Evidence for non-hydrostatic gas from the cluster X-ray to lensing mass ratio

By A. Mahdavi, H. Hoekstra, Arif Babul, J. Henry. 2007

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Using a uniform analysis procedure, we measure spatially resolved weak gravitational lensing and hydrostatic X-ray masses for a sample of 18 clusters of galaxies. We find a radial trend in the X-ray to lensing mass ratio: at r 2500 , we obtain a ratio M X /M L = 1.03 ± 0.07 which decreases to M X /M L = 0.78 ± 0.09 at r 500 . This difference is significant at 3a once we account for correlations between the measurements. We show that correcting the lensing mass for excess correlated structure outside the virial radius slightly reduces, but does not eliminate this trend. An X-ray mass underestimate, perhaps due to non-thermal pressure support, can explain the residual trend. The trend is not correlated with the presence or absence of a cool core. We also examine the cluster gas fraction f gas and find no correlation with M L , an important result for techniques that aim to determine cosmological parameters using f gas .

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/cb4df0f2bc8dba460f1db9c1c1cbf6ee6c421162

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Citations in the corpus

Lensing and x-ray mass estimates of clusters (simulations) (2012, methodology): “We compare the gravitational lensing masses with the X-ray masses following the same fitting procedure described in Mahdavi et al. (2008) and M10 to whom we address the curious reader for a detailed description.”
The Canadian Cluster Comparison Project: detailed study of systematics and updated weak lensing masses (2015, methodology): “The comparison to the X-ray properties, presented in Mahdavi et al. (2008) and Mahdavi et al. (2013) confirmed the predictions from numerical simulations that the hydrostatic mass estimates are biased low.”
RESIDUAL GAS MOTIONS IN THE INTRACLUSTER MEDIUM AND BIAS IN HYDROSTATIC MEASUREMENTS OF MASS PROFILES OF CLUSTERS (2009, methodology): “More recently, mass estimates via strong lensing (Smith et al. 2005), weak lensing (e.g., Dahle 2006; Mahdavi et al. 2008; Zhang et al. 2008), combined strong and weak lensing (Bradač et al. 2006; Limousin et al. 2007; Oguri et al. 2009), and Sunyaev-Zel’dovich effect (e.g., Carlstrom et al. 2002,…”
LoCuSS: Subaru Weak Lensing Study of 30 Galaxy Clusters (2009, methodology): “In other words the three-dimensional spherical mass can be estimated from the aperture mass by correcting for the mass bias, assuming an NFW profile (see Mahdavi et al. 2008 for such an example).”
New constraints on dark energy from the observed growth of the most X-ray luminous galaxy clusters (2007, background): “Mahdavi et al. (2008) have compared masses determined from X-rays and lensing for 18 clusters and find a bias of −22 ± 9 per cent at r500, assuming the lensing masses are accurate.”
The MCXC: a meta-catalogue of x-ray detected clusters of galaxies (2010, background): “…has also been made in understanding the systematics affecting X-ray mass estimates via simulations (e.g., Rasia et al. 2006; Nagai et al. 2007a; Piffaretti & Valdarnini 2008) and via combination with gravitational lensing (e.g., Mahdavi et al. 2008; Zhang et al. 2010; Meneghetti et al. 2010).”
Weighing simulated galaxy clusters using lensing and X-ray (2009, methodology): “As an example, we overplot with asterisks the mass measurements of a sample of 18 galaxy clusters reported by Mahdavi et al. (2008) (M08 in the following discussion).”
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): “We present a similar exercise for a sample of X-ray luminous clusters (A68, A209, A267, A383, A963, A1689, A1763, A2218, A2390, A2219) from Hoekstra (2007) with weak lensing masses from Mahdavi et al. (2008).”
COSMOLOGICAL CONSTRAINTS FROM SUNYAEV–ZEL'DOVICH-SELECTED CLUSTERS WITH X-RAY OBSERVATIONS IN THE FIRST 178 deg2 OF THE SOUTH POLE TELESCOPE SURVEY (2011, background): “More recently, the weak-lensing masses from Hoekstra (2007) have twice been updated by the same author (Mahdavi et al. 2008; Hoekstra et al. 2012).”
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).”
The Observed Growth of Massive Galaxy Clusters I: Statistical Methods and Cosmological Constraints (2009, methodology): “This procedure is known to underestimate the mass by tens of per cent (e.g. Nagai, Vikhlinin & Kravtsov 2007; Mahdavi et al. 2008), since the intracluster medium is not supported solely by thermal pressure.”
A WEAK LENSING STUDY OF X-RAY GROUPS IN THE COSMOS SURVEY: FORM AND EVOLUTION OF THE MASS–LUMINOSITY RELATION (2009, background): “…measurements: the SDSS results from Rykoff et al. (2008) (hereafter R08), four groups from Bergé et al. (2008) (hereafter BE08), cluster data from Hoekstra (2007b) (hereafter H07) with masses updated in Mahdavi et al. (2008), and cluster data from Bardeau et al. (2007) (hereafter BA07).”
X-ray spectroscopy of galaxy clusters: studying astrophysical processes in the largest celestial laboratories (2009, background): “studies (Zhang et al. 2008; Mahdavi et al. 2008) showing that the X-ray mass determination provides a much smaller individual uncertainty.”
ON THE ACCURACY OF WEAK-LENSING CLUSTER MASS RECONSTRUCTIONS (2010, background): “A recent analysis by Mahdavi et al. (2008) has indeed indicated that the HSE X-ray derived masses are biased low by≈ 10% with respect to the WL masses, although no such bias has been detected in other recent studies (Zhang et al. 2008; Vikhlinin et al. 2009; Zhang et al. 2010).”
CONSTRAINING THE SCATTER IN THE MASS–RICHNESS RELATION OF maxBCG CLUSTERS WITH WEAK LENSING AND X-RAY DATA (2008, methodology): “A similar analysis has been carried out by Mahdavi et al. (2008), who used the weak lensing mass estimates of Hoekstra (2007) and their own analysis of Chandra public data to obtainMwl = (1.28±0.15)MX. Finally, using XMM X-ray observations and the weak lensingdata of Bardeau et al. (2005), Bardeau…”
Cosmological Parameters from Observations of Galaxy Clusters (2011, background): “Potentially increased levels of non-thermal pressure support (e.g. Nagai, Vikhlinin & Kravtsov 2007; Pfrommer et al. 2007; Mahdavi et al. 2008) and gas clumping (Simionescu et al. 2011) can also complicate measurements at large radii.”
Masses of Galaxy Clusters from Gravitational Lensing (2013, background): “Furthermore, pressure support by turbulent motion of the ICM leads to biases in the hydrostatic masses (e.g., Nagai et al. 2007; Mahdavi et al. 2008, 2012), which need to be calibrated observationally.”
Detailed cluster lensing profiles at large radii and the impact on cluster weak lensing studies (2011, background): “…massive clusters, we can detect weak lensing signals out to virial radii, which allows direct measurements of virial masses (e.g., Dahle 2006; Broadhurst et al. 2008; Mahdavi et al. 2008; Okabe & Umetsu 2008; Oguri et al. 2009; Umetsu et al. 2009, 2011; Medezinski et al. 2010; Okabe et al. 2010).”
Planck 2013 results. XX. Cosmology from Sunyaev-Zeldovich cluster counts (2013, background): “…with some studies finding good agreement between HE and WL masses (e.g., Vikhlinin et al. 2009a; Zhang et al. 2010), some finding that HE masses are lower than WL masses, (e.g., Mahdavi et al. 2008), and some even finding that HE masses are higher than WL masses (Planck Collaboration Int.”