The Wendelstein Weak Lensing (WWL) pathfinder: accurate weak lensing masses for Planck clusters

Seitz, S.; Bender, Ralf; Riffeser, A.; Kluge, Matthias; Goessl, Claus; Hopp, U.; Mana, A.; Ries, C.; Schmidt, Michael

doi:10.1093/mnras/stz817

Cited by 5 publications

(5 citation statements)

References 67 publications

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“…Most authors that are using three filters do not attempt to derive individual redshift estimates (von der Linden et al 2014;Hoekstra et al 2012;Medezinski et al 2010) and use polygonal shaped regions in colorcolor space to exclude cluster members. Empirically derived photo-z's of individual galaxies using three filters is rather rare in cluster weak lensing studies but was previously used in smaller studies by Gruen et al (2014) and Rehmann et al (2019).…”

Section: The Angular Diameter Distance Ratiomentioning

confidence: 99%

Weak lensing measurements of the APEX-SZ galaxy cluster sample

Klein

Israel

Nagarajan

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present a weak lensing analysis for galaxy clusters from the APEX-SZ survey. For 39 massive galaxy clusters that were observed via the Sunyaev-Zel'dovich effect (SZE) with the APEX telescope, we analyse deep optical imaging data from WFI(@2.2mMPG/ESO) and Suprime-Cam(@SUBARU) in three bands. The masses obtained in this study, including an X-ray selected subsample of 27 clusters, are optimised for and used in studies constraining the mass to observable scaling relations at fixed cosmology. A novel focus of our weak lensing analysis is the multi-colour background selection to suppress effects of cosmic variance on the redshift distribution of source galaxies. We investigate the effects of cluster member contamination through galaxy density, shear profile, and recovered concentrations. We quantify the impact of variance in source redshift distribution on the mass estimate by studying nine subfields of the COSMOS survey for different cluster redshift and manitude limits. We measure a standard deviation of ∼ 6% on the mean angular diameter distance ratio for a cluster at z = 0.45 and shallow imaging data of R ≈ 23 mag. It falls to ∼ 1% for deep, R = 26 mag, observations. This corresponds to 8.4% and 1.4% scatter in M 200 . Our background selection reduces this scatter by 20 − 40%, depending on cluster redshift and imaging depth. We derived cluster masses with and without using a mass concentration relation and find consistent results, and concentrations consistent with the used mass-concentration relation.

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Section: The Angular Diameter Distance Ratiomentioning

confidence: 99%

Weak lensing measurements of the APEX-SZ galaxy cluster sample

Klein

Israel

Nagarajan

et al. 2019

Monthly Notices of the Royal Astronomical Society

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show abstract

“…Wide-field observations of weak lensing with ground-based telescopes have successfully measured clusters' properties, including their mass (e.g. Umetsu et al 2014Umetsu et al , 2019Okabe & Smith 2016;Medezinski et al 2018a;Herbonnet et al 2019;McClintock et al 2019;Miyatake et al 2019;Rehmann et al 2019) and halo shape (e.g. Evans & Bridle 2009;Oguri et al 2010;Clampitt & Jain 2016;van Uitert et al 2017;Chiu et al 2018;Shin et al 2018;Umetsu et al 2018).…”

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confidence: 99%

The distribution of dark matter and gas spanning 6 Mpc around the post-merger galaxy cluster MS 0451−03

Tam

Jauzac

Massey

et al. 2020

Monthly Notices of the Royal Astronomical Society

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ABSTRACT Using the largest mosaic of Hubble Space Telescope images around a galaxy cluster, we map the distribution of dark matter throughout an ∼6 × 6 Mpc2 area centred on the cluster MS 0451−03 (z = 0.54, $M_{200}=1.65\times 10^{15}\, {\rm M}_{\odot }$). Our joint strong- and weak-lensing analysis shows three possible filaments extending from the cluster, encompassing six group-scale substructures. The dark matter distribution in the cluster core is elongated, consists of two distinct components, and is characterized by a concentration parameter of c200 = 3.79 ± 0.36. By contrast, XMM–Newton observations show the gas distribution to be more spherical, with excess entropy near the core, and a lower concentration of $c_{200}=2.35^{+0.89}_{-0.70}$ (assuming hydrostatic equilibrium). Such a configuration is predicted in simulations of major mergers 2–7 Gyr after the first core passage, when the two dark matter haloes approach second turnaround, and before their gas has relaxed. This post-merger scenario finds further support in optical spectroscopy of the cluster’s member galaxies, which shows that star formation was abruptly quenched 5 Gyr ago. MS 0451−03 will be an ideal target for future studies of the growth of structure along filaments, star formation processes after a major merger, and the late-stage evolution of cluster collisions.

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“…Wide-field observations of weak lensing with groundbased telescopes have successfully measured clusters' properties, including their mass (e.g. Umetsu et al 2014b;Okabe & Smith 2016;Medezinski et al 2018a;McClintock et al 2019;Miyatake et al 2019;Umetsu et al 2019;Rehmann et al 2019;Herbonnet et al 2019) and halo shape (e.g. Evans & Bridle 2009;Oguri et al 2010;Clampitt & Jain 2016;van Uitert et al 2017;Shin et al 2018;Umetsu et al 2018;Chiu et al 2018).…”

Section: Introductionmentioning

confidence: 99%

The distribution of dark matter and gas spanning six megaparsecs around the post-merger galaxy cluster MS0451-03

Tam,

Jauzac,

Massey

et al. 2020

Preprint

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Using the largest mosaic of Hubble Space Telescope images around a galaxy cluster, we map the distribution of dark matter throughout a ∼6 × 6 Mpc 2 area centred on the cluster MS 0451−03 (z = 0.54, M 200 = 1.65 × 10 15 M ). Our joint strong-and weak-lensing analysis shows three possible filaments extending from the cluster, encompassing six group-scale substructures. The dark-matter distribution in the cluster core is elongated, consists of two distinct components, and is characterized by a concentration parameter of c 200 = 3.79 ± 0.36. By contrast, XMM-Newton observations show the gas distribution to be more spherical, with excess entropy near the core, and a lower concentration of c 200 = 2.35 +0.89 −0.70 (assuming hydrostatic equilibrium). Such a configuration is predicted in simulations of major mergers 2-7 Gyr after the first core passage, when the two dark-matter halos approach second turnaround, and before their gas has relaxed. This post-merger scenario finds further support in optical spectroscopy of the cluster's member galaxies, which shows that star formation was abruptly quenched 5 Gyr ago. MS 0451−03 will be an ideal target for future studies of the growth of structure along filaments, star-formation processes after a major merger, and the late-stage evolution of cluster collisions.

show abstract

The Wendelstein Weak Lensing (WWL) pathfinder: accurate weak lensing masses for Planck clusters

Cited by 5 publications

References 67 publications

Weak lensing measurements of the APEX-SZ galaxy cluster sample

Weak lensing measurements of the APEX-SZ galaxy cluster sample

The distribution of dark matter and gas spanning 6 Mpc around the post-merger galaxy cluster MS 0451−03

The distribution of dark matter and gas spanning six megaparsecs around the post-merger galaxy cluster MS0451-03

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