NEOWISE image fits do not detect a W1 or W2 change in WD J0234−0406 between 2014–2016 and 2022–2024 under the stated error model

WD J0234−0406 has dust emission and gas from planetary debris. We test whether its mean infrared flux changed between 2014–2016 and 2022–2024. We fit signed fluxes at fixed positions in public NEOWISE images. Four controls set the local profile, position offset, and gain correction. The main sample has 196 paired W1 and W2 exposures in 21 visits. Each time window gives the two scan seasons equal weight. The covariance includes image errors, whole-control resampling, and an independent 0.02 mag floor per visit and band. The late/early minus one estimates are −9.20% in W1 and −1.23% in W2. The nominal 97.5% Fieller sets are −23.84% to +6.64% and −46.41% to +61.95%. Neither band passes the two-band Bonferroni test at family level 0.05. Every estimable sensitivity check also includes zero change. A smaller fit radius fails the control-coverage rule and is reported as not estimable. Historical WISE profiles give the same test outcome. Catalog inclusion changes the image subset and its point estimates, which supports a separate image analysis for this faint source. The result applies to the two mean fluxes under the stated model. It does not establish constant emission at all times. W2 gives a weak constraint. Profile, position, and correlated calibration errors are not fully measured. The flux includes the unresolved star and surrounding material; no planet or dust mass is inferred. The package contains exact image patches, archive receipts, code, figures, and offline reproduction checks.

WD J0234−0406 · PHL 1360 · white dwarf · planetary debris · NEOWISE · infrared photometry · forced photometry · Fieller sets · reproducible research