3D cosmic shear: cosmology from CFHTLenS

T. D. Kitching, A. F. Heavens, J. Alsing, T. Erben, C. Heymans, H. Hildebrandt, H. Hoekstra, A. Jaffe, A. Kiessling, Y. Mellier, L. Miller, L. van Waerbeke, J. Benjamin, J. Coupon, L. Fu, M. J. Hudson, M. Kilbinger, K. Kuijken, B. T. P. Rowe, T. SchrabbackE. Semboloni, M. Velander

Research output: Contribution to journalArticlepeer-review

Abstract

This paper presents the first application of 3D cosmic shear to a wide-field weak lensing survey. 3D cosmic shear is a technique that analyses weak lensing in three dimensions using a spherical harmonic approach, and does not bin data in the redshift direction. This is applied to CFHTLenS, a 154 square degree imaging survey with a median redshift of 0.7 and an effective number density of 11 galaxies per square arcminute usable for weak lensing. To account for survey masks we apply a 3D pseudo-C-a"" approach on weak lensing data, and to avoid uncertainties in the highly non-linear regime, we separately analyse radial wavenumbers k a parts per thousand currency sign 1.5 and 5.0 h Mpc(-1), and angular wavenumbers a"" a parts per thousand 400-5000. We show how one can recover 2D and tomographic power spectra from the full 3D cosmic shear power spectra and present a measurement of the 2D cosmic shear power spectrum, and measurements of a set of 2-bin and 6-bin cosmic shear tomographic power spectra; in doing so we find that using the 3D power in the calculation of such 2D and tomographic power spectra from data naturally accounts for a minimum scale in the matter power spectrum. We use 3D cosmic shear to constrain cosmologies with parameters Omega(M), Omega(B), sigma(8), h , n(s), w(0) and w(a). For a non-evolving dark energy equation of state, and assuming a flat cosmology, lensing combined with Wilkinson Microwave Anisotropy Probe 7 results in h = 0.78 +/- 0.12, Omega(M) = 0.252 +/- 0.079, sigma(8) = 0.88 +/- 0.23 and w = -1.16 +/- 0.38 using only scales k a parts per thousand currency sign 1.5 h Mpc(-1). We also present results of lensing combined with first year Planck results, where we find no tension with the results from this analysis, but we also find no significant improvement over the Planck results alone. We find evidence of a suppression of power compared to Lambda cold dark matter (LCDM) on small scales 1.5 <k a parts per thousand currency sign 5.0 h Mpc(-1) in the lensing data, which is consistent with predictions of the effect of baryonic feedback on the matter power spectrum.

Original languageEnglish
Pages (from-to)1326-1349
Number of pages24
JournalMonthly Notices of the Royal Astronomical Society
Volume442
Issue number2
DOIs
Publication statusPublished - 1 Aug 2014

Keywords

  • gravitational lensing: weak
  • cosmological parameters
  • WEAK-LENSING SURVEYS
  • GALAXY SHAPE MEASUREMENT
  • MATTER POWER SPECTRUM
  • HUBBLE-SPACE-TELESCOPE
  • DARK ENERGY
  • INTRINSIC ALIGNMENTS
  • PRECISION COSMOLOGY
  • COVARIANCE-MATRIX
  • HALO MODEL
  • CONSTRAINTS

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