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Rest-Frame near-IR Luminosity Evolution of Early-Type Galaxies

Rest-Frame near-IR Luminosity Evolution of Early-Type Galaxies. Arjen van der Wel – JHU Baltimore. Marijn Franx - Leiden Pieter van Dokkum - Yale Jiasheng Huang - Harvard Hans-Walter Rix - MPIA Garth Illingworth - UCSC Stijn Wuyts - Leiden.

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Rest-Frame near-IR Luminosity Evolution of Early-Type Galaxies

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  1. Rest-Frame near-IR Luminosity Evolution of Early-Type Galaxies Arjen van der Wel – JHU Baltimore

  2. Marijn Franx - LeidenPieter van Dokkum - YaleJiasheng Huang - HarvardHans-Walter Rix - MPIAGarth Illingworth - UCSCStijn Wuyts - Leiden

  3. The optical FP at z~1 in the CDFS- IRAC GTO observations- Rest-frame near-IR L-evolution- Optical and near-IR colors and M/L: observations and models

  4. Redshift/magnitude/color/morphology selection GOODS ACS imaging (Giavalisco et al. 2004); COMBO-17 photo-z’s (Wolf et al. 2003); Coleman et al. 1980 template spectra

  5. All: Δ ln (M/LB) / z = ( -1.66 +/- 0.08 ) M > 2 ∙1011 Msun: Δ ln (M/LB) / z = ( -1.15 +/- 0.12 )

  6. M vs. M/L of distant field galaxies

  7. Massive early-types evolve slowly, independent of environment- Early-type galaxies show mass-dependent luminosity evolution.- We do not have an un-biased view on evolution of L* early-types because of selection effects.

  8. GTO IRAC data • 500s exposures • PSF matching • ACS, ISAAC (from ESO), IRAC data • rest-frame B-through-K band colors • comparison with local FP sampe • (Pahre et al. 1998) •  rest-frame K-band luminosity evolution

  9. Evolution of M/LK Δ ln ( M/LK ) / z = -1.18 +/- 0.10 Δ ln ( M/LB ) / z = -1.46 +/- 0.09

  10. Evolution in B vs. Evolution in K

  11. Top-Heavy IMF?

  12. Dusty, young populations?

  13. Conclusions • - K-band L-evolution: 1.3 mag at z=1 • - K-band luminosity is not a mass indicator • Bruzual & Charlot (2003) model: • Problems in the near-IR • Maraston (2005) model: • Problems in the optical

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