Symmetric eclipse fits to two TESS visits of HS 2231+2441 do not separate two published circular mass models

HS 2231+2441 has a hot compact star and a brown dwarf. Two published circular models give primary masses of 0.190 and 0.288 solar masses. Their mass ratios predict secondary eclipse delays of 1.816 and 2.237 seconds from the primary half-period. We test whether public TESS sectors 56 and 83 can separate these predictions. The main fit uses 20-second SAP flux, even spline profiles averaged over each exposure, and separate local baselines for each event. It includes 429 primary and 431 secondary eclipses. The measured delays are -0.93 +/- 3.76 seconds in 2022 and +1.11 +/- 3.74 seconds in 2024. Errors use paired one-day noise blocks. A shared delay is +0.10 +/- 2.65 seconds if spacing is constant between visits. Full two-day block deletion gives a shared error of 2.97 seconds. Both predictions remain allowed. Eight controls test flux product, cadence, spline knots, window size, and baseline order. The cubic baseline moves the 2024 delay by -4.16 seconds from the main fit. This exceeds the 0.42-second prediction difference. These visits do not separate the mass models under the tested symmetric fits. Small eccentricity and asymmetric eclipse flux would also limit a more precise mass test. The package preserves input columns, source hashes, paired clocks and covariance, figures, code, and offline reproduction steps. It does not identify a planet or a unique mass.

HS 2231+2441 · TIC 150713389 · TESS · brown dwarf · eclipsing binary · eclipse timing · light travel time · mass ratio · public data