CLEANING THE TESS OBSERVATIONS OF WASP-33 B TRANSITS FROM THE HOST STAR PHOTOMETRIC VARIABILITY
Section: EXOPLANETS
Authors:
1.
Saint Petersburg State University
Special Astrophysical Observatory of the Russian Academy of Sciences
Special Astrophysical Observatory of the Russian Academy of Sciences
2.
Central Astronomical Observatory at Pulkovo, Russian Academy of Sciences
Type:
Сonference article
Published:
27.12.2024
Subject area:
UDK 52
UDK 53
UDK 520
UDK 521
UDK 523
UDK 524
UDK 52-1
UDK 52-6
GRNTI 41.00
GRNTI 29.35
GRNTI 29.31
GRNTI 29.33
GRNTI 29.27
GRNTI 29.05
OKSO 03.06.01
OKSO 03.05.01
OKSO 03.04.03
BBK 2
BBK 223
TBK 614
TBK 6135
BISAC SCI004000 Astronomy
BISAC SCI005000 Physics / Astrophysics
UDK 53
UDK 520
UDK 521
UDK 523
UDK 524
UDK 52-1
UDK 52-6
GRNTI 41.00
GRNTI 29.35
GRNTI 29.31
GRNTI 29.33
GRNTI 29.27
GRNTI 29.05
OKSO 03.06.01
OKSO 03.05.01
OKSO 03.04.03
BBK 2
BBK 223
TBK 614
TBK 6135
BISAC SCI004000 Astronomy
BISAC SCI005000 Physics / Astrophysics
Language:
English
Keywords:
techniques: photometric; stars: variables: delta Scuti; stars: individual: WASP-33; planets and satellites: detection
Abstract (English):
Based on the TESS observations of a $\delta$ Scuti variable WASP-33 obtained in 2019 and 2022, we thoroughly investigate the power spectrum of its photometric flux and construct a statistically exhaustive model for its variation. This model contains 30 robustly justified harmonics, the red noise, and quasiperiodic noise components. This compound model allows us to greatly improve the transit timing accuracy of the exoplanet WASP-33 b. The rms of its transit timing variation residuals is drastically reduced by a factor of 3.5, from 63 s to 18 s.
Based on the TESS observations of a $\delta$ Scuti variable WASP-33 obtained in 2019 and 2022, we thoroughly investigate the power spectrum of its photometric flux and construct a statistically exhaustive model for its variation. This model contains 30 robustly justified harmonics, the red noise, and quasiperiodic noise components. This compound model allows us to greatly improve the transit timing accuracy of the exoplanet WASP-33 b. The rms of its transit timing variation residuals is drastically reduced by a factor of 3.5, from 63 s to 18 s.
Keywords:
techniques: photometric; stars: variables: delta Scuti; stars: individual: WASP-33; planets and satellites: detection
techniques: photometric; stars: variables: delta Scuti; stars: individual: WASP-33; planets and satellites: detection
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4. von Essen C., Mallonn M., Borre C.C., et al., 2020, Astronomy and Astrophysics, 639, A34
