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.

恒星形成星系的生命周期非常复杂：冷气体变成恒星；形成的恒星群通过恒星风、辐射和超新星爆炸搅拌、混合、浓缩、加热和排出气体；然后气体可以落回星系，冷却并形成新一代的恒星。虽然我们定性地了解了控制气体循环的物理过程，但我们仍然没有对它们进行清晰的定量描述。因此，限制星系如何将气体转变为恒星，这些恒星的反馈如何扰乱气体并调节星系的生长，以及这些过程如何随着整个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。该项目将通过揭示和研究附近星系中的恒星种群来解决解决这一问题的关键部分。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来研究许多不同环境中的恒星形成，最重要的是，在相关物理发生的小尺度和解析尺度上。根据甚大望远镜上的积分场摄谱仪 MUSE 和哈勃太空望远镜的数据，将以前所未有的详细程度研究附近星系 NGC 300 的恒星群，并将其直接与恒星形成气体储层联系起来。星系。一旦到位，开发的分析方法就可以应用于其他附近的星系（例如使用加拿大-法国-夏威夷望远镜上的SITELLE仪器进行观测），从而提供一个量化星系气体和恒星生命周期的框架。