the SINS survey of galaxy kinematics at z~2 : turbulent thick disks and evidence for rapid secular evolution Reinhard Genzel, Natascha Förster Schreiber, Nicolas Bouché, Giovanni Cresci, Kristen Shapiro, Linda Tacconi MPE (and others in the room…) for the SINS team MPE, 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

integral field spectroscopy 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

properties of SINS galaxies compared to z~2 magnitude limited samples For many SINS z ~ 2 star-forming galaxies:  ~ gas ~ 500 Myr ~ 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)

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..9 Msun 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

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

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

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

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

Sizes of giant star forming clumps likely set by the fragmentation scale in the disk 8kpc Q2343-BX610 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

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

central disk/bulge NGS/LGSF data sets: ~0.2” resolution (1.6 kpc) Hα vels BX482 z=2.2 0.5” Hα + R-band NIC2 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

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

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

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

origin of large turbulent velocities disk virial radius 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

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