{
  "id": "2204.01649",
  "version": "v1",
  "published": "2022-04-04T16:55:44.000Z",
  "updated": "2022-04-04T16:55:44.000Z",
  "title": "Cosmic star formation history with tomographic CIB-galaxy cross-correlation",
  "authors": [
    "Ziang Yan",
    "Ludovic van Waerbeke",
    "Angus H. Wright",
    "Maciej Bilicki",
    "Shiming Gu",
    "Hendrik Hildebrandt",
    "Abhishek S. Maniyar",
    "Tilman Tröster"
  ],
  "comment": "22 pages, 14 figures, 3 tables, the abstract is abridged",
  "categories": [
    "astro-ph.GA",
    "astro-ph.CO"
  ],
  "abstract": "In this work, we probe the star formation history of the Universe using tomographic cross-correlation between the cosmic infrared background (CIB) and galaxy samples. The galaxy samples are from the Kilo-Degree Survey (KiDS), while the CIB maps are made from \\planck\\, sky maps. We measure the cross-correlation in harmonic space with a significance of 43$\\sigma$. We model the cross-correlation with a halo model, which links CIB anisotropies to star formation rates (SFR) and galaxy abundance. We assume that SFR has a lognormal dependence on halo mass, while galaxy abundance follows the halo occupation distribution (HOD) model. The cross-correlations give a best-fit maximum star formation efficiency of $\\eta_{\\mathrm{max}}= 0.41^{+0.09}_{-0.14}$ at a halo mass $\\log_{10}(M_{\\mathrm{peak}}/M_{\\odot})= {12.14\\pm 0.36}$. The derived star formation rate density (SFRD) is well constrained up to $z\\sim 1.5$. The constraining power at high redshift is mainly limited by the KiDS survey depth. A combination with external SFRD measurements from previous studies gives $\\log_{10}(M_{\\mathrm{peak}}/M_{\\odot})=12.42^{+0.35}_{-0.19}$. This tightens the SFRD constraint up to $z=4$, yielding a peak SFRD of $0.09_{-0.004}^{+0.003}\\,M_{\\odot} \\mathrm { year }^{-1} \\mathrm{Mpc}^{-3}$ at $z=1.74^{+0.06}_{-0.02}$, corresponding to a lookback time of $10.05^{+0.12}_{-0.03}$ Gyr. Both constraints are consistent, and the derived SFRD agrees with previous studies and simulations. Additionally, we estimate the galaxy bias $b$ of KiDS galaxies from the constrained HOD parameters and yield an increasing bias from $b=1.1_{-0.31}^{+0.17}$ at $z=0$ to $b=1.96_{-0.64}^{+0.18}$ at $z=1.5$. Finally, we provide a forecast for future galaxy surveys and conclude that, due to their considerable depth, future surveys will yield a much tighter constraint on the evolution of the SFRD.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2022-04-04T16:55:44.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "cosmic star formation history",
      "tomographic cib-galaxy cross-correlation",
      "star formation rate density",
      "best-fit maximum star formation efficiency"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 22,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}