CFHTLenS: the Canada–France–Hawaii Telescope Lensing Survey – imaging data and catalogue products

By Catherine Heymans, L. Waerbeke, L. Miller, T. Erben, H. Hildebrandt, H. Hoekstra, Thomas D. Kitching, Y. Mellier, P. Simon, C. Bonnett and 12 more. 2012

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We present data products from the Canada–France–Hawaii Telescope Lensing Survey (CFHTLenS). CFHTLenS is based on the Wide component of the Canada–France–Hawaii Telescope Legacy Survey (CFHTLS). It encompasses 154 deg^2 of deep, optical, high-quality, sub-arcsecond imaging data in the five optical filters u*g′r′i′z′. The scientific aims of the CFHTLenS team are weak gravitational lensing studies supported by photometric redshift estimates for the galaxies. This paper presents our data processing of the complete CFHTLenS data set. We were able to obtain a data set with very good image quality and high-quality astrometric and photometric calibration. Our external astrometric accuracy is between 60 and 70 mas with respect to Sloan Digital Sky Survey (SDSS) data, and the internal alignment in all filters is around 30 mas. Our average photometric calibration shows a dispersion of the order of 0.01–0.03 mag for g′r′i′z′ and about 0.04 mag for u* with respect to SDSS sources down to i_(SDSS) ≤ 21. We demonstrate in accompanying papers that our data meet necessary requirements to fully exploit the survey for weak gravitational lensing analyses in connection with photometric redshift studies. In the spirit of the CFHTLS, all our data products are released to the astronomical community via the Canadian Astronomy Data Centre at http://www.cadc-ccda.hia-iha.nrc-cnrc.gc.ca/community/CFHTLens/query.html. We give a description and how-to manuals of the public products which include image pixel data, source catalogues with photometric redshift estimates and all relevant quantities to perform weak lensing studies.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/c2ede7b5c791265607874b3682c50fd63785ef09

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Citations in the corpus

H0LiCOW - V. New COSMOGRAIL time delays of HE 0435-1223: H0 to 3.8 per cent precision from strong lensing in a flat ΛCDM model (2016, methodology): “We compare weighted galaxy number counts around the lens, given an aperture and flux limit, to those through similar apertures and flux limits in CFHTLenS (Heymans et al. 2012).”
Photometric redshift analysis in the Dark Energy Survey Science Verification data (2014, methodology): “Of particular interest is the comparison to the CFHTLS and CFHTLenS (which are two different reductions of the same survey), photo-z results (Coupon et al. 2009; Hildebrandt et al. 2012), due to the similitudes between CFHTLS and DES in terms of survey specifications.”
Updated results on neutrino mass and mass hierarchy from cosmology with Planck 2018 likelihoods (2019, result): “The model also produces lower σ8 and S8 values compared to other models considered in the paper, leading to a decrease in the σ8 tension present between Planck and cosmic shear experiments like CFHTLenS [97], KiDS-450 [98] etc. – 17 –”
Dark Energy Survey Year 1 results: weak lensing shape catalogues (2017, neutral): “Stage II surveys included DLS (Jee et al. 2013), SDSS (Lin et al. 2012; Huff et al. 2014), RCSLenS (Hildebrandt et al. 2016), CFHTLenS (Heymans et al. 2012) as well as early science verification (SV) DES results in Jarvis et al. (2016).”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Constraining modified gravity (2016, methodology): “One source of tension is shown when the lensing measurements of the amplitude of matter clustering from CFHTLS (Heymans et al. 2012) and KiDS (Hildebrandt et al. 2016) are compared to those made with Planck CMB measurements including CMB-lensing, with the KiDS data showing a 2.3σ tension with the Pl”
KiDS-450: The tomographic weak lensing power spectrum and constraints on cosmological parameters (2017, methodology): “We calculate the effective number density of galaxies used in the lensing analysis following Heymans et al. (2012) as neff = 1 ( ∑ i wi) 2∑ i w 2 i , (13) where w is the lensfit weight and the unmasked area is denoted as .”
QUANTIFYING DISCORDANCE IN THE 2015 PLANCK CMB SPECTRUM (2015, background): “…is assumed, including a 2.5σ tension with the Riess et al. (2011) determination of the Hubble constant, H0, 2 − 3σ tension with weak lensing measurements of the CFHTLens survey (Heymans et al. 2012), and tension with the abundance of massive galaxy clusters (e.g., Planck Collaboration XXIV 2015).”
Dark Energy Survey Year 1 Results: The Photometric Data Set for Cosmology (2017, methodology): “Specifically, our CFHTLenS stellar selection was (FITCLASS = 1) OR (CLASS STAR > 0.98) and our galaxy selection was (FITCLASS = 0) OR (CLASS STAR 0.2).”
Cosmology from cosmic shear power spectra with Subaru Hyper Suprime-Cam first-year data (2018, background): “For instance, the Canada-FranceHawaii Telescope Lensing Survey (CFHTLS) survey observed ∼ 107 galaxies over 154 square degrees of the sky (CFHTLenS; Heymans et al. 2012) to conduct tomographic analyses (Hu 1999) of cosmic shear (Heymans et al. 2013; Kilbinger et al. 2013; Kitching et al. 2014).”
DETECTION OF LENSING SUBSTRUCTURE USING ALMA OBSERVATIONS OF THE DUSTY GALAXY SDP.81 (2016, background): “…George St., Toronto ON M5S 3H8, Canada 12 Hubble Fellow 13 Canada Research Chair in Astrophysics servations, including cosmic microwave background (CMB) anisotropies (Planck Collaboration et al. 2015), galaxy clustering (Anderson et al. 2014), and weak gravitational lensing (Heymans et al. 2012).”
The DES Science Verification weak lensing shear catalogues (2015, methodology): “Most of our null tests were similar to ones that have been performed in previous analyses (cf. e.g. Jarvis et al. 2003; Schrabback et al. 2010; Velander et al. 2011; Heymans et al. 2012b; Jee et al. 2013; Kuijken et al. 2015).”
Gravitational lensing analysis of the Kilo-Degree Survey (2015, methodology): “Over the past two decades, telescopes equipped with larger and larger CCD cameras have provided the means to make wide-area weak lensing studies possible: most recently from the CFHTLenS analysis of the CFHT Legacy Survey (Heymans et al. 2012, henceforth H+12), which targeted galaxies (see for examp”
EIGHT ULTRA-FAINT GALAXY CANDIDATES DISCOVERED IN YEAR TWO OF THE DARK ENERGY SURVEY (2015, methodology): “For the CFHTLenS matching, we identified probable stars in the CFHTLenS catalog using a combination of the class_star output from SExtractor and the fitclass output from the lensfit code (Heymans et al. 2012).”
FORTY-SEVEN MILKY WAY-SIZED, EXTREMELY DIFFUSE GALAXIES IN THE COMA CLUSTER (2014, background): “INTRODUCTION While there have been tremendous advances in deep, high resolution imaging surveys over the past decades (e.g., Scoville et al. 2007; Heymans et al. 2012), the low surface brightness sky remains relatively unexplored.”
The Hyper Suprime-Cam SSP Survey: Overview and Survey Design (2017, background): “For example, the CFHT Lens Survey (Heymans et al. 2012) covers 154 deg2 in five bands, to i′ = 25.5.”
Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: Cosmological implications from two decades of spectroscopic surveys at the Apache Point Observatory (2020, background): “…has been supplemented by increasingly robust and statistically sensitive estimates of weak lensing based on galaxy shapes, including CFHTLenS (Heymans et al. 2012), KiDS (Köhlinger et al. 2017), Dark Energy Survey (DES; Zuntz et al. 2018; Abbott et al. 2018), and Hyper Suprime-Cam survey…”