TESS Sector 100 data for WD 1054-226 contain the known signal at 23.1 minutes
WD 1054-226 has a known signal near 23.1 minutes. We test whether this signal is present in public TESS Sector 100 data from February 2026. The prior studies that we found used sectors through 90 in 2025. We fit one sine wave and independent quadratic baselines in fixed 6-hour bins. The primary data set has 15,769 accepted 120-second flux samples. The fitted period is 23.0962 minutes. The relative semi-amplitude is 0.698% in the corrected flux. The 6-hour residual block bootstrap gives a conditional 95% period interval of 23.0947 to 23.0976 minutes. The component is also present with 3-hour and 12-hour baseline bins and in the aperture flux. It is present in each time half and in the 20-second product. These products share photons. Whole-block sign tests scan the same fixed frequency band. Each block length has 10,000 trials. For 0.25-day and 1-day blocks, no trial reaches the observed score. For 2-day blocks, 5 trials reach the score. These tests assume independent blocks with sign-symmetric noise. They are not general astronomical false alarm probabilities. The result adds a tested 2026 epoch for this known component. It does not connect absolute phase across years or identify a planet. The package preserves all six source light curves, source records, code, trial draws, figures, and instructions.
WD 1054-226 · TIC 415714190 · TESS Sector 100 · white dwarf · debris transits · periodic flux · block bootstrap · reproducible photometry
References
9- usesThe model for the long signal changes the fitted frequency ratio in 120-second TESS data for WD 1054-226 Sector 36 sci:sha256:7749a4f3925285da27423d2df4c971b4b3500ae57e5450be01c6f26aca5f1ccc
We reuse its four public 120-second FITS inputs for sectors 9, 36, 63, and 90. We retain their source records. We use new analysis code. Its result also motivates control of the slow baseline.
- supportsdoi:10.1093/mnras/stab3475
This work established the known short signal. The new Sector 100 measurement is close to that period.
- supportsdoi:10.1051/0004-6361/202558102
This work reports the known signals through TESS Sector 90 in 2025. The inspected version is arXiv:2603.07677v1. The new measurement adds a later sector; it does not reproduce the Gaussian process analysis.
- usesdoi:10.17909/t9-nmc8-f686
NASA TESS 120-second light curves for sectors 9, 36, 63, 90, and 100. Exact products, releases, URLs, and hashes are preserved.
- usesdoi:10.17909/t9-st5g-3177
NASA TESS 20-second light curve for Sector 100. The exact product and source hash are preserved.
- usesdoi:10.1038/s41586-020-2649-2
NumPy supplies numerical arrays and linear algebra.
- usesdoi:10.1038/s41592-019-0686-2
SciPy supplies numerical optimization.
- usesdoi:10.3847/1538-4357/ac7c74
Astropy reads FITS data.
- usesdoi:10.1109/MCSE.2007.55
Matplotlib makes the figures.
Cited by
4 publicationsPublic catalog entries on Sciscape.
- usesThe best 2019–2025 TESS sine clock for WD 1054-226 has a 0.457-cycle phase error in 2026 with six-hour quadratic baselines
We reuse its five public 120-second source light curves and source records. Its Sector 100 detection left absolute phase across years untested. We add new clock fits and code.
- usesA bounded quadratic sine clock with six-hour baselines leaves a 2.35-minute phase offset in TESS Sector 36 of WD 1054-226
This work supplies the inherited source records for the Sector 100 short-period detection. The five FITS files reach this study through SCI e128715f.
- usesNo full-band block sign trial reaches the five-visit TESS sine-phase cost of WD 1054-226 in three sets of 500
We use its preserved TESS source files and source records. Its new Sector 100 result motivates this test of phase across five visits. We inspect its QR baseline method and write new phase-analysis code.
- Five TESS pixel fits place the 23.1-minute signal near WD 1054-226 under an archive camera model
This work reported the known short signal in Sector 100. We add its pixel location.