Characterizing the Cluster Lens Population

By J. Hennawi, N. Dalal, Paul Bode, Jeremiah P. Ostriker. 2005

154 citations recorded by the source corpus.

We present a detailed investigation into which properties of CDM halos make them effective strong gravitational lenses. Strong-lensing cross sections of 878 clusters from an N-body simulation are measured by ray-tracing through 13,594 unique projections. We measure concentrations, axis ratios, orientations, and the substructure of each cluster, and compare the lensing-weighted distribution of each quantity to that of the cluster population as a whole. The concentrations of lensing clusters are on average 34% larger than the typical cluster in the universe. Despite this bias, the anomalously high concentrations (c > 14) recently measured by several groups appear to be inconsistent with the concentration distribution in our simulations, which predict that <2% of lensing clusters should have concentrations this high. No correlation is found between lensing cross section and substructure. We introduce several types of simplified dark matter halos and use them to isolate which properties of CDM clusters make them effective lenses. The abundance of giant arcs is primarily determined by the mass distribution within an average overdensity of ~10,000. A multiple-lens-plane ray-tracing algorithm is used to show that projections of large-scale structure increase the giant arc abundance modestly, by <7%. We revisit the claimed excess of giant arcs behind high redshift clusters in the RCS survey and find that the number of high-redshift (z > 0.6) lenses is in good agreement with ΛCDM, although our simulations predict more low-redshift (z < 0.6) lenses than observed.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/38f2651808899898e9651670d1857b32ca7b321b

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Citations in the corpus

DETECTION OF LENSING SUBSTRUCTURE USING ALMA OBSERVATIONS OF THE DUSTY GALAXY SDP.81 (2016, background): “Also note that our assumption of spherical symmetry might lead us to underestimate the average substructure abundance around lenses, since strong lenses are preferentially viewed along the major axis of their host halos (Rozo et al. 2007; Hennawi et al. 2007).”
New Multiply-Lensed Galaxies Identified in ACS/NIC3 Observations of Cl0024+1654, Using an Improved Mass Model (2009, result): “This value is significantly larger than theoretically expected (cvir ' 5) for the standard ΛCDM model (Bullock et al. 2001, Neto et al. 2007, Duffy et al. 2008), even after accounting for expected projection bias (Oguri et al. 2005, Hennawi et al. 2007, Corless, King & Clowe 2008).”
The flattening of the concentration–mass relation towards low halo masses and its implications for the annihilation signal boost (2013, background): “Most of the existing c(M) median relations proposed in the literature were derived from well resolved simulations in the halo mass range from 1010 – 1015h−1M⊙, e.g., B01, Hennawi et al. (2007); Neto et al. (2007); Duffy et al. (2008), M08, Muñoz-Cuartas et al. (2011), P12.”
The observed concentration–mass relation for galaxy clusters (2007, background): “Hennawi et al. (2007) identified lensing clusters from their simulated sample by using ray trcing to compute strong lensing cross sections for each cluster, andfound that the simulated strong lensing clusters have on average 34% higher concentrations than the total simulated cluster population.”
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).”
CLASH: JOINT ANALYSIS OF STRONG-LENSING, WEAK-LENSING SHEAR, AND MAGNIFICATION DATA FOR 20 GALAXY CLUSTERS (2015, background): “A population of such superlenses might also be biased toward halos with intrinsically higher concentrations (Hennawi et al. 2007).”
LoCuSS: Subaru Weak Lensing Study of 30 Galaxy Clusters (2009, background): “Specifically, strong lensing clusters are likely to be biased towards clusters with high concentrations and/or a significantly non-spherical mass distributions (e.g., Oguri et al. 2005; Hennawi et al. 2007; Corless et al. 2009).”
Formation of Galaxy Clusters (2012, background): “Accounting for such triaxiality is particularly importantin theoretical predictions and observational analyses of weak and strong lensing (Becker & Kravtsov 2011; Clowe, De Lucia & King 2004; Corless & King 2007; Dalal & Keeton 2003; Hennawi et al. 2007; Oguri et al. 2005).”
Gravitational lensing (2010, background): “It is a puzzling and potentially highly important problem that strong-lensing analyses of galaxy clusters in many cases find that NFW density profiles well reproduce the observed image configurations, but with concentration parameters that are substantially larger than expected from numerical simula”
SIMULATION OF THE COSMIC EVOLUTION OF ATOMIC AND MOLECULAR HYDROGEN IN GALAXIES (2009, methodology): “Here we shall use the result of Hennawi et al. (2007), chalo = 12.3 1 + z ( Mvir 1.3 · 1013 h−1M⊙ )−0.13 , (33) which is consistent with recent empirical values of the matter concentration in galaxy clusters derived from X-ray measurements and strong lensing data (Comerford & Natarajan 2007).”
Combining Lens Distortion and Depletion to Map the Mass Distribution of A1689 (2007, methodology): “…part of this discrepancy from lensing observations could be reconciled by observational effects such as triaxiality of CDM halos (Oguri et al. 2005; Hennawi et al. 2007; Sereno 2007; Corless & King 2007), and the projection of structure along the line of sight (e.g., King & Corless 2007), both of…”
THE DENSITY PROFILES OF MASSIVE, RELAXED GALAXY CLUSTERS. I. THE TOTAL DENSITY OVER THREE DECADES IN RADIUS (2012, background): “Interpreting this requires careful study of possible measurement biases or selection effects (Hennawi et al. 2007; Meneghetti et al. 2010a).”
THE CLUSTER LENSING AND SUPERNOVA SURVEY WITH HUBBLE: AN OVERVIEW (2011, background): “…they are not preferentially aligned along the line of sight, in contrast with a purely lensing-selected sample, where the surface mass density is, on average, biased upwards along the line of sight by intrinsic triaxiality (Hennawi et al. 2007; Oguri et al. 2009; Meneghetti et al. 2010a, 2011).”
Characterization of subhalo structural properties and implications for dark matter annihilation signals (2016, background): “…studied in the past and several concentration-mass relations, c(M), have been proposed in the literature (see, e.g., Bullock et al. (2001); Hennawi et al. (2007); Neto et al. (2007); Duffy et al. (2008); Macciò et al. (2008); Muñoz Cuartas et al. (2011); Prada et al. (2012); Ludlow et…”
Strong-lensing optical depths in a ΛCDM universe – II. The influence of the stellar mass in galaxies (2007, background): “Hennawi et al. (2007) estimated the number of expected number of quasars with very large image separations in similar samples.”
Combined strong and weak lensing analysis of 28 clusters from the Sloan Giant Arcs Survey (2011, methodology): “We note that the mean mass measured by the stacking analysis agrees well with the mean mass of strong lens selected clusters predicted by ray-tracing simulations, 〈Mvir〉 ∼ 4.2×1014h−1M⊙ (Hennawi et al. 2007, see also Bayliss et al. 2011b).”
Dark matter halo concentrations in the Wilkinson Microwave Anisotropy Probe year 5 cosmology (2008, result): “…test this hypothesis and generally confirm the anti-correlation between c and M (e.g. Buote et al. 2007; Schmidt & Allen 2007), although the concentrations inferred from strong gravitational lensing may exceed those predicted by the simulations (e.g. Hennawi et al. 2007; Broadhurst & Barkana 2008).”