Cosmological measurements from angular power spectra analysis of BOSS DR12 tomography
Cosmological measurements from angular power spectra analysis of BOSS DR12 tomography
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DOI：
10.1093/mnras/stz191
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发表时间：
2018-09
影响因子：
4.8
通讯作者：
A. Loureiro;B. Moraes;F. Abdalla;A. Cuceu;Michael McLeod;L. Whiteway;S. Balan;A. Benoit-Lévy;O. Lahav;M. Manera;R. Rollins;H. S. Xavier
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作者：
A. Loureiro;B. Moraes;F. Abdalla;A. Cuceu;Michael McLeod;L. Whiteway;S. Balan;A. Benoit-Lévy;O. Lahav;M. Manera;R. Rollins;H. S. Xavier
我们通过分析重子振荡光谱调查DR12星系的角功率谱来约束宇宙学参数，这是对超过9376度的约130万个SDSS星系的光谱跟踪，有效体积为∼6.5(GPC h^−1)^3，红移范围为0.15≤|$z$|<；0.80。我们将这个样本分成13个层析像元(Δ|$z$|=0.0 5)；使用伪C_L估计器计算角功率谱，并使用对数正态模拟图估计协方差矩阵。从这些数据获得的宇宙学约束与普朗克宇宙微波背景实验以及JLA超新星汇编的约束相结合。考虑在k_max=0.07h Mpc^−1尺度上测量的|$w$|cdm宇宙模型，我们在1σ水平上约束一个暗能量恒定的状态方程，其误差为：|$w_0=-0.993^{+0.046}_{-0.043}$|，Ω_m=0.330±0.012，Ω_b=0.0505±0.002，|$S_8\EQUV\SIGMA_8\SQRT{\OMEGA_\MATHORM{m}/0.3}=0.863\pm 0.016$|，h=0.661±0.012。对于相同的数据集组合，但现在考虑具有大质量中微子和相同尺度截断的Λ冷暗物质模型，我们得到Ω_m=0.328±0.009，|$\omega_\mathm{b}=0.05017^{+0.0009}_{-0.0008}$|，S_8=0.862±0.017，|$h=0.663^{+0.006}_{-0.007}$|，∑m_ν<的可信区间上限为95%；0.14 EV，适用于正常层次结构。这些结果即使不比使用相同数据集的标准分析更具竞争力，也表明这应该是未来调查的一种选择方法，为它们在相互关系探测中的充分利用打开了大门。
We constrain cosmological parameters by analysing the angular power spectra of the Baryon Oscillation Spectroscopic Survey DR12 galaxies, a spectroscopic follow-up of around 1.3 million SDSS galaxies over 9376 deg^2 with an effective volume of ∼6.5 (Gpc h^−1)^3 in the redshift range 0.15 ≤ |$z$| < 0.80. We split this sample into 13 tomographic bins (Δ|$z$| = 0.05); angular power spectra were calculated using a Pseudo-C_l estimator, and covariance matrices were estimated using lognormal simulated maps. Cosmological constraints obtained from these data were combined with constraints from Planck cosmic microwave background experiment as well as the JLA supernovae compilation. Considering a |$w$|CDM cosmological model measured on scales up to k_max = 0.07h Mpc^−1, we constrain a constant dark energy equation-of-state with an |${\sim } 4{{\ \rm per\ cent}}$| error at the 1σ level: |$w_0 = -0.993^{+0.046}_{-0.043}$|, together with Ω_m = 0.330 ± 0.012, Ω_b = 0.0505 ± 0.002, |$S_8 \equiv \sigma _8 \sqrt{\Omega _\mathrm{ m}/0.3} = 0.863 \pm 0.016$|, and h = 0.661 ± 0.012. For the same combination of data sets, but now considering a ΛCDM (lambda cold dark matter) model with massive neutrinos and the same scale cut, we find Ω_m = 0.328 ± 0.009, |$\Omega _\mathrm{ b} = 0.05017^{+0.0009}_{-0.0008}$|, S_8 = 0.862 ± 0.017, and |$h = 0.663^{+0.006}_{-0.007}$|, and a 95 per cent credible interval (CI) upper limit of ∑m_ν < 0.14 eV for a normal hierarchy. These results are competitive if not better than standard analyses with the same data set, and demonstrate that this should be a method of choice for future surveys, opening the door for their full exploitation in cross-correlation probes.