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

Approximate 95% bounds from 26 ESPRESSO profiles are below 1.33 m/s for six HD 111232 blend models with independent errors

A second star can change a measured radial velocity and imitate a planet. We test small motion of a faint copy of the HD 111232 mean cross-correlation profile. We reuse 26 public ESPRESSO exposures from 2024 and 2025. We remove continuum, depth, translation and width changes. We then measure the remaining shape at the fixed 19.6793-day candidate period, with free phase. The grid has 27 separation and width pairs. An identical copy at zero separation is blind to this test. No other cell has a detected signal; a shared wild bootstrap gives p=0.825 for the maximum statistic. With independent exposure errors, approximate 95% bounds corrected for the 26 measurable cells are 0.81 to 1.32 m/s for separations of minus or plus 2 km/s and width ratios of 0.8, 1.0 or 1.25. The bounds describe equivalent apparent velocity. The same-width bounds at minus and plus 0.5 km/s are 46.62 and 19.19 m/s. At the six 2 km/s cells, removal of single exposures gives bounds up to 1.64 m/s. A narrower profile window gives a bound up to 1.87 m/s. Specified Gaussian time-correlation controls give bounds up to 1.51 m/s. Finite injections check the local motion approximation. These are conditional limits on specified profile copies. They do not exclude all blends or stellar activity, and they do not confirm a planet. The package contains the original FITS files, source records, code, measurements, figures and offline instructions.

HD 111232 · radial velocity · spectral line shape · stellar blends · ESPRESSO · planet candidates · reproducible research

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References

11
  1. usesFits to 26 ESPRESSO spectra show no significant blue to red velocity signal at 19.679 days in HD 111232 sci:sha256:e1a1fc81724c24c63901a29ba3d6d44f613ccbe3fa0d3e39033349290afa0744

    We reuse its complete set of 26 original ESO ESPRESSO CCF FITS files and source manifest. It tested wavelength dependence; we measure conditional moving-copy shape limits.

  2. usesIndependent RVs reject 13 of 25 testable HARPS-RVBank v2 candidates (3 if HARPS errors double) and agree with a 19.7-day HD 111232 signal, with linear-trend nuisance models sci:sha256:1b429149b29b478f8b85a22182153f1e36c4ea06d284bbeb276a362b6f2254b1

    This study supplied the fixed HARPS period and identified the later ESO sample. Its velocity support motivated the shape test.

  3. A blind Keplerian search of 743 HARPS-RVBank v2 stars with 30 or more nights recovers 248 of 465 known planets and finds 57 signals (FAP < 0.1 %) with no known match that pass activity tests sci:sha256:17e2629023ac1bcbb507eb643afc93a73a34d8a9d1ba2357cc22bd7bc4f108cb

    The blind HARPS-RVBank v2 search reported the candidate tested here.

  4. A 19.68-day model fits 26 ESPRESSO velocities of HD 111232 better than eight tested aliases under independent Gaussian noise sci:sha256:f99835023bf371d706c7c405b229b57bd4ae5e6ffe87da7dd394c2d501cca99f

    This prior study tested aliases in the same ESPRESSO sample. We do not repeat that question.

  5. Joint fits retain the HD 111232 19.7-day amplitude across tested noise models in 26 ESPRESSO nights sci:sha256:bab2345a61b6a53232ad4b6e38ef724720603e3811d54e517feb7c26f0f4149e

    This prior study tested the velocity amplitude under noise models. Our new quantity is residual CCF shape.

  6. A 39.36-day noise model with long coherence lowers the log likelihood gain of the 19.7-day HD 111232 signal in 117 nights sci:sha256:dbc7cec3b40cdce04782c83042dbc4f1d9415147bd0c677f7388541e213f6d05

    This prior study tested joint long-orbit and harmonic-noise models.

  7. A persistent periodic process matches the HD 111232 signal in 32 later velocities at a fixed 19.68-day period sci:sha256:64f2e5aeba91f9454798375e136a87b8f46f34997f88b30b275bb920162d0515

    This prior study showed the limits of identifying physical causes from phase agreement.

  8. doi:10.48550/arXiv.1505.02663

    Santerne et al. 2015 describe spectroscopic blend diagnostics, blind cases, and CCF velocity dilution.

  9. doi:10.1093/mnras/stab1323

    Collier Cameron et al. 2021 use translation-invariant CCF information to separate line variability from Doppler shifts.

  10. usesdoi:10.18727/archive/21

    ESO Science Archive data collection containing the public ESPRESSO observations.

  11. doi:10.1051/0004-6361/202038306

    Pepe et al. 2021 describe ESPRESSO.

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