Numerical simulation of sky localization for LISA-TAIJI joint observation

Wang, Gang; Ni, Wei-Tou; Han, Wen-Biao; Yang, Shaoyan; Zhong, Xin

doi:10.1103/physrevd.102.024089

Cited by 42 publications

(36 citation statements)

References 64 publications

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“…In Fig. 3, we show the target sensitivity S(f ) for LISA (Robson, Cornish, & Liu 2019), Taiji (Wang et al 2020) and TianQin (Huang et al 2020), along with the Galactic confusion noise for T = 10yr (Robson, Cornish, & Liu 2019). For LISA with the armlength of 2.5Gm, the A-and E-channels can be regarded as the main data streams for BBH detection at f 30mHz (Prince et al 2002).…”

Section: Evolution Of Individual Binary Black Holesmentioning

confidence: 99%

“…Thus, the coincident operation is more advantageous than the sequential operation for detecting stellarmass BBHs. The coincident operation is also beneficial for sky localization of merging massive black hole binaries (see e.g., Ruan et al 2018;Wang et al 2020) and for correlation analysis of stochastic backgrounds (see e.g., Seto 2020).…”

Section: Joint Operationmentioning

confidence: 99%

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How many extra-Galactic stellar-mass binary black holes will be detected by space gravitational-wave interferometers?

Seto,

Kyutoku

2022

Preprint

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On the basis of GWTC-3, we discuss the detection prospect of extra-Galactic binary black holes (BBHs) by space gravitational-wave interferometers. In particular, targeting BBHs with component masses around 5-100M , we directly incorporate the chirp mass distribution of the 62 BBHs detected at high significance. We find that, due to the reduction of both the comoving merger rate and a weighted average of chirp masses, the expected detection numbers are generally much smaller than the results obtained by the same authors immediately after the report of GW150914. For LISA, the total BBH detections are estimated to be N tot ∼ 2(T /4yr) 3/2 (ρ thr /10) −3 , dominated by nearly monochromatic BBHs (ρ thr : the detection threshold, T : the observational period). TianQin will have a total detection number N tot similar to LISA. Meanwhile, TianQin has potential to find N mer ∼ 0.6(T /4yr) 7/4 (ρ thr /10) −3 BBHs that merge in the observational period. This number for merging BBHs is 4-5 times larger than that of LISA, because of the difference between the optimal bands. We also investigate prospects for joint operations of multiple detectors, finding that concurrent observations will be more advantageous than sequential ones.

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Section: Evolution Of Individual Binary Black Holesmentioning

confidence: 99%

Section: Joint Operationmentioning

confidence: 99%

How many extra-Galactic stellar-mass binary black holes will be detected by space gravitational-wave interferometers?

Seto,

Kyutoku

2022

Preprint

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“…These three combinations should cover all the possible dual detector scenarios except the LISA with a co-located TAIJI having a −60 • inclination which would be insipid because neither the large separation benefiting for the compact binary observation nor strong cross-correlation for the SGWB observation is expected. The numerical orbits for the TAIJIp and TAIJIc are from our work in [24,32], and the orbit for TAIJIm is newly obtained from our optimization method in [32][33][34][35][36][37].…”

Section: A the Lisa And Taiji Orbital Configurationsmentioning

confidence: 99%

“…To achieve stable interferometer arms, the S/C formation plane of the LISA/TAIJI is designed to be ±60 • with the ecliptic by employing the Clohessy-Wiltshire framework [22]. By assuming the TAIJI is leading the Earth by 20 • and LISA is trailing the Earth by 20 • , Ruan et al [23] and Wang et al [24] investigated the sky localization improvement of the LISA-TAIJI network compared to the single LISA mission. Omiya and Seto [25], Seto [26], and Orlando et al [27] evaluated network capabilities for the SGWB obser-vation.…”

Section: Introductionmentioning

confidence: 99%

Alternative LISA-TAIJI networks

Wang,

Ni,

Han

et al. 2021

Preprint

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The space-borne gravitational wave (GW) detectors, LISA and TAIJI, are planned to be launched in the 2030s. The dual detectors with comparable sensitivities will form a network observing GW with significant advantages. In this work, we investigate the three possible LISA-TAIJI networks for the different location and orientation compositions of LISA orbit (+60 • inclination and trailing the Earth by 20 • ) and alternative TAIJI orbit configurations including TAIJIp (+60 • inclination and leading the Earth by 20 • ), TAIJIc (+60 • inclination and co-located with LISA), TAIJIm (−60 • inclination and leading the Earth by 20 • ). In the three LISA-TAIJI configurations, the LISA-TAIJIm network shows the best performance on the sky localization and polarization determination for the massive binary system due to their better complementary antenna pattern, and LISA-TAIJIc could achieve the best cross-correlation and observe the stochastic GW background with an optimal sensitivity.

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“…Since Taiji would launch in the same period [ 3 ], it is possible to combine these two space-based GW observatories into a LISA-Taiji network [ 4 ], which can improve the sky localization of GW sources due to the faraway separation of the two constellations ( Figure 1 ). In this letter, we investigate for the first time the network's potential ability to localize GW sources (Notice that the localization capacity of the LISA-Taiji network was further studied in [ 5 ] after the present work appeared on arXiv.).…”

Section: Introductionmentioning

confidence: 99%

The LISA-Taiji Network: Precision Localization of Coalescing Massive Black Hole Binaries

et al. 2021

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We explore a potential LISA-Taiji network to fast and accurately localize the coalescing massive black hole binaries. For an equal-mass binary located at redshift of 1 with a total intrinsic mass of 105M⊙, the LISA-Taiji network may achieve almost four orders of magnitude improvement on the source localization region compared to an individual detector. The precision measurement of sky location from the gravitational-wave signal may completely identify the host galaxy with low redshifts prior to the final black hole merger. Such identification of the host galaxy is vital for the follow-up variability in electromagnetic emissions of the circumbinary disc when the binary merges to a new black hole and enables the coalescing massive black hole binaries to be used as a standard siren to probe the expansion history of the Universe.

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Numerical simulation of sky localization for LISA-TAIJI joint observation

Cited by 42 publications

References 64 publications

How many extra-Galactic stellar-mass binary black holes will be detected by space gravitational-wave interferometers?

How many extra-Galactic stellar-mass binary black holes will be detected by space gravitational-wave interferometers?

Alternative LISA-TAIJI networks

The LISA-Taiji Network: Precision Localization of Coalescing Massive Black Hole Binaries

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