Angular Momentum on Galactic Scales: The Roles of Initial Conditions, Non-linear Evolution, and Randomness
In this talk we will go on a journey across cosmic time and follow the buildup of the angular momentum of galaxies and their host halos. Galactic angular momentum, which is a strong driver of galactic morphology, has its origins in the relatively simple linear growth phase of structure formation, but is also governed by complex non-linear processes. We will hence explore its relation to dark matter angular momentum, and the roles of baryonic physics...
3D mapping of the dusty, magnetized ISM with starlight polarization
The coming decade will mark a milestone in our understanding of interstellar magnetism: achieving a first reconstruction of the Galactic magnetic field in 3D. This will be crucial for progress in fields such as CMB cosmology and cosmic ray physics. Achieving this goal relies on the combination of (a) high-accuracy data that probe interstellar magnetism and (b) novel algorithms that enable the combination of different datasets. A first step towards this direction can be made through the use of starlight polarization in... Read more about ITC Seminar - Georgia (Gina) Panopoulou (Caltech)
ZFOURGE & MOSEL : Tracking Galaxy Growth at Cosmic Noon
Abstract -- ZFOURGE and MOSEL are deep observational surveys that track how galaxies assemble over cosmic time. ZFOURGE identifies approximately 70,000 objects up to redshifts of z~7 using a custom set of near-infrared imaging filters that provide high precision photometric redshifts. MOSEL targets galaxies at 2<z<4 from ZFOURGE for spectroscopic follow-up to measure properties including star formation histories and kinematics. Here I highlight results that include using the SED fitting code Prospector... Read more about ITC Colloquium - Kim-Vy Tran (University of New South Wales)
"The Formation of Ultra-Diffuse Galaxies from Passive Evolution in the RomulusC Galaxy Cluster Simulation"
Current cosmological simulations have so far been limited to studying the formation of ultra diffuse galaxies (UDGs) in isolation, or with environmental effects applied artificially. Here I present the first self consistent prediction for the formation of UDGs in a galaxy cluster. With unprecedented resolution, the RomulusC cosmological simulation of a 10^14 Msun galaxy cluster is uniquely able to resolve cluster member galaxies down to 10^7 Msun in halos as small as 3e9...
“Dynamical Chaos near Corotation: Limits on cold radial migration”
After an initial epoch of assembly, spiral galaxies like the Milky Way evolve primarily under the influence of slow, internal processes. This secular evolution rearranges the orbital angular momentum and energy of the disk, thus altering its kinematics, morphology and chemical distribution. Dynamical resonances with spiral arms cause stars to migrate large radial distances from their birth radii....