Constraining neutrino mass remains an elusive challenge in modern physics.Precision measurements are expected from several upcoming cosmological probes of large-scale structure.Achieving this goal relies on an equal level of precision from theoretical predictions of neutrino clustering.Numerical simulations of the non-linear evolution of cold dark matter and neutrinos play a pivotal role in this process.We incorporate neutrinos into the cosmological N-body code CUBEP3M and discuss the challenges associated with pushing to the extreme scales demanded by the neutrino problem.We highlight code optimizations made to exploit modern high performance computing architectures and present a novel method of data compression that reduces the phase-space particle footprint from 24 bytes in single precision to roughly 9 bytes.We scale the neutrino problem to the Tianhe-2 supercomputer and provide details of our production run,named Tian Nu,which uses 86%of the machine(13 824 compute nodes).With a total of 2.97 trillion particles,Tian Nu is currently the world’s largest cosmological N-body simulation and improves upon previous neutrino simulations by two orders of magnitude in scale.We finish with a discussion of the unanticipated computational challenges that were encountered during the Tian Nu runtime.
最近的宇宙学观测结果给出了一个具有原初连续谱功率指数(RSI-CDM)的ΛCDM冷暗物质宇宙模型,而不是标准的尺度无关谱(PL-CDM).基于这个结果,应用半解析近似,对Jenkins et al(J01)质量方程进行了研究,同时在各个连续谱指数暗能量宇宙学模型下计算出这些模型对应的宇宙中最大暗物质晕的位里质量.结果表明,PL-CDM和RSI-CDM宇宙学模型在低红移处有微小差别.与PL-CDM相比,RSI-CDM在低红移处小质量暗晕的质量丰度较大,但在大结构质量晕中两者差别不明显,而且这个差异随着红移降低而增大.RSI-CDM在高红移处压低了任何尺度的暗晕质量丰度.关于最大位里质量,平坦空间ΛCDM宇宙学模型在PL-CDM和RSI-CDM都给出更多大质量天体.因此,对PL-CDM和RSI-CDM功率谱模型,都可以用最大位里质量来区别不同的宇宙学模型.
With large-scale homogeneity,the universe is locally inhomogeneous,clustering into stars,galaxies and larger structures.Such property is described by the smoothness parameter α which is defined as the proportion of matter in the form of intergalactic medium.If we consider the inhomogeneities over a small scale,there should be modifications of the cosmological distances compared to a homogenous model.Dyer and Roeder developed a second-order ordinary differential equation（D-R equation） that describes the angular diameter distance-redshift relation for inhomogeneous cosmological models.Furthermore,we may obtain the D-R equation for observational H（z） data（OHD）.The density-parameter ΩM,the state of dark energy ω,and the smoothness-parameter α are constrained by a set of OHD in a spatially flat XCDM universe as well as a spatially flat XCDM universe.By using a χ2 minimization method,we get α = 0.81＋0.19-0.20 and ΩM = 0.32＋0.12-0.06 at the 1σ confidence level.If we assume a Gaussian prior of ΩM = 0.26 ± 0.1,we get α = 0.93＋0.07-0.19 and ΩM = 0.31＋0.06-0.05.For the XCDM model,α is constrained to α≥ 0.80 but ω is weakly constrained around-1,where ω describes the equation of state of the dark energy（pX = ωρX）.We conclude that OHD constrains the smoothness parameter more effectively than the data of SNe Ia and compact radio sources.
Hao-Ran Yu1,Tian Lan1,Hao-Yi Wan2,Tong-Jie Zhang1,3 and Bao-Quan Wang4 1 Department of Astronomy,Beijing Normal University,Beijing 100875,China 2 Business Office,Beijing Planetarium,Beijing 100044,China 3 Center for High Energy Physics,Peking University,Beijing 100871,China 4 Department of Physics,Dezhou University,Dezhou 253023,China
