Astrophysics Research at Liverpool John Moores University: Consolidated Grant Renewal (2018-2021)

我们将利用观测和理论在天体物理学的前沿开展工作。ARI的使命是成为世界领先的研究中心，达到国际最高水平。我们的研究使用最先进的设施和数据分析技术，ARI的工作人员正在领导许多新一代的调查。这种情况下的项目在技术上要求很高，需要PDRA和其他支持来帮助科学的交付。基于ARI在星星形成（SF）方面世界领先的专业知识，我们将通过以下方式研究SF与银河系气体物理之间的联系：绘制3D SF效率图，并研究SF与靠近银河系中心的气体分布之间的联系。在一项平行的研究中，我们将通过推导银河系中心新发现的大质量前恒星核的性质来确定超大质量恒星是如何聚集的。利用JCMT和Herschel的调查数据以及世界上最好的毫米天文台阿尔马的大量时间分配，我们将回答有关SF和稠密气体物理之间的联系以及怪物恒星的早期生长的关键问题。我们还将模拟球状星团中恒星的形成。这将显着扩展以前的工作，通过纳入现实的处理的前体气体的第一次，并提供了一个重要的一步，在了解这些系统的形成。在恒星种群的领域，我们将提供一个新的视角的物理过程，确定银河系的形成和结构，使用广泛的数据从APOGEE-2，盖亚和WEAVE。这些数据将用于确定银河系恒星的轨道特性，并与来自星系形成模型的模拟星表（如EAGLE模拟）相结合。在时域天体物理学方面，我们将执行一个深入的方案，研究伽马射线爆发、超新星类型：Ia、II和Ib/c及其环境的特性。我们将通过测量本星系群内外一类新的快速复发新星的大小来建立通往Ia型超新星的途径。我们还将参与引力波的新科学，寻找与合并双星对应的电磁波。我们将使用最具能量的瞬变作为高红移宇宙的探测器，提供再电离时恒星形成密度的新估计。这些活动利用了ARI在这一领域不断增长的专业知识，并利用了我们的特权：（i）SN探测调查iPTF/ZTF;（ii）LIGO-Virgo EM后续实验;（iii）基于Swift的SHOALS调查;（iv）对一系列领先天文设施的观测，包括我们自己的利物浦望远镜（LT）。建立在我们领先的瞬态极化测量，我们将利用新的时域偏振计（MOPTOP）的LT。我们将因此在极端环境中遇到的伽玛射线暴，耀变体和新星的磁场和物理几何形状的新的约束。在星系演化中，我们将研究宇宙中的重子质量组合，重点是低光度星系和星系内及周围漫射光的观测。这对于充分利用新设施（如欧几里得、eROSITA和LSST）的科学至关重要，申请人在这些设施上有很强的投资。ARI是使用EAGLE和BAHAMAS模拟开发星系形成的真实模型的最前沿。因此，通过与我们的观测工作并行的举措，我们将开发复杂的虚拟观测，提供光线跟踪的弱透镜图和对微弱恒星晕光的预测，以与盖亚的结果进行比较，欧几里得和LSST。为了让公众参与STFC科学，我们建议为5个项目开发一系列资源，涵盖以下领域：i）星星的寿命ii）“大”和“开放”数据iii）天文学和宇宙学模拟。

We will carry out work at the forefront of astrophysics using both observations and theory. The ARI's mission is to be a world-leading research centre at the highest international level of excellence. Our research uses the most advanced facilities and data analysis techniques and ARI staff are leading many of the new generation surveys. The projects in this case are technically demanding and require PDRA and other support to aid the delivery of the science. Building on ARI's world-leading expertise in star formation (SF), we will investigate the connection between SF and gas physics in the Milky Way by: mapping the SF efficiency in 3-D and studying the connection between SF and the gas distribution close to the Galactic Centre. In a parallel study we will determine how very massive stars assemble by deriving properties of newly identified high mass pre-stellar cores in the Galactic Centre. Exploiting survey data from JCMT and Herschel and large allocations of time on the world's best mm observatory, ALMA, we will answer key questions about the connection between SF and the dense-gas physics, and the early growth of monster stars. We will also carry out simulations of the formation of stars in globular clusters. This will significantly extend previous work by incorporating realistic treatment of the precursor gas for the first time and provide a major step forward in understanding the formation of these systems.In the area of stellar populations we will deliver a new perspective on the physical processes determining the formation and structure of the Milky Way, using extensive data from APOGEE-2, Gaia and WEAVE. These data will be used to determine orbital properties of Galactic stars and integrated with mock catalogues from models of galaxy formation, such as the EAGLE simulations.In time-domain astrophysics we will perform an in-depth programme to study the properties of gamma-ray bursts, Supernovae Types: Ia, II and Ib/c, and their environments. We will establish the pathways to SNe Type Ia by measuring the size of a new class of Rapidly Recurring Novae in and beyond the Local Group. We will also partake in the new science of gravitational waves by searching for the electro-magnetic counterparts to coalescing binaries. We will use the most energetic transients as probes of the high-redshift Universe providing new estimates of the star-formation density at reionization. These activities capitalise on ARI's growing expertise in this field and exploit our privileged access to: (i) the SN detection surveys iPTF/ZTF; (ii) LIGO-Virgo EM follow-up experiments; (iii) the Swift-based SHOALS survey; (iv) observations on a range of leading astronomical facilities including our own Liverpool Telescope (LT). Building on our lead in polarization measurements of transients, we will exploit the new time-domain polarimeter (MOPTOP) on the LT. We will thereby place new constraints on the magnetic field and physical geometries in extreme environments encountered in gamma-ray bursts, blazars and novae. In galaxy evolution we will investigate the baryonic mass assembly in the Universe focussing on observations of low-luminosity galaxies and diffuse light in and around galaxies. This is essential to fully exploit the science from new facilities such as Euclid, eROSITA and LSST, in which the applicants have a strong investment. The ARI is at the forefront of developing realistic models of galaxy formation using the EAGLE and BAHAMAS simulations. Thus, through a parallel initiative to our observational work we will develop sophisticated virtual observations, delivering both ray-traced weak lensing maps and predictions of the faint stellar halo light for comparison with results from Gaia, Euclid and LSST.To engage the public in STFC science we propose to develop a range of resources for 5 projects covering the areas i) life of a star ii) "big" and "open" data iii) astronomical and cosmological simulations.