论文标题
Forever22：RedShifts $ Z \ Simeq 10-20 $的第一个具有人口III星的明亮星系，并与JWST数据进行比较
FOREVER22: the first bright galaxies with population III stars at redshifts $z \simeq 10-20$ and comparisons with JWST data
论文作者
论文摘要
我们研究了由SSA22（Forever22）模拟项目激励的极度密度区域中星系的形成和演化建模的过度密度区域中第一个星系的形成。我们的模拟成功地重现了星形构成率，$ m _ {\ rm UV} -M _ {\ rm star} $ $ z \ sim 10-14 $ james Webb Space Telescope（JWST）观察到的候选星系的关系10-14 $。我们建议观察到的星系由带有$ M _ {\ rm H} \ gtrsim 10^{10}〜{\ rm m _ {\ odot}} $的黑色halo托管，并处于短期period starburst阶段。另一方面，即使是过度密度区域中的模拟大型星系也无法再现$ z \ sim 16 $的强烈恒星形成率和大量观察到的候选人。另外，我们表明，随着恒星质量的增加，人口III恒星对UV通量的贡献减小，对于具有$ M _ {\ rm star} \ sim 10^{7}〜{\ rm m _ {\ rm m _ {\ rm m _ {\ odot}} $的星系的百分之几。因此，JWST观察到的一部分通量可能是人口III星的光。 Our simulations suggest that the UV flux can be dominated by population III stars and the UV-slope shows $β\lesssim -3$ if future observations would reach galaxies with $M_{\rm stars} \sim 10^{5}~{\rm M_{\odot}}$ at $z \sim 20$ of which the mass fraction of population III stars can be greater than 10百分比。
We study the formation of the first galaxies in overdense regions modelled by the FORmation and EVolution of galaxies in Extremely overdense Regions motivated by SSA22 (FOREVER22) simulation project. Our simulations successfully reproduce the star formation rates and the $M_{\rm UV}-M_{\rm star}$ relations of candidate galaxies at $z \sim 10-14$ observed by the James Webb Space Telescope (JWST). We suggest that the observed galaxies are hosted by dark-matter haloes with $M_{\rm h} \gtrsim 10^{10}~{\rm M_{\odot}}$ and are in short-period starburst phases. On the other hand, even simulated massive galaxies in overdense regions cannot reproduce the intense star formation rates and the large stellar masses of observed candidates at $z \sim 16$. Also, we show that the contribution of population III stars to the UV flux decreases as the stellar mass increases and it is a few percent for galaxies with $M_{\rm star} \sim 10^{7}~{\rm M_{\odot}}$. Therefore, a part of the observed flux by JWST could be the light from population III stars. Our simulations suggest that the UV flux can be dominated by population III stars and the UV-slope shows $β\lesssim -3$ if future observations would reach galaxies with $M_{\rm stars} \sim 10^{5}~{\rm M_{\odot}}$ at $z \sim 20$ of which the mass fraction of population III stars can be greater than 10 percent.
