{
  "abstract": "We test the idea proposed by Laporte \\& Orkney that $ω$ Centauri ($ω$Cen) is the central nuclear star cluster of the Gaia-Sausage-Enceladus galaxy (GSE) which got dislodged by the bar. We run a series of simulations in time-evolving bar potentials with present-day pattern speeds within Portail et al's $Ω_{b}=39\\pm3.5\\,\\rm{km\\,s^{-1}\\,kpc^{-1}}$ and rate of slow-down $\\dotΩ_{\\rm b}= 4.5 \\pm 1.4 \\,\\rm{km \\,s^{-1}\\,kpc^{-1}\\, Gyr^{-1}}$ to study how bar resonances modulate the angular momentum and energies of both GSE-debris and $ω$Cen's location in $(E,L_{z})$ space. We find that the retrograde $3:2$ resonance is capable of inflicting changes of $ΔE\\approx0.4\\times10^{5}\\,\\rm{km^{2}\\, s^{-2}}$, $ΔL_{z}\\approx0.3-0.5\\times10^{3}\\, \\rm{km \\, s^{-1}\\, kpc^{-1}}$ within timescales of $Δt\\approx 0.5-1\\,\\rm{Gyr}$, well within the bar's lifespan $t_{\\rm{bar}}\\approx10-8\\,\\rm{Gyr}$. These results are independent of the choice of potential or modelling. We uncover a sample of N-rich stars with metallicities $-2.0<[\\rm{Fe/H}]<-1.0$ and aluminium enrichments consistent with $ω$Cen. In ($E,L_{z}$) space, the map reveals a corridor of trailing N-rich stars clustered about the region connecting $ω$Cen to the GSE's debris centroid, matching $ω$Cen's past predicted track. This provides the best evidence yet that $ω$Cen is the nuclear star cluster of the GSE. Using M54 and $ω$Cen's chemistry we show that neither first nor second generations follow general galaxy-wide scale chemical enrichment trends. This is empirical evidence that GC chemical trends are a cluster-scale physics problem, not a galaxy-wide one.",
  "abstract_shown": true,
  "affiliations": [],
  "article_type": null,
  "arxiv": "2610.07581",
  "author_total": 5,
  "authors": [
    {
      "name": "Axel Mannu"
    },
    {
      "name": "Chervin F. P. Laporte"
    },
    {
      "name": "Matthew D. A. Orkney"
    },
    {
      "name": "Yassin Rany Khalil"
    },
    {
      "name": "Benoit Famaey"
    }
  ],
  "bibtex": "https://research.draconitic.com/paper/8n662emqks41p.bib",
  "cited_by": 0,
  "doi": "10.48550/arxiv.2610.07581",
  "fulltext_url": null,
  "id": "8n662emqks41p",
  "issns": [],
  "landing_url": "https://arxiv.org/abs/2610.07581",
  "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.GA"
    ],
    [
      "openalex",
      "3103|Stellar, planetary, and galactic studies"
    ]
  ],
  "openalex": "W7220992256",
  "pdf_url": "https://arxiv.org/pdf/2610.07581",
  "pmcid": null,
  "pmid": null,
  "published": "2026-10-06",
  "publisher": null,
  "ris": "https://research.draconitic.com/paper/8n662emqks41p.ris",
  "sources": [
    {
      "first_seen": "2026-10-30T12:27:22Z",
      "native_id": "2610.07581",
      "source": "arxiv",
      "url": "https://arxiv.org/abs/2610.07581"
    }
  ],
  "subjects": [
    {
      "field": "astronomy",
      "origin": "arxiv:astro-ph.GA",
      "subfield": "galaxies"
    }
  ],
  "title": "Stirred, not shaken: Dislodging $ω$ Centauri from the Sausage galaxy through bar resonances",
  "title_text": "Stirred, not shaken: Dislodging ω Centauri from the Sausage galaxy through bar resonances",
  "type": "preprint",
  "updated_at": "2026-10-30T12:27:22Z",
  "url": "https://research.draconitic.com/paper/8n662emqks41p",
  "venue": "arXiv",
  "versions": []
}