量化元素重要性以从III型超新星产率拟合中恢复质量
Quantifying Element Importance for Mass Recovery from Population III Supernova Yield Fits
AI总结：
研究通过分析元素对恢复恒星初始质量的影响，确定关键元素及产率模型的精度限制，为III型恒星初始质量函数提供实用约束。
摘要：
目前尚无观测到的III型恒星，但可通过恒星考古学推断其初始质量函数（IMF）：通过拟合核心坍缩超新星产率模型到低质量、长寿命、金属贫乏恒星的元素丰度。尽管先前研究显示产率拟合可恢复前体属性，但尚不清楚哪些测量元素最影响质量恢复质量，以及给定元素集合能实现的IMF精度水平。我们进行了系统研究，使用Heger & Woosley (2010)产率网格生成模拟观测，拟合初始质量，并评估分数质量恢复的典型性能。通过添加/移除单个元素实验和不同基线元素集的比较，对元素重要性进行排名。我们发现，对准确质量恢复最重要的元素是C、N、Na和K，当可用时O、Al、Co和Ni也持续提高性能。总体而言，使用目前可测量的高分辨率光谱学元素，恒星考古学可在核心坍缩超新星产率模型良好代表早期宇宙恒星演化的假设下，提供实用的III型恒星IMF约束。
英文摘要：
Massive Population III stars are currently not observed, but their initial mass function (IMF) can be inferred through stellar archaeology: fitting core-collapse supernova yield models to elemental abundances of low-mass, long-lived metal-poor stars. While prior work demonstrates that yield fitting can recover progenitor properties, it remains unclear which measured elements most control mass recovery quality and what level of IMF precision is achievable for a measured element set. We perform a systematic study of element importance for progenitor mass recovery. Using the Heger & Woosley (2010) yield grid, we generate mock observations, fit the initial mass, and evaluate the typical performance on the fractional mass recovery. Add/remove-one-element experiments and comparisons among different baseline element sets are used to rank elements by importance. We find that the most important elements for accurate mass recovery are C, N, Na, and K, with O, Al, Co, and Ni consistently improving performance when available. Overall, with currently measurable elements from high-resolution spectroscopy, stellar archaeology can deliver practical Population III IMF constraints assuming the core-collapse supernova yield models provide a good representation of stellar evolution in the early universe.
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