Measuring Ωm with the ROSAT Deep Cluster Survey

By Stefano Borgani, Piero Rosati, P. Tozzi, S. Stanford, P. Eisenhardt, C. Lidman, B. Holden, R. Della Ceca, C. Norman, G. Squires. 2001

239 citations recorded by the source corpus.

We analyze the ROSAT Deep Cluster Survey (RDCS) to derive cosmological constraints from the evolution of the cluster X-ray luminosity distribution. The sample contains 103 galaxy clusters out to z ≃ 0.85 and flux limit Flim = 3 × 10-14 ergs s-1 cm-2 (RDCS-3) in the [0.5-2.0] keV energy band, with a high-redshift extension containing four clusters at 0.90 ≤ z ≤ 1.26 and brighter than Flim = 1 × 10-14 ergs s-1 cm-2 (RDCS-1). We assume cosmological models to be specified by the matter density parameter Ωm, the rms fluctuation amplitude at the 8 h-1 Mpc scale σ8, and the shape parameter for the cold dark matter-like power spectrum Γ. Model predictions for the cluster mass function are converted into the X-ray luminosity function in two steps. First, we convert mass into intracluster gas temperature by assuming hydrostatic equilibrium. Then, temperature is converted into X-ray luminosity by using the most recent data on the LX-TX relation for nearby and distant clusters. These include the Chandra data for six distant clusters at 0.57 ≤ z ≤ 1.27. From RDCS-3 we find Ωm = 0.35 and σ8 = 0.66 for a spatially flat universe with a cosmological constant, with no significant constraint on Γ (errors correspond to 1 σ confidence levels for three fitting parameters). Even accounting for both theoretical and observational uncertainties in the mass-X-ray luminosity conversion, an Einstein-de Sitter model is always excluded at far more than the 3 σ level. We also show that the number of X-ray-bright clusters in RDCS-1 at z > 0.9 is expected from the evolution inferred at z < 0.9 data.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/4ffbf2d3b28637ba3d8a702d2814238e388afd79

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

COSMOLOGICAL CONSTRAINTS FROM THE SLOAN DIGITAL SKY SURVEY MaxBCG CLUSTER CATALOG (2009, background): “…despite a spread in central values that range from σ8 ≈ 0.65 to σ8 ≈ 1.0 (Viana & Liddle 1996, 1999; Henry & Arnaud 1991; Henry 2000; Pierpaoli et al. 2001; Borgani et al. 2001; Seljak 2002; Viana et al. 2002; Schuecker et al. 2003; Allen et al. 2003; Bahcall et al. 2003; Bahcall & Bode 2003;…”
COSMOS: Three-dimensional Weak Lensing and the Growth of Structure (2007, result): “Our result is also larger than most estimates of cluster abundance from X-ray surveys (e.g., Borgani et al. 2001; Schneider et al. 2002), and from other recent spacebased weak-lensing measurements (Heymans et al. 2005; Schrabback et al. 2007).”
The Observed Growth of Massive Galaxy Clusters I: Statistical Methods and Cosmological Constraints (2009, methodology): “…around binning the detected clusters in redshift and flux (or luminosity) and either adopting external priors on the luminosity–mass relation (e.g. Borgani et al. 2001) or simultaneously fitting an external luminosity–mass data set without accounting for selection effects (e.g. Allen et al.…”
THE EVOLUTION OF X-RAY CLUSTERS OF GALAXIES (2002, methodology): “Borgani et al. (2001b) analyzed the RDCS sample to quantify the systematics in the determination of cosmological parameters induced by the uncertainty in the mass–luminosity relation (Borgani et al. 1998).”
The REFLEX galaxy cluster survey - VII. Omega(m) and sigma(8) from cluster abundance and large-scale clustering (2002, methodology): “…small σ8 values were also obtained by Markevitch (1998) using a local cluster sample with ASCA X-ray temperatures and ROSAT X-ray luminosities, by Borgani et al. (2001) using the ROSAT Deep Cluster Survey, by Seljak (2001) from the empirical mass/X-ray temperature relation of nearby clusters,…”
A kinematical approach to dark energy studies (2006, background): “…(Allen et al. 2002, 2004; Ettori et al. 2003), measurements of the mean matter density and amplitude of matter fluctuations from X-ray clusters (Borgani et al. 2001; Allen et al. 2003; Reiprich & Böhringer 2002; Schuecker et al. 2003; Voevodkin & Vikhlinin 2004), measurements of the matter…”
CHANDRA CLUSTER COSMOLOGY PROJECT III: COSMOLOGICAL PARAMETER CONSTRAINTS (2008, methodology): “Despite these limitations, reasonable con- straints could still be derived on ΩM (e.g., Borgani et al. 2001; Henry 2004).”
A SPITZER-SELECTED GALAXY CLUSTER AT z = 1.62 (2010, background): “…Service d’Astrophysique, CEA Saclay, 91191 Gif sur Yvette,France and shape of the initial power spectrum, as well as on the dark energy equation of state (e.g., Eke et al. 1998; Bahcall et al. 1999; Borgani et al. 2001; Haiman et al. 2001; Springel et al. 2005; Pacaud et al. 2007; Jee et al. 2009).”
The XMM-Newton Wide-Field Survey in the COSMOS Field: Statistical Properties of Clusters of Galaxies (2006, result): “Overall, these results consistently show a lack of evolution of the XLF for L < L∗ ≃ 3 ·1044 erg s−1 out to z ≃ 0.8, At the same time, however, they confirm the early findings from the Einstein Medium Sensitivity Survey (EMSS, Gioia et al 1990; Henry et al. 1992) of a mild evolution of the bright en”
THE EVOLUTION OF SWIFT/BAT BLAZARS AND THE ORIGIN OF THE MeV BACKGROUND (2009, background): “…dropping terms which are not model dependent, we obtain: S = −2 ∑ i wi ln[ρ(LX,i, zi)] + 2 ∫ LX,max LX,min ∫ zmax zmin λ(LX,i, zi)dLXdz (11) where following Borgani et al. (2001) we have introduce a weighting term wi which takes into account the uncertainties in the luminosity of each single…”
X‐ray properties of galaxy clusters and groups from a cosmological hydrodynamical simulation (2003, background): “…semi–analytical models (e.g., Balogh et al. 1999; Tozzi & Norman 2001) and numerical simulations (e.g., Bialek et al. 2001; Brighenti & Mathews 2001; Borgani et al. 2001a, 2002) were able to demonstrate that observational data can be reproduced by assigning a heating energy of about 0.5–1 keV per…”
Cosmological Parameters from Observations of Galaxy Clusters (2011, result): “X-ray studies in particular showed that the amplitude was lower than had been accepted previously (e.g. Borgani et al. 2001; Reiprich & Böhringer 2002; Seljak 2002; Pierpaoli et al. 2003; Allen et al. 2003; Schuecker et al. 2003), a result later confirmed by CMB and cosmic shear measurements.”
X-ray spectroscopy of galaxy clusters: studying astrophysical processes in the largest celestial laboratories (2009, methodology): “Since galaxy clusters are very sensitive tracers of structure growth, a census of the cluster population as a function of redshift can be used to test cosmological models (e.g. Borgani et al. 2001; Schuecker et al. 2003a,b; Henry 2004; Vikhlinin et al. 2003, 2009; Henry et al. 2009).”
The Cosmological Constant and Dark Energy (2002, unknown): “90 Examples include Blanchard et al. (2000), and Borgani et al. (2001).”