The tested temperature map lowers the shared fitted albedo in blackbody models of 389 TESS eclipse records
We test how surface temperature changes the thermal model for 389 public TESS eclipse records. We keep the published eclipse depths, errors, and geometry fixed. The temperature map conserves absorbed power. It has the same disk bolometric flux as the source effective temperature. The shared fitted geometric albedo falls from 0.0219 to 0.0044. This result uses the source convention of zero Bond albedo. The same direction holds under grey Lambert reflection and after each of 389 single record removals. With no heat redistribution, predicted thermal light increases in 388 records. The median increase is 12.8 percent, or 2.30 parts per million in eclipse depth. KELT-9 b is the only decrease. All six temperature bins retain negative mean residual albedos after the thermal correction. The data still need no strong reflected light within these models. Both common parameter fits have large residual scatter. These results test the model choice; they do not measure a common physical albedo or prove a new planet. The surface spectrum effect is established prior work. The contribution is its measured application to this fixed survey. The package contains the signed source, input tables, code, figures, all primary fitted grids, and exact repeat checks.
TESS · secondary eclipse · thermal emission · geometric albedo · temperature map · blackbody spectrum · hot Jupiters · model sensitivity · reproducible analysis
References
5- usesUniform TESS 120-s photometry (Sectors 1–107) detects eclipses of 35 of 420 hot Jupiters at z ≥ 3 (2.2 false expected), 9 with no published TESS depth; blackbody emission explains the stacked depths sci:sha256:59aa18ecf235f3a1537ef68883cfb4cb1737ce4c9e945510c455729d2eea26a5
We use its published depths, errors, geometry, response, and selection for 389 of its 420 records. We preserve the complete signed source and reproduce its four original population grid minima. We then test a surface temperature map with the same disk bolometric flux.
- usesdoi:10.1088/0004-637X/729/1/54
Equation 3 gives the prior no transport surface spectrum. Equation 4 gives the disk effective temperature used in the source survey. We use the same disk bolometric flux in our paired comparison.
- usesdoi:10.1093/mnras/stv470
Section 3.2.1 and Figure 6 explain the prior sum of blackbodies correction to optical thermal light and inferred albedo. We apply this established reasoning to the fixed TESS survey.
- doi:10.26133/NEA13
The source survey used this archive composite table. We preserve its snapshot and fitted geometry; we make no new archive query.
- doi:10.17909/t9-nmc8-f686
The source survey used these TESS SPOC light curves. Our analysis starts from its published depths and preserves its observation provenance. We make no new light curve measurement.
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