TY - JOUR
T1 - Formation of the first galaxies in the aftermath of the first supernovae
AU - Abe, Makito
AU - Yajima, Hidenobu
AU - Khochfar, Sadegh
AU - Dalla Vecchia, Claudio
AU - Omukai, Kazuyuki
N1 - Funding Information:
This work is financially supported by the Grants-in-Aid for Basic Research by theMinistry of Education, Science and Culture of Japan (HY:17H04827, 20H04724, 21H04489, KO:25287040, 17H01102, 17H02869), National Astronomical Observatory of Japan (NAOJ) ALMA Scientific Research Grant Number 2019-11A, JST FOREST Program, Grant Number JPMJFR202Y (HY). CDV acknowledges support through grants RYC-2015-18078 and PGC2018-094975- C22 from the Spanish Ministry of Science and Innovation.
Publisher Copyright:
© 2021 The Author(s).
PY - 2021/12/1
Y1 - 2021/12/1
N2 - We perform high-resolution cosmological hydrodynamic simulations to study the formation of the first galaxies that reach the masses of 108 - 9 h-1 M at z = 9. The resolution of the simulations is high enough to resolve minihaloes and allow us to successfully pursue the formation of multiple Population (Pop) III stars, their supernova (SN) explosions, resultant metal-enrichment of the inter-galactic medium (IGM) in the course of the build-up of the system. Metals are ejected into the IGM by multiple Pop III SNe, but some of the metal-enriched gas falls back on to the halo after gtrsim 100~\rm Myr$. The star formation history of the first galaxy depends sensitively on the initial mass function (IMF) of Pop III stars. The dominant stellar population transits from Pop III to Pop II at z ∼12-15 in the case of power-law Pop III IMF, dn/dM ≤M-2.35 with the mass range 10-500 M. At z ≤12, stars are stably formed in the first galaxies with a star formation rate of ∼10-3-10-1 M yr -1. In contrast, for the case with a flat IMF, gas-deprived first galaxies form due to frequent Pop III pair-instability SNe, resulting in the suppression of subsequent Pop II star formation. In addition, we calculate UV continuum, Lyα- and Hα-line fluxes from the first galaxies. We show that the James Webb Space Telescope will be able to detect both UV continuum, Lyα and Hα line emission from first galaxies with halo mass ≤109 M at z ≤10.
AB - We perform high-resolution cosmological hydrodynamic simulations to study the formation of the first galaxies that reach the masses of 108 - 9 h-1 M at z = 9. The resolution of the simulations is high enough to resolve minihaloes and allow us to successfully pursue the formation of multiple Population (Pop) III stars, their supernova (SN) explosions, resultant metal-enrichment of the inter-galactic medium (IGM) in the course of the build-up of the system. Metals are ejected into the IGM by multiple Pop III SNe, but some of the metal-enriched gas falls back on to the halo after gtrsim 100~\rm Myr$. The star formation history of the first galaxy depends sensitively on the initial mass function (IMF) of Pop III stars. The dominant stellar population transits from Pop III to Pop II at z ∼12-15 in the case of power-law Pop III IMF, dn/dM ≤M-2.35 with the mass range 10-500 M. At z ≤12, stars are stably formed in the first galaxies with a star formation rate of ∼10-3-10-1 M yr -1. In contrast, for the case with a flat IMF, gas-deprived first galaxies form due to frequent Pop III pair-instability SNe, resulting in the suppression of subsequent Pop II star formation. In addition, we calculate UV continuum, Lyα- and Hα-line fluxes from the first galaxies. We show that the James Webb Space Telescope will be able to detect both UV continuum, Lyα and Hα line emission from first galaxies with halo mass ≤109 M at z ≤10.
KW - galaxies: evolution
KW - galaxies: formation
KW - galaxies: high-redshift
KW - stars: Population III
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U2 - 10.1093/mnras/stab2637
DO - 10.1093/mnras/stab2637
M3 - Article
AN - SCOPUS:85119492197
SN - 0035-8711
VL - 508
SP - 3226
EP - 3238
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 3
ER -