The Three-Dimensional Shapes of Galaxy Clusters

Limousin, M.; Morandi, Andrea; Sereno, Mauro; Meneghetti, M.; Ettori, S.; Bartelmann, Matthias; Verdugo, T.

doi:10.1007/s11214-013-9980-y

Cited by 123 publications

(144 citation statements)

References 177 publications

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“…This results in two image systems with two and four images, respectively, and is a configuration that is also commonly found in other strong lensing systems (e.g., Gavazzi et al 2008;Tu et al 2009;Limousin et al 2009;Bayliss et al 2011). We fitted the centroid position in right ascension, ∆RA, and declination, ∆Dec, the velocity dispersion of the PIEMD, σ PIEMD , as well as its ellipticity, , and position angle, PA (see also Limousin et al 2013;Bonamigo et al 2015). The core and cutoff radii are poorly constrained with an Einstein ring of about 6.2 kpc at z = 1.525.…”

Section: Lens Modeling and Source Reconstructionmentioning

confidence: 60%

Planck’s dusty GEMS

Cañameras

Nesvadba

Kneißl

et al. 2017

A&A

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We study the properties of the foreground galaxy of the Ruby, the brightest gravitationally lensed high-redshift galaxy on the sub-millimeter sky as probed by the Planck satellite, and part of our sample of Planck's Dusty GEMS. The Ruby consists of an Einstein ring of 1.4 diameter at z = 3.005 observed with ALMA at 0.1 resolution, centered on a faint, red, massive lensing galaxy seen with HST/WFC3, which itself has an exceptionally high redshift, z = 1.525 ± 0.001, as confirmed with VLT/X-Shooter spectroscopy. Here we focus on the properties of the lens and the lensing model obtained with LENSTOOL. The rest-frame optical morphology of this system is strongly dominated by the lens, while the Ruby itself is highly obscured, and contributes less than 10 % to the photometry out to the K band. The foreground galaxy has a lensing mass of (3.70 ± 0.35) × 10 11 M . Magnification factors are between 7 and 38 for individual clumps forming two image families along the Einstein ring. We present a decomposition of the foreground and background sources in the WFC3 images, and stellar population synthesis modeling with a range of star-formation histories for Chabrier and Salpeter initial mass functions (IMFs). Only the stellar mass range obtained with the latter agrees well with the lensing mass. This is consistent with the bottom-heavy IMFs of massive high-redshift galaxies expected from detailed studies of the stellar masses and mass profiles of their low-redshift descendants, and from models of turbulent gas fragmentation. This may be the first direct constraint on the IMF in a lens at z = 1.5, which is not a cluster central galaxy.

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Section: Lens Modeling and Source Reconstructionmentioning

confidence: 60%

Planck’s dusty GEMS

Cañameras

Nesvadba

Kneißl

et al. 2017

A&A

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“…Limousin et al 2013 and references therein). Dynamically young clusters within filaments are also expected to be more elongated than relaxed clusters.…”

Section: Discussionmentioning

confidence: 99%

Large-Scale Filamentary Structures Around the Virgo Cluster Revisited

Kim

Rey

Bureau

et al. 2016

ApJ

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We revisit the filamentary structures of galaxies around the Virgo cluster, exploiting a larger dataset based on the HyperLeda database than previous studies. In particular, this includes a large number of low-luminosity galaxies, resulting in better sampled individual structures. We confirm seven known structures in the distance range 4 h −1 Mpc < SGY < 16 h −1 Mpc, now identified as filaments, where SGY is the axis of the supergalactic coordinate system roughly along the line of sight. The Hubble diagram of the filament galaxies suggests they are infalling toward the main-body of the Virgo cluster. We propose that the collinear distribution of giant elliptical galaxies along the fundamental axis of the Virgo cluster is smoothly connected to two of these filaments (Leo II A and B). Behind the Virgo cluster (16 h −1 Mpc < SGY < 27 h −1 Mpc), we also identify a new filament elongated toward the NGC 5353/4 group ("NGC 5353/4 filament") and confirm a sheet that includes galaxies from the W and M clouds of the Virgo cluster ("W-M sheet"). In the Hubble diagram, the NGC 5353/4 filament galaxies show infall toward the NGC 5353/4 group, whereas the W-M sheet galaxies do not show hints of gravitational influence from the Virgo cluster. The filamentary structures identified can now be used to better understand the generic role of filaments in the build-up of galaxy clusters at z ≈ 0.

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“…Hence knowledge of the intrinsic shape and orientation of halos is crucial for an unbiased determination of their masses. As reviewed in Limousin et al (2012) multi-wavelength observations of the ICM and mass can be used to quantify and account for triaxiality.…”

Section: Some General Considerationsmentioning

confidence: 99%

Scaling Relations for Galaxy Clusters: Properties and Evolution

et al. 2013

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Well-calibrated scaling relations between the observable properties and the total masses of clusters of galaxies are important for understanding the physical processes that give rise to these relations. They are also a critical ingredient for studies that aim to constrain cosmological parameters using galaxy clusters. For this reason much effort has been spent during the last decade to better understand and interpret relations of the properties of the intra-cluster medium. Improved X-ray data have expanded the mass range down to galaxy groups, whereas SZ surveys have openened a new observational window on the intracluster medium. In addition, continued progress in the performance of cosmological simulations has allowed a better understanding of the physical processes and selection effects affecting the observed scaling relations. Here we review the recent literature on various scaling relations, focussing on the latest observational measurements and the progress in our understanding of the deviations from self similarity.

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The Three-Dimensional Shapes of Galaxy Clusters

Cited by 123 publications

References 177 publications

Planck’s dusty GEMS

Planck’s dusty GEMS

Large-Scale Filamentary Structures Around the Virgo Cluster Revisited

Scaling Relations for Galaxy Clusters: Properties and Evolution

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