CAESAR for the laser interferometer space antenna mission." Classical and Quantum Gravity 13, no. 11A (November 1, 1996): A259—A270. http://dx.doi.org/10.1088/0264-9381/13/11a/035.

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21

Dotti, M., M. Colpi, and F. Haardt. "Laser Interferometer Space Antenna double black holes: dynamics in gaseous nuclear discs." Monthly Notices of the Royal Astronomical Society 367, no. 1 (March 21, 2006): 103–12. http://dx.doi.org/10.1111/j.1365-2966.2005.09956.x.

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Thorpe, James Ira, Rachel Jean Cruz, Shannon Reynier Sankar, Guido Mueller, and Paul McNamara. "First step toward a benchtop model of the Laser Interferometer Space Antenna." Optics Letters 29, no. 24 (December 15, 2004): 2843. http://dx.doi.org/10.1364/ol.29.002843.

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23

Schuldt, Thilo, Martin Gohlke, Dennis Weise, Achim Peters, Ulrich Johann, and Claus Braxmaier. "High-Resolution Dimensional Metrology for Industrial Applications." Key Engineering Materials 437 (May 2010): 113–17. http://dx.doi.org/10.4028/www.scientific.net/kem.437.113.

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In this paper, we present the current status of our heterodyne interferometer with demonstrated noise levels below 5 pm/Hz in translation and below 10 nrad/Hz in tilt measurement, both for frequencies above 10-2 Hz. The interferometer, based on a highly symmetric design where reference and measurement beam have the same frequency and polarization, utilizes intensity stabilization and phaselock of the heterodyne frequency. Currently, we develop a new enhanced interferometer setup based on a mechanically and thermally highly stable glass ceramic. While the interferometer was developed with respect to the specific requirements of the LISA (Laser Interferometer Space Antenna) space mission, it is also the basis for applications in high-precision dilatometry and industrial metrology. We present a prototype dilatometer with which we measured the coefficient of thermal expansion (CTE) of carbon-fiber reinforced plastic (CFRP) with an accuracy below 10-7/K. For surface property measurements, we develop an actuation of the measurement beam over the surface under investigation.

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24

Meshksar, N., L. Ferraioli, D. Mance, J. ten Pierick, and D. Giardini. "Analysis of the accuracy of actuation electronics for the laser interferometer space antenna." Review of Scientific Instruments 91, no. 9 (September 1, 2020): 095003. http://dx.doi.org/10.1063/5.0018536.

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25

Chen, Kun, Xiaofeng Zhang, Tong Guo, and Zhi-Ming Cai. "Key technologies analysis and design of ultra-clean & ultra-stable spacecraft for gravitational wave detection." International Journal of Modern Physics A 36, no. 11n12 (April 9, 2021): 2140021. http://dx.doi.org/10.1142/s0217751x21400212.

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The observation of gravitational wave enables human to explore the origin, formation and evolution of universe governed by the gravitational interaction and the nature of gravity beyond general theory of relativity. The groundbreaking discovery of Gravitational Wave by Laser Interferometer Gravitational-Wave Observatory provides a brand-new observation way. While detecting gravitational wave on ground is limited by noises and test scale, space detection is an optimized alternative to learn rich sources in range of 0.1 mHz–1 Hz. Considering the great significance of space gravitational wave detection, ESA proposed LISA project, CAS also proposed Taiji project. Due to the extremely weak gravitational wave signal and high measurement accuracy requirement, the spaceborne GW observation antenna is accomplished by three spacecrafts constitute isosceles triangle formation intersatellite interferometer. The arm length of the interferometer reaches millions of kilometers between them, and the measurement accuracy reaches pico-meter magnitude. There are many key technologies including pm magnitude space laser interferometer metrology, drag-free control using TM of Gravity Reference Sensor, [Formula: see text]N micro thruster, ultra-clean & ultra-stable spacecraft, etc. This paper focuses on key technologies of the ultra-clean & ultra-stable spacecraft, analyzing the design of mechanical, thermal control and magnetic clean. Moreover, it reports the preliminary results of the technological breakthrough.

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26

Vetrugno, D. "LISA Pathfinder first results." International Journal of Modern Physics D 26, no. 05 (April 2017): 1741023. http://dx.doi.org/10.1142/s0218271817410231.

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LISA Pathfinder (LPF) is an in-flight technological demonstrator designed and launched to prove the feasibility of sub-femto-[Formula: see text] free fall of kilo-sized test masses (TM), an essential ingredient for the future gravitational wave observatory from space. Half a year after launch, the first results are available and show an incredibly well-performing instrument. The results represent a first and important step towards the long awaited construction and launch of LISA, the Laser Interferometer Space Antenna.

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Cooray, Asantha, and Naoki Seto. "Can the Laser Interferometer Space Antenna Resolve the Distance to the Large Magellanic Cloud?" Astrophysical Journal 623, no. 2 (March 16, 2005): L113—L116. http://dx.doi.org/10.1086/430132.

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Canizares, Priscilla, and Carlos F. Sopuerta. "Time-domain modelling of Extreme-Mass-Ratio Inspirals for the Laser Interferometer Space Antenna." Journal of Physics: Conference Series 314 (September 22, 2011): 012075. http://dx.doi.org/10.1088/1742-6596/314/1/012075.

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29

Breivik, Katelyn, Kyle Kremer, Michael Bueno, Shane L. Larson, Scott Coughlin, and Vassiliki Kalogera. "Characterizing Accreting Double White Dwarf Binaries with the Laser Interferometer Space Antenna and Gaia." Astrophysical Journal 854, no. 1 (February 5, 2018): L1. http://dx.doi.org/10.3847/2041-8213/aaaa23.

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Armano, M., H. Audley, J. Baird, M. Born, D. Bortoluzzi, N. Cardines, E. Castelli, et al. "Analysis of the accuracy of actuation electronics in the laser interferometer space antenna pathfinder." Review of Scientific Instruments 91, no. 4 (April 1, 2020): 045003. http://dx.doi.org/10.1063/1.5140406.

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Cooray, Asantha, Alison J. Farmer, and Naoki Seto. "The Optical Identification of Close White Dwarf Binaries in the Laser Interferometer Space Antenna Era." Astrophysical Journal 601, no. 1 (January 16, 2004): L47—L50. http://dx.doi.org/10.1086/381780.

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32

KAWASHIMA, Nobuki. "Cosmos and Measurement. Laser Interferometer Gravitational Wave Antenna in Space with a 500km Arm Length." Journal of the Japan Society for Precision Engineering 63, no. 10 (1997): 1368–73. http://dx.doi.org/10.2493/jjspe.63.1368.

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Zhang, Min, Gang Jin, and Ziren Luo. "Overall discussion on the key problems of a space-borne laser interferometer gravitational wave antenna." Chinese Science Bulletin 64, no. 24 (August 1, 2019): 2468–74. http://dx.doi.org/10.1360/tb-2019-0055.

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34

Rubbo, Louis J., Kelly Holley-Bockelmann, and Lee Samuel Finn. "Event Rate for Extreme Mass Ratio Burst Signals in the Laser Interferometer Space Antenna Band." Astrophysical Journal 649, no. 1 (September 8, 2006): L25—L28. http://dx.doi.org/10.1086/508326.

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35

Benacquista, M. J., J. DeGoes, and D. Lunder. "A simulation of the laser interferometer space antenna data stream from galactic white dwarf binaries." Classical and Quantum Gravity 21, no. 5 (February 5, 2004): S509—S514. http://dx.doi.org/10.1088/0264-9381/21/5/018.

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36

Seto, Naoki. "Long-term operation of the Laser Interferometer Space Antenna and Galactic close white dwarf binaries." Monthly Notices of the Royal Astronomical Society 333, no. 2 (June 2002): 469–74. http://dx.doi.org/10.1046/j.1365-8711.2002.05432.x.

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37

Tröbs, Michael, Peter Wessels, and Carsten Fallnich. "Phase-noise properties of an ytterbium-doped fiber amplifier for the Laser Interferometer Space Antenna." Optics Letters 30, no. 7 (April 1, 2005): 789. http://dx.doi.org/10.1364/ol.30.000789.

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38

McNAMARA, PAUL W. "THE LISA PATHFINDER MISSION." International Journal of Modern Physics D 22, no. 01 (January 2013): 1341001. http://dx.doi.org/10.1142/s0218271813410010.

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Laser Interferometer Space Antenna (LISA) Pathfinder (formerly known as SMART-2) is a European Space Agency mission designed to pave the way for the joint ESA/NASA LISA mission by testing in flight the critical technologies required for space borne gravitational wave detection; it will put two test masses in a near-perfect gravitational free-fall and control and measure their motion with unprecedented accuracy. This is achieved through technology comprising inertial sensors, high precision laser metrology, drag-free control and an ultra precise micro-Newton propulsion system. LISA Pathfinder (LPF) essentially mimics one arm of space-borne gravitational wave detectors by shrinking the million kilometer scale armlengths down to a few tens of centimeters, giving up the sensitivity to gravitational waves, but keeping the measurement technology. The scientific objective of the LPF mission consists then of the first in-flight test of low frequency gravitational wave detection metrology.

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Di Pace, Sibilla, Arwa Dabbech, Vitalii Khodnevych, Michel Lintz, and Nicoleta Dinu-Jaeger. "Particle contamination monitoring in the backscattering light experiment for LISA." Open Material Sciences 5, no. 1 (January 1, 2019): 12–18. http://dx.doi.org/10.1515/oms-2019-0002.

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Abstract In the context of space-based optics, contamination due to particle deposition on the optics is inevitable and constitutes a critical issue. This gets more challenging for the sensitive heterodyne measurements of the Laser Interferometer Space Antenna (LISA), the space-based gravitational wave observatory to be launched in 2034. Therefore, table-top experiments need to be developed for a better understanding of how micrometer to millimeter sized dust particles, present on optical surfaces, affect LISA measurements. In this work, we present an experimental setup for the simultaneous measurement of the coherent backscattering and the monitoring of particles deposition on the optics to be tested. The results of the first measurements are presented and discussed in this article.

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Wolz, Anna, Kent Yagi, Nick Anderson, and Andrew J. Taylor. "Measuring individual masses of binary white dwarfs with space-based gravitational-wave interferometers." Monthly Notices of the Royal Astronomical Society: Letters 500, no. 1 (November 15, 2020): L52—L56. http://dx.doi.org/10.1093/mnrasl/slaa183.

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ABSTRACT Unlike gravitational waves from merging black holes and neutron stars that chirp significantly over the observational period of ground-based detectors, gravitational waves from binary white dwarfs are almost monochromatic. This makes it extremely challenging to measure their individual masses. Here, we take a novel approach of using finite-size effects and applying certain universal relations to measure individual masses of binary white dwarfs using Laser Interferometer Space Antenna. We found quasi-universal relations among the mass, moment of inertia, and tidal deformability of a white dwarf that do not depend sensitively on the white dwarf composition. These relations allow us to rewrite the moments of inertia and tidal deformabilities in the waveform in terms of the masses. We then carried out a Fisher analysis to estimate how accurately one can measure the individual masses from the chirp mass and finite-size measurements. We found that the individual white dwarf masses can be measured with LISA for a 4-yr observation if the initial frequency is high enough (∼0.02 Hz) and either the binary separation is small (∼1 kpc) or the masses are relatively large (m ≳ 0.8 M⊙). This opens a new possibility of measuring individual masses of binary white dwarfs with space-based interferometers.

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Tröbs, M., S. Barke, Th Theeg, D. Kracht, G. Heinzel, and K. Danzmann. "Differential phase-noise properties of a ytterbium-doped fiber amplifier for the Laser Interferometer Space Antenna." Optics Letters 35, no. 3 (January 29, 2010): 435. http://dx.doi.org/10.1364/ol.35.000435.

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Sanjuán, J., A. Preston, D. Korytov, A. Spector, A. Freise, G. Dixon, J. Livas, and G. Mueller. "Carbon fiber reinforced polymer dimensional stability investigations for use on the laser interferometer space antenna mission telescope." Review of Scientific Instruments 82, no. 12 (December 2011): 124501. http://dx.doi.org/10.1063/1.3662470.

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Sanjuán, J., A. Lobo, and J. Ramos-Castro. "Analog-to-digital converters nonlinear errors correction in thermal diagnostics for the laser interferometer space antenna mission." Review of Scientific Instruments 80, no. 11 (November 2009): 114901. http://dx.doi.org/10.1063/1.3258145.

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LI, GUANGYU, ZHAOHUA YI, GERHARD HEINZEL, ALBRECHT RÜDIGER, OLIVER JENNRICH, LI WANG, YAN XIA, FEI ZENG, and HAIBIN ZHAO. "METHODS FOR ORBIT OPTIMIZATION FOR THE LISA GRAVITATIONAL WAVE OBSERVATORY." International Journal of Modern Physics D 17, no. 07 (July 2008): 1021–42. http://dx.doi.org/10.1142/s021827180801267x.

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The Laser Interferometer Space Antenna (LISA) mission is a joint ESA-NASA mission for detecting low-frequency gravitational waves in the frequency range from 0.1 mHz to 1 Hz, by using accurate distance measurements with laser interferometry between three spacecraft, which will be launched around 2015 and one year later reach their orbits around the Sun. In order to operate successfully, it is crucial for the constellation of the three spacecraft to have extremely high stability. In this paper, several problems of the orbit optimization of the LISA constellation are discussed by using numerical and analytical methods for satisfying the requirements of accuracy. On the basis of the coorbital restricted problem, analytical expressions of the heliocentric distance and the trailing angle to the Earth of the constellation's barycenter are deduced, with the result that the approximate analytical solution of first order will meet the accuracy requirement of the spacecraft orbit design. It is proved that there is a value of the inclination of the constellation plane that will make the variation of the arm-length a minimum. The principle for selecting the optimum starting elements of orbits at any epoch is proposed. The method and programming principles of finding the optimized orbits are also presented together with examples of the optimization design.

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Hyde, T. T., P. G. Maghami, and S. M. Merkowitz. "Pointing acquisition and performance for the laser interferometry space antenna mission." Classical and Quantum Gravity 21, no. 5 (February 9, 2004): S635—S640. http://dx.doi.org/10.1088/0264-9381/21/5/036.

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Toscani, Martina, Giuseppe Lodato, and Elena Maria Rossi. "Discovering intermediate massive black holes through tidally disrupted stars." International Journal of Modern Physics D 28, no. 14 (October 2019): 1944015. http://dx.doi.org/10.1142/s0218271819440152.

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Stars are spheres of gas held together by self-gravity. When flying by a black hole, however, the star self-binding force can be overwhelmed by the black hole tides and the star can be torn apart. This is a physically rich and fascinating event which will be described by first introducing the concept of black hole from a mathematical point of view. We will then dive into the physics of the tidal disruption and proceed describing the accompanying electromagnetic flare and gravitational wave burst in the frequency range of the Laser Interferometer Space Antenna. This empowers such events to discover the elusive black holes with mass intermediate between the solar and the million/billion solar masses.

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BERTI, EMANUELE, and VITOR CARDOSO. "SUPERMASSIVE BLACK HOLES OR BOSON STARS? HAIR COUNTING WITH GRAVITATIONAL WAVE DETECTORS." International Journal of Modern Physics D 15, no. 12 (December 2006): 2209–16. http://dx.doi.org/10.1142/s0218271806009637.

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The evidence for supermassive Kerr black holes in galactic centers is strong and growing, but only the detection of gravitational waves will convincingly rule out other possibilities to explain the observations. The Kerr space–time is completely specified by the first two multipole moments: mass and angular momentum. This is usually referred to as the "no-hair theorem," but it is really a "two-hair" theorem. If general relativity is the correct theory of gravity, the most plausible alternative to a supermassive Kerr black hole is a rotating boson star. Numerical calculations indicate that the space–time of rotating boson stars is determined by the first three multipole moments ("three-hair theorem"). The Laser Interferometer Space Antenna (LISA) could accurately measure the oscillation frequencies of these supermassive objects. We propose to use these measurements to "count their hair," unambiguously determining their nature and properties.

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Trias, Miquel, Alberto Vecchio, and John Veitch. "Studying stellar binary systems with the Laser Interferometer Space Antenna using delayed rejection Markov chain Monte Carlo methods." Classical and Quantum Gravity 26, no. 20 (October 6, 2009): 204024. http://dx.doi.org/10.1088/0264-9381/26/20/204024.

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Zwick, Lorenz, Pedro R. Capelo, Elisa Bortolas, Lucio Mayer, and Pau Amaro-Seoane. "Improved gravitational radiation time-scales: significance for LISA and LIGO-Virgo sources." Monthly Notices of the Royal Astronomical Society 495, no. 2 (May 20, 2020): 2321–31. http://dx.doi.org/10.1093/mnras/staa1314.

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ABSTRACT We present a revised version of Peters’ time-scale for the gravitational wave (GW)-induced decay of two point masses. The new formula includes the effects of the first-order post-Newtonian perturbation and additionally provides a simple fit to account for the Newtonian self-consistent evolution of the eccentricity. The revised time-scale is found by multiplying Peters’ estimate by two factors, $R(e_0)= 8^{1-\sqrt{1-e_0}}$ and Qf(p0) = exp (2.5(rS/p0)), where e0 and p0 are the initial eccentricity and periapsis, respectively, and rS the Schwarzschild radius of the system. Their use can correct errors of a factor of 1–10 that arise from using the original Peters’ formula. We apply the revised time-scales to a set of typical sources for existing ground-based laser interferometers and for the future Laser Interferometer Space Antenna (LISA), at the onset of their GW-driven decay. We argue that our more accurate model for the orbital evolution will affect current event- and detection-rate estimates for mergers of compact object binaries, with stronger deviations for eccentric LISA sources, such as extreme and intermediate mass-ratio inspirals. We propose the correction factors R and Qf as a simple prescription to quantify decay time-scales more accurately in future population synthesis models. We also suggest that the corrected time-scale may be used as a computationally efficient alternative to numerical integration in other applications that include the modelling of radiation reaction for eccentric sources.

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Stroeer, Alexander, Matthew Benacquista, and Frank Ceballos. "Detecting Double Degenerate Progenitors of SNe Ia with LISA." Proceedings of the International Astronomical Union 7, S281 (July 2011): 217–20. http://dx.doi.org/10.1017/s1743921312015062.

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AbstractThe Galactic population of close white dwarf binaries is expected to provide the largest number of gravitational wave sources for low frequency detectors such as the Laser Interferometer Space Antenna (LISA). Current data analysis techniques have demonstrated the capability of resolving on the order of 104 white dwarf binaries from a 2 year observation. Resolved binaries are either at high frequencies or large amplitudes. Such systems are more likely to be high-mass binaries, a subset of which will be progenitors of SNe Ia in the double degenerate scenario. We report on results of a study of the properties of resolved binaries using a population synthesis model of the Galactic white dwarf binaries and a LISA data analysis algorithm using Mock LISA Data Challenge tools.

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