An HD 20794 design predicts 2.87 times the squared distance increase from uniform dates for a fixed source and periods under independent 0.5 m/s noise
We test how future dates can separate a fixed eccentric velocity curve for HD 20794 from a fitted pair of circular signals. We reproduce a source fit to 811 public night means. We choose 60 nights from 913 dates that pass geometric visibility tests at Paranal from November 2026 through October 2030. Future points share a separate free instrument offset. Each has an assumed independent total error of 0.5 m/s. We fit the rival coefficients again on the combined old and new times. At fixed periods, the chosen dates increase squared weighted model distance by 6.677. Uniform eligible-night indices increase it by 2.326. The increase ratio is 2.87. The chosen schedule exceeds 1000 random-order schedules. This comparison is not a p-value. The gain remains with free rival periods, future trends, and year offsets. A fixed 0.3 m/s correlated component with a 30-day time scale reduces the increase ratio to 1.38. The result is conditional on a fixed source curve and stated noise. It does not give a planet probability or detection power. The package includes source data, dates, code, figures, controls, provenance, and reproduction checks.
HD 20794 · radial velocity · observation times · experimental design · eccentricity · harmonic ambiguity · reproducible research
References
9- A 647.6-day eccentric curve fits 811 HD 20794 nights better than a fixed 2:1 circular pair under a 1 m/s noise term sci:sha256:c409aa928d17822b918d8d0c69baf99de3f193127237bc0490155837d246d0c2
[Legacy relation: reproduces] We reproduce its 811-night eccentric fit and reuse its MIT preprocessing code. We extend its model-distance calculation to future dates with a free future offset.
- usesA Gaia motion correction reduces the difference between two public HD 20794 velocity tables on 64 nights in 2019–2023 sci:sha256:6039fff418f96a889c4a9ed1fc8c320f137bf96e956099d423f22839f0ff73c5
We use its proposed perspective acceleration correction for the public sBART velocities.
- usesAn eccentric 647.6-day model lowers mean squared error in 9 of 18 omitted HD 20794 seasons in a fit with fixed periods and independent Gaussian noise sci:sha256:33d2a5aaa63141db39d6bccc13412d17b7337d9dca639abce667e5bdc293104c
Its season and offset results motivate our fixed-schedule future year-offset control.
- usesdoi:10.1051/0004-6361/202451769
This source reports the HD 20794 velocity signals and their physical and noise context.
- usesdoi:10.26093/cds/vizier.36930297
We use three unchanged public velocity tables from this catalogue.
- doi:10.1088/0004-637X/709/1/168
This work explains the ambiguity between an eccentric signal and a circular pair in a 2:1 period ratio.
- doi:10.1051/0004-6361/201525872
This work tests the distinction between eccentric signals and circular pairs.
- doi:10.1111/j.1365-2966.2008.13656.x
This prior work describes optimal observation times for tests between rival planet models.
- usesdoi:10.1051/0004-6361/202243940
Gaia DR3 astrometry enters the inherited motion correction.
Cited by
2 publicationsPublic catalog entries on Sciscape.
- usesA 60-night HD 20794 design reduces the largest third harmonic error by 1.6% from uniform dates under a fixed covariance at three periods
We reuse its verified public night means, approximate visibility grid, uniform schedule, prior selected schedule, and MIT grid code. We test a different measurement goal with a common correlated covariance and future year offsets.
- A free sixth cycle component removes more than 99.8% of 682.5-day signal information at the central HD 161098 periods
Its catalog abstract reports conditional weighted model distance tests for HD 20794. We reviewed the abstract for context and did not reuse its files.