Suchergebnisse

We introduce the Uchuu suite of large high-resolution cosmological N-body simulations. The largest simulation, named Uchuu, consists of 2.1 trillion (12 8003) dark matter particles in a box of side-length 2.0 h-1, Gpc$, with particle mass of 3.27 × 108, h-1, M⊙. The highest resolution simulation, Shin-Uchuu, consists of 262 billion (64003) particles in a box of side-length 140 h-1, Mpc, with particle mass of 8.97 × 105, h-1, M⊙. Combining these simulations, we can follow the evolution of dark matter haloes and subhaloes spanning those hosting dwarf galaxies to massive galaxy clusters across an unprecedented volume. In this first paper, we present basic statistics, dark matter power spectra, and the halo and subhalo mass functions, which demonstrate the wide dynamic range and superb statistics of the Uchuu suite. From an analysis of the evolution of the power spectra, we conclude that our simulations remain accurate from the baryon acoustic oscillation scale down to the very small. We also provide parameters of a mass-concentration model, which describes the evolution of halo concentration and reproduces our simulation data to within 5 per cent for haloes with masses spanning nearly eight orders of magnitude at redshift 0 ≤ z ≤ 14. There is an upturn in the mass-concentration relation for the population of all haloes and of relaxed haloes at z ≳ 0.5, whereas no upturn is detected at z < 0.5. We make publicly available various N-body products as part of Uchuu Data Release 1 on the Skies & Universes site. Future releases will include gravitational lensing maps and mock galaxy, X-ray cluster, and active galactic nucleus catalogues. © 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. ; The Uchuu simulations were carried out on Aterui II supercomputer at Center for Computational Astrophysics, CfCA, of National Astronomical Observatory of Japan, and the K computer at the RIKEN Advanced Institute for Computational Science (Proposal numbers hp180180, hp190161). The Uchuu DR1 effort has made use of the skun6@IAA facility managed by the IAA-CSIC in Spain, this equipment was funded by the Spanish MICINN EU-FEDER infrastructure grant EQC2018-004366-P. The skun@IAA_RedIRIS server was funded by the MICINN grant AYA2014-60641-C2-1-P. The numerical analysis was partially carried out on XC40 at the Yukawa Institute Computer Facility in Kyoto University. TI has been supported by MEXT via the 'Priority Issue on Post-K computer' (Elucidation of the Fundamental Laws and Evolution of the Universe), JICFUS, and MEXT via the 'Program for Promoting Researches on the Supercomputer Fugaku' (Toward a unified view of the universe: from large scale structures to planets, proposal numbers hp200124). TI thanks the support by MEXT/JSPS KAKENHI Grant Numbers JP17H04828, JP18H04337, JP19KK0344, and JP20H05245. FP, AK, and DM thank the support of the Spanish Ministry of Science and Innovation funding grant PGC2018-101931-B-I00. Parts of this research were conducted under the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. EJ acknowledges financial support from CNRS. FP and EJ want to thank a French–Spanish international collaboration grant from CNRS and CSIC. CVM acknowledges support from FONDECYT through grant 3200918, and he also acknowledges previous support from the Max Planck Society through a Partner Group grant. SAC acknowledges funding from Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET, PIP-0387), Agencia Nacional de Promoción de la Investigación, el Desarrollo Tecnológico y la Innovación (Agencia I+D+i, PICT-2018-03743), and Universidad Nacional de La Plata (G11-150), Argentina. ; With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709. ; Peer reviewed

We introduce the THE THREE HUNDRED project, an endeavour to model 324 large galaxy clusters with full-physics hydrodynamical re-simulations. Here we present the data set and study the differences to observations for fundamental galaxy cluster properties and scaling relations.We find that the modelled galaxy clusters are generally in reasonable agreement with observations with respect to baryonic fractions and gas scaling relations at redshift z = 0. However, there are still some (model-dependent) differences, such as central galaxies being too massive, and galaxy colours (g - r) being bluer (about 0.2 dex lower at the peak position) than in observations. The agreement in gas scaling relations down to 1013 h -1 M· between the simulations indicates that particulars of the sub-grid modelling of the baryonic physics only has a weak influence on these relations.We also include - where appropriate - a comparison to three semi-analytical galaxy formation models as applied to the same underlying dark-matter only simulation. All simulations and derived data products are publicly available. ; The work has received financial support from the European Union's Horizon 2020 Research and Innovation programme under the Marie Sklodowskaw-Curie grant agreement number 734374, i.e. the LACEGAL project14. The workshop where this work has been finished was sponsored in part by the Higgs Centre for Theoretical Physics at the University of Edinburgh´ WC, AK, GY and RM are supported by the Ministerio de Economía y Competitividad and the Fondo Europeo de Desarrollo Regional (MINECO/FEDER, UE) in Spain through grant AYA2015-63810-P. WC further thanks TaiLai Cui (崔泰莱) for all the joys. AK is also supported by the Spanish Red Consolider MultiDark FPA2017- 90566-REDC and further thanks Krog for making the days counts. CP acknowledges the Australia Research Council (ARC) Centre of Excellence (CoE) ASTRO 3D through project number CE170100013. PJE is supported by the ARC CoE ASTRO 3D through project number CE170100013. SB acknowledged financial support from PRIN-MIUR grant 2015W7KAWC, the agreement ASI-INAF n.2017-14-H.0, the INFN INDARK grant, the EU H2020 Research and Innovation Programme under the ExaNeSt project (Grant Agreement No. 671553). ER acknowledge the ExaNeSt and Euro Exa projects, funded by the European Union's Horizon 2020 research and innovation programme under grant agreement No 671553 and No 754337 and financial contribution from the agreement ASI-INAF n.2017-14-H.0. DS' fellowship is funded by the Spanish Ministry of Economy and Competitiveness (MINECO) under the 2014 Severo Ochoa Predoctoral Training Programme. J.V-F acknowledges the hospitality of the Physics & Astronomy Department at the University of Pennsylvania for hosting him during the preparation of this work. YW is supported by the national science foundation of China (No. 11643005). XY is supported by the National Key Basic Research Program of China (No. 2015CB857002), national science foundation of China (No. 11233005, 11621303). JTA acknowledges support from a postgraduate award from STFC. SAC acknowledges funding from Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET, PIP-0387), Agencia Nacional de Promoción Científica y Tecnológica (ANPCyT, PICT-2013- 0317), and Universidad Nacional de La Plata (G11-124), Argentina. CVM acknowledges CONICET, Argentina, for their supporting fellowships. ASB, GC and MDP are supported by Sapienza University of Rome-Progetti di Ricerca Anno 2016. ASB also acknowledges funding from Sapienza Universit_a di Roma under minor grant Progetti per Avvio alla Ricerca Anno 2017, prot. AR11715C82402BC7. RC is supported by the MERAC foundation postdoctoral grant awarded to Claudia Lagos and by the Consejo Nacional de Ciencia y Tecnología CONACYT CVU 520137 Scholar 290609 Overseas Scholarship 438594. SE acknowledges fi- nancial contribution from the contracts NARO15 ASI-INAF I/037/12/0, ASI 2015-046-R.0 and ASI-INAF n.2017-14- H.0. SEN is member of the Carrera del Investigador Científico of CONICET. SP is supported by the Fundamental Research Program of Presidium of the RAS #28. JS acknowledges support from the "Centre National d'etudes spatiales" (CNES) postdoctoral fellowship program as well as from the "l'Oreal-UNESCO pour les femmes et la Science" fellowship program