A Complete Sample of 12 Very X-Ray Luminous Galaxy Clusters at
                    <i>z</i>
                    &gt; 0.5

Ebeling, H.; Barrett, Elizabeth Ann; Donovan, David; Ma, Chien‐Ching; Edge, A. C.; Speybroeck, L. van

doi:10.1086/518603

Cited by 291 publications

(427 citation statements)

References 11 publications

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“…The X-ray luminous galaxy cluster MACS J0717.5+3745, independently observed at redshift z obs = 0.546 by the MACS survey (Ebeling et al 2001(Ebeling et al , 2007 and as a host of a diffuse radio source by Edge et al (2003), is a quite remarkable system. The cluster is connected to a 4 Mpc long large-scale filament (Ebeling et al 2004) that leads into the cluster and exhibits ongoing merging activity (Ma et al 2008).…”

Section: The Cluster Macs J07175+3745mentioning

confidence: 99%

The strongest gravitational lenses

Waizmann

Redlich

Bartelmann

2012

A&A

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Context. With the amount and quality of galaxy cluster data increasing, the question arises whether or not the standard cosmological model can be questioned on the basis of a single observed extreme galaxy cluster. Usually, the word extreme refers directly to cluster mass, which is not a direct observable and thus subject to substantial uncertainty. Hence, it is desirable to extend studies of extreme clusters to direct observables, such as the Einstein radius. Aims. We aim to evaluate the occurrence probability of the large observed Einstein radius of MACS J0717.5+3745 within the standard ΛCDM cosmology. In particular, we want to model the distribution function of the single largest Einstein radius in a given cosmological volume and to study which underlying assumptions and effects have the strongest impact on the results. Methods. We obtain this distribution by a Monte Carlo approach, based on the semi-analytic modelling of the halo population on the past lightcone. After sampling the distribution, we fit the results with the general extreme value (GEV) distribution which we use for the subsequent analysis. Results. We find that the distribution of the maximum Einstein radius is particularly sensitive to the precise choice of the halo mass function, lens triaxiality, the inner slope of the halo density profile and the mass-concentration relation. Using the distributions so obtained, we study the occurrence probability of the large Einstein radius of MACS J0717.5+3745, finding that this system is not in tension with ΛCDM. We also find that the GEV distribution can be used to fit very accurately the sampled distributions and that all of them can be described by a (type-II) Fréchet distribution. Conclusions. With a multitude of effects that strongly influence the distribution of the single largest Einstein radius, it is more than doubtful that the standard ΛCDM cosmology can be ruled out on the basis of a single observation. If, despite the large uncertainties in the underlying assumptions, one wanted to do so, a much larger Einstein radius ( > ∼ 100 ) than that of MACS J0717.5+3745 would have to be observed.

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Section: The Cluster Macs J07175+3745mentioning

confidence: 99%

The strongest gravitational lenses

Waizmann

Redlich

Bartelmann

2012

A&A

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“…MACSJ0717.5+3745 was discovered by Edge et al (2003) as part of the MAssive Cluster Survey (MACS; Ebeling et al 2001) and is located at a redshift of z=0.5458. The cluster is very hot, with a global X-ray temperature of 11.6±0.5 keV (Ebeling et al 2007). MACSJ0717.5+3745 is one of the most complex and dynamically disturbed clusters known.…”

Section: Introductionmentioning

confidence: 99%

Chandra and JVLA Observations of HST Frontier Fields Cluster MACS J0717.5+3745

Weeren

Ogrean

Jones

et al. 2017

ApJ

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To investigate the relationship between thermal and non-thermal components in merger galaxy clusters, we present deep JVLA and Chandraobservations of the HST Frontier Fields cluster MACSJ0717.5+3745. The Chandraimage shows a complex merger event, with at least four components belonging to different merging subclusters. Northwestof the cluster, ∼0.7 Mpc from the center, there is a ram-pressure-stripped core that appears to have traversed the densest parts of the cluster after entering the intracluster medium (ICM) from the direction of a galaxy filament to the southeast. We detect a density discontinuity north-northeastof this core, which we speculate is associated with a cold front. Our radio images reveal new details for the complex radio relic and radio halo in this cluster. In addition, we discover several new filamentary radio sources with sizes of 100-300kpc. A few of these seem to be connected to the main radio relic, while others are either embedded within the radio halo or projected onto it. A narrow-angled-tailed (NAT) radio galaxy, a cluster member, is located at the center of the radio relic. The steep spectrum tails of this active galactic nucleuslead into the large radio relic where the radio spectrum flattens again. This morphological connection between the NAT radio galaxy and relic provides evidence for reacceleration (revival) of fossil electrons. The presence of hot 20 keV ICM gas detected by Chandranear the relic location provides additional support for this re-acceleration scenario.

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“…This spiral arm is distorted into an Einstein ring by the gravitational potential of a foreground elliptical galaxy. That elliptical galaxy lens also resides within MACS J1149.6+2223, a strong-lensing galaxy cluster at z=0.54 that is fast becoming one of the crown jewels of the Massive Cluster Survey  (Ebeling et al 2001(Ebeling et al , 2007. The galactic-scale lens, augmented by the cluster lens, causes SNRefsdal to appear to us as four images with separations of ∼2″, arranged in an "Einstein Cross" configuration (see Figure 1) reminiscent of the quadruplyimaged quasar that originated this term (Huchra et al 1985;Adam et al 1989).…”

Section: Introductionmentioning

confidence: 99%

Sn Refsdal: Photometry and Time Delay Measurements of the First Einstein Cross Supernova

Rodney

Strolger

Kelly

et al. 2016

ApJ

102

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We present the first year of Hubble Space Telescope imaging of the unique supernova (SN) "Refsdal," a gravitationally lensed SN at z=1.488±0.001 with multiple images behind the galaxy cluster MACS J1149.6 +2223. The first four observed images of SN Refsdal (images S1-S4) exhibited a slow rise (over ∼150 days) to reach a broad peak brightness around 2015 April 20. Using a set of light curve templates constructed from SN 1987A-like peculiar Type II SNe, we measure time delays for the four images relative to S1 of 4±4 (for S2), 2±5 (S3), and 24±7 days (S4). The measured magnification ratios relative to S1 are 1.15±0.05 (S2), 1.01±0.04 (S3), and 0.34±0.02 (S4). None of the template light curves fully captures the photometric behavior of SN Refsdal, so we also derive complementary measurements for these parameters using polynomials to represent the intrinsic light curve shape. These more flexible fits deliver fully consistent time delays of 7±2 (S2), 0.6±3 (S3), and 27±8 days (S4). The lensing magnification ratios are similarly consistent, measured as 1.17±0.02 (S2), 1.00±0.01 (S3), and 0.38±0.02 (S4). We compare these measurements against published predictions from lens models, and find that the majority of model predictions are in very good agreement with our measurements. Finally, we discuss avenues for future improvement of time delay measurements-both for SN Refsdal and for other strongly lensed SNe yet to come.

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A Complete Sample of 12 Very X-Ray Luminous Galaxy Clusters at z > 0.5

Cited by 291 publications

References 11 publications

The strongest gravitational lenses

The strongest gravitational lenses

Chandra and JVLA Observations of HST Frontier Fields Cluster MACS J0717.5+3745

Sn Refsdal: Photometry and Time Delay Measurements of the First Einstein Cross Supernova

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