A spherical harmonic approach to redshift distortion and a measurement of Formula from the 1.2-Jy IRAS Redshift Survey

Fisher, Karl B.; Scharf, Caleb; Lahav, O.

doi:10.1093/mnras/266.1.219

Cited by 152 publications

(193 citation statements)

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“…The effects of redshift space distortions are included as described in [34,35]. The likelihood combines the four measured redshift bins and includes the full covariance as a result of photometric errors scattering galaxies between bins and therefore correlating slices.…”

Section: Figmentioning

confidence: 99%

Upper Bound of 0.28 eV on Neutrino Masses from the Largest Photometric Redshift Survey

2010

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We present a new upper limit of mν ≤ 0.28 (95% CL) on the sum of the neutrino masses assuming a flat ΛCDM cosmology. This relaxes slightly to mν ≤ 0.34 and mν ≤ 0.47 when quasi non-linear scales are removed and w = −1, respectively. These bounds are derived from a new photometric redshift catalogue of over 700,000 Luminous Red Galaxies (MegaZ DR7) with a volume of 3.3 (Gpc h −1 ) 3 , extending over the redshift range 0.45 < z < 0.65 and up to angular scales of max = 300. The data are combined with WMAP 5-year CMB fluctuations, Baryon Acoustic Oscillations (BAO), type 1a Supernovae (SNe) and an HST prior on the Hubble parameter. This is the first combined constraint from a photometric redshift catalogue with other cosmological probes. When combined with WMAP this data set proves to be as constraining as the addition of all SNe and BAO data available to date. The upper limit is one of the tightest and 'cleanest' constraints on the neutrino mass from cosmology or particle physics. Furthermore, if the aforementioned bounds hold, they all predict that current-to-next generation neutrino experiments, such as KATRIN, are unlikely to obtain a detection.

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Section: Figmentioning

confidence: 99%

Upper Bound of 0.28 eV on Neutrino Masses from the Largest Photometric Redshift Survey

2010

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“…The spherical harmonic analysis has been applied to the Infrared Astronomical Satellite galaxy catalog (Scharf et al 1992;Fisher et al 1994), the Point Source Catalog redshift galaxy catalog ( Tadros et al 1999), and, recently, the Two Degree Field Galaxy Redshift Survey catalog ( Percival et al 2004). We adopt the formulation in Heavens & Taylor (1995) and describe it here briefly.…”

Section: Appendix Spherical Harmonic Analysismentioning

confidence: 99%

Exploring Large‐Scale Structure with Billions of Galaxies

Zhan¹,

Knox²,

Margoniner³

2006

ApJ

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We consider cosmological applications of galaxy number density correlations to be inferred from future deep and wide multiband optical surveys. We mostly focus on very large scales as a probe of possible features in the primordial power spectrum. We find the proposed survey of the Large Synoptic Survey Telescope may be competitive with future all-sky CMB experiments over a broad range of scales. On very large scales the inferred power spectrum is robust to photometric redshift errors and, given a sufficient number density of galaxies, to angular variations in dust extinction and photometric calibration errors. We also consider other applications, such as constraining dark energy with the two CMB-calibrated standard rulers in the matter power spectrum and controlling the effect of photometric redshift errors to facilitate the interpretation of cosmic shear data. We find that deep photometric surveys over a wide area can provide constraints that are competitive with spectroscopic surveys in small volumes.

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“…Spherical harmonics transform alternatives to Fourier analysis exist and are well known, at least for the power spectrum (e.g. [11,[13][14][15]), although their application to surveys is not done as often due to their computational cost. For this reason in this paper we concentrate on Fourier analysis and how to tackle fast estimation of redshift-space power spectrum and bispectrum multipoles in the presence of radial distortions.…”

Section: Introductionmentioning

confidence: 99%

Fast estimators for redshift-space clustering

2015

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Redshift-space distortions in galaxy surveys happen along the radial direction, breaking statistical translation invariance. We construct estimators for radial distortions that, using only Fast Fourier Transforms (FFTs) of the overdensity field multipoles for a given survey geometry, compute the power spectrum monopole, quadrupole and hexadecapole, and generalize such estimators to the bispectrum. Using realistic mock catalogs we compare the signal to noise of two estimators for the power spectrum hexadecapole that require different number of FFTs and measure the bispectrum monopole, quadrupole and hexadecapole. The resulting algorithm is very efficient, e.g. for the BOSS survey requires about three minutes for = 0, 2, 4 power spectra for scales up to k = 0.3 h Mpc −1 and about fifteen additional minutes for = 0, 2, 4 bispectra for all scales and triangle shapes up to k = 0.2 h Mpc −1 on a single core. The speed of these estimators is essential as it makes possible to compute covariance matrices from large number of realizations of mock catalogs with realistic survey characteristics, and paves the way for improved constrains of gravity on cosmological scales, inflation and galaxy bias.

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A spherical harmonic approach to redshift distortion and a measurement of Formula from the 1.2-Jy IRAS Redshift Survey

Cited by 152 publications

References 0 publications

Upper Bound of 0.28 eV on Neutrino Masses from the Largest Photometric Redshift Survey

Upper Bound of 0.28 eV on Neutrino Masses from the Largest Photometric Redshift Survey

Exploring Large‐Scale Structure with Billions of Galaxies

Fast estimators for redshift-space clustering

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