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A design study is currently in progress for a third generationgravitational-wave (GW) detector called Einstein Telescope (ET). An importantkind of source for ET will be the inspiral and merger of binary neutron stars(BNS) up to $z \sim 2$. If BNS mergers are the progenitors of short-hard$\gamma$-ray bursts, then some fraction of them will be seen bothelectromagnetically and through GW, so that the luminosity distance and theredshift of the source can be determined separately. An important property ofthese `standard sirens' is that they are \emph{self-calibrating}: theluminosity distance can be inferred directly from the GW signal, with no needfor a cosmic distance ladder. Thus, standard sirens will provide a powerfulindependent check of the $\Lambda$CDM model. In previous work, estimates weremade of how well ET would be able to measure a subset of the cosmologicalparameters (such as the dark energy parameter $w_0$) it will have access to,assuming that the others had been determined to great accuracy by alternativemeans. Here we perform a more careful analysis by explicitly using thepotential Planck CMB data as prior information for these other parameters. Wefind that ET will be able to constrain $w_0$ and $w_a$ with accuracies $\Deltaw_0 = 0.099$ and $\Delta w_a = 0.302$, respectively. These results are comparedwith projected accuracies for the JDEM Baryon Acoustic Oscillations project andthe SNAP Type Ia supernovae observations.

Determination of Dark Energy by the Einstein Telescope: Comparing with CMB, BAO and SNIa Observations