This study reports a probabilistic insight into the stellar-mass and supernovae (SNe) explosion energy of five CEMP-no stars' possible progenitors. As such, a direct comparison between the abundance ratios [X/Fe] of the light-elements and the predicted nucleosynthetic yields of SN of high-mass metal-free stars has been performed. This comparison suggests that the possible progenitors have a stellar-mass range of 11 − 22 M_⊙ and explosion energies of 0.3 − 1.8 × 10⁵¹ erg. In addition, we investigate the kinematic signatures, derived from Gaia DR2, to conclude that these five CEMP-no stars have halo-like kinematic and do not enter the outer-halo region. In addition, we link the abundance patterns with kinematic signatures to investigate the Gaia-Sausage and Gaia-Sequoia memberships. This chemo-dynamical analysis suggests that these CEMP-no stars are neither Gaia-Sausage nor Gaia-Sequoia remnant stars, but another accretion event might be responsible for the contribution of these stars to the Galactic Halo.

中文翻译：

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用自动行星探测器望远镜观察到的贫金属恒星。三、CEMP-无星是星族III星的后代

这项研究报告了对五颗 CEMP 恒星的可能祖先的恒星质量和超新星 (SNe) 爆炸能量的概率洞察。因此，已经对轻元素的丰度比 [X/Fe] 与大质量无金属恒星的 SN 的预测核合成产率进行了直接比较。这种比较表明，可能的前身星的恒星质量范围为 11 − 22 M _⊙，爆炸能量为 0.3 − 1.8 × 10 ⁵¹  erg。此外，我们研究了源自Gaia DR2的运动学特征，得出的结论是这五颗 CEMP-no 恒星具有类似晕的运动学，并且没有进入外晕区。此外，我们将丰度模式与运动学特征联系起来，以研究盖亚-香肠和盖亚 -红杉会员。这种化学动力学分析表明，这些 CEMP-no 恒星既不是Gaia- Sausage 也不是Gaia- Sequoia 残余恒星，但另一个吸积事件可能是这些恒星对银河晕的贡献的原因。