Massive Population III stars can die as energetic supernovae that enrich the early Universe with metals and determine the properties of the first galaxies. With masses of about 109 M ⊙ at z ≳ 10, these galaxies are believed to be the ancestors of the Milky Way. This paper investigates the impact of Population III supernova remnants (SNRs) from both Salpeter-like and top-heavy initial mass functions (IMFs) on the formation of first galaxies with high-resolution radiation-hydrodynamical simulations with the ENZO code. Our findings indicate that SNRs from a top-heavy Population III IMF produce more metals, leading to more efficient gas cooling and earlier Population II star formation in the first galaxies. From a few hundred to a few thousand Population II stars can form in the central regions of these galaxies. These stars have metallicities of 10−3–10−2, Z ⊙, greater than those of extremely metal-poor (EMP) stars. Their mass function follows a power-law distribution with , where M * is stellar mass, and α = 2.66–5.83 and is steeper for a top-heavy IMF. We thus find that EMP stars were not typical of most primitive galaxies.
Description
How Population III Supernovae Determined the Properties of the First Galaxies - IOPscience
%0 Journal Article
%1 chen2024population
%A Chen, Ke-Jung
%A Tang, Ching-Yao
%A Whalen, Daniel J.
%A Ho, Meng-Yuan
%A Tsai, Sung-Han
%A Ou, Po-Sheng
%A Ono, Masaomi
%D 2024
%I The American Astronomical Society
%J The Astrophysical Journal
%K astronomy galaxy population_iii supernovae
%N 1
%P 91
%R 10.3847/1538-4357/ad2684
%T How Population III Supernovae Determined the Properties of the First Galaxies
%U https://dx.doi.org/10.3847/1538-4357/ad2684
%V 964
%X Massive Population III stars can die as energetic supernovae that enrich the early Universe with metals and determine the properties of the first galaxies. With masses of about 109 M ⊙ at z ≳ 10, these galaxies are believed to be the ancestors of the Milky Way. This paper investigates the impact of Population III supernova remnants (SNRs) from both Salpeter-like and top-heavy initial mass functions (IMFs) on the formation of first galaxies with high-resolution radiation-hydrodynamical simulations with the ENZO code. Our findings indicate that SNRs from a top-heavy Population III IMF produce more metals, leading to more efficient gas cooling and earlier Population II star formation in the first galaxies. From a few hundred to a few thousand Population II stars can form in the central regions of these galaxies. These stars have metallicities of 10−3–10−2, Z ⊙, greater than those of extremely metal-poor (EMP) stars. Their mass function follows a power-law distribution with , where M * is stellar mass, and α = 2.66–5.83 and is steeper for a top-heavy IMF. We thus find that EMP stars were not typical of most primitive galaxies.
@article{chen2024population,
abstract = {Massive Population III stars can die as energetic supernovae that enrich the early Universe with metals and determine the properties of the first galaxies. With masses of about 109 M ⊙ at z ≳ 10, these galaxies are believed to be the ancestors of the Milky Way. This paper investigates the impact of Population III supernova remnants (SNRs) from both Salpeter-like and top-heavy initial mass functions (IMFs) on the formation of first galaxies with high-resolution radiation-hydrodynamical simulations with the ENZO code. Our findings indicate that SNRs from a top-heavy Population III IMF produce more metals, leading to more efficient gas cooling and earlier Population II star formation in the first galaxies. From a few hundred to a few thousand Population II stars can form in the central regions of these galaxies. These stars have metallicities of 10−3–10−2, Z ⊙, greater than those of extremely metal-poor (EMP) stars. Their mass function follows a power-law distribution with , where M * is stellar mass, and α = 2.66–5.83 and is steeper for a top-heavy IMF. We thus find that EMP stars were not typical of most primitive galaxies.},
added-at = {2024-03-24T09:46:21.000+0100},
author = {Chen, Ke-Jung and Tang, Ching-Yao and Whalen, Daniel J. and Ho, Meng-Yuan and Tsai, Sung-Han and Ou, Po-Sheng and Ono, Masaomi},
biburl = {https://www.bibsonomy.org/bibtex/23604de5f05487314d370a06e0a5d1ae5/tabularii},
description = {How Population III Supernovae Determined the Properties of the First Galaxies - IOPscience},
doi = {10.3847/1538-4357/ad2684},
interhash = {aaae16339d19ce3c9d18de62a9032103},
intrahash = {3604de5f05487314d370a06e0a5d1ae5},
journal = {The Astrophysical Journal},
keywords = {astronomy galaxy population_iii supernovae},
month = mar,
number = 1,
pages = 91,
publisher = {The American Astronomical Society},
timestamp = {2024-03-24T09:46:21.000+0100},
title = {How Population III Supernovae Determined the Properties of the First Galaxies},
url = {https://dx.doi.org/10.3847/1538-4357/ad2684},
volume = 964,
year = 2024
}