Galaxy Formation and Evolution since z = 1

Abstract

Determination of the star formation rate can be done using mid-IR photometry or Balmer line luminosity after a proper correction for extinction effects. Both methods show convergent results while those based on UV or on [OII]λ3727 luminosities underestimate the SFR by factors ranging from 5 to 40 for starbursts and for luminous IR galaxies, respectively. Most of the evolution of the cosmic star formation density is related to the evolution of luminous compact galaxies and to luminous IR galaxies. Because they were metal deficient and were forming stars at very high rates (40 to 100 M_⊙ yr^–1), it is probable that these (massive) galaxies were actively forming the bulk of their stellar/metal content at z ≤ 1.

Keywords

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