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 TacconiMPE

(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 0808.0194Shapiro et al. 2008, astro-ph 0802.0879, Förster Schreiber et al. 2008a,b, Cresci et al. 2008

SINS Survey Förster Schreiber et al. 2008a

near-IRintegral field spectroscopy

Hα ([NII], [OIII])of z~1.5-3.2

star forming galaxieswith SINFONI, +AO,

at the VLT

complemented withnear-IR imaging

with HST/NICMOS and VLT/NACO+AO

Förster Schreiber et al. (2006, 2008); Genzel et al. (2006, 2008), Tacconi et al. (2008)

(FIREWORKS/CDFS data: Wuyts et al. 2008)

For many SINS z ~ 2 star-forming galaxies:

~ gas ~ 500 Myr ~ several dyn << tHubble

SMGs

properties of SINS galaxies compared to z~2 magnitude limited samples

clumpy high-z galaxies: mergers or clumpy disks ?

Cowie, Hu, Giavalisco, van den Bergh, Elmegreen & Elmegreen, Labbé, Stockton 1995-2007

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

a large fraction of z>1 star forming galaxies are clumpy (chains, clump-clusters)

HST UDF

-200-260(±33)FWHM

0.5”(4kpc)

Hα -130

0 +200+65 +400(±130)

-65

+130

BzK 15504 z=2.38: a thick, clumpy & globally unstable disk

Mdyn(<10 kpc) ~1011 M

vc=230 km/s, Rd=4 kpcSFR = 150 Myr-1, Q=0.8Σgas~ 300 M pc-2

, fgas~0.3Genzel et al. 1996, Nature 442, 786

SINFONI +AO (VLT): 0.2” (1.6 kpc) resolution

Hα K-cont.

BzK15504 z=2.38

kinemetry and v-R relation

Shapiro et al. 2008, astro-ph 0802.0879

0 200 400 6000

5

10

15

median uncertainty

vd(km/s)

disk

sca

le le

ngth

(kp

c)

SMGs

BX/BzK

Bouché et al. 2007

λhalo~0.09

~30% major mergers

size high-z disks ~ low-z disks

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)

-100

+100

N2 850.2 (2.45)

-220

+200

1” (8 kpc)

dispersiondominated

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

30BM 1163 (1.41)

BX 404 (2.03)

-5

30

merger

rotation-

dominated

-60

70

K20-6 (2.2)

-80

100BX 599 (2.33)

GK 167 (2.58)

-60

30

-70

70

GK2252 (2.41)

-280

280

BX389 (2.2)

170

K20-5 (2.2)-170

dispersiondominated

-120

120BzK 4165 (1.7)

-70

150SA12 6192 (1.51)

-10080

K20-8 (2.2)

ZC1101592 (1.41)

-240

240

GK2471 (2.43)

-170

170

+ 130

- 90

BzK 6004 (2.4)

-170

200

BX 610 (2.2)

240

-160K20-9 (2.0)

+160

-120

BX663 (2.4)

-70

110

BX528 (2.3)

160

-3050

GK 2113 (1.61)

0+380

-80

K20-7 (2.2)

120

200

-200

BzK 15504 (2.4)

-160

160

ZC782941 (2.2) -200

+200

BX482 (2.2)

SA12 8768 (2.2)

80

-45

1” (8 kpc)

170

-170

MD 41 (2.2)

-145

145

D3a 6397 (1.51)

The SINS surveyof galaxy kinematics at z~1.5-2.5(Förster Schreiber et al. 2006, 2008)

Genzel et al. 2008, astro-ph 0807.1184

z~2 disks are turbulent

0.1

0.2

0.3

0.4

0.5

0 0.2 0.4

BzK6004

BX610

BX389

BX482

MD41

[NII]/HM

dyn(

0.4"

/Mdy

n(1.

2")

0

2

4

6

0.2 0.5 1 2 5

BX502

SFR

(Msun

yr-1kpc-2)

v d/

0

0

2

4

6

0 0.2 0.4

BX482

BX502

[NII]/H

0.01

0.1

1

0 0.1 0.2 0.3 0.4 0.50.01

0.1

1

BzK6004

MD41BX482

BX502

[NII]H

M*/S

FR

(H)

(G

yr)

0

10

20

0.1 0.2 0.3 0.4 0.5

0.1 0.2 0.3 0.4

resolution HST

resolution SINFONI

FWHM size (arcseconds)

num

ber

of c

lum

pssize (kpc)

Sizes of giant star forming clumps likely set by the fragmentation scale in the disk

Genzel et al. 2008, Foerster Schreiber et al. 2008b,Elmegreen & Elmegreen 2005, Elmegreen et al. 2007

8kpc

Q2343-BX610 Q2346-BX482

Q2343-BX389

SSA22-MD41

NICMOS H160

Foerster Schreiber, Shapley et al. 2008

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

SFR

,

observed SFR can be accounted for by DM simulations for

SFR ~ 0.5 0.18

cold flow/'streams' regime

mostly gaseous accretion

dmz M

bM

central disk/bulge

Genzel et al. 2008 astro-ph 0807.1184, Förster Schreiber et al. 2008b

00 0.5 1.0

0 2 4 6 8

0

100

200

300

intrinsic

circ

ular

vel

ocity

(km

/s)

0 0.5 1.0

0 2 4 6 8

0

1

2

3

Hlight

mass

surf

ace

dens

ity/b

right

ness

radius (kpc)

-300

-200

-100

0

100

200

300

-1 0 1

-10 0 10

circ

ular

vel

ocity

(km

/s)

50

100

150

200

-1 0 1

-10 0 10

position along major axis (arcseconds)ve

loci

ty d

ispe

rsio

n (k

m/s

)

0

10

-1 0 1

-10 0 10

0

H/([OIII]/H)[OIII]/H

norm

aliz

ed s

urfa

ce b

right

ness

position (kpc)

00 0.5 1.0

0 2 4 6 8

0

1x1011

radius (arcseconds)

encl

osed

mas

s (M

sun)

NGS/LGSF data sets: ~0.2” resolution (1.6 kpc)

0.5”

Hα + R-band NIC2Hα vels

BX482 z=2.2

• R~7 kpc star forming, rotating ring with little in the center• this is not a post-merger gas disk!

central disk/bulge

Genzel et al. 2008 astro-ph 0807.1184, Förster Schreiber et al. 2008b

+ 140

-130

-200

+190

1”(8 kpc)

BzK 15504 z=2.4

BzK 6004 z=2.4z=2.2

-160

BzK-ZC782941

BX 482 z=2.2

+210

-240

+160

NGS/LGSF data sets: ~0.15-0.4” resolution (1.6 kpc)

M(≤3 kpc)/M(≤15 kpc)~0.2-0.4

0.1

0.2

0.3

0.4

0.5

0 0.2 0.4

BzK6004

BX610

BX389

BX482

MD41

[NII]/HM

dyn(

0.4"

/Md

yn(

1.2"

)

0

2

4

6

0.2 0.5 1 2 5

BX502

SFR

(Msun

yr-1kpc-2)

v d/

0

0

2

4

6

0 0.2 0.4

BX482

BX502

[NII]/H

0.01

0.1

1

0 0.1 0.2 0.3 0.4 0.50.01

0.1

1

BzK6004

MD41BX482

BX502

[NII]H

M*/S

FR

(H)

(G

yr)

Inside-out [NII]/Hα gradients

[NII]/HαNIC2 H160 +Hα

Q2343-BX610 z=z.21

K-cont.& Hα [NII]/Hα

BzK 6004 z=2.39

1”

[NII]/Hα

BzK6397 z=1.514

blue/red & continuum

Buschkamp, Foerster Schreiber et al. 2008

rapid secular evolution at z~2

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

2 2

0

~ ( ) (R) dvis df dyn dyn

Jeans

R vt t t R t

at z~0: tvis,df~5-10 Gyrsat z~2: tvis,df~ a few 102 Myrs

Genzel et al. 2008

a highly turbulent, massive gas rich disk evolves rapidly by fragmention and secular effects

origin of large turbulent velocities

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

origin of large turbulent motions: gravitational energy of accreting gas, feedback, dynamical instabilities in clumpy disk

1/ 2 1.11 0.04250 6 2 12

0

~ 5 10 1 /3.2 de

vv R z M

disk

virial radius

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