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KO Aql is classified as an Algol-type eclipsing system. It is a semi-detached system consisting of a main-sequence star and a giant which fills its Roche lobe. Photometric observations of KO Aql were conducted using the 0.4 meter telescope at Mount Laguna Observatory during the months of June through September, 1993. Sixteen nights of observation resulted in 110 measurements in the u, v, b, y, and o filters, and 104 measurements in the i filter. Due to the mass transfer in this system, the period is known to be slowly increasing. Therefore, a new ephemeris was calculated for the system. An analysis of the data was done using the Wilson-Devinney program. The spectral type of the primary star was known from previous work, so the temperature of the primary star was estimated through its spectral type. The temperature of the secondary star was not known, so it, along with the phase shift, inclination, potential of the primary star, and the luminosity of the primary star, were allowed to be adjusted by the program. The best fit was calculated by the program for seven different mass ratios. The minima in the errors from each solution resulted in the best mass ratio for the system. All of this was done by setting the parameter F1 to 1, that is, the primary star is in synchronous rotation. To determine if this was the actual case, the program was run again setting the parameter F1 to 2, 3, and 4 to see if there was any change in the solution. There was no significant change in the results, so the initial solution was accurate.
