2020
DOI: 10.1103/physrevd.102.023502
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Measuring lensing ratios with future cosmological surveys

Abstract: The ratio between the CMB lensing/galaxy counts and the galaxy shear/galaxy counts cross-correlations combines the information from different cosmological probes to infer cosmographic measurements that are less dependent on astrophysical uncertainties and can constrain the geometry of the Universe. We discuss the future perspectives for the measurement of this lensing ratio as previously introduced, i.e., with the use of the Limber and flat-sky approximations and neglecting all the effects on the galaxy survey… Show more

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Cited by 4 publications
(7 citation statements)
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“…For the functional form of the redshift dependence, sðzÞ, we derive the magnification bias for LSST, EMU, and SKA1 based on the luminosity functions and methodology by [102]. For the Euclid-like surveys, we adopt the sðzÞ functional forms by [103] for the photometric sample and by [32] for the spectroscopic sample. For SPHEREx, since there is not in the literature a derivation of its magnification bias or an estimation for its luminosity function, we assume a constant value sðzÞ ¼ 0.42.…”
Section: Discussionmentioning
confidence: 99%
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“…For the functional form of the redshift dependence, sðzÞ, we derive the magnification bias for LSST, EMU, and SKA1 based on the luminosity functions and methodology by [102]. For the Euclid-like surveys, we adopt the sðzÞ functional forms by [103] for the photometric sample and by [32] for the spectroscopic sample. For SPHEREx, since there is not in the literature a derivation of its magnification bias or an estimation for its luminosity function, we assume a constant value sðzÞ ¼ 0.42.…”
Section: Discussionmentioning
confidence: 99%
“…Here, Δ k ðzÞ is the total number counts fluctuation in Newtonian gauge, usually approximated to Δ k ðzÞ ≃ b G ðzÞδ c k ðzÞ on subhorizon scales, where b G ðzÞ is the galaxy bias and δ c k ðzÞ is the comoving-gauge linear matter density perturbation. While lensing and other light cone effects on the galaxy number counts angular power spectra have a small impact on the uncertainties on cosmological parameters, it will be necessary to model these contributions in order to avoid biases on cosmological parameters, such as darkenergy parameters and the total neutrino mass [20,32,[48][49][50][51][52]. We summarize in Appendix A all the RSD and GR contributions to Δ k ðzÞ.…”
Section: Cmb Galaxy Counts and Their Cross-correlationmentioning
confidence: 99%
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“…Here ∆ k (z) is the total number counts fluctuation in Newtonian gauge, usually approximated to ∆ k (z) b G (z)δ c k (z) on sub-horizon scales, where b G (z) is the galaxy bias and δ c k (z) is the comovinggauge linear matter density perturbation. While lensing and other lightcone effects on the galaxy number counts angular power spectra have a small impact on the uncertainties on cosmological parameters, it will be necessary to model these contributions in order to avoid biases on cosmological parameters such as dark-energy parameters and the total neutrino mass [14,26,[36][37][38][39][40]. We summarize in appendix A all the RSD and GR contributions to ∆ k (z).…”
Section: Cmb Galaxy Counts and Their Cross-correlationmentioning
confidence: 99%
“…It has been studied how this cross-correlation will contribute to the measurements of the amplitude of matter fluctuations, neutrino mass [19,20], primordial non-Gaussianities [20][21][22] and galaxy bias. The cross-correlations of CMB lensing with galaxies and galaxy shear is also used in lensing ratio estimators, which can mitigate the uncertainties of the galaxy bias [23][24][25][26].…”
Section: Introductionmentioning
confidence: 99%