SINS high redshift galaxy Spectroscopic Imaging survey in the Near-IR with SINFONI N.M. Förster Schreiber SINS SINFONI GTO science program on high redshift galaxies MPE-IR/Submm Group, USM/MPE Group, NOVA.
Download ReportTranscript SINS high redshift galaxy Spectroscopic Imaging survey in the Near-IR with SINFONI N.M. Förster Schreiber SINS SINFONI GTO science program on high redshift galaxies MPE-IR/Submm Group, USM/MPE Group, NOVA.
SINS high redshift galaxy Spectroscopic Imaging survey in the Near-IR with SINFONI N.M. Förster Schreiber 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.E. Shapley, D.K. Erb, C.C. Steidel Princeton/CfA/Caltech A. Cimatti, E. Daddi, A. Renzini, X. Kong, V. Mignoli, N. Arimoto Bologna/CEA Saclay/Padova/Hefei China/NAO Japan Galaxy Formation and Evolution Open issues... Angular momentum? Baryonic mass accretion? Inside-out? Connection between bulge and disk formation? Timescales? Star formation efficiency? Evolution as function of mass? Dissipation? Feedback? Environment? Relation between DM and baryons? Where do observed populations fit? SINS Survey of z ~ 1 – 4 galaxy populations from NIR integral field spectroscopy with SINFONI @ VLT 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 To date: ~50 objects (BM/BX, BzK, K bright, LBGs, SMGs, ...) SINFONI at the VLT SPIFFI (MPE/NOVA/ESO, P.I. F. Eisenhauer) Cryogenic integral field spectrometer with reflective image slicer HAWAII 2RG 2k2 detector 3 pixel scales: 25, 100, 250 mas FOVs 0.80.8, 3.23.2, 88 4 gratings: J, H, K, H+K R ~ 2000 – 4500 Total throughput ~ 30% MACAO (ESO, P.I. H. Bonnet) 60-element curvature sensor AO system / bimorph mirror with APDs Natural & Laser Guide Star operations, seeing-limited mode Eisenhauer et al. (2003) Bonnet et al. (2004) ESO PR 24b/04 SPIFFI:3D principle 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] Q1623–BX663 z=2.43 SSA22a–MD41 z=2.17 Q2343–BX389 z=2.17 Q2343–BX610 z=2.21 Q2346–BX416 z=2.24 Q2346–BX482 z=2.26 Q2346–BX404 z=2.03 Q2346–BX405 z=2.03 1 [NII] K20–ID5 z=2.23 [OIII] BzK–7144 z=1.65 [NII] K20–ID6 z=2.23 K20–ID7 z=2.22 [NII] K20–ID8 z=2.22 [NII] K20–ID9 z=2.04 BzK–6004 z=2.39 [OIII] BzK–12556 z=1.59 SA12–6192 z=1.51 [NII] SA15–5365 z=1.53 Q0347–383–c5 z=3.23 SA12–6339 z=2.30 BzK–15504 z=2.38 [NII] SA12–5241 z=1.36 500km/s [NII] [NII] Q1422+231–d81 z=3.10 SMM14011+0252 SMM04431+0210 z=2.56 z=2.51 [NII] [OIII] [OIII] [OIII] [OIII] [NII] [NII] [NII] [NII] 2D kinematics with SINFONI Orbital motions at z~2 BX galaxies FWHM ~ 0.5 – 0.6 ~ 4.5 kpc Förster Schreiber et al. (2006) (SINFONI sample drawn from Erb et al. 2006) Properties of SINFONI BX sample 15 BX galaxies at z~2.2 Rotation curves to r ~ 10 kpc at z ~ 2 <vc> = 180 ± 90 km s-1 <r 1/2> = 4.4 kpc (range: 2–7 kpc) 10 M dyn ~ (0.5 – 25) 10 M 3 –2 dyn ~ 10 M pc Förster Schreiber et al. (2006) j~ 103 km s–1 kpc vc/σ ~ 2–4 local late-type spirals rapid accretion/ gas exhaustion gas-rich 2D kinematics with SINFONI+AO BzK–15504 at z 2.38 17 V=16.7 K=19.2 Genzel et al. (2006) (Daddi et al. 2004; Kong et al. 2006) FWHM ~ 0.15 ~ 1.2 kpc A “Protodisk” at z~2 Rel. offset (kpc) BzK–15504 at z 2.38 vc = 230 km s-1 r 1/e 4.5 kpc v /σ 3 c Rel. offset (arcsec) Rel. offset (kpc) Large, massive, gas-rich disk Converting rapidly a significant fraction of its baryonic mass into stars Rel. offset (arcsec) Rel. offset (kpc) 250 180 130 110 -200 -150 0.5 v(Hα) (km/s) -50 0 50 60 150 σ(Hα)0.5 (km/s) 30 200 Rel. offset (arcsec) Genzel et al. (2006) v(Hα) (km/s) Mdyn 1.1 1011 M 11 M 0.8 10 M 11 M gas 0.4 10 M –2 gas ~ 350 M pc ~ gas ~ 500 Myr –1 SFR ~ 150 M yr –1 –2 SFR ~ 1 M yr kpc σ(Hα) (km/s) Dynamics on small scales 1E0657-56 Arc+Core: strongly lensed LBG at z 3.24 Core (r 0.5 kpc) ACS F814W Arc Magnification ~20x FWHM ~ 0.5 ~ 200 pc Mdyn ~ 2 109 M 3 –2 dyn ~ 3 10 M pc ~ bulges of local L* spirals 8 Core Forman-Jones et al. SINFONI [OIII] (greyscale) R band (contours) (Mehlert et al. 2001) Nesvadba et al. (2006) Summary SINS: spatially-resolved studies at z ~ 1 – 4 with SINFONI Witnessing galaxy mass assembly in detail This talk: 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) Spatially-resolved metallicity & SF Q2343–BX610 at z = 2.21 Hα [NII] [NII]/Hα v (Hα) K continuum 1 Förster Schreiber et al. (2006) Δv (Hα) (FWHM) Spatially-resolved metallicity & SF BzK–15504 at z = 2.38 Hα K continuum continuum/Hα 0.07 0.25 1 0.19 [NII] [NII]/Hα 0.15 [NII]/Hα 0.3 0.1 0.4 0.5 0.6 0.6 0.3 0.8 0.4 0.5 0.25 0 Genzel et al. (2006) Spatially-resolved metallicity & SF Q2343–BX389 at z 2.17 Line maps A B H C [OIII]5007 Velocity fields H [OIII]5007 C B A flux 6 CIV 4 HeII CIII] 2 normalised flux nucleus (θ=1”) Lyα 0 1200 1400 1600 1800 2000 rest wavelength 1.0 normalised flux 0.8 normalised flux BzK-15504 (z=2.38) 8 Kong et al. 2006 Daddi et al. 2003, 2004 0.6 0.4 0.2 0.0 -3000 -2000 -1000 0 1000 2000 velocity offset (km/s) 3000 Rotation and angular momentum BX/K Abadi et al. 2003 Model rotating disk 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 BM/BX objects BX 404/405 z = 2.03 3 30 1 BX405 20 flux 8.3 kpc Ks 10 0 -1000 0 1000 velocity offset (rel. to z=2.03) BX404 H 30 30 10 [NII] [NII] 20 flux flux 20 0 -1000 0 1000 velocity offset (rel. to z=2.03) Shapley et al. 2004; Erb et al. 2003, 2004 Förster Schreiber et al. 2006 SINFONI H (2h K-band) 10 0 -1000 0 1000 velocity offset (rel. to z=2.03) BM/BX objects MD41 z = 2.17 1 8 kpc v = –200 km/s v = –100 km/s H channel maps v = 0 km/s v = +100 km/s SINFONI Ha v = +200 km/s v = +300 km/s HST/WFPC2 Shapley et al. 2004; Erb et al. 2003, 2004 Förster Schreiber et al. (in prep.) Lyman-Break Galaxies [OIII]5007 Q0347–383 C5 z = 3.23 1 7.5 kpc HST/WFPC2 F702W A B SINFONI (4h K-band) [OIII] 5007 velocity field SINFONI Pettini et al. 2001 Nesvadba 2005 (PhD Thesis) A B Submm-selected Galaxies SMMJ14011+0252 z = 2.56 2 n SINFONI H line map (colours) Line-free K continuum J2 c se J1 J2 J1 ISAAC K-band Line-free K continuum WFPC2 F702W (contours) SINFONI n 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 H line map (colours) Line-free K continuum J1 J2 J1 J2 SMMJ14011+0252 z = 2.56 SINFONI 2 J1 J1 n J2 n se J2 c J2 J1 ISAAC K-band Tecza et al. 2004; Nesvadba 2005 (PhD Thesis) Modelling i = 20 i = 40 Exponential disk model i = 60 i = 80 Model + noise i = 80° SNR(peak) = 7 Nesvadba 2005 (PhD Thesis) Förster Schreiber et al. (in prep.) M = 3 1010 M i = 20° – 80° scale length = 1 thickness = 0.2 seeing 0.5 Extracting robust 2D kinematics … from IFS of z~2 galaxies Smoothing Voronoi binning Smoothing Voronoi binning BX610 MD41 BX482 BzK-15504 Shapiro 2006 (PhD Thesis) Cresci et al. Galaxy Formation and Evolution Gas-rich mergers + vigorous feedback 140 kpc Baryonic component complex physical processes (angular momentum exchange/loss, cooling, feedback, ...) Robertson et al. (2005) Gas-rich star-forming disk: disk fragmentation + bulge formation 2 Gyr 38 kpc Immeli et al. (2004) Galaxy Formation from Simulations Mass accretion and star formation process Spiral Elliptical Frenk, Baugh, & Cole (1996) smooth vs complex accretion… angular momentum … dissipative vs non-dissipative collapse Observations vs Simulations V-band morphologies: models vs data Complex X-band morphologies in UDF Elmegreen & Elmegreen (2005) Immeli et al. (2004) van den Bergh et al. (1996)