Wide‐Field Weak Lensing by RX J1347−1145

Kling, Thomas; Dell’Antonio, Ian; Wittman, David

doi:10.1086/428891

Cited by 17 publications

(21 citation statements)

References 17 publications

(48 reference statements)

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“…In addition, if only r s of an NFW profile was given in the literature, we multiplied it (and its error) by the concentration parameter given to obtain an r 200 . This is only a rough estimate of the error, Cohen & Kneib (2002) 910 ± 130 kinematic Allen et al (2002) 1590 ± 150 38 ± 8 X-ray Kling et al (2005) 1400 Fischer & Tyson (1997) The high core radius required to fit the mass profile in this work is compensated for by an unusually high velocity dispersion. A singular isothermal sphere would have a much lower velocity dispersion (in the range 1450−1600 km s −1 ) as can be seen at least qualitatively by extending the degeneracy of the two parameters in Fig.…”

Section: Comparison To Previous Mass Estimatesmentioning

confidence: 72%

“…0 5± 0.37 X-ray (DDg1) Schindler et al (1997) 35 1.78 X-ray Sahu et al (1998) 3 5 5 . 3 4 S L This work 35 2.56 ± 0.12 SL Bradač et al (2005) 90 12.00 ± 3.00 SWL This work 90 8.69 ± 1.37 SL Kling et al (2005) 124 12.86 ± 2.86 WL (SIS) Kling et al (2005) 124 15.00 +1.43 −2.14 WL (NFW) This work 124 12.60 ± 2.58 SL Gitti et al (2007) 147 9.95 ± 1.03 X-ray (SO) Gitti et al (2007) 147 9.17 ± 1.79 X-ray (DDg1) Fischer & Tyson (1997) 294 28.81 ± 6.78 WL with the Chandra X-ray telescope is presented in Bradač et al (2007).…”

Section: Comparison To Previous Mass Estimatesmentioning

confidence: 87%

“…Gravitational lensing based only on the arcs has also been used to estimate the mass (Sahu et al 1998) as has weak lensing (Fischer & Tyson 1997;Kling et al 2005). Recently a combination of both the weak and strong lensing has also been used (Bradač et al 2005).…”

Section: Article Published By Edp Sciencesmentioning

confidence: 99%

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The mass distribution of RX J1347–1145 from strong lensing

Halkola

Hildebrandt

Schrabback

et al. 2008

A&A

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Aims. We determine the central mass distribution of galaxy cluster RX J1347−1145 using strong gravitational lensing. Methods. High-resolution HST/ACS images of the galaxy cluster RX J1347−1145 have enabled us to identify several new multipleimage candidates in the cluster, including a 5-image system with a central image. The multiple-images allow us to construct an accurate 2-dimensional mass map of the central part of the cluster. The modelling of the cluster mass includes the most prominent cluster galaxies modelled as truncated isothermal spheres and a smooth halo component that is described with 2 parametric profiles. The mass reconstruction is done using a Markov chain Monte Carlo method that provides us with a total projected mass density, as well as with estimates for the parameters of interest and their respective errors. Results. Inside the Einstein radius of the cluster (∼35 , or ∼200 kpc, for a source at redshift 1.8), we obtain a total mass of (2.6 ± 0.1) × 10 14 M . The mass profile of the cluster is well-fitted by both a Navarro, Frenk, and White profile with a moderate concentration of c = 5.3 −0.1 Mpc, and a non-singular isothermal sphere with velocity dispersion σ = 1949 ± 40 km s −1 and a core radius of r c = 20 ± 2 . The mass profile agrees with previous mass estimates based on the X-ray emission from the hot intra-cluster gas, although the X-ray mass estimates are systematically lower than what we obtain with gravitational lensing.

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Section: Comparison To Previous Mass Estimatesmentioning

confidence: 72%

Section: Comparison To Previous Mass Estimatesmentioning

confidence: 87%

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The mass distribution of RX J1347–1145 from strong lensing

Halkola

Hildebrandt

Schrabback

et al. 2008

A&A

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show abstract

“…Lensing, both strong and weak, is frequently used to estimate the mass and the NFW concentration parameter of clusters, which are then compared to those from simulations or X-ray measurements, with lensing usually finding a higher mass and concentration [11,32,33,30,31]. Therefore, it is of interest to study whether an underlying Sérsic profile could cause a bias in the mass and c estimate, if an NFW profile is assumed in the strong lensing modelling.…”

Section: Mass and Concentrationmentioning

confidence: 99%

A comparison of the strong lensing properties of the Sérsic and the Navarro, Frenk and White profiles

Elíasdóttir¹,

Möller²

2007

J. Cosmol. Astropart. Phys.

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Abstract. We investigate the strong lensing properties of the Sérsic profile as an alternative to the NFW profile, focusing on applications to lens modelling of clusters. Given an underlying Sérsic dark matter profile, we study whether an NFW profile can provide an acceptable fit to strong lensing constraints in the form of single or multiple measured Einstein radii. We conclude that although an NFW profile that fits the lensing constraints can be found in many cases, the derived parameters may be biased. In particular, we find that for n ∼ 2, which corresponds to massive clusters, the mass at r 200 of the best fit NFW is overestimated (by a factor of ∼ 2) and the concentration is very low (c ∼ 2). The differences are important enough to warrant the inclusion of Sérsic profile for future analysis of strong lensing clusters.

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“…Although information about the cluster is still there, as a practical matter the effort to recover it may not be justified given the logarithmic dependence on θ max . The shear around a massive cluster can clearly be observed out to at least 15 from the center (e.g., Kling et al 2005), so θ max = 15 should be a conservative value. Thus Equation (9) is approximately equal to 17n, and only weakly dependent on the adopted values of θ min and θ max .…”

Section: Basic Idea and Toy Modelmentioning

confidence: 99%

Constraining Source Redshift Distributions With Gravitational Lensing

Wittman

Dawson

2012

ApJ

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We introduce a new method for constraining the redshift distribution of a set of galaxies, using weak gravitational lensing shear. Instead of using observed shears and redshifts to constrain cosmological parameters, we ask how well the shears around clusters can constrain the redshifts, assuming fixed cosmological parameters. This provides a check on photometric redshifts, independent of source spectral energy distribution properties and therefore free of confounding factors such as misidentification of spectral breaks. We find that ∼40 massive (σ v = 1200 km s −1 ) cluster lenses are sufficient to determine the fraction of sources in each of six coarse redshift bins to ∼11%, given weak (20%) priors on the masses of the highest-redshift lenses, tight (5%) priors on the masses of the lowest-redshift lenses, and only modest (20%-50%) priors on calibration and evolution effects. Additional massive lenses drive down uncertainties as N − 1 2 lens , but the improvement slows as one is forced to use lenses further down the mass function. Future large surveys contain enough clusters to reach 1% precision in the bin fractions if the tight lens-mass priors can be maintained for large samples of lenses. In practice this will be difficult to achieve, but the method may be valuable as a complement to other more precise methods because it is based on different physics and therefore has different systematic errors.

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Wide‐Field Weak Lensing by RX J1347−1145

Cited by 17 publications

References 17 publications

The mass distribution of RX J1347–1145 from strong lensing

The mass distribution of RX J1347–1145 from strong lensing

A comparison of the strong lensing properties of the Sérsic and the Navarro, Frenk and White profiles

Constraining Source Redshift Distributions With Gravitational Lensing

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