ERRATUM: “GALAXY CLUSTERS IDENTIFIED FROM THE SLOAN DIGITAL SKY SURVEY DR6 AND THEIR PROPERTIES” (2009, ApJS, 183, 197)

Wen, Z. L.; Han, J. L.; Liu, F. S.

doi:10.1088/0067-0049/187/1/272

Cited by 37 publications

(97 citation statements)

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“…The columns "X-ray" and distance show a flux of X-ray in the literature and a positional difference between detected peak and X-ray source. a WHO: (Wen et al 2009(Wen et al , 2010. b 1WGA: ftp://cdsarc.u-strasbg.fr/cats/IX/30/ReadMe.…”

Section: Comparison With Earlier Resultsmentioning

confidence: 99%

Reducing Systematic Error in Weak Lensing Cluster Surveys

Utsumi¹,

Miyazaki²,

Geller³

et al. 2014

ApJ

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Weak lensing provides an important route toward collecting samples of clusters of galaxies selected by mass. Subtle systematic errors in image reduction can compromise the power of this technique. We use the B-mode signal to quantify this systematic error and to test methods for reducing this error. We show that two procedures are efficient in suppressing systematic error in the B-mode:(1) refinement of the mosaic CCD warping procedure to conform to absolute celestial coordinates and (2) truncation of the smoothing procedure on a scale of 10 . Application of these procedures reduces the systematic error to 20% of its original amplitude. We provide an analytic expression for the distribution of the highest peaks in noise maps that can be used to estimate the fraction of false peaks in the weak-lensing κ-signal-to-noise ratio (S/N) maps as a function of the detection threshold. Based on this analysis, we select a threshold S/N = 4.56 for identifying an uncontaminated set of weak-lensing peaks in two test fields covering a total area of ∼3 deg 2 . Taken together these fields contain seven peaks above the threshold. Among these, six are probable systems of galaxies and one is a superposition. We confirm the reliability of these peaks with dense redshift surveys, X-ray, and imaging observations. The systematic error reduction procedures we apply are general and can be applied to future large-area weak-lensing surveys. Our high-peak analysis suggests that with an S/N threshold of 4.5, there should be only 2.7 spurious weak-lensing peaks even in an area of 1000 deg 2 , where we expect ∼2000 peaks based on our Subaru fields.

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Section: Comparison With Earlier Resultsmentioning

confidence: 99%

Reducing Systematic Error in Weak Lensing Cluster Surveys

Utsumi¹,

Miyazaki²,

Geller³

et al. 2014

ApJ

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“…5). A galaxy cluster WHLJ083744.3+145247 with a photometric redshift 0.2875 is co-spatial with these galaxies (Wen et al 2009(Wen et al , 2010. No X-ray source is known at this location.…”

Section: A Complex Blend Of Radio Sources and A Galaxy Filament?mentioning

confidence: 89%

The Extended GMRT Radio Halo Survey

Kale

Venturi

Giacintucci

et al. 2013

A&A

122

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Context. A fraction of galaxy clusters host diffuse radio sources called radio halos, radio relics and mini-halos. These are associated with the relativistic electrons and magnetic fields present on ∼Mpc scales in the intra-cluster medium. Aims. We aim to carry out a systematic radio survey of all luminous galaxy clusters selected from the REFLEX and eBCS X-ray catalogues with the Giant Metrewave Radio Telescope, to understand the statistical properties of the diffuse radio emission in galaxy clusters. Methods. We present the sample and first results from the Extended GMRT Radio Halo Survey (EGRHS), which is an extension of the GMRT Radio Halo Survey (GRHS, Venturi et al. 2007. Analysis of radio data at 610/ 235/ 325 MHz on 12 galaxy clusters are presented. Results. We report the detection of a newly discovered mini-halo in the cluster RX J1532.9+3021 at 610 MHz. The presence of a small-scale relic (∼200 kpc) is suspected in the cluster Z348. We do not detect cluster-scale diffuse emission in 11 clusters. Robust upper limits on the detection of radio halo of size of 1 Mpc are determined. We also present upper limits on the detections of minihalos in a sub-sample of cool-core clusters. The upper limits for radio halos and mini-halos are plotted in the radio power-X-ray luminosity plane and the correlations are discussed. Diffuse extended emission that is not related to the target clusters, but detected as by-products in the sensitive images of two of the cluster fields (A689 and RX J0439.0+0715) is also reported. Conclusions. Based on the information about the presence of radio halos (or upper limits), available on 48 clusters out of the total sample of 67 clusters (EGRHS+GRHS), we find that 23±7% of the clusters host radio halos. The radio halo fraction rises to 31±11%, when only the clusters with X-ray luminosities >8 × 10 44 erg s −1 are considered. Mini-halos are found in ∼50% of cool-core clusters. A qualitative examination of the X-ray images of the clusters with no diffuse radio emission indicates that a majority of these clusters do not show extreme dynamical disturbances and supports the idea that mergers play an important role in generating radio halos and relics. The analysis of the full sample will be presented in a future work.

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“…There is a galaxy brighter than the chosen BCG and coincident to the X-ray position, but with velocity offset equal to 3868.2 km s −1 . This is the BCG of the background cluster WHL J135915.1+275834, with photometric redshift z phot = 0.0746 (Wen et al 2010). Its BCG has redshift z = 0.0759.…”

Section: Appendix C: Notes On Individual Clustersmentioning

confidence: 99%

Optical substructure and BCG offsets of Sunyaev–Zel’dovich and X-ray-selected galaxy clusters

Lopes

Trevisan

Laganá

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We used optical imaging and spectroscopic data to derive substructure estimates for local Universe (z < 0.11) galaxy clusters from two different samples. The first was selected through the Sunyaev-Zel'dovich (SZ) effect by the Planck satellite and the second is an X-ray selected sample. In agreement to X-ray substructure estimates we found that the SZ systems have a larger fraction of substructure than the X-ray clusters. We have also found evidence that the higher mass regime of the SZ clusters, compared to the X-ray sample, explains the larger fraction of disturbed objects in the Planck data. Although we detect a redshift evolution in the substructure fraction, it is not sufficient to explain the different results between the higher-z SZ sample and the X-ray one. We have also verified a good agreement (∼60%) between the optical and X-ray substructure estimates. However, the best level of agreement is given by the substructure classification given by measures based on the brightest cluster galaxy (BCG), either the BCG−X-ray centroid offset, or the magnitude gap between the first and second BCGs. We advocate the use of those two parameters as the most reliable and cheap way to assess cluster dynamical state. We recommend an offset cut of ∼0.01×R 500 to separate relaxed and disturbed clusters. Regarding the magnitude gap the separation can be done at ∆m 12 = 1.0. The central galaxy paradigm (CGP) may not be valid for ∼20% of relaxed massive clusters. This fraction increases to ∼60% for disturbed systems.

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ERRATUM: “GALAXY CLUSTERS IDENTIFIED FROM THE SLOAN DIGITAL SKY SURVEY DR6 AND THEIR PROPERTIES” (2009, ApJS, 183, 197)

Cited by 37 publications

References 0 publications

Reducing Systematic Error in Weak Lensing Cluster Surveys

Reducing Systematic Error in Weak Lensing Cluster Surveys

The Extended GMRT Radio Halo Survey

Optical substructure and BCG offsets of Sunyaev–Zel’dovich and X-ray-selected galaxy clusters

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