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SINS high redshift galaxy S pectroscopic I maging survey in the N ear-IR with S INFONI N.M. Förster Schreiber A.E. Shapley, D.K. Erb, C.C. Steidel Princeton/CfA/Caltech SINS SINFONI GTO science program on high redshift galaxies MPE-IR/Submm Group, USM/MPE Group, NOVA Group

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slide1

SINS

high redshift galaxy

SpectroscopicImagingsurvey

in the

Near-IR with SINFONI

N.M.

Förster

Schreiber

slide2

A.E. Shapley, D.K. Erb, C.C. Steidel

Princeton/CfA/Caltech

SINS

SINFONI GTO science program on high redshift galaxies

MPE-IR/Submm Group, USM/MPE Group, NOVA Group

and collaborations

N.M. Förster Schreiber, R. Genzel, M. D. Lehnert, L.J. Tacconi,

A. Verma, N. Bouché, N. Nesvadba, R. Davies, D. Lutz,

F. Eisenhauer, K. Shapiro, G. Cresci, R. Abuter, S. Gillessen,

A. Gilbert, R. Bender, S. Seitz, A. Sternberg

MPE/USM/Oxford/Berkeley/LLNL/Tel Aviv

A. Cimatti, E. Daddi, A. Renzini, X. Kong, V. Mignoli, N. Arimoto

Bologna/CEA Saclay/Padova/Hefei China/NAO Japan

slide3

Open issues...

Angular momentum?

Dissipation?

Connection between bulge and disk formation?

Timescales?

Star formation efficiency?

Baryonic mass accretion?

Feedback? Environment?

Where do observed populations fit?

Relation between DM and baryons?

Evolution as function of mass?

Inside-out?

?

Galaxy Formation and Evolution

slide4

spatially resolved kinematics, morphologies, metallicities, ionization

dynamical masses, dynamical timescales, angular momentum

evolution of dynamics, star formation, metallicity

relationships between various high redshift samples

role of feedback, role of environmental effects

SINS

Survey of z ~ 1 – 4 galaxy populations from

NIR integral field spectroscopy with SINFONI @ VLT

To date: ~50 objects (BM/BX, BzK, K bright, LBGs, SMGs, ...)

slide5

SPIFFI

MACAO

(MPE/NOVA/ESO, P.I. F. Eisenhauer)

(ESO, P.I. H. Bonnet)

60-element curvature sensor AO system / bimorph mirror with APDs

Cryogenic integral field spectrometer with reflective image slicer

Natural & Laser Guide Star operations, seeing-limited mode

HAWAII 2RG 2k2 detector

3 pixel scales: 25, 100, 250 mas FOVs 0.80.8, 3.23.2, 88

4 gratings: J, H, K, H+KR ~ 2000 – 4500

Total throughput ~ 30%

Eisenhauer et al. (2003) Bonnet et al. (2004)

ESO PR 24b/04

SINFONI at the VLT

slide7

Q1307–BM1163

z=1.41

Q1623-BX376a

z=2.41

Q1623-BX447

z=2.15

Q1623-BX543

z=2.52

Q1623–BX455

z=2.41

Q1623–BX502

z=2.16

Q1623–BX528

z=2.27

Q1623–BX599

z=2.33

1

[NII]

[NII]

Q2343–BX610

z=2.21

Q2346–BX416

z=2.24

Q2346–BX404

z=2.03

Q1623–BX663

z=2.43

SSA22a–MD41

z=2.17

Q2343–BX389

z=2.17

Q2346–BX482

z=2.26

Q2346–BX405

z=2.03

[NII]

[NII]

[NII]

[NII]

500km/s

K20–ID5

z=2.23

K20–ID6

z=2.23

K20–ID7

z=2.22

K20–ID8

z=2.22

K20–ID9

z=2.04

BzK–6004

z=2.39

BzK–15504

z=2.38

SA12–6339

z=2.30

[OIII]

[OIII]

[NII]

[NII]

BzK–12556

z=1.59

SA12–5241

z=1.36

SA12–6192

z=1.51

SA15–5365

z=1.53

BzK–7144

z=1.65

[NII]

[NII]

[NII]

Q1422+231–d81

z=3.10

Q0347–383–c5

z=3.23

SMM14011+0252

z=2.56

SMM04431+0210

z=2.51

[OIII]

[OIII]

[NII]

[NII]

[NII]

[NII]

[OIII]

[OIII]

1

slide8

BX galaxies

FWHM ~ 0.5 – 0.6  ~ 4.5 kpc

Förster Schreiber et al. (2006)

(SINFONI sample drawn from Erb et al. 2006)

2D kinematics with SINFONI

Orbital motions at z~2

slide9

Rotation curves to r ~ 10 kpc at z ~ 2

15 BX galaxies at z~2.2

 local

late-type

spirals

rapid accretion/

gas exhaustion

gas-rich

<r1/2> = 4.4 kpc (range: 2–7 kpc)

<vc> = 180 ± 90 km s-1

Mdyn ~ (0.5 – 25) 1010 M

vc/σ ~ 2–4

j ~ 103 km s–1 kpc

dyn ~ 103 M pc–2

Förster Schreiber et al. (2006)

Properties of SINFONI BX sample

slide10

17

BzK–15504 at z  2.38

V=16.7

FWHM ~ 0.15  ~ 1.2 kpc

K=19.2

Genzel et al. (2006)

(Daddi et al. 2004; Kong et al. 2006)

2D kinematics with SINFONI+AO

slide11

Rel. offset (kpc)

250

180

130

110

60

30

-200

-150

-50

0

50

150

200

Rel. offset (arcsec)

Large, massive, gas-rich disk

0.5

0.5

Rel. offset (kpc)

Converting rapidly

v(Hα) (km/s)

σ(Hα) (km/s)

a significant fraction of

its baryonic mass into stars

Rel. offset (arcsec)

Rel. offset (kpc)

vc = 230 km s-1

r1/e 4.5 kpc

gas ~ 350 M pc–2

Mdyn  1.1  1011 M

vc/σ 3

M 0.8  1011 M

SFR ~ 1 M yr–1kpc–2

SFR ~ 150 M yr–1

Mgas 0.4  1011 M

~ gas~500 Myr

Rel. offset (arcsec)

A “Protodisk” at z~2

BzK–15504 at z  2.38

v(Hα) (km/s)

σ(Hα) (km/s)

Genzel et al. (2006)

slide12

Core (r  0.5 kpc)

Magnification ~20x

FWHM ~ 0.5  ~ 200 pc

~ bulges of local L* spirals

Mdyn ~ 2  109 M

dyn ~ 3  103 M pc–2

Dynamics on small scales

1E0657-56 Arc+Core: strongly lensed LBG at z  3.24

ACS F814W

Arc

8

Core

Forman-Jones et al.

SINFONI [OIII]

(greyscale)

R band (contours)

(Mehlert et al. 2001)

Nesvadba et al. (2006)

slide13

SINS: spatially-resolved studies at z ~ 1 – 4 with SINFONI

This talk:

Witnessing galaxy mass assembly in detail

Evidence for large, massive, gas-rich rotating disks at z~2–3

Significant amount of baryonic mass in central regions at z~2–3

Inside-out scenario

2 Gyr

38 kpc

Genzel et al. (2006)

Immeli et al. (2004)

Summary

slide14

[NII]

K continuum

1

[NII]/Hα

v (Hα)

Δv (Hα) (FWHM)

Förster Schreiber et al. (2006)

Spatially-resolved metallicity & SF

Q2343–BX610 at z = 2.21

slide15

Kcontinuum

continuum/Hα

0.07

0.25

1

0.19

[NII]

[NII]/Hα

[NII]/Hα

0.15

0.3

0.1

0.5

0.6

0.4

0.6

0.3

0.8

0.5

0.4

0.25

0

Genzel et al. (2006)

Spatially-resolved metallicity & SF

BzK–15504 at z = 2.38

slide16

Line maps

A

B

H

[OIII]5007

Velocity fields

C

C

B

A

[OIII]5007

H

Spatially-resolved metallicity & SF

Q2343–BX389 at z 2.17

slide17

nucleus

(θ=1”)

Lyα

CIV

HeII

CIII]

BzK-15504 (z=2.38)

Kong et al. 2006

Daddi et al. 2003, 2004

slide18

BX/K

Abadi et al. 2003

Rotation and angular momentum

slide19

model rotating exponential disk

flux

velocity

dispersion

  • Characteristic signatures of a rotating disk
  • maximum, smooth velocity gradient along morphogical major axis
  • velocity dispersion peaks at center of velocity gradient (and continuum peak if present)
  • ‘spider’ diagram of iso-velocity contours = sinosoidal variation of velocities as a function of disk angle
  • kinematic inclination = morphological inclination

Model rotating disk

slide20

3

1

BX405

8.3 kpc

Ks

BX404

SINFONI H (2h K-band)

Shapley et al. 2004; Erb et al. 2003, 2004

Förster Schreiber et al. 2006

BM/BX objects

BX 404/405 z = 2.03

slide21

v = –200 km/s

v = –100 km/s

v = 0 km/s

HST/WFPC2

v = +100 km/s

SINFONI Ha

v = +200 km/s

v = +300 km/s

1

8 kpc

Shapley et al. 2004; Erb et al. 2003, 2004

Förster Schreiber et al. (in prep.)

BM/BX objects

MD41 z = 2.17

H channel maps

slide22

[OIII]5007

HST/WFPC2

F702W

1

7.5 kpc

A

B

SINFONI (4h K-band)

A

B

[OIII] 5007 velocity field

SINFONI

Lyman-Break Galaxies

Q0347–383 C5 z = 3.23

Pettini et al. 2001

Nesvadba 2005 (PhD Thesis)

slide23

SINFONI

H line map (colours)

Line-free K continuum

n

J2

c

J2

se

J1

J1

ISAAC K-band

Line-free K continuum

WFPC2 F702W (contours)

SINFONI

2

SINFONI

5h40 K-band

1h30 H-band

1h10 J-band

Tecza et al. 2004; Nesvadba 2005 (PhD Thesis)

e.g. Ivison et al. 2001; Smail et al. 2005

Submm-selected Galaxies

SMMJ14011+0252 z = 2.56

n

slide24

J1

J2

H line map (colours)

J2

Line-free K continuum

J1

SINFONI

2

J1

J1

n

J2

J2

c

J2

se

J1

Submm-selected Galaxies

SMMJ14011+0252 z = 2.56

n

ISAAC K-band

Tecza et al. 2004; Nesvadba 2005 (PhD Thesis)

slide25

i = 20

i = 40

Exponential disk model

i = 60

M = 3  1010 M

i = 20° – 80°

scale length = 1

i = 80

thickness = 0.2

seeing  0.5

Model + noise

i = 80°

SNR(peak) = 7

Nesvadba 2005 (PhD Thesis)

Förster Schreiber et al. (in prep.)

Modelling

slide26

Smoothing

Voronoi binning

Smoothing

Voronoi binning

BX610

MD41

BX482

BzK-15504

Extracting robust 2D kinematics

… from IFS of z~2 galaxies

Shapiro 2006 (PhD Thesis)

Cresci et al.

slide27

Gas-rich mergers + vigorous feedback

140 kpc

Baryonic component

complex physical processes

(angular momentum exchange/loss,

cooling, feedback, ...)

2 Gyr

Robertson et al. (2005)

Gas-rich star-forming disk: disk fragmentation + bulge formation

38 kpc

Immeli et al. (2004)

Galaxy Formation and Evolution

slide28

Spiral

Elliptical

Frenk, Baugh, & Cole (1996)

smooth vs complex accretion…

angular momentum …

dissipative vs non-dissipative collapse

Galaxy Formation from Simulations

Mass accretion and star formation process

slide29

V-band morphologies: models vs data

Complex X-band morphologies in UDF

Immeli et al. (2004)

van den Bergh et al. (1996)

Elmegreen & Elmegreen (2005)

Observations vs Simulations