A Wide-Field Hubble Space Telescope Study of the Cluster Cl 0024+1654 at z=0.4. II. The Cluster Mass Distribution

By Jean-Paul Kneib, P. Hudelot, Richard S. Ellis, T. Treu, Graham P. Smith, P. Marshall, O. Czoske, I. Smail, P. Natarajan. 2003

197 citations recorded by the source corpus.

We present a comprehensive lensing analysis of the rich cluster Cl 0024+1654 (z = 0.395) based on panoramic sparse-sampled imaging conducted with the WFPC2 and STIS cameras on board the Hubble Space Telescope. By comparing higher fidelity signals in the limited STIS data with the wider field data available from WFPC2, we demonstrate an ability to detect reliably weak-lensing signals to a cluster radius of ≃5 h Mpc, where the mean shear is around 1%. This enables us to study the distribution of dark matter with respect to the cluster light over an unprecedented range of cluster radii and environments. The projected mass distribution reveals a secondary concentration representing 30% of the overall cluster mass, which is also visible in the distribution of cluster member galaxies. We develop a method to derive the projected mass profile of the main cluster taking into account the influence of the secondary clump. We normalize the mass profile determined from the shear by assuming that background galaxies selected with 23 < I < 26 have a redshift distribution statistically similar to that inferred photometrically in the Hubble Deep Fields. The total mass within the central region of the cluster is independently determined from strong-lensing constraints according to a detailed model that utilizes the multiply imaged arc at z = 1.675. Combining strong and weak constraints, we are able to probe the mass profile of the cluster on scales of 0.1-5 Mpc, thus providing a valuable test of the universal form proposed by Navarro, Frenk, & White (NFW) on large scales. A generalized power-law fit indicates an asymptotic three-dimensional density distribution of ρ ∝ r-n with n > 2.4. An isothermal mass profile is therefore strongly rejected, whereas an NFW profile with M200 = 6.1 × 1014 h M☉ provides a good fit to the lensing data. We isolate cluster members according to their optical/near-infrared colors; the red cluster light closely traces the dark matter with a mean mass-to-light ratio of M/LK = 40 ± 5 h65 M☉/L☉. Similar profiles for mass and light on 1-5 Mpc scales are expected if cluster assembly is largely governed by infalling groups.

Subfields: Astronomy and Astrophysics, Biophysics, Ecology

View Paper: https://www.semanticscholar.org/paper/b94c8415a73751b9100f30b1a9d6d389a6ed7bec

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Citations in the corpus

Characterizing the Cluster Lens Population (2005, background): “The anomalously high concentrations c > 14 recently reported by several groups (Kneib et al. 2003; Gavazzi et al. 2003; Broadhurst et al. 2005b) appear inconsistent with the concentration distribution in our simulations, which predict that < 2% of lensing clusters should have concentrations this…”
The Dark Matter Distribution in the Central Regions of Galaxy Clusters: Implications for Cold Dark Matter (2003, background): “Much larger values of rsc seem to be ruled out on observational grounds as well (Gavazzi et al. 2003; Kneib et al. 2003; Wu & Xue 2000).”
Combining Lens Distortion and Depletion to Map the Mass Distribution of A1689 (2007, background): “Such a high concentration is also seen in other massive clusters from careful lensing work, such as MS 2137-23 (c200 ≃ 12, Gavazzi et al. 2003) and CL0024+1654 (c200 ≃ 22, Kneib et al. 2003).”
Combining Strong and Weak Gravitational Lensing in Abell 1689 (2006, result): “A similar trendwas also observed inCl 0024 (Kneib et al. 2003).”
A Bayesian approach to strong lensing modelling of galaxy clusters (2007, background): “Observations are not yet giving definitive answers relative to the value of the inner slope (Gavazzi et al. 2003; Sand et al. 2004, 2007) or the concentration (Kneib et al. 2003; Gavazzi et al. 2003), but progress is being made steadily.”
The CFHTLS strong lensing legacy survey - I. Survey overview and T0002 release sample (2006, methodology): “The observation of gravitational lensing effects produced by mass concentrations is a powerful tool to directly probe dark matter haloes and their interplay with visible mass (Schneider et al. 1992; Blandford & Narayan 1992; Miralda-Escude & Lehar 1992; Mellier 2002; Kneib et al. 2003).”
New Multiply-Lensed Galaxies Identified in ACS/NIC3 Observations of Cl0024+1654, Using an Improved Mass Model (2009, methodology): “A significant substructure is found in the WL maps at a radius of about 3.5′ from the cluster centre, in good agreement with the location of a secondary sub-structure found by Kneib et al. (2003), based on independent mosaic HST imaging.”
LoCuSS: Subaru Weak Lensing Study of 30 Galaxy Clusters (2009, methodology): “…none of our morphologically unbiased X-ray selected sample of clusters, including those with the highest masses (& 1015 Mˇ), show very high concentrations of cvir & 10 as have been found for some strong lensing clusters (e.g., Gavazzi et al. 2003; Kneib et al. 2003; Broadhurst et al. 2005, 2008).”
A Wide-Field Survey of Two z ~ 0.5 Galaxy Clusters: Identifying the Physical Processes Responsible for the Observed Transformation of Spirals into S0s (2007, background): “The large structure to the NW is also detected in both the weak lensing map (Kneib et al. 2003, hereafter, Paper II) andXMM/Newtonobservations (Zhang et al. 2005), which additionally suggestthe presence of a shock front at the interface between the group and the main cluster.”
THE DENSITY PROFILES OF MASSIVE, RELAXED GALAXY CLUSTERS. I. THE TOTAL DENSITY OVER THREE DECADES IN RADIUS (2012, background): “X-ray and lensing studies have shown that NFW profiles can generally provide adequate descriptions of cluster halos at radii r & 50 kpc (e.g., Kneib et al. 2003; Broadhurst et al. 2005; Mandelbaum et al. 2006; Schmidt & Allen 2007; Okabe et al. 2010; Umetsu et al. 2011; Coe et al. 2012; Morandi &…”
The observed concentration–mass relation for galaxy clusters (2007, background): “For example, Kneib et al. (2003) identify a main clump with high concentration as well as a secondary, low concentration clump, while this paper (Table 1) fits threecvir ∼ 5 clumps to ZwCl 0024+1652.”
Lensing is Low: Cosmology, Galaxy Formation, or New Physics? (2016, methodology): “A boost correction factor is sometimes applied in order to account for the dilution of the signal by physically associated sources (e.g. Kneib et al. 2003; Hirata et al. 2004; Sheldon et al. 2004; Mandelbaum et al. 2006b).”
Discovery of a Ringlike Dark Matter Structure in the Core of the Galaxy Cluster Cl 0024+17 (2007, methodology): “Kneib et al. (2003) presented a reduced shear profile of Cl 0024+17 at 5000 < r < 100000 based on two passband (F450W and F814W) WFPC2 observations.”
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): “…of clusters (e.g. Carlberg et al. 1997a; Geller et al. 1999; van der Marel et al. 2000; King et al. 2002; Biviano & Girardi 2003; Rines et al. 2003a; Kneib et al. 2003; Katgert et al. 2004; Arnaud et al. 2005; Broadhurst et al. 2005; Umetsu et al. 2011; Oguri et al. 2012; Okabe et al. 2013).”
Gravitational lensing (2010, unknown): “Similarly, it is found in [255] in a combined weakand strong-lensing analysis of Cl 0024+1654 that an isothermal mass profile can be rejected, while the NFW profile fits the data well.”
LoCuSS: first results from strong-lensing analysis of 20 massive galaxy clusters at z= 0.2 (2009, methodology): “The identification of background galaxies forming strong lensing arcs in cluster cores is a direct measurement of the enclosed mass within the Einstein radius θE , providing an accurate normalisation of cluster mass models both in the core, and extending to larger radii (e.g. Kneib et al. 2003).”
LoCuSS: comparison of observed X-ray and lensing galaxy cluster scaling relations with simulations (2008, methodology): “However, for some clusters, especially merging clusters, a NFW model is not favored statistically, and the SIS model has only been ruled out at large significance in a small number of cases (e.g. Kneib et al. 2003).”