The ROSAT-ESO Flux Limited X-ray (REFLEX) Galaxy cluster survey. V. The cluster catalogue

By H. Böhringer, P. Schuecker, L. Guzzo, C. Collins, Wolfgang Voges, R. Cruddace, A. Ortiz-Gil, G. Chincarini, S. Grandi, A. Edge and 4 more. 2004

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We present the catalogue of the REFLEX Cluster Survey providing information on the X-ray properties, redshifts, and some identification details of the clusters in the REFLEX sample. The catalogue describes a statistically complete X-ray flux-limited sample of 447 galaxy clusters above an X-ray flux of 3 $\times$ 10 -12 erg s -1 cm -2 (0.1 to 2.4 keV) in an area of 4.24 ster in the southern sky. The cluster candidates were first selected by their X-ray emission in the ROSAT-All Sky Survey and subsequently spectroscopically identified in the frame of an ESO key programme. Previously described tests have shown that the sample is more than 90% complete and there is a conservative upper limit of 9% on the fraction of clusters with a dominant X-ray contamination from AGN. In addition to the cluster catalogue we also describe the complete selection criteria as a function of the sky position and the conversion functions used to analyse the X-ray data. These are essential for the precise statistical analysis of the large-scale cluster distribution. This data set is at present the largest, statistically complete X-ray galaxy cluster sample. Together with these data set we also provide for the first time the full three-dimensional selection function. The sample forms the basis of several cosmological studies, one of the most important applications being the assessment of the statistics of the large-scale structure of the universe and the test of cosmological models. Part of these cosmological results have already been published.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/04e55c8491a733084a99c2e46d5f81b16a126229

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Citations in the corpus

NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL PARAMETER RESULTS (2012, methodology): “These clusters were taken from the REFLEX sample (Böhringer et al. 2004) in the southern hemisphere, and the extended BCS sample (Ebeling et al. 1998, 2000) in the northern hemisphere.”
GALAXY CLUSTERS DISCOVERED VIA THE SUNYAEV–ZEL'DOVICH EFFECT IN THE 2500-SQUARE-DEGREE SPT-SZ SURVEY (2014, background): “In Figure 6, we compare the mass and redshift distribution of the SPT sample to those from other large cluster catalogs selected via their ICM observables: namely the clusters detected in the all-sky ROSAT survey (Piffaretti et al. 2011), which includes the NORAS (Böhringer et al. 2000), REFLEX (Bo”
Planck 2013 results. XX. Cosmology from Sunyaev-Zeldovich cluster counts (2013, methodology): “X-ray cluster surveys include both the NORAS (Böhringer et al. 2000) and REFLEX (Böhringer et al. 2004) surveys, based on ROSAT satellite observations, which have been used as source catalogues for higherprecision observations by the Chandra and XMM-Newton satellites, as well as surveys with XMM-New”
New constraints on dark energy from the observed growth of the most X-ray luminous galaxy clusters (2007, methodology): “The ROSAT Brightest Cluster Sample (BCS; Ebeling et al. 1998, 2000) and ROSAT- c© 2008 RAS ESO Flux Limited X-ray sample (REFLEX; Böhringer et al. 2004) together cover approximately two-thirds of the sky out to redshift z ∼ 0.3 and contain more than 750 clusters.”
LoCuSS: THE SLOW QUENCHING OF STAR FORMATION IN CLUSTER GALAXIES AND THE NEED FOR PRE-PROCESSING (2015, methodology): “LoCuSS is a multi-wavelength survey of X-ray luminous galaxy clusters at 0.15 ⩽ z ⩽ 0.3 (Smith et al. 2010a) drawn from the ROSAT All Sky Survey cluster catalogs (Böhringer et al. 2004).”
GMRT radio halo survey in galaxy clusters at z = 0.2–0.4 - II. The eBCS clusters and analysis of the complete sample (2008, methodology): “From the ROSAT–ESO Flux Limited X–ray galaxy cluster catalogue (REFLEX, Böhringer et al. 2004) and from the extended ROSAT Brightest Cluster Sample catalogue (BCS, Ebeling et al. 1998, 2000) we selected all clusters satisfying the following constraints: 1) LX(0.1–2.4 keV) > 5 × 1044 erg s−1; 2)…”