A WEAK LENSING STUDY OF X-RAY GROUPS IN THE COSMOS SURVEY: FORM AND EVOLUTION OF THE MASS–LUMINOSITY RELATION

By A. Leauthaud, A. Finoguenov, Jean-Paul Kneib, James E. Taylor, Richard J. Massey, Jason D. Rhodes, O. Ilbert, K. Bundy, J. Tinker, M. George and 20 more. 2009

218 citations recorded by the source corpus.

Measurements of X-ray scaling laws are critical for improving cosmological constraints derived with the halo mass function and for understanding the physical processes that govern the heating and cooling of the intracluster medium. In this paper, we use a sample of 206 X-ray-selected galaxy groups to investigate the scaling relation between X-ray luminosity (LX) and halo mass (M200) where M200 is derived via stacked weak gravitational lensing. This work draws upon a broad array of multi-wavelength COSMOS observations including 1.64 degrees2 of contiguous imaging with the Advanced Camera for Surveys to a limiting magnitude of IF814W = 26.5 and deep XMM-Newton/Chandra imaging to a limiting flux of 1.0 × 10−15 erg cm−2 s−1 in the 0.5–2 keV band. The combined depth of these two data sets allows us to probe the lensing signals of X-ray-detected structures at both higher redshifts and lower masses than previously explored. Weak lensing profiles and halo masses are derived for nine sub-samples, narrowly binned in luminosity and redshift. The COSMOS data alone are well fit by a power law, M200 ∝ (LX)α, with a slope of α = 0.66 ± 0.14. These results significantly extend the dynamic range for which the halo masses of X-ray-selected structures have been measured with weak gravitational lensing. As a result, tight constraints are obtained for the slope of the M–LX relation. The combination of our group data with previously published cluster data demonstrates that the M–LX relation is well described by a single power law, α = 0.64 ± 0.03, over two decades in mass, M200 ∼ 1013.5–1015.5 h−172 M☉. These results are inconsistent at the 3.7σ level with the self-similar prediction of α = 0.75. We examine the redshift dependence of the M–LX relation and find little evidence for evolution beyond the rate predicted by self-similarity from z ∼ 0.25 to z ∼ 0.8.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/7565936a1b89afcc277e108a8a6072478812e9b0

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

Origins of weak lensing systematics, and requirements on future instrumentation (or knowledge of instrumentation) (2012, methodology): “A much more robust technique, demonstrated by Leauthaud et al. (2010), is to apply a physicallymotivated correction scheme at the pixel level as the first process during data reduction (e.g. Massey 2010; Anderson & Bedin 2010).”
Combined strong and weak lensing analysis of 28 clusters from the Sloan Giant Arcs Survey (2011, methodology): “This stacked lensing analysis has c© RAS, MNRAS 000, 1–22 been successful for constraining mean dark matter distributions of cluster samples (e.g., Mandelbaum et al. 2006b; Johnston et al. 2007; Leauthaud et al. 2010; Okabe et al. 2010).”
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): “These data points are directly comparable to ours since we have used exactly the same stellar masses and confirm that our results are consistent with Leauthaud et al. (2010).”
CFHTLenS: the relation between galaxy dark matter haloes and baryons from weak gravitational lensing (2013, result): “Additionally, the results from the COSMOS analysis of X-ray selected groups presented in Leauthaud et al. (2010), which is centred on a redshift similar to ours and also shown in Figure 10 of Leauthaud et al. (2012) as grey squares, agree better with our results for higher stellar masses.”
The first-year shear catalog of the Subaru Hyper Suprime-Cam Subaru Strategic Program Survey (2017, background): “…2011), and provides an important means to calibrate mass-observable relations of clusters for using cluster abundances to constrain cosmology (e.g., Leauthaud et al. 2010; Okabe et al. 2010; Donahue et al. 2014; von der Linden et al. 2014; Hoekstra et al. 2015; Okabe & Smith 2016; Battaglia et al.…”
A DIRECT MEASUREMENT OF THE BARYONIC MASS FUNCTION OF GALAXIES AND IMPLICATIONS FOR THE GALACTIC BARYON FRACTION (2012, background): “The small cyan, red and blue circles correspond to galaxies with measurements of their halo mass Mh from weak lensing (Mandelbaum et al. 2006; Hoekstra 2007; Leauthaud et al. 2010).”
Cosmological Parameters from Observations of Galaxy Clusters (2011, methodology): “Stacking analyses of clusters detected in survey fields have also proved successful in calibrating the mean mass–observable scaling relations down to relatively low masses (e.g. Johnston et al. 2007; Rykoff et al. 2008; Leauthaud et al. 2010).”
SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION (2010, methodology): “Scaling relations, gas pressure, and entropy of lowmass clusters and groups have been studied in the literature.41 Leauthaud et al. (2010) obtained a relation between LX of 206 X-ray-selected galaxy groups and the mass (M200) derived from the stacking analysis of weak lensing measurements.”
Weak Lensing Measurement of the Mass--Richness Relation of SDSS redMaPPer Clusters (2016, methodology): “Weak lensing has been commonly used to characterize the matter in galaxies (e.g. Brainerd et al. 1996), groups (e.g. Leauthaud et al. 2010) and galaxy clusters (e.g. Sheldon et al. 2004a; Johnston et al. 2007a; von der Linden et al. 2014; Hoekstra et al. 2015; Okabe & Smith 2015; van Uitert et al.…”
A mature cluster with X-ray emission at z = 2.07 (2010, result): “On the basis of establishedLX − M correlations (Leauthaud et al. 2010), the luminosity corresponds to a total mass of M200 = (5.3 ± 1) × 1013 M⊙, comparable to that of Virgo.”
Masses of Galaxy Clusters from Gravitational Lensing (2013, methodology): “Leauthaud et al. (2010) used this data set to investigate the weak lensing properties of a sample of 206 X-ray–selected galaxy groups with 0.2<z< 0.9 from Finoguenov et al. (2007).”
Weighing the Giants - I. Weak-lensing masses for 51 massive galaxy clusters: project overview, data analysis methods and cluster images (2012, background): “For larger samples of less massive systems, stacking analyses enable the determination of the mean cluster mass in bins of survey observable (Johnston et al. 2007; Leauthaud et al. 2010).”
CFHTLenS: Improving the quality of photometric redshifts with precision photometry (2011, background): “…lenses, the average properties of clusters (Johnston et al. 2007; Hildebrandt et al. 2011) and groups (Hoekstra et al. 2001; Parker et al. 2005; Leauthaud et al. 2010) or even galaxies (e.g. Brainerd et al. 1996; Hudson et al. 1998; Hoekstra et al. 2004; Heymans et al. 2006; Mandelbaum et al.…”
The dependence of star formation activity on environment and stellar mass at z∼ 1 from the HiZELS-Hα survey (2010, background): “…the survey is able to probe a luminous and massive (M500 ≈ 1014.3 M ) X-ray selected cluster in COSMOS at z = 0.835 (see Figure 2), along with other nearby lower luminosity X-ray groups at z = 0.85 which have already been reported by the COSMOS team (Finoguenov et al. 2007; Leauthaud et al. 2010).”