1. +160 -120 BX663 (2.4) -170 170 MD 41 (2.2) +240 -160 K20-9 (2.0) +380 -80 K20-7 (2.2) -100 80 K20-8 (2.2) 70 -70 D3a 4751 (2.27) SA12 6339 (2.3) -50 30 SA12 8768 (2.2) 80 -45 GK2471 (2.43) -170 170 ZC1101592 (1.41) -240 240 -170 170 K20-5 (2.2) -120 120 BzK 4165 (1.7) 35 -20 BX 502 (2.16) BX 405 (2.03) -35 40 -30 30 BM 1163 (1.41) BX 404 (2.03) -5 30 -70 150 SA12 6192 (1.51) merger-like rotation- dominated -60 70 K20-6 (2.2) -80 100 BX 599 (2.33) -30 50 GK 2113 (1.61) GK 167 (2.58) -60 30 -70 70 GK2252 (2.41) + 130 - 90 BzK 6004 (2.4) 200 -200 BzK 15504 (2.4) -70 + 110 + 160 BX528 (2.3) -160 +160 ZC782941 (2.2) -140 140 D3a 6397 (1.51) -280 280 BX389 (2.2) 1” (8 kpc) -170 200 BX 610 (2.2) -260 +210 BX482 (2.2) increasing dispersion Förster, Bouché,Cresci, Genzel, Shapiro et al. 06-08 SINS 70 Galaxies 1.5-2.5 Disk: 30-40% (v/σ ~ 2 – 4) Disp: 30% (v/σ < 1) Merger: 20-30% Forster Schreiber et al. 09 Shapiro et al. 09

2. SINS “rotators” Cresci et al. 09

3. SINS “rotators” Cresci et al. 09

4. SINS “rotators” Cresci et al. 09

5. Étude des galaxies à faible masse MUSE Workshop March 18/19 N. Bouché (MPE  LATT)

6. The Hubble sequence still unexplained  Need to study progenitors!

7. Why study low-mass galaxies? Ocvirk, Teyssier 08 VVDS SINS LBG

8. Where are the baryons? S. White & co (SDSS) M halo

9. New insights in galaxy formation Scaling relations (SFR-Mass, TF, etc..) see H. Flores, M. Puech, L. Tresse Z=2 GOODS sBzK K<22.5 Daddi + Elbaz 07 Z=0 SDSS Puech 08, Cresci 09  Mergers not dominant

10. Questions Why SFR ~ 200 M/yr at z=2? Origin of scaling relations: TF, SFR-Mass? Role of feedback in low-mass end (z=2)? What happens at z>5 ?

11. the millenium cosmological simulation high-sigma halos: fed by relatively thin, dense filaments → cold flows typical halos: reside in relatively thick filaments, fed ~spherically → no cold flows

12. Genel et al. 08 DM accretion rate M halo Insights from Millennium Simulation EPS dM/dt ~ 35 M h 1.0 (1+z) 2.2 SFR =ε 0.18 dM h /dt SINS ε must be ~1

13. Dark + baryon accretion Prediction: >>50% baryons accreted as cold gas! (but clumpy)

14. New insights in galaxy formation Scaling relations (SFR-Mass, TF, etc..) see H. Flores, M. Puech, L. Tresse Z=2 GOODS sBzK K<22.5 Daddi + Elbaz 07 Z=0 SDSS EPS

15. f_baryon at z=0 Observation at z=0 Toy model prediction Strongly tied to only assumption

16. Gas fractions @z=2.2: 50% @z=1 : 30% @z=0 : 10% 30-50%Tacconi/Daddi 30%Tacconi 10% Ω(HI)/Ω(star) Accretion prediction Observations

17. Questions Why SFR ~ 200 M/yr at z=2? Origin of scaling relations: TF, SFR-Mass? Role of feedback in low-mass end (z=2)? What happens at z>5 ?

18. Galaxy formation with MUSE  Need Resolved spectroscopy (  Mdyn, Mh, SFR, O/H, etc..) of low-mass galaxies A.Feedback processes (IGM, MZ relation) (z~0.7 – 1.0) B.High redshift Lyman alpha emitters C.Cold accretion

19. Galaxy formation with MUSE  Need Resolved spectroscopy (  Mdyn, Mh, SFR, O/H, etc..) of low-mass galaxies A.Feedback processes (IGM, MZ relation) (z~0.7 – 1.0) B.High redshift Lyman alpha emitters C.Cold accretion

20. Galaxy formation with MUSE  Need Resolved spectroscopy (  Mdyn, Mh, SFR, O/H, etc..) of low-mass galaxies A.Feedback processes (IGM, MZ relation) (z~0.7 – 1.0) B.High redshift Lyman alpha emitters C.Cold accretion (z~3) 1’

21. How? Study low-mass galaxies at z~1 [OII] Study filaments at z~3 [Lya] LAE at z~4,5 LAE at z>6 Verhamme  Need KMOS (OII)  Measure ε_SFR (M halo)  Need KMOS / Hawk-I etc  SF UDF MDF

22. Cold Accretion