Binary Population and Spectral Synthesis Version 2.1: Construction, Observational Verification, and New Results
Binary Population and Spectral Synthesis Version 2.1: Construction, Observational Verification, and New Results
复制标题
DOI：
10.1017/pasa.2017.51
复制
发表时间：
2017-11-16
影响因子：
6.3
通讯作者：
Bray, J. C.
中科院分区：
文献类型：
--
作者：
Eldridge, J. J.;Stanway, E. R.;Bray, J. C.
双星群体和光谱合成套件双星演化模型和合成恒星群体提供了一个框架，用于对来自遥远恒星群体的综合光和附近恒星群体的详细特性进行物理动机分析。我们提出了一个新的版本2.1数据发布这些模型，详细介绍了方法，其中二进制人口和光谱合成结合二进制质量转移及其对恒星演化途径的影响。以及简单恒星种群的构建。我们展示了最新的二进制人口和光谱合成模型套件的关键测试，展示了其再现解决恒星人口的颜色和衍生特性的能力，包括良好约束的食双星。我们考虑了观测约束的比例大质量星星类型和恒星残余质量的分布。我们描述了我们的模型中的超新星祖先的识别，并表现出良好的协议所观察到的祖先的属性。我们还测试我们的模型对光度和光谱观测未解决的恒星种群，无论是在本地和遥远的宇宙。发现二进制模型提供了一个自洽的解释观测星系的性质在一个广泛的红移范围。最后，我们仔细描述了我们的模型的局限性。以及我们希望在未来版本中看到重大改进的领域。
The Binary Population and Spectral Synthesis suite of binary stellar evolution models and synthetic stellar populations provides a framework for the physically motivated analysis of both the integrated light from distant stellar populations and the detailed properties of those nearby. We present a new version 2.1 data release of these models, detailing the methodology by which Binary Population and Spectral Synthesis incorporates binary mass transfer and its effect on stellar evolution pathways. as well as the construction of simple stellar populations. We demonstrate key tests of the latest Binary Population and Spectral Synthesis model suite demonstrating its ability to reproduce the colours and derived properties of resolved stellar populations, including well-constrained eclipsing binaries. We consider observational constraints on the ratio of massive star types and the distribution of stellar remnant masses. We describe the identification of supernova progenitors in our models, and demonstrate a good agreement to the properties of observed progenitors. We also test our models against photometric and spectroscopic observations of unresolved stellar populations, both in the local and distant Universe. finding that binary models provide a self-consistent explanation for observed galaxy properties across a broad redshift range. Finally, we carefully describe the limitations of our models. and areas where we expect to see significant improvement in future versions.