Search

Deep imaging in the rest-frame UV has constrained both the evolution of the cosmic star formation rate density [1] and its time integral, the growth of the cosmic stellar mass density [2]. Short-wavelength studies give an incomplete picture, however, since an important population of high-redshift galaxies is heavily dust-obscured. The strength of the extragalactic mid- and far-IR/submillimeter background indicates that about half of the cosmic energy density comes from dusty luminous and ultra-luminous infrared galaxies (LIRGs/ULIRGs: LIR ~ 1011.5 to 1013.5L⊙) at z ≥ 1 [3,4]. Because the brightest of these submillimeter galaxies (SMGs; see [5] and references therein) tend to lack strong X-ray emission [6], their large IR luminosities probably correspond to high star formation rates [7]. As the strikingly different appearances of the Hubble Deep Field at 0.83 μm [8] and 850 μm [9] exemplify, SMGs are rarer and forming stars much more intensely than typical optically selected systems [8,9]. Here we discuss new observations that shed light on the importance of SMGs in the history of galaxy mass assembly (all numbers assuming a flat ΩΛ = 0.7 cosmology with H0 = 70 km s-1 Mpc-1). [ABSTRACT FROM AUTHOR]

Using the near-infrared integral-field spectrograph SINFONI on the VLT, we studied the spatially-resolved dynamics in the optical emission line gas around the z = 2.2 powerful radio galaxy MRC1138-262, a likely progenitor of the massive low-z galaxy population. Velocities and FWHMs of up to 2400 km s-1 indicate an outflow driven by energies similar to the energy output of the AGN and fulfilling tight evolutionary constraints set by massive low-z galaxies. Is this the "smoking gun" of high-z AGN feedback? High-z AGN feedback plays a major role in recent cosmological simulations, but observational constraints are still missing. [ABSTRACT FROM AUTHOR]