We propose to conduct a unique and very efficient Pa-beta imaging (1.4hrs science time!) of the best-studied galaxy cluster in formation, called "Spiderweb" protocluster, at z=2.16, with the NIRCam F405N filter. Our primary goal is to map the entire star formation activities across this starbursting protocluster, and within individual galaxies

JWST will be the most sensitive tool ever built for studying the accretion onto supermassive black holes (SMBHs) at the centers of galaxies. While quasars and bright active galactic nuclei (AGN) provide spectacular examples of this accretion, a vast majority of galaxies have black holes accreting at much lower rates. Although these low luminosity

The recent era of large, ground-based abundance surveys has unraveled the chemical structures of our Milky Way galaxy. The most striking abundance feature is the alpha-abundance bimodality. The low-alpha stars are younger (1-8 Gyr) while the high-alpha stars are older (8-12 Gyr) and have a thicker distribution. There are a number of different

We propose to observe the Ring Nebula, NGC 6720, at unprecedented spatial resolution and spectral sensitivity using MIRI, NIRSpec and NIRCam, with the aim of measuring and analyzing the emission from a range of atomic, molecular and particulate components commonly found in astrophysical environments. We will use this planetary nebula (PN) as an

The atmospheric characterisation of multiple exoplanets in the same system can provide a window into the processes that underpinned their formation and evolution. The planetary C/O ratios are of particular interest as they encode information about where the planet formed with respect to different ice lines, but precise measurements of this using

Galaxy evolution models are strongly underpinned by anchoring constraints made locally in the Milky Way. In this proposal, we aim to perform a pilot study toward providing a secondary local anchor in the form of a detailed mapping in element abundances of the stellar populations of the Andromeda galaxy, M31. Primarily, we will use NIRSpec