Weak Lensing by High‐Redshift Clusters of Galaxies. I. Cluster Mass Reconstruction

Clowe, Douglas; Luppino, Gerard A.; Kaiser, Nick; Gioia, I. M.

doi:10.1086/309242

Cited by 109 publications

(161 citation statements)

References 50 publications

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“…The local sky level and its gradient are measured around each object from the mode of pixel values on a circular annulus defined by inner and outer radii of 16r g and 32r g (see Clowe et al 2000). In order to avoid contamination in the background estimation by bright neighboring stars and/or foreground galaxies, all pixels within 3r g of another object are excluded from the mode calculation.…”

Section: Object Detectionmentioning

confidence: 99%

Combining Lens Distortion and Depletion to Map the Mass Distribution of A1689

Umetsu

Broadhurst

2008

Astrophysical Journal

139

199

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We derive a projected 2D mass map of the well-studied galaxy cluster A1689 based on an entropy-regularized maximum likelihood combination of the lens magnification and distortion of red background galaxies registered in deep Subaru images. The method is not restricted to the weak regime but applies to the whole area outside the tangential critical curve, where nonlinearity between the surface mass density and the observables extends to a radius of a few arcminutes. The known strong-lensing information is also readily incorporated in this approach, represented as a central pixel with a mean surface density close to the critical value. We also utilize the distortion measurements to locally downweight the intrinsic clustering noise, which otherwise perturbs the depletion signal. The projected mass profile continuously steepens with radius and is well fitted by the Navarro-Frenk-White model, but with a surprisingly large concentration c vir ¼ 13:4 þ5:3 À3:3 , lying far from the predicted value of c vir $ 5, corresponding to the measured virial mass, M vir ¼ (2:1 AE 0:2) ; 10 15 M , posing a challenge to the standard assumptions defining the ÃCDM model. We examine the consistency of our results with estimates derived with the standard weak-lensing estimators and by comparison with the inner mass profile obtained from strong lensing. All the reconstructions tested here imply a virial mass in the range M vir ¼ (1:5Y2:1) ; 10 15 M , and the combined ACS and Subaru 2D mass reconstruction yields a tight constraint on the concentration parameter, c vir ¼ 12:7 AE 1 AE 2:8 (c 200 $ 10), improving upon the statistical accuracy of our earlier 1D analysis. Importantly, our best-fitting profile properly reproduces the observed Einstein radius of 45 00 (z s ¼ 1), in contrast to other weak-lensing work, reporting lower concentration profiles, which underestimate the observed Einstein radius.

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Section: Object Detectionmentioning

confidence: 99%

Combining Lens Distortion and Depletion to Map the Mass Distribution of A1689

Umetsu

Broadhurst

2008

Astrophysical Journal

139

199

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“…It consists of two components, one main cluster and a smaller subcluster. Clowe et al (2004) fitted the main cluster to a NFW profile and measured the mass of the subcluster using aperture densitometry (Clowe et al 2000;Fahlman et al 1994). -Abell 2744 is made up of two subclusters aligned along the line-of-sight (Boschin et al 2006).…”

Section: Cluster Lens Models and Number Countsmentioning

confidence: 99%

A LABOCA survey of submillimeter galaxies behind galaxy clusters

Johansson

Sigurdarson

Horellou

2011

A&A

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Context. Submillimeter galaxies are a population of dusty star-forming galaxies at high redshift. Measuring their properties will help relate them to other types of galaxies, both at high and low redshift. This is needed in order to understand the formation and evolution of galaxies. Aims. The aim is to use gravitational lensing by galaxy clusters to probe the faint and abundant submillimeter galaxy population down to a lower flux density level than what can be achieved in blank-field observations. Methods. We use the LABOCA bolometer camera on the APEX telescope to observe five clusters of galaxies at a wavelength of 870 μm. The final maps have an angular resolution of 27.5 and a point source noise level of 1.2-2.2 mJy. We model the mass distribution in the clusters as superpositions of spherical NFW halos and derive magnification maps that we use to calculate intrinsic flux densities as well as area-weighted number counts. We also use the positions of Spitzer MIPS 24 μm sources in four of the fields for a stacking analysis. Results. We detected 37 submm sources, out of which 14 have not been previously reported. One source has a sub-mJy intrinsic flux density. The derived number counts are consistent with previous results, after correction for gravitational magnification and completeness levels. The stacking analysis reveals an intrinsic 870 μm signal of 390 ± 27 μJy at 14.5σ significance. We study the S 24 μm -S 870 μm relation by stacking on subsamples of the 24 μm sources and find a linear relation at S 24 μm < 300 μJy, followed by a flattening at higher 24 μm flux densities. The signal from the significantly detected sources in the maps accounts for 13% of the Extragalactic Background Light discovered by COBE, and the stacked signal accounts for 11%.

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“…Among the latter are those based on an analysis of the distribution and temperature of the X-ray-emitting gas (e.g., Markevitch et al 1999;Allen et al 2002;Arabadjis, Bautz, & Garmire 2002;Pratt & Arnaud 2002), those based on an analysis of the weak-lensing distortion of background galaxies (e.g., Lombardi et al 2000;Clowe et al 2000;Clowe & Schneider 2001;Athreya et al 2002;Hoekstra et al 2002;King et al 2002;Dahle, Hannestad, & SommerLarsen 2003), and those based on an analysis of the projected phase-space distribution of the galaxies (e.g., Geller et al 1999;van der Marel et al 2000;Rines et al 2002;Biviano & Girardi 2003). In some of these analyses, not only was consistency with an NFW-type mass profile established, but an upper limit to the size of a core could also be given (e.g., Arieli & Rephaeli 2003;Dahle et al 2003).…”

Section: The Mass Profilementioning

confidence: 99%

The ESO Nearby Abell Cluster Survey. XII. The Mass and Mass‐to‐Light Ratio Profiles of Rich Clusters

Katgert

Biviano

Mazure

2004

ApJ

118

173

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We determine the mass profile of an ensemble cluster built from 3056 galaxies in 59 nearby clusters observed in the ESO Nearby Abell Cluster Survey. The mass profile is derived from the distribution and kinematics of the early-type (elliptical and S0) galaxies only, with projected distances from the centers of their clusters 1.5r 200 . These galaxies are most likely to meet the conditions for the application of the Jeans equation, since they are the oldest cluster population and are thus quite likely to be in dynamical equilibrium with the cluster potential. In addition, the assumption that the early-type galaxies have isotropic orbits is supported by the shape of their velocity distribution. For galaxies of other types (the brightest elliptical galaxies, with M R À22 þ 5 log h, and the early and late spirals) these assumptions are much less likely to be satisfied. For the determination of the mass profile we also exclude early-type galaxies in subclusters. Application of the Jeans equation yields a nonparametric estimate of the cumulative mass profile M(

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Weak Lensing by High‐Redshift Clusters of Galaxies. I. Cluster Mass Reconstruction

Cited by 109 publications

References 50 publications

Combining Lens Distortion and Depletion to Map the Mass Distribution of A1689

Combining Lens Distortion and Depletion to Map the Mass Distribution of A1689

A LABOCA survey of submillimeter galaxies behind galaxy clusters

The ESO Nearby Abell Cluster Survey. XII. The Mass and Mass‐to‐Light Ratio Profiles of Rich Clusters

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