1. 0.2  = 1.6 kpc Prominent “new” issues  IMF  Metallicity (gas, stars!)  Environment (is it important at high z?)  Feedback (not new, but not solved; esp. star formation feedback, again issue of timescales!)  SFHs, Dust... (maybe for a future workshop?)  Connection between structural parameters and SF activity (red sequence, gradual “cross-over”, dense objects, higher diversity at high z?)  SFGs == Stream-fed galaxies, timescales, dynamics ...

2. 0.2  = 1.6 kpc  Consistent comparisons over different redshift ranges (tracers/diagnostics; populations)  Account for observational selection effects and biases  Consistent comparisons between observations and simulations/models (same “measured” quantities) Challenges ...

3. 0.2  = 1.6 kpc Ways Forward  Cf. “challenges”: can be already tackled, awareness increasing!  Complementary approaches: which is better for what aspects? - wider/deeper surveys (  stacking) - wavelength regimes - spatially-resolved properties  Environment at high z: modellers: make predictions now for near-future observations!  In massive galaxies: relative importance of - AGN feedback? - SF feedback?  Is the time come to play with IMF, or can we still happily ignore it for a while?  Is it worthwhile to update individual bits to complex models/simulations?  Two quotes: “Should we bother making simulations?” “Should we bother making observations”? Vote! ...

4. Quotes  Should we bother making simulations?  Anonymous observer  Should we bother making observations?  Anonymous modeller YES and YES!

5. Thank you!