The ROSAT Brightest Cluster Sample — IV. The extended sample

Ebeling, H.; Edge, A. C.; Allen, S. W.; Crawford, C. S.; Fabian, A. C.; Huchra, J. P.

doi:10.1046/j.1365-8711.2000.03549.x

Cited by 352 publications

(420 citation statements)

References 40 publications

Supporting

Mentioning

415

Contrasting

Order By: Relevance

“…The sample comprises 50 clusters (Table 1) drawn from the ROSAT All Sky Survey cluster catalogues (Ebeling et al 1998(Ebeling et al , 2000Böhringer et al 2004) that satisfy the criteria: −25 • < δ < +65 • , nH 7 × 10 20 cm −2 , 0.15 z 0.3, LX /E(z) > 4.1 × 10 44 erg s −1 where LX is in the 0.1 − 2.4 keV band and E(z) = ΩM (1 + z) 3 + ΩΛ. The sample is X-ray luminosity-limited, and therefore approximately mass-limited.…”

Section: Samplementioning

confidence: 99%

LoCuSS: weak-lensing mass calibration of galaxy clusters

Okabe

Smith

2016

Mon. Not. R. Astron. Soc.

152

179

View full text Add to dashboard Cite

We present weak-lensing mass measurements of 50 X-ray luminous galaxy clusters at 0.15 z 0.3, based on uniform high quality observations with Suprime-Cam mounted on the 8.2-m Subaru telescope. We pay close attention to possible systematic biases, aiming to control them at the ∼ < 4 per cent level. The dominant source of systematic bias in weak-lensing measurements of the mass of individual galaxy clusters is contamination of background galaxy catalogues by faint cluster and foreground galaxies. We extend our conservative method for selecting background galaxies with (V − i ′ ) colours redder than the red sequence of cluster members to use a colour-cut that depends on cluster-centric radius. This allows us to define background galaxy samples that suffer 1 per cent contamination, and comprise 13 galaxies per square arcminute. Thanks to the purity of our background galaxy catalogue, the largest systematic that we identify in our analysis is a shape measurement bias of 3 per cent, that we measure using simulations that probe weak shears upto g = 0.3. Our individual cluster mass and concentration measurements are in excellent agreement with predictions of the mass-concentration relation. Equally, our stacked shear profile is in excellent agreement with the Navarro Frenk and White profile. Our new LoCuSS mass measurements are consistent with the CCCP and CLASH surveys, and in tension with the Weighing the Giants at ∼ 1 − 2σ significance. Overall, the consensus at z 0.3 that is emerging from these complementary surveys represents important progress for cluster mass calibration, and augurs well for cluster cosmology.

show abstract

Section: Samplementioning

confidence: 99%

LoCuSS: weak-lensing mass calibration of galaxy clusters

Okabe

Smith

2016

Mon. Not. R. Astron. Soc.

152

179

View full text Add to dashboard Cite

show abstract

“…The sample of BCGs presented in this work was extracted from the EGRHS (V07, V08, K13, and K15), which consists of galaxy clusters selected from the ROSAT-ESO flux-limited X-ray (REFLEX) galaxy cluster catalogue (Böhringer et al 2004) and from the extended ROSAT Brightest Cluster Sample (EBCS) catalogue (Ebeling et al 1998(Ebeling et al , 2000 according to the following criteria:…”

Section: Bcg Samplementioning

confidence: 99%

Brightest cluster galaxies in the extended GMRT radio halo cluster sample

Kale

Venturi

Cassano

et al. 2015

A&A

View full text Add to dashboard Cite

Aims. First-ranked galaxies in clusters, usually referred to as brightest cluster galaxies (BCGs), show exceptional properties over the whole electromagnetic spectrum. They are the most massive elliptical galaxies and show the highest probability to be radio loud. Moreover, their special location at the centres of galaxy clusters raises the question of the role of the environment in shaping their radio properties. In the attempt to separate the effect of the galaxy mass and of the environment on their statistical radio properties, we investigate the possible dependence of the occurrence of radio loudness and of the fractional radio luminosity function on the dynamical state of the hosting cluster. Methods. We studied the radio properties of the BCGs in the Extended GMRT Radio Halo Survey (EGRHS), which consists of 65 clusters in the redshift range 0.2-0.4, with X-ray luminosity L X ≥ 5 × 10 44 erg s −1 , and quantitative information on their dynamical state from high-quality Chandra imaging. We obtained a statistical sample of 59 BCGs, which we divided into two classes, depending on whether the dynamical state of the host cluster was merging (M) or relaxed (R). Results. Of the 59 BCGs, 28 are radio loud and 31 are radio quiet. The radio-loud sources are favourably located in relaxed clusters (71%), while the reverse is true for the radio-quiet BCGs, which are mostly located in merging systems (81%). The fractional radio luminosity function for the BCGs in merging and relaxed clusters is different, and it is considerably higher for BCGs in relaxed clusters, where the total fraction of radio loudness reaches almost 90%, to be compared to the ∼30% in merging clusters. For relaxed clusters, we found a positive correlation between the radio power of the BCGs and the strength of the cool core, consistent with previous studies on local samples. Conclusions. Our study suggests that the radio loudness of the BCGs strongly depends on the cluster dynamics; their fraction is considerably higher in relaxed clusters. We compare our results with similar investigations and briefly discuss them in the framework of AGN feedback.

show abstract

“…For the present comparison, we chose to use published results from LoCuSS, which is an all-sky X-ray-selected sample of 100 massive galaxy clusters at 0.1 < z < 0.3 drawn from the REFLEX (Böhringer et al 2004) and eBCS (Ebeling et al 2000) catalogues, for which gravitational lensing data from the Hubble Space Telescope and Subaru Telescope are being accumulated. At the time of writing, relevant data from only part of the full sample have been published, as detailed below.…”

Section: Sample Selection and Data Setsmentioning

confidence: 99%

Planckintermediate results

Ade¹,

Aghanim²,

Arnaud³

et al. 2013

A&A

View full text Add to dashboard Cite

We examine the relation between the galaxy cluster mass M and Sunyaev-Zeldovich (SZ) effect signal D 2 A Y 500 for a sample of 19 objects for which weak lensing (WL) mass measurements obtained from Subaru Telescope data are available in the literature. Hydrostatic X-ray masses are derived from XMM-Newton archive data, and the SZ effect signal is measured from Planck all-sky survey data. We find an M WL −D 2 A Y 500 relation that is consistent in slope and normalisation with previous determinations using weak lensing masses; however, there is a normalisation offset with respect to previous measures based on hydrostatic X-ray mass-proxy relations. We verify that our SZ effect measurements are in excellent agreement with previous determinations from Planck data. For the present sample, the hydrostatic X-ray masses at R 500 are on average ∼20 percent larger than the corresponding weak lensing masses, which is contrary to expectations. We show that the mass discrepancy is driven by a difference in mass concentration as measured by the two methods and, for the present sample, that the mass discrepancy and difference in mass concentration are especially large for disturbed systems. The mass discrepancy is also linked to the offset in centres used by the X-ray and weak lensing analyses, which again is most important in disturbed systems. We outline several approaches that are needed to help achieve convergence in cluster mass measurement with X-ray and weak lensing observations.

show abstract

The ROSAT Brightest Cluster Sample — IV. The extended sample

Cited by 352 publications

References 40 publications

LoCuSS: weak-lensing mass calibration of galaxy clusters

LoCuSS: weak-lensing mass calibration of galaxy clusters

Brightest cluster galaxies in the extended GMRT radio halo cluster sample

Planckintermediate results

Contact Info

Product

Resources

About