Flaming, bright galaxies along the filaments of A 2744

Braglia, F. G.; Pierini, D.; Böhringer, H.

doi:10.1051/0004-6361:20077257

Cited by 42 publications

(66 citation statements)

References 44 publications

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“…4. A filament is a low density environment and as such is dominated by blue late-type galaxies (Braglia et al 2007). We found that 12 of the 14 galaxies inside r 200 brighter than L * are on the cluster red-sequence.…”

Section: Discussionmentioning

confidence: 99%

Weak lensing observations of potentially X-ray underluminous galaxy clusters

Biviano

Popesso

Zhang³

et al. 2009

A&A

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Optically selected clusters of galaxies display a relation between their optical mass estimates and their X-ray luminosities L X that has a large scatter. A substantial fraction of optically selected clusters have L X estimates or upper limits significantly below the values expected from the L X -mass relation established for X-ray selected clusters, i.e., these clusters are X-ray underluminous for their mass. We attempt to confirm or falsify the X-ray underluminous nature of two clusters, Abell 315 and Abell 1456, by using weak gravitational lensing as a third and independent measure of the clusters' masses. We obtained optical wide-field imaging data and selected background galaxies using their colors and measured the shear exerted by the tidal field of the foreground galaxy clusters. We then fitted parametrized models to our shear catalogs. After accounting for projections of large-scale structure and halo triaxiality, we find that A 315 is significantly X-ray underluminous for its mass, while no significant lensing signal was detected for A 1456. We re-evaluate earlier kinematic and X-ray analyses of these two clusters and discuss the nature of the X-ray underluminous cluster A 315 and why A 1456 was probably erroneously identified as being X-ray underluminous.

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Section: Discussionmentioning

confidence: 99%

Weak lensing observations of potentially X-ray underluminous galaxy clusters

Biviano

Popesso

Zhang³

et al. 2009

A&A

Self Cite

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“…Red galaxies with low levels of ongoing star formation are assumed to be the descendants of blue star-forming galaxies that have been accreted from the surrounding filamentary structure and quenched by specific processes operating within the cluster environment (e.g. Braglia et al 2007;Verdugo et al 2012). How spirals were transformed into ellipticals remains unclear (e.g.…”

Section: Blue-galaxy Fractionmentioning

confidence: 99%

Probing cluster dynamics in RXC J1504.1-0248 via radial and two-dimensional gas and galaxy properties

Zhang

Verdugo

Klein

et al. 2012

A&A

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We study one of the most X-ray luminous cluster of galaxies in the REFLEX survey, RXC J1504.1-0248 (hereafter R1504; z cl = 0.2153), using XMM-Newton X-ray imaging spectroscopy, VLT/VIMOS optical spectroscopy, and WFI optical imaging. The mass distributions were determined using both the so-called hydrostatic method with X-ray imaging spectroscopy and the dynamical method with optical spectroscopy, respectively, which yield M H.E. 500 = (5.81 ± 0.49) × 10 14 M and M caustic 500 = (4.17 ± 0.42) × 10 14 M . According to recent calibrations, the richness-derived mass estimates closely agree with the hydrostatic and dynamical mass estimates. The line-of-sight velocities of spectroscopic members reveal a group of galaxies with high velocities (>1000 km s −1 ) at a projected distance of about r H.E. 500 = (1.18 ± 0.03) Mpc south-east of the cluster centroid, which is also indicated in the X-ray two-dimensional (2D) temperature, density, entropy, and pressure maps. The dynamical mass estimate is 80% of the hydrostatic mass estimate at r H.E. 500 . It can be partially explained by the ∼20% scatter in the 2D pressure map that can be propagated into the hydrostatic mass estimate. The uncertainty in the dynamical mass estimate caused by the substructure of the high velocity group is ∼14%. The dynamical mass estimate using blue members is 1.23 times that obtained using red members. The global properties of R1504 obey the observed scaling relations of nearby clusters, although its stellar-mass fraction is rather low.

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“…The precise lensing mass distribution has been determined by utilizing the deepest HST data from the Frontier Fields program Wang et al 2015). Large-scale galaxy filaments in the south and northwest directions were first noted by Braglia et al (2007). Spectroscopically identified 343 member galaxies within 3 Mpc from the cluster center were catalogued by Owers et al (2011), with which a galaxy concentration in the east-northeast was also recognized.…”

Section: Introductionmentioning

confidence: 99%

Search for the warm–hot intergalactic medium around A 2744 using Suzaku

Hattori

Ota

Zhang

et al. 2017

Publications of the Astronomical Society of Japan

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We present the results from the Suzaku satellite of the surrounding region of a galaxy cluster, A2744, at z = 0.3. To search for oxygen emission lines from the warm-hot intergalactic medium (WHIM), we analyzed X-ray spectra from two northeast regions 2.2-3.3 and 3.3-4.4 Mpc from the center of the cluster, which offers the first test on the presence of a WHIM near the typical accretion shock radius (∼ 2r 200 ) predicted by hydrodynamical simulations. For the 2.2-3.3 Mpc region, the spectral fit significantly (99.2% significance) improved when we include O VII and O VIII lines in the spectral model. A comparable WHIM surface brightness was obtained in the 3.3-4.4 Mpc region and the redshift of O VIII line is consistent with z = 0.3 within errors. The present results support that the observed soft X-ray emission originated from the WHIM. However, considering both statistical and systematic uncertainties, O VIII detection in the northeast regions was marginal. The surface brightness of the O VIII line in 10 −7 photons cm −2 s −1 arcmin −2 was measured to be 2.7 ± 1.0, 2.1 ± 1.2 for the 2.2-3.3, 3.3-4.4 Mpc regions, giving the upper limit on the baryon overdensity of δ = 319(< 443), 283(< 446), respectively. This is comparable with previous observations of cluster outskirts and their theoretical predictions. The future prospect for WHIM detection using the Athena X-IFU microcalorimeter is briefly discussed here. In addition, we also derived the ICM temperature distribution of A2744 to detect a clear discontinuity at the location of the radio relic. This suggests that the cluster has undergone strong shock heating by mass accretion along the filament.

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Flaming, bright galaxies along the filaments of A 2744

Cited by 42 publications

References 44 publications

Weak lensing observations of potentially X-ray underluminous galaxy clusters

Weak lensing observations of potentially X-ray underluminous galaxy clusters

Probing cluster dynamics in RXC J1504.1-0248 via radial and two-dimensional gas and galaxy properties

Search for the warm–hot intergalactic medium around A 2744 using Suzaku

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