Abstract
We compute and study the infrared and sub-mm properties of high redshift
(z>1) simulated clusters and proto-clusters, by coupling the results of a large
set of hydro-dynamical zoom-in simulations including active galactic nuclei
(AGN) feedback (Ragone-Figueroa et al. 2013), with the recently developed
radiative transfer code GRASIL3D (Dominguez-Tenreiro et al. 2014), which
accounts for the effect of dust reprocessing in an arbitrary geometry, and we
customized for the present purpose. While this field is in its infancy from the
observational point of view, a rapid development is expected in the near
future, thanks to observations performed in the far IR and sub-mm bands.
Notably, we find that in this spectral regime our prediction are little
affected by the assumption required by this post-processing, and the emission
is mostly powered by star formation rather than accretion onto super massive
black hole (SMBH). The comparison with the little observational information
available so far, highlights that the simulated cluster regions never attain
the impressive star formation rates suggested by these observations. This
problem becomes more intriguing taking into account that the brightest cluster
galaxies (BCGs) in the same simulations turns out to be too massive
(Ragone-Figueroa et al. 2013). It seems that the interplay between the feedback
schemes and the starformation model should be revised, possibly incorporating a
positive feedback mode.
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