CHANDRA CLUSTER COSMOLOGY PROJECT. II. SAMPLES AND X-RAY DATA REDUCTION

By A. Vikhlinin, R. Burenin, H. Ebeling, W. Forman, A. Hornstrup, C. Jones, Andrey V. Kravtsov, S. Murray, D. Nagai, H. Quintana and 1 more. 2008

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We discuss the measurements of the galaxy cluster mass functions at z ≈ 0.05 and z ≈ 0.5 using high-quality Chandra observations of samples derived from the ROSAT PSPC All-Sky and 400 deg2 surveys. We provide a full reference for the data analysis procedures, present updated calibration of relations between the total cluster mass and its X-ray indicators (TX, Mgas, and YX) based on a subsample of low-z relaxed clusters, and present a first measurement of the evolving LX–Mtot relation (with Mtot estimated from YX) obtained from a well defined statistically complete cluster sample and with appropriate corrections for the Malmquist bias applied. Finally, we present the derived cluster mass functions, estimate the systematic uncertainties in this measurement, and discuss the calculation of the likelihood function. We confidently measure the evolution in the cluster comoving number density at a fixed mass threshold, e.g., by a factor of 5.0 ± 1.2 at M500 = 2.5 × 1014 h−1 M☉ between z = 0 and 0.5. This evolution reflects the growth of density perturbations, and can be used for the cosmological constraints complementing those from the distance–redshift relation.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/54b4924f8b53a9bfa74d12d26a335597ba25b2c9

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Citations in the corpus

The MCXC: a meta-catalogue of x-ray detected clusters of galaxies (2010, methodology): “…with the current generation of Xray satellitesXMM-Newton, Chandra andSuzaku, have provided statistical samples for cosmological studies (e.g., Vikhlinin et al. 2009; Mantz et al. 2009) and detailed information on the structural properties of the cluster population (e.g., Vikhlinin et al.…”
The universal galaxy cluster pressure profile from a representative sample of nearby systems (REXCESS) and the Y-SZ-M-500 relation (2009, background): “The local M500–YX relation for relaxed clusters has recently been calibrated (Nagai et al. 2007; Maughan 2007; Arnaud et al. 2007; Vikhlinin et al. 2009), with excellent agreement achieved between various observations (e.g., see Arnaud et al. 2007).”
LoCuSS: Subaru Weak Lensing Study of 30 Galaxy Clusters (2009, methodology): “The masses M2500 and M500 are often used when estimating cluster masses based on X-ray observations (e.g., Vikhlinin et al. 2006, 2009a).”
Cosmological Parameters from Observations of Galaxy Clusters (2011, methodology): “Vikhlinin et al. (2009b) also used X-ray selected clusters, but pursued a different survey strategy.”
Planck 2013 results. XX. Cosmology from Sunyaev-Zeldovich cluster counts (2013, methodology): “(A.1)), taken from Arnaud et al. (2010), is not measurable; neither is it measurable for the best-fit Chandra YX–MHE500 relation published in Vikhlinin et al. (2009a).”
The X-ray brightest clusters of galaxies from the Massive Cluster Survey (2010, result): “2 and compared to that of the BCS, EMSS, WARPS, and 400-sq.-deg. cluster samples (Ebeling et al. 1998, 2000; Gioia & Luppino 1994; Perlman et al. 2002; Burenin et al. 2007; Horner et al. 2008; Vikhlinin et al. 2009).”
THE ATACAMA COSMOLOGY TELESCOPE: ACT-CL J0102−4915 “EL GORDO,” A MASSIVE MERGING CLUSTER AT REDSHIFT 0.87 (2011, methodology): “For the gas temperature and luminosity we essentially follow the prescriptions in Vikhlinin et al. (2009) to apply those scaling laws to the X-ray data.”
DETECTION OF AN UNIDENTIFIED EMISSION LINE IN THE STACKED X-RAY SPECTRUM OF GALAXY CLUSTERS (2014, methodology): “The overdensity radii were calculated using the Vikhlinin et al. (2009) masstemperature scaling relation for each cluster.”
ROBUST OPTICAL RICHNESS ESTIMATION WITH REDUCED SCATTER (2011, methodology): “We adopt the fiducial values αLX |M = 1.61 and σM|LX = 0.246 as per Vikhlinin et al. (2009).”
A new method to quantify the effects of baryons on the matter power spectrum (2015, unknown): “2.19) Cosmic baryon fraction Gonzalez et al. 2013 Vikhlinin et al. 2009 Sun et al. 2008 1012 1013 1014 1015 M200 [M¯/h] 0.01 0.02 0.03 0.04 0.05 f c ga l( M 2 00 ) Kravtsov et al 2014 Gonzalez et al 2013 Reyes et al 2012 Abundance matching Figure 2.”
Towards a realistic population of simulated galaxy groups and clusters (2013, methodology): “In both cases, we have converted the observed mean X-ray temperature into a halo mass using the mass–temperature relation of Vikhlinin et al. (2009).”
DARK MATTER HALO PROFILES OF MASSIVE CLUSTERS: THEORY VERSUS OBSERVATIONS (2011, background): “…Okabe et al. 2010; Oguri et al. 2011) X-ray observations of relaxed clusters (e.g., Buote et al. 2007; Vikhlinin et al. 2006; Schmidt & Allen 2007; Vikhlinin et al. 2009) and relaxed and unrelaxed clusters (Ettori et al. 2011), and cluster kinematics (e.g., Rines & Diaferio 2006; Wojtak & Lokas…”
ON THE ACCURACY OF WEAK-LENSING CLUSTER MASS RECONSTRUCTIONS (2010, background): “…Relations Recently, samples of galaxy clusters with masses inferred from weak lensing have grown to the point where scaling relations between cluster observables and WL masses can be analyzed in detail (e.g., Zhang et al. 2008; Vikhlinin et al. 2009; Henry et al. 2009; Okabe et al. 2010b).”
JOINT ANALYSIS OF CLUSTER OBSERVATIONS. II. CHANDRA/XMM-NEWTON X-RAY AND WEAK LENSING SCALING RELATIONS FOR A SAMPLE OF 50 RICH CLUSTERS OF GALAXIES (2012, methodology): “In numerical simulation studies, this pressure-like quantity has been shown be a much better mass proxy and has been successfully deployed in measurements of cosmological parameters including the dark energy equation of state (Vikhlinin et al. 2009a, 2009b).”
The Observed Growth of Massive Galaxy Clusters I: Statistical Methods and Cosmological Constraints (2009, methodology): “As discussed by Vikhlinin et al. (2009b), the method used to estimate masses has an effect on the constraints obtained because different mass proxies have different dependencies on distance, with gas mass (Mgas ∝ d 2.5) being more sensitive than temperature or YX .”
The Atacama Cosmology Telescope: Sunyaev-Zel'dovich selected galaxy clusters at 148 GHz from three seasons of data (2013, methodology): “The use of YX as a mass proxy has, in turn, been calibrated to weak lensing masses [115].”
Weighing the Giants - I. Weak-lensing masses for 51 massive galaxy clusters: project overview, data analysis methods and cluster images (2012, background): “Recently, measurements of the evolution of the cluster number density have provided some of the most precise and robust constraints on dark energy (Vikhlinin et al. 2009b; Mantz et al. 2010a), as well as departures from General Relativity on cosmological scales (Rapetti et al. 2010, 2013; Schmidt…”
MEASURING THE ULTIMATE HALO MASS OF GALAXY CLUSTERS: REDSHIFTS AND MASS PROFILES FROM THE HECTOSPEC CLUSTER SURVEY (HeCS) (2012, background): “Vikhlinin et al (2009) estimate a large mass for RXJ1504 based on Chandra observations and the YX estimator.”