Welcome to the new version of CaltechAUTHORS. Login is currently restricted to library staff. If you notice any issues, please email coda@library.caltech.edu
Published June 11, 2016 | Submitted + Published
Journal Article Open

Large-scale mass distribution in the Illustris simulation

Abstract

Observations at low redshifts thus far fail to account for all of the baryons expected in the Universe according to cosmological constraints. A large fraction of the baryons presumably resides in a thin and warm–hot medium between the galaxies, where they are difficult to observe due to their low densities and high temperatures. Cosmological simulations of structure formation can be used to verify this picture and provide quantitative predictions for the distribution of mass in different large-scale structure components. Here we study the distribution of baryons and dark matter at different epochs using data from the Illustris simulation. We identify regions of different dark matter density with the primary constituents of large-scale structure, allowing us to measure mass and volume of haloes, filaments and voids. At redshift zero, we find that 49 per cent of the dark matter and 23 per cent of the baryons are within haloes more massive than the resolution limit of 2 × 108 M⊙. The filaments of the cosmic web host a further 45 per cent of the dark matter and 46 per cent of the baryons. The remaining 31 per cent of the baryons reside in voids. The majority of these baryons have been transported there through active galactic nuclei feedback. We note that the feedback model of Illustris is too strong for heavy haloes, therefore it is likely that we are overestimating this amount. Categorizing the baryons according to their density and temperature, we find that 17.8 per cent of them are in a condensed state, 21.6 per cent are present as cold, diffuse gas, and 53.9 per cent are found in the state of a warm–hot intergalactic medium.

Additional Information

© 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2016 January 8. Received 2015 December 21. In original form 2015 August 6. First published online February 24, 2016. MH and DS thank their colleagues at the Institute for Astro- and Particle Physics at the University of Innsbruck for usefull discussions, especially Francine Marleau, Dominic Clancy, Rebecca Habas and Matteo Bianconi. DS acknowledges the research grant from the office of the vice rector for research of the University of Innsbruck (project DB: 194272) and the doctoral school – Computational Interdisciplinary Modelling FWF DK-plus (W1227). This work was supported by the Austrian Federal Ministry of Science, Research and Economy as part of the UniInfrastrukturprogramm of the Focal Point Scientific Computing at the University of Innsbruck. SG acknowledges support provided by NASA through Hubble Fellowship grant HST-HF2-51341.001-A awarded by the STScI, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. VS acknowledges support through the European Research Council through ERC-StG grant EXAGAL-308037.

Attached Files

Published - stw077.pdf

Submitted - 1508_01525.pdf

Files

1508_01525.pdf
Files (15.6 MB)
Name Size Download all
md5:75d516469950c0dceca06014d75c65a2
9.9 MB Preview Download
md5:ec78105e28e494d2cd7d665807988079
5.6 MB Preview Download

Additional details

Created:
September 28, 2023
Modified:
October 24, 2023