Calibrating the nonlinear matter power spectrum: Requirements for future weak lensing surveys

By D. Huterer, M. Takada. 2004

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Abstract Uncertainties in predicting the nonlinear clustering of matter are among the most serious theoretical systematics facing the upcoming wide-field weak gravitational lensing surveys. We estimate the accuracy with which the matter power spectrum will need to be calibrated in order not to contribute appreciably to the error budget for future weak lensing surveys. We consider the random statistical errors and the systematic biases in P ( k ), as well as some estimates based on current N-body simulations. While the power spectrum on relevant scales (0.1 ≲ k / h Mpc −1 ≲ 10) is currently calibrated with N-body simulations to about 5–10%, in the future it will have to be calibrated to about 1–2% accuracy, depending on the specifications of the survey. Encouragingly, we find that even the worst-case error that mimics the effect of cosmological parameters needs to be calibrated to no better than about 0.5–1%. These goals require a suite of high resolution N-body simulations on a relatively fine grid in cosmological parameter space, and should be achievable in the near future.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

Effects of Photometric Redshift Uncertainties on Weak-Lensing Tomography (2005, background): “…has addressed systematic errors from the computation of the non-linear power spectrum (Vale & White 2003; White & Vale 2004; Heitmann et al. 2004; Huterer & Takada 2005; Hagan, Ma & Kravtsov 2005), baryonic cooling and pressure forces on the distribution of large-scale structures (White 2004;…”
Galaxy Alignments: An Overview (2015, methodology): “This was re-derived and applied to the case of measurement of the matter power spectrum in Huterer & Takada (2005), and applied to the case of weak lensing systematics in Huterer et al. (2006) and Taylor et al. (2007); the approach was subsequently re-derived in Amara & Réfrégier (2008).”
Putting the precision in precision cosmology: How accurate should your data covariance matrix be? (2012, background): “Attention has been focussed on the accuracy of the predictions of the mean value – e.g., the model power spectra – and the effect of biases or errors in the mean (e.g., Huterer & Takada, 2005; Huterer, et al., 2006; Taylor et al., 2007).”
Cosmology from cosmic shear power spectra with Subaru Hyper Suprime-Cam first-year data (2018, background): “There are also uncertainties in modeling the matter power spectrum on small scales due to baryonic effects such as star formation and supernovae and AGN feedbacks (White 2004; Zhan & Knox 2004; Huterer & Takada 2005; Jing et al. 2006; Bernstein 2009; Semboloni et al. 2011).”
Transients from initial conditions in cosmological simulations (2006, methodology): “The use of better initial conditions should be a useful tool in reaching future goals of simulating the nonlinear power spectrum to an accuracy of better than 1% percent needed for the next-generation of weak gravitational lensing surveys (Huterer & Takada 2005).”
The impact of non‐Gaussian errors on weak lensing surveys (2008, background): “We note in passing that the issue of accurate power spectra for general dark energy cosmologiesstill needs to be addressed carefully (Huterer & Takada 2005; also see Ma 2007 for the related discussion).”
The Influence of Baryons on the Clustering of Matter and Weak-Lensing Surveys (2005, methodology): “To match the accuracy of future lensing surveys, the matter power spectrum at the scales discussed in this Letter must be calibrated to∼1% accuracy (Huterer & Takada 2005).”
THE COYOTE UNIVERSE. I. PRECISION DETERMINATION OF THE NONLINEAR MATTER POWER SPECTRUM (2008, background): “Huterer & Takada (2005) show that in order to avoid errors from imprecise theoretical templates mimicking the effect of cosmological parameter variations, the power spectrum has to be calibrated at about 0.5-1% for 0.1hMpc−1 ≤ k ≤ 10hMpc−1.”
Halo mass function and scale-dependent bias from N-body simulations with non-Gaussian initial conditions (2008, methodology): “For parameter estimation, a comparable accuracy will be required on model spectra within a wide range of wavenumbers centred around k ∼ 1 h Mpc−1 (Huterer & Takada 2005).”
Multipoint propagators in cosmological gravitational instability (2008, background): “With the advent of precision observations of the large-scale structure, in particular in the context of the search for dark energy signatures in the growth of structure, this is clearly insufficient [10].”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, background): “Currently only N-body simulations allow us to capture the non-linear structure formation, but for a survey such as Euclid an accuracy of ∼ 1% is needed [622, 626].”
The effects of galaxy formation on the matter power spectrum: a challenge for precision cosmology (2011, background): “…capable of, surveys such as LSST,1 EUCLID,2 and WFIRST3 need to be calibrated using theoretical models that retain 1% accuracies on these scales (Huterer & Takada 2005; Laureijs 2009).4 This is, however, not as straightforward as increasing the resolution of existing N-body simulations: many…”
REVISING THE HALOFIT MODEL FOR THE NONLINEAR MATTER POWER SPECTRUM (2012, background): “For instance, Huterer & Takada (2005) argued that we typically need P (k) within a few percent accuracy at the wavenumber k < 10 h Mpc−1 in order for the uncertainty of P (k) not to degrade cosmological constraints in DES and LSST (see also Eifler 2011; Hearin et al. 2012, in which a similar…”
Systematic bias in cosmic shear: extending the Fisher matrix (2007, methodology): “A similar bias formalism was intro- duced by Huterer and Takada (2005) and applied to theoretical uncertainties in modeling the matter power spectrum with N-body simulations.”