The Mass Distribution of SDSS J1004$+$4112 Revisited

By M. Oguri. 2010

278 citations recorded by the source corpus.

We present a strong lens analysis of SDSS J1004+4112, a unique quasar lens produced by a massive cluster of galaxies at z = 0.68, using newly developed software for gravitational lensing. We find that our parametric mass model well reproduces all observations, including the positions of quasar images as well as those of multiply imaged galaxies with measured spectroscopic redshifts, time delays between quasar images, and the positions of faint central images. The predicted large total magnification of � � 70 suggests that the lens system is indeed a useful site for studying the fine structure of a distant quasar and its host galaxy. The dark halo component is found to be unimodal, centered on the brightest cluster galaxy and the Chandra X-ray surface brightness profile. In addition, the orientation of the halo component is quite consistent with those of the brightest cluster galaxy and member galaxy distribution, implying that the lensing cluster is a relaxed system. The radial profile of the best-fit mass model is in good agreement with a mass profile inferred from the X-ray observation. While the inner radial slope of the dark halo component is consistent with being � 1, a clear dependence of the predicted A–D time delay on the slope indicates that an additional time-delay measurement will improve constraints on the mass model.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/fb08e9f4cd59935b5ca1e6db6304748a0bbab5a3

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In Astronomy and Astrophysics

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Citations in the corpus

• The z ∼ 6 Luminosity Function Fainter than −15 mag from the Hubble Frontier Fields: The Impact of Magnification Uncertainties (2016, methodology): “…sources, we take the median of the model magnifications from the CATS (Jullo & Kneib 2009; Richard et al. 2014; Jauzac et al. 2015a,b),GLAFIC (Oguri 2010; Ishigaki et al. 2015; Kawamata et al. 2016), Sharon/Johnson (John- 5 son et al. 2014), and Zitrin parametric NFW models (Zitrin-NFW:…”
• HUBBLE FRONTIER FIELDS FIRST COMPLETE CLUSTER DATA: FAINT GALAXIES AT z ∼ 5–10 FOR UV LUMINOSITY FUNCTIONS AND COSMIC REIONIZATION (2014, methodology): “In this section, we construct a mass model of Abell 2744 at z = 0.308 using the parametric gravitational lensing package glafic (Oguri 2010).”
• JWST Census for the Mass–Metallicity Star Formation Relations at z = 4–10 with Self-consistent Flux Calibration and Proper Metallicity Calibrators (2023, methodology): “To correct for the magni fi cation factors, we use the glafic ( Oguri 2010, 2021 ) mass model of Kawamata et al. ( 2018 ) with a minor update based on Multi Unit Spectroscopic Explorer ( MUSE ) follow-up spectroscopy ( Bergamini et al. 2023 ) .”
• LENS MODELS AND MAGNIFICATION MAPS OF THE SIX HUBBLE FRONTIER FIELDS CLUSTERS (2014, methodology): “…of several innovative computational softwares for lens modeling (e.g., LENSTOOL, 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);…”
• The Dearth of z ∼ 10 Galaxies in All HST Legacy Fields—The Rapid Evolution of the Galaxy Population in the First 500 Myr (2017, methodology): “In particular, for those four clusters, our baseline lens model throughout this paper will be based on the glafic code (Oguri 2010) as described in Kawamata et al. (2016).”
• CLASH: WEAK-LENSING SHEAR-AND-MAGNIFICATION ANALYSIS OF 20 GALAXY CLUSTERS (2014, methodology): “The shear+magnification method has been tested (Umetsu 2013) against synthetic weak-lensing catalogs from simulations of analytical NFW lenses performed using the public package glafic (Oguri 2010).”
• Combined strong and weak lensing analysis of 28 clusters from the Sloan Giant Arcs Survey (2011, methodology): “The best-fit critical curves for individual clusters are presented in Appendix B. Strong lensing analysis for some of these clusters has been published in the literature (e.g., Oguri et al. 2009; Koester et al. 2010; Bayliss et al. 2010; Oguri 2010; Gralla et al. 2011).”
• 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): “The GLAFIC code performs the socalled parametric lens mass modeling, where shapes of the mass distributions of the cluster are described by a superposition of a small number of lens mass components with known profile shapes, and parameters characterizing the lens mass components are determined so as”
• CLASH: JOINT ANALYSIS OF STRONG-LENSING, WEAK-LENSING SHEAR, AND MAGNIFICATION DATA FOR 20 GALAXY CLUSTERS (2015, methodology): “The method has been tested (Umetsu 2013) with synthetic weaklensing catalogs from simulations of analytical NFW lenses performed using the public package GLAFIC (Oguri 2010).”
• Full-data Results of Hubble Frontier Fields: UV Luminosity Functions at z ∼ 6–10 and a Consistent Picture of Cosmic Reionization (2017, methodology): “We create images of the mock galaxies with writeimage function in the lens model software glafic (Oguri 2010).”
• The Frontier Fields lens modelling comparison project (2016, methodology): “For example, in addition to the standard external shear, one can add higher-order perturbations with arbitrary multipole orders (see Oguri 2010).”
• The evolution of the galaxy UV luminosity function at redshifts z ≃ 8 – 15 from deep JWST and ground-based near-infrared imaging (2022, methodology): “In the case of the SMACS0723 field, the volume was adjusted by the magnification factor which was computed from GLAFIC (Oguri 2010).”