Maximum likelihood estimates of the two- and three-dimensional power spectra of the APM Galaxy Survey
Maximum likelihood estimates of the two- and three-dimensional power spectra of the APM Galaxy Survey
复制标题
APM 星系巡天二维和三维功率谱的最大似然估计
DOI：
10.1046/j.1365-8711.2001.04575.x
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发表时间：
2000
影响因子：
4.8
通讯作者：
S. Moody
中科院分区：
文献类型：
--
作者：
G. Efstathiou;S. Moody
我们估计的二维和三维的功率谱，P2（K）和P3（K），星系分布的应用最大似然估计APM星系巡天的像素地图。分析提供了最佳估计的功率谱和协方差矩阵，如果波动被假定为高斯。我们对P2（K）和P3（k）的估计与以前的工作很好地一致，但我们发现在一些早期的研究中低估了低波数的误差。如果假设星系功率谱与质量功率谱具有相同的形状，那么在k≤0.19 h Mpc−1时的APM最大似然P3（k）估计将标度不变CDM模型的振幅和形状参数限制在2σ范围0.74≤（σ8）g≤1.28和0.06≤Γ≤0.46内。使用Schlegel，Finkbeiner和Davis的银河系灭绝估计，我们表明，银河系的遮蔽对APM星系巡天的大部分区域的星系团的影响可以忽略不计。
We estimate the two- and three-dimensional power spectra, P2(K) and P3(k), of the galaxy distribution by applying a maximum likelihood estimator to pixel maps of the APM Galaxy Survey. The analysis provides optimal estimates of the power spectra and of their covariance matrices if the fluctuations are assumed to be Gaussian. Our estimates of P2(K) and P3(k) are in good agreement with previous work, but we find that the errors at low wavenumbers have been underestimated in some earlier studies. If the galaxy power spectrum is assumed to have the same shape as the mass power spectrum, then the APM maximum likelihood P3(k) estimates at k≤0.19 h Mpc−1 constrain the amplitude and shape parameter of a scale-invariant CDM model to lie within the 2σ ranges 0.74≤(σ8)g≤1.28 and 0.06≤Γ≤0.46. Using the Galactic extinction estimates of Schlegel, Finkbeiner & Davis, we show that Galactic obscuration has a negligible effect on galaxy clustering over most of the area of the APM Galaxy Survey.