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Resolved stellar populations in nearby galaxies

解决了附近星系中的恒星种群问题

基本信息

批准号：
2567276
负责人：
金额：
--
依托单位：
Durham University
依托单位国家：
英国
项目类别：
Studentship
财政年份：
2021
资助国家：
英国
起止时间：
2021 至无数据
项目状态：
已结题

来源：
https://gtr.ukri.org/projects?ref=studentship-2567276
关键词：
Resolved stellar populations nearby galaxies

项目摘要

The lifecycle of star-forming galaxies is very complex: cold gas is turned into stars; the formed stellar populations stir, mix, enrich, heat, and expel the gas via stellar winds, radiation, and supernova explosions; the gas can then fall back onto the galaxy, cool, and form new generations of stars. While we qualitatively understand the involved physical processes governing the gas recycle, we still do not have a clear quantitative description of them. As a consequence, constraining how galaxies turn their gas into stars, how feedback from these stars disrupts gas and regulates the growth of galaxies, and how these processes have changed with galactic environment across cosmic time, is one of the fundamental problems in modern astrophysics.This project will address a key part in solving this problem by revealing and studying stellar populations in nearby galaxies. Indeed, nearby galaxies are our best laboratories to study the interplay between stars and gas: they provide the necessary numbers to study star formation across many different environments and, crucially, on the small and resolved scales at which the relevant physics happens.By combining data from the integral field spectrograph MUSE on the Very Large Telescope with data from the Hubble Space Telescope, the stellar population of the nearby galaxy NGC 300 will be studied at unprecedented levels of detail, and directly connected to the star-forming gas reservoir in the galaxy. Once in place, the developed analysis methods can then be applied to other nearby galaxies (observed e.g. with the SITELLE instrument on the Canada-France-Hawaii Telescope), therefore providing a framework to quantify the galactic lifecycle of gas and stars.

形成恒星的星系的生命周期非常复杂：低温气体变成恒星；形成的恒星群搅动、混合、丰富、加热，并通过恒星风、辐射和超新星爆炸排出气体；然后，这些气体会落回星系，冷却，形成新一代的恒星。虽然我们定性地了解了控制气体循环所涉及的物理过程，但我们仍然没有对它们进行明确的定量描述。因此，限制星系如何将气体转化为恒星，这些恒星的反馈如何破坏气体并调节星系的生长，以及这些过程如何随着宇宙时间的星系环境而变化，是现代天体物理学的基本问题之一。这个项目将通过揭示和研究附近星系的恒星群来解决这个问题的关键部分。事实上，附近的星系是我们研究恒星和气体之间相互作用的最佳实验室：它们提供了必要的数据，可以在许多不同的环境中研究恒星的形成，更重要的是，在相关物理发生的小而精细的尺度上。通过将超大望远镜上的积分场光谱仪MUSE的数据与哈勃太空望远镜的数据相结合，将对附近星系NGC 300的恒星群进行前所未有的详细研究，并将其与星系中形成恒星的气藏直接联系起来。一旦到位，开发的分析方法就可以应用到其他附近的星系（例如用加拿大-法国-夏威夷望远镜上的SITELLE仪器观察），因此提供了一个框架来量化星系的气体和恒星的生命周期。