Headline

• Does the IMF differ between the two modes of star formation?
• steeper mass function of star clusters by major mergers; is this consistent with the linear relation of halo mass and GC total mass?
• triple distribution in the Age-Metallicity diagram? due to major mergers?

• low-mass galaxies: what about their SFH?
• turbulent SF suppress SMBH growth? What if in case of mergers? the result seems to be quite different from those predicted by Volker's simulations

• What's the role of mergers, and bars?
• BH mass at fixed bulge mass at high z is higher than low z, as recently found in some z>6 quasars by Feige Wang & Xiaohui Fan, using ALMA data.
• SF in supergiant shells at high z has been overlooked. Where will these stars go? moving together to the central region, or distributed more widely?

diverse kinematics + metallicity gradients at z~2. Xiacheng Ma+2017b, MNRAS, 466, 4780

HiZFIRE, Ma+18a

GCs form efficiently in gas-rich, turbulent ISM, Ma+20a, MNRAS, 493, 4315