Genzel et al. 2008, astro-ph 0807.1184, Genel et al. astro-ph 0808.0194

1. the SINS survey of galaxy kinematics at z~2 : turbulent thick disks and evidence for rapid secular evolutionReinhard Genzel, Natascha Förster Schreiber, Nicolas Bouché, Giovanni Cresci, Kristen Shapiro, Linda TacconiMPE(and others in the room…)for the SINS teamMPE, UCB, USM, INAF, CEA, CfA, UCLA, CTI, ETH, TAU Genzel et al. 2008, astro-ph 0807.1184, Genel et al. astro-ph 0808.0194 Shapiro et al. 2008, astro-ph 0802.0879, Förster Schreiber et al. 2008a,b, Cresci et al. 2008

2. SINS Survey Förster Schreiber et al. 2008a near-IR integral field spectroscopy Hα ([NII], [OIII]) of z~1.5-3.2 star forming galaxies with SINFONI, +AO, at the VLT complemented with near-IR imaging with HST/NICMOS and VLT/NACO+AO

3. properties of SINS galaxies compared to z~2 magnitude limited samples For many SINS z ~ 2 star-forming galaxies:  ~ gas ~ 500Myr ~ several dyn << tHubble SMGs Förster Schreiber et al. (2006, 2008); Genzel et al. (2006, 2008), Tacconi et al. (2008) (FIREWORKS/CDFS data: Wuyts et al. 2008)

4. clumpy high-z galaxies: mergers or clumpy disks ? HST UDF a large fraction of z>1 star forming galaxies are clumpy (chains, clump-clusters) 0.5”=4kpc 108..9Msun clumps d ~ 1kpc flat surface brightness (nS ~1-2) 102.2..2.7 Msunpc-2 Nclump~3-10, ~40% of light Cowie, Hu, Giavalisco, van den Bergh, Elmegreen & Elmegreen, Labbé, Stockton 1995-2007

5. 0.5” (4kpc) -65 FWHM -130 -200 -260(±33) Hα BzK15504 z=2.38 0 +65 +130 +200 +400(±130) K-cont. Hα BzK 15504 z=2.38: a thick, clumpy & globally unstable disk Mdyn(<10 kpc) ~1011 M vc=230 km/s, Rd=4 kpc SFR = 150 Myr-1, Q=0.8Σgas~ 300 M pc-2, fgas~0.3 SINFONI +AO (VLT): 0.2” (1.6 kpc) resolution Genzel et al. 1996, Nature 442, 786

6. λhalo~0.09 BX/BzK SMGs Bouché et al. 2007 kinemetry and v-R relation ~30% major mergers size high-z disks ~ low-z disks Shapiro et al. 2008, astro-ph 0802.0879

7. BX663 (2.4) rotation- dominated rotation- dominated BX 610 (2.2) MD 41 (2.2) -120 dispersion dominated dispersion dominated -170 BX 404 (2.03) +160 N2 850.2 (2.45) HDF 76 (2.20) -220 30 K20-5 (2.2) 170 -170 -100 -5 170 +200 D3a 6397 (1.51) +100 SA12 8768 (2.2) BzK 15504 (2.4) 145 SA12 6339 (2.3) -200 HDF 169 (1.2) -50 -250 -145 HDF 242 (2.49) BX 502 (2.16) +50 30 K20-8 (2.2) BzK 6004 (2.4) 35 200 +250 -200 1” (8 kpc) -20 - 90 K20-6 (2.2) 80 ZC1101592 (1.41) -150 SMMJ09431 (3.35) 240 K20-9 (2.0) GK 167 (2.58) -100 SA12 6192 (1.51) BX 405 (2.03) -160 150 ZC782941 (2.2) 70 +200 H7 +500 40 160 -45 200 -60 BX482 (2.2) -60 + 130 +60 -70 -240 H6 +100 240 GK2471 (2.43) BzK 4165 (1.7) -160 80 120 -35 -100 170 BX389 (2.2) -170 -170 30 1” (8 kpc) -120 D3a 4751 (2.27) 70 BM 1163 (1.41) 30 BX 599 (2.33) -70 100 N2850.4 (2.38) BX528 (2.3) -30 SMMJ131201 (3.41) GK2252 (2.41) 160 -300 +350 SMMJ105141 (1.21) K20-7 (2.2) -80 merger GK 2113 (1.61) 280 +200 -80 +300 merger 70 -70 120 -200 0 -30 -70 50 -350 110 +380 -280 The SINS survey of galaxy kinematics at z~1.5-2.5 (Förster Schreiber et al. 2006, 2008)

8. z~2 disks are turbulent Genzel et al. 2008, astro-ph 0807.1184

9. Q2343-BX610 8kpc Sizes of giant star forming clumps likely set by the fragmentation scale in the disk Q2346-BX482 Q2343-BX389 SSA22-MD41 NICMOS H160 Foerster Schreiber, Shapley et al. 2008 Genzel et al. 2008, Foerster Schreiber et al. 2008b, Elmegreen & Elmegreen 2005, Elmegreen et al. 2007

10. The large star formation rates are consistent with CDM simulations (even) without major mergers Genel et al. 2008, astro-ph 0808.0194, Dekel et al. 2008

11. BX482 z=2.2 0.5” Hα vels Hα + R-band NIC2 central disk/bulge NGS/LGSF data sets: ~0.2” resolution (1.6 kpc) • R~7 kpc star forming, rotating ring with little in the center • this is not a post-merger gas disk! Genzel et al. 2008 astro-ph 0807.1184, Förster Schreiber et al. 2008b

12. -200 z=2.4 BzK 15504 BX 482 z=2.2 1” (8 kpc) -240 +210 -130 +190 BzK-ZC782941 z=2.2 +160 z=2.4 BzK 6004 -160 + 140 central disk/bulge NGS/LGSF data sets: ~0.15-0.4” resolution (1.6 kpc) M(≤3 kpc)/M(≤15 kpc)~0.2-0.4 Genzel et al. 2008 astro-ph 0807.1184, Förster Schreiber et al. 2008b

13. Q2343-BX610 z=z.21 BzK6397 z=1.514 [NII]/Hα 1” BzK 6004 z=2.39 blue/red & continuum NIC2 H160 +Hα K-cont.& Hα [NII]/Hα [NII]/Hα Inside-out [NII]/Hα gradients Buschkamp, Foerster Schreiber et al. 2008

14. rapid secular evolution at z~2 a highly turbulent, massive gas rich disk evolves rapidly by fragmention and secular effects at z~0: tvis,df~5-10 Gyrs at z~2: tvis,df~ a few 102 Myrs Genzel et al. 2008 Fall & Efstathiou 1980, Mo, Mao & White 1998,Silk 2001, Lin & Pringle 1987, Noguchi 1999, Semelin & Combes 2002, Immeli et al. 2004, Bournaud et al. 2007

15. virial radius disk origin of large turbulent velocities origin of large turbulent motions: gravitational energy of accreting gas, feedback, dynamical instabilities in clumpy disk Förster Schreiber et al. 2006, Dib, Bell & Burkert 2006, Genzel et al. 2008, Immeli et al. 2004, Bournaud et al. 2007, Dekel & Birnboim 2003, 2006, Keres et al. 2005, Ocvirk et al. 2008

16. Conclusions • many of the massive UV/optically selected z~2 star forming galaxies are clumpy, turbulent disks; only ~1/3 mergers (SMGs !) • evidence for growing large bulges/central disks within disks • large star forming rates can be accounted for by combination of rapid cold flows along cosmic web filaments, plus high star formation efficiency at high density • under these conditions gas rich disks go through a transient clumpy, turbulent phase with rapid internal (secular) evolution, leading to formation of central disks and bulges on a time scale ~1 Gyr