A Measurement of the Quadrupole Power Spectrum in the Clustering of the 2dF QSO Survey

By Kazuhiro Yamamoto, Masashi Nakamichi, Akinari Kamino, Bruce A. Bassett, H. Nishioka. 2005

176 citations recorded by the source corpus.

We report on a measurement of the quadrupole power spectrum in the two degree field (2dF) QSO redshift (2QZ) survey. The analysis used an algorithm parallel to that for estimating the standard monopole power spectrum without first requiring computation of the correlation function or the anisotropic power spectrum. The error on the quadrupole spectrum was rather large, but the best-fit value of the bias parameter from the quadrupole spectrum is consistent with that from previous investigations of the 2dF data.

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/82d7fb41278ca543dd89c922015cc64ed01e3d6f

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In Nuclear and High Energy Physics

Citations in the corpus

The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: baryon acoustic oscillations in the Fourier space (2016, unknown): “The first two non-zero power spectrum multipoles can be calculated as (Feldman, Kaiser & Peacock 1993; Yamamoto et al. 2006) P0(k) = 1 2A [F0(k)F ∗0 (k) − S], (2) P2(k) = 5 4A F0(k)[3F ∗2 (k) − F ∗0 (k)], (3) with F0(k) = A0(k), (4) F2(k) = 1 k2 [k2xBxx + k2yByy + k2zBzz + 2(kzkyBxy + kxkzBxz +…”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: RSD measurement from the power spectrum and bispectrum of the DR12 BOSS galaxies (2016, methodology): “An extension of this estimator based the Yamamoto estimator (Yamamoto et al. 2006) for the quadrupole of the bispectrum would be possible (see Scoccimarro 2015), although for simplicity (especially on the modelling) we do not consider this quantity here.”
The WiggleZ Dark Energy Survey: the growth rate of cosmic structure since redshift z=0.9 (2011, methodology): “• We considered various methods for presenting the information contained in the redshift-space power spectra, including deriving the multipole moments Pℓ(k) using direct integration of the binned power spectrum P (k, µ) and by implementing the estimator described by Yamamoto et al. (2006).”
Cosmology from cosmic shear power spectra with Subaru Hyper Suprime-Cam first-year data (2018, background): “…density fields including CMB (e.g., Hinshaw et al. 2013; Planck Collaboration et al. 2016), the distribution of galaxies (e.g., Cole et al. 2005; Yamamoto et al. 2006; Percival et al. 2010; Reid et al. 2010; Blake et al. 2011; Oka et al. 2014; Alam et al. 2017; Beutler et al. 2017), and the…”
Simultaneous constraints on the growth of structure and cosmic expansion from the multipole power spectra of the SDSS DR7 LRG sample (2013, methodology): “In our measurement of the multipole power spectra, we adopt an estimator, P̂ℓ(k), for discrete density fields (Yamamoto et al. 2006a): P̂ℓ(k) = 2ℓ+ 1 ∆Vk ∫ ∆Vk d3k {Rℓ(k)− Sℓ(k)}, (3) where ∆Vk is the volume of a shell in the Fourier space, Rℓ and Sℓ, are defined by Rℓ(k) = A −1 [ NLRG…”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: tomographic BAO analysis of DR12 combined sample in Fourier space (2016, methodology): “3.3 The estimator for P (k) To measure the power spectrum multipole, we need to perform Fourier transformations of the overdensity field (r) defined in equation (4) (Yamamoto et al. 2006).”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Testing gravity with redshift-space distortions using the power spectrum multipoles (2013, methodology): “1 0 C O N C L U S I O N This paper analyses the BOSS CMASS-DR11 data set employing a power spectrum estimator suggested by Yamamoto et al. (2006), which allows us to measure the power spectrum monopole and quadrupole in a wide-angle survey like BOSS.”
The power spectrum and bispectrum of SDSS DR11 BOSS galaxies – I. Bias and gravity (2014, methodology): “Except for narrow angle surveys (Blake et al. 2013), higher order multipoles, such as the quadrupole or hexadecapole, require a more complex estimator, such as described by Yamamoto et al. (2006), as is implemented in Beutler et al. (2014) for the CMASS DR11 galaxy sample.”
The completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: BAO and RSD measurements from the anisotropic power spectrum of the quasar sample between redshift 0.8 and 2.2 (2020, methodology): “For the calculation of the power spectrum, we use the method of Yamamoto et al. (2006).”
nbodykit: An Open-source, Massively Parallel Toolkit for Large-scale Structure (2017, methodology): “…FFT-based estimator presented by Bianchi et al. (2015) and Scoccimarro (2015), building on the ideas of previous power spectrum estimators (Feldman et al. 1994; Yamamoto et al. 2006), and in particular, the treatment of the anisotropic 2PCF using spherical harmonics of Slepian & Eisenstein (2015b).”
Consistent modeling of velocity statistics and redshift-space distortions in one-loop perturbation theory (2020, unknown): “produce power spectrum multipoles P`(k) [92, 105–107].”