1. Benjamin D. Oppenheimer Leiden Observatory Simone Weinmann, Romeel Dave, Kristian Finlator, Jason Tumlinson, Rob Crain & others

2. Abundance matching- Behroozi et al. (2012) Main Sequence Integration- Leitner (2012) VESPA SSP Modelling- Tojeiro et al. (2009)

3. Behroozi, Wechsler, & Conroy 2o12 SFHs independent of ΛCDM dark matter assembly are difficult to reproduce in SAMs and simulations (Weinmann et al. 2012).

4. “The overproduction of low-mass galaxies at z > 0.5 in all SAMs and hydrodynamical simulations explored here may thus be symptomatic of the limited range of feedback prescriptions currently in use, and indicates that alternative models of feedback need to be explored.” --Weinmann et al. (2012) Weinmann et al. (2012)

5. Opp. et al. 2010 All Assembly w/ wind mode W/O Wind Mode Opp. et al. 2010 We separated stellar assembly based on whether stars formed from pristine, cold accretion or re-accreted winds accreted from the circumgalactic medium (CGM).

6. Opp. et al. 2010 All Assembly w/ wind mode W/O Wind Mode Opp. et al. 2010 Wind recycling is a way of moving stellar mass assembly to late times via cycles through the circum-galactic medium (CGM). Weinmann et al. (2012) M * =10 9.27 -10 9.77 M sol

7. Oppenheimer-style resolution of the same 10 11.2 M sol halo 129 orbits to observe the CGM of z=0-0.1 dwarfs at 20-150 kpcs (PI J. Tumlinson)

8. No Winds: No Metals in CGM, most baryons form into stars. Fast Winds: 700 km/s blows most baryons out of CGM, only a cool few metals left behind Momentum-driven Winds: slower winds, 100-200 km/s, keep baryons recycling and participating in galaxy formation, plenty of cool metals.

9. Thanks to Rongmon Bordoloi & Jason Tumlinson.

10. Energy-conserved feedback (ezw) where v wind ~ σ, η ~ 1/σ 2 where low-mass galaxies are suppressed more than momentum-conserved feedback (vzw): η ~ 1/σ. Missing baryons are ejected into the CGMs of these halos. *Let’s hope not. CGMCGM CGMCGM CGMCGM

11. 14 Gyrs 1 Gyr vzw: η ~ 1/σ 14 Gyrs 1 Gyr ezw: η ~ 1/σ 2 M acc ×f b M sf cold M sf wind Early winds suppress SF relative to baryon accretion rate. Returning winds that recycle on timescales of Gyrs add to late time stellar assembly, increasing late time specific SFR’s.

12. Wind recycling returns material back onto dwarf galaxies raising the sSFR’s for lower mass galaxies at late times (z=0).

13. “I think it's possible that Simone's dwarf SFH problem will disappear given the new wind model plus the new faint- end data which is steeper at high-z.” --Romeel Davé

14. Cold Mode Hot Mode Wind Mode

15. Cold Mode Hot Mode Wind Mode

16. 1. The shallow potential wells of low-mass halos are very sensitive testbeds for feedback processes affecting galaxy formation. 2. We are banking on finding a large fraction of the low-mass halo missing baryons in their local CGMs, where launched winds can re-participate in late galaxy formation. 3. Putting in 2-3 new, non-traditional parameters into SAMs (e.g. recyling parameters) should be able to divorce stellar assembly histories from dark matter accretion histories and reproduce most key observations of low-mass galaxy formation.

17. Patel et al. (2013)

18. Behroozi et al. 2012: star formation rate divided by baryon accretion rate for halos of various masses from z=8->0.