Combining Strong and Weak Gravitational Lensing in Abell 1689

By M. Limousin, J. Richard, E. Jullo, Jean-Paul Kneib, B. Fort, G. Soucail, Á. Elı́asdóttir, P. Natarajan, Richard S. Ellis, I. Smail and 7 more. 2006

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We present a reconstruction of the mass distribution of galaxy cluster Abell 1689 at z = 0.18 using detected strong lensing features from deep ACS observations and extensive ground based spectroscopy. Earlier analyses have reported up to 32 multiply imaged systems in this cluster, of which only 3 were spectroscopically confirmed. In this work, we present a parametric strong lensing mass reconstruction using 34 multiply imaged systems of which 24 have newly determined spectroscopic redshifts, which is a major step forward in building a robust mass model. In turn, the new spectroscopic data allows a more secure identification of multiply imaged systems. The resultant mass model enables us to reliably predict the redshifts of additional multiply imaged systems for which no spectra are currently available, and to use the location of these systems to further constrain the mass model. Using our strong lensing mass model, we predict on larger scale a shear signal which is consistent with that inferred from our large scale weak lensing analysis derived using CFH12K wide field images. Thanks to a new method for reliably selecting a well defined background lensed galaxy population, we resolve the discrepancy found between the NFW concentration parameters derived from earlier strong and weak lensing analysis. The derived parameters for the best fit NFW profile is found to be c200 = 7.6 ± 1.6 and r200 = 2.16 ± 0.10 h Mpc (corresponding to a 3D mass equal to M200 = [1.32 ± 0.2] × 1015 h70 M☉). The large number of new constraints incorporated in this work makes Abell 1689 the most reliably reconstructed cluster to date. This well calibrated mass model, which we here make publicly available, will enable us to exploit Abell 1689 efficiently as a gravitational telescope, as well as to potentially constrain cosmology.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/ff59a5e598397084e6b303277712842ad451a2b4

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Citations in the corpus

THE CLUSTER LENSING AND SUPERNOVA SURVEY WITH HUBBLE: AN OVERVIEW (2011, methodology): “As part of a Guaranteed Time Observation (GTO) program, deep (20-orbit) multiband (4-6 filter) observations were obtained for five galaxy clusters: Abell 1689 (Broadhurst et al. 2005; Limousin et al. 2007; Coe et al. ar X iv :1 10 6.”
Mass and magnification maps for the Hubble Space Telescope Frontier Fields clusters: implications for high-redshift studies (2014, methodology): “Following our successful strategy from previous lensing work (e.g. Limousin et al. 2007, 2012; Richard et al. 2010a,b), we adopt a parametric model combining both large-scale (cluster or group size) mass clumps as well as galaxy-scale mass clumps.”
HUBBLE SPACE TELESCOPE COMBINED STRONG AND WEAK LENSING ANALYSIS OF THE CLASH SAMPLE: MASS AND MAGNIFICATION MODELS AND SYSTEMATIC UNCERTAINTIES (2014, background): “Various studies have previously combined SL+WL (e.g., Bradač et al. 2006; Limousin et al. 2007; Merten et al. 2009, 2011; Umetsu et al. 2011a, 2011b, 2012; Oguri et al. 2012; Newman et al. 2013a, 2013b).”
RESIDUAL GAS MOTIONS IN THE INTRACLUSTER MEDIUM AND BIAS IN HYDROSTATIC MEASUREMENTS OF MASS PROFILES OF CLUSTERS (2009, background): “…(Smith et al. 2005), weak lensing (e.g., Dahle 2006; Mahdavi et al. 2008; Zhang et al. 2008), combined strong and weak lensing (Bradač et al. 2006; Limousin et al. 2007; Oguri et al. 2009), and Sunyaev-Zel’dovich effect (e.g., Carlstrom et al. 2002, for a recent review) have become available.”
LoCuSS: Subaru Weak Lensing Study of 30 Galaxy Clusters (2009, background): “…distribution of cluster concentrations with the high-concentration results obtained for several well-known strong lensing clusters, notably A 1689, Cl 0024, and MS 2137 (Gavazzi et al. 2003; Kneib et al. 2003; Broadhurst et al. 2005; Limousin et al. 2007; Broadhurst et al. 2008; Oguri et al. 2009).”
A Bayesian approach to strong lensing modelling of galaxy clusters (2007, methodology): “…disagreement over its concentration (Clowe and Schneider 2001; King et al. 2002; Bardeau et al. 2005; Broadhurst et al. 2005; Halkola et al. 2006), Limousin et al. (2007) came to a consensus value of cvir ∼ 6− 8 after careful and detailed modelling of the previously-analysed data combined with…”
THE DENSITY PROFILES OF MASSIVE, RELAXED GALAXY CLUSTERS. I. THE TOTAL DENSITY OVER THREE DECADES IN RADIUS (2012, methodology): “′′3, with a scatter of up to ∼ 3′′ in the best-studied clusters (e.g., Limousin et al. 2007).”
LENS MODELS AND MAGNIFICATION MAPS OF THE SIX HUBBLE FRONTIER FIELDS CLUSTERS (2014, unknown): “′′3 (following Jullo et al. 2007; Limousin et al. 2007).14 Moreover, identifying features by eye works better than automated measurement in scenarios where im- 14 We also ran an identical set of models using a positional error ages are close to the critical curves and the magnification gradient…”
Multiscale cluster lens mass mapping - I. Strong lensing modelling (2009, methodology): “However, in place of an NFW mass distribution, we build the grid from a more realistic input mass map based on a simplified version of the mass model of the galaxy cluster Abell 1689 reported in Limousin et al. (2007).”
LoCuSS: comparison of observed X-ray and lensing galaxy cluster scaling relations with simulations (2008, methodology): “…10 clusters from CFH12k data (Bardeau et al. 2005, 2007); 15 clusters from observations at the Nordic Optical Telescope and UH 88in (Dahle 2006); one cluster, Abell 1689, has also been studied using both CFHT and Subaru data (Limousin et al. 2007; Halkola et al. 2006; Broadhurst et al. 2005).”
The Frontier Fields lens modelling comparison project (2016, methodology): “The image-plane root mean squared (RMSi) distance of the images predicted by the model were used to compare with the observed positions as an accuracy estimator of the model (Limousin et al. 2007).”
Combining Lens Distortion and Depletion to Map the Mass Distribution of A1689 (2007, methodology): “In contrast, an Einstein radius of 24 ± 11 arcsec at zs = 1 is implied by the NFW fit to this cluster by Limousin et al. (2007), to independent weak lensing data from CFHT (cvir ∼ 9.6, Mvir ∼ 1.5×1015M⊙; see Table 5, Figures 15 and 16).”
Metallicity evolution, metallicity gradients, and gas fractions at z ~ 3.4 (2013, methodology): “Four of these are lensed by the cluster Abell 1689, and their magnification factor has been obtained by constructing a lens model of the cluster by using the 34 multiply images systems published in Limousin et al. (2007) .”
UV CONTINUUM SLOPE AND DUST OBSCURATION FROM z ∼ 6 TO z ∼ 2: THE STAR FORMATION RATE DENSITY AT HIGH REDSHIFT (2009, methodology): “For Abell 2218, MS1358, CL0024 (sometimes known as CL0024+1652), Abell 1689, and Abell 1703, we adopt the models constructed by Eĺıasdóttir et al. (2007), Franx et al. (1997), Jee et al. (2007), Limousin et al. (2007), and Limousin et al. (2008), respectively.”
LoCuSS: first results from strong-lensing analysis of 20 massive galaxy clusters at z= 0.2 (2009, methodology): “We note that other galaxy-galaxy weak-lensing works have obtained different values for r∗cut, but within the range 10 < r⋆cut < 100kpc (Natarajan et al. 2002; Limousin et al. 2007a; Halkola et al. 2007).”
Ultraviolet emission lines in young low-mass galaxies at z ≃ 2: physical properties and implications for studies at z > 7 (2014, background): “…lensed galaxies that are now being discovered with deep imaging and grism spectroscopy from theHubble Space Telescope (e.g., Richard et al. 2007, Limousin et al. 2007, Bradley et al. 2013, Schmidt et al. 2014, Atek et al. 2014a, Coe et al. 2014), it is becoming feasible to explore the…”
Revealing the Properties of Dark Matter in the Merging Cluster MACS J0025.4–1222 (2008, background): “…weak lensing data can provide a second effective redshift plane, allowing us to tightly constrain the mass, at least around the NW peak; in practice, however, the weak lensing data are too noisy to completely break the mass-sheet degeneracy (see e.g. Bradač et al. 2004b; Limousin et al. 2007).”
Weighing simulated galaxy clusters using lensing and X-ray (2009, methodology): “…profile: ρPIEMD(r) = ρ0 (1 + r2/r2core)(1 + r2/r2cut) · (12) We chose the PIEMD model because this is widely used for modeling the lensing properties of cluster galaxies in observations (see e.g. Limousin et al. 2007; Riemer-Sørensen et al. 2009; Donnarumma et al. 2009, for some recent references).”