The WASP-33 signal at 27.795 cycles per day was weaker in the 2024 TESS data than in 2022
We test whether strong known signals in WASP-33 kept their measured amplitudes in a later public TESS visit. We fit 36 published frequencies and time trends to the 120-second light curves from Sectors 18, 58, and 85. The primary comparison contains six signals selected from published earlier amplitudes. The known H6 signal at 27.794848 cycles per day has fitted semi-amplitudes of 275.4, 580.0, and 273.8 parts per million in 2019, 2022, and 2024. The 2024-to-2022 ratio is 0.472, with a conditional 95% interval of 0.436 to 0.508. The difference is -306.2 parts per million. Its simultaneous 95% band across the 12 reported contrasts is -341.5 to -270.9 parts per million. The decrease persists with aperture flux, different trends, a wider eclipse mask, a free local frequency, and separate halves of each visit. The strong H24 signal changes much less. The 2024 H6 amplitude is consistent with its 2019 value. This extends earlier measurements to Sector 85. It does not identify a new mode or planet. The intervals depend on the fitted frequency list and assumptions about residual correlation. Unresolved beating and detector effects remain possible causes. We preserve the original archive files, numeric source facts, code, results, figures, and instructions for reproduction.
WASP-33 · TIC 129979528 · TESS Sector 85 · stellar pulsations · amplitude variation · public astronomical data · reproducible analysis
References
4- usesdoi:10.1093/mnras/staf011
We use numeric periods and amplitudes from Table 1, the Table 5 orbital period, and the first Table 6 transit time. We extend the earlier TESS amplitude comparison to Sector 85.
- usesdoi:10.17909/t9-nmc8-f686
We use the public SPOC TESS light curves at 120-second cadence for TIC 129979528 in Sectors 18, 58, and 85. Exact archive products and hashes are preserved.
- doi:10.1051/0004-6361/202452151
This study provides context for the effect of stellar variation on WASP-33 b measurements.
- usesdoi:10.3847/1538-4357/ac7c74
We use Astropy for FITS files, time conversion, and the Lomb-Scargle spectrum display.
Cited by
1 publicationPublic catalog entries on Sciscape.
- usesFitting stellar signals reduces the apparent 2019 to 2024 TESS half-depth transit width decrease of WASP-33 b from 2.90 to 0.62 minutes
We use its input product records and numerical stellar period table, and adapt its quality selection and slow trend design. We download the FITS data again from MAST and verify the same hashes.