2015
DOI: 10.1093/mnras/stv398
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Mass and galaxy distributions of four massive galaxy clusters from Dark Energy Survey Science Verification data

Abstract: We measure the weak-lensing masses and galaxy distributions of four massive galaxy clusters observed during the Science Verification phase of the Dark Energy Survey. This pathfinder study is meant to 1) validate the DECam imager for the task of measuring weak-lensing shapes, and 2) utilize DECam's large field of view to map out the clusters and their environments over 90 arcmin. We conduct a series of rigorous tests on astrometry, photometry, image quality, PSF modeling, and shear measurement accuracy to singl… Show more

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Cited by 66 publications
(76 citation statements)
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“…They also identified a second galaxy cluster in the field of view at redshift ∼0.6, with an estimated mass of M 200m = 4.0 +3.7 −2.6 × 10 14 M . Melchior et al (2015) studied the weak lensing masses and galaxy distributions of four massive clusters observed during the DES SV period, including RXJ2248. They found M 200c = 17.5 +4.3 −3.7 × 10 14 M , which is in agreement with previous mass estimates.…”
Section: T H E C L U S T E R R X C J 2 2 4 8 7 −4 4mentioning
confidence: 99%
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“…They also identified a second galaxy cluster in the field of view at redshift ∼0.6, with an estimated mass of M 200m = 4.0 +3.7 −2.6 × 10 14 M . Melchior et al (2015) studied the weak lensing masses and galaxy distributions of four massive clusters observed during the DES SV period, including RXJ2248. They found M 200c = 17.5 +4.3 −3.7 × 10 14 M , which is in agreement with previous mass estimates.…”
Section: T H E C L U S T E R R X C J 2 2 4 8 7 −4 4mentioning
confidence: 99%
“…We study the galaxy completeness c g , defined as the ratio of the number of true 2 A comparison of weak lensing measurements between DES and CLASH was not performed because they predominantly reveal differences in the shear calibration. The majority of galaxies with shape measurement in both catalogues are very faint for DES, resulting in large and noisy calibration factors (see section 4.2.1 in Melchior et al 2015). In addition, the high density of galaxies in the central region of this cluster creates many more close galaxy pairs or even blends in ground-based DES images than when viewed with HST, rendering shape measurement even more challenging.…”
Section: Star/galaxy Separationmentioning
confidence: 99%
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