Special Astrophysical Observatory of the Russian Academy of Sciences
UDK 53 Физика
UDK 520 Инструменты, приборы и методы астрономических наблюдений, измерений и анализа
UDK 521 Теоретическая астрономия. Небесная механика. Фундаментальная астрономия. Теория динамической и позиционной астрономии
UDK 523 Солнечная система
UDK 524 Звезды и звездные системы. Вселенная Солнце и Солнечная система
UDK 52-1 Метод изучения
UDK 52-6 Излучение и связанные с ним процессы
GRNTI 41.00 АСТРОНОМИЯ
GRNTI 29.35 Радиофизика. Физические основы электроники
GRNTI 29.31 Оптика
GRNTI 29.33 Лазерная физика
GRNTI 29.27 Физика плазмы
GRNTI 29.05 Физика элементарных частиц. Теория полей. Физика высоких энергий
OKSO 03.06.01 Физика и астрономия
OKSO 03.05.01 Астрономия
OKSO 03.04.03 Радиофизика
BBK 2 ЕСТЕСТВЕННЫЕ НАУКИ
BBK 223 Физика
TBK 614 Астрономия
TBK 6135 Оптика
BISAC SCI004000 Astronomy
BISAC SCI005000 Physics / Astrophysics
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
1. Astropy Collaboration, Robitaille T.P., Tollerud E.J., et al., 2013, A&A, 558, id. A33
2. Baluev R.V., 2013, Astronomy and Computing, 2, p. 18
3. Baluev R.V., 2018, Astronomy and Computing, 25, p. 221
4. Baluev R.V. and Shaidulin V.S., 2015, MNRAS, 454, 4379
5. Baluev R.V., Sokov E.N., Shaidulin V.S., et al., 2015, MNRAS, 450, p. 3101
6. Bonomo A.S., Desidera S., Benatti S., et al., 2017, A&A, 602, id. A107
7. Bradley L., Sip o cz B., Robitaille T., et al., 2024, astropy/photutils: 1.13.0
8. de Wit J., Gillon M., Demory B.O., et al., 2012, A&A, 548, id. A128
9. Evans T.M., Aigrain S., Gibson N., et al., 2015, MNRAS, 451, p. 680
10. Fedotov A.A. and Baluev R.V., 2022, Astronomy at the Epoch of Multimessenger Studies, Proc. All-Russian Astron. Conf. (VAK-2021), p. 227
11. Knutson H.A., Charbonneau D., Allen L.E., et al., 2007, Nature, 447, p. 183
12. Majeau C., Agol E., Cowan N.B., 2012, ApJL, 757, id. L32
13. Rauscher E. and Menou K., 2013, ApJ, 764, p. 103
