1. A NEAR-INFRARED MULTIPLE-OBJECT INTEGRAL-FIELD SPECTROMETER FOR THE VLT The Science Case Matt Lehnert, MPE

2. Distant Galaxy Science Drivers Growth and dynamics of intermediate redshift clusters -- How do cluster galaxies grow and evolve? When was the morphology density put into place? What’s the role of “dry” vs. “wet” mergers? Can we see differences between cluster and field galaxies at high redshifts? Dynamics of intermediate and high redshift galaxies -- How do galaxies grow? Why were galaxies “downsized”? Gas accretion quasi-adiabatically or through merging? What is the source of angular momentum? Does it grow linearly with time? How did mass surface density evolve? Gas phase metal abundances and absorption lines in distant galaxies – What is the evolution of mass and metallicity? How was the ISM polluted with metals? Early enrichment? Metal distribution -- Is this consistent with “inside-out” galaxy formation models? Evolution of AGN – What is the relationship between the growth of BHs and growth of galaxies? Did this happen in “fits, stops, and starts”?

3. z 1 2 3 4 5 6 7 8 >9 Mg B G Band 4000Å Lyα He II [OII] HβHβ [OIII] HαHα CaT Iz-bands: 0.80-1.05 µm J band: 1.05-1.37 µm H band: 1.45-1.85µm K band: 1.95-2.50 µm SFR, extinction, dynamics metallicity, dynamics extinction, metallicity SFR, metallicity, density Pop III/AGN Reionization, escape fraction Stellar populations 

4. V(r,  ),  (r,  ),  v, M virial, f line (r,  ) J/M,v rot /σ etc. – not with photometry or slitlets Spatially-Resolved Properties v rot /  =f(M, z) & J/M = f(M, z) Mergers vs. Infall dM/dt =f(M, r, z) Superwinds & Self-regulation [O/H]=f(M, r, z)

5. Local Universe Science Drivers Stellar populations in the MW and other nearby galaxies. When did the disk form in other galaxies? What is the relationship between metallicity and dynamics for individual stars and clusters? What is the age and metallicity distribution of the stars in, for example, the GC. The dynamics of merging/interacting and star-bursting galaxies. Do the compact young clusters have the same ages as the background stars? Are the clusters long-lived? What fraction of the star-formation is in clusters? What about metallicity versus age – what is the mixing time scale for metals? The properties of stars embedded in their natal molecular cloud. What is the initial mass function? What is the impact of the stars on the surrounding nebula? IFUs are crucial for removing the nebular emission from stellar recombination lines.

6. Diagnostic lines in the Near-IR Ionization: [SiVI] and other highly ionized forbidden lines for AGN, Bracket and Paschen lines in emission, various HeI lines, H 2 vib-rotational lines for X-ray heating and PDR diagnostics, etc. Shocks: H 2 vib-rotational lines, FeII lines, etc. Ages, surface gravities, and temperatures of stars: CO- bandheads in the H and K bands, SiI, MgI (in the K and z- band), CaI, Bracket and Paschen lines in absorption, the Calcium triplet in the z-band, etc

7. Galaxy Number Counts Förster-Schreiber et al. (2004) and (2006)

8. K Selected Galaxies K Selected Galaxies Daddi et al. (2004) … highly efficient way of selecting distant galaxies … for 20 1.4 … about 4 sources arcmin -2 over 53 arcmin 2 … KMOS FOV

9. z  1-3 Star-Forming Galaxies Populating the “redshift desert” z=1.5-3.5 SFR  20-60 M  yr -1 [M/H]  0.8[M/H]  Selects only actively star-forming galaxies! Steidel et al. (2004)

10. Clustering of z~3 LBGs Steidel et al. (2000) 3.06<z spec <3.12 (24) “Narrow band excess” (72) “Giant Ly  blob” (2) … 162 objects that are likely to be associated …

11. Likely Sensitivity of KMOS In 8 hrs integration (1 night): 5  limits for compact galaxies and between OH lines are: J~22, H~21.2, K~19.4 … but with SINFONI, in 3 hours, at ~0.5” seeing, for … F H   1.7x10 -16 ergs s -1 cm -2 K s =19.2 5σ in 1 hour for SINFONI of: K~18.4 & F H   4x10 -17 ergs s -1 cm -2 µ H   4x10 -17 ergs s -1 arcsec -2 3 hours of total integration time BX galaxy at z=2.2101

12. Sensitivity Comparison in I/z bands KMOS has better sensitivity, better sampling, 3-D capability, and comparable or higher multiplex, and is more flexible … Stoichiometry for Cd 1-y Zn y Te

13. Galaxies in Pieces – Standard Model Dark matter distribution on 100s kpc scale. Abadi et al. (2002) Gill et al. (2004)

14. Merger Tree Frenk, Baugh, & Cole (1996) Ultimately: SpiralElliptical smooth vs complex … angular momentum … dissipative vs. non-dissipative collapse

15. Angular momentum problem Steinmetz & Navarro (2000) Galaxies have J Disk ≈ J Halo SPH plus N-body predict J that is too low

16. Formation of Disks in Mergers? Gas-rich mergers plus vigorous feedback Robertson et al. (2005) Predicts enough angular momentum, but needs robust feedback to keep disk from collapsing … No BH BH

17. Disk formation – accretion? forms individual clumps of ~few x 10 9 M  which coalesce to form a bulge in a few dynamical times … In highly dissipative accretion/collapse, disks are very unstable … Immeli et al. (2004) ~Gyr ~6 kpc Early insights: ELS ‘62, Silk (1977), Binney (1977), Ostriker & Rees (1977)

18. Disk formation – accretion … properties appear similar to model predictions … but which model … Elmegreen & Elmegreen (2005) Clumpy galaxies in the UDF …

19. 170 -170 2343-610 300 400 200 -170 170 SSA22-MD41 0 170 250 500 100 300 FWHM -200 200 v 1623-663 2346-482 -110 110 200 330 -60 1623-528 60 180 320 -60 Velocity fields of z~2 Galaxies Förster Schreiber, Genzel, Lehnert et al. (2006) In best cases: 2-D velocity field is smooth and consistent with orbital motion – rotating disks?

20. evidence for high μ K, metal-rich stellar population at the dynamical center of BX610 Q2343-BX610 Hα [NII] line-free K-continuum[NII]/Hα Range 0.25 - 0.55 Förster Schreiber et al. (2006) ≈dynamical center

21. Puech et al. (2006)Mergers Image Velocity map Dispersion map z~2 galaxy Model “analogued” Model “original”

22. Lensed LBG at z~3.2 ACS image F814W [OIII] image + R-band contours … a galaxy at high spatial resolution … ~200 pc at M~20 Nesvadba, Lehnert, et al. (2006a)

23. Lensed LBG at z~3.2 Offset (kpc) … a rotation curve at z~3.2 like a local galaxy … V (km s -1 ) Nesvadba, Lehnert, et al. (2006a)

24. Dark Matter Mass and Angular momentum If rotational support, compared to dark matter halos implies (Mo, Mao &White ‘98): M halo  10 11.7 (v c /180 kms -1 ) 3 (1+z/3.2) -1.5 M  j halo  10 2.8 0.05 (v c /180 kms -1 ) 2 (1+z/3.2) -1.5 km s -1 kpc j disk problem persists v circular  v virial since dynamical and clustering estimates are in rough agreement Abadi et al. (2003) z~2 Förster Schreiber, Genzel, Lehnert et al. (2006)

25. Summary of z~2-3 Galaxy Results ~ few x 10 10 M  v circular  v virial Σ dyn ~ few x 10 9 M  kpc -2 (M dyn /Area ½ ) J z~2 ~ J spiral local, angular momentum “in place” v/σ and angular momentum may imply rapid accretion “inside-out” galaxy formation scenario Emphasizing the role of gas accretion … and larger samples!!!!

26. LBGs at z>5 BDF1:10 z=5.774 8191.8Ǻ 8083.0Ǻ BDF2:19 z=5.645 7315.5Ǻ BDF1:18 z=5.017 8351.4Ǻ BDF1:19 z=5.870 7362.0Ǻ BDF1:26 z=5.056

27. HST VIz images of V-band “dropouts” S/N(Z)>5 S/N(I)>3 S/N(B) 26.3 V-I>1.7 (contaminants included) Median UV half-light-radii: 1kpc

28. Night Sky Problem … gaps in the night sky are used for narrow band searches … … KMOS not a particularly good redshift machine … … KMOS can be used to investigate their complex morphologies … R>3000 important for both night sky subtraction, HeII, and identifying source as Ly  emission R=3200

29. Stars in the Galactic Center 3D spectroscopy critical in removing nebular emission and absorption from stellar resonance and recombination lines

30. KMOS 3-D spectroscopy is crucial for studying in situ galaxy evolution; While emphasizing the distant galaxy science case, KMOS is flexible and can do a wide range of studies; The combination of large FOV, 2 dozen IFUs, and a flexible arm placement means that KMOS will be highly efficient at getting the most important targets in any science field; Will provide robust statistical samples w/ 3-D data.