Squaring the circle: making sense of the dusty, magnetized interstellar medium beyond two dimensions

星际介质（ISM），银河系中恒星之间的气体和尘埃，是一个巨大的水库，新的恒星和行星正在诞生，因此是理解星系演化的核心。随着气相从冷到热，从分子到原子，从中性到电离，一个动态的重要磁场，以及湍流运动，ISM处于混乱之中。物理过程和天文现象的复杂性使我们能够理解我团队中年轻研究人员的激励培训环境，他们利用计算天体物理学，统计学和数据密集型分析在非常极端的条件下应用广泛的现代物理学。使用普朗克卫星，我们在分析偏振热辐射方面取得了巨大进展。 尘埃和相关的磁场在天空中的投影中被看到，缺乏深度理解所需的距离和3D视角。 然而，这即将改变，这是一场由盖亚卫星提供的数十亿恒星距离发动的革命。 量化恒星的尘埃消光（散射加上吸收）可以确定尘埃的距离。 为了确保深入探测致密分子恒星形成云中的尘埃，我的团队将对恒星进行光谱分类，这是一种新的多路复用红外光谱仪WIFIS的新应用。为了获得最佳的角分辨率和3D分布，我们将使用Herschel的热发射产生新的尘埃光学深度图。尘埃如何随着3D环境演变需要新的见解。 我们将专注于一组独特的观测，明确测量相同的灰尘在多个频率，旨在自洽的灰尘模型。将校准亚毫米光学深度与光学消光的比率，量化3D中不透明度的演变。 测量散射光的数量，利用蜻蜓长焦阵列的超宽场灵敏度，与热发射相比，将通过相位函数和相位函数提供补充证据。 BLAST-TNG观测到的热尘埃发射的分数偏振的频率依赖性相比，星际偏振将严格约束尘埃成分的混合物。我们正在开发更复杂的三维模型和模拟的磁化ISM，静态和动态，结合结构如何演变的磁场。 我们已经表明，在投影中的ISM结构和磁场的相对取向是平行的扩散介质中，但在高柱密度垂直。我们将进一步探索尘埃偏振与BLAST-TNG在更高的角分辨率。 我们的模型雄心勃勃地解决了银河系尘埃前景B模式偏振如何污染原始宇宙学B模式信号，致密区域的晶粒排列，以及磁场在云组装和支持中的作用。

The interstellar medium (ISM), gas and dust between the stars in the Milky Way, is a vast reservoir from which new stars and planets are being born, and so at the heart of understanding galaxy evolution. With gas phases ranging from cold to hot, molecular to atomic, and neutral to ionized, a dynamically important magnetic field, and turbulent motions, the ISM is in turmoil. The complexity of physical processes and astronomical phenomena stretch our ability to comprehend a stimulating training environment for young researchers on my team, who draw on computational astrophysics, statistics, and data-intensive analysis to apply a broad range of modern physics in very extreme conditions.Using the Planck satellite, we made great progress analysing polarized thermal emission. Dust and associated magnetic fields are seen in projection on the sky, lacking distances and the 3D perspective needed for deep understanding. However, this is about to change, a revolution launched by billions of stellar distances provided by the Gaia satellite. Quantifying dust extinction (scattering plus absorption) of stars locates the dust in distance. To ensure that dust in dense molecular star-forming clouds is probed deeply, my team will make spectral classifications of stars, a novel application of a new multiplexing infrared spectrograph WIFIS. For the best angular resolution, and so 3D distribution, we will produce new maps of dust optical depth based on thermal emission using Herschel.How dust evolves with 3D environment requires new insights. We will focus on a unique set of observations that explicitly measure the same dust at multiple frequencies, aiming for self-consistent dust models. The ratio of optical depth in the submillimetre to extinction in the optical will be calibrated, quantifying the evolution of opacity in 3D. Measuring the amount of scattered light, exploiting the superb wide field sensitivity of the Dragonfly Telephoto Array, compared to thermal emission will provide complementary evidence via albedo and phase function. BLAST-TNG observations of the frequency dependence of the fractional polarization of thermal dust emission compared to interstellar polarization will tightly constrain mixtures of dust components.We are developing more sophisticated 3D models and simulations of the magnetized ISM, both static and dynamic, incorporating how structures evolve in relation to the magnetic field. We have shown that in projection the relative orientation of ISM structures and the magnetic field is parallel in the diffuse medium, but perpendicular at high column density. We will explore dust polarization further with BLAST-TNG at higher angular resolution. Our models ambitiously tackle how the Galactic dust foreground B-mode polarization contaminates the primordial cosmological B-mode signal, grain alignment in dense regions, and the role of the magnetic field in cloud assembly and support.