The paper quantifies the bimodal color-magnitude distribution of galaxies from the Sloan Digital Sky Survey (SDSS). It analyzes the color-magnitude (CM) relations for red and blue galaxies, which are associated with early-type (red) and late-type (blue) galaxies, respectively. The study uses a sample of galaxies with redshifts between 0.004 and 0.08 and absolute magnitudes between -23.5 and -15.5. The bimodality of the distribution is traced by fitting double-Gaussian functions to the color functions in absolute magnitude bins. The CM relations are well fit by a straight line plus a tanh function, with shallow slopes of about -0.04 and -0.05 for the red and blue distributions, respectively. The midpoints of the transitions occur at $ M_r = -19.8 $ and -20.8 for the red and blue distributions, respectively. The red distribution has a more luminous characteristic magnitude and a shallower faint-end slope compared to the blue distribution. These are converted to galaxy stellar mass functions. The red distribution galaxies have a higher number density per magnitude for masses greater than about $ 3 \times 10^{10} M_\odot $. A simple merger model is used to show that the differences between the two functions are consistent with the red distribution being formed from major galaxy mergers. The study also finds that the CM relations for the red and blue distributions are well fit by a straight line plus a tanh function, with the red distribution having a shallower slope and the blue distribution having a steeper slope. The luminosity functions for the red and blue distributions are obtained, with the red distribution having a more luminous characteristic magnitude and a shallower faint-end slope. The results are converted to stellar mass functions, showing that the red distribution is shifted to higher masses compared to the blue distribution. The study also finds that the bimodal distribution can be explained by different processes leading to two dominant populations of galaxies with different average colors and/or color dispersions. The results are consistent with the red distribution being formed from major galaxy mergers. The study also finds that the CM relations for the red and blue distributions are similar between different environments, and that the transition in the CM relations is due to an increasing contribution from recent star formation with decreasing galaxy luminosity. The study also finds that the dispersion-magnitude relation for the red distribution goes through a transition at the same magnitude as the CM relation, consistent with the transition being due to an increasing contribution from recent star formation with decreasing galaxy luminosity. The study also finds that the dispersion-magnitude relation for the blue distribution is influenced by an increase in dust content and a decrease in recent star formation relative to the total stellar mass of the galaxy. The results are consistent with the red distribution being formed from major galaxy mergers. The study also finds thatThe paper quantifies the bimodal color-magnitude distribution of galaxies from the Sloan Digital Sky Survey (SDSS). It analyzes the color-magnitude (CM) relations for red and blue galaxies, which are associated with early-type (red) and late-type (blue) galaxies, respectively. The study uses a sample of galaxies with redshifts between 0.004 and 0.08 and absolute magnitudes between -23.5 and -15.5. The bimodality of the distribution is traced by fitting double-Gaussian functions to the color functions in absolute magnitude bins. The CM relations are well fit by a straight line plus a tanh function, with shallow slopes of about -0.04 and -0.05 for the red and blue distributions, respectively. The midpoints of the transitions occur at $ M_r = -19.8 $ and -20.8 for the red and blue distributions, respectively. The red distribution has a more luminous characteristic magnitude and a shallower faint-end slope compared to the blue distribution. These are converted to galaxy stellar mass functions. The red distribution galaxies have a higher number density per magnitude for masses greater than about $ 3 \times 10^{10} M_\odot $. A simple merger model is used to show that the differences between the two functions are consistent with the red distribution being formed from major galaxy mergers. The study also finds that the CM relations for the red and blue distributions are well fit by a straight line plus a tanh function, with the red distribution having a shallower slope and the blue distribution having a steeper slope. The luminosity functions for the red and blue distributions are obtained, with the red distribution having a more luminous characteristic magnitude and a shallower faint-end slope. The results are converted to stellar mass functions, showing that the red distribution is shifted to higher masses compared to the blue distribution. The study also finds that the bimodal distribution can be explained by different processes leading to two dominant populations of galaxies with different average colors and/or color dispersions. The results are consistent with the red distribution being formed from major galaxy mergers. The study also finds that the CM relations for the red and blue distributions are similar between different environments, and that the transition in the CM relations is due to an increasing contribution from recent star formation with decreasing galaxy luminosity. The study also finds that the dispersion-magnitude relation for the red distribution goes through a transition at the same magnitude as the CM relation, consistent with the transition being due to an increasing contribution from recent star formation with decreasing galaxy luminosity. The study also finds that the dispersion-magnitude relation for the blue distribution is influenced by an increase in dust content and a decrease in recent star formation relative to the total stellar mass of the galaxy. The results are consistent with the red distribution being formed from major galaxy mergers. The study also finds that