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astro-ph.IM · Instrumentation and Methods for Astrophysicsastro-ph.SR · Solar and Stellar Astrophysics

The QLP small aperture to image depth ratio increases by 38% between two GG Orionis secondary eclipses in TESS Sector 98

We test whether one depth correction can match six GG Orionis eclipses in the TESS Sector 98 QLP small aperture flux. We compare QLP v01 flux with direct image flux at the same exposures. A free linear fit uses the observed image eclipse profile. The small aperture to image amplitude ratio rises from 0.21635 to 0.29843 between the first and last complete secondary eclipses. This is a 37.94% increase over 39.79 days. Changes to the baseline, window, and reference aperture give increases of 37.1% to 38.8%. A separate center median estimate gives 37.23%. The ratios are not monotonic. For these six measured ratios, any common positive correction leaves at least 15.94% error in one event against the image reference. The main aperture ratio rises by 4.36% between the same secondary events. The large aperture ratio changes by -0.52%. An earlier SCI study found QLP depth errors after Sector 94. This work adds a test of separate events within one sector. The result applies to one binary, six complete events, and the saved QLP version. The image sum is a reference and is not exact total stellar flux. Conditional residual errors omit full reference and pipeline errors. The cause remains unknown. The result does not show a change in the stars. The package preserves exact data, source records, code, figures, controls, and checks for a repeat without network access.

TESS · GG Orionis · TIC 72782654 · QLP · eclipse depths · photometry · aperture calibration · reproducible astronomy

Admitted 1 citing publication

References

14
  1. supportsFrom TESS Sector 94, QLP eclipse depths of 49 southern CVZ binaries are 11% smaller in the 3x3 aperture and 36% smaller in the 1x1 aperture than before, while SPOC depths do not change sci:sha256:298e00ff618495fcec0eb623e314b89a45905b03d6a9b8d74503468776f9ffc1

    This earlier study found QLP depth errors after Sector 94 in 49 southern continuous viewing zone binaries. We add a comparison of separate events within Sector 98 for GG Orionis. We do not claim the general depth error as new.

  2. usesA common profile fit gives a 272-second eclipse spacing decrease in GG Orionis between TESS sectors 6 and 98 sci:sha256:1e16d6be847356e486e2e2113a805609d0075a90a6694ad4b73599e5b1297f18

    We reuse its exact compressed Sector 98 TESScut file and source records. We checked its QLP file against a fresh MAST download. Its eclipse spacing result is prior work; no source code is reused.

  3. A local period scale reduces the effect of time coordinates below 0.1 s in 12 GG Orionis eclipses from TESS Sector 98 sci:sha256:559c55732401352271e05433c27f9bd19df0112e5af8381ee76b6890c426b777

    This prior study used the same GG Orionis observations to test eclipse times and time coordinates. We report a separate depth comparison.

  4. TESS data show a 275 s decrease in the interval from primary to secondary eclipse of GG Orionis from 2018–2019 to 2025–2026 sci:sha256:37219a9fe1143fc78e84873e4270ce08af6db11b8b9156c314ca6cc6e22ce82b

    This prior study reported eclipse spacing changes in the same GG Orionis observations. We do not claim a new timing result.

  5. usesdoi:10.17909/t9-r086-e880

    We use the public QLP v01 Sector 98 light curve for TIC 72782654 from this MAST data collection.

  6. doi:10.3847/2515-5172/ae5790

    The QLP release note describes the change to TGLC methods from Sector 94. We consulted its abstract and the public QLP documentation.

  7. doi:10.3847/1538-3881/acaaa7

    This paper describes TGLC photometry. We do not run that pipeline or assign a cause to the measured depth changes.

  8. doi:10.1086/316855

    This paper gives the established binary star context for GG Orionis.

  9. usesdoi:10.1117/1.JATIS.1.1.014003

    We use public TESS observations.

  10. usesdoi:10.3847/2515-5172/abca2e

    This paper describes QLP, which produced the light curve tested here.

  11. usesdoi:10.3847/1538-4357/ac7c74

    Astropy reads the FITS data and the image coordinate system.

  12. usesdoi:10.1038/s41592-019-0686-2

    SciPy supplies a separate numerical check of the common correction bound.

  13. Fixed-shape fits give smaller depths in TGLC PSF flux for two of three reported TESS exocomet events sci:sha256:47f30d35b46e1aaceb78fd8e6d24325dd24d5f44738f07930516fdd8be65c148

    This prior work uses fixed time shapes to compare depths in public flux products. We use a measured image profile to compare separate events in GG Orionis. No code or data from that study are reused.

  14. A within-sector transit-depth F-test of 1,473 TESS objects of interest with periods below 2 days finds no new disintegrating-planet candidate and shows that TOI-2593.01 has a 4.41-day period sci:sha256:1137d1ab713085f746b07c82081e865272d44bb1f1e3d671df52eed7abd3ebcb

    This related survey tests transit depth changes within TESS sectors. It gives context for the use of event depth comparisons. It does not supply inputs to our GG Orionis test.

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