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

Erben, T.; Hildebrandt, Hendrik; Miller, L.; Waerbeke, Ludovic Van; Heymans, Catherine; Hoekstra, Henk; Kitching, Thomas D.; Mellier, Y.; Benjamin, J.; Blake, Chris; Bonnett, C.; Cordes, O.; Coupon, J.; Fu, Liping; Gavazzi, R.; Gillis, B.; Grocutt, Emma; Gwyn, Stephen; Holhjem, K.; Hudson, Michael J.; Kilbinger, M.; Kuijken, Konrad; Milkeraitis, Martha; Rowe, Barnaby; Schrabback, T.; Semboloni, Elisabetta; Simon, Patrick; Smit, Merijn; Toader, O.; Vafaei, Sanaz; Uitert, Edo van; Velander, Malin

doi:10.1093/mnras/stt928

Cited by 400 publications

(471 citation statements)

References 59 publications

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“…The largest of the Stage II weak lensing programs was the CFHT Legacy Survey. After a thorough analysis, the lensing results and cosmological implications were recently published (Heymans et al, 2012b;Benjamin et al, 2012;Erben et al, 2012;Kilbinger et al, 2012;Miller et al, 2013). They appear consistent with the standard ΛCDM cosmology with WMAPderived initial conditions, with the amplitude σ 8 measured to ±0.03.…”

Section: Cosmic Shearsupporting

confidence: 53%

Observational probes of cosmic acceleration

et al. 2013

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The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious efforts to understand its origin, with experiments that aim to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and the abundance of galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski effect, and direct measurements of the Hubble constant H 0 . We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from General Relativity, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and cosmic microwave background data. We also show the level of precision required for clusters or other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets that support a wide range of scientific investigations, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales.

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Section: Cosmic Shearsupporting

confidence: 53%

Observational probes of cosmic acceleration

et al. 2013

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“…The r-band data were also reduced with the THELI pipeline (Erben et al 2013), independently of the ASTRO-WISE pipeline, in order to measure the shapes of galaxies. We used only the r-band data for shape measurements, since the r-band observing conditions are significantly better than in the other three bands (see de Jong et al 2013); combining different bands is not expected to result in a useful improvement in shape measurements.…”

Section: Shape Measurementsmentioning

confidence: 99%

The masses of satellites in GAMA galaxy groups from 100 square degrees of KiDS weak lensing data

Sifón¹,

Cacciato²,

Hoekstra³

et al. 2015

Mon. Not. R. Astron. Soc.

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We use the first 100 deg 2 of overlap between the Kilo-Degree Survey (KiDS) and the Galaxy And Mass Assembly (GAMA) survey to determine the galaxy halo mass of ∼10,000 spectroscopically-confirmed satellite galaxies in massive (M > 10 13 h −1 M ) galaxy groups. Separating the sample as a function of projected distance to the group centre, we jointly model the satellites and their host groups with Navarro-Frenk-White (NFW) density profiles, fully accounting for the data covariance. The probed satellite galaxies in these groups have total masses log M sub /(h −1 M ) ≈ 11.7 − 12.2 consistent across group-centric distance within the errorbars. Given their typical stellar masses, log M ,sat /(h −2 M ) ∼ 10.5, such total masses imply stellar mass fractions of M ,sat /M sub ≈ 0.04 h −1 . The average subhalo hosting these satellite galaxies has a mass M sub ∼ 0.015M host independent of host halo mass, in broad agreement with the expectations of structure formation in a ΛCDM universe.

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“…CS82 covers a large fraction of the SDSS Stripe 82 with high quality i-band imaging under excellent seeing conditions in the range of 0.4 to 0.8 arcsec with an average of 0.59 arcsec. The survey contains a total of 173 tiles, 165 of which from CS82 observations and 8 from CFHT-LS Wide (Erben et al 2013). Each CS82 tile was obtained from 4 consecutive dithered observations each with an exposure time of 410 seconds.…”

Section: Cfht Stripe 8survey and Weak Lensing Cataloguesmentioning

confidence: 99%

“…The index MASK describes the mask information at an object's position. Objects with MASK ≤ 1 can safely be used for most weak lensing analyses (Erben et al 2013). No magnitude cut is applied for the catalogue as fainter galaxies have lower weights.…”

Section: Cfht Stripe 8survey and Weak Lensing Cataloguesmentioning

confidence: 99%

Cosmological constraints from weak lensing peak statistics with Canada-France-Hawaii Telescope Stripe 82 Survey

Liu¹,

Pan²,

Li³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We derived constraints on cosmological parameters using weak lensing peak statistics measured on the ∼ 130 deg 2 of the Canada-France-Hawaii Telescope Stripe 82 Survey (CS82). This analysis demonstrates the feasibility of using peak statistics in cosmological studies. For our measurements, we considered peaks with signal-to-noise ratio in the range of ν = [3, 6]. For a flat ΛCDM model with only (Ω m , σ 8 ) as free parameters, we constrained the parameters of the following relation Σ 8 = σ 8 (Ω m /0.27) α to be: Σ 8 = 0.82 ± 0.03 and α = 0.43 ± 0.02. The α value found is considerably smaller than the one measured in two-point and three-point cosmic shear correlation analyses, showing a significant complement of peak statistics to standard weak lensing cosmological studies. The derived constraints on (Ω m , σ 8 ) are fully consistent with the ones from either WMAP9 or Planck. From the weak lensing peak abundances alone, we obtained marginalised mean values of Ω m = 0.38 +0.27 −0.24 and σ 8 = 0.81 ± 0.26. Finally, we also explored the potential of using weak lensing peak statistics to constrain the mass-concentration relation of dark matter halos simultaneously with cosmological parameters.

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

Cited by 400 publications

References 59 publications

Observational probes of cosmic acceleration

Observational probes of cosmic acceleration

The masses of satellites in GAMA galaxy groups from 100 square degrees of KiDS weak lensing data

Cosmological constraints from weak lensing peak statistics with Canada-France-Hawaii Telescope Stripe 82 Survey

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