First Results on Shear‐selected Clusters from the Deep Lens Survey: Optical Imaging, Spectroscopy, and X‐Ray Follow‐up

Wittman, David; Dell’Antonio, Ian; Hughes, John P.; Margoniner, V. E.; Tyson, J. A.; Cohen, Judith G.; Norman, Dara

doi:10.1086/502621

Cited by 151 publications

(226 citation statements)

References 42 publications

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“…They base the convergence (κ) map on sources in the range 22.0 < R < 25.5. After removal of objects which are too small relative to the point-spread function (PSF), so large that they are probably nearby, or so elongated that they are probably superpositions (Wittman et al 2006), the source catalog contains 328,000 galaxies or 23 galaxies arcmin −2 . This source density is within the range of other ground-based surveys (Miyazaki et al 2007;Schirmer et al 2007;Gavazzi & Soucail 2007).…”

Section: The Dls Map (F2)mentioning

confidence: 99%

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Shels: Testing Weak-Lensing Maps With Redshift Surveys

Geller

Kurtz

Dell’Antonio

et al. 2010

ApJ

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Weak-lensing surveys are emerging as an important tool for the construction of "mass-selected" clusters of galaxies. We evaluate both the efficiency and completeness of a weak-lensing selection by combining a dense, complete redshift survey, the Smithsonian Hectospec Lensing Survey (SHELS), with a weak-lensing map from the Deep Lens Survey (DLS). SHELS includes 11,692 redshifts for galaxies with R 20.6 in the 4 deg 2 DLS field; the survey is a solid basis for identifying massive clusters of galaxies with redshift z 0.55. The range of sensitivity of the redshift survey is similar to the range for the DLS convergence map. Only four of the 12 convergence peaks with signal to noise 3.5 correspond to clusters of galaxies with M 1.7 × 10 14 M . Four of the eight massive clusters in SHELS are detected in the weak-lensing map yielding a completeness of ∼50%. We examine the seven known extended cluster X-ray sources in the DLS field: three can be detected in the weak-lensing map, three should not be detected without boosting from superposed large-scale structure, and one is mysteriously undetected even though its optical properties suggest that it should produce a detectable lensing signal. Taken together, these results underscore the need for more extensive comparisons among different methods of massive cluster identification.

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Section: The Dls Map (F2)mentioning

confidence: 99%

“…9 Notes. a Chandra 0.5-2 keV flux from Table 3 of Wittman et al (2006). b For these entries, we list the number of galaxies within the intercepted large-scale structure.…”

Section: Known X-ray Clusters In the Dls Fieldmentioning

confidence: 99%

Shels: Testing Weak-Lensing Maps With Redshift Surveys

Geller

Kurtz

Dell’Antonio

et al. 2010

ApJ

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“…To overcome this limitation, higher order cosmic shear correlation analyses are a natural extension (e.g., Semboloni et al 2011;van Waerbeke et al 2013;Fu et al 2014). Weak lensing peak statistics, i.e., concentrating on high signal regions, is another way to probe efficiently the nonlinear regime of the structure formation, and thus can provide important complements to the cosmic shear 2-pt correlation analysis (e.g., White et al 2002;Hamana et al 2004;Tang & Fan 2005;Hennawi & Spergel 2005;Dietrich & Hartlap 2010;Kratochvil et al 2010;Yang et al 2011;Marian et al 2012;Hilbert et al 2012;Bard et al 2013;Lin & Kilbinger 2015) Observationally, different analyses have proved the feasibility of performing weak lensing peak searches from data (e.g., Wittman et al 2006;Gavazzi & Soucail 2007;Miyazaki et al 2007;Geller et al 2010). However, up to now, few cosmological constraints are derived from weak lensing peak statistics in real observations.…”

Section: Introductionmentioning

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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“…Thanks to considerable efforts with on-going cluster surveys, which are utilizing a variety of methods (e.g., Gladders & Yee 2000;Rosati et al 2002;Eisenhardt et al 2004;Wilson et al 2005;Wittman et al 2006;Fassbender 2008;Staniszewski et al 2009;Andreon et al 2009;Demarco et al 2010, and references therein), the number of known high-redshift clusters is increasing, however only a handful of spectroscopically confirmed galaxy clusters beyond redshift 1.3 have been discovered to date (Mullis et al 2005;Stanford et al 2005Stanford et al , 2006Eisenhardt et al 2008;Wilson et al 2009;Papovich et al 2010;Tanaka et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Cluster galaxies in XMMU J2235-2557: galaxy population properties in most massive environments atz ~ 1.4

Strazzullo

Rosati

Pannella

et al. 2010

A&A

130

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We present a multi-wavelength study of galaxy populations in the core of the massive, X-ray luminous cluster XMMU J2235 at z = 1.39, based on high quality VLT and HST photometry at optical and near-infrared wavelengths. We derive luminosity functions in the z, H, and K s bands, approximately corresponding to restframe U, R and z band. These show a faint-end slope consistent with being flat, and a characteristic magnitude M * close to passive evolution predictions of M * of local massive clusters, with a formation redshift z > 2. The color−magnitude and color-mass diagrams show evidence of a tight red sequence (intrinsic scatter < ∼ 0.08) of massive galaxies already in place, with overall old stellar populations and generally early-type morphology. Beside the red colors, these massive (>6 × 10 10 M ) galaxies typically show early-type spectral features, and rest-frame far-UV emission consistent with very low star formation rates (SFR < 0.2 M yr −1 ). Star forming spectroscopic members, with SFR of up to ∼100 M /yr, are all located at clustercentric distances > ∼ 250 kpc, with the central cluster region already appearing effectively quenched. Most part of the cluster galaxies more massive than 6 × 10 10 M within the studied area do not appear to host significant levels of star formation. The high-mass end of the galaxy populations in the core of this cluster appears to be in a very advanced evolutionary stage, not only in terms of formation of the stellar populations, but also of the assembly of the stellar mass. The high-mass end of the galaxy stellar mass function is essentially already in place. The stellar mass fraction estimated within r 500 (∼1%, Kroupa IMF) is already similar to that of local massive clusters. On the other hand, surface brightness distribution modeling of the massive red sequence galaxies may suggest that their size is often smaller than expected based on the local stellar mass vs. size relation. An evolution of the stellar mass vs. size relation might imply that, in spite of the overall early assembly of these sources, their evolution is not complete, and processes like minor (and likely dry) merging might still shape the structural properties of these objects to resemble those of their local counterparts, without substantially affecting their stellar mass or host stellar populations. Nonetheless, a definite conclusion on the actual relevance of size evolution for the studied early-type sample is precluded by possible systematics and biases.

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First Results on Shear‐selected Clusters from the Deep Lens Survey: Optical Imaging, Spectroscopy, and X‐Ray Follow‐up

Cited by 151 publications

References 42 publications

Shels: Testing Weak-Lensing Maps With Redshift Surveys

Shels: Testing Weak-Lensing Maps With Redshift Surveys

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

Cluster galaxies in XMMU J2235-2557: galaxy population properties in most massive environments atz ~ 1.4

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