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We use the Fisher information matrix method to calculate the parameterestimation accuracy of inspiraling supermassive black holes binaries forTianQin, a space-borne laser interferometric detector aimed at detectinggravitational waves in the millihertz frequency band. The `restricted'post-Newtonian waveform in which third order post-Newtonian (3PN) phaseincluding spin effects (spin-orbit $\beta$ and spin-spin $\sigma$) andfirst-order eccentricity contribution is employed. Monte Carlo simulationsusing $10^3$ binaries for mass pairs with component masses in the range of$({10^5},{10^7}){M_ \odot }$ and cosmological redshift $z=0.5$ show that themedians 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 bedetermined 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 thesignal-to-noise ratio, have also been given. We show that adding spinparameters 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 the first-order eccentricity correction to the phase worsensthe estimation accuracy comparing with the circular cases. We also show theeffects of post-Newtonian order on parameter estimation accuracy by comparingthe results based on second order and third order post-Newtonian phases.Moreover, we calculate the horizon distance of supermassive black hole binariesfor TianQin.

Preliminary study on parameter estimation accuracy of supermassive black hole binary inspirals for TianQin