The stellar Initial Mass Function (IMF) seems to be close to universal in the local star‐forming regions. However, this quantity of a newborn stellar population responds differently at gas metallicities Z ∼ Z_⊙ than Z = 0. A view on the cosmic star formation history suggests that the cooling agents in the gas vary both in their types and molecular abundances. For instance, in the primordial gas environment, the gas temperature can be higher by a factor of 30 as compared to the present day. Stellar radiation feedback and cosmic microwave background (CMB) radiation may even contribute toward increasing the floor temperature of the star‐forming gas which subsequently can leave profound impacts on the IMF. We present the contribution of the radiation sources toward the thermodynamical evolution of the Jeans unstable gas cloud which experiences fragmentation and mass accretion. We find evidence which suggests that the latter becomes the dominant process for star formation efficiencies (SFE) above 5–7%, thus increasing the average mass of the stars. We focus on the isolated and binary stellar configurations emerging during the gas collapse. The binary fraction on average remains 0.476 and contributes significantly toward the total SFE of 15%.

中文翻译：

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一系列红移中的恒星初始质量函数

恒星的初始质量函数（IMF）在本地恒星形成区域似乎已接近普遍。然而，新生恒星群的这个量在气体金属丰的反应不同ž  〜 Z ^ _⊙比ž =0。对宇宙恒星形成历史的看法表明，气体中的冷却剂的类型和分子丰度都不同。例如，在原始气体环境中，气体温度与当前相比可能高出30倍。恒星辐射反馈和宇宙微波背景（CMB）辐射甚至可能会导致形成恒星的气体的底面温度升高，从而对IMF产生深远影响。我们介绍了辐射源对Jeans不稳定气体云的热力学演化的贡献，该气体经历了碎片和质量积聚。我们发现证据表明，后者成为5-7％以上的恒星形成效率（SFE）的主要过程，从而增加了恒星的平均质量。我们着眼于气体崩塌过程中出现的孤立和二元恒星构型。二元分数平均仍为0.476，对总SFE的15％贡献显着。