Cosmology with space-based gravitational-wave detectors --- dark energy
  and primordial gravitational waves ---

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Abstract

Proposed space-based gravitational-wave (GW) detectors such as DECIGO and BBO will detect ~10^6 neutron-star (NS) binaries and determine the luminosity distances to the binaries with high precision. Combining the luminosity distances with cosmologically-induced phase corrections on the GWs, cosmological expansion out to high redshift can be measured without the redshift determinations of host galaxies by electromagnetic observation and be a unique probe for dark energy. On the other hand, such a NS-binary foreground should be subtracted to detect primordial GWs produced during inflation. Thus, the constraining power on dark energy and the detectability of the primordial gravitational waves strongly depend on the detector sensitivity and are in close relation with one another. In this paper, we investigate the constraints on the equation of state of dark energy with future space-based GW detectors with/without identifying the redshifts of host galaxies. We also study the sensitivity to the primordial GWs, properly dealing with the residual of the NS binary foreground. Based on the results, we discuss the detector sensitivity required to achieve the forementioned targeted study of cosmology.

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Accelerating Universes with Scaling Dark Matter

M. Chevallier, D. Polarski (2000)

Friedmann-Robertson-Walker universes with a presently large fraction of the energy density stored in an \(X\)-component with \(w_X<-1/3\), are considered. We find all the critical points of the system for constant equations of state in that range. We consider further several background quantities that can distinguish the models with different \(w_X\) values. Using a simple toy model with a varying equation of state, we show that even a large variation of \(w_X\) at small redshifts is very difficult to observe with \(d_L(z)\) measurements up to \(z\sim 1\). Therefore, it will require accurate measurements in the range \(1

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Gravitational Waves from Mergin Compact Binaries: How Accurately Can One Extract the Binary's Parameters from the Inspiral Waveform?

Curt Cutler, Eanna Flanagan (1994)

The most promising source of gravitational waves for the planned detectors LIGO and VIRGO are merging compact binaries, i.e., neutron star/neutron star (NS/NS), neutron star/black hole (NS/BH), and black hole/black-hole (BH/BH) binaries. We investigate how accurately the distance to the source and the masses and spins of the two bodies will be measured from the gravitational wave signals by the three detector LIGO/VIRGO network using ``advanced detectors'' (those present a few years after initial operation). The combination \({\cal M} \equiv (M_1 M_2)^{3/5}(M_1 +M_2)^{-1/5}\) of the masses of the two bodies is measurable with an accuracy \(\approx 0.1\%-1\%\). The reduced mass is measurable to \(\sim 10\%-15\%\) for NS/NS and NS/BH binaries, and \(\sim 50\%\) for BH/BH binaries (assuming \(10M_\odot\) BH's). Measurements of the masses and spins are strongly correlated; there is a combination of \(\mu\) and the spin angular momenta that is measured to within \(\sim 1\%\). We also estimate that distance measurement accuracies will be \(\le 15\%\) for \(\sim 8\%\) of the detected signals, and \(\le 30\%\) for \(\sim 60\%\) of the signals, for the LIGO/VIRGO 3-detector network.