并非那么重金属 I：低金属丰度增强高红移超亮超新星的发生率
Not So Heavy Metal I: Low Metallicity Enhances the Rate of high-redshift Superluminous Supernovae
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中文总结 AI 辅助
本研究提出新理论框架，结合金属丰度标度关系与恒星质量分布，预测低金属丰度使高红移超亮超新星发生率提升近一个数量级，影响未来巡天探测。
中文摘要 AI 辅助
I型超亮超新星（SLSNe）是极其明亮的恒星爆炸，源于大质量恒星的核心坍缩。然而，与普通的核心坍缩超新星不同，超亮超新星几乎只出现在金属贫乏的环境中。因此，它们的体积发生率不应简单地追踪宇宙恒星形成历史，而应随着宇宙时间中星系的金属丰度分布而演化。在这项工作中，我们引入了一个新的理论框架，用于建模天体物理源的体积发生率作为红移和金属丰度的函数。我们的形式体系结合了金属丰度标度关系、恒星质量分布函数以及依赖金属丰度的产生效率。重要的是，它还区分了基于O/H和Fe/H丰度的金属丰度度量。将我们的新形式体系应用于超亮超新星，我们预测在$z \gtrsim 2$处的体积发生率比仅追踪宇宙恒星形成率的模型高出近一个数量级。这对使用Vera C. Rubin天文台及其他时域巡天探测高红移超亮超新星的前景有直接影响。
英文摘要
Type-I superluminous supernovae (SLSNe) are extremely luminous stellar explosions originating from the core collapse of massive stars. Unlike normal core-collapse supernovae, however, SLSNe occur almost exclusively in metal-poor environments. As a result, their volumetric rate should not simply trace the cosmic star-formation history, but instead evolve with the metallicity distribution of galaxies across cosmic time. In this work, we introduce a new theoretical framework for modeling the volumetric rate of astrophysical sources as a function of redshift and metallicity. Our formalism combines metallicity scaling relations, stellar-mass distribution functions, and metallicity-dependent production efficiencies. Importantly, it also distinguishes between metallicity measures based on O/H and Fe/H abundances. Applying our new formalism to SLSNe, we predict volumetric rates that are nearly an order of magnitude higher at $z \gtrsim 2$ compared to models in which the rate traces the cosmic star-formation rate alone. This has direct implications on the detection prospects of high-$z$ SLSNe with the Vera C. Rubin Observatory and other time-domain surveys.
发表机构
- University of Minnesota（明尼苏达大学）
- Northwestern University（西北大学）
- Weizmann Institute of Science（魏茨曼科学研究所）
机构由 AI 辅助整理，请以论文原文为准。
