1. 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 , Genel et al. astro-ph
Shapiro et al. 2008, astro-ph , Förster Schreiber et al. 2008a,b, Cresci et al. 2008

2. integral field spectroscopy
SINS Survey
Förster Schreiber et al. 2008a
near-IR
integral field spectroscopy
Hα ([NII], [OIII])
of z~
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 ~ 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)

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
Msun clumps d ~ 1kpc flat surface brightness
(nS ~1-2)
Msunpc-2
Nclump~3-10, ~40% of light
Cowie, Hu, Giavalisco, van den Bergh, Elmegreen & Elmegreen, Labbé, Stockton

5. 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

6. 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

7. 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
N (2.38)
SMMJ (3.41)
+200
-200
+250
-250
HDF 169 (1.2)
SMMJ (1.21)
+300
-350
HDF 76 (2.20)
N (2.45)
-220
1” (8 kpc)
dispersion 70
-70
D3a 4751 (2.27)
SA (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
SA (1.51) 80
K20-8 (2.2)
ZC (1.41)
-240
240
GK2471 (2.43)
+ 130
- 90
BzK (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 (2.4)
ZC (2.2)
BX482 (2.2)
SA (2.2)
-45
MD 41 (2.2)
-145
145
D3a 6397 (1.51)
The SINS survey
of galaxy kinematics at z~
(Förster Schreiber et al. 2006, 2008)

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

9. 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

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

11. 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 astro-ph , Förster Schreiber et al. 2008b

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

13. 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

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. 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

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