An optically-selected cluster catalog at redshift 0.1 &amp;lt; <i>z</i> &amp;lt; 1.1 from the Hyper Suprime-Cam Subaru Strategic Program S16A data

Oguri, Masamune; Lin, Yen-Ting; Lin, Sheng-Chieh; Nishizawa, Atsushi J.; More, Anupreeta; More, Surhud; Hsieh, Bau-Ching; Medezinski, Elinor; Miyatake, Hironao; Jian, Hung-Yu; Lin, Lihwai; Takada, Masahiro; Okabe, Nobuhiko; Speagle, Joshua S.; Coupon, J.; Leauthaud, Alexie; Lupton, Robert H.; Miyazaki, Satoshi; Price, P. A.; Tanaka, Masayuki; Chiu, I-Non; Komiyama, Yutaka; Okura, Yuki; Tanaka, M.; Usuda, Tomonori

doi:10.1093/pasj/psx042

Cited by 146 publications

(121 citation statements)

References 97 publications

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“…This result indicates that the ∆Σ-estimator with the weight Σ −2 cr is beneficial to extract the greater information in a given survey, especially for stacked lensing measurements of galaxy groups and clusters at high redshifts, which can be obtained in ongoing imaging surveys (e.g. Oguri et al 2018) and ground-based CMB experiments via the Sunyaev-Zel'dovich effect (e.g. Hasselfield et al 2013;Bleem et al 2015).…”

Section: Dependence On Lss Tracers and Survey Parametersmentioning

confidence: 99%

Stacked lensing estimators and their covariance matrices: excess surface mass density versus lensing shear

Shirasaki

Takada

2018

Monthly Notices of the Royal Astronomical Society

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Stacked lensing is a powerful means of measuring the average mass distribution around largescale structure tracers. There are two stacked lensing estimators used in the literature, denoted as ∆Σ and γ + , which are related as ∆Σ = Σ cr γ + , where Σ cr (z l , z s ) is the critical surface mass density for each lens-source pair (z l and z s are lens and source redshifts, respectively). In this paper we derive a formula for the covariance matrix of ∆Σ-estimator focusing on "weight" function to improve the signal-to-noise (S/N). We assume that the lensing fields and the distribution of lensing objects obey the Gaussian statistics. With this formula, we show that, if background galaxy shapes are weighted by an amount of Σ −2 cr (z l , z s ), the ∆Σ-estimator maximizes the S/N in the shot noise limited regime. We also show that the ∆Σ-estimator with the weight Σ −2 cr gives a greater (S/N) 2 than that of the γ + -estimator by about 5-25% for lensing objects at redshifts comparable with or higher than the median of source galaxy redshifts for hypothetical Subaru HSC and DES surveys. However, for low-redshift lenses such as z l < ∼ 0.3, the γ + -estimator has higher (S/N) 2 than ∆Σ. We also discuss that the (S/N) 2 for ∆Σ at large separations in the sample variance limited regime can be boosted, by up to a factor of 1.5, if one adopts a weight of Σ −α cr with α > 2. Our formula allows one to explore how the combination of the different estimators can approach an optimal estimator in all regimes of redshifts and separation scales.

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Section: Dependence On Lss Tracers and Survey Parametersmentioning

confidence: 99%

Stacked lensing estimators and their covariance matrices: excess surface mass density versus lensing shear

Shirasaki

Takada

2018

Monthly Notices of the Royal Astronomical Society

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“…The typical observed blue fraction of massive clusters is only 0.2 in the local Universe (e.g., Butcher & Oemler 1984). E-mail: tetsuya@phys.nthu.edu.tw So far, great efforts have been made to identify higher redshift galaxy clusters, targeting not only red galaxies but also star-forming emission-line galaxies (e.g., Koyama et al 2010;Hayashi et al 2012Hayashi et al , 2018Oguri et al 2018). In contrast to the local Universe, high-z clusters obviously include a number of star-forming galaxies (e.g., Hayashi et al 2018).…”

Section: Introductionmentioning

confidence: 99%

A young galaxy cluster in the old Universe

Hashimoto

Goto

Momose

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Galaxies evolve from a blue star-forming phase into a red quiescent one by quenching their star formation activity. In high density environments, this galaxy evolution proceeds earlier and more efficiently. Therefore, local galaxy clusters are dominated by well-evolved red, elliptical galaxies. The fraction of blue galaxies in clusters monotonically declines with decreasing redshift, i.e., the Butcher-Oemler effect. In the local Universe, observed blue fractions of massive clusters are as small as 0.2. Here we report a discovery of a "blue cluster", that is a local galaxy cluster with an unprecedentedly high fraction of blue star-forming galaxies yet hosted by a massive dark matter halo. The blue fraction is 0.57, which is 4.0 σ higher than those of the other comparison clusters under the same selection and identification criteria. The velocity dispersion of the member galaxies is 510 km s −1 , which corresponds to a dark matter halo mass of 2.0 +1.9 −1.0 × 10 14 M . The blue fraction of the cluster is more than 4.7 σ beyond the standard theoretical predictions including semi-analytic models of galaxy formation. The probability to find such a high blue fraction in an individual cluster is only 0.003%, which challenges the current standard frameworks of the galaxy formation and evolution in the ΛCDM Universe. The spatial distribution of galaxies around the blue cluster suggests that filamentary cold gas streams can exist in massive halos even in the local Universe. However these cold streams have already disappeared in the theoretically simulated local universes.

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“…Galaxy clusters are known to harbor red sequence (RS) galaxies, so named because these galaxies rest on a tight relation in the color-magnitude space (Bower et al 1992). The phenomenon has been employed in finding clusters from optical data (e.g., Gladders & Yee 2000;Miller et al 2005;Koester et al 2007;Rykoff et al 2016;Oguri et al 2018) and developing cluster mass proxies (e.g., Rykoff et al 2012). Red sequence galaxies also attract attention in astrophysics studies as they exhibit little star formation activity.…”

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confidence: 99%

Galaxies in X-ray selected clusters and groups in Dark Energy Survey data – II. Hierarchical Bayesian modelling of the red-sequence galaxy luminosity function

Zhang

Miller

Rooney

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Using ∼ 100 X-ray selected clusters in the Dark Energy Survey Science Verification data, we constrain the luminosity function (LF) of cluster red sequence galaxies as a function of redshift. This is the first homogeneous optical/X-ray sample large enough to constrain the evolution of the luminosity function simultaneously in redshift (0.1 < z < 1.05) and cluster mass (13.5 ≤ log 10 (M 200crit ) ∼< 15.0). We pay particular attention to completeness issues and the detection limit of the galaxy sample. We then apply a hierarchical Bayesian model to fit the cluster galaxy LFs via a Schecter function, including its characteristic break (m * ) to a faint end power-law slope (α). Our method enables us to avoid known issues in similar analyses based on stacking or binning the clusters. We find weak and statistically insignificant (∼ 1.9σ) evolution in the faint end slope α versus redshift. We also find no dependence in α or m * with the X-ray inferred cluster masses. However, the amplitude of the LF as a function of cluster mass is constrained to ∼ 20% precision. As a by-product of our algorithm, we utilize the correlation between the LF and cluster mass to provide an improved estimate of the individual cluster masses as well as the scatter in true mass given the X-ray inferred masses. This technique can be applied to a larger sample of X-ray or optically selected clusters from the Dark Energy Survey, significantly improving the sensitivity of the analysis.Galaxy clusters are special for both cosmology and astrophysics studies. As the structures that correspond to the massive end of halo mass function, they are sensitive probes of the ΛCDM cos-

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An optically-selected cluster catalog at redshift 0.1 < z < 1.1 from the Hyper Suprime-Cam Subaru Strategic Program S16A data

Cited by 146 publications

References 97 publications

Stacked lensing estimators and their covariance matrices: excess surface mass density versus lensing shear

Stacked lensing estimators and their covariance matrices: excess surface mass density versus lensing shear

A young galaxy cluster in the old Universe

Galaxies in X-ray selected clusters and groups in Dark Energy Survey data – II. Hierarchical Bayesian modelling of the red-sequence galaxy luminosity function

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An optically-selected cluster catalog at redshift 0.1 &lt; z &lt; 1.1 from the Hyper Suprime-Cam Subaru Strategic Program S16A data

Cited by 146 publications

References 97 publications

Stacked lensing estimators and their covariance matrices: excess surface mass density versus lensing shear

Stacked lensing estimators and their covariance matrices: excess surface mass density versus lensing shear

A young galaxy cluster in the old Universe

Galaxies in X-ray selected clusters and groups in Dark Energy Survey data – II. Hierarchical Bayesian modelling of the red-sequence galaxy luminosity function

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An optically-selected cluster catalog at redshift 0.1 < z < 1.1 from the Hyper Suprime-Cam Subaru Strategic Program S16A data