A comparison of weak-lensing masses and X-ray properties of galaxy clusters

By H. Hoekstra. 2007

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We present measurements of the masses of 20 X-ray luminous clusters of galaxies at intermediate redshifts, determined from a weak-lensing analysis of deep archival R-band data obtained using the Canada-France-Hawaii Telescope. Compared to previous work, our analysis accounts for a number of effects that are typically ignored, but can lead to small biases, or incorrect error estimates. We derive masses that are essentially model-independent and find that they agree well with measurements of the velocity dispersion of cluster galaxies and with the results of X-ray studies. Assuming a power law between the lensing mass and the X-ray temperature, M 2500 oc T α , we find a best-fitting slope of a = 1.34 +0.30 -0.28 . This slope agrees with self-similar cluster models and studies based on X-ray data alone. For a cluster with a temperature of kT = 5 keV we obtain a mass M 2500 = (1.4 ± 0.2) x 10 14 h -1 M⊙ in fair agreement with recent Chandra and XMM studies.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/84634c87af93d6a4f5b0758f3f58af540111a331

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Citations in the corpus

CHANDRA CLUSTER COSMOLOGY PROJECT. II. SAMPLES AND X-RAY DATA REDUCTION (2008, methodology): “Such data are only starting to become available now (Hoekstra 2007; Mahdavi et al. 2008; Zhang et al. 2008) and we in fact use them to place limits on systematic errors in our calibration of the Mtot measurements (Section 4.3.1).”
COSMOLOGICAL CONSTRAINTS FROM GALAXY CLUSTERS IN THE 2500 SQUARE-DEGREE SPT-SZ SURVEY (2016, methodology): “In V09, the normalization was cross-checked against weak lensing mass estimates from Hoekstra (2007) for the 10 clusters at z 0.3 that, at the time, also had sufficient Chandra observations to measure YX.”
ON THE ACCURACY OF WEAK-LENSING CLUSTER MASS RECONSTRUCTIONS (2010, background): “…there is also significant hope that masses measured using weak lensing (WL) observations can be used to accurately calibrate such relations (e.g., Hoekstra 2007; Mahdavi et al. 1 Department of Physics, 5720 S. Ellis Avenue, The Universityof Chicago, Chicago, IL 60637 2 Kavli Institute for…”
Gravitational lensing (2010, background): “[86, 198, 220, 228, 231, 307, 518]), significant discrepancies between cluster masses derived from weak lensing and x-ray observations are often found [6, 149, 209, 274, 391] and interpreted as signalling dynamical processes in unrelaxed cluster cores.”
Improved constraints on dark energy from Chandra X-ray observations of the largest relaxed galaxy clusters (2007, methodology): “Ground and space-based gravitational lensing studies will provide important, independent constraints on the mass distributions in clusters; a large program using the Subaru telescope and Hubble Space Telescope is underway, as is similar work by other groups (e.g. Hoekstra 2007).”
CFHTLenS: Improving the quality of photometric redshifts with precision photometry (2011, methodology): “Thanks to the steady progress in analysis tools and better knowledge of the source redshift distribution WL studies have become an important tool to calibrate the masses of individual galaxy clusters (Hoekstra 2007; Heymans et al. 2008; Okabe et al. 2010; Hoekstra et al. 2011; Jee et al. 2011).”
CHANDRA CLUSTER COSMOLOGY PROJECT III: COSMOLOGICAL PARAMETER CONSTRAINTS (2008, result): “%) is estimated from comparison of Chandramasses with two recent weak lensing studies (Hoekstra 2007; Zhang et al. 2008).”
Cosmological Parameters from Observations of Galaxy Clusters (2011, methodology): “The most common technique employed in weak lensing mass measurements is fitting the observed, azimuthally-averaged gravitational shear profile with a simple parameterized mass model (e.g. Hoekstra 2007).”
Weighing the Giants – III. Methods and measurements of accurate galaxy cluster weak-lensing masses (2012, methodology): “Bardeau et al. (2007) measured weak-lensing masses for eleven clusters using three-band imaging with the CFH12K camera at the CFHT (some of these data were also used in the Hoekstra 2007 and Mahdavi et al. 2008 analyses).”
Masses of Galaxy Clusters from Gravitational Lensing (2013, methodology): “One way to estimate its value, is to use the results from a parametric model that is fit to the data (Hoekstra 2007).”
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): “Hoekstra (2007) and Hoekstra et al. (2012) removed galaxies that lie on the cluster red-sequence and boosted the signal based on excess number counts of galaxies.”
Evidence for non-hydrostatic gas from the cluster X-ray to lensing mass ratio (2007, methodology): “We refer interested readers to Hoekstra (2007) for details of the data reduction and weak lensing analysis procedure.”
NEW CONSTRAINTS ON THE EVOLUTION OF THE STELLAR-TO-DARK MATTER CONNECTION: A COMBINED ANALYSIS OF GALAXY–GALAXY LENSING, CLUSTERING, AND STELLAR MASS FUNCTIONS FROM z = 0.2 to z = 1 (2011, methodology): “As discussed in Section 5.5.1, the extrapolation of our model is in good agreement with results from Blanton et al. (2008) at low M∗ and with Hoekstra (2007) at high M∗.”