VI/146 Galaxies in the Cosmic Dawn II simulation (Ocvirk+, 2020)
Cosmic Dawn II (CoDa II): a new radiation-hydrodynamics simulation of the
self-consistent coupling of galaxy formation and reionization.
Ocvirk P., Aubert D., Sorce J.G., Shapiro P.R., Deparis N., Dawoodbhoy T.,
Lewis J., Teyssier R., Yepes G., Gottloeber S., Ahn K., Iliev I.T.,
Hoffman Y.
<Mon. Not. R. Astron. Soc., 496, 4087-4107 (2020)>
=2020MNRAS.496.4087O 2020MNRAS.496.4087O
=2020yCat.6146....0O 2020yCat.6146....0O
ADC_Keywords: Models ; Clusters, galaxy ; Galaxies
Keywords: radiative transfer - methods: numerical - intergalactic medium -
Local Group - galaxies: formation - galaxies: high redshift
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 40963
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 108M☉. Using the same hybrid
CPU-GPU code RAMSES-CUDATON as CoDa I in Ocvirk et al.
(2016MNRAS.463.1462O 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 ∼2x109M☉,
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.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
halo6.dat 117 4330547 Simulated Galaxy catalogue for z=6
halo7.dat 117 3654273 Simulated Galaxy catalogue for z=7
halo8.dat 117 2879910 Simulated Galaxy catalogue for z=8
halo10.dat 117 1369444 Simulated Galaxy catalogue for z=10
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Byte-by-byte Description of file: halo*.dat
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Bytes Format Units Label Explanations
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1- 12 E12.7 Msun Mhalo Dark matter halo mass of the galaxy
14- 25 E12.7 --- Xpos x position of galaxy in code units (1)
27- 38 E12.7 --- Ypos y position of galaxy in code units (1)
40- 51 E12.7 --- Zpos z position of galaxy in code units (1)
53- 64 E12.7 Msun M* ?=0 Stellar mass of galaxy
66- 77 E12.7 Myr Ageo ?=0 Age of the oldest star
79- 90 E12.7 Myr Agey ?=0 Age of the youngest star
92-104 E13.8 Msun/yr SFR ?=-1 Star Formation rate (2)
105-117 E13.8 mag MAB1600 ?=99 Galaxy's MAB1600 magnitude
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Note (1): Coordinates are in box unit. Multiply by box size (94.44 cMpc)
to obtain comoving coordinates.
Note (2): Computed as the stellar mass formed in the last 10Myr.
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Acknowledgements:
Pierre Ocvirk, pierre.ocvirk(at)astro.unistra.fr
References:
Ocvirk et al., 2016MNRAS.463.1462O 2016MNRAS.463.1462O, CoDa I
(End) Pierre Ocvirk, Patricia Vannier [CDS] 19-May-2020