Discovery of a Large-Scale Filament Connected to the Massive Galaxy Cluster MACS J0717.5+3745 at z  = 0.55

2004 ◽  
Vol 609 (2) ◽  
pp. L49-L52 ◽  
Author(s):  
H. Ebeling ◽  
E. Barrett ◽  
D. Donovan
Keyword(s):  
Large Scale ◽  
Galaxy Cluster ◽  
Massive Galaxy

scholarly journals A weak lensing mass reconstruction of the large-scale filament feeding the massive galaxy cluster MACS J0717.5+3745

2012 ◽  
Vol 426 (4) ◽  
pp. 3369-3384 ◽  
Author(s):  
Mathilde Jauzac ◽  
Eric Jullo ◽  
Jean-Paul Kneib ◽  
Harald Ebeling ◽  
Alexie Leauthaud ◽  
...  
Keyword(s):  
Large Scale ◽  
Galaxy Cluster ◽  
Weak Lensing ◽  
Massive Galaxy ◽  
Mass Reconstruction

scholarly journals IDCS J1426.5+3508: THE MOST MASSIVE GALAXY CLUSTER ATz> 1.5

2016 ◽  
Vol 817 (2) ◽  
pp. 122 ◽  
Author(s):  
Mark Brodwin ◽  
Michael McDonald ◽  
Anthony H. Gonzalez ◽  
S. A. Stanford ◽  
Peter R. Eisenhardt ◽  
...  
Keyword(s):  
Galaxy Cluster ◽  
Massive Galaxy

scholarly journals A MOMENT METHOD FOR MEASURING THE HIGHER-ORDER WEAK GRAVITATIONAL LENSING EFFECTS

2008 ◽  
Vol 23 (17n20) ◽  
pp. 1506-1513 ◽  
Author(s):  
KEIICHI UMETSU ◽  
YUKI OKURA ◽  
TOSHIFUMI FUTAMASE
Keyword(s):  
Gravitational Lensing ◽  
Galaxy Cluster ◽  
Higher Order ◽  
Local Concentration ◽  
Fourier Space ◽  
Cluster Galaxy ◽  
Point Spread ◽  
Image Characteristics ◽  
Spread Function ◽  
Massive Galaxy

We present a method for measuring higher-order weak lensing distortions of faint background galaxies, namely the weak gravitational flexion, by fully extending the Kaiser, Squires & Broadhurst method to include higher-order lensing image characteristics (HOLICs) introduced by Okura, Umetsu, & Futamase. Our HOLICs formalism allows accurate measurements of flexion from practical observational data in the presence of non-circular, anisotropic point spread function. We have applied our method to ground-based Subaru observations of the massive galaxy cluster A1689 at a redshift of z = 0.183. From the high-precision measurements of spin-1 first flexion, we obtain a high-resolution mass map in the central region of A1689. The reconstructed mass map shows a bimodal feature in the central 4′ × 4′ region of the cluster. The major, pronounced mass peak is associated with the brightest cluster galaxy and central cluster members, while the secondary peak is associated with a local concentration of bright galaxies. In Fourier space we separate the reconstructed mass distribution into cluster and subhalo components, from which we obtain projected subhalo masses associated with the primary and the secondary peaks to be M1 = (2.2 ± 0.4) × 1013M⊙/h, and M2 = (1.1 ± 0.3) × 1013M⊙/h, respectively.

scholarly journals Abell 3627: A Nearby, X-Ray Bright, and Massive Galaxy Cluster

1996 ◽  
Vol 467 ◽  
pp. 168 ◽  
Author(s):  
H. Boehringer ◽  
D. M. Neumann ◽  
S. Schindler ◽  
R. C. Kraan-Korteweg
Keyword(s):  
Galaxy Cluster ◽  
X Ray ◽  
Massive Galaxy

scholarly journals FM6: Summary of Session #5 on Accretion and Feedback in Active Galactic Nuclei

2015 ◽  
Vol 11 (A29B) ◽  
pp. 101-112
Author(s):  
Laura Brenneman
Keyword(s):  
Active Galactic Nuclei ◽  
Large Scale ◽  
Galaxy Cluster ◽  
Galactic Nuclei ◽  
Starburst Galaxies ◽  
X Ray ◽  
Large Scale Structures ◽  
Scale Structures

AbstractFocus Meeting 6 of the IAU 2015 Symposium centered around the topic of “X-ray Surveys of the Hot and Energetic Universe.” Within this two-day meeting seven sessions (31 total talks) were presented, whose topics included galaxy cluster physics and evolution, cluster cosmological studies, AGN demographics and X-ray binary populations, first quasars, accretion and feedback, large-scale structures, and normal and starburst galaxies. Herein, I summarize the results presented during session #5, which focused on AGN accretion and feedback. Six authors contributed their work to our session: Laura Brenneman, Kazushi Iwasawa, Massimo Gaspari, Michaela Hirschmann, Franz Bauer and Yuan Liu. I provide a brief introduction below, followed by the details of the presentations of each author in the order in which the presentations were given.

scholarly journals ASCA Observations of a Nearby and Massive Galaxy Cluster Abell 3627

1998 ◽  
Vol 50 (2) ◽  
pp. 195-201 ◽  
Author(s):  
Takayuki Tamura ◽  
Yasushi Fukazawa ◽  
Hidehiro Kaneda ◽  
Kazuo Makishima ◽  
Makoto Tashiro ◽  
...  
Keyword(s):  
Galaxy Cluster ◽  
Massive Galaxy

scholarly journals Cluster Magnetic Fields from Large-Scale Structure and Galaxy Cluster Shocks

2006 ◽  
Vol 642 (1) ◽  
pp. L1-L4 ◽  
Author(s):  
Mikhail V. Medvedev ◽  
Luis O. Silva ◽  
Marc Kamionkowski
Keyword(s):  
Magnetic Fields ◽  
Large Scale ◽  
Galaxy Cluster ◽  
Large Scale Structure ◽  
Scale Structure

scholarly journals Low-frequency radio emission in the massive galaxy cluster MACSJ0717.5 + 3745

2013 ◽  
Vol 557 ◽  
pp. A117 ◽  
Author(s):  
M. Pandey-Pommier ◽  
J. Richard ◽  
F. Combes ◽  
K. S. Dwarakanath ◽  
B. Guiderdoni ◽  
...  
Keyword(s):  
Radio Emission ◽  
Low Frequency ◽  
Galaxy Cluster ◽  
Massive Galaxy

scholarly journals Towards a better understanding of galaxy clusters

2014 ◽  
Vol 10 (S306) ◽  
pp. 273-275
Author(s):  
Pedro T. P. Viana
Keyword(s):  
Distribution Function ◽  
Probability Distribution ◽  
Probability Distribution Function ◽  
Large Scale ◽  
Posterior Probability ◽  
Galaxy Cluster ◽  
Relevant Information ◽  
Posterior Probability Distribution ◽  
Cluster Properties ◽  
The Universe

AbstractObservational data on clusters of galaxies holds relevant information that can be used to determine the relative plausibility of different models for the large-scale evolution of the Universe, or estimate the joint posterior probability distribution function of the parameters that pertain to each model. Within the next few years, several surveys of the sky will yield large galaxy cluster catalogues. In order to make use of the vast amount of information they will contain, their selection functions will have to be properly understood. We argue this, as well as the estimation of the full joint posterior probability distribution function of the most relevant cluster properties, can be best achieved in the framework of bayesian statistics.

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