Galaxies in the Cosmic Dawn II simulation Virtual Observatory Resource

Authors
  1. Ocvirk P.
  2. Aubert D.
  3. Sorce J.G.
  4. Shapiro P.R.
  5. Deparis N.
  6. Dawoodbhoy T.,Lewis J.
  7. Teyssier R.
  8. Yepes G.
  9. Gottloeber S.
  10. Ahn K.
  11. Iliev I.T.,Hoffman Y.
  12. Published by
    CDS
Abstract

Cosmic Dawn II (CoDa II) is a new, fully-coupled radiation-hydrodynamics simulation of cosmic reionization and galaxy formation and their mutual impact, to redshift z<6. With 4096^3^ particles and cells in a 94Mpc box, it is large enough to model global reionization and its feedback on galaxy formation while resolving all haloes above 10^8^M_{sun}_. Using the same hybrid CPU-GPU code RAMSES-CUDATON as CoDa I in Ocvirk et al. (2016MNRAS.463.1462O), CoDa II modified and re-calibrated the subgrid star-formation algorithm, making reionization end earlier, at z>~6, thereby better matching the observations of intergalactic Lyman-alpha opacity from quasar spectra and electron-scattering optical depth from cosmic microwave background fluctuations. CoDa II predicts a UV continuum luminosity function in good agreement with observations of high-z galaxies, especially at z=6. As in CoDa I, reionization feedback suppresses star formation in haloes below ~2x10^9^M_{sun}_, though suppression here is less severe, a possible consequence of modifying the star-formation algorithm. Suppression is environment-dependent, occurring earlier (later) in overdense (underdense) regions, in response to their local reionization times. Using a constrained realization of {LAMBDA}CDM constructed from galaxy survey data to reproduce the large-scale structure and major objects of the present-day Local Universe, CoDa II serves to model both global and local reionization. In CoDa II, the Milky Way and M31 appear as individual islands of reionization, i.e. they were not reionized by the progenitor of the Virgo cluster, nor by nearby groups, nor by each other. Description: The galaxy catalogs for redshifts z=10 down to z=6 (the simulation ended at z=5.8) are provided. Galaxies are identified as Friends-of-Friends dark matter haloes with a linking length ll=0.2. Stars are associated to each halo if they are within a sphere of radius r200. Magnitudes are computed using a BPASS stellar population model, as detailed in the article. No dust opacity is considered.

Keywords
  1. Astronomical models
  2. Galaxy clusters
  3. Galaxies
Bibliographic source Bibcode
2020MNRAS.496.4087O
See also HTML
https://cdsarc.cds.unistra.fr/viz-bin/cat/VI/146
IVOA Identifier IVOID
ivo://CDS.VizieR/VI/146
Document Object Identifer DOI
bibcode:2020yCat.6146....0O

Access

Web browser access HTML
http://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=VI/146
https://vizier.iucaa.in/viz-bin/VizieR-2?-source=VI/146
http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=VI/146
IVOA Table Access TAP
http://tapvizier.cds.unistra.fr/TAPVizieR/tap
Run SQL-like queries with TAP-enabled clients (e.g., TOPCAT).

History

2020-09-03T13:33:10Z
Resource record created
2020-09-03T13:33:10Z
Created
2021-03-23T12:19:09Z
Updated

Contact

Name
CDS support team
Postal Address
CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France
E-Mail
cds-question@unistra.fr