Very weak lensing in the CFHTLS Wide: Cosmology from cosmic shear in the linear regime

By L. Fu, E. Semboloni, H. Hoekstra, M. Kilbinger, L. Waerbeke, Ismael Tereno, Y. Mellier, Catherine Heymans, Jean Coupon, K. Benabed and 9 more. 2007

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Aims. We present an exploration of weak lensing by large-scale structure in the linear regime, using the third-year (T0003) CFHTLS Wide data release. Our results place tight constraints on the scaling of the amplitude of the matter power spectrum σ8 with the matter density Ωm. Methods. Spanning 57 square degrees to i � = 24.5 over three independent fields, the unprecedented contiguous area of this survey permits high signal-to-noise measurements of two-point shear statistics from 1 arcmin to 4 degrees. Understanding systematic errors in our analysis is vital in interpreting the results. We therefore demonstrate the percent-level accuracy of our method using STEP simulations, an E/B-mode decomposition of the data, and the star-galaxy cross correlation function. We also present a thorough analysis of the galaxy redshift distribution using redshift data from the CFHTLS T0003 Deep fields that probe the same spatial regions as the Wide fields. Results. We find σ8(Ωm/0.25) 0.64 = 0.785 ± 0.043 using the aperture-mass statistic for the full range of angular scales for an assumed flat cosmology, in excellent agreement with WMAP3 constraints. The largest physical scale probed by our analysis is 85 Mpc, assuming a mean redshift of lenses of 0.5 and a ΛCDM cosmology. This allows for the first time to constrain cosmology using only cosmic shear measurements in the linear regime. Using only angular scales θ> 85 arcmin, we find σ8(Ωm/0.25) 0.53 lin = 0.837 ± 0.084, which agree with the results from our full analysis. Combining our results with data from WMAP3, we find Ωm = 0.248 ± 0.019 and σ8 = 0.771 ± 0.029.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/0b1759b31062cc360c6c3692d44ea6746413a2c2

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Citations in the corpus

Consistently large cosmic flows on scales of 100 h−1 Mpc: a challenge for the standard ΛCDM cosmology (2008, background): “The most recent weak-lensing result from the Canada–France–Hawaii Telescope Legacy Survey (CFHTLS; Fu et al. 2008) find σ 8( m/0.25)0.64 = 0.785 ± 0.043 when all angular scales are analysed, but σ 8( m/0.25)0.53 = 0.837 ± 0.084 when only scales in the linear regime are studied.”
Galaxy Masses: A Review (2013, methodology): “In this situation the galaxy power spectrum is b(2) times the matter power spectrum, P (k) which can be measured through cosmic shear studies (Hoekstra & Jain 2008; Fu et al. 2008)). The value of the bias parameter b is not known a priori. Similarly, the galaxy-mass cross-power spectrum will be b× r”
Evidence of the accelerated expansion of the Universe from weak lensing tomography with COSMOS (2009, positive): “…al. 2003; Jarvis et al. 2003; Massey et al. 2005; Van Waerbeke et al. 2005; Hoekstra et al. 2006; Semboloni et al. 2006; Hetterscheidt et al. 2007; Fu et al. 2008), while tests on simulated data have led to a better understanding of PSF systematics (Heymans et al. 2006a; Massey et al. 2007a;…”
Measuring the galaxy–mass and galaxy–dust correlations through magnification and reddening (2009, background): “…sources can be magnified, as detected by Scranton et al. (2005), and galaxy shapes can be distorted as measured through galaxygalaxy lensing (cf. Hoekstra et al. 2002, Sheldon et al. 2004, Mandelbaum et al. 2005, Leauthaud et al. 2007; Parker et al. 2007) and cosmic shear (e.g. Fu et al. 2008).”
The effects of galaxy formation on the matter power spectrum: a challenge for precision cosmology (2011, background): “Some of the most accurate measurements of the matter power spectrum come from studies of weak, gravitational lensing (e.g. Massey et al. 2007; Fu et al. 2008; Schrabback et al. 2010), galaxy clustering (e.g. Cole et al. 2005; Reid et al. 2010) and the Lyα forest (e.g. Viel et al. 2004; McDonald et…”
Ray-tracing through the Millennium Simulation: Born corrections and lens-lens coupling in cosmic shear and galaxy-galaxy lensing (2008, background): “…of the cosmic matter distribution (e.g. Semboloni et al. 2006; Hoekstra et al. 2006; Simon et al. 2007; Benjamin et al. 2007; Massey et al. 2007b; Fu et al. 2008), the growth of structure (e.g. Bacon et al. 2005; Massey et al. 2007c), and the nature of the dark energy (e.g. Taylor et al. 2007;…”
Quantifying the effect of baryon physics on weak lensing tomography (2011, methodology): “The cosmic shear signal has been measured using large ground-based surveys (e.g., Hoekstra et al. 2006; Fu et al. 2008) and from space (e.g., Massey et al. 2007; Schrabback et al. 2010).”
CFHTLenS: Improving the quality of photometric redshifts with precision photometry (2011, background): “…2000; Wittman et al. 2000; Semboloni et al. 2006; Hoekstra et al. 2006; Hetterscheidt et al. 2007; Schrabback et al. 2007, 2010; Massey et al. 2007; Fu et al. 2008), has been identified as one of the most promising probes of the effects of dark energy (DE; Albrecht et al. 2006; Peacock et al.…”
CFHTLenS: the Canada–France–Hawaii Telescope Lensing Survey – imaging data and catalogue products (2012, methodology): “In addition a problem with the redshift-scaling of the two-point shear correlation function soon became apparent when the data used in Fu et al. (2008) were combined with photometric redshift measurements from Coupon et al. (2009), (see Kilbinger et al. 2009, for more details).”
Multiscale cluster lens mass mapping - I. Strong lensing modelling (2009, background): “Since the early 90’s, gravitational lensing has appeared asa robust tool to model the mass distribution of cosmological objects alike galaxies, galaxy clusters and large scale structures (Gavazzi et al. 2007; Limousin et al. 2007; Massey et al. 2007; Fu et al. 2008).”
Results of the GREAT08 Challenge?: an image analysis competition for cosmological lensing: Results o (2009, background): “5 of Fu et al. 2008) (see also cosmic shear ring statistics described in Schneider & Kilbinger 2007; Eifler, Schneider & Krause 2009).”
CFHTLenS: combined probe cosmological model comparison using 2D weak gravitational lensing (2012, methodology): “…analyses of the CFHTLS used the first data release (T0001) with 4 deg2 of the Deep survey (Semboloni et al. 2005) and 22 deg2 of the Wide part of the survey (Hoekstra et al. 2006), followed by the third data release (T0003) comprising 55 deg2 (Benjamin et al. 2007; Fu et al. 2008, hereafter F08).”