Mass, Metallicity and Dynamics in high redshift galaxies

Transcription

1 Mass, Metallicity and Dynamics in high redshift galaxies Filippo Mannucci IRA-INAF, Arcetri R. Maiolino, T. Nagao, A. Marconi, G. Cresci L. Pozzetti, M. Lehnert, A. Fontana, S. Ballero, A. Cimatti, G.L. Granato, F. Matteucci, G. Pastorini, L. Pentericci, A. Pipino, G. Risaliti, M. Salvati, L. Silva Ringberg 30/10/2007 LGS

2 Problems with high-redshift galaxies How and when galaxies of different masses formed Mass assembly and star formation Inflows and outflows Merging: dry and wet Origin of different morphologies Morphological segregation (early type in clusters) Interplay among different type of galaxies at high- and lowredshifts (E, S, Irr, vs. LBG, SMG, DRG, LyαG.) 1. Dependence of the evolution with mass 2. Detailed structure of local and high redshift galaxies

3 Morphology and Dynamics Mass: 1- Dark 2- Stellar 3- Gas Dark halo mass - directly linked to theory Gas/Stellar = evolutionary stage Velocity / mass / size relations, angular momentum Morphologies, spatially resolved stellar populations LBG: progenitors of ETG or subgalactic clumps? LARGE: theory: Mo et al clustering: Aldelberger et al. 1998, 2005 dynamics: Pettini et al., 2001, Erb et al., 2003 SMALL: theory: Somerville et al clustering: Wechsler et al dynamics: Weatherley & Warren 2003, 2005 Total dimensions: ~1 arcsec high spatial resolution Cresci et al. (2006), Bouche et al. (2007), Förster Schreiber et al (2006), Genzel et al. (2006), Rix et al. (1998), Lehnert et al., 1996, Pettini et al. (2001), Erb et al. (2003, 2006), Weatherley & Warren 2003, 2005, Lemoine-Busserolle et al (2002), Moorwood et al. (2003), Shapley et al.

4 Mass-metallicity relation Integrated properties of star formation Evolutionary stage Sensitive to in/outfows and merging SDSS galaxies Tremonti et al. (2004) Drivers: 1. Mass loss? 2. Downsizing? 3. IMF? Evolution with redshift Spitzer 8µm M82 Sun LMC SMC Engelbracht+06

5 Mass-metallicity relation z=0.1 Tremonti+ (2004) z=0.4 Savaglio+ (2005) z=0.75 Maiolino+ (2007) z=2.2 Erb+ (2006) ricalib. Caveats: 1. Effect of dust extinction 2. Mass determination 3. Different diagnostics at different redshifts 4. Two branches for R23 Kolbuniki & Kewley 2004, Shapley et al. 2004, Maier et al. 2004, Meyer et al. 2006, Rix et al. 2004, Erb et al. 2006, Bouchet et al. 2006,2007 Dalcanton et al. 2006, Dave et al. 2007, De Lucia et al. 2004, De Rossi et al. 2007, Brooks et al. 2007, Cid Fernandez et al Tissera et al. 2005, Kobayashi et al. 2006, Kewley et al. 2005, Koppen et al. 2007, Ferrara et al. 2005, Galazzi et al. 2006, Forster-Schreiber+ 2006, Liang et al. 2006

6 Morphology, Metallicity and Dynamics z>3: large evolution of the model expectations from z=0 M * ~0.1 of local value Before the peak of cosmic star formation (z~ ) Metallicity: [OII] in H, [OIII] in K, no Ha Large spectral coverage More robust (gas) metallicity estimators

7 Measuring metallicity F λ [OII] H+K band at 3<z<3.6 [OIII] Hβ Hα R 23 = ([OII]+[OIII])/Hβ log(O/H) [OIII] / [OII] log(O/H) [NeIII] Hγ [NII] [SII] [OIII] / Hβ 10 [NeIII] / [OII] wavelength (Å) log(O/H) Nagao log(O/H)

8 Morphology, Metallicity and Dynamics z>3: large evolution of the model expectations from z=0 M * ~0.1 of local value) Before the peak of cosmic star formation Metallicity: [OII] in H, [OIII] in K, no Ha Large spectral coverage More robust (gas) metallicity estimators High spatial resolution to resolve small galaxies Beyond SINS.

9 LSD LBG Stellar populations and Dynamics 10 UV-selected LBGs at z~3, R<25 (Steidel et al. sample) NGS Adaptive Optics Near bright stars No other selections: representative of the full LBG sample PI: F. Mannucci; CoIs: R. Maiolino, A. Marconi, G. Cresci L. Pozzetti, M. Lehnert

10 LSD LBG Stellar populations and Dynamics R AB ~24.5 K AB ~23.5 ESO/VLT, 66h SINFONI, IFU, adaptive optics, resolution~0.10 R=1500 Status: 100% complete, excellent quality, data analysis ongoing 1. Dynamics 2. Metallicity

11 Dynamics Seeing 0.6 AO NTT arcsec arcsec arcsec

12 Dynamics

13 Dynamics

14 Dynamics

15 Dynamics WORK IN PROGRESS Merging events are very common at z=3 Not so many large, rotationally supported disks compact systems Stellar mass densities similar to (but lower than) the local ellipticals

16 AMAZE Assessing the Mass-Metallicity Redshift Evolution ESO large project (P78,79, ), 180h, SINFONI PI: R. Maiolino CoIs: T. Nagao, A. Marconi, A. Fontana, A. Grazian, S. Ballero, A. Cimatti, G.L. Granato, F. Mannucci, F. Matteucci, G. Pastorini, L. Pentericci, A. Pipino, G. Risaliti, M. Salvati, L. Silva 30 targets: 22 galaxies at 3.2<z<3.8, 8 galaxies at 4.5<z<5.2 Seeing limited (aaargh!) 1

17 Determination of the metallicity

18 Evolution of the Mass-Metallicity relation z~0.1 (Tremonti+04) gas metallicity: 12+log(O/H) z~0.7 (CDFS and Savaglio+05, recalib.) z~2.2 (Erb+06, recalib.) z~3.3 AMAZE + LSD log M(stars) [M ] Maiolino+08 Mannucci +08

19 Comparison with hierarchical models Kobayashi, Springel & White 2007 model observations ~ bad

20 Comparison with hierarchical models of disk formation Brooks et al model observations good (?)

21 Step forward: Metallicity gradients 13 Gyr Chiappini Gyr bulge 2.5 Gyr Mollla + 97 Chiappini+ 01 disk Fingerprint of galaxy evolution: 1. Radial dependence of star formation history 2. Radial dependence of gas accretion 3. Stellar winds 4. Dynamic Metallicity mixing Put together spatially resolved evidences on kinematics, morphology and metallicity Special objects

22 Metallicity gradients F z = 3.47 E 1 F E A A B C D 0.6 seeing B C D HST-ACS I-band λ rest ~2000 Å [OIII]5007 metallicity map Z/Z

23 The role of LGS 1. Sky coverage: 1. Dedicated surveys (SWAN, Cresci et al., 2006) 2. larger samples: Steidel LBGs, ~1000 galaxies, normal extragal. fields Limit mag Dist ( ) Number Further selections Rare interesting objects (gravitational lenses) 3. Rare peculiar objects 4. brighter objects! 2. Larger corrections: natural stars are always faint and 30 away! 3. More stable and known PSFs

24 Conclusions and future work for LGS Deep integral-field spectroscopy in capable to shed new light on high redshift galaxies Evidence of strong evolution of the mass-metallicity relation at z>3, challenging the models Importance of having spatially resolved spectra: Comparison stellar and dynamical mass Mass/velocity/size relations Importance of mergers Further work on LBG possible only with LGSs Metallicity maps

25 Comparison with hierarchical models De Rossi, Tissera & Scannapieco 2007 model observations ~ bad