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The frequency by mass of Galactic carbon stars inferred from Gaia measurements of star cluster members
Monthly Notices of the Royal Astronomical Society ( IF 4.8 ) Pub Date : 2021-07-09 , DOI: 10.1093/mnras/stab1967
Tathagata Pal 1 , G Worthey 1
Affiliation  

We investigate the frequency of occurrence of Galactic carbon stars as a function of progenitor mass using Gaia data. Small number statistics limit fidelity, but C-star frequency agrees with that observed in the Magellanic Clouds (MCs) down to m ≈ 1.67 M⊙. At m ≈ 1.38 M⊙, the frequency rises by a factor of three even though the frequency appears to drop to zero for the MCs. In fact this is due to a lack of clusters at the key age range in the MCs. At m ≈ 1.24 M⊙ and below, no C-stars are observed, corresponding to ages older than 4 Gyr. Within uncertainties, C-star frequency in M 31 is consistent with that of the Galaxy and the MCs. We find an ambiguous C-star candidate at ∼7 M⊙.

中文翻译:

从星团成员的盖亚测量中推断出银河碳星的质量频率

我们使用 Gaia 数据研究银河碳星的出现频率与前身质量的关系。小数字统计限制了保真度,但 C 星频率与在麦哲伦云 (MC) 中观测到的一致,低至 m ≈ 1.67 M⊙。在 m ≈ 1.38 M⊙ 时,频率上升了三倍,尽管 MC 的频率似乎下降到零。事实上,这是由于 MC 的关键年龄范围内缺乏集群。在 m ≈ 1.24 M⊙ 及以下,没有观测到 C 星,对应的年龄超过 4 Gyr。在不确定性范围内,M 31 中的 C 星频率与银河系和 MC 的频率一致。我们在 ∼7 M⊙ 处发现了一个模棱两可的 C 星候选者。
更新日期:2021-07-09
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