Distant Cluster Hunting. II. A Comparison of X‐Ray and Optical Cluster Detection Techniques and Catalogs from the<i>ROSAT</i>Optical X‐Ray Survey

Donahue, M.; Scharf, Caleb; Mack, J.; Lee, Y. Paul; Postman, Marc; Rosati, P.; Dickinson, Mark; Voit, G. Mark; Stocke, John T.

doi:10.1086/339401

Cited by 68 publications

(86 citation statements)

References 54 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Moreover, using the RASS-SDSS galaxy cluster catalogue, Popesso et al (2004) show that a distinct class of "X-ray underluminous Abell clusters" does exist, with an X-ray luminosity L X that is one order of magnitude fainter than that expected for their mass according to the typical L X -mass relation (Popesso et al 2007a). This supports the concern of Donahue et al (2002) about the possible existence of biases in catalogues selected in different wavebands.…”

Section: Introductionsupporting

confidence: 79%

“…For example, it was shown by the first joint X-ray/optical survey (Donahue et al 2002) that only ∼20% of optically selected clusters appeared to be identifiable in X-rays, while ∼60% of the X-ray clusters were included in the optical sample. Understanding the possible selection effects hidden behind the different survey strategies is crucial to explain the small size of the overlap between the two different cluster catalogues (see for example Ledlow et al 2003;Gilbank et al 2004).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The VIMOS-VLT deep survey: the group catalogue

Cucciati

Marinoni

Iovino³

et al. 2010

A&A

View full text Add to dashboard Cite

Aims. We present a homogeneous and complete catalogue of optical galaxy groups identified in the purely flux-limited (17.5 ≤ I AB ≤ 24.0) VIMOS-VLT deep redshift Survey (VVDS). Methods. We use mock catalogues extracted from the Millennium Simulation, to correct for potential systematics that might affect the overall distribution as well as the individual properties of the identified systems. Simulated samples allow us to forecast the number and properties of groups that can be potentially found in a survey with VVDS-like selection functions. We use them to correct for the expected incompleteness and, to asses in addition, how well galaxy redshifts trace the line-of-sight velocity dispersion of the underlying mass overdensity. In particular, on these mock catalogues we train the adopted group-finding technique i.e., the Voronoi-Delaunay Method (VDM). The goal is to fine-tune its free parameters, recover in a robust and unbiased way the redshift and velocity dispersion distributions of groups (n(z) and n(σ), respectively), and maximize, at the same time, the level of completeness and purity of the group catalogue. Results. We identify 318 VVDS groups with at least 2 members in the range 0.2 ≤ z ≤ 1.0, among which 144 (/30) with at least 3 (/5) members. The sample has an overall completeness of ∼60% and a purity of ∼50%. Nearly 45% of the groups with at least 3 members are still recovered if we run the algorithm with a particular parameter set that maximizes the purity (∼75%) of the resulting catalogue. We use the group sample to explore the redshift evolution of the fraction f b of blue galaxies (U − B ≤ 1) in the redshift range 0.2 ≤ z ≤ 1. We find that the fraction of blue galaxies is significantly lower in groups than in the global population (i.e. in the whole ensemble of galaxies irrespective of their environment). Both of these quantities increase with redshift, the fraction of blue galaxies in groups exhibiting a marginally significant steeper increase. We also investigate the dependence of f b on group richness: not only we confirm that, at any redshift, the blue fraction decreases in systems with increasing richness, but we find that this result continues to hold towards fainter luminosities.

show abstract

Section: Introductionsupporting

confidence: 79%

Section: Introductionmentioning

confidence: 99%

The VIMOS-VLT deep survey: the group catalogue

Cucciati

Marinoni

Iovino³

et al. 2010

A&A

View full text Add to dashboard Cite

show abstract

“…Vikhlinin et al (1998), on whose 160d ROSAT catalogue the 400d sample builds (cf. Burenin et al 2007) detect four clusters in the field: VMF 189 (A 2246), VMF 190 (CL 1701+6414), VMF 191,and VMF 192. In an independent ROSAT analysis, Donahue et al (2002) detect these same four clusters plus RX J1702+6407, which we do not detect in WL. The redshift of z = 0.7 found for the Donahue et al (2002) optical counterpart of CL 1701+6414 deviates from the redshift of z = 0.45 measured by Burenin et al (2007) and all other references.…”

Section: Appendix A: Photometric Calibration Detailscontrasting

confidence: 43%

The 400d Galaxy Cluster Survey weak lensing programme

Israel¹,

Erben²,

Reiprich³

et al. 2012

A&A

View full text Add to dashboard Cite

Context. Evolution in the mass function of galaxy clusters sensitively traces both the expansion history of the Universe and cosmological structure formation. Robust cluster mass determinations are a key ingredient for a reliable measurement of this evolution, especially at high redshift. Weak gravitational lensing is a promising tool for, on average, unbiased mass estimates. Aims. This weak lensing project aims at measuring reliable weak lensing masses for a complete X-ray selected sample of 36 high redshift (0.35 < z < 0.9) clusters. The goal of this paper is to demonstrate the robustness of the methodology against commonly encountered problems, including pure instrumental effects, the presence of bright (8-9 mag) stars close to the cluster centre, ground based measurements of high-z (z ∼ 0.8) clusters, and the presence of massive unrelated structures along the line-sight. Methods. We select a subsample of seven clusters observed with MMT/MegaCam. Instrumental effects are checked in detail by cross-comparison with an archival CFHT/MegaCam observation. We derive mass estimates for seven clusters by modelling the tangential shear with an NFW profile, in two cases with multiple components to account for projected structures in the line-of-sight. Results. We firmly detect lensing signals from all seven clusters at more than 3.5σ and determine their masses, ranging from 10 14 M to 10 15 M , despite the presence of nearby bright stars. We retrieve the lensing signal of more than one cluster in the CL 1701+6414 field, while apparently observing CL 1701+6414 through a massive foreground filament. We also find a multi-peaked shear signal in CL 1641+4001. Shear structures measured in the MMT and CFHT images of CL 1701+6414 are highly correlated. Conclusions. We confirm the capability of MMT/MegaCam to infer weak lensing masses from high-z clusters, demonstrated by the high level of consistency between MMT and CFHT results for CL 1701+6414. This shows that, when a sophisticated analysis is applied, instrumental effects are well under control.

show abstract

“…From its application to the SDSS, they produced a "CE cluster catalog" that included different galaxy density profiles, luminosity functions, and clusters dominated by either spirals or faint ellipticals. Additionally, Donahue et al (2002) have suggested that the CRS could be characteristic of massive clusters only (e.g., Aguerri et al 2007;Ascaso et al 2012). …”

Section: Introductionmentioning

confidence: 99%

A 3D Voronoi+Gapper Galaxy Cluster Finder in Redshift Space to z ∼ 0.2 I: an Algorithm Optimized for the 2dFGRS

Pereira

Campusano

Hitschfeld

et al. 2017

ApJ

View full text Add to dashboard Cite

This paper is the first in a series, presenting a new galaxy cluster finder based on a three-dimensional Voronoi Tesselation plus a maximum likelihood estimator, followed by gapping-filtering in radial velocity(VoML+G). The scientific aim of the series is a reassessment of the diversity of optical clusters in the local universe. A mock galaxy database mimicking the southern strip of the magnitude(blue)-limited 2dF Galaxy Redshift Survey (2dFGRS), for the redshift range 0.009<z<0.22, is built on the basis of the Millennium Simulation of the LCDM cosmology and a reference catalog of "Millennium clusters," spannning across the 1.0×1012 -1.0×1015 M e h −1 dark matter (DM) halo mass range, is recorded. The validation of VoML+G is performed through its application to the mock data and the ensuing determination of the completeness and purity of the cluster detections by comparison with the reference catalog. The execution of VoML+G over the 2dFGRS mock data identified 1614 clusters, 22% with N g 10, 64 percent with 10>N g 5, and 14% with N g <5. The ensemble of VoML+G clusters has a ∼59% completeness and a ∼66% purity, whereas the subsample with N g 10, to z∼0.14, has greatly improved mean rates of ∼75% and ∼90%, respectively. The VoML+G cluster velocity dispersions are found to be compatible with those corresponding to "Millennium clusters" over the 300-1000 km s −1 interval, i.e., for cluster halo masses in excess of ∼3.0×1013 M e h −1 .

show abstract

Distant Cluster Hunting. II. A Comparison of X‐Ray and Optical Cluster Detection Techniques and Catalogs from theROSATOptical X‐Ray Survey

Cited by 68 publications

References 54 publications

The VIMOS-VLT deep survey: the group catalogue

The VIMOS-VLT deep survey: the group catalogue

The 400d Galaxy Cluster Survey weak lensing programme

A 3D Voronoi+Gapper Galaxy Cluster Finder in Redshift Space to z ∼ 0.2 I: an Algorithm Optimized for the 2dFGRS

Contact Info

Product

Resources

About