The early phase of coalescence of supermassive black hole binaries (SMBHBs) from their host galaxies provides a guaranteed source of low-frequency gravitational wave (GW) radiation by pulsar timing observations. Nowadays, SMBHBs 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. A binary population synthesis (BPS) approach has been applied to study the characteristics of clusters and galaxies. Here we report how BPS, using SDSS results, can be used to determine the GW radiation from SMBHBs. In this study we show numerical results under the assumption that SMBHBs 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.