The Quijote simulations are a set of 44,100 full N-body simulations spanning
more than 7,000 cosmological models in the $\{\Omega_{\rm m}, \Omega_{\rm b},
h, n_s, \sigma_8, M_\nu, w \}$ hyperplane. At a single redshift the simulations
contain more than 8.5 trillions of particles over a combined volume of 44,100
$(h^{-1}{\rm Gpc})^3$; each simulation follow the evolution of $256^3$, $512^3$
or $1024^3$ particles in a box of $1~h^{-1}{\rm Gpc}$ length. Billions of dark
matter halos and cosmic voids have been identified in the simulations, whose
runs required more than 35 million core hours. The Quijote simulations have
been designed for two main purposes: 1) to quantify the information content on
cosmological observables, and 2) to provide enough data to train machine
learning algorithms. In this paper we describe the simulations and show a few
of their applications. We also release the Petabyte of data generated,
comprising hundreds of thousands of simulation snapshots at multiple redshifts,
halo and void catalogs, together with millions of summary statistics such as
power spectra, bispectra, correlation functions, marked power spectra, and
estimated probability density functions.

该论文描述了一组称为 Quijote 模拟的 N 体模拟，涵盖了超过 7000 种不同的宇宙学模型，并为夸克和重子物质、暗物质、暗能量、弱引力透镜等宇宙学观测量提供了足够的数据，可以在机器学习算法中使用，同时，还发布了千兆字节的数据，包括多个红移快照、暗物质晕和宇宙空洞目录，以及数百万个摘要统计量。

Quijote 模拟

The Quijote simulations

We propose an efficient analytical method for estimating the luminosity
distance in a homogenous Friedmann-Lema\^itre-Robertson-Walker (FLRW) model of
the Universe. This method is based on the homotopy perturbation method (HPM),
which has high accuracy in many nonlinear problems, and can be easily
implemented. For analytical calculation of the luminosity distance, we offer to
proceed not from the computation of the integral, which determines it, but from
the solution of a certain differential equation with corresponding initial
conditions. Solving this equation by means of HPM, we obtain the approximate
analytical expressions for the luminosity distance as a function of redshift
for two different types of homotopy. Possible extension of this method to other
cosmological models is also discussed.

本论文提出了基于同伦摄动法的高效分析方法，用于估计宇宙均质弗里德曼 - 勒梅特 - 罗伯逊 - 沃克模型（FLRW）中的亮度距离，并探讨了该方法推广到其他宇宙模型的可能性。

利用同伦摄动方法计算 FLRW 宇宙学中的红移与亮度距离

Calculating Luminosity Distance versus Redshift in FLRW Cosmology via  Homotopy Perturbation Method

Modern sky surveys are returning precision measurements of cosmological
statistics such as weak lensing shear correlations, the distribution of
galaxies, and cluster abundance. To fully exploit these observations, theorists
must provide predictions that are at least as accurate as the measurements, as
well as robust estimates of systematic errors that are inherent to the modeling
process. In the nonlinear regime of structure formation, this challenge can
only be overcome by developing a large-scale, multi-physics simulation
capability covering a range of cosmological models and astrophysical processes.
As a first step to achieving this goal, we have recently developed a prediction
scheme for the matter power spectrum (a so-called emulator), accurate at the 1%
level out to k~1/Mpc and z=1 for wCDM cosmologies based on a set of
high-accuracy N-body simulations. It is highly desirable to increase the range
in both redshift and wavenumber and to extend the reach in cosmological
parameter space. To make progress in this direction, while minimizing
computational cost, we present a strategy that maximally re-uses the original
simulations. We demonstrate improvement over the original spatial dynamic range
by an order of magnitude, reaching k~10 h/Mpc, a four-fold increase in redshift
coverage, to z=4, and now include the Hubble parameter as a new independent
variable. To further the range in k and z, a new set of nested simulations run
at modest cost is added to the original set. The extension in h is performed by
including perturbation theory results within a multi-scale procedure for
building the emulator. This economical methodology still gives excellent error
control, ~5% near the edges of the domain of applicability of the emulator. A
public domain code for the new emulator is released as part of the work
presented in this paper.

该研究利用 N 体模拟等方法，开发出一种高效、经济的宇宙学模拟方法以更准确地推测宇宙学和天文学现象，同时取得了显著的模拟效果提升，并在此基础上发布了公共代码。

Coyote Universe Extended：物质功率谱的精确仿真

The Coyote Universe Extended: Precision Emulation of the Matter Power  Spectrum

This paper presents cosmological results from the final data release of the
WiggleZ Dark Energy Survey. We perform full analyses of different cosmological
models using the WiggleZ power spectra measured at z=0.22, 0.41, 0.60, and
0.78, combined with other cosmological datasets. The limiting factor in this
analysis is the theoretical modelling of the galaxy power spectrum, including
non-linearities, galaxy bias, and redshift-space distortions. In this paper we
assess several different methods for modelling the theoretical power spectrum,
testing them against the Gigaparsec WiggleZ simulations (GiggleZ). We fit for a
base set of 6 cosmological parameters, {Omega_b h^2, Omega_CDM h^2, H_0, tau,
A_s, n_s}, and 5 supplementary parameters {n_run, r, w, Omega_k, sum m_nu}. In
combination with the Cosmic Microwave Background (CMB), our results are
consistent with the LambdaCDM concordance cosmology, with a measurement of the
matter density of Omega_m =0.29 +/- 0.016 and amplitude of fluctuations sigma_8
= 0.825 +/- 0.017. Using WiggleZ data with CMB and other distance and matter
power spectra data, we find no evidence for any of the extension parameters
being inconsistent with their LambdaCDM model values. The power spectra data
and theoretical modelling tools are available for use as a module for CosmoMC,
which we here make publicly available at this http URL . We
also release the data and random catalogues used to construct the baryon
acoustic oscillation correlation function.

该研究论文从 Galaxy power spectrum 的理论建模、各种宇宙模型和实测数据出发，通过多种不同的参数拟合，发现基于 LambdaCDM 模型参数的宇宙学模型能够较好地解释数据，未发现不符合模型的证据，并提供了模型工具和可供使用的数据。

WiggleZ 暗能量探测：终极数据发布与宇宙学结果

The WiggleZ Dark Energy Survey: Final data release and cosmological  results

We present measurements of galaxy clustering from the Baryon Oscillation
Spectroscopic Survey (BOSS), which is part of the Sloan Digital Sky Survey III
(SDSS-III). These use the Data Release 9 (DR9) CMASS sample, which contains
264,283 massive galaxies covering 3275 square degrees with an effective
redshift z=0.57 and redshift range 0.43 < z < 0.7. Assuming a concordance
Lambda-CDM cosmological model, this sample covers an effective volume of 2.2
Gpc^3, and represents the largest sample of the Universe ever surveyed at this
density, n = 3 x 10^-4 h^-3 Mpc^3. We measure the angle-averaged galaxy
correlation function and power spectrum, including density-field reconstruction
of the baryon acoustic oscillation (BAO) feature. The acoustic features are
detected at a significance of 5\sigma in both the correlation function and
power spectrum. Combining with the SDSS-II Luminous Red Galaxy Sample, the
detection significance increases to 6.7\sigma. Fitting for the position of the
acoustic features measures the distance to z=0.57 relative to the sound horizon
DV /rs = 13.67 +/- 0.22 at z=0.57. Assuming a fiducial sound horizon of 153.19
Mpc, which matches cosmic microwave background constraints, this corresponds to
a distance DV(z=0.57) = 2094 +/- 34 Mpc. At 1.7 per cent, this is the most
precise distance constraint ever obtained from a galaxy survey. We place this
result alongside previous BAO measurements in a cosmological distance ladder
and find excellent agreement with the current supernova measurements. We use
these distance measurements to constrain various cosmological models, finding
continuing support for a flat Universe with a cosmological constant.

该研究使用 BOSS 观察了 264,283 个海量星系的角度平均相关函数和功率谱，采用共鸣 - Lambda-CDM 宇宙学模型，用声学特征探测测定了从 z = 0.57 到声音地平线 DV /rs = 13.67 的距离约为 2094 +/- 34 Mpc，从而给出了最精确的距离限制，这对于宇宙学距离梯形和宇宙学模型的研究具有重要意义。

SDSS-III 巴氏振荡光谱测量中星系的聚类：基于数据发布 9 光谱星系样品的重子声学振荡

The clustering of galaxies in the SDSS-III Baryon Oscillation  Spectroscopic Survey: Baryon Acoustic Oscillations in the Data Release 9  Spectroscopic Galaxy Sample

A survey that can cover the sky in optical bands over wide fields to faint
magnitudes with a fast cadence will enable many of the exciting science
opportunities of the next decade. The Large Synoptic Survey Telescope (LSST)
will have an effective aperture of 6.7 meters and an imaging camera with field
of view of 9.6 deg^2, and will be devoted to a ten-year imaging survey over
20,000 deg^2 south of +15 deg. Each pointing will be imaged 2000 times with
fifteen second exposures in six broad bands from 0.35 to 1.1 microns, to a
total point-source depth of r~27.5. The LSST Science Book describes the basic
parameters of the LSST hardware, software, and observing plans. The book
discusses educational and outreach opportunities, then goes on to describe a
broad range of science that LSST will revolutionize: mapping the inner and
outer Solar System, stellar populations in the Milky Way and nearby galaxies,
the structure of the Milky Way disk and halo and other objects in the Local
Volume, transient and variable objects both at low and high redshift, and the
properties of normal and active galaxies at low and high redshift. It then
turns to far-field cosmological topics, exploring properties of supernovae to
z~1, strong and weak lensing, the large-scale distribution of galaxies and
baryon oscillations, and how these different probes may be combined to
constrain cosmological models and the physics of dark energy.

LSST 是一项为期 10 年的成像调查，光学带可以覆盖大面积并对光强度进行快速检测，它可以革命性地映射我们的宇宙，探索不同宇宙模型以及黑暗能量的物理学问题。

LSST 科学书，版本 2.0

LSST Science Book, Version 2.0

The first cosmological results from the ESSENCE supernova survey (Wood-Vasey
et al. 2007) are extended to a wider range of cosmological models including
dynamical dark energy and non-standard cosmological models. We fold in a
greater number of external data sets such as the recent Higher-z release of
high-redshift supernovae (Riess et al. 2007) as well as several complementary
cosmological probes. Model comparison statistics such as the Bayesian and
Akaike information criteria are applied to gauge the worth of models. These
statistics favor models that give a good fit with fewer parameters.
Based on this analysis, the preferred cosmological model is the flat
cosmological constant model, where the expansion history of the universe can be
adequately described with only one free parameter describing the energy content
of the universe. Among the more exotic models that provide good fits to the
data, we note a preference for models whose best-fit parameters reduce them to
the cosmological constant model.

通过 ESSENCE 超新星调查，我们将纳入更多的外部数据集和一些互补的宇宙学探针。我们应用贝叶斯信息准则和艾克信息准则等模型比较统计量来判断模型的价值。在分析的基础上，我们发现首选宇宙学模型是平直宇宙学常数模型，最能充分地描述宇宙的能量内容。虽然还有一些能够很好地拟合数据的更具实验性的模型，但我们还是更倾向于把它们转换成宇宙学常数模型。