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astro-ph.EP · Earth and Planetary Astrophysicsastro-ph.IM · Instrumentation and Methods for Astrophysics

Uniform 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

We measured the TESS secondary-eclipse depths of all hot Jupiters with P < 10 d, Rp > 0.5 RJ and Tmag < 12 with one uniform method. We used the SPOC 120-s PDCSAP light curves of Sectors 1 to 107. For each planet, we fitted a transit ephemeris with TESS data only, fitted each eclipse event with a local baseline and combined the events. We calibrated the errors with 16931 measurements at false eclipse phases. Of 439 planets, 420 have a depth (11 have no 120-s data and 8 have grazing orbits). 35 planets have z ≥ 3 and 24 have 2 ≤ z < 3. The false phases give 2.2 and 9.2 false signals (upper estimates). For the 37 planets with a published TESS depth, the sum of (Δ/σ)² is 43.5, and 4 values differ by more than 2σ. Nine detections have no robustness flag and no published TESS eclipse depth that we found: MASCARA-1 b, TOI-1181 b, WASP-48 b and WASP-87 b (z = 4.2 to 14.9), and HD 149026 b, WASP-95 b, HD 202772 A b, HAT-P-40 b and TOI-2046 b (z = 3.0 to 3.3). One or two of the last five can be noise. For the 389 planets with no transit-fit flag, the stacked geometric albedo Ag increases from −0.03 ± 0.04 (Teq0 < 1300 K) to 0.78 ± 0.10 (Teq0 ≥ 2600 K) if all eclipse light is reflected light. After we subtract the largest blackbody thermal flux (no heat redistribution, Bond albedo 0), the stacked values are negative in all six Teq0 bins (−0.05 to −0.19). Thus thermal emission explains the stacked depths, and the data need no strong reflected light. A global fit gives Ag = 0.020 (0.010 to 0.035) and heat redistribution ε = 0.29 (0.27 to 0.32). For Teq0 ≥ 2200 K, one (Ag, ε) pair does not fit all planets (χ²r = 5.9). No planet is clearly too bright for thermal emission plus a normal albedo. On average, the eclipses of the 32 detections with no flag occur at the predicted time (mean shift −0.37 ± 0.23 min). For 63 of 386 planets, the TESS transit time differs from the archive ephemeris by more than 3σ. For 7 hosts with strong periodic stellar signals, the removal of these signals gave a valid depth for 3. Assumptions: the PDCSAP systematics and crowding corrections are correct, the transit model uses a circular orbit, the planet and the star are blackbodies, and one error scale factor applies to all stars. The supporting ZIP has the code, the input tables, the depths and upper limits of all 420 planets, the null measurements, the figures and the reproduction instructions.

exoplanets · hot Jupiters · TESS · secondary eclipse · occultation · geometric albedo · heat redistribution · brightness temperature · uniform survey · null test · false-alarm calibration · eclipse timing · transit ephemeris · stellar pulsations · prewhitening · MASCARA-1 b · TOI-1181 b · WASP-48 b · WASP-87 b · population study

Admitted 2 citing publications

References

41
  1. usesdoi:10.17909/t9-nmc8-f686

    We used the TESS SPOC 120-s light curves (PDCSAP flux) of Sectors 1 to 107 from MAST.

  2. usesdoi:10.26133/NEA13

    We selected the sample and took orbital and stellar parameters from the NASA Exoplanet Archive Planetary Systems Composite Parameters table.

  3. usesdoi:10.1117/1.JATIS.1.1.014003

    TESS mission description and spectral response used for the band-integrated brightness temperatures.

  4. supportsdoi:10.3847/1538-3881/ababad

    Wong et al. 2020 TESS year-1 eclipse depths agree with our uniform depths for most planets in common. WASP-5 b is an exception: our depth is 212 +- 54 ppm and theirs is 31 +- 64 ppm (difference 2.2 sigma).

  5. supportsdoi:10.3847/1538-3881/ac0c7d

    Wong et al. 2021 TESS year-2 eclipse depths agree with our uniform depths for most planets in common. KELT-1 b is an exception: our depth is 216 +- 33 ppm and theirs is 388 +- 66 ppm (difference -2.3 sigma).

  6. doi:10.48550/arXiv.2204.03327

    Earlier TESS phase-curve analysis of a set of hot Jupiters (Blazek et al. 2022).

  7. supportsdoi:10.48550/arXiv.2410.04804

    Arora and Goyal 2024 TESS occultation depths of WASP-77 A b and WASP-17 b; we compare our depths with them.

  8. supportsdoi:10.48550/arXiv.2004.10767

    von Essen et al. 2020 TESS eclipse depth of WASP-33 b; we compare our depth with it.

  9. doi:10.1093/mnras/staa814

    Jansen and Kipping 2020 analysed the TESS phase curve and occultation of WASP-100 b. Our comparison table uses the WASP-100 b value of Wong et al. 2020.

  10. doi:10.3847/1538-3881/ac26bd

    Wong et al. 2021 TESS phase curve of TOI-2109 b. Our eclipse depth from 2 sectors, 889 +- 29 ppm, is 2.9 sigma larger than their 731 +- 46 ppm.

  11. doi:10.3847/1538-3881/ac224e

    Addison et al. 2021 TESS eclipse depth of TOI-1431 b (MASCARA-5 b), 127 +- 5 ppm. Our depth from 9 sectors, 107 +- 9 ppm, is 1.9 sigma smaller.

  12. supportsdoi:10.1051/0004-6361/202348270

    Demangeon et al. 2024 TESS and CHEOPS eclipse of WASP-76 b; we compare our depth with it.

  13. supportsdoi:10.48550/arXiv.2403.12311

    Subjak et al. 2024 TESS eclipse depth of BD-14 3065 b; our depth agrees with it.

  14. supportsdoi:10.48550/arXiv.2403.19468

    Kalman et al. 2024 TESS phase curve of WASP-167 b; we compare our eclipse depth with it.

  15. doi:10.1051/0004-6361/202346705

    Pagano et al. 2024 TESS eclipse depth of WASP-178 b, 70 +- 40 ppm, from photometry without the contaminated pixels. Our main catalog value is not a measurement (many events clipped). Our prewhitened depth, 185 +- 41 ppm, is 2.0 sigma larger.

  16. supportsdoi:10.48550/arXiv.2506.20432

    Garai et al. 2025 TESS eclipse depth of KELT-7 b, 69 +- 9 ppm. Our depth from 8 sectors, 79 +- 12 ppm, agrees within 0.7 sigma.

  17. doi:10.48550/arXiv.2512.05175

    Patel et al. 2026 TESS phase curve of WASP-189 b, eclipse depth 203 +- 16 ppm. Our depth from 1 sector, 152 +- 17 ppm, is 2.2 sigma smaller.

  18. supportsdoi:10.3847/1538-3881/ad09bd

    Wang and Espinoza 2024 found a 0.2-d variable star near KELT-8. Our KELT-8 light curve has a 0.197-d signal that explains the alternating eclipse depths.

  19. supportsdoi:10.1038/s41586-022-04453-2

    Lothringer et al. 2022 found an eclipsing binary that contaminates the TESS light curve of WASP-178. Our 0.185-d signal is half of its orbital period.

  20. supportsdoi:10.1088/0004-6256/150/6/197

    Hartman et al. 2015 found periodic signals near 1.84 cycles/d in HAT-P-57. We find a 1.86 cycles/d signal in TESS.

  21. supportsdoi:10.48550/arXiv.2601.11313

    Balkoova et al. 2026 found delta Scuti pulsations of HAT-P-57 A at 8.0935 cycles/d in TESS Sector 80. Our periodogram gives the same frequency.

  22. supportsdoi:10.3847/1538-4357/ab59d0

    Ahlers et al. (2020) found a 130 +- 20 ppm eclipse of MASCARA-4 b in TESS 30-min FFI data of Sectors 10 and 11. Our 120-s depth agrees within 1 sigma.

  23. supportsdoi:10.3847/1538-3881/ac1ba3

    Cabot et al. (2021) found a 364 +- 28 ppm TESS eclipse of TOI-1518 b. Our uniform depth agrees within 1 sigma.

  24. doi:10.48550/arXiv.2504.13997

    Wang et al. (2025) predicted a 53 ppm TESS eclipse of HAT-P-67 b and found no clear eclipse in the TESS data. Our tentative depth of 62 +- 24 ppm (z = 2.6) agrees with the prediction.

  25. Local circular fits to 53 TESS eclipses leave the 2022 to 2024 change unresolved for KELT-1 b sci:sha256:17d42abf0d5835d4d020ff6a63534770e4aa73ab601c7e9de2ff5793a2dff74a

    Local fits to the same three KELT-1 b TESS sectors gave sector coefficients of 330, 147 and 199 ppm. We compare our mean depth of all sectors with these values.

  26. Local fits give apparent decreases at eclipse and phase 0.75 in six WASP-121 b TESS sectors sci:sha256:adde673bfd380ffb8dc6e242a9d4dc231b7366ad6445edc9ef75bf6ed0536ad9

    A control phase at 0.75 gave an apparent depth change as large as the eclipse change for WASP-121 b. This is an example of the false-phase signals that our null calibration measures for all planets.

  27. doi:10.48550/arXiv.2109.05031

    Hooton et al. (2022) measured a CHEOPS occultation depth of 133 +- 19 ppm for MASCARA-1 b. We give the first TESS-band depth that we found and compare it with the bluer CHEOPS value.

  28. usesdoi:10.48550/arXiv.2205.01860

    Kabath et al. (2022) confirmed TOI-1181 b and TOI-2046 b. We report new TESS eclipse detections of these planets with the archive system parameters.

  29. doi:10.48550/arXiv.1702.03797

    de Wit et al. (2017) found tidally excited stellar pulsations of HAT-P-2 at harmonics of the orbital frequency. These pulsations can change our TESS eclipse depth of HAT-P-2 b, and we give this as a caveat.

  30. supportsLocal circular fits to 40 TESS eclipses do not resolve a mean depth change for KELT-20 b from 2019-2022 to 2024 sci:sha256:1f2571d64165342e8f232506e8c434619bb2cf54d3e29f0a3bbc66ccb9a6899e

    This SCI publication did not resolve a change of the mean TESS eclipse depth of KELT-20 b from 2019-2022 to 2024. Our test of all 7 sectors also finds no significant change (p = 0.10).

  31. supportsLocal TESS fits do not detect a change in HAT-P-7 b eclipse depth from 2019 to 2024 with independent event errors sci:sha256:bce7c5e8320ee4cf1a3df556122d1441d671bd592ad4d440283fe97174a63f25

    This SCI publication did not detect a change of the TESS eclipse depth of HAT-P-7 b from 2019 to 2024. Our test of all 10 sectors agrees (p = 0.96).

  32. A local circular model gives a lower TESS secondary eclipse depth for TOI-1518 b in late 2024 than in 2022 sci:sha256:60e289bcfad7e6152dab3220b06620d4349f3f25d0810512d404a2e5af482cf8

    This SCI publication reported a lower TESS eclipse depth of TOI-1518 b in late 2024. Our Sector 84 depth (288 +- 35 ppm) is lower than Sector 57 (375 +- 31 ppm) and Sector 58 (400 +- 33 ppm), but our test of all 5 sectors gives p = 0.26.

  33. A spline fit gives a conditional 95% interval of -72 to 44 ppm for the 2022 to late 2024 orbital contrast change of TOI-1518 b sci:sha256:0fd59adf6c86beaa950090525311f2342e45a1fa1011a30998c0ee4c370bac3e

    This SCI publication fitted the TOI-1518 b orbital contrast with a spline baseline and found no resolved change from 2022 to late 2024. We use a local quadratic baseline for each eclipse of all planets.

  34. supportsLocal fits to six TESS sectors do not resolve a KELT-9 b eclipse depth change from 2019 to 2024 sci:sha256:a6203af39c5839b4acca6c41bd66edb381d894a74311589743fb8b933c7f02a7

    This SCI publication did not resolve a change of the TESS eclipse depth of KELT-9 b from 2019 to 2024. Our test of all 6 sectors agrees (p = 0.97).

  35. supportsFixed-shape eclipse fits to TESS sectors 96 and 103–106 do not resolve a depth change in WASP-18 b sci:sha256:941dee6ee301412c38413dc6d0e026a8e7eb7bab5ca809c25e46e9a386411d8f

    This SCI publication did not resolve a change of the TESS eclipse depth of WASP-18 b between 2025 and 2026. Our test of all 10 sectors also finds no significant change (p = 0.14).

  36. supportsLocal TESS fits with a circular orbit do not resolve a change in the eclipse depth of WASP-100 b from 2018 to 2026 sci:sha256:bf0737aa330a6f62d845a4f6dc831f9c15897d24caf55317bd05aef3f69118d0

    This SCI publication did not resolve a change of the TESS eclipse depth of WASP-100 b from 2018 to 2026. Our test of all 43 sectors agrees (p = 0.56).

  37. supportsTESS 2-minute transit times of 153 bright hot Jupiters missed the NASA Exoplanet Archive default ephemeris predictions by more than 3 sigma for 33 planets (sectors 21-107) sci:sha256:1895bf428f65ddb5d621f1e1b67e6fe70b4074599f4ced66ffdc1cf0a99b69fe

    This SCI publication found that the archive default ephemerides missed the TESS transit times of 33 of 153 hot Jupiters by more than 3 sigma. We find 63 of 386 with the same test. For this reason we fitted a TESS ephemeris for each planet before the eclipse fits.

  38. doi:10.1088/0004-637X/754/2/136

    Stevenson et al. 2012 found Spitzer eclipses of HD 149026 b that agree with a circular orbit. Our TESS eclipse shift of -34 +- 5 min is thus probably noise or a systematic error.

  39. doi:10.48550/arXiv.1310.0011

    O'Rourke et al. 2014 measured Spitzer eclipses of WASP-48 b. We give a new TESS-band eclipse depth of WASP-48 b (174 +- 29 ppm, z = 6.0).

  40. doi:10.48550/arXiv.1710.07642

    Zhang et al. 2018 measured Spitzer phase curves and eclipses of HD 149026 b. We give a TESS-band eclipse depth of HD 149026 b (31 +- 9 ppm, z = 3.3).

  41. doi:10.48550/arXiv.2408.13680

    Adams et al. 2024 measured Spitzer secondary eclipses of hot Jupiters, including HD 202772 A b. We give a TESS-band eclipse depth of HD 202772 A b (45 +- 14 ppm, z = 3.3).

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