An Overview of the Laser Interferometer Space Antenna

Shaddock, D. A.

doi:10.1071/as08059

Cited by 9 publications

(8 citation statements)

References 19 publications

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“…Further work is needed to develop an easy-toimplement and robust method to estimate these requirements for configurations that have not yet been simulated in NR codes; work in this area is already underway [56]. It would be useful to make estimates of waveform length requirements for the construction of analytic models, both phenomenological and EOB; to extend this study to possible future detectors, like LISA [57] and the Einstein Telescope [58]; and, finally, much more work is required to understand the length requirements for parameter estimation, and to balance the needs of GW astronomy with the computational cost of numerical simulations.…”

Section: Discussionmentioning

confidence: 99%

Length requirements for numerical-relativity waveforms

et al. 2010

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One way to produce complete inspiral-merger-ringdown gravitational waveforms from black-hole-binary systems is to connect post-Newtonian (PN) and numerical-relativity (NR) results to create ``hybrid'' waveforms. Hybrid waveforms are central to the construction of some phenomenological models for GW search templates, and for tests of GW search pipelines. The dominant error source in hybrid waveforms arises from the PN contribution, and can be reduced by increasing the number of NR GW cycles that are included in the hybrid. Hybrid waveforms are considered sufficiently accurate for GW detection if their mismatch error is below 3% (i.e., a fitting factor about 0.97). We address the question of the length requirements of NR waveforms such that the final hybrid waveforms meet this requirement, considering nonspinning binaries with q = M_2/M_1 \in [1,4] and equal-mass binaries with \chi = S_i/M_i^2 \in [-0.5,0.5]. We conclude that for the cases we study simulations must contain between three (in the equal-mass nonspinning case) and ten (the \chi = 0.5 case) orbits before merger, but there is also evidence that these are the regions of parameter space for which the least number of cycles will be needed

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Section: Discussionmentioning

confidence: 99%

Length requirements for numerical-relativity waveforms

et al. 2010

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“…At the same time, pulsars act as natural gravitational wave detectors [25], strongly constraining the amplitude of the GW with the narrow range of frequencies, f ∼ 10 −9 − 10 −8 Hz, to 10 6 Ω gw h 2 < 10 −2 [26]. Large scale interferometers for gravitational wave detection (e.g., LIGO [27], LISA [28], VIRGO [29]) are also looking for gravitational wave signals. A recent bound of 10 6 Ω gw h 2 < 6.9 has been obtained at 10 2 Hz from the Laser Interferometer Gravitational Wave Observatory (LIGO) [30].…”

Section: Introductionmentioning

confidence: 99%

Improved limits on short-wavelength gravitational waves from the cosmic microwave background

Sendra

Smith

2012

Phys. Rev. D

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The cosmic microwave background (CMB) is affected by the total radiation density around the time of decoupling. At that epoch, neutrinos comprised a significant fraction of the radiative energy, but there could also be a contribution from primordial gravitational waves with frequencies greater than ∼ 10 −15 Hz. If this cosmological gravitational wave background (CGWB) were produced under adiabatic initial conditions, its effects on the CMB and matter power spectrum would mimic massless non-interacting neutrinos. However, with homogenous initial conditions, as one might expect from certain models of inflation, pre big-bang models, phase transitions and other scenarios, the effect on the CMB would be distinct. We present updated observational bounds for both initial conditions using the latest CMB data at small scales from the South Pole Telescope (SPT) in combination with Wilkinson Microwave Anisotropy Probe (WMAP), current measurements of the baryon acoustic oscillations, and the Hubble parameter. With the inclusion of the data from SPT the adiabatic bound on the CGWB density is improved by a factor of 1.7 to 10 6 Ωgwh 2 8.7 at the 95% confidence level (C. L.), with weak evidence in favor of an additional radiation component consistent with previous analyses. The constraint can be converted into an upper limit on the tension of horizon-sized cosmic strings that could generate this gravitational wave component, with Gµ 2 × 10 −7 at 95% C. L., for string tension Gµ. The homogeneous bound improves by a factor of 3.5 to 10 6 Ωgwh 2 1.0 at 95% C. L., with no evidence for such a component from current data.

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“…The slope of the above-mentioned µ 2 -variance relationship is equal to the combinationξh/ω of the GW, where the factor ξ is included to take account of ξ for different pulsars. We inject different GW strain into the timing residuals and perform linear fit to the resulting µ 2 -variance pairs, and we plot the fitted slope, i.e., the estimated (ξh/ω) 2 as a function of the injected value of (ξ 0 h/ω) 2 , in Figure 4, where ξ 0 is the parameter ξ when γ is fixed to 2φ in Equation (4). The error bars show the 3σ error of the slope given by the fitting process.…”

Section: Testing the Methods With Simulated Datamentioning

confidence: 99%

“…Introduction The recent direct detection of gravitational waves (GWs) [1] marks the beginning of GW astronomy era, after about five decades of effort on GW detection [2][3][4][5][6][7][8][9]. Among the various proposed methods, the pulsar timing array (PTA) method shows promise in identifying GWimprinted structure in the timing residuals of a number of pulsars [10,11].…”

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confidence: 99%

Detecting super-Nyquist-frequency gravitational waves using a pulsar timing array

Zhang

2016

Sci. China Phys. Mech. Astron.

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The maximum frequency of gravitational waves (GWs) detectable with traditional pulsar timing methods is set by the Nyquist frequency ( f Ny ) of the observation. Beyond this frequency, GWs leave no temporal-correlated signals; instead, they appear as white noise in the timing residuals. The variance of the GW-induced white noise is a function of the position of the pulsars relative to the GW source. By observing this unique functional form in the timing data, we propose that we can detect GWs of frequency > f Ny (super-Nyquist frequency GWs; SNFGWs). We demonstrate the feasibility of the proposed method with simulated timing data. Using a selected dataset from the Parkes Pulsar Timing Array data release 1 and the North American Nanohertz Observatory for Gravitational Waves publicly available datasets, we try to detect the signals from single SNFGW sources. The result is consistent with no GW detection with 65.5% probability. An all-sky map of the sensitivity of the selected pulsar timing array to single SNFGW sources is generated, and the position of the GW source where the selected pulsar timing array is most sensitive to is λ s = −0.82, β s = −1.03 (rad); the corresponding minimum GW strain is h = 6.31 × 10 −11 at f = 1 × 10 −5 Hz. gravitational wave, pulsar, black hole PACS number(s): 25.60. Je, 21.10.Jx, 25.40.Lw, 26.20.+f

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An Overview of the Laser Interferometer Space Antenna

Abstract: Abstract:The 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.

Cited by 9 publications

References 19 publications

Length requirements for numerical-relativity waveforms

Length requirements for numerical-relativity waveforms

Improved limits on short-wavelength gravitational waves from the cosmic microwave background

Detecting super-Nyquist-frequency gravitational waves using a pulsar timing array

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