{
  "id": "2502.03532",
  "version": "v1",
  "published": "2025-02-05T19:00:03.000Z",
  "updated": "2025-02-05T19:00:03.000Z",
  "title": "COSMOS-Web: The emergence of the Hubble Sequence",
  "authors": [
    "M. Huertas-Company",
    "M. Shuntov",
    "Y. Dong",
    "M. Walmsley",
    "O. Ilbert",
    "H. J. McCracken",
    "H. B. Akins",
    "N. Allen",
    "C. M. Casey",
    "L. Costantin",
    "E. Daddi",
    "A. Dekel",
    "M. Franco",
    "I. L. Garland",
    "T. Géron",
    "G. Gozaliasl",
    "M. Hirschmann",
    "J. S. Kartaltepe",
    "A. M. Koekemoer",
    "C. Lintott",
    "D. Liu",
    "R. Lucas",
    "K. Masters",
    "F. Pacucci",
    "L. Paquereau",
    "P. G. P'erez-Gonz'alez",
    "J. D. Rhodes",
    "B. E. Robertson",
    "B. Simmons",
    "R. Smethurst",
    "S. Toft",
    "L. Yang"
  ],
  "comment": "subnmitted to A&A. Comments Welcome",
  "categories": [
    "astro-ph.GA",
    "astro-ph.CO"
  ],
  "abstract": "Leveraging the wide area coverage of the COSMOS-Web survey, we quantify the abundance of different morphological types from $z\\sim 7$ with unprecedented statistics and establish robust constraints on the epoch of emergence of the Hubble sequence. We measure the global (spheroids, disk-dominated, bulge-dominated, peculiar) and resolved (stellar bars) morphologies for about 400,000 galaxies down to F150W=27 using deep learning, representing a two-orders-of-magnitude increase over previous studies. We then provide reference Stellar Mass Functions (SMFs) of different morphologies between $z\\sim 0.2$ and $z\\sim 7$ and best-fit parameters to inform models of galaxy formation. All catalogs and data are made publicly available. (a)At redshift z > 4.5, the massive galaxy population ($\\log M_*/M_\\odot>10$) is dominated by disturbed morphologies (~70%) -- even in the optical rest frame -- and very compact objects (~30%) with effective radii smaller than ~500pc. This confirms that a significant fraction of the star formation at cosmic dawn occurs in very dense regions, although the stellar mass for these systems could be overestimated.(b)Galaxies with Hubble-type morphologies -- including bulge and disk-dominated galaxies -- arose rapidly around $z\\sim 4$ and dominate the morphological diversity of massive galaxies as early as $z\\sim 3$. (c)Using stellar bars as a proxy, we speculate that stellar disks in massive galaxies might have been common (>50%) among the star-forming population since cosmic noon ($z\\sim2$-2.5) and formed as early as $z\\sim 7$ (d)Massive quenched galaxies are predominantly bulge-dominated from z~4 onward, suggesting that morphological transformations briefly precede or are simultaneous to quenching mechanisms at the high-mass end. (e) Low-mass ($\\log M_*/M_\\odot<10$) quenched galaxies are typically disk-dominated, pointing to different quenching routes in the two ends of the stellar mass spectrum from cosmic dawn.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2025-02-05T19:00:03.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "hubble sequence",
      "massive galaxy",
      "cosmos-web",
      "morphologies",
      "reference stellar mass functions"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 0,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}