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