LoCuSS: Subaru Weak Lensing Study of 30 Galaxy Clusters

By N. Okabe, M. Takada, Keiichi Umetsu, Toshifumi Futamase, U. GrahamP.SmithTohoku, Ipmu, Asiaa, Birmingham. 2009

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(Abridged) We use Subaru data to conduct a detailed weak-lensing study of the dark matter distribution in a sample of 30 X-ray luminous galaxy clusters at 0.15<z<0.3. A weak-lensing signal is detected at high statistical significance in each cluster, the total detection S/N ranging from 5 to 13. In this paper we concentrate on fitting spherical models to the tangential distortion profiles of the clusters. When the models are fitted to the clusters individually, we are unable to discriminate statistically between SIS and NFW models. However when the tangential distortion profiles of the individual clusters are combined, and models fitted to the stacked profile, the SIS model is rejected at 6- and 11-sigma, respectively, for low- and high-mass bins. We also use the individual cluster NFW model fits to investigate the relationship between cluster mass (M_vir) and concentration (c_vir), finding an anti-correlation of c_vir and M_vir. The best-fit c_vir-M_vir relation is: c_vir(M_vir) propto M_vir^{-alpha} with alpha=0.41+/-0.19 -- i.e. a non-zero slope is detected at 2sigma significance. We then investigate the optimal radius within which to measure cluster mass, finding that the typical fractional errors are improved to sigma(M_Delta)/M_Delta ~ 0.1-0.2 for cluster masses at higher over-densities Delta=500-2000, from 0.2-0.3 for the virial over-density (~110). Further comparisons between mass measurements based on spherical model fitting and the model-independent aperture mass method reveal that the 2D aperture mass enclosed within a cylinder of a given aperture radius is systematically greater than the 3D spherical mass obtained from NFW model fitting: M_2D/M_3D= 1.34 and 1.40 for Delta=500 and 110, respectively. The amplitude of this effect agrees well with that predicted by integrating the NFW model along the line-of-sight.

Subfields: Astronomy and Astrophysics, Instrumentation, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/53cd441674f884b3a9f04deed8585edeb576c609

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Citations in the corpus

Weighing the giants – IV. Cosmology and neutrino mass (2014, background): “Note also that the full Planck data set (including polarization) should be significantly more powerful than the 28 The size of the lensing sample could be straightforwardly increased (approximately doubled) by incorporating data already present in the archives of SuprimeCam and MegaPrime/MegaCam, su”
Masses of Galaxy Clusters from Gravitational Lensing (2013, methodology): “Hence, by only picking galaxies redder than, and clearly separated from, the red sequence, a robust selection of background galaxies with negligible contamination can be performed (e.g., Okabe et al. 2010).”
CLASH: THE ENHANCED LENSING EFFICIENCY OF THE HIGHLY ELONGATED MERGING CLUSTER MACS J0416.1−2403 (2012, background): “…al. 2008; Broadhurst & Barkana 2008), is often attributed to a lensing selection bias towards higher concentrations of triaxial clusters preferentially aligned with the line of sight (see also Hennawi et al. 2007; Sereno et al. 2010; Oguri et al. 2012a; Okabe et al. 2010, and references therein).”
Combined strong and weak lensing analysis of 28 clusters from the Sloan Giant Arcs Survey (2011, methodology): “Detailed lensing measurements of massive clusters have confirmed this prediction by and large, although there does appear to be some cluster-to-cluster variations (e.g., Okabe et al. 2010; Umetsu et al. 2011b).”
Detailed cluster lensing profiles at large radii and the impact on cluster weak lensing studies (2011, background): “…massive clusters, we can detect weak lensing signals out to virial radii, which allows direct measurements of virial masses (e.g., Dahle 2006; Broadhurst et al. 2008; Mahdavi et al. 2008; Okabe & Umetsu 2008; Oguri et al. 2009; Umetsu et al. 2009, 2011; Medezinski et al. 2010; Okabe et al. 2010).”
ON THE ACCURACY OF WEAK-LENSING CLUSTER MASS RECONSTRUCTIONS (2010, methodology): “Future samples of clusters which will be much larger than the 12 clusters used by Okabe et al. (2010b) will test our conclusions and predictions in detail.”
LoCuSS: THE SLOW QUENCHING OF STAR FORMATION IN CLUSTER GALAXIES AND THE NEED FOR PRE-PROCESSING (2015, background): “The first 30 clusters from our survey benefit from a particularly rich dataset, including: Subaru/Suprime-Cam optical imaging (Okabe et al. 2010), Spitzer /MIPS 24 μm maps, Herschel/PACS+SPIRE 100–500 μm maps, Chandra and/or XMM X-ray data, GALEX UV data, and near-infrared (NIR) imaging.”
The Canadian Cluster Comparison Project: detailed study of systematics and updated weak lensing masses (2015, background): “Results for 30 clusters, of which 13 overlap with CCCP are presented in Okabe et al. (2010).”
CLASH: WEAK-LENSING SHEAR-AND-MAGNIFICATION ANALYSIS OF 20 GALAXY CLUSTERS (2014, methodology): “Here α 2 g is the softening constant variance, taken to be αg = 0.4 (e.g., Umetsu & Broadhurst 2008; Umetsu et al. 2009, 2012; Okabe et al. 2010).”
Weighing the Giants – III. Methods and measurements of accurate galaxy cluster weak-lensing masses (2012, methodology): “We also note that Okabe et al. (2010) fit for the concentration, rather than assuming a specific value of mass-concentration relation.”
Galaxy Alignments: Observations and Impact on Cosmology (2015, background): “As an example, tangential shear is important in determining the masses of galaxy clusters (Okabe et al. 2010; Applegate et al. 2014; Hoekstra et al. 2015), where ensemble-averaged tangential shear as a function of cluster-centric radius can be related to the projected mass, or fit by a parametric…”
Robust weak-lensing mass calibration of Planck galaxy clusters (2014, background): “With current samples of 30–50 clusters (Okabe et al. 2010; Hoekstra et al. 2012, WtG), the statistical precision achievable is already, in principle, better than 10 per cent, requiring a detailed understanding of the systematic uncertainties involved.”
CLASH-VLT: The mass, velocity-anisotropy, and pseudo-phase-space density profiles of the z = 0.44 galaxy cluster MACS J1206.2-0847 (2013, background): “…between the observedcMr (e.g. Łokas et al. 2006b; Rines & Diaferio 2006; Buote et al. 2007; Schmidt & Allen 2007; Biviano 2008; Ettori et al. 2010; Okabe et al. 2010; Oguri et al. 2012; Newman et al. 2012) and that obtained inΛCDM cosmological simulations (e.g. Navarro et al. 1997; Bullock et…”
Creation of cosmic structure in the complex galaxy cluster merger Abell 2744 (2011, unknown): “4-1222) (Bradač et al. 2008), the Cosmic Train Wreck (Abell 520) (Mahdavi et al. 2007; Okabe & Umetsu 2008), Abell 2146 (Russell et al. 2010), Abell 521 (Giacintucci et al. 2008; Okabe et al. 2010a) and Abell 3667 (Finoguenov et al. 2010).”
The Atacama Cosmology Telescope: Sunyaev-Zel'dovich selected galaxy clusters at 148 GHz from three seasons of data (2013, methodology): “X-ray data are obtained from the XMM-Newton archive, and weak lensing masses for the clusters we consider here originate in [82].”
The Phoenix Project: the dark side of rich galaxy clusters (2012, result): “Outside the very centre, the cluster mass profile can be measured through weaklensing (see, e.g., Okabe et al. 2010; Oguri et al. 2011; Umetsu etal.”
Lensing and x-ray mass estimates of clusters (simulations) (2012, background): “…common and easy alternative to measure the mass (e.g. Clowe & Schneider 2002; Hoekstra et al. 2000; Jee et al. 2005; Dahle 2006; Paulin-Henriksson et al. 2007; Bardeau et al. 2007; Oguri et al. 2009; Kubo et al. 2007; Okabe et al. 2010; Romano et al. 2010; Umetsu et al. 2011; Zitrin et al. 2011).”
MEASURING THE ULTIMATE HALO MASS OF GALAXY CLUSTERS: REDSHIFTS AND MASS PROFILES FROM THE HECTOSPEC CLUSTER SURVEY (HeCS) (2012, background): “Note that the weak lensing map of Okabe et al. (2010a) shows two distinct mass components centered approximately on MS0906 (component A750-C in their Figure 32) and A750 (component A750-NW1 in their Figure 32); MS0906 has larger surface mass density and A750 has a larger luminosity density of…”