Cosmology with photometric weak lensing surveys: Constraints with redshift tomography of convergence peaks and moments
Abstract
Weak gravitational lensing is becoming a mature technique for constraining cosmological parameters, and future surveys will be able to constrain the dark energy equation of state w. When analyzing galaxy surveys, redshift information has proven to be a valuable addition to angular shear correlations. We forecast parameter constraints on the triplet (Ω _{m},w,σ _{8}) for a LSSTlike photometric galaxy survey, using tomography of the shearshear power spectrum, convergence peak counts and higher convergence moments. Here we find that redshift tomography with the power spectrum reduces the area of the 1σ confidence interval in (Ω _{m},w) space by a factor of 8 with respect to the case of the single highest redshift bin. We also find that adding nonGaussian information from the peak counts and higherorder moments of the convergence field and its spatial derivatives further reduces the constrained area in (Ω _{m},w) by factors of 3 and 4, respectively. When we add cosmic microwave background parameter priors from Planck to our analysis, tomography improves power spectrum constraints by a factor of 3. Adding moments yields an improvement by an additional factor of 2, and adding both moments and peaks improves by almost a factor of 3 over power spectrum tomographymore »
 Authors:
 Columbia Univ., New York, NY (United States). Dept. of Physics; Brookhaven National Lab. (BNL), Upton, NY (United States). Dept. of Physics
 Brookhaven National Lab. (BNL), Upton, NY (United States). Dept. of Physics
 Columbia Univ., New York, NY (United States). Dept. of Astronomy
 Publication Date:
 Research Org.:
 Brookhaven National Laboratory (BNL), Upton, NY (United States)
 Sponsoring Org.:
 USDOE Office of Science (SC), High Energy Physics (HEP) (SC25)
 OSTI Identifier:
 1336177
 Report Number(s):
 BNL1131762016JA
Journal ID: ISSN 24700010; PRVDAQ; KA2301020
 Grant/Contract Number:
 SC0012704; ACI1053575; AST1210877; SC00112704
 Resource Type:
 Journal Article: Accepted Manuscript
 Journal Name:
 Physical Review D
 Additional Journal Information:
 Journal Volume: 94; Journal Issue: 6; Journal ID: ISSN 24700010
 Publisher:
 American Physical Society (APS)
 Country of Publication:
 United States
 Language:
 English
 Subject:
 79 ASTRONOMY AND ASTROPHYSICS
Citation Formats
Petri, Andrea, May, Morgan, and Haiman, Zoltán. Cosmology with photometric weak lensing surveys: Constraints with redshift tomography of convergence peaks and moments. United States: N. p., 2016.
Web. doi:10.1103/PhysRevD.94.063534.
Petri, Andrea, May, Morgan, & Haiman, Zoltán. Cosmology with photometric weak lensing surveys: Constraints with redshift tomography of convergence peaks and moments. United States. doi:10.1103/PhysRevD.94.063534.
Petri, Andrea, May, Morgan, and Haiman, Zoltán. 2016.
"Cosmology with photometric weak lensing surveys: Constraints with redshift tomography of convergence peaks and moments". United States.
doi:10.1103/PhysRevD.94.063534. https://www.osti.gov/servlets/purl/1336177.
@article{osti_1336177,
title = {Cosmology with photometric weak lensing surveys: Constraints with redshift tomography of convergence peaks and moments},
author = {Petri, Andrea and May, Morgan and Haiman, Zoltán},
abstractNote = {Weak gravitational lensing is becoming a mature technique for constraining cosmological parameters, and future surveys will be able to constrain the dark energy equation of state w. When analyzing galaxy surveys, redshift information has proven to be a valuable addition to angular shear correlations. We forecast parameter constraints on the triplet (Ωm,w,σ8) for a LSSTlike photometric galaxy survey, using tomography of the shearshear power spectrum, convergence peak counts and higher convergence moments. Here we find that redshift tomography with the power spectrum reduces the area of the 1σ confidence interval in (Ωm,w) space by a factor of 8 with respect to the case of the single highest redshift bin. We also find that adding nonGaussian information from the peak counts and higherorder moments of the convergence field and its spatial derivatives further reduces the constrained area in (Ωm,w) by factors of 3 and 4, respectively. When we add cosmic microwave background parameter priors from Planck to our analysis, tomography improves power spectrum constraints by a factor of 3. Adding moments yields an improvement by an additional factor of 2, and adding both moments and peaks improves by almost a factor of 3 over power spectrum tomography alone. We evaluate the effect of uncorrected systematic photometric redshift errors on the parameter constraints. In conclusion, we find that different statistics lead to different bias directions in parameter space, suggesting the possibility of eliminating this bias via selfcalibration.},
doi = {10.1103/PhysRevD.94.063534},
journal = {Physical Review D},
number = 6,
volume = 94,
place = {United States},
year = 2016,
month = 9
}
Web of Science

Using cross correlations to calibrate lensing source redshift distributions: Improving cosmological constraints from upcoming weak lensing surveys
Cross correlations between the galaxy number density in a lensing source sample and that in an overlapping spectroscopic sample can in principle be used to calibrate the lensing source redshift distribution. In this paper, we study in detail to what extent this crosscorrelation method can mitigate the loss of cosmological information in upcoming weak lensing surveys (combined with a cosmic microwave background prior) due to lack of knowledge of the source distribution. We consider a scenario where photometric redshifts are available and find that, unless the photometric redshift distribution p(z {sub ph}z) is calibrated very accurately a priori (bias andmore » 
Selfcalibration of photometric redshift scatter in weaklensing surveys
Photoz errors, especially catastrophic errors, are a major uncertainty for precision weak lensing cosmology. We find that the shear(galaxy number) density and densitydensity cross correlation measurements between photoz bins, available from the same lensing surveys, contain valuable information for selfcalibration of the scattering probabilities between the truez and photoz bins. The selfcalibration technique we propose does not rely on cosmological priors nor parameterization of the photoz probability distribution function, and preserves all of the cosmological information available from shearshear measurement. We estimate the calibration accuracy through the Fisher matrix formalism. We find that, for advanced lensing surveys such as themore »Cited by 22 
Combining weaklensing tomography and spectroscopic redshift surveys
Redshift space distortion (RSD) is a powerful way of measuring the growth of structure and testing General Relativity, but it is limited by cosmic variance and the degeneracy between galaxy bias b and the growth rate factor f. The crosscorrelation of lensing shear with the galaxy density field can in principle measure b in a manner free from cosmic variance limits, breaking the fb degeneracy and allowing inference of the matter power spectrum from the galaxy survey. We analyze the growth constraints from a realistic tomographic weak lensing photoz survey combined with a spectroscopic galaxy redshift survey over the samemore »Cited by 23 
A CLIPPING METHOD TO MITIGATE THE IMPACT OF CATASTROPHIC PHOTOMETRIC REDSHIFT ERRORS ON WEAK LENSING TOMOGRAPHY
We use a mock catalog of galaxies based on the COSMOS galaxy catalog, including information on photometric redshift (photoz) and spectral energy distribution types of galaxies, in order to study how to define a galaxy subsample suitable for weak lensing tomography feasible with optical (and nearIR) multiband data. Since most useful cosmological information arises from the sample variance limited regime for upcoming lensing surveys, a suitable subsample can be obtained by discarding a large fraction of galaxies that have less reliable photoz estimations. We develop a method to efficiently identify photoz outliers by monitoring the width of the posterior likelihoodmore »