Special Astrophysical Observatory of the Russian Academy of Sciences
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03.06.01
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03.04.03
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In this work we process infrared light curves for 13 secondary eclipses of the exoplanet HD 209458 b, obtained with the Spitzer Space Telescope. The objective of the study was to identify any discrepancies that might be attributed to the inhomogeneity of the planet's surface brightness or a difference of the planet's shape from a sphere. Firstly, an attempt was made to ascertain whether the observed midpoint of the secondary eclipse exhibited a shift from the ephemeris moment. This could indicate the presence of a hot spot on the planet's surface that is shifted from the central meridian. The analysis allowed for the correlated noise that remained in the IRAC detector data after aperture photometry by approximating the noise with a Gaussian random process. As a result, we detected two components of red noise with different time scales: $\sim\!10$ s and $\sim\!5$ min. In addition, we constructed a unified model of the effect of inhomogeneous pixel sensitivity as a periodic function of the brightness centroid coordinates, which works well for all the analyzed eclipses. According to the results, the main parameters of the HD 209458 b eclipse coincided with those obtained by other authors: a depth of $0.125 \pm 0.004$% and a shift of the observed midpoint of $-0.53 \pm 0.61$ min.
planets and satellites: surfaces, general; stars: planetary systems; techniques: photometric; methods: data analysis; stars: individual: HD 209458
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