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ETHOS – an effective theory of structure formation: predictions for the high-redshift Universe – abundance of galaxies and reionization
Name
1711.10497.pdf
Description
Accepted version
Size
5.9 MB
Format
Adobe PDF
Checksum (MD5)
77f803599ba3d2cf200e56f5c8474a92
Author(s)
Lovell, Mark R
Zavala, Jesús
Vogelsberger, Mark
Shen, Xuejian
Cyr-Racine, Francis-Yan
Pfrommer, Christoph
Sigurdson, Kris
Boylan-Kolchin, Michael
Pillepich, Annalisa
Journal
Monthly Notices of the Royal Astronomical Society
Publisher
Oxford University Press (OUP)
Version
Author's final manuscript
Abstract
© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. We contrast predictions for the high-redshift galaxy population and reionization history between cold dark matter (CDM) and an alternative self-interacting dark matter model based on the recently developed ETHOS framework that alleviates the small-scale CDM challenges within the Local Group.We perform the highest resolution hydrodynamical cosmological simulations (a 36 Mpc3 volume with gas cell mass of ~105M⊙ and minimum gas softening of ~180 pc) within ETHOS to date - plus a CDM counterpart - to quantify the abundance of galaxies at high redshift and their impact on reionization. We find that ETHOS predicts galaxies with higher ultraviolet (UV) luminosities than their CDM counterparts and a faster build-up of the faint end of the UV luminosity function. These effects, however, make the optical depth to reionization less sensitive to the power spectrum cut-off: the ETHOS model differs from the CDM τ value by only 10 per cent and is consistent with Planck limits if the effective escape fraction of UV photons is 0.1-0.5. We conclude that current observations of high-redshift luminosity functions cannot differentiate between ETHOS and CDM models, but deep James Webb Space Telescope surveys of strongly lensed, inherently faint galaxies have the potential to test non-CDM models that offer attractive solutions to CDM's Local Group problems.
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Creative Commons Attribution-Noncommercial-Share Alike
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DOI of Published Version
10.1093/MNRAS/STY818
