The early phase of coalescence of massive black hole binaries(MBHBs)from their host galaxies provides a guaranteed source of low-frequency gravitational wave(GW)radiation by pulsar timing observations.Nowadays,MBHBs are ubiquitous in the nuclei of galaxies.A latest sample of close galaxy pairs has been released from the Sloan Digital Sky Survey(SDSS)Data,such as the star formation rate,the merger rate of massive galaxies,the demographics of MBHBs at low redshif and the dynamics of MBHBs.A binary population synthesis(BPS)approach has been applied to study the characteristics of clusters and galaxies4.And this method also has been systematically taken up by some groups to investigate the GW radiation from compact binaries in the Galaxy.However,the studies of GW radiation from MBHBs,combined with the BPS and observations,are not well known.Here we report how BPS,using SDSS results,can be used to determine the GW radiation from MBHBs.In this study we show numerical results under the assumption that MBHBs formed through the merger of two galaxies and give the waveform evolution using post-Newtonian approximation methods.Based on the sensitivity of the International Pulsar Timing Array(IPTA)and Square Kilometer Array(SKA)detectors,we show that the value of strain amplitude h can be changed from about 10-14 to 10-15 during the observation of 20 years,which can be considered as a precise evolution.We also find that our estimate for the number of MBHB sources that can be detected by IPTA detector is greater than 100.This number of binary sources depends on a convolution over redshift of merger rate of galaxies with the fraction of galaxies that harbor massive BHs.This study provides new detailed specifics and characteristics of the recently published result(A&A,Liu et al.2012).