The projected gravitational potential of the galaxy cluster MACS J1206 derived from galaxy kinematics

Stock, Dennis; Meyer, Sven; Sarli, Eleonora; Bartelmann, Matthias; Balestra, I.; Grillo, C.; Koekemoer, Anton M.; Mercurio, A.; Nonino, M.; Rosati, P.

doi:10.1051/0004-6361/201527035

Cited by 9 publications

(9 citation statements)

References 39 publications

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“…The regular morphology of MACS1206 makes it an excellent candidate to the application of the shape theorem. The projected gravitational potential of MACS1206 as inferred from galaxy kinematics under the hypothesis of spherical symmetry agrees well with the reconstruction of the gravitational potential from weak and strong gravitational lensing or X-ray measurements (Stock et al 2015).…”

Section: Icmsupporting

confidence: 72%

CLUMP-3D: three-dimensional lensing and multi-probe analysis of MACS J1206.2−0847, a remarkably regular cluster

Sereno

Ettori

Meneghetti

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Multi-wavelength techniques can probe the distribution and the physical properties of baryons and dark matter in galaxy clusters from the inner regions out to the peripheries. We present a full three-dimensional analysis combining strong and weak lensing, X-ray surface brightness and temperature, and the Sunyaev-Zel'dovich effect. The method is applied to MACS J1206.2-0847, a remarkably regular, face-on, massive, M 200 = (1.1 ± 0.2) × 10 15 M /h, cluster at z = 0.44. The measured concentration, c 200 = 6.3 ± 1.2, and the triaxial shape are common to halos formed in a ΛCDM scenario. The gas has settled in and follows the shape of the gravitational potential, which is evidence of pressure equilibrium via the shape theorem. There is no evidence for significant non-thermal pressure and the equilibrium is hydrostatic.

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Section: Icmsupporting

confidence: 72%

CLUMP-3D: three-dimensional lensing and multi-probe analysis of MACS J1206.2−0847, a remarkably regular cluster

Sereno

Ettori

Meneghetti

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…The overall cluster mass distribution was further studied through a combination of weak and strong lensing (Umetsu et al 2012) and galaxy dynamics based on a large redshift sample of cluster members from the CLASH-VLT project (Biviano et al 2013;Rosati et al 2014). Further analysis of its gravitational potential and mass distribution have included a combination of methods and multiwavelength data sets (Stock et al 2015;Sereno et al 2017). The stellar content of MACS 1206 has also been the subject of a number of studies using spectrophotometric and kinematical information from the CLASH-VLT data set: Presotto et al (2014) has studied the color and morphological properties of its prominent intracluster light (ICL), detailed investigations of its galaxy populations, and internal structure have been presented in Annunziatella et al (2014) and Girardi et al (2015), and more recently in Kuchner et al (2017).…”

Section: Introductionmentioning

confidence: 99%

Mass distribution in the core of MACS J1206

Caminha

Grillo

Rosati

et al. 2017

A&A

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We present a new strong lensing analysis of the galaxy cluster MACS J1206.2−0847 (MACS 1206), at z = 0.44, using deep spectroscopy from CLASH-VLT and VLT/MUSE archival data in combination with imaging from the Cluster Lensing and Supernova survey with Hubble. MUSE observations enable the spectroscopic identification of 23 new multiply imaged sources, extending the previous compilations by a factor of approximately five. In total, we use the positional measurements of 82 spectroscopic multiple images belonging to 27 families at z = 1.0 − 6.1 to reconstruct the projected total mass distribution of MACS 1206. Remarkably, 11 multiple images are found within 50 kpc of the brightest cluster galaxy, making this an unprecedented set of constraints for the innermost projected mass distribution of a galaxy cluster. We thus find that, although dynamically relaxed, the smooth matter component (dark matter plus hot gas) of MACS 1206 shows a significant asymmetry, which closely follows the asymmetric distribution of the stellar component (galaxy members and intracluster light). We determine the value of the innermost logarithmic slope of the projected total mass density profile and find it to be close to the canonical Navarro-Frenk-White value. We demonstrate that this quantity is very robust against different parametrizations of the diffuse mass component; however, this is not the case when only one central image is used in the mass reconstruction. We also show that the mass density profile from our new strong lensing model is in very good agreement with dynamical and X-ray measurements at larger radii, where they overlap.

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“…The latter is essential to prevent the algorithm from overfitting. Alternatively, the three-dimensional gravitational potential can also be reconstructed from cluster member velocity dispersion measurements, as shown in Stock et al (2015), in case a coupling of dynamics and lensing on cluster scale may become necessary in the future.…”

Section: Breaking Degeneracies By Non-lensing Observables (Velocity Dmentioning

confidence: 99%

Generalised model-independent characterisation of strong gravitational lenses – VI. The origin of the formalism intrinsic degeneracies and their influence on H0

Wagner

2019

Monthly Notices of the Royal Astronomical Society

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We give a physical interpretation of the formalism intrinsic degeneracies of the gravitational lensing formalism that we derived on a mathematical basis in part IV of this series. We find that all degeneracies occur due to the partition of the mass density along the line of sight. Usually, it is partitioned into a background (cosmic) density and a foreground deflecting object. The latter can be further partitioned into a main deflecting object and perturbers. Weak deflecting objects along the line of sight are also added, either to the deflecting object or as a correction of the angular diameter distances, perturbing the cosmological background density. A priori, this is an arbitrary choice of reference frame and partition. They can be redefined without changing the lensing observables which are sensitive to the integrated deflecting mass density along the entire line of sight. Reformulating the time delay equation such that this interpretation of the degeneracies becomes easily visible, we note that the source can be eliminated from this formulation, which simplifies reconstructions of the deflecting mass distribution or the inference of the Hubble constant, H 0 . Subsequently, we list necessary conditions to break the formalism intrinsic degeneracies and discuss ways to break them by model choices or including non-lensing observables like velocity dispersions along the line of sight with their advantages and disadvantages. We conclude with a systematic summary of all formalism intrinsic degeneracies and possibilities to break them.

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The projected gravitational potential of the galaxy cluster MACS J1206 derived from galaxy kinematics

Cited by 9 publications

References 39 publications

CLUMP-3D: three-dimensional lensing and multi-probe analysis of MACS J1206.2−0847, a remarkably regular cluster

CLUMP-3D: three-dimensional lensing and multi-probe analysis of MACS J1206.2−0847, a remarkably regular cluster

Mass distribution in the core of MACS J1206

Generalised model-independent characterisation of strong gravitational lenses – VI. The origin of the formalism intrinsic degeneracies and their influence on H0

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