Sensitivity curves for spaceborne gravitational wave interferometers

Larson, Shane L.; Hiscock, William A.; Hellings, Ronald W.

doi:10.1103/physrevd.62.062001

Cited by 212 publications

(303 citation statements)

References 11 publications

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“…[50] and the LISA Pre-Phase A Report], computed by a combination of three factors, including: (i) the raw spectral noise density S n , (ii) the gravitational-wave transfer (response) function R and (iii) the noise transfer (response) function R n . They combine together in [51] …”

Section: Appendix C: Lisa Noise Curvementioning

confidence: 99%

Gravitational-wave spectroscopy of massive black holes with the space interferometer LISA

Berti¹,

Cardoso²,

Will³

2006

Phys. Rev. D

739

1,048

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Newly formed black holes are expected to emit characteristic radiation in the form of quasi-normal modes, called ringdown waves, with discrete frequencies. LISA should be able to detect the ringdown waves emitted by oscillating supermassive black holes throughout the observable Universe. We develop a multi-mode formalism, applicable to any interferometric detectors, for detecting ringdown signals, for estimating black hole parameters from those signals, and for testing the no-hair theorem of general relativity. Focusing on LISA, we use current models of its sensitivity to compute the expected signal-to-noise ratio for ringdown events, the relative parameter estimation accuracy, and the resolvability of different modes. We also discuss the extent to which uncertainties on physical parameters, such as the black hole spin and the energy emitted in each mode, will affect our ability to do black hole spectroscopy.

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Section: Appendix C: Lisa Noise Curvementioning

confidence: 99%

Gravitational-wave spectroscopy of massive black holes with the space interferometer LISA

Berti¹,

Cardoso²,

Will³

2006

Phys. Rev. D

739

1,048

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“…where S n is the total strain noise spectral density, h f is the root spectral density and R is the GW transfer function given by Larson et al (2000). For a continuous monochromatic source, such as a DWD with a circular orbit, which is observed over a time T , the root spectral density will appear in a Fourier spectrum as a single spectral line in the form )…”

Section: The Total Gw Amplitude Spectrum From Dwds and Comparison Witmentioning

confidence: 99%

The gravitational wave signal from diverse populations of double white dwarf binaries in the Galaxy

Jeffery

2010

A&A

130

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Context. The gravitational wave (GW) background in the range 0.01−30 mHz has been assumed to be dominated by unresolved radiation from double white dwarf binaries (DWDs). Recent investigations indicate that, at short periods, a number of DWDs should be resolvable sources of GW. Aims. We characterize the GW signal which would be detected by LISA from DWDs in the Galaxy. Methods. We have constructed a Galactic model in which we consider distinct contributions from the bulge, thin disc, thick disc, and halo, and subsequently executed a population synthesis approach to determine the birth rates, numbers, and period distributions of DWDs within each component. Results. In the Galaxy as a whole, our model predicts the current birth rate of DWDs to be 3.21 × 10 −2 yr −1 , the local density to be 2.2 × 10 −4 pc −3 and the total number to be 2.76 × 10 8 . Assuming SNIa are formed from the merger of two CO white dwarfs, the SNIa rate should be 0.0013 yr −1 . The frequency spectra of DWD strain amplitude and number distribution are presented as a function of galactic component, DWD type, formation channel, and metallicity. Conclusions. We confirm that CO+He and He+He white dwarf (WD) pairs should dominate the GW signal at very high frequencies (log f Hz −1 > −2.3), while CO+CO and ONeMg WD pairs have a dominant contribution at log f Hz −1 ≤ −2.3. Formation channels involving two common-envelope (CE) phases or a stable Roche lobe overflow phase followed by a CE phase dominate the production of DWDs detectable by LISA at log f Hz −1 > −4.5. DWDs with the shortest orbital periods will come from the CE+CE channel. The Exposed Core plus CE channel is a minor channel. A number of resolved DWDs would be detected, making up 0.012% of the total number of DWDs in the Galaxy. The majority of these would be CO+He and He+He pairs formed through the CE+CE channel.

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“…Utmost care is needed Sensitivity of a few representative mission options whose sensitivity curves are labeled by their corresponding total position noise budget levels. Also shown is the standard single Michelson sensitivity of LISA for comparison [20]. The optimistic confusion noise level generated by both galactic and extra-galactic cosmological compact binaries (mainly WD-WD) given in [17] is adopted in drawing the solid lines, and the dash-dotted curve stands for the pure instrumental noise for the most ambitious design.…”

Section: Mission Designmentioning

confidence: 99%