Lensing convergence and the neutrino mass scale in galaxy redshift surveys

Cardona, Wilmar; Durrer, Ruth; Kunz, M.; Montanari, Francesco

doi:10.1103/physrevd.94.043007

Cited by 57 publications

(87 citation statements)

References 65 publications

(119 reference statements)

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“…As a first result, we compute the total biases on cosmological parameters if the magnification effect is not accounted for in the model, but is present in the clustering and galaxy-galaxy-lensing data. Our results are consistent with previous work as detailed in Duncan et al (2014); Lorenz et al (2018); Cardona et al (2016). We find that parameter biases are typically comparable to or smaller than statistical uncertainty for the DES-Y1 application.…”

Section: Discussionsupporting

confidence: 92%

“…excluding the galaxy bias parameters we marginalise over) and n p is the number of parameters in the set. For the Euclid-like survey, we find that with the sole exception of Ω B , all parameters are significantly biased by the neglect of the magnification signal as found in Duncan et al (2014); Lorenz et al (2018); Cardona et al (2016) and reinforcing the conclusion that magnification must be measured and modelled to avoid catastrophic parameter bias in the 3x2pt analysis of Euclid data.…”

Section: Cosmological Parameter Bias From Magnificationsupporting

confidence: 71%

“…Finally, the shear-shear signal is unaffected by magnification at first order, but can receive second-order contributions due to the magnification of the sources and their perturbed observed positions (Cooray & Hu 2002;Schmidt et al 2009b;Krause & Hirata 2010). The impact of such effects is now well studied, and recent investigations (Duncan et al 2014;Cardona et al 2016;Lorenz et al 2018) all indicate that whilst the magnification does not significantly contribute to the precision of cosmological constraints, it can catastrophically affect the accuracy of such constraints if it is not appropriately modelled, even where redshift-bin cross-correlations in the clustering data (where magnification is a larger relative contribution to the total signal) are removed from the data vector. Such model bias results from the requirement that the incomplete model (e.g.…”

Section: Introductionmentioning

confidence: 99%

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Disentangling magnification in combined shear-clustering analyses

Thiele

Duncan

Alonso

2019

Monthly Notices of the Royal Astronomical Society

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We investigate the sensitivity to the effects of lensing magnification on large-scale structure analyses combining photometric cosmic shear and galaxy clustering data (i.e. the now commonly called "3×2-point" analysis). Using a Fisher matrix bias formalism, we disentangle the contribution to the bias on cosmological parameters caused by ignoring the effects of magnification in a theory fit from individual elements in the data vector, for Stage-III and Stage-IV surveys. We show that the removal of elements of the data vectors that are dominated by magnification does not guarantee a reduction in the cosmological bias due to the magnification signal, but can instead increase the sensitivity to magnification. We find that the most sensitive elements of the data vector come from the shear-clustering cross-correlations, particularly between the highestredshift shear bin and any lower-redshift lens sample, and that the parameters Ω M , S 8 = σ 8 Ω M /0.3 and w 0 show the most significant biases for both survey models. Our forecasts predict that current analyses are not significantly biased by magnification, but this bias will become highly significant with the continued increase of statistical power in the near future. We therefore conclude that future surveys should measure and model the magnification as part of their flagship "3×2-point" analysis.

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Section: Discussionsupporting

confidence: 92%

Section: Cosmological Parameter Bias From Magnificationsupporting

confidence: 71%

Section: Introductionmentioning

confidence: 99%

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Disentangling magnification in combined shear-clustering analyses

Thiele

Duncan

Alonso

2019

Monthly Notices of the Royal Astronomical Society

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“…The importance of the integrated terms has been investigated in [54][55][56][57][58], showing that future single-tracer surveys can detect the lensing term at high significance [54,55,58], while multi-tracer surveys will be needed to detect the time-delay term [56,57]. The correlation function for individual configurations is probably below detection, but a full analysis that averages suitably over configurations will be needed to assess the detectability of signals in future surveys.…”

Section: Discussionmentioning

confidence: 99%

Lensing and time-delay contributions to galaxy correlations

et al. 2016

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Galaxy clustering on very large scales can be probed via the 2-point correlation function in the general case of wide and deep separations, including all the lightcone and relativistic effects. Using our recently developed formalism, we analyze the behavior of the local and integrated contributions and how these depend on redshift range, linear and angular separations and luminosity function. Relativistic corrections to the local part of the correlation can be non-negligible but they remain generally sub-dominant. On the other hand, the additional correlations arising from lensing convergence and time-delay effects can become very important and even dominate the observed total correlation function. We investigate different configurations formed by the observer and the pair of galaxies, and we find that the case of near-radial large-scale separations is where these effects will be the most important.

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“…Apart from the last term, all relativistic contributions are relevant only on very large scales corresponding to 10. The gravitational lensing contribution is relevant in wide redshift bins, at relatively high redshifts, z 1, or in widely separated redshift bins [30,32,33]. For the redshift bin widths used in this work, we discuss briefly in Appendix D the importance of lensing in angular power spectra, relative to the RSD contribution.…”

Section: Introductionmentioning

confidence: 99%

Nonlinear contributions to angular power spectra

et al. 2020

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Future galaxy clustering surveys will probe small scales where non-linearities become important. Since the number of modes accessible on intermediate to small scales is very high, having a precise model at these scales is important especially in the context of discriminating alternative cosmological models from the standard one. In the mildly nonlinear regime, such models typically differ from each other, and galaxy clustering data will become very precise on these scales in the near future. As the observable quantity is the angular power spectrum in redshift space, it is important to study the effects of non-linear density and redshift space distortion (RSD) in the angular power spectrum. We compute non-linear contributions to the angular power spectrum using a flat-sky approximation that we introduce in this work, and compare the results of different perturbative approaches with N -body simulations. We find that the TNS perturbative approach is significantly closer to the N -body result than Eulerian or Lagrangian 1-loop approximations, effective field theory of large scale structure or a halofit-inspired model. However, none of these prescriptions is accurate enough to model the angular power spectrum well into the non-linear regime. In addition, for narrow redshift bins, ∆z 0.01, the angular power spectrum acquires nonlinear contributions on all scales, right down to = 2, and is hence not a reliable tool at this time. To overcome this problem, we need to model non-linear RSD terms, for example as TNS does, but for a matter power spectrum that remains reasonably accurate well into the deeply non-linear regime, such as halofit.

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Lensing convergence and the neutrino mass scale in galaxy redshift surveys

Cited by 57 publications

References 65 publications

Disentangling magnification in combined shear-clustering analyses

Disentangling magnification in combined shear-clustering analyses

Lensing and time-delay contributions to galaxy correlations

Nonlinear contributions to angular power spectra

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