%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 }