http://arxiv.org/abs/1901.02159
We use Fisher information matrix method to calculate the parameter estimation accuracy of inspiralling supermassive black holes binaries for TianQin, a space-borne laser interferometric detector aimed at detecting gravitational waves in millihertz frequency band. The `restricted’ post-Newtonian waveform in which third order post-Newtonian (3PN) phase including spin effects (spin-orbit $\beta$ and spin-spin $\sigma$) and first-order eccentricity contribution is employed. Monte Carlo simulations using $10^3$ binaries for each mass pairs with component masses in the range of $({10^5},{10^7}){M_ \odot }$ and cosmological redshift $z=0.5$ show that the medians of the root-mean-square error distributions for the chirp mass $M_c$ and symmetric mass ratio $\eta$ are in the range of $\sim 0.02\% – 0.7\% $ and $\sim 4\% – 8\% $, respectively. The luminosity distance $D_L$ can be determined to be $\sim 1\% – 3\% $ and the angular resolution of source $\Delta \Omega $ is better than 12 deg$^2$. The corresponding results for $z=1.0$ and $2.0$, which are deteriorated with the decreasing of the signal-to-noise ratio, have also been given. We show that adding spin parameters degrades measurement accuracy of the mass parameters (${M_c}$, $\eta$), and the time and the orbital phase of coalescence ($t_c$, $\phi _c$); the inclusion of first-order eccentricity correction to the phase worsens the estimation accuracy comparing with the circular cases. We also show the effects of post-Newtonian order on parameter estimation accuracy by comparing the results based on second order and third order post-Newtonian phase. Moreover, we calculate the horizon distance of supermassive black hole binaries for TianQin.
W. Feng, H. Wang, X. Hu, et. al.
Wed, 9 Jan 19
9/46
Comments: 15 pages, 5 figures, 4 tables