CONSTRAINING THE SCATTER IN THE MASS-RICHNESS RELATION OF maxBCG CLUSTERS WITH WEAK LENSING AND X-RAY DATA

Rozo, Eduardo; Rykoff, E. S.; Evrard, A. E.; Becker, M. R.; McKay, Timothy A.; Wechsler, Risa H.; Koester, Benjamin P.; Hao, Jiangang; Hansen, S. M.; Sheldon, E.; Johnston, David; Annis, J.; Frieman, Joshua A.

doi:10.1088/0004-637x/699/1/768

Cited by 149 publications

(245 citation statements)

References 46 publications

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“…Removing the outlier discussed in Section 3.3.1 changes the correlation coefficient by < ∼ 0.02. The significant covariance between the scatter in Y2D and M2D we found is consistent with previous theoretical studies on covariance between cluster observables (White, Cohn & Smit 2010;Stanek et al 2010;Angulo et al 2012;Noh & Cohn 2012) and observational work (e.g., Rozo et al 2009). …”

Section: Covariance In the Y − M Relationsupporting

confidence: 91%

Covariance in the thermal SZ–weak lensing mass scaling relation of galaxy clusters

Shirasaki

Nagai

Lau

2016

Mon. Not. R. Astron. Soc.

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The thermal Sunyaev-Zel'dovich (tSZ) effect signal is widely recognized as a robust mass proxy of galaxy clusters with small intrinsic scatter. However, recent observational calibration of the tSZ scaling relation using weak lensing (WL) mass exhibits considerably larger scatter than the intrinsic scatter predicted from numerical simulations. This raises a question as to whether we can realize the full statistical power of ongoing and upcoming tSZ-WL observations of galaxy clusters. In this work, we investigate the origin of observed scatter in the tSZ-WL scaling relation, using mock maps of galaxy clusters extracted from cosmological hydrodynamic simulations. We show that the inferred intrinsic scatter from mock tSZ-WL analyses is considerably larger than the intrinsic scatter measured in simulations, and comparable to the scatter in the observed tSZ-WL relation. We show that this enhanced scatter originates from the combination of the projection of correlated structures along the line of sight and the uncertainty in the cluster radius associated with WL mass estimates, causing the amplitude of the scatter to depend on the covariance between tSZ and WL signals. We present a statistical model to recover the unbiased cluster scaling relation and cosmological parameter by taking into account the covariance in the tSZ-WL mass relation from multi-wavelength cluster surveys.

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Section: Covariance In the Y − M Relationsupporting

confidence: 91%

Covariance in the thermal SZ–weak lensing mass scaling relation of galaxy clusters

Shirasaki

Nagai

Lau

2016

Mon. Not. R. Astron. Soc.

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“…This is particularly crucial for cosmological purposes with galaxy cluster counts (e.g. Rozo et al 2009). We have measured the accuracy with which we can calibrate cluster and group masses with multiple medium-band photometry mimicking the ALHAMBRA data (section §4.1).…”

Section: Dark Matter Halo Mass -Optical Richness Calibrationmentioning

confidence: 99%

Galaxy clusters and groups in the ALHAMBRA survey

Ascaso

Benı́tez

Fernández-Soto

et al. 2015

Mon. Not. R. Astron. Soc.

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We present a catalogue of 348 galaxy clusters and groups with 0.2 < z < 1.2 selected in the 2.78 deg 2 ALHAMBRA Survey. The high precision of our photometric redshifts, close to 1%, and the wide spread of the seven ALHAMBRA pointings ensure that this catalogue has better mass sensitivity and is less affected by cosmic variance than comparable samples.The detection has been carried out with the Bayesian Cluster Finder (BCF), whose performance has been checked in ALHAMBRA-like light-cone mock catalogues. Great care has been taken to ensure that the observable properties of the mocks photometry accurately correspond to those of real catalogues. From our simulations, we expect to detect galaxy clusters and groups with both 70% completeness and purity down to dark matter halo masses of M h ∼ 3 × 10 13 M ⊙ for z < 0.85. Cluster redshifts are expected to be recovered with ∼ 0.6% precision for z < 1. We also expect to measure cluster masses with σ M h |M * CL ∼ 0.25 − 0.35 dex precision down to ∼ 3 × 10 13 M ⊙ , masses which are 50% smaller than those reached by similar work.We have compared these detections with previous optical, spectroscopic and Xrays work, finding an excellent agreement with the rates reported from the simulations. We have also explored the overall properties of these detections such as the presence of a colour-magnitude relation, the evolution of the photometric blue fraction and the clustering of these sources in the different ALHAMBRA fields. Despite the small numbers, we observe tentative evidence that, for a fixed stellar mass, the environment is playing a crucial role at lower redshifts (z<0.5).

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“…Another is the fact that numerous authors have studied the catalogue, providing extensive information on its properties. In particular, Sheldon et al (2009) and Mandelbaum et al (2008a) have published mass estimates from weak gravitational lensing analyses, which Johnston et al (2007) and Rozo et al (2009) use to construct mass-richness (M 500 −N 200 ) relations. We apply this relation, as outlined below, to adapt our SZ filter measurements for each individual cluster according to its given richness, N 200 , as well as in our model predictions.…”

Section: The Maxbcg Optical Cluster Cataloguementioning

confidence: 99%

“…In their discussion, Rozo et al (2009) identify the differences between the Sheldon et al (2009) and Mandelbaum et al (2008a) mass estimates and the impact on the deduced mass-richness relation. They trace the systematically higher mass estimates of Mandelbaum et al (2008a) to these authors' more detailed treatment of photometric redshift uncertainties (Mandelbaum et al 2008b).…”

Section: The Maxbcg Optical Cluster Cataloguementioning

confidence: 99%

“…For this initial study, we chose the MaxBCG catalogue for its large sample size, wide mass range and well-characterized selection function, and because its properties have been extensively studied. In particular, we benefit from weak-lensing mass measurements and mass-richness relations (Johnston et al 2007;Mandelbaum et al 2008a;Sheldon et al 2009;Rozo et al 2009). A combined SZ-optical study over such a large catalogue is unprecedented and Planck is a unique SZ instrument for this task, as its all-sky coverage encompasses the complete SDSS area and the full MaxBCG cluster sample.…”

Section: Introductionmentioning

confidence: 99%

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Planckearly results. XII. Cluster Sunyaev-Zeldovich optical scaling relations

Aghanim

Arnaud

Ashdown

et al. 2011

A&A

103

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We present the Sunyaev-Zeldovich (SZ) signal-to-richness scaling relation (Y 500 − N 200 ) for the MaxBCG cluster catalogue. Employing a multifrequency matched filter on the Planck sky maps, we measure the SZ signal for each cluster by adapting the filter according to weak-lensing calibrated mass-richness relations (N 200 − M 500 ). We bin our individual measurements and detect the SZ signal down to the lowest richness systems (N 200 = 10) with high significance, achieving a detection of the SZ signal in systems with mass as low as M 500 ≈ 5 × 10 13 M . The observed Y 500 − N 200 relation is well modeled by a power law over the full richness range. It has a lower normalisation at given N 200 than predicted based on X-ray models and published mass-richness relations. An X-ray subsample, however, does conform to the predicted scaling, and model predictions do reproduce the relation between our measured bin-average SZ signal and measured bin-average X-ray luminosities. At fixed richness, we find an intrinsic dispersion in the Y 500 − N 200 relation of 60% rising to of order 100% at low richness. Thanks to its all-sky coverage, Planck provides observations for more than 13 000 MaxBCG clusters and an unprecedented SZ/optical data set, extending the list of known cluster scaling laws to include SZ-optical properties. The data set offers essential clues for models of galaxy formation. Moreover, the lower normalisation of the SZ-mass relation implied by the observed SZ-richness scaling has important consequences for cluster physics and cosmological studies with SZ clusters.

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CONSTRAINING THE SCATTER IN THE MASS-RICHNESS RELATION OF maxBCG CLUSTERS WITH WEAK LENSING AND X-RAY DATA

Cited by 149 publications

References 46 publications

Covariance in the thermal SZ–weak lensing mass scaling relation of galaxy clusters

Covariance in the thermal SZ–weak lensing mass scaling relation of galaxy clusters

Galaxy clusters and groups in the ALHAMBRA survey

Planckearly results. XII. Cluster Sunyaev-Zeldovich optical scaling relations

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