Strong-Lensing Analysis of A1689 from Deep Advanced Camera Images

By T. Broadhurst, N. Benı́tez, D. Coe, K. Sharon, K. Zekser, R. White, H. C. Ford, R. Bouwens, J. Blakeslee, M. Clampin and 32 more. 2004

288 citations recorded by the source corpus.

We analyze deep multicolor Advanced Camera images of the largest known gravitational lens, A1689. Radial and tangential arcs delineate the critical curves in unprecedented detail, and many small counterimages are found near the center of mass. We construct a flexible light deflection field to predict the appearance and positions of counterimages. The model is refined as new counterimages are identified and incorporated to improve the model, yielding a total of 106 images of 30 multiply lensed background galaxies, spanning a wide redshift range, 1.0 < z < 5.5. The resulting mass map is more circular in projection than the clumpy distribution of cluster galaxies, and the light is more concentrated than the mass within r < 50 kpc h-1. The projected mass profile flattens steadily toward the center with a shallow mean slope of d log Σ/d log r ≃ -0.55 ± 0.1, over the observed range r < 250 kpc h-1, matching well an NFW profile, but with a relatively high concentration, Cvir = 8.2. A softened isothermal profile (rcore = 20 ± 2'') is not conclusively excluded, illustrating that lensing constrains only projected quantities. Regarding cosmology, we clearly detect the purely geometric increase of bend angles with redshift. The dependence on the cosmological parameters is weak owing to the proximity of A1689, z = 0.18, constraining the locus, ΩM + ΩΛ ≤ 1.2. This consistency with standard cosmology provides independent support for our model, because the redshift information is not required to derive an accurate mass map. Similarly, the relative fluxes of the multiple images are reproduced well by our best-fitting lens model.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/8420b977a8fa87f2213274670c28d9d936e36641

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Citations in the corpus

Multiscale cluster lens mass mapping - I. Strong lensing modelling (2009, background): “In Abell 1689, Limousin et al. (2007) obtain an RMS of 2.87” for 34 systems of multiple images, Halkola et al. (2006) report an RMS of 2.7” and Broadhurst et al. (2005) an RMS of 3.2”.”
The Frontier Fields lens modelling comparison project (2016, methodology): “The Zitrin light-traces-mass (LTM) method (Zitrin et al. 2009; Broadhurst et al. 2005), was designed primarily to be a very simple, straightforward modeling method with a MNRAS 000, 1–??”
HUBBLE SPACE TELESCOPE COMBINED STRONG AND WEAK LENSING ANALYSIS OF THE CLASH SAMPLE: MASS AND MAGNIFICATION MODELS AND SYSTEMATIC UNCERTAINTIES (2014, methodology): “…galaxies are also multiply imaged, allowing for high-resolution constraints to be placed on the mass distribution and profile (Kneib et al. 2004; Broadhurst et al. 2005; Smith et al. 2005; Limousin et al. 2008; Newman et al. 2009; Richard et al. 2010, 2014; Bradač et al. 2008; Liesenborgs et…”
Combining Strong and Weak Gravitational Lensing in Abell 1689 (2006, methodology): “Broadhurst et al. (2005a) found a higher concentration, cvir 13 (corresponding to c200 ¼ 10:8),when fitting simultaneously both strong- andweaklensing data points.”
New Multiply-Lensed Galaxies Identified in ACS/NIC3 Observations of Cl0024+1654, Using an Improved Mass Model (2009, methodology): “This approach is similar to that of Broadhurst et al. (2005a), which was successfully used to identify over 30 sets of multiple images in similarly deep ACS/GTO imaging of A1689, and also for the more distant cluster SDSS1004+4112 which was discovered to have 4 bright lensed QSO images (Oguri et…”
The observed concentration–mass relation for galaxy clusters (2007, unknown): “+1 −1 Broadhurst et al. (2005) WL 30.4 37.4 Halkola et al. (2006) WL 22.1+2.9−4.7 27.2 +3.5 −5.7 Medezinski et al. (2006) WL 3.5+0.5−0.3 14.1 +6.3 −4.7 4.5 +0.6 −0.4 17.1 +7.8 −5.8 Bardeau et al. (2005) WL 11.0+1.14−0.90 17.3 ± 1.7 13.7+1.4−1.1 19.3 ± 2.0 Broadhurst et al. (2005) WL 7.9 9.9 Clowe…”
The CFHTLS strong lensing legacy survey - I. Survey overview and T0002 release sample (2006, background): “They are known to occur around massive clusters (>1014 h−1 M ) and show radii up to ∼40′′ in very luminous X-ray clusters (see for example the spectacular case of A 1689 Broadhurst et al. 2005).”
Combining Lens Distortion and Depletion to Map the Mass Distribution of A1689 (2007, background): “This is based on the fact that the enclosed mass interior to the Einstein radius is given by fundamental constants and with knowledge of distances involved, namely κ̄(θE) = 1 or M(< θE) = π(DdθE) 2Σcrit, provided that the critical curve is nearly circular; this is the case for A1689 (B05b).”
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).”
Mass and magnification maps for the Hubble Space Telescope Frontier Fields clusters: implications for high-redshift studies (2014, background): “…(HST) for such studies is exemplified by the identification of 42 multiple-image systems in Advanced Camera for Surveys (ACS) observations of the massive cluster Abell 1689 (Broadhurst et al. 2005), 24 of them with measured redshifts from deep Keck and VLT spectroscopy (Limousin et al. 2007).”
LoCuSS: first results from strong-lensing analysis of 20 massive galaxy clusters at z= 0.2 (2009, background): “More recent strong lensing studies of cluster mass distributions have generally continued to concentrate on detailed studies of spectacular individual strong lensing clusters based on deep multi-filter HST observations (e.g. Broadhurst et al. 2005; Limousin et al. 2007b; Richard et al. 2009).”
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”
A Bayesian approach to strong lensing modelling of galaxy clusters (2007, background): “For example, in Abell 1689, after much 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…”
LENS MODELS AND MAGNIFICATION MAPS OF THE SIX HUBBLE FRONTIER FIELDS CLUSTERS (2014, unknown): “…Jullo et al. (2007); LensPerfect, Coe et al. (2008); glafic, Oguri (2010); GRALE, Liesenborgs et al. (2010); strong and weak lensing united, Bradač et al. (2005); SaWLens, Merten et al. (2009); light-traces-mass, Broadhurst et al. (2005) and Zitrin et al. (2009b); GRAVLENS, Keeton (2001)).”
A Comprehensive Study of Galaxies at z ∼ 9–16 Found in the Early JWST Data: Ultraviolet Luminosity Functions and Cosmic Star Formation History at the Pre-reionization Epoch (2022, methodology): “Golubchik et al. (2022) recently presented a mass model of SMACS J0723 developed by the light-traces-mass (LTM; Broadhurst et al. 2005; Zitrin et al. 2009, 2015) approach before the JWST ERO data release, and subsequently Pascale et al. (2022) presented LTM modeling with the JWST ERO data.”
THE DENSITY PROFILES OF MASSIVE, RELAXED GALAXY CLUSTERS. I. THE TOTAL DENSITY OVER THREE DECADES IN RADIUS (2012, background): “…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 & Limousin…”
CLASH: THE ENHANCED LENSING EFFICIENCY OF THE HIGHLY ELONGATED MERGING CLUSTER MACS J0416.1−2403 (2012, methodology): “First, instead of power-law profiles traditionally used to represent the galaxies in our method (Broadhurst et al. 2005; Zitrin et al. 2009b), we model each galaxy with a Pseudo-Isothermal Elliptical Mass Distribution (PIEMD; Kassiola & Kovner 1993), adopting the exact formulation from Jullo et al.…”