Sky location of massive black hole binaries in the foreground of Galactic white dwarf binaries

For space-based gravitational wave (GW) detection, the main noise source for massive black hole binaries (MBHBs) is attributed to approximately 107 double white dwarf binaries in the foreground. For a GW source, the amplitude of the detector response, recorded by a space-based gravitational wave detector, exhibits a modulation effect with a year period when observing the source from various orbital positions. Under the adverse conditions mentioned above, where there is a strong foreground noise and annual modulation in the signals, we employed the wavelet transform and the strong-amplitude relevant orbital position search methods, which allows the weak MBHB sources to achieve higher locating accuracy. In detail, for two MBHB sources of lower intensity, the precision of luminosity distance, represented by the ratio Delta DL/DL at the 95% confidence level, is enhanced by factors of similar to 2. The angular resolutions, denoted by Delta Omega s, are enhanced by a factor of similar to 20. These improvements increase the number of detectable GW sources, facilitate multi-messenger follow-up observations and provide constraints on the cosmological constant.