Details of the mass-temperature relation for clusters of galaxies

By A. Finoguenov, T. Reiprich, H. Böhringer. 2000

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We present results on the total mass and temperature determination using two samples of clusters of galaxies. One sample is constructed with emphasis on the completeness of the sample, while the advantage of the other is the use of the temperature profiles, derived with ASCA. We obtain remarkably similar fits to the $M-T$ relation for both samples, with the normalization and the slope significantly different from both prediction of self-similar collapse and hydrodynamical simulations. We discuss the origin of these discrepancies and also combine the X-ray mass with velocity dispersion measurements to provide a comparison with high-resolution dark matter simulations. Finally, we discuss the importance of a cluster formation epoch in the observed $M-T$ relation.

Subfields: Astronomy and Astrophysics, Global and Planetary Change

View Paper: https://www.semanticscholar.org/paper/172ca70baf26010ac461dccd3224071ec2a6b328

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Citations in the corpus

Total mass biases in X-ray galaxy clusters (2008, background): “…the optical galaxy populations (e.g. Biviano & Girardi 2003; Rines et al. 2003), observations of the X-ray emitting intracluster medium (ICM) (e.g. Finoguenov et al. 2001; Reiprich & Böhringer 2002; Ettori et al. 2002; Arnaud et al. 2005; Vikhlinin et al. 2006) and on gravitational lensing (e.g.…”
GALAXY CLUSTERS IDENTIFIED FROM THE SDSS DR6 AND THEIR PROPERTIES (2009, background): “Correlations of the richness and optical luminosity with the cluster mass The X-ray luminosity and temperature have been found to be tightly correlated with cluster mass (Finoguenov et al. 2001; Allen et al. 2001; Xu et al. 2001; Reiprich & Böhringer 2002; Shimizu et al. 2003).”
INTRACLUSTER MEDIUM ENTROPY PROFILES FOR A CHANDRA ARCHIVAL SAMPLE OF GALAXY CLUSTERS (2009, background): “However, numerous observational studies have shown that clusters do not follow the tight mass-observable scaling relations predicted by simulations (Edge & Stewart 1991; Allen & Fabian 1998; Markevitch 1998; Arnaud & Evrard 1999; Horner et al. 1999; Nevalainen et al. 2000; Finoguenov et al. 2001).”
CHANDRA STUDIES OF THE X-RAY GAS PROPERTIES OF GALAXY GROUPS (2008, background): “There had been a lot of work on the cluster M −T relation before the Chandra and XMM-Newton era (e.g., Finoguenov et al. 2001; Sanderson et al. 2003).”
Cosmological constraints from the local X-ray luminosity function of the most X-ray-luminous galaxy clusters (2002, methodology): “9 shows the result of Seljak (2002), σ8 = (0.44 ± 0.04) Ω−0.44m (Γ/0.2)0.08 , using the observed local X-ray temperature function of rich clusters (Pierpaoli, Scott & White 2002) and a mass-temperature relation determined from ASCA and ROSAT observations (Finoguenov et al. 2001).”
Near-Infrared Properties of Galaxy Clusters: Luminosity as a Binding Mass Predictor and the State of Cluster Baryons (2003, methodology): “Finoguenov et al. (2001b) provide several M − TX relations that arise from different subsets of a cluster ensemble.”
The mass profile of A1413 observed with XMM-Newton: Implications for the M-T relation (2002, result): “While observations have, for hot clusters at least, recovered the slope of this relation, observed masses imply a normalisation consistently lower than found by simulations (e.g., Horner et al. 1999; Nevalainen et al. 2000; Finoguenov et al. 2001).”
Modified Entropy Models for the Intracluster Medium (2002, methodology): “2 and in the cluster data of Finoguenov et al. (2001).”
Scaling laws in X-ray galaxy clusters at redshift between 0.4 and 1.3 (2003, methodology): “We compare our distribution in the EzMtot − T plane with the local relations measured by (i) Ettori et al. (2002; BeppoSAX data), (ii) Finoguenov et al. (2001) for their subsample of 26 clusters with spatially resolved temperatures and emissionweighted values larger than 3 keV as measured with ASCA…”
ERRATUM: “CHANDRA SAMPLE OF NEARBY RELAXED GALAXY CLUSTERS: MASS, GAS FRACTION, AND MASS–TEMPERATURE RELATION” (2006, ApJ, 640, 691) (2005, methodology): “A tight relation between the cluster temperature and total mass is expected on theoretical grounds, which is indeed observed, at least for the hydrostatic mass estimates (Nevalainen et al. 2000; Horner et al. 1999; Finoguenov et al. 2001; Xu et al. 2001; Sanderson et al. 2003).”
THE EVOLUTION OF X-RAY CLUSTERS OF GALAXIES (2002, methodology): “T relation, usually measured at some fixed overdensity from observational data, seems to have a lower normalization than that calibrated from hydrodynamical simulations (e.g. Finoguenov et al. 2001, Allen et al. 2001, Ettori et al. 2002).”
LoCuSS: comparison of observed X-ray and lensing galaxy cluster scaling relations with simulations (2008, methodology): “Pacaud et al. (2007) found r500 = 0.375(T/keV)0.63h73(z)−1 Mpc based on the measurements in Finoguenov et al. (2001), which is in agreement with ours within the uncertainty.”
What is a cool-core cluster? a detailed analysis of the cores of the X-ray flux-limited HIFLUGCS cluster sample (2009, methodology): “We note that these values may be overestimates of r500 andr180 since they are based on early simulations (e.g. Finoguenov et al. 2001).”
Radio and X-ray diffuse emission in six clusters of galaxies (2001, background): “Observationally the study by Finoguenov et al. 2001 shows that the assumption of isothermality in general may lead to an overestimate of the mass by about 20% at the virial radius.”