Two TESS pixel fits place the early 11.4-hour signal near WD 1054-226 with an archive camera model

The early 11.4-hour signal in WD 1054-226 has been linked to transiting debris. A nearby variable star could change that interpretation. We fit its position in public TESS target-pixel data from Sectors 9 and 36. The test uses the published base frequencies and second harmonics. It also fits the 25.02-hour pattern, baseline changes and pointing terms. An archive camera model gives offsets from the white dwarf of 0.389 and 0.131 pixel. One-day residual sign trials with a wider position search give 95th-percentile displacements of 0.742 and 0.280 pixel. Fixed-position fits favor the white dwarf over the nearest Gaia star and the brightest field star. The central 95% trial ranges of their cost differences remain positive in both visits. Some Sector 9 trials favor distant positions. Changes to the main time model keep the joint fits close to the white dwarf. Sector 9 has a weak second harmonic with a poorly determined separate position. The result adds a spatial constraint on a known signal. It assumes a valid camera response model and a useful residual sign model. It does not establish a unique source, an orbit or a planet. The package has calibrated pixel extracts, source hashes, camera models, code, figures and trial results.

WD 1054-226 · TESS · white dwarf · transiting debris · pixel signal position · 11.4-hour signal · source contamination · Gaia DR3