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annote = {Comment: Accepted for publication in MNRAS, 28 pages, 27 figures},  file = {arXiv\:1508.07888 PDF:/home/deparis/.zotero/zotero/ur7cam7o.default/zotero/storage/QIDW7PVE/Aubert et al. - 2015 - EMMA an AMR cosmological simulation code with rad.pdf:application/pdf;arXiv.org Snapshot:/home/deparis/.zotero/zotero/ur7cam7o.default/zotero/storage/XQ8H4EBF/1508.html:text/html},  }  @article{ocvirk_cosmic_2015,  title = {{Cosmic {Dawn} ({CoDa}): the {First} {Radiation}-{Hydrodynamics} {Simulation} of {Reionization} and {Galaxy} {Formation} in the {Local} {Universe}}},  volume = {1511},  shorttitle = {Cosmic {Dawn} ({CoDa})},  url = {http://adsabs.harvard.edu/abs/2015arXiv151100011O},  abstract = {Cosmic reionization by starlight from early galaxies affected their evolution, thereby impacting reionization, itself. Star formation suppression, for example, may explain the observed underabundance of Local Group dwarfs relative to N-body predictions for Cold Dark Matter. Reionization modelling requires simulating volumes large enough {\textasciitilde}(100 Mpc){\textasciicircum}3 to sample reionization patchiness, while resolving millions of galaxy sources above {\textasciitilde}10{\textasciicircum}8 Msun, combining gravitational and gas dynamics with radiative transfer. Modelling the Local Group requires initial cosmological density fluctuations pre-selected to form the well-known structures of the local universe today. Cosmic Dawn (CoDa) is the first such fully-coupled, radiation-hydrodynamics simulation of reionization of the local universe. Our new hybrid CPU-GPU code RAMSES-CUDATON, performs hundreds of radiative transfer and ionization rate-solver timesteps on the GPUs for each hydro-gravity timestep on the CPUs. CoDa simulated (91 Mpc){\textasciicircum}3 with 4096{\textasciicircum}3 particles and cells, to redshift 4.23, on ORNL supercomputer Titan, utilizing 8192 cores and 8192 GPUs. Global reionization ended slightly later than observed. However, a simple temporal rescaling which brings the evolution of ionized fraction into agreement with observations also reconciles ionizing flux density, cosmic star formation history, CMB electron scattering optical depth and galaxy UV luminosity function with their observed values. Haloes below {\textasciitilde}3 x 10{\textasciicircum}9 Msun were severely affected by the rising UV background: photoionization heating suppressed their star formation. For most of reionization, star formation was dominated by haloes between 10{\textasciicircum}10 - 10{\textasciicircum}11Msun. Intergalactic filaments display sheathed structures, with hot envelopes surrounding cooler cores, but do not self-shield, unlike regions denser than 100 rho\_average.},  urldate = {2015-12-07},  journal = {ArXiv e-prints},  author = {Ocvirk, Pierre and Gillet, Nicolas and Shapiro, Paul R. and Aubert, Dominique and Iliev, Ilian T. and Teyssier, Romain and Yepes, Gustavo and Choi, Jun-Hwan and Sullivan, David and Knebe, Alexander and Gottloeber, Stefan and D'Aloisio, Anson and Park, Hyunbae and Hoffman, Yehuda and Stranex, Timothy},  month = {oct},  year = {2015},  keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},  pages = {11},  }