A methodology for the uniform processing of observations in the 3.6 μm band of the Spitzer/IRAC telescope was constructed. The objective was to identify distinctive inhomogeneities in the infrared brightness profile of exoplanets, which manifest as systematic deviations in the moments of secondary eclipses. The model parameters were selected using the maximum likelihood method within the Gaussian process model. To date, the observations of four exoplanets have been processed, resulting in the determination of the depths of secondary eclipses and the shift of the eclipse centres relative to the circular orbit model.