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A NEAR-INFRARED MULTIPLE-OBJECT INTEGRAL-FIELD SPECTROMETER FOR THE VLT The Science Case

A NEAR-INFRARED MULTIPLE-OBJECT INTEGRAL-FIELD SPECTROMETER FOR THE VLT The Science Case. Matt Lehnert, MPE. Distant Galaxy Science Drivers. Growth and dynamics of intermediate redshift clusters -- How do cluster galaxies grow and evolve? When was the morphology density put

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A NEAR-INFRARED MULTIPLE-OBJECT INTEGRAL-FIELD SPECTROMETER FOR THE VLT The Science Case

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  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. Reionization, escape fraction Pop III/AGN SFR, metallicity, density extinction, metallicity metallicity, dynamics SFR, extinction, dynamics  Stellar populations z 1 2 3 4 5 6 7 8 >9 Lyα He II [OII] Hβ [OIII] Hα 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 4000Å G Band Mg B CaT

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

  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, H2 vib-rotational lines for X-ray heating and PDR diagnostics, etc. Shocks: H2 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 … highly efficient way of selecting distant galaxies … for 20 < K < 22, z>1.4 … about 4 sources arcmin-2 over 53 arcmin2 … KMOS FOV Daddi et al. (2004)

  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 3.06<zspec<3.12 (24) “Narrow band excess” (72) “Giant Ly blob” (2) … 162 objects that are likely to be associated … Steidel et al. (2000)

  11. Likely Sensitivity of KMOS BX galaxy at z=2.2101 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 … FH1.7x10-16 ergs s-1 cm-2 Ks=19.2 5σ in 1 hour for SINFONI of: K~18.4 & FH4x10-17 ergs s-1 cm-2 µH4x10-17 ergs s-1 arcsec-2 3 hours of total integration time

  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 Cd1-yZnyTe

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

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

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

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

  17. ~Gyr ~6 kpc Immeli et al. (2004) Disk formation – accretion? Early insights: ELS ‘62, Silk (1977), Binney (1977), Ostriker & Rees (1977) In highly dissipative accretion/collapse, disks are very unstable … forms individual clumps of ~few x 109 M which coalesce to form a bulge in a few dynamical times …

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

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

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

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

  22. Dark Matter Mass and Angular momentum If rotational support, compared to dark matter halos implies (Mo, Mao &White ‘98): Mhalo1011.7 (vc/180 kms-1)3 (1+z/3.2)-1.5 M jhalo102.8 0.05(vc/180 kms-1)2 (1+z/3.2)-1.5 km s-1 kpc • jdisk problem persists • vcircularvvirial since dynamical and clustering estimates are in rough agreement z~2 Abadi et al. (2003) Förster Schreiber, Genzel, Lehnert et al. (2006)

  23. Summary of z~2-3 Galaxy Results • <Mdyn> ~ few x 1010 M • vcircular vvirial • Σdyn ~ few x 109M kpc-2 (Mdyn/Area½) • Jz~2 ~ Jspirallocal, 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!!!!

  24. LBGs at z>5 8191.8Ǻ BDF1:10 z=5.774 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

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

  26. Night Sky Problem R=3200 … 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

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

  28. 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.

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