The stellar content of galaxies has been investigated by means of narrow-band photoelectric photometry performed in twelve colors. The photometry consists of seven continuum colors from X 3400 to 7300 and five line indices, including Na D, Mg b, TiO, and Ha. Observations in this photometric system were made of twenty galaxies of various morphological types and ninety-three stars of all luminosity classes, ranging in spectral type from B7 to M6. Synthesis of the observed galaxies from the observed field stars was performed according to the following criteria: (1) match the seven colors, (2) match the five line indices, (3) use a reasonable color-magnitude array, (4) use a reasonable Hess diagram distribution, (5) account for Morgan's nuclear type, (6) account for the large observed values of mass-to-light ratio. The synthesis was very successful for the E and SO galaxies, and a good correlation was exhibited between M and the com uted M/L: the more luminous galaxies contain relatively more dwarf stars. The computed stellar M L values, however, are approximately three times smaller than the dynamic M/L values. Consideration of white dwarf stars, very late M dwarf stars, and interstellar matter does not offer a satisfactory solution for this discrepancy. The model used for the k-nuclei systems was patterned after the old galactic cluster M67, with the addition of more late dwarfs, more late giants, and a stronger horizontal branch. For synthesis of spiral arms or nuclei of earlier-type galaxies, the model used was more like a young galactic cluster. Indications are that all galaxies synthesized have an integrated metal-to-hydrogen ratio which is essentially the same as that for our own Galaxy.