CONCERTO: High-fidelity simulation of millimeter line emissions of galaxies and [CII] intensity mapping

Authors:
  • MBM. Bethermin
    M. Bethermin
  • AGA. Gkogkou
    A. Gkogkou
  • MCM. Van Cuyck
    M. Van Cuyck
  • GLG. Lagache
    G. Lagache
  • ABA. Beelen
    A. Beelen
Open Access
Publisher website
Google Scholar
Abstract
The intensity mapping of the [CII] 158-μm line redshifted to the submillimeter window is a promising probe of the z > 4 star formation and its spatial distribution into large-scale structures. To prepare the first-generation experiments (e.g., CONCERTO), we need realistic simulations of the submillimeter extragalactic sky in spectroscopy. We present a new version of the simulated infrared dusty extragalactic sky (SIDES) model including the main submillimeter lines around 1 mm (CO, [CII], [CI]). This approach successfully reproduces the observed line luminosity functions. We then use our simulation to generate CONCERTO-like cubes (125–305 GHz) and forecast the power spectra of the fluctuations caused by the various astrophysical components at those frequencies. Depending on our assumptions on the relation between the star formation rate and [CII] luminosity, and the star formation history, our predictions of the z ∼ 6 [CII] power spectrum vary by two orders of magnitude. This highlights how uncertain the predictions are and how important future measurements will be to improve our understanding of this early epoch. SIDES can reproduce the CO shot noise recently measured at ∼100 GHz by the millimeter-wavelength intensity mapping experiment (mmIME). Finally, we compare the contribution of the different astrophysical components at various redshifts to the power spectra. The continuum is by far the brightest, by a factor of three to 100, depending on the frequency. At 300 GHz, the CO foreground power spectrum is higher than the [CII] one for our base scenario. At lower frequencies, the contrast between [CII] and extragalactic foregrounds is even worse. Masking the known galaxies from deep surveys should allow us to reduce the foregrounds to 20% of the [CII] power spectrum up to z ∼ 6.5. However, this masking method will not be sufficient at higher redshifts. The code and the products of our simulation are released publicly, and can be used for both intensity mapping experiments and submillimeter continuum and line surveys.
Funding Information
  • ERC (788212, H2020/740120)
  • Aix-Marseille University-A*Midex
  • FONDECYT (1211951)

This publication has 160 references indexed in Scilit: