A multivariate approach to decode star formation histories from galaxy spectra.

河外天体物理学的一个重要方面是确定星系过去的恒星形成历史。这使我们能够追溯星系的形成过程，了解星系是如何与内在属性--如质量或大小--或与它们所处的环境有关的。这个博士项目的重点是改进传统技术，目的是从星系光谱中提取吸收线指标，这取决于潜在的、未分解的恒星群体的年龄和金属丰度分布。该方法涉及新的多变量技术，可以从大量数据(通常是从数千个星系光谱)中最佳地提取信息。除了恒星数量的标准测量之外，这种及时的扩展将侧重于NUV光谱范围，结合光学信息，这将使我们能够解开恒星形成历史不同阶段的贡献。近紫外光特别重要，因为非常遥远的高红移星系，只有在它们的光谱近紫外光静止框架中才能被详细观察到。

One of the key aspects of extragalactic astrophysics involves the determination of the past star formation history of galaxies. Thisallows us to backtrack the formation process, to understand how galaxies form in relation to intrinsic properties -- such as mass orsize -- or to the environment where they live. This PhD project focuses on improving over traditional techniques aimed at extractingabsorption line indicators from galaxy spectra, which are dependent on the age and metallicity distribution of the underlying, unresolvedstellar populations. The methodology involves new multi-variate techniques that optimally extract information from a large volume ofdata (typically from thousands of galaxy spectra). This timely extension beyond standard measurements of stellar populations willemphasize on the NUV spectral range, which -- in combination with optical information -- will enable us to disentangle the contributionsfrom different stages of the star formation history. The NUV is especially important as very distant, high redshift galaxies, can onlybe observed in detail in their spectral NUV rest frame.