Optical and X-Ray Observations of the Merging Cluster As1063

Gómez, Percy; Valkonen, Laura; Romer, A. K.; Lloyd-Davies, E. J.; Verdugo, T.; Cantalupo, C. M.; Daub, M. D.; Goldstein, Jonathan; Kuo, Chao-Lin; Lange, A. E.; Lueker, M.; Holzapfel, W. L.; Peterson, Jim; Ruhl, J. E.; Runyan, M. C.; Reichardt, Christian; Sabirli, Kivanc

doi:10.1088/0004-6256/144/3/79

Cited by 58 publications

(69 citation statements)

References 42 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Like the other Frontier Field clusters, its map of galaxy density shows significant substructure, with an X-ray peak offset from the primary peak of galaxy density (Gómez et al 2012). Weak-lensing analysis also identified multiple substructures, and gives a mass of the central cluster in agreement with X-ray and SZ calculations (Gruen et al 2013).…”

Section: Abell S1063mentioning

confidence: 57%

“…Abell S1063 (also known as RXC J2248.7-4431 and SPT-CL J2248-4431), is the southernmost Frontier Fields cluster with z=0.3461 (Abell et al 1989;Böhringer et al 2004;Gómez et al 2012). Abell S1063 is a massive cluster with a large velocity dispersion .…”

Section: Abell S1063mentioning

confidence: 99%

“…Abell S1063 is a massive cluster with a large velocity dispersion . Its X-ray luminosity between 0.5 and 2.0 keV is (1.8±0.2) ×10 45 erg s −1 (Williamson et al 2011), and the cluster has one of the highest known X-ray temperatures (>11.5 keV) (Gómez et al 2012). It is also among the clusters most strongly detected via the Sunyaev-Zel'dovich (SZ) effect in the South Pole Telescope survey (Williamson et al 2011), with an SZ-derived mass Ḿ M 1.4 10 500 15…”

Section: Abell S1063mentioning

confidence: 99%

See 2 more Smart Citations

The Frontier Fields: Survey Design and Initial Results

Lotz

Koekemoer

Coe

et al. 2017

ApJ

609

574

View full text Add to dashboard Cite

What are the faintest distant galaxies we can see with the Hubble Space Telescope (HST) now, before the launch of the James Webb Space Telescope? This is the challenge taken up by the Frontier Fields, a Director's discretionary time campaign with HST and the Spitzer Space Telescope to see deeper into the universe than ever before. The Frontier Fields combines the power of HST and Spitzer with the natural gravitational telescopes of massive highmagnification clusters of galaxies to produce the deepest observations of clusters and their lensed galaxies ever obtained. Six clusters-Abell 2744, MACSJ0416.1-2403, MACSJ0717.5+3745, MACSJ1149.5+2223, Abell S1063, and Abell 370-have been targeted by the HST ACS/WFC and WFC3/IR cameras with coordinated parallel fields for over 840 HST orbits. The parallel fields are the second-deepest observations thus far by HST with 5σ point-source depths of ∼29th ABmag. Galaxies behind the clusters experience typical magnification factors of a few, with small regions magnified by factors of 10-100. Therefore, the Frontier Field cluster HST images achieve intrinsic depths of ∼30-33 mag over very small volumes. Spitzer has obtained over 1000 hr of Director's discretionary imaging of the Frontier Field cluster and parallels in IRAC 3.6 and 4.5 μm bands to 5σ point-source depths of ∼26.5, 26.0 ABmag. We demonstrate the exceptional sensitivity of the HST Frontier Field images to faint high-redshift galaxies, and review the initial results related to the primary science goals.

show abstract

Section: Abell S1063mentioning

confidence: 57%

Section: Abell S1063mentioning

confidence: 99%

Section: Abell S1063mentioning

confidence: 99%

See 1 more Smart Citation

The Frontier Fields: Survey Design and Initial Results

Lotz

Koekemoer

Coe

et al. 2017

ApJ

609

574

View full text Add to dashboard Cite

show abstract

“…Gómez et al (2012) indicates that the galaxy cluster has undergone a recent off-axis merger, and Melchior et al (2015) find the cluster to be embedded in a filament with corresponding orientation. However, moderately deep X-ray Chandra observations show an elongated but regular shape, with no evidence of massive substructures in the inner region (see Fig.…”

Section: Rxc J2248mentioning

confidence: 99%

CLASH-VLT: A highly precise strong lensing model of the galaxy cluster RXC J2248.7−4431 (Abell S1063) and prospects for cosmography

Caminha

Grillo

Rosati

et al. 2016

A&A

123

View full text Add to dashboard Cite

Aims. We perform a comprehensive study of the total mass distribution of the galaxy cluster RXC J2248.7−4431 (z = 0.348) with a set of highprecision strong lensing models, which take advantage of extensive spectroscopic information on many multiply lensed systems. In the effort to understand and quantify inherent systematics in parametric strong lensing modelling, we explore a collection of 22 models in which we use different samples of multiple image families, different parametrizations of the mass distribution and cosmological parameters. Methods. As input information for the strong lensing models, we use the Cluster Lensing And Supernova survey with Hubble (CLASH) imaging data and spectroscopic follow-up observations, with the VIsible Multi-Object Spectrograph (VIMOS) and Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope (VLT), to identify and characterize bona fide multiple image families and measure their redshifts down to m F814W 26. A total of 16 background sources, over the redshift range 1.0−6.1, are multiply lensed into 47 images, 24 of which are spectroscopically confirmed and belong to ten individual sources. These also include a multiply lensed Lyman-α blob at z = 3.118. The cluster total mass distribution and underlying cosmology in the models are optimized by matching the observed positions of the multiple images on the lens plane. Bayesian Markov chain Monte Carlo techniques are used to quantify errors and covariances of the best-fit parameters. Results. We show that with a careful selection of a large sample of spectroscopically confirmed multiple images, the best-fit model can reproduce their observed positions with a rms scatter of 0. 3 in a fixed flat ΛCDM cosmology, whereas the lack of spectroscopic information or the use of inaccurate photometric redshifts can lead to biases in the values of the model parameters. We find that the best-fit parametrization for the cluster total mass distribution is composed of an elliptical pseudo-isothermal mass distribution with a significant core for the overall cluster halo and truncated pseudo-isothermal mass profiles for the cluster galaxies. We show that by adding bona fide photometric-selected multiple images to the sample of spectroscopic families, one can slightly improve constraints on the model parameters. In particular, we find that the degeneracy between the lens total mass distribution and the underlying geometry of the Universe, which is probed via angular diameter distance ratios between the lens and sources and the observer and sources, can be partially removed. Allowing cosmological parameters to vary together with the cluster parameters, we find (at 68% confidence level) Ω m = 0.25 for a Universe with w = −1 and free curvature. Finally, using toy models mimicking the overall configuration of multiple images and cluster total mass distribution, we estimate the impact of the line-of-sight mass structure on the positional rms to be 0. 3 ± 0. 1. We argue that the apparent sensitivity of our lensing model to cosmograp...

show abstract

“…For example, the galaxy at the center is clearly the BCG, unlike other clusters which have multiple galaxies of relatively equal brightness. Yet it may be more complicated than it appears: dynamical studies have shown that it could be going through a merging event (Gómez et al 2012). Our models are able to fit the data with only two halos, the fewest of the HFF clusters.…”

Section: Abell S1063mentioning

confidence: 91%

Exploring effects on magnifications due to line-of-sight galaxies in the Hubble Frontier Fields

Raney

Keeton

Brennan

2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Cluster lensing has become an important tool in the search for high redshift galaxies through its ability to magnify sources. In order to determine the intrinsic properties of these galaxies, lensing mass models must be constructed to determine the magnification of the images. These models are traditionally two-dimensional, focusing on the mass within the cluster and either ignoring or approximating any contribution from line-of-sight galaxies. In this paper, we present the first full set of three-dimensional mass models of the six Hubble Frontier Fields and use them to test for systematic biases in magnifications due to using the traditional 2D approach. We find that omitting foreground or background galaxies causes image position offsets between 0.1-0.4", a non-negligible fraction of the typical 0.3-0.7" residuals of current state-of-the-art models. We also find that median image magnifications can shift by up to 6%, though it is dependent on the field. This can be alleviated in some cases by approximating the mass in the lensing plane, but a 5% magnification bias still exists in other cases; image position offsets are also improved, but are still present at 0.10".

show abstract

Optical and X-Ray Observations of the Merging Cluster As1063

Cited by 58 publications

References 42 publications

The Frontier Fields: Survey Design and Initial Results

The Frontier Fields: Survey Design and Initial Results

CLASH-VLT: A highly precise strong lensing model of the galaxy cluster RXC J2248.7−4431 (Abell S1063) and prospects for cosmography

Exploring effects on magnifications due to line-of-sight galaxies in the Hubble Frontier Fields

Contact Info

Product

Resources

About