{
  "abstract": "Millimeter-wave line intensity mapping aims to observe the high-redshift universe through the 158 $μ$m fine-structure line of [C II], the brightest far-infrared line of star-forming galaxies. Whether a [C II] experiment at $z>4$ measures the clustering of large-scale structure, which carries rich cosmological information, rather than the shot noise of the emitters depends on the amplitude and the shape of the [C II] power spectrum. Forecasts often build the power spectrum from a halo mass--luminosity relation, $L(M_h)$, chained from scaling relations measured in other regimes or read off simulations, without a quantified uncertainty. We instead calibrate a double power-law $L(M_h,z)$ on [C II] data alone: the mean [C II] intensity from tomographic cross-correlation at $0.4<z<4.2$ and the luminosity-function measurements and limits at $z\\simeq0$ and $4.3\\lesssim z\\lesssim8$. The four parameters of the double power law are fitted at $z=4.5$ and $5.5$ separately, with no assumption about their evolution, and then jointly across $0<z<7$, and we examine how the uncertainty depends on the modeling assumptions. The shape of the power spectrum is settled by the existing data. The clustering peak stands a factor of $45\\,(23$-$93)$ and $64\\,(38$-$112)$ above the shot-noise floor at $z=4.5$ and $5.5$, and the two cross at $k_c\\simeq0.37$ and $0.44\\,h$Mpc$^{-1}$. The amplitude is known less well, the clustering power to $0.5-0.6$ dex and the shot noise to $0.7-0.9$ dex. The results show that the signal comes from halos accessible by current galaxy surveys, those that host the Lyman-break galaxies and Ly$α$ emitters at these redshifts. The luminosity-weighted bias is relatively high, with values of $4-5$.",
  "abstract_shown": true,
  "affiliations": [],
  "article_type": null,
  "arxiv": "2610.40550",
  "author_total": 2,
  "authors": [
    {
      "name": "Oliver Jeong"
    },
    {
      "name": "Martin White"
    }
  ],
  "bibtex": "https://research.draconitic.com/paper/7tpf4r72m5ar0.bib",
  "cited_by": 0,
  "doi": "10.48550/arxiv.2610.40550",
  "fulltext_url": null,
  "id": "7tpf4r72m5ar0",
  "issns": [],
  "landing_url": "https://arxiv.org/abs/2610.40550",
  "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.CO"
    ],
    [
      "arxiv",
      "astro-ph.GA"
    ]
  ],
  "openalex": null,
  "pdf_url": "https://arxiv.org/pdf/2610.40550",
  "pmcid": null,
  "pmid": null,
  "published": "2026-10-29",
  "publisher": null,
  "ris": "https://research.draconitic.com/paper/7tpf4r72m5ar0.ris",
  "sources": [
    {
      "first_seen": "2026-10-30T12:36:28Z",
      "native_id": "2610.40550",
      "source": "arxiv",
      "url": "https://arxiv.org/abs/2610.40550"
    }
  ],
  "subjects": [
    {
      "field": "astronomy",
      "origin": "arxiv:astro-ph.CO",
      "subfield": "cosmology"
    },
    {
      "field": "astronomy",
      "origin": "arxiv:astro-ph.GA",
      "subfield": "galaxies"
    }
  ],
  "title": "An Empirically Calibrated [C II] Luminosity-Halo Mass Relation for Line Intensity Mapping",
  "title_text": "An Empirically Calibrated [C II] Luminosity-Halo Mass Relation for Line Intensity Mapping",
  "type": "preprint",
  "updated_at": "2026-11-01T12:20:47Z",
  "url": "https://research.draconitic.com/paper/7tpf4r72m5ar0",
  "venue": "arXiv",
  "versions": []
}