This is seriously lifechanging I can now copy files in peace

This is amazing!!

This type of model pushes the limits of current data, needing large numbers of precise abundances that will be possible in coming years with PFS/4MOST/ELTs. It’s also extremely powerful, providing unprecedented time resolution in low-mass dwarf galaxies inaccessible with direct observations.

YST and I realized that you can get really large metallicity gaps due to Type Ia SNe enrichment during long quiescent periods in a galaxy’s star formation history. The SNe keep going off even though you stop forming stars, which can show up in chemical evolution.

I think there’s very convincing evidence that it’s actually part of a globular cluster stream! (Which was of course once part of a dwarf galaxy :) )

#dwarfgalaxies2024 6/24 (25%) of the HI dwarfs are in pairs, compared to 5% in optical spectroscopic surveys, which may be biased against dwarfs due to fiber collisions. Preliminarily, ~10-13% of galaxies have a companion (2x higher rate than SDSS).

#dwarfgalaxies2024 J0139+4328: a HI detection in FAST, 4e6 in stellar mass but 6e7 Msun in gas. What is the Mbary-Mhalo relation (instead of Mstar-Mhalo)?

#dwarfgalaxies2024 public data release planned 2025!

#dwarfgalaxies2024 Daniel Piacitelli: studies simulated CGM of dwarf galaxies Ryoungwook Kang: compares numerical/feedback choices in GADGET vs RAMSES for high-z simulations

#dwarfgalaxies2024 Zhu also ran hydrodynamical simulations showing that the CGM of dwarf galaxies is removed very quickly and leaves CGM tails (that form HI but not stars).