{
  "abstract": "The Little Red Dots (LRDs) are compact, broad-line sources that appear to contain accreting black holes (BHs) embedded in dense gas. Proposed models for their central environments (including quasi-stars, radiative BH envelopes and super-Eddington accretion discs) predict gas densities at the radii probed by an extreme-mass-ratio inspiral that differ by many orders of magnitude. We compute the inspiral of a $10$--$30\\Msun$ BH for a range of LRD interior models, including environmental effects from the gas, and test with a mismatch criterion whether the resulting waveforms can be distinguished from vacuum and from one another. Dense interiors (Bondi-like free-fall cavities and radiative envelopes) produce measurable deviations from vacuum in essentially every detectable event. Convective quasi-star interiors are measurable for $\\MBH\\lesssim10^5\\Msun$ and $z\\lesssim0.6$, while a co-rotating disc leaves no measurable imprint. In favorable cases the models are also mutually distinguishable. None of the 14 JWST LRDs at $z>3.9$ would be detectable with a $10\\Msun$ companion, but 30 of 31 LRDs at $z<0.9$ would be if their black holes are $\\sim100$ times less massive than their virial estimates, and in many of them the interior's imprint would be measurable. Across the LRD population to $z=6$, a 4-yr LISA mission would yield $0.08$--$0.8$ detectable events for $10^5\\Msun$ hosts and $10\\Msun$ companions ($1.5$--$15$ for $30\\Msun$) if LRD nuclei host inspirals at the rate of ordinary galactic nuclei. In dense clusters, where captures are plunges, this falls to $\\lesssim10^{-4}$.",
  "abstract_shown": true,
  "affiliations": [],
  "article_type": null,
  "arxiv": "2610.08964",
  "author_total": 4,
  "authors": [
    {
      "name": "Samuel Gómez Gómez"
    },
    {
      "name": "Xisco Jimenez Forteza"
    },
    {
      "name": "Carlos Palenzuela"
    },
    {
      "name": "Rosalba Perna"
    }
  ],
  "bibtex": "https://research.draconitic.com/paper/32mn9yq4nrqd3.bib",
  "cited_by": 0,
  "doi": "10.48550/arxiv.2610.08964",
  "fulltext_url": null,
  "id": "32mn9yq4nrqd3",
  "issns": [],
  "landing_url": "https://arxiv.org/abs/2610.08964",
  "language": null,
  "licence": "LicenseRef-arXiv-nonexclusive-1.0",
  "licence_label": "arXiv licence",
  "licence_source": "article",
  "licence_url": "http://arxiv.org/licenses/nonexclusive-distrib/1.0/",
  "metadata_licence": "CC0-1.0",
  "native_subjects": [
    [
      "arxiv",
      "astro-ph.HE"
    ],
    [
      "arxiv",
      "gr-qc"
    ],
    [
      "openalex",
      "3103|Pulsars and Gravitational Waves Research"
    ]
  ],
  "openalex": "W7221027112",
  "pdf_url": "https://arxiv.org/pdf/2610.08964",
  "pmcid": null,
  "pmid": null,
  "published": "2026-10-06",
  "publisher": null,
  "ris": "https://research.draconitic.com/paper/32mn9yq4nrqd3.ris",
  "sources": [
    {
      "first_seen": "2026-10-30T12:27:37Z",
      "native_id": "2610.08964",
      "source": "arxiv",
      "url": "https://arxiv.org/abs/2610.08964"
    }
  ],
  "subjects": [
    {
      "field": "astronomy",
      "origin": "arxiv:astro-ph.HE",
      "subfield": "high-energy-astrophysics"
    },
    {
      "field": "physics",
      "origin": "arxiv:gr-qc",
      "subfield": "gravitation"
    }
  ],
  "title": "Can LISA See Inside the Little Red Dots?",
  "title_text": "Can LISA See Inside the Little Red Dots?",
  "type": "preprint",
  "updated_at": "2026-10-30T12:27:37Z",
  "url": "https://research.draconitic.com/paper/32mn9yq4nrqd3",
  "venue": "arXiv",
  "versions": []
}