{
  "abstract": "The Neptunian desert and savanna are separated by a ridge, an overdensity at orbital periods of approximately 3-6 d identified with Kepler. Like the hot Jupiter pileup at larger radii, this feature has been linked to the accumulation of successful outcomes of high-eccentricity migration (HEM). We revisit the ridge independently using TESS occurrence posteriors for FGK main-sequence stars. We quantify its excess over adjacent regions and compare six occurrence profiles using leave-one-out cross-validation and Bayesian evidence. For planets with radii of approximately 5-8 $R_\\oplus$, the ridge has twice the occurrence density of the denser neighbouring region ($J=2.05^{+0.52}_{-0.44}$), with 99.9% posterior support (one-sided Gaussian equivalent of $3.1σ$). This contrast agrees with the discovery study and earlier Kepler occurrence measurements. Both predictive performance and Bayesian evidence strongly favour profiles peaking within the ridge over a single power law. The lognormal is preferred, suggesting a narrower inner wing and a more extended outer wing, although evidence for asymmetry remains weak. In the same period window, the analysis recovers the hot Jupiter pileup (approximately 10-16 $R_\\oplus$) with a contrast consistent with that of the ridge and excludes an analogous excess among sub-Neptunes (approximately 2-4 $R_\\oplus$) with $3.4σ$ posterior support. TESS thus provides an independent detection of the Neptunian ridge. Its possible asymmetry would be compatible with HEM, in which tidal disruption could produce a sharper inner edge and variations in circularisation efficiency a more gradual outer decline. Establishing whether the ridge has this shape requires more precise occurrence measurements, with PLATO's expected planet yield offering a promising opportunity to help unveil its morphology.",
  "abstract_shown": true,
  "affiliations": [],
  "article_type": null,
  "arxiv": "2611.03643",
  "author_total": 1,
  "authors": [
    {
      "name": "Amadeo Castro-González"
    }
  ],
  "bibtex": "https://research.draconitic.com/paper/etpsatwq1tedj.bib",
  "cited_by": 0,
  "doi": "10.48550/arxiv.2611.03643",
  "fulltext_url": null,
  "id": "etpsatwq1tedj",
  "issns": [],
  "landing_url": "https://arxiv.org/abs/2611.03643",
  "language": null,
  "licence": "CC-BY-4.0",
  "licence_label": "CC BY 4.0",
  "licence_source": "article",
  "licence_url": "http://creativecommons.org/licenses/by/4.0/",
  "metadata_licence": "CC0-1.0",
  "native_subjects": [
    [
      "arxiv",
      "astro-ph.EP"
    ]
  ],
  "openalex": null,
  "pdf_url": "https://arxiv.org/pdf/2611.03643",
  "pmcid": null,
  "pmid": null,
  "published": "2026-11-02",
  "publisher": null,
  "ris": "https://research.draconitic.com/paper/etpsatwq1tedj.ris",
  "sources": [
    {
      "first_seen": "2026-11-03T12:21:04Z",
      "native_id": "2611.03643",
      "source": "arxiv",
      "url": "https://arxiv.org/abs/2611.03643"
    }
  ],
  "subjects": [
    {
      "field": "astronomy",
      "origin": "arxiv:astro-ph.EP",
      "subfield": "planetary"
    }
  ],
  "title": "The Neptunian ridge through the lens of TESS",
  "title_text": "The Neptunian ridge through the lens of TESS",
  "type": "preprint",
  "updated_at": "2026-11-05T15:20:21Z",
  "url": "https://research.draconitic.com/paper/etpsatwq1tedj",
  "venue": "arXiv",
  "versions": []
}