X‐ray emission from RX J1720.1+2638 and Abell 267: A comparison between a fossil and a non‐fossil system

Jiménez‐Bailón, E.; Lozada-Muñoz, M.; Aguerri, J. A. L.

doi:10.1002/asna.201211861

Cited by 4 publications

(7 citation statements)

References 24 publications

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“…The mass and concentration posteriors are consistent with the well established M 200 − c 200 relation derived from N-body simulations (Dutton & Macciò 2014). The corresponding mass profile (Figure 10) is in good agreement with previously measured masses of A267 from X-ray and weak-lensing measurements (Jiménez-Bailón et al 2013;Okabe et al 2010), as well as the dynamical estimate based on the caustic technique (Rines et al 2013). Interestingly, the dynamical mass previously estimated directly from the galaxy velocity dispersion (assuming no sub-substructure; Rines et al 2013) is larger than we infer when we allow for N subs = 5 sub-populations, but in good agreement with the mass profile we obtain if we restrict our Jeans model to N subs = 0 sub-populations.…”

Section: Discussionsupporting

confidence: 89%

Section: Results For A267supporting

confidence: 83%

“…Like previous plots, the dark and light regions show the 68% and 95% confidence intervals of the PDFs, and the solid and dashed black curves show the median posterior and maximum likelihood velocity dispersion profiles, respectively. For comparison we include previous mass measurements of A267 from a variety of different techniques: in green the weak lensing mass M WL 200 (Okabe & Smith 2016), in red and purple the caustic mass M Caustic 200 and viral mass calculated with velocity dispersion of cluster members M Dispersion vir , respectively , and in blue we show the X-ray derived mass M X 500 (Jiménez-Bailón et al 2013). Our results are consistent with M X 500 , M Caustic…”

Section: Jeans Analysissupporting

confidence: 77%

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Galaxy Cluster Mass Estimates in the Presence of Substructure

Tucker

Walker

Mateo

et al. 2020

ApJ

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We develop and implement a model to analyze the internal kinematics of galaxy clusters that may contain subpopulations of galaxies that do not independently trace the cluster potential. The model allows for substructures within the cluster environment, disentangles cluster members from contaminating foreground and background galaxies, and includes an overall cluster rotation term as part of the cluster kinematics. We estimate the cluster velocity dispersion and/or mass while marginalizing over uncertainties in all of the above complexities. In a first application to our published data for Abell 267 (A267), we find no evidence for cluster rotation but we identify up to five distinct galaxy subpopulations. We use these results to explore the sensitivity of inferred cluster properties to the treatment of substructure. Compared to a model that assumes no substructure, our substructure model reduces the dynamical mass of A267 by ∼ 20% and shifts the cluster mean velocity by ∼ 100 km s −1 , approximately doubling the offset with respect to the velocity of A267's brightest cluster galaxy. Embedding the spherical Jeans equation within this framework, we infer for A267 a dark matter halo of mass M 200 = 6.77 ± 1.06 × 10 14 M /h, concentration log 10 c 200 = 0.61 ± 0.39, consistent with the mass-concentration relation found in cosmological simulations.

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Section: Discussionsupporting

confidence: 89%

Section: Results For A267supporting

confidence: 83%

Section: Jeans Analysissupporting

confidence: 77%

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Galaxy Cluster Mass Estimates in the Presence of Substructure

Tucker

Walker

Mateo

et al. 2020

ApJ

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“…Our smooth parametric fit shows a decrease in temperature in the outskirts at a significance of 11.8σ, and both our density and temperature profiles are in excellent agreement with the ACCEPT values. Jiménez-Bailón et al (2013) found a shock front with >16keV gas 2 NW of cluster, and this elongated cluster is possibly undergoing a large merger event (Boschin et al 2004). Further evidence for a major merger was detailed in Canning et al (2015), who used Chandra data to identify numerous cold and shock fronts, along with a large temperature spike ∼ 25 away from the core of the cluster.…”

Section: Discussionmentioning

confidence: 94%

Thermodynamic profiles of galaxy clusters from a joint X-ray/SZ analysis

Shitanishi

Pierpaoli

Sayers

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We jointly analyze Bolocam Sunyaev-Zeldovich (SZ) effect and Chandra X-ray data for a set of 45 clusters to derive gas density and temperature profiles without using spectroscopic information. The sample spans the mass and redshift range 3×10 14 M ≤ M 500 ≤ 25 × 10 14 M and 0.15 ≤ z ≤ 0.89. We define cool-core (CC) and non-cool core (NCC) subsamples based on the central X-ray luminosity, and 17/45 clusters are classified as CC. In general, the profiles derived from our analysis are found to be in good agreement with previous analyses, and profile constraints beyond r 500 are obtained for 34/45 clusters. In approximately 30% of the CC clusters our analysis shows a central temperature drop with a statistical significance of > 3σ; this modest detection fraction is due mainly to a combination of coarse angular resolution and modest S/N in the SZ data. Most clusters are consistent with an isothermal profile at the largest radii near r 500 , although 9/45 show a significant temperature decrease with increasing radius. The sample mean density profile is in good agreement with previous studies, and shows a minimum intrinsic scatter of approximately 10% near 0.5 × r 500 . The sample mean temperature profile is consistent with isothermal, and has an intrinsic scatter of approximately 50% independent of radius. This scatter is significantly higher compared to earlier X-ray-only studies, which find intrinsic scatters near 10%, likely due to a combination of unaccounted for non-idealities in the SZ noise, projection effects, and sample selection. X-ray/SZ Galaxy Cluster Deprojections 3determined for both the full cluster sample and various sub-samples. The standard flat ΛCDM model is used, with Ω m = 0.3, Ω Λ = 0.7, and the dimensionless Hubble parameter h = 0.7. The outline of the paper is as follows: Sec. 2 describes the cluster sample, Sec. 3 details the data reduction, and Sec. 4 reviews the modeling and fitting methods. Sec. 5 describes detailed consistency tests based on mock observations of smooth cluster models, Sec. 6 reviews the individual and joint cluster results, and Sec. 7 presents the overall conclusions. CLUSTER SAMPLEThe Bolocam X-ray/SZ (BOXSZ) sample consists of 45 clusters observed by both Bolocam and Chandra, and Tab. 1 lists some important characteristics of the clusters. The images from both instruments are approximately 14 in size. Given the relatively high median redshift of the sample, z = 0.44 (see Fig. 1), these images in general contain information beyond r 500 and therefore allow for studies of the clusters' outskirts. The clusters' masses, as estimated from X-rays according to the procedures described in Mantz et al. (2010b), span the range M 500 3 − 25 × 10 14 M .As in Sayers et al. (2013b), CC and NCC clusters are differentiated using an X-ray luminosity ratio cut. If the luminosity within 0.05r 500 is greater than 0.17 times the total luminosity within r 500 , then the cluster is classified as CC. Within the BOXSZ sample, the CC clusters have a lower median redshift compared to the NCC cluste...

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“…Further contributions in the present conference summary volume by Marziani et al (2013), Jiménez-Bailón et al (2013), and Gu et al (2013) discuss various connections of cluster properties to the galaxy population in the clusters.…”

Section: Simulationsmentioning

confidence: 98%

X‐ray galaxy cluster studies for astro‐physics and cosmology

Böhringer

Schartel

2013

Astron Nachr

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The field of research on galaxy clusters has received an enormous increase in attention in the last years, since galaxy clusters have been more and more recognized as very important laboratories for astrophysical studies and observational probes for testing cosmological models. X-ray observations of these largest clearly defined objects in our Universe have been by far the most fruitful approach that has provided us with rich astrophysical and cosmological insights. ESA's XMM-Newton and NASA's Chandra observatories have been the powerhorses of this research. In this article we therefore like to summarize the major advances made in the field of galaxy cluster research primarily by these two instruments. We will touch the progress in understanding the structure of galaxy clusters and its statistics, the AGN feedback processes in the center of clusters, cosmic evolution of clusters, cluster mass measurements, the thermodynamic structure of the intracluster medium and its chemistry, X-ray surveys of clusters, and the use of galaxy clusters for cosmological tests.

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X‐ray emission from RX J1720.1+2638 and Abell 267: A comparison between a fossil and a non‐fossil system

Cited by 4 publications

References 24 publications

Galaxy Cluster Mass Estimates in the Presence of Substructure

Galaxy Cluster Mass Estimates in the Presence of Substructure

Thermodynamic profiles of galaxy clusters from a joint X-ray/SZ analysis

X‐ray galaxy cluster studies for astro‐physics and cosmology

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