The REFLEX galaxy cluster survey

Schuecker, P.; Böhringer, H.; Collins, Chris; Guzzo, L.

doi:10.1051/0004-6361:20021715

Cited by 194 publications

(218 citation statements)

References 60 publications

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“…The second simulation followed the evolution of 512 3 % 1:34 ; 10 8 particles in the same cosmology but in a 80 h À1 Mpc % 114:29 Mpc box and with a power spectrum normalization of 8 ¼ 0:75. This normalization is suggested by several recent measurements (e.g., Borgani et al 2001;Pierpaoli et al 2001;Lahav et al 2002;Schuecker et al 2003;Jarvis et al 2003).…”

Section: Simulationsmentioning

confidence: 81%

The Dark Side of the Halo Occupation Distribution

Kravtsov

Berlind

Wechsler

et al. 2004

ApJ

894

1,183

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We analyze the halo occupation distribution (HOD) and two-point correlation function of galaxy-size dark matter halos using high-resolution dissipationless simulations of the concordance flat ÃCDM model. The halo samples include both the host halos and the ''subhalos,'' distinct gravitationally bound halos within the virialized regions of larger host systems. We find that the HOD, the probability distribution for a halo of mass M to host a number of subhalos N, is similar to that found in semianalytic and N-body+gasdynamics studies. Its first moment, hN i M , has a complicated shape consisting of a step, a shoulder, and a power-law high-mass tail. The HOD can be described by Poisson statistics at high halo masses but becomes sub-Poisson for hN i M P 4. We show that the HOD can be understood as a combination of the probability for a halo of mass M to host a central galaxy and the probability to host a given number N s of satellite galaxies. The former can be approximated by a steplike function, while the latter can be well approximated by a Poisson distribution, fully specified by its first moment. The first moment of the satellite HOD can be well described by a simple power law hN s i / M with % 1 for a wide range of number densities, redshifts, and different power spectrum normalizations. This formulation provides a simple but accurate model for the halo occupation distribution found in simulations. At z ¼ 0, the twopoint correlation function (CF) of galactic halos can be well fitted by a power law down to $100 h À1 kpc with an amplitude and slope similar to those of observed galaxies. The dependence of correlation amplitude on the number density of objects is in general agreement with results from the Sloan Digital Sky Survey. At redshifts z k 1, we find significant departures from the power-law shape of the CF at small scales, where the CF steepens because of a more pronounced one-halo component. The departures from the power law may thus be easier to detect in high-redshift galaxy surveys than at the present-day epoch. They can be used to put useful constraints on the environments and formation of galaxies. If the deviations are as strong as indicated by our results, the assumption of the single power law often used in observational analyses of high-redshift clustering is dangerous and is likely to bias the estimates of the correlation length and slope of the correlation function.

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Section: Simulationsmentioning

confidence: 81%

The Dark Side of the Halo Occupation Distribution

Kravtsov

Berlind

Wechsler

et al. 2004

ApJ

894

1,183

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“…X-ray) permit a complete census of clusters covering a wide range of masses and redshifts, and survey data themselves can provide estimates of the mass of these objects. This is why large surveys in the X-ray wavelengths aimed at constraining cosmology with galaxy clusters have been developed since the early years of X-ray astronomy (Jones & Forman 1984;Henry & Arnaud 1991;Bahcall & Cen 1993), with a notable stepchange brought about by the ROSAT all-sky survey (RASS; Ebeling et al 2000;Ikebe et al 2002;Schuecker et al 2003) and ROSAT serendipitous surveys (Rosati et al 1998;Romer et al 2000;Burke et al 2003;Burenin et al 2007) and the support of Chandra and XMM-Newton (Pacaud et al 2006;Vikhlinin et al 2009;Finoguenov et al 2010;Mantz et al 2010;Clerc et al 2014;Pierre et al 2016). The next major advance in the field will be offered by eROSITA (extended ROentgen Survey with an Imaging Telescope Array; Predehl et al 2014) which will survey the entire sky in the 0.3-10 keV energy range at depths 10-30 times deeper than ROSAT.…”

Section: Introductionmentioning

confidence: 99%

SPIDERS: the spectroscopic follow-up of X-ray-selected clusters of galaxies in SDSS-IV

Clerc

Merloni

Zhang

et al. 2016

Mon. Not. R. Astron. Soc.

105

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SPIDERS (The SPectroscopic IDentification of eROSITA Sources) is a programme dedicated to the homogeneous and complete spectroscopic follow-up of X-ray active galactic nuclei and galaxy clusters over a large area (∼7500 deg 2 ) of the extragalactic sky. SPIDERS is part of the Sloan Digital Sky Survey (SDSS)-IV project, together with the Extended Baryon Oscillation Spectroscopic Survey and the Time-Domain Spectroscopic Survey. This paper describes the largest project within SPIDERS before the launch of eROSITA: an optical spectroscopic survey of X-ray-selected, massive (∼10 14 -10 15 M ) galaxy clusters discovered in ROSAT and XMMNewton imaging. The immediate aim is to determine precise ( z ∼ 0.001) redshifts for 4000-5000 of these systems out to z ∼ 0.6. The scientific goal of the program is precision cosmology, using clusters as probes of large-scale structure in the expanding Universe. We present the cluster samples, target selection algorithms and observation strategies. We demonstrate the efficiency of selecting targets using a combination of SDSS imaging data, a robust red-sequence finder and a dedicated prioritization scheme. We describe a set of algorithms and workflow developed to collate spectra and assign cluster membership, and to deliver catalogues of spectroscopically confirmed clusters. We discuss the relevance of line-of-sight velocity dispersion estimators for the richer systems. We illustrate our techniques by constructing a catalogue of 230 spectroscopically validated clusters (0.031 < z < 0.658), found in pilot observations. We discuss two potential science applications of the SPIDERS sample: the study of the X-ray luminosity-velocity dispersion (L X -σ ) relation and the building of stacked phase-space diagrams.

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“…Reiprich & Böhringer 2002;Allen et al 2011). Reliable measurements of cluster masses allow us to measure both the mass function and the power spectrum (Schuecker et al 2003), which directly probe the cosmological models.…”

Section: Introductionmentioning

confidence: 99%

The 2XMMi/SDSS Galaxy Cluster Survey

Takey

Schwope

Lamer

2013

A&A

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Aims. We compile a sample of X-ray-selected galaxy groups and clusters from the XMM-Newton serendipitous source catalogue (2XMMi-DR3) with optical confirmation and redshift measurement from the Sloan Digital Sky Survey (SDSS). We present an analysis of the X-ray properties of this new sample with particular emphasis on the X-ray luminosity-temperature (L X − T ) relation. Methods. The X-ray cluster candidates were selected from the 2XMMi-DR3 catalogue in the footprint of the SDSS-DR7. We developed a finding algorithm to search for overdensities of galaxies at the positions of the X-ray cluster candidates in the photometric redshift space and to measure the redshifts of the clusters from the SDSS data. For optically confirmed clusters with good quality X-ray data we derived the X-ray flux, luminosity, and temperature from proper spectral fits, while the X-ray flux for clusters with low-quality X-ray data was obtained from the 2XMMi-DR3 catalogue. Results. The detection algorithm provides the photometric redshift of 530 galaxy clusters. Of these, 310 clusters have a spectroscopic redshift for at least one member galaxy. About 75 percent of the optically confirmed cluster sample are newly discovered X-ray clusters. Moreover, 301 systems are known as optically selected clusters in the literature while the remainder are new discoveries in X-ray and optical bands. The optically confirmed cluster sample spans a wide redshift range 0.03−0.70 (median z = 0.32). In this paper, we present the catalogue of X-ray-selected galaxy groups and clusters from the 2XMMi/SDSS galaxy cluster survey. The catalogue has two subsamples: (i) a cluster sample comprising 345 objects with their X-ray spectroscopic temperature and flux from the spectral fitting; and (ii) a cluster sample consisting of 185 systems with their X-ray flux from the 2XMMi-DR3 catalogue, because their X-ray data are insufficient for spectral fitting. For each cluster, the catalogue also provides the X-ray bolometric luminosity and the cluster mass at R 500 based on scaling relations and the position of the likely brightest cluster galaxy (BCG). The updated L X − T relation of the current sample with X-ray spectroscopic parameters is presented. We found the slope of the L X − T relation to be consistent with published ones. We see no evidence for evolution in the slope and intrinsic scatter of the L X − T relation with redshift when excluding the low-luminosity groups.

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The REFLEX galaxy cluster survey

Cited by 194 publications

References 60 publications

The Dark Side of the Halo Occupation Distribution

The Dark Side of the Halo Occupation Distribution

SPIDERS: the spectroscopic follow-up of X-ray-selected clusters of galaxies in SDSS-IV

The 2XMMi/SDSS Galaxy Cluster Survey

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