Статті в журналах: "LISA space mission"

1

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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Schuldt, Thilo, Klaus Döringshoff, Markus Oswald, Evgeny V. Kovalchuk, Achim Peters, and Claus Braxmaier. "Absolute laser frequency stabilization for LISA." International Journal of Modern Physics D 28, no. 12 (September 2019): 1845002. http://dx.doi.org/10.1142/s0218271818450025.

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The LISA space mission requires laser frequency pre-stabilization of the 1064[Formula: see text]nm laser sources. While cavity-based systems are the current baseline, laser frequencies stabilized to a hyperfine transition in molecular iodine near 532[Formula: see text]nm are a possible alternative. Several setups with respect to space applications were developed, putting special emphasis on compactness and mechanical and thermal stability of the optical setup. Vibration testing and thermal cycling were performed. These setups show frequency noise below 20[Formula: see text]Hz/[Formula: see text] for frequencies between 4[Formula: see text]mHz and 1[Formula: see text]Hz with an absolute frequency reproducibility better than 1[Formula: see text]kHz. They fulfil the LISA requirements and offer an absolute laser frequency simplifying the initial spacecraft acquisition procedure. We present the current status of iodine-based frequency references and their applicability in space missions, especially within the LISA mission.

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3

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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4

Racca, Giuseppe D., and Paul W. McNamara. "The LISA Pathfinder Mission." Space Science Reviews 151, no. 1-3 (December 15, 2009): 159–81. http://dx.doi.org/10.1007/s11214-009-9602-x.

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5

Banks, Michael. "Europe gives green light to LISA gravitational-wave mission." Physics World 37, no. 3 (March 1, 2024): 13i. http://dx.doi.org/10.1088/2058-7058/37/03/16.

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6

RÜEDIGER, ALBRECHT. "Detecting gravitational waves with ground and space interferometers – with special attention to the space project ASTROD." International Journal of Modern Physics D 11, no. 07 (August 2002): 963–94. http://dx.doi.org/10.1142/s0218271802002505.

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The existence of gravitational waves is the most prominent of Einstein's predictions that has not yet been directly verified. The space projects LISA and (partially) ASTROD share their goal and principle of operation with the ground-based interferometers currently under construction: the detection and measurement of gravitational waves by laser interferometry. Ground and space detection differ in their frequency ranges, and thus the detectable sources. Towards low frequencies, ground-based detection is limited by seismic noise, and yet more fundamentally by 'gravity gradient noise', thus covering the range from a few Hz to a few kHz. On five sites worldwide, detectors of armlengths from 0.3 to 4 km are nearing completion. they will progressively be put in operation in the years 2002 and 2003. Future enhanced versions are being planned, with scientific data not expected until 2008, i.e. near the launch of the space project LISA. It is only in space that detection of signals below, say, 1 Hz is possible, opening a wide window to a different class of interesting sources of gravitational waves. The project LISA consists of three spacecraft in heliocentric orbits, forming a triangle of 5 million km sides. A technology demonstrator, designed to test vital LISA technologies, is to be launched, aboard a SMART-2 mission, in 2006. The proposed mission ASTROD will, among other goals, also aim at detecting gravitational waves, at even lower frequencies than LISA. Its later start will allow it to benefit from the expertise gained with LISA.

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7

Martens, Waldemar, and Eric Joffre. "Trajectory Design for the ESA LISA Mission." Journal of the Astronautical Sciences 68, no. 2 (June 2021): 402–43. http://dx.doi.org/10.1007/s40295-021-00263-2.

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AbstractThe three Laser Interferometer Space Antenna (LISA) spacecraft are going to be placed in a triangular formation in an Earth-trailing or Earth-leading orbit. They will be launched together on a single rocket and transferred to that science orbit using Solar Electric Propulsion. Since the transfer Δv depends on the chosen science orbit, both transfer and science orbit have been optimised together. For a thrust level of 90 mN, an allocation of 1092 m/s per spacecraft is sufficient for an all-year launch in 2034. For every launch month a dedicated science orbit is designed with a corner angle variation of 60° ± 1.0° and an arm length rate of maximum 10 m/s. Moreover, a detailed navigation analysis of the science orbit insertion and the impact on insertion errors on the constellation stability has been conducted. The analysis shows that Range/Doppler measurements together with a series of correction manoeuvres at the beginning of the science orbit phase can reduce insertion dispersions to a level where corner angle variations remain at about 60° ± 1.1° at 99% C.L. However, the situation can become significantly worse if the self-gravity accelerations acting during the science orbit phase are not sufficiently characterised prior to science orbit insertion.

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8

Dei Tos, Diogene A., Mirco Rasotto, Florian Renk, and Francesco Topputo. "LISA Pathfinder mission extension: A feasibility analysis." Advances in Space Research 63, no. 12 (June 2019): 3863–83. http://dx.doi.org/10.1016/j.asr.2019.02.035.

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9

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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10

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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11

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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12

WANG Zhi, 王智, 马军 MA Jun, and 李静秋 LI Jing-qiu. "Space-based gravitational wave detection mission: design highlights of LISA system." Chinese Optics 8, no. 6 (2015): 980–87. http://dx.doi.org/10.3788/co.20150806.0980.

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13

Johann, U. A., M. Ayre, P. F. Gath, W. Holota, P. Marenaci, H. R. Schulte, P. Weimer, and D. Weise. "The European Space Agency's LISA mission study: status and present results." Journal of Physics: Conference Series 122 (July 1, 2008): 012005. http://dx.doi.org/10.1088/1742-6596/122/1/012005.

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14

SUMNER, TIMOTHY J., and DIANA N. A. SHAUL. "THE OBSERVATION OF GRAVITATIONAL WAVES FROM SPACE USING LISA." Modern Physics Letters A 19, no. 11 (April 10, 2004): 785–800. http://dx.doi.org/10.1142/s0217732304013647.

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The observation of gravitational waves using space-borne instrumentation allows the detection of astrophysical sources in a much longer wavelength part of the spectrum than ground-based instruments can reach. This opens up the prospect of a completely different view of the Universe than can be achieved in any other way. This article summarises the scientific goals of the LISA mission in its search for sources within the 10-4 to 10-1 Hz window and describes the current status of the overall project.

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15

Armano, M., H. Audley, J. Baird, P. Binetruy, M. Born, D. Bortoluzzi, E. Castelli, et al. "Temperature stability in the sub-milliHertz band with LISA Pathfinder." Monthly Notices of the Royal Astronomical Society 486, no. 3 (April 12, 2019): 3368–79. http://dx.doi.org/10.1093/mnras/stz1017.

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Abstract LISA Pathfinder (LPF) was a technology pioneering mission designed to test key technologies required for gravitational wave detection in space. In the low frequency regime (milliHertz and below), where space-based gravitational wave observatories will operate, temperature fluctuations play a crucial role since they can couple into the interferometric measurement and the test masses’ free-fall accuracy in many ways. A dedicated temperature measurement subsystem, with noise levels in 10 $\mu$K Hz−1/2 down to 1 mHz was part of the diagnostics unit onboard LPF. In this paper we report on the temperature measurements throughout mission operations, characterize the thermal environment, estimate transfer functions between different locations, and report temperature stability (and its time evolution) at frequencies as low as 10 $\mu$Hz, where typically values around 1 K Hz−1/2 were measured.

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16

Soyuer, Deniz, Lorenz Zwick, Daniel J. D’Orazio, and Prasenjit Saha. "Searching for gravitational waves via Doppler tracking by future missions to Uranus and Neptune." Monthly Notices of the Royal Astronomical Society: Letters 503, no. 1 (March 13, 2021): L73—L79. http://dx.doi.org/10.1093/mnrasl/slab025.

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ABSTRACT The past year has seen numerous publications underlining the importance of a space mission to the ice giants in the upcoming decade. Proposed mission plans involve a ∼10 yr cruise time to the ice giants. This cruise time can be utilized to search for low-frequency gravitational waves (GWs) by observing the Doppler shift caused by them in the Earth–spacecraft radio link. We calculate the sensitivity of prospective ice giant missions to GWs. Then, adopting a steady-state black hole binary population, we derive a conservative estimate for the detection rate of extreme mass ratio inspirals (EMRIs), supermassive black hole (SMBH), and stellar mass binary black hole (sBBH) mergers. We link the SMBH population to the fraction of quasars fbin resulting from Galaxy mergers that pair SMBHs to a binary. For a total of 10 40-d observations during the cruise of a single spacecraft, $\mathcal {O}(f_\mathrm{bin})\sim 0.5$ detections of SMBH mergers are likely, if Allan deviation of Cassini-era noise is improved by ∼102 in the 10−5 − 10−3 Hz range. For EMRIs the number of detections lies between $\mathcal {O}(0.1) \ \mathrm{ and} \ \mathcal {O}(100)$. Furthermore, ice giant missions combined with the Laser Interferometer Space Antenna (LISA) would improve the localization by an order of magnitude compared to LISA by itself.

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Kang, Yacheng, Chang Liu, and Lijing Shao. "Prospects for Detecting Exoplanets around Double White Dwarfs with LISA and Taiji." Astronomical Journal 162, no. 6 (November 18, 2021): 247. http://dx.doi.org/10.3847/1538-3881/ac23d8.

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Abstract Recently, Tamanini & Danielski discussed the possibility of detecting circumbinary exoplanets (CBPs) orbiting double white dwarfs (DWDs) with the Laser Interferometer Space Antenna (LISA). Extending their methods and criteria, we discuss the prospects for detecting exoplanets around DWDs not only by LISA, but also by Taiji, a Chinese space-borne gravitational-wave (GW) mission that has slightly better sensitivity at low frequencies. We first explore how different binary masses and mass ratios affect the abilities of LISA and Taiji to detect CBPs. Second, for certain known detached DWDs with high signal-to-noise ratios, we quantify the possibility of CBP detections around them. Third, based on the DWD population obtained from the Mock LISA Data Challenge, we present basic assessments of the CBP detections in our Galaxy during a 4 yr mission time for LISA and Taiji. We discuss the constraints on the detectable zone of each system, as well as the distributions of the inner/outer edge of the detectable zone. With the DWD population, we further inject two different planet distributions with an occurrence rate of 50% and constrain the total detection rates. We briefly discuss the prospects for detecting habitable CBPs around DWDs with a simplified model. These results can provide helpful inputs for upcoming exoplanetary projects and help analyze planetary systems after the common envelope phase.

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18

He, Jian-Guo, Yong Shao, Shi-Jie Gao, and Xiang-Dong Li. "Detection Prospects of Fast-merging Gravitational Wave Sources in M31." Astrophysical Journal 953, no. 2 (August 1, 2023): 153. http://dx.doi.org/10.3847/1538-4357/ace348.

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Abstract It is widely accepted that quite a number of double compact objects (DCOs) in the Milky Way can be identified by future space-based gravitational wave (GW) detectors, while systematic investigations on the detection of the GW sources in nearby galaxies are still lacking. In this paper, we present calculations of potential populations of GW sources for all types of DCOs in the Local Group galaxy M31. For M31, we use an age-dependent model for the evolution of the metallicity and the star formation rate. By varying assumptions of common-envelope ejection efficiencies and supernova-explosion mechanisms during binary evolution, we make predictions on the properties of DCOs that can be detected by the Laser Interferometer Space Antenna (LISA). Our calculations indicate that a few (a dozen) DCOs are likely to be observed by LISA during its 4 (10) yr mission. We expect that the sources with black hole components are more likely to be first identified during a 4 yr mission since these binaries have relatively large chirp masses, while the systems with white-dwarf components dominate the overall population of detectable GW sources during a 10 yr mission. LISA can only detect very tight fast-merging systems in M31, corresponding to the peak of orbital period distribution from ∼2 minutes for double white dwarfs to ∼20 minutes for double black holes.

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Middleton, Kevin F. "Prototype optical bench instrument in the interferometer for the LISA–Pathfinder space mission." Optical Engineering 45, no. 12 (December 1, 2006): 125601. http://dx.doi.org/10.1117/1.2405348.

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20

Sabbatini, Federico, and Catia Grimani. "Symbolic knowledge extraction from opaque predictors applied to cosmic-ray data gathered with LISA Pathfinder." Aeronautics and Aerospace Open Access Journal 6, no. 3 (July 26, 2022): 90–95. http://dx.doi.org/10.15406/aaoaj.2022.06.00145.

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Machine learning models are nowadays ubiquitous in space missions, performing a wide variety of tasks ranging from the prediction of multivariate time series through the detection of specific patterns in the input data. Adopted models are usually deep neural networks or other complex machine learning algorithms providing predictions that are opaque, i.e., human users are not allowed to understand the rationale behind the provided predictions. Several techniques exist in the literature to combine the impressive predictive performance of opaque machine learning models with human-intelligible prediction explanations, as for instance the application of symbolic knowledge extraction procedures. In this paper are reported the results of different knowledge extractors applied to an ensemble predictor capable of reproducing cosmic-ray data gathered on board the LISA Pathfinder space mission. A discussion about the readability/fidelity trade-off of the extracted knowledge is also presented.

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21

Wang, Gang, Wei-Tou Ni, and An-Ming Wu. "Orbit design and thruster requirement for various constant arm space mission concepts for gravitational-wave observation." International Journal of Modern Physics D 29, no. 04 (January 30, 2020): 1940006. http://dx.doi.org/10.1142/s0218271819400066.

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In previous papers, we have addressed the issues of orbit design and thruster requirement for the constant arm versions of Astrodynamical Middle-frequency Interferometric Gravitational-wave Observatory (AMIGO) mission concept and for the constant arm gravitational wave (GW) mission concept of Atom Interferometric Gravitational-wave Space Observatory (AIGSO). In this paper, we apply similar methods to the orbit design and thruster requirement for the constant arm GW missions B-DECIGO and DECIGO, and estimate the yearly propellant requirements at the specific impulse [Formula: see text][Formula: see text]s and [Formula: see text][Formula: see text]s. For the geocentric orbit options of B-DECIGO which we have explored, the fuel mass requirement is a concern. For the heliocentric orbit options of B-DECIGO and DECIGO, the fuel requirement to keep the arm equal and constant should be easily satisfied. Furthermore, we explore the thruster and propellant requirements for constant arm versions of LISA and TAIJI missions and find the fuel mass requirement is not a show stopper either. The proof mass actuation noise is a concern. To have enough dynamical range, an alternate proof mass is required. Detailed laboratory study is warranted.

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22

GRIMANI, CATIA. "IMPLICATIONS OF GALACTIC AND SOLAR PARTICLE MEASUREMENTS ON BOARD INTERFEROMETERS FOR GRAVITATIONAL WAVE DETECTION IN SPACE." International Journal of Modern Physics D 22, no. 01 (January 2013): 1341006. http://dx.doi.org/10.1142/s021827181341006x.

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Test-mass charging due to galactic cosmic rays (GCRs) and solar energetic particles (SEPs) represents one of the major sources of noise for missions devoted to gravitational wave detection in space. Particle detectors on board future space interferometers will help in monitoring the test-mass charging process. Variations and fluctuations of GCRs and evolution of SEP events of different intensities are discussed here for the correlation of SEP radiation monitor observations and particle fluxes charging the test masses. We consider the performance of the radiation monitors designed for the LISA Pathfinder mission for the results presented in this work. We point out that in addition to the primary use of test-mass charging monitoring, particle detectors on board space interferometers will naturally provide SEP observations at different intervals in heliolongitude and distances from Earth for space weather applications.

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23

Moore, Christopher J., Davide Gerosa, and Antoine Klein. "Are stellar-mass black-hole binaries too quiet for LISA?" Monthly Notices of the Royal Astronomical Society: Letters 488, no. 1 (July 1, 2019): L94—L98. http://dx.doi.org/10.1093/mnrasl/slz104.

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ABSTRACT The progenitors of the high-mass black-hole mergers observed by LIGO and Virgo are potential LISA sources and promising candidates for multiband GW observations. In this letter, we consider the minimum signal-to-noise ratio these sources must have to be detected by LISA bearing in mind the long duration and complexity of the signals. Our revised threshold of ρthr ∼ 15 is higher than previous estimates, which significantly reduces the expected number of events. We also point out the importance of the detector performance at high frequencies and the duration of the LISA mission, which both influence the event rate substantially.

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Wagg, T., F. S. Broekgaarden, S. E. de Mink, N. Frankel, L. A. C. van Son, and S. Justham. "Gravitational Wave Sources in Our Galactic Backyard: Predictions for BHBH, BHNS, and NSNS Binaries Detectable with LISA." Astrophysical Journal 937, no. 2 (October 1, 2022): 118. http://dx.doi.org/10.3847/1538-4357/ac8675.

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Abstract Future searches for gravitational waves from space will be sensitive to double compact objects in our Milky Way. We present new simulations of the populations of double black holes (BHBHs), BH neutron stars (BHNSs), and double neutron stars (NSNSs) that will be detectable by the planned space-based gravitational-wave detector called Laser Interferometer Space Antenna (LISA). For our estimates, we use an empirically informed model of the metallicity-dependent star formation history of the Milky Way. We populate it using an extensive suite of binary population-synthesis predictions for varying assumptions relating to mass transfer, common-envelope, supernova kicks, remnant masses, and wind mass-loss physics. For a 4(10) yr LISA mission, we predict between 30–370(50–550) detections over these variations, out of which 6–154 (9–238) are BHBHs, 2–198 (3–289) are BHNSs, and 3–35 (4–57) are NSNSs. We expect that about 50% (60%) can be distinguished from double white dwarf sources based on their mass or eccentricity and localization. Specifically, for about 10% (15%), we expect to be able to determine chirp masses better than 10%. For 13% (13%), we expect sky-localizations better than 1°. We discuss how the variations in the physics assumptions alter the distribution of properties of the detectable systems, even when the detection rates are unchanged. We further discuss the possibility of multimessenger observations of pulsar populations with the Square Kilometre Array and assess the benefits of extending the LISA mission.

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Bourgoin, A., C. Le Poncin-Lafitte, S. Mathis, and M. C. Angonin. "Magnetic fields in galactic binaries and gravitational waves." Proceedings of the International Astronomical Union 16, S363 (June 2020): 361–62. http://dx.doi.org/10.1017/s1743921322000813.

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AbstractThe Laser Interferometer Space Antenna (LISA) mission will observe from space gravitational waves emitted by neutron stars and white dwarfs within galactic binaries. These compact stars can have intense magnetic fields. Therefore, the impact of the magnetic fields on the orbital and the spins evolution of binary systems can potentially be detected by LISA through the GW’s strain. Within the magnetic dipole-dipole approximation, we found that magnetism generates a secular drift of the mean longitude which, in turn, shifts all the frequencies contained in the GW signal. For a quasi-circular orbit, the signal is mainly monochromatic and the magnetic shift is proportional to the product of the magnetic moments and is inversely proportional to the 7/2 power of the semi-major axis. Hence, for a highly magnetic binary system in compact orbit, a non-negligible amount of the frequency measured by LISA might have a magnetic origin.

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26

Letson, Benjamin C., Simon Barke, Peter Wass, Guido Mueller, Fan Ren, Stephen J. Pearton, and John W. Conklin. "Deep UV AlGaN LED reliability for long duration space missions." Journal of Vacuum Science & Technology A 41, no. 1 (January 2023): 013202. http://dx.doi.org/10.1116/6.0002199.

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Space-based gravitational wave detection will be carried out by the laser interferometer space antenna (LISA), a joint European Space Agency and NASA collaboration. The configuration of this antenna will include three identical spacecraft in a triangular formation separated by [Formula: see text], flying in a drag-free formation around free-falling test masses. Charging of the test masses by cosmic ray fluxes and solar energetic particles must be compensated by photons that contain more energy than the effective work function of gold ([Formula: see text]). The UV photons will be provided by AlGaN light emitting diodes, which must operate reliably for the duration of the mission. We have tested a large number (96 for dc and pulsed testing, more than 200 for all tests) of UV LEDs over a period of up to 600 days to characterize their performance over a wide range of operating conditions, assessing the lifetime performance under dc (1–[Formula: see text] drive current) and pulsed conditions (500–100 000 pulses per second) and temperatures ranging from [Formula: see text] to [Formula: see text]. Degradation of UV light output is faster at elevated temperatures and dc conditions. Preselection of LEDs based on initial spectral ratio of peak-to-midgap emission and ideality factor provides a positive correlation with subsequent reliability. The UV LEDs used for LISA will need to support 2 years of cruise and commissioning plus a 4-year baseline science mission.

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Korol, Valeriya, Na’ama Hallakoun, Silvia Toonen, and Nikolaos Karnesis. "Observationally driven Galactic double white dwarf population for LISA." Monthly Notices of the Royal Astronomical Society 511, no. 4 (February 16, 2022): 5936–47. http://dx.doi.org/10.1093/mnras/stac415.

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ABSTRACT Realistic models of the Galactic double white dwarf (DWD) population are crucial for testing and quantitatively defining the science objectives of the Laser Interferometer Space Antenna (LISA), a future European Space Agency’s gravitational-wave observatory. In addition to numerous individually detectable DWDs, LISA will also detect an unresolved confusion foreground produced by the underlying Galactic population, which will affect the detectability of all LISA sources at frequencies below a few mHz. So far, the modelling of the DWD population for LISA has been based on binary population synthesis (BPS) techniques. The aim of this study is to construct an observationally driven population. To achieve this, we employ a model developed by Maoz, Hallakoun & Badenes for the statistical analysis of the local DWD population using two complementary large, multi-epoch, spectroscopic samples: the Sloan Digital Sky Survey, and the Supernova Ia Progenitor surveY. We calculate the number of LISA-detectable DWDs and the Galactic confusion foreground, based on their assumptions and results. We find that the observationally driven estimates yield (1) 2–5 times more individually detectable DWDs than various BPS forecasts, and (2) a significantly different shape of the DWD confusion foreground. Both results have important implications for the LISA mission. A comparison between several variations to our underlying assumptions shows that our observationally driven model is robust, and that the uncertainty on the total number of LISA-detectable DWDs is in the order of 20 per cent.

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28

Gath, Peter F., Hans Reiner Schulte, and Dennis Weise. "Challenges in the Measurement and Data-Processing Chain of the LISA Mission." Space Science Reviews 151, no. 1-3 (December 15, 2009): 61–73. http://dx.doi.org/10.1007/s11214-009-9604-8.

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29

Lau, Mike Y. M., Ilya Mandel, Alejandro Vigna-Gómez, Coenraad J. Neijssel, Simon Stevenson, and Alberto Sesana. "Detecting double neutron stars with LISA." Monthly Notices of the Royal Astronomical Society 492, no. 3 (January 10, 2020): 3061–72. http://dx.doi.org/10.1093/mnras/staa002.

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ABSTRACT We estimate the properties of the double neutron star (DNS) population that will be observable by the planned space-based interferometer Laser Interferometer Space Antenna (LISA). By following the gravitational radiation-driven evolution of DNSs generated from rapid population synthesis of massive binary stars, we estimate that around 35 DNSs will accumulate a signal-to-noise ratio above 8 over a 4-yr LISA mission. The observed population mainly comprises Galactic DNSs (94 per cent), but detections in the LMC (5 per cent) and SMC (1 per cent) may also be expected. The median orbital frequency of detected DNSs is expected to be 0.8 mHz, and many of them will be eccentric (median eccentricity of 0.11). LISA is expected to localize these DNSs to a typical angular resolution of 2°. We expect the best-constrained DNSs to have eccentricities known to a few parts in a thousand, chirp masses measured to better than 1 per cent fractional uncertainty, and sky localization at the level of a few arcminutes. The orbital properties will provide insights into DNS progenitors and formation channels. The localizations may allow neutron star natal kick magnitudes to be constrained through the Galactic distribution of DNSs, and make it possible to follow up the sources with radio pulsar searches. LISA is also expected to resolve ∼104 Galactic double white dwarfs, many of which may have binary parameters that resemble DNSs; we discuss how the combined measurement of binary eccentricity, chirp mass, and sky location may aid the identification of a DNS.

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30

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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31

Danzmann, K. "LISA — An ESA cornerstone mission for the detection and observation of gravitational waves." Advances in Space Research 32, no. 7 (October 2003): 1233–42. http://dx.doi.org/10.1016/s0273-1177(03)90323-1.

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32

Ren, Liangliang, Chengyuan Li, Bo Ma, Sihao Cheng, Shun-Jia Huang, Baitian Tang, and Yi-ming Hu. "A Systematic Search for Short-period Close White Dwarf Binary Candidates Based on Gaia EDR3 Catalog and Zwicky Transient Facility Data." Astrophysical Journal Supplement Series 264, no. 2 (January 31, 2023): 39. http://dx.doi.org/10.3847/1538-4365/aca09e.

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Abstract Galactic short-period close white dwarf binaries (CWDBs) are important objects for space-borne gravitational-wave (GW) detectors in the millihertz frequency bands. Due to the intrinsically low luminosity, only about 25 identified CWDBs are detectable by the Laser Interferometer Space Antenna (LISA), which are also known as verification binaries (VBs). The Gaia Early Data Release 3 (EDR3) provids a catalog containing a large number of CWDB candidates, which also includes parallax and photometry measurements. We crossmatch the Gaia EDR3 and Zwicky Transient Facility public data release 8, and apply period-finding algorithms to obtain a sample of periodic variables. The phase-folded light curves are inspected, and finally we obtain a binary sample containing 429 CWDB candidates. We further classify the samples into eclipsing binaries (including 58 HW Vir-type binaries, 65 EA-type binaries, 56 EB-type binaries, and 41 EW-type binaries) and ellipsoidal variations (209 ELL-type binaries). We discovered four ultrashort period binary candidates with unique light-curve shapes. We estimate the GW amplitude of all of our binary candidates, and calculate the corresponding signal-to-noise ratio (S/N) for TianQin and LISA. We find two (six) potential GW candidates with S/Ns greater than 5 in the nominal mission time of TianQin (LISA), which increases the total number of candidate VBs for TianQin (LISA) to 18 (31).

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33

Kupfer, Thomas, Valeriya Korol, Tyson B. Littenberg, Sweta Shah, Etienne Savalle, Paul J. Groot, Thomas R. Marsh, et al. "LISA Galactic Binaries with Astrometry from Gaia DR3." Astrophysical Journal 963, no. 2 (March 1, 2024): 100. http://dx.doi.org/10.3847/1538-4357/ad2068.

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Abstract Galactic compact binaries with orbital periods shorter than a few hours emit detectable gravitational waves (GWs) at low frequencies. Their GW signals can be detected with the future Laser Interferometer Space Antenna (LISA). Crucially, they may be useful in the early months of the mission operation in helping to validate LISA's performance in comparison to prelaunch expectations. We present an updated list of 55 candidate LISA-detectable binaries with measured properties, for which we derive distances based on Gaia Data Release 3 astrometry. Based on the known properties from electromagnetic observations, we predict the LISA detectability after 1, 3, 6, and 48 months using Bayesian analysis methods. We distinguish between verification and detectable binaries as being detectable after 3 and 48 months, respectively. We find 18 verification binaries and 22 detectable sources, which triples the number of known LISA binaries over the last few years. These include detached double white dwarfs, AM CVn binaries, one ultracompact X-ray binary, and two hot subdwarf binaries. We find that across this sample the GW amplitude is expected to be measured to ≈10% on average, while the inclination is expected to be determined with ≈15° precision. For detectable binaries, these average errors increase to ≈50% and ≈40°, respectively.

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34

Armano, M., H. Audley, J. Baird, P. Binetruy, M. Born, D. Bortoluzzi, E. Castelli, et al. "Spacecraft and interplanetary contributions to the magnetic environment on-board LISA Pathfinder." Monthly Notices of the Royal Astronomical Society 494, no. 2 (April 18, 2020): 3014–27. http://dx.doi.org/10.1093/mnras/staa830.

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ABSTRACT 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. LPF 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 LPF operations. We characterize the magnetic environment within the spacecraft, study the time evolution of the magnetic field and its stability down to 20 μHz, 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 characterize the non-stationary component of the fluctuations of the magnetic field below the mHz and relate them to the dynamics of the solar wind.

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35

Digman, Matthew C., and Neil J. Cornish. "LISA Gravitational Wave Sources in a Time-varying Galactic Stochastic Background." Astrophysical Journal 940, no. 1 (November 1, 2022): 10. http://dx.doi.org/10.3847/1538-4357/ac9139.

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Abstract A unique challenge for data analysis with the Laser Interferometer Space Antenna (LISA) is that the noise backgrounds from instrumental noise and astrophysical sources will change significantly over both the year and the entire mission. Variations in the noise levels will be on timescales comparable to, or shorter than, the time most signals spend in the detector’s sensitive band. The variation in the amplitude of the galactic stochastic GW background from galactic binaries as the antenna pattern rotates relative to the galactic center is a particularly significant component of the noise variation. LISA’s sensitivity to different source classes will therefore vary as a function of sky location and time. The variation will impact both overall signal-to-noise and the efficiency of alerts to EM observers to search for multimessenger counterparts.

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36

Xie, Yafei, Ji Fan, Chun Zhao, Shitao Yan, Chenyuan Hu, and Liangcheng Tu. "Modeling and Analysis of the Noise Performance of the Capacitive Sensing Circuit with a Differential Transformer." Micromachines 10, no. 5 (May 15, 2019): 325. http://dx.doi.org/10.3390/mi10050325.

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Capacitive sensing is a key technique to measure the test mass movement with a high resolution for space-borne gravitational wave detectors, such as Laser Interferometer Space Antenna (LISA) and TianQin. The capacitance resolution requirement of TianQin is higher than that of LISA, as the arm length of TianQin is about 15 times shorter. In this paper, the transfer function and capacitance measurement noise of the circuit are modeled and analyzed. Figure-of-merits, including the product of the inductance L and the quality factor Q of the transformer, are proposed to optimize the transformer and the capacitance measurement resolution of the circuit. The LQ product improvement and the resonant frequency augmentation are the key factors to enhance the capacitance measurement resolution. We fabricated a transformer with a high LQ product over a wide frequency band. The evaluation showed that the transformer can generate a capacitance resolution of 0.11 aF/Hz1/2 at a resonant frequency of 200 kHz, and the amplitude of the injection wave would be 0.6 V. This result supports the potential application of the proposed transformer in space-borne gravitational wave detection and demonstrates that it could relieve the stringent requirements for other parameters in the TianQin mission.

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37

Shirokov, S. I., and Yu V. Baryshev. "A crucial test of the phantom closed cosmological model." Monthly Notices of the Royal Astronomical Society: Letters 499, no. 1 (September 24, 2020): L101—L104. http://dx.doi.org/10.1093/mnrasl/slaa167.

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ABSTRACT We suggest a crucial direct-observational test for measuring distinction between the standard ΛCDM model and recently proposed phantom dark energy positive curvature cosmological model. The test is based on the fundamental distance–flux–redshift relation for general Friedmann models. It does not depend on the CMBR data, on the large-scale structure growth models, and also on the value of the Hubble constant H0. Our crucial test can be performed by future gamma-ray burst observations with THESEUS space mission and by using gravitational-wave standard siren observations with modern advanced LIGO–Virgo and also forthcoming LISA detectors.

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38

Baumgartner, Sandra, Mauro Bernardini, José R. Canivete Cuissa, Hugues de Laroussilhe, Alison M. W. Mitchell, Benno A. Neuenschwander, Prasenjit Saha, Timothée Schaeffer, Deniz Soyuer, and Lorenz Zwick. "Towards a polarization prediction for LISA via intensity interferometry." Monthly Notices of the Royal Astronomical Society 498, no. 3 (September 2, 2020): 4577–89. http://dx.doi.org/10.1093/mnras/staa2638.

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ABSTRACT Compact Galactic Binary Systems with orbital periods of a few hours are expected to be detected in gravitational waves (GW) by Laser Interferometer Space Antenna (LISA) or a similar mission. At present, these so-called verification binaries provide predictions for GW frequency and amplitude. A full polarization prediction would provide a new method to calibrate LISA and other GW observatories, but requires resolving the orientation of the binary on the sky, which is not currently possible. We suggest a method to determine the elusive binary orientation and hence predict the GW polarization, using km-scale optical intensity interferometry. The most promising candidate is CD–30° 11223, consisting of a hot helium subdwarf with mB = 12 and a much fainter white dwarf companion, in a nearly edge-on orbit with period 70.5 min. We estimate that the brighter star is tidally stretched by 6 per cent. Resolving the tidal stretching would provide the binary orientation. The resolution needed is far beyond any current instrument, but not beyond current technology. We consider scenarios where an array of telescopes with km-scale baselines and/or the Very Large Telescope (VLT) and Extremely Large Telescope (ELT) are equipped with recently developed kilopixel sub-ns single-photon counters and used for intensity interferometry. We estimate that a team-up of the VLT and ELT could measure the orientation to ±1° at 2σ confidence in 24 h of observation.

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39

Naoz, Smadar, and Zoltán Haiman. "The Enhanced Population of Extreme Mass-ratio Inspirals in the LISA Band from Supermassive Black Hole Binaries." Astrophysical Journal Letters 955, no. 2 (September 26, 2023): L27. http://dx.doi.org/10.3847/2041-8213/acf8c9.

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Abstract Extreme mass-ratio inspirals (EMRIs) take place when a stellar-mass black hole (BH) merges with a supermassive BH (SMBH). The gravitational-wave emission from such an event is expected to be detectable by the future Laser Interferometer Space Antenna (LISA) and other millihertz detectors. It was recently suggested that the EMRI rate in SMBH binary systems is orders of magnitude higher than the EMRI rate around a single SMBH with the same total mass. Here we show that this high rate can produce thousands of SMBH–BH sources at a redshift of unity. We predict that LISA may detect a few hundred of these EMRIs with signal-to-noise ratio above S/N ≥8 within a 4 yr mission lifetime. The remaining subthreshold sources will contribute to a large confusion noise, which is approximately an order of magnitude above LISA’s sensitivity level. Finally, we suggest that the individually detectable systems, as well as the background noise from the subthreshold EMRIs, can be used to constrain the SMBH binary fraction in the low-redshift Universe.

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40

Zhang, Fupeng, Xian Chen, Lijing Shao, and Kohei Inayoshi. "The Eccentric and Accelerating Stellar Binary Black Hole Mergers in Galactic Nuclei: Observing in Ground and Space Gravitational-wave Observatories." Astrophysical Journal 923, no. 2 (December 1, 2021): 139. http://dx.doi.org/10.3847/1538-4357/ac2c07.

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Abstract We study the stellar binary black holes (BBHs) inspiraling/merging in galactic nuclei based on our numerical method GNC. We find that 3%–40% of all newborn BBHs will finally merge due to various dynamical effects. In a five-year mission, up to 104, 105, and ∼100 of BBHs inspiraling/merging in galactic nuclei can be detected with signal-to-noise ration >8 in Advanced LIGO (aLIGO), Einstein/DECIGO, and TianQin/LISA/TaiJi, respectively. Roughly tens are detectable in both LISA/TaiJi/TianQin and aLIGO. These BBHs have two unique characteristics. (1) Significant eccentricities: 1%–3%, 2%–7%, or 30%–90% of them have e i > 0.1 when they enter into aLIGO, Einstein, or space observatories, respectively. Such high eccentricities provide a possible explanation for that of GW190521. Most highly eccentric BBHs are not detectable in LISA/Tianqin/TaiJi before entering into aLIGO/Einstein, as their strain becomes significant only at f GW ≳ 0.1 Hz. DECIGO becomes an ideal observatory to detect those events, as it can fully cover the rising phase. (2) Up to 2% of BBHs can inspiral/merge at distances ≲103 r SW from the massive black hole, with significant accelerations, such that the Doppler phase drift of ∼10–105 of them can be detected with signal-to-noise ratio >8 in space observatories. The energy density of the gravitational-wave backgrounds (GWBs) contributed by these BBHs deviates from the power-law slope of 2/3 at f GW ≲ 1 mHz. The high eccentricity, significant accelerations, and the different profile of the GWB of these sources make them distinguishable, and thus interesting for future gravitational-wave detections and tests of relativities.

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41

CAMP, JORDAN, ALEXANDER STROEER, JOHN CANNIZZO, and ROBERT SCHOFIELD. "SEARCHING FOR GRAVITATIONAL WAVES WITH THE HILBERT–HUANG TRANSFORM." Advances in Adaptive Data Analysis 01, no. 04 (October 2009): 643–66. http://dx.doi.org/10.1142/s1793536909000254.

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Gravitational waves are a consequence of Einstein's theory of general relativity applied to the motion of very dense and massive objects such as black holes and neutron stars. Their detection will reveal a wealth of information about these mysterious objects that cannot be obtained with electromagnetic probes. Two projects are underway to attempt the detection of gravitational waves: LISA, a space based mission being designed to search for waves from supermassive black holes at the centers of galaxies, and LIGO, a ground based facility that is now searching for waves from supernovae, pulsars, and the coalescence of black hole and neutron star systems. Because general relativity is an inherently nonlinear theory, many of the predicted source waveforms show strong frequency modulation. In addition, the LIGO and LISA detectors are highly sensitive devices that produce a variety of nonlinear, transient noise features. Thus the unique capabilities of the HHT, the extraction of intrawave modulation and the characterization of nonlinear and nonstationary signals, have a natural application to both signal detection and experimental characterization of the detectors.

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42

Lamberts, Astrid, Sarah Blunt, Tyson B. Littenberg, Shea Garrison-Kimmel, Thomas Kupfer, and Robyn E. Sanderson. "Predicting the LISA white dwarf binary population in the Milky Way with cosmological simulations." Monthly Notices of the Royal Astronomical Society 490, no. 4 (October 10, 2019): 5888–903. http://dx.doi.org/10.1093/mnras/stz2834.

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ABSTRACT White dwarf binaries with orbital periods below 1 h will be the most numerous sources for the space-based gravitational wave detector Laser Interferometer Space Antenna (LISA). Based on thousands of individually resolved systems, we will be able to constrain binary evolution and provide a new map of the Milky Way and its close surroundings. In this paper we predict the main properties of populations of different types of detached white dwarf binaries detected by LISA over time. For the first time, we combine a high-resolution cosmological simulation of a Milky Way-mass galaxy (taken from the FIRE project) with a binary population synthesis model for low- and intermediate-mass stars. Our Galaxy model therefore provides a cosmologically realistic star formation and metallicity history for the Galaxy and naturally produces its different components such as the thin and thick disc, the bulge, the stellar halo, and satellite galaxies and streams. Thanks to the simulation, we show how different Galactic components contribute differently to the gravitational wave signal, mostly due to their typical age and distance distributions. We find that the dominant LISA sources will be He–He double white dwarfs (DWDs) and He–CO DWDs with important contributions from the thick disc and bulge. The resulting sky map of the sources is different from previous models, with important consequences for the searches for electromagnetic counterparts and data analysis. We also emphasize that much of the science-enabling information regarding white dwarf binaries, such as the chirp mass and the sky localization, becomes increasingly rich with long observations, including an extended mission up to 8 yr.

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43

Jin, Hong-Bo, and Peng Xu. "The pipeline of data processing for TAIJI-1 space mission in the TAIJI program for the detection of gravitational wave." International Journal of Modern Physics A 36, no. 11n12 (March 10, 2021): 2140025. http://dx.doi.org/10.1142/s0217751x2140025x.

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TAIJI-1 is a micro-gravity experiment spacecraft. The mission target is to verify some key techniques of the spacecraft payloads for the gravitational wave detection, which involve laser interferometer, gravity reference sensor, drag-free control technology, micro-propulsion system, super-quiescent spacecraft platform, etc. The verification of the data processing pipeline required by the next stage of TAIJI Program is also performed. In order to benefit from the joint observatory between TAIJI and LISA in the future, as a space mission, the science operations refer to the existing ESA and NASA standard models, which include the Mission Operations Center (MOC), the Science Operations Center (SOC), the Data Processing Center (DPC), etc. The data processing pipeline connects between SOC and DPC. The SOC obtains the level-0 data from MOC and DPC performs the data processing and distributes the level-2 and level-3 data to SOC. For TAIJI-1 mission, SOC and DPC are two subsystems, which are included into the named science application system (SAS). That is the one of the six-function systems, which operate Chinese space mission. MOC is relevant to the ground support system (GSS) and spacecraft control system, that are also the ones of six-function systems of Chinese space mission. The on-orbit experiment plannings are transported from SAS to GSS, that is similar to from SOC to MOC in NASA standard models. The computer construction and computer software are the basic elements of the SAS, that are constructed completely, before the TAIJI-1 was launched. After TAIJI-1 enters the orbit, the data processing pipeline begins to work and the experimental items of TAIJI-1 are performed in the pipeline. The basic functions, performances and optimization functions of the detection devices in the payloads are verified completely 3 months after launch. In the same time, the methods of data analysis and processing are also verified. As a result, the required indicators of key techniques of the spacecraft for the gravitational wave detection are justified. The data processing pipeline is also reasonable. The relevant codes for data analysis and processing will benefit the next stage of TAIJI Program.

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44

Gao, Zucheng, Xian Chen, Yi-Ming Hu, Jian-Dong Zhang, and Shun-Jia Huang. "A higher probability of detecting lensed supermassive black hole binaries by LISA." Monthly Notices of the Royal Astronomical Society 512, no. 1 (February 11, 2022): 1–10. http://dx.doi.org/10.1093/mnras/stac365.

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ABSTRACT Gravitational lensing of gravitational waves (GWs) is a powerful probe of the matter distribution in the universe. Here we revisit the wave-optics effects induced by dark matter (DM) haloes on the GW signals of merging massive black hole binaries (MBHBs), and we study the possibility of discerning these effects using the Laser Interferometer Space Antenna (LISA). In particular, we include the haloes in the low-mass range of $10^5\!-\!10^8\, \mathrm{M}_\odot$ since they are the most numerous according to the cold DM model. We simulate the lensed signals corresponding to a wide range of impact parameters, and we find distinguishable deviation from the standard best-fitting GW templates even when the impact parameter is as large y ≃ 50. Consequently, we estimate that over $(0.1\!-\!1.6){{\ \rm per\ cent}}$ of the MBHBs in the mass range of $10^{5.0}\!-\!10^{6.5}\, \mathrm{M}_\odot$ and the redshift range of 4 − 10 should show detectable wave-optics effects. This probability is one order of magnitude higher than that derived in previous works. The uncertainty comes mainly from the mass function of the DM haloes. Not detecting any signal during the LISA mission would imply that DM haloes with $10^5\!-\!10^8\, \mathrm{M}_\odot$ are less numerous than what the cold DM model predicts.

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45

Pfister, Hugo, Martina Toscani, Thomas Hong Tsun Wong, Jane Lixin Dai, Giuseppe Lodato, and Elena M. Rossi. "Observable gravitational waves from tidal disruption events and their electromagnetic counterpart." Monthly Notices of the Royal Astronomical Society 510, no. 2 (November 26, 2021): 2025–40. http://dx.doi.org/10.1093/mnras/stab3387.

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ABSTRACT We estimate the rate of tidal disruption events (TDEs) that will be detectable with future gravitational wave detectors as well as the most probable properties of these events and their possible electromagnetic counterpart. To this purpose, we combine standard gravitational waves and electromagnetic results with detailed rates estimates. We find that the Laser Interferometer Space Antenna (LISA) should not detect any TDEs, unless black holes (BHs) are typically embedded by a young stellar population, which, in this situation, could lead up to few 10 events during the duration of the mission. If there are gravitational wave observations, these events should also be observable in the X-ray or the optical/UV part of the electromagnetic spectrum, which may open up the multimessenger era for TDEs. The generation of detectors following LISA will at least yearly observe 104 TDEs at cosmological distances, allowing to do population studies and constrain the black hole mass function. In all cases, most probable events should be around black holes with a mass such that the Keplerian frequency at the Schwarzschild radius is similar to the optimal frequency of the detector and with a large penetration factor.

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46

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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47

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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48

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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49

Fragione, Giacomo. "Mergers of Supermassive and Intermediate-mass Black Holes in Galactic Nuclei from Disruptions of Star Clusters." Astrophysical Journal 939, no. 2 (November 1, 2022): 97. http://dx.doi.org/10.3847/1538-4357/ac98b6.

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Abstract Gravitational waves (GWs) offer an unprecedented opportunity to survey the sky and detect mergers of compact objects. While intermediate-mass black holes (IMBHs) have not been detected beyond any reasonable doubt with either dynamical or accretion signatures, the GW landscape appears very promising. Mergers of an IMBH with a supermassive black hole (SMBH) will be primary sources for the planned space-based mission LISA and could be observed up to the distant universe. SMBH–IMBH binaries can be formed as a result of the migration and merger of stellar clusters at the center of galaxies, where an SMBH lurks. We build for the first time a semianalytical framework to model this scenario and find that the comoving merger rate of SMBH–IMBH binaries is ∼10−4 Gpc−3 yr−1 in the local universe for a unity IMBH occupation fraction, scales linearly with it, and has a peak at z ≈ 0.5–2. Our model predicts ∼0.1 events yr−1 within redshift z ≈ 3.5 if 10% of the inspiraled star clusters hosted an IMBH, while ∼1 event yr−1 for a unity occupation fraction. More than 90% of these systems will be detectable with LISA with a signal-to-noise ratio larger than 10, promising to potentially find a family of IMBHs.

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50

Xuan, Zeyuan, Smadar Naoz, Bence Kocsis, and Erez Michaely. "Detecting Gravitational Wave Bursts from Stellar-mass Binaries in the mHz Band." Astrophysical Journal 965, no. 2 (April 1, 2024): 148. http://dx.doi.org/10.3847/1538-4357/ad2c94.

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Abstract The dynamical formation channels of gravitational wave (GW) sources typically involve a stage when the compact object binary source interacts with the environment, which may excite its eccentricity, yielding efficient GW emission. For the wide eccentric compact object binaries, the GW emission happens mostly near the pericenter passage, creating a unique, burst-like signature in the waveform. This work examines the possibility of stellar-mass bursting sources in the mHz band for future LISA detections. Because of their long lifetime (∼107 yr) and promising detectability, the number of mHz bursting sources can be large in the local Universe. For example, based on our estimates, there will be ∼3–45 bursting binary black holes in the Milky Way, with ∼102–104 bursts detected during the LISA mission. Moreover, we find that the number of bursting sources strongly depends on their formation history. If certain regions undergo active formation of compact object binaries in the recent few million years, there will be a significantly higher bursting source fraction. Thus, the detection of mHz GW bursts not only serves as a clue for distinguishing different formation channels, but also helps us understand the star formation history in different regions of the Milky Way.

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