Improving Fisher matrix forecasts for galaxy surveys: window function, bin cross-correlation and bin redshift uncertainty

Bailoni, Alberto; Mancini, Alessio Spurio; Amendola, Luca

doi:10.1093/mnras/stx1209

Cited by 21 publications

(18 citation statements)

References 38 publications

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“…The AP effect instead has a main impact on the late-time parameters [91]. Overall, the impact of the geometrical distortions and of the AP term included in the analysis, see Eqs.…”

Section: Resultsmentioning

confidence: 99%

Probing primordial features with future galaxy surveys

Ballardini

Finelli⋆

Fedeli

et al. 2016

J. Cosmol. Astropart. Phys.

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Abstract. We study the capability of future measurements of the galaxy clustering power spectrum to probe departures from a power-law spectrum for primordial fluctuations. On considering the information from the galaxy clustering power spectrum up to quasi-linear scales, i.e. k < 0.1 h Mpc −1 , we present forecasts for DESI, Euclid and SPHEREx in combination with CMB measurements. As examples of departures in the primordial power spectrum from a simple power-law, we consider four P lanck 2015 best-fits motivated by inflationary models with different breaking of the slowroll approximation. These four representative models provide an improved fit to CMB temperature anisotropies, although not at statistical significant level. As for other extensions in the matter content of the simplest ΛCDM model, the complementarity of the information in the resulting matter power spectrum expected from these galaxy surveys and in the primordial power spectrum from CMB anisotropies can be effective in constraining cosmological models. We find that the three galaxy surveys can add significant information to CMB to better constrain the extra parameters of the four models considered.

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“…The AP effect instead has a main impact on the late-time parameters [91]. Overall, the impact of the geometrical distortions and of the AP term included in the analysis, see Eqs.…”

Section: Resultsmentioning

confidence: 99%

Probing primordial features with future galaxy surveys

Ballardini

Finelli⋆

Fedeli

et al. 2016

J. Cosmol. Astropart. Phys.

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show abstract

“…For instance, Ruggeri et al (2017) apply a set of weights to extract RSD measurements as a function of redshift, acknowledging that future surveys covering a broad redshift range can no longer ignore cosmic evolution. Bailoni et al (2017) improve upon the standard 3D P (k) Fisher method by taking into account three effects: the finite window function, the correlation between redshift bins and the uncertainty on redshift estimation. Gil-Marín et al (2016) use a line-of-sight dependent power spectrum to deal with the large sky coverage of the Sloan Digital Sky Survey (SDSS) DR12 catalogue.…”

Section: Fourier Power Spectrummentioning

confidence: 99%

Optimized angular power spectra for spectroscopic galaxy surveys

Camera

Fonseca

Maartens

et al. 2018

Monthly Notices of the Royal Astronomical Society

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The angular power spectrum C (z i , z j ) is a gauge-independent observable that is in principle the natural tool for analysing galaxy number counts. In practice, the problem is that the computational requirements for next-generation spectroscopic surveys such as Euclid and the Square Kilometre Array are currently unfeasible. We propose a new method to save computational time for spectroscopic angular power spectra. This hybrid method is modelled on the Fourier power spectrum approach of treating relatively thick redshift bins (∆z ∼ 0.1) as separate surveys. In the hybrid method, each thick bin is further subdivided into thin bins (δz ∼ 0.01); all the correlations within each thick bin are computed, while cross-bin correlations beyond the thick bins are neglected. Constraints on cosmological parameters from the hybrid method are comparable to those from the standard galaxy P g (k, z) analysis-but they have the advantage that cosmic evolution, wide-angle and lensing effects are naturally included, while no Alcock-Paczynski correction is needed. The hybrid method delivers much tighter constraints than a 2D tomographic approach that is typical for photometric surveys, which considers only thick bins and the correlations between them. Furthermore, for standard cosmological parameters our method is not biased by neglecting the effects of lensing on number counts, while the tomographic method is strongly biased.

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“…We will consider the smallest wavenumber k min to be k min = 0.0079h/Mpc , while the maximum wavenumber will be k max = 0.15h/Mpc for the linear forecasts and k max = 0.5h/Mpc for the non-linear forecasts. In the above formulation of the Galaxy Clustering Fisher matrix, we neglect the correlation among different redshift bins and possible redshift bin uncertainties as was explored recently in [67], we will use for our forecasts the more standard recipe specified in the Euclid Redbook [53]. Table 2.…”

Section: B Galaxy Clusteringmentioning

confidence: 99%

Linear and non-linear Modified Gravity forecasts with future surveys

Casas

Kunz

Martinelli

et al. 2017

Physics of the Dark Universe

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Modified Gravity theories generally affect the Poisson equation and the gravitational slip (effective anisotropic stress) in an observable way, that can be parameterized by two generic functions (η and µ) of time and space. We bin the time dependence of these functions in redshift and present forecasts on each bin for future surveys like Euclid. We consider both Galaxy Clustering and Weak Lensing surveys, showing the impact of the non-linear regime, treated with two different semi-analytical approximations. In addition to these future observables, we use a prior covariance matrix derived from the Planck observations of the Cosmic Microwave Background. Our results show that η and µ in different redshift bins are significantly correlated, but including non-linear scales reduces or even eliminates the correlation, breaking the degeneracy between Modified Gravity parameters and the overall amplitude of the matter power spectrum. We further decorrelate parameters with a Zerophase Component Analysis and identify which combinations of the Modified Gravity parameter amplitudes, in different redshift bins, are best constrained by future surveys. We also extend the analysis to two particular parameterizations of the time evolution of µ and η and consider, in addition to Euclid, also SKA1, SKA2, DESI: we find in this case that future surveys will be able to constrain the current values of η and µ at the 2-5% level when using only linear scales (wavevector k < 0.15 h/Mpc), depending on the specific time parameterization; sensitivity improves to about 1% when non-linearities are included. CONTENTS

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Improving Fisher matrix forecasts for galaxy surveys: window function, bin cross-correlation and bin redshift uncertainty

Cited by 21 publications

References 38 publications

Probing primordial features with future galaxy surveys

Probing primordial features with future galaxy surveys

Optimized angular power spectra for spectroscopic galaxy surveys

Linear and non-linear Modified Gravity forecasts with future surveys

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