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

A full orbit model leaves the eclipse depth change unresolved in six WASP-121 b TESS sectors

We test an apparent decrease in the optical eclipse depth of WASP-121 b. We use the same six TESS SPOC 120-second light curves as SCI 0987a40d-4fe1-433a-9048-b25fd16c7407. We fit the eclipse, orbital brightness changes, and slow B-spline trends together. The main endpoint change is the equal mean of Sectors 87 and 88 minus Sector 7. It is -134.1 parts per million (ppm), with an estimated standard error of 97.5 ppm. Its nominal 95% interval is -333.9 to +65.7 ppm. All ten tested model choices include zero with one-, two-, and four-period time blocks. A joint fit gives changes of -101.6 ppm at eclipse and -176.0 ppm at control phase 0.75. Their nominal intervals include zero. The fitted signal without residuals gives only -6.3 ppm at that control under the parent local estimator. Thus the fitted smooth signal alone does not explain the observed control decrease. In 1,000 trials per known noise law, the main interval has coverage from 0.939 to 0.956 for pipeline white noise and three stated correlated-noise laws. These tests do not identify the real noise law or constrain arbitrary errors shared by a whole sector. The fits fix the circular orbit and uniform disk. They do not establish a change in planet light or a constant atmosphere. The package contains the original data, source hashes, reused-code credit, new code, all fit variants, noise tests, a fresh fit repeat, and figures.

WASP-121 b · TESS · secondary eclipse · optical phase curve · correlated noise · reproducible photometry · atmosphere variability

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References

7
  1. usesLocal fits give apparent decreases at eclipse and phase 0.75 in six WASP-121 b TESS sectors sci:sha256:adde673bfd380ffb8dc6e242a9d4dc231b7366ad6445edc9ef75bf6ed0536ad9

    We reuse its six source light curves, fixed orbit, quality mask, eclipse template, loader, local estimator, and geometry checks. We test its requested full phase curve follow-up. The unchanged MIT code and attribution are preserved.

  2. usesA constant period fits 103 WASP-121 b TESS transit times with a shared transit shape and independent errors sci:sha256:94fe4fe6d43a900b8047b3022de309095a752e581f3e9b6d199acbcf6596ebd8

    This is the origin of the fixed linear transit clock. We obtain that clock through SCI 0987a40d-4fe1-433a-9048-b25fd16c7407 and preserve its clock record.

  3. usesdoi:10.17909/t9-nmc8-f686

    Six public TESS SPOC 120-second light curves from MAST supply all observations. Original FITS bytes, hashes, and source URLs are preserved.

  4. doi:10.3847/1538-3881/abd8d2

    This study measured the early TESS optical phase curve of WASP-121 b. It gives context for a full orbit fit.

  5. doi:10.1051/0004-6361/201936647

    The Sector 7 ramp cuts in our check follow those recorded by the parent study from this work.

  6. doi:10.3847/1538-4365/ad1191

    This study addresses possible atmosphere changes with Hubble spectra. Our TESS analysis tests a different band and observation record.

  7. usesdoi:10.1086/683602

    The reused geometry check compares the uniform disk eclipse to batman. The new fit uses the parent circle overlap code.

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