Journal Article

Cosmic evolution of the C <span class="smallCaps">iv</span> in high-resolution hydrodynamic simulations

E. Tescari, M. Viel, V. D'Odorico, S. Cristiani, F. Calura, S. Borgani and L. Tornatore

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 411, issue 2, pages 826-848
Published in print February 2011 | ISSN: 0035-8711
Published online February 2011 | e-ISSN: 1365-2966 | DOI: http://dx.doi.org/10.1111/j.1365-2966.2010.17761.x
Cosmic evolution of the C iv in high-resolution hydrodynamic simulations

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We investigate the properties of triply ionized carbon (C iv) in the intergalactic medium (IGM) using a set of high resolution and large box size cosmological hydrodynamic simulations of a Lambda cold dark matter (ΛCDM) model. We rely on a modification of the publicly available TreeSPH code gadget-2 that self-consistently follows the metal enrichment mechanism by means of a detailed chemical evolution model. We focus on several numerical implementations of galactic feedback: galactic winds in the energy-driven and momentum-driven prescriptions, galactic winds hydrodynamically coupled to the surrounding gas and active galactic nuclei (AGNs) powered by gas accretion on to massive black holes. Furthermore, our results are compared to a run in which galactic feedback is not present and we also explore different initial stellar mass function. After having addressed some global properties of the simulated volume like the impact on the star formation rate and the content in carbon and C iv, we extract mock IGM transmission spectra in neutral hydrogen (H i) and C iv and perform Voigt profile fitting. The results are then compared with high-resolution quasar (QSO) spectra obtained with the Ultraviolet Echelle Spectrograph (UVES) at the Very Large Telescope (VLT) and the High Resolution Echelle Spectrograph (HIRES) at Keck. We find that feedback has little impact on statistics related to the neutral hydrogen, while C iv is more affected by galactic winds and/or AGN feedback. The feedback schemes investigated have a different strength and redshift evolution with a general tendency for AGN feedback to be more effective at lower redshift than galactic winds. When the same analysis is performed over observed and simulated C iv lines, we find a reasonably good agreement between data and simulations over the column density range NC IV= 1012.5-15 cm−2. Also the C iv linewidth distribution appears to be in agreement with the observed values, while the H i Doppler parameters, bH I, are in general too large, showing that the diffuse cosmic web is heated more than what is inferred by observations. The simulation without feedback fails in reproducing the C iv systems at high column densities at all redshift, while the AGN feedback case agrees with observations only at z < 3, when this form of feedback is particularly effective. We also present scatter plots in the bN and in the NC IVNH I planes, showing that there is rough agreement between observations and simulations only when feedback is taken into account.

Although it seems difficult to constrain the nature and the strength of galactic feedback using the present framework and find a unique model that fits all the observations, these simulations offer the perspective of understanding the galaxy–IGM interplay and how metals produced by stars can reach the low-density IGM.

Keywords: methods: numerical; galaxies: formation; intergalactic medium; quasars: absorption lines; cosmology: theory

Journal Article.  13232 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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