Frequency response of space-based interferometric gravitational-wave detectors

Liang, Dicong; Gong, Yungui; Weinstein, A. J.; Zhang, Chao

doi:10.1103/physrevd.99.104027

Cited by 40 publications

(42 citation statements)

References 68 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…µ 1 = cos θ 1 /v gw , µ 2 = cos θ 2 /v gw , cos θ 2 = cos σ cos θ 1 + sin σ sin θ 1 cos . In the massless or high frequency limit, v gw = c and we recover those results in [55]. In the low frequency and massless limits, m g ω 2πf * , we get R + = R × = R x = R y = sin 2 σ/5 and R b = R l = sin 2 σ/15.…”

Section: Discussionsupporting

confidence: 83%

“…In the high frequency limit, we find that R P ∝ 1/ω 2 for the tensor and breathing modes, R P ∝ 1/ω for the longitudinal mode and R P ∝ ln(ω)/ω 2 for the vector mode, which are the same as those for the equal (B11) and (B12), it is easy to see that in the low frequency limit, R A E ∝ ω 2 . In the high frequency limit, we find that R E ∝ 1/ω 2 for the tensor and breathing modes, R E ∝ 1/ω for the longitudinal mode and R E ∝ ln(ω)/ω 2 for the vector mode, which are the same as those for the equal arm interferometric GW detector without optical cavities derived in [55].…”

Section: Analytical Formulas Of Averaged Response Functionssupporting

confidence: 74%

“…In this section, we derive analytical formulas for the averaged response functions and analyze their asymptotic behaviors. We work in the source coordinate system and follow the notation used in [54,55]. In particular, µ 1 = cos θ 1 = (µ 2 cos σ + sin θ 2 sin σ cos )L 3 /L 1 − µ 2 L 2 /L 1 , µ 3 = cos θ 3 = µ 2 cos σ + sin θ 2 sin σ cos , µ 2 = cos θ 2 , κ 1 = sin θ 2 cos σ − µ 2 sin σ cos , κ 2 = (sin θ 2 cos σ − µ 2 sin σ cos )L 3 /L 1 − sin θ 2 L 2 /L 1 , is the angle between the plane containingn 2 andΩ and the plane of the interferometer, σ is the opening angle between two arms and cos σ = (L 2 2 + L 2 3 − L 2 1 )/(2L 2 L 3 ).…”

Section: Analytical Formulas Of Averaged Response Functionsmentioning

confidence: 99%

See 2 more Smart Citations

Frequency response of time-delay interferometry for space-based gravitational wave antenna

et al. 2019

Self Cite

View full text Add to dashboard Cite

Space-based gravitational wave detectors cannot keep rigid structures and precise arm length equality, so the precise equality of detector arms which is required in a ground-based interferometer to cancel the overwhelming laser noise is impossible. The time-delay interferometry method is applied to unequal arm lengths to cancel the laser frequency noise. We give analytical formulas of the averaged response functions for tensor, vector, breathing and longitudinal polarizations in different TDI combinations, and obtain their asymptotic behaviors. At low frequencies, f f * , the averaged response functions of all TDI combinations increase as f 2 for all six polarizations. The one exception is the averaged response functions of ζ for all six polarizations increase as f 4 in the equilateral-triangle case. At high frequencies, f f * , the averaged response functions of all TDI combinations for the tensor and breathing modes fall off as 1/f 2 , the averaged response functions of all TDI combinations for the vector mode fall off as ln(f )/f 2 , and the averaged response functions of all TDI combinations for the longitudinal mode fall as 1/f . We also give LISA and TianQin sensitivity curves in different TDI combinations for tensor, vector, breathing and longitudinal polarizations.

show abstract

Section: Discussionsupporting

confidence: 83%

Section: Analytical Formulas Of Averaged Response Functionssupporting

confidence: 74%

Section: Analytical Formulas Of Averaged Response Functionsmentioning

confidence: 99%

See 1 more Smart Citation

Frequency response of time-delay interferometry for space-based gravitational wave antenna

et al. 2019

Self Cite

View full text Add to dashboard Cite

show abstract

“…The response functions of LISA-like detectors can be found in the references (Cornish & Rubbo 2003;Rubbo et al 2004;Cornish & Larson 2001;Liang et al 2019). In this Appendix, we will give the expressions of antenna pattern function in a specific coordinate system.…”

Section: Resultsmentioning

confidence: 99%

Constraining Screened Modified Gravity with Spaceborne Gravitational-wave Detectors

Niu¹,

Zhang²,

Liu³

et al. 2020

ApJ

View full text Add to dashboard Cite

The screened modified gravity (SMG) is a unified theoretical framework, which describes the scalar-tensor gravity with screening mechanism. Based on the gravitationalwave (GW) waveform produced by the compact binary coalescence in the general SMG, derived in our previous work (Liu et al. 2018b), in this article we investigate the potential constraints on SMG theory through the observation of extreme-mass-ratio inspirals (EMRIs) by the future space-borne GW detectors, including LISA, TianQin and Taiji.We find that, for the EMRIs consisting of a massive black hole and a neutron star, if the EMRIs are at Virgo cluster, the GW signals can be detected by the detectors at quite high significant level, and the screened parameter NS can be constrained at about O(10 −5 ), which is more than one order of magnitude tighter than the potential constraint given by ground-based Einstein telescope. However, for the EMRIs consisting of a massive black hole and a white dwarf, the signal-to-noise ratios of the GW signals are less than 10, if the location of the source and the mass of black hole are same with the previous case. For the specific SMG models, including chameleon, symmetron and dilaton, we find these constraints are complementary with that from Cassini experiment, but weaker than those from lunar laser ranging observations and binary pulsars, due to the strong gravitational potentials on the surface of neutron stars. By analyzing the deviation of GW waveform in SMG from that in general relativity, as anticipated, we find the dominant contribution of the SMG constraining comes from the correction terms in the GW phases, rather than the extra polarization modes or the correction terms in the GW amplitudes.

show abstract

“…The induced GWs can be tested by space based GW observatory like Laser Interferometer Space Antenna (LISA) [42,43], TianQin [44] and TaiJi [45], and the Pulsar Timing Array (PTA) [46][47][48][49] including the Square Kilometer Array (SKA) [50] in the future. For simple test, we compare the strength of induced GWs with the sensitivity curves of those detectors [51][52][53]. On the other hand, the observations of induced GWs can also be used to constrain the power spectrum.…”

Section: Introductionmentioning

confidence: 99%

Constraints on primordial curvature perturbations from primordial black hole dark matter and secondary gravitational waves

Gong

Zhu

et al. 2019

J. Cosmol. Astropart. Phys.

Self Cite

View full text Add to dashboard Cite

Primordial black holes and secondary gravitational waves can be used to probe the small scale physics at very early time. For secondary gravitational waves produced after the horizon reentry, we derive an analytical formula for the time integral of the source and analytical behavior of the time dependence of the energy density of induced gravitational waves is obtained. By proposing a piecewise power law parametrization for the power spectrum of primordial curvature perturbations, we use the observational constraints on primordial black hole dark matter to obtain an upper bound on the power spectrum, and discuss the test of the model with future space based gravitational wave antenna.

show abstract

Frequency response of space-based interferometric gravitational-wave detectors

Cited by 40 publications

References 68 publications

Frequency response of time-delay interferometry for space-based gravitational wave antenna

Frequency response of time-delay interferometry for space-based gravitational wave antenna

Constraining Screened Modified Gravity with Spaceborne Gravitational-wave Detectors

Constraints on primordial curvature perturbations from primordial black hole dark matter and secondary gravitational waves

Contact Info

Product

Resources

About