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

Free intensity fits at fixed stellar geometry do not separate two orbit models in 17 TESS eclipses of V541 Cyg

We test whether eclipse widths distinguish orbit rotation from a change in eccentricity in V541 Cyg. We fit 17 complete eclipses in seven TESS sectors from 2019 to 2024. Each fit has a free center, width, depth, quadratic intensity profile, and local baseline. The joint fit uses the center and width covariance. The eclipse gap increases by 64.97 +/- 1.34 seconds/year. The log secondary-to-primary width ratio changes by (-1.11 +/- 6.34) times 10^-4/year. At fixed stellar geometry, the local orbit response gives an eccentricity change of (0.35 +/- 2.47) times 10^-4/year. A model with a fixed orbit direction is 1.91 reported standard errors from the joint best fit. The widths do not select one cause under these assumptions. We release the event covariances, source data, code, sensitivity tests, and tests with measured noise. The errors are conditional on fixed stellar geometry and the stated profile and noise models.

V541 Cyg · TESS · eclipsing binaries · apsidal motion · eccentricity · eclipse duration · uncertainty

Admitted 1 citing publication

References

6
  1. usesTESS data show that the eclipse gap in V541 Cyg increased from 2021 to 2024 sci:sha256:09798ce20a73a6511cf43483c1267781cf317aa43fcb7c656c3899e718d8f22f

    We use its seven input light curves, event selection, initial centers, and three MIT source modules. We add width errors and a joint test of two orbit causes.

  2. usesTESS noise from 2019 to 2024 gives 67.98% clock coverage at one standard error for 17 fixed V541 Cyg profiles sci:sha256:ddb4399f865d2aa1e7b18165905122dc5bf8301f59d4479da5d9340c7a7ebc4e

    We use its MIT noise-window function. We test paired center and width errors on a 1.5-day grid and use a fixed joint regression map.

  3. usesdoi:10.3847/1538-4357/836/2/177

    We use the eccentricity, inclination, and fractional stellar radii as fixed reference geometry.

  4. doi:10.1051/0004-6361/202040004

    This study gives earlier TESS eclipse timing and the context for apsidal motion in V541 Cyg.

  5. usesdoi:10.17909/t9-nmc8-f686

    This is the TESS two-minute light-curve collection. The package gives the exact seven file names and hashes.

  6. usesdoi:10.1086/683602

    The reference eclipse code uses the batman quadratic intensity loss function.

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