The structural and scaling properties of nearby galaxy clusters. II. The M-T relation

By M. Arnaud, E. Pointecouteau, G. W. P. S. D. CEA-Saclay, F. M. Garching, Heidelberg · Germany. 2005

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Using a sample of ten nearby ($z\lesssim 0.15$), relaxed galaxy clusters in the temperature range [2–9]$~\rm keV$, we have investigated the scaling relation between the mass at various density contrasts ($\delta=2500,1000,500,200$) and the cluster temperature. The masses are derived from NFW-type model fits to mass profiles, obtained under the hydrostatic assumption using precise measurements, with , at least down to $\delta=1000$. The logarithmic slope of the M – T relation is well constrained and is the same at all δ , reflecting the self-similarity of the mass profiles. At $\delta=500$, the slope of the relation for the sub-sample of hot clusters ($kT>3.5~\rm keV$) is consistent with the standard self-similar expectation: $\alpha= 1.49\pm0.15$. The relation steepens when the whole sample is considered: $\alpha=1.71\pm0.09$. The normalisation of the relation is discrepant (by ~30 per cent), at all density contrasts, with the prediction from purely gravitation based models. Models that take into account radiative cooling and galaxy feedback are generally in better agreement with our data. We argue that remaining discrepancies, in particular at low δ , are more likely due to problems with models of the ICM thermal structure rather than to an incorrect estimate of the mass from X-ray data.

Subfields: Astronomy and Astrophysics, Global and Planetary Change, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/1b2ac6ccacdbb98d99b1fd2e0dbd7f238b1d46ca

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Citations in the corpus

THE REDMAPPER GALAXY CLUSTER CATALOG FROM DES SCIENCE VERIFICATION DATA (2016, methodology): “An r2500 radius was derived from this temperature via the empirical relation found in Arnaud et al. (2005).”
Searching for cool core clusters at high redshift (2008, background): “We corrected the gas density for the cosmological expansion: attending theMgas − T andR − T scaling relations (Arnaud et al. 2005a) it follows thatngas should be scaled byh(z)−2 to account for the more compact shape of distant clusters.”
CHANDRA STUDIES OF THE X-RAY GAS PROPERTIES OF GALAXY GROUPS (2008, methodology): “The Chandra exposure is short but the best-fit values of our temperature profile agree well with the XMM-Newton results by Snowden et al. (2008).”
ERRATUM: “CHANDRA SAMPLE OF NEARBY RELAXED GALAXY CLUSTERS: MASS, GAS FRACTION, AND MASS–TEMPERATURE RELATION” (2006, ApJ, 640, 691) (2005, methodology): “T relation is very close to that derived by Arnaud et al. (2005) using XMM-Newton data.”
Planck2013 results. XXIX. ThePlanckcatalogue of Sunyaev-Zeldovich sources (2013, background): “In this regard the X-ray selected samples are considerably more powerful,due to the tighter correlations of X-ray properties with mass (Arnaud et al. 2005; Vikhlinin et al. 2006; Pratt et al. 2009; Reichert et al. 2011; Maughan et al. 2012).”
Planck intermediate results: V. Pressure profiles of galaxy clusters from the Sunyaev-Zeldovich effect (2012, unknown): “…and the ensuing similarity yields both a universal dark matter distribution and simple global scaling relations that should describe the entire halo population (Bertschinger 1985; Kaiser et al. 1995; Navarro et al. 1995; Evrard et al. 1996; Navarro et al. 1997; Voit 2005; Arnaud et al. 2005).”
STELLAR AND TOTAL BARYON MASS FRACTIONS IN GROUPS AND CLUSTERS SINCE REDSHIFT 1 (2009, background): “The largest radius for which reliable X-ray hydrostatic masses are available is R500 (e.g. Arnaud et al. 2005; Vikhlinin et al. 2006; Sun et al. 2009).”
A SPITZER-SELECTED GALAXY CLUSTER AT z = 1.62 (2010, background): “× 1014 M⊙ based on the local luminosity–temperature and mass–temperature relations (Arnaud & Evrard 1999; Arnaud et al. 2005).”
X-ray spectroscopy of galaxy clusters: studying astrophysical processes in the largest celestial laboratories (2009, background): “…to the disproportionate influence of the central cool cores as will becomeaparant below, and it has thus become standard to quote the mean temperature in the radial region = 0.15−1× r500 as the most reliable single observable mass proxy for clusters (e.g. Arnaud et al. 2005; Pratt et al. 2008)1.”
Total mass biases in X-ray galaxy clusters (2008, background): “…& 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. Smith et al. 2002; Mahdavi et al. 2008).”
CLASH-VLT: The mass, velocity-anisotropy, and pseudo-phase-space density profiles of the z = 0.44 galaxy cluster MACS J1206.2-0847 (2013, background): “…of clusters (e.g. Carlberg et al. 1997a; Geller et al. 1999; van der Marel et al. 2000; King et al. 2002; Biviano & Girardi 2003; Rines et al. 2003a; Kneib et al. 2003; Katgert et al. 2004; Arnaud et al. 2005; Broadhurst et al. 2005; Umetsu et al. 2011; Oguri et al. 2012; Okabe et al. 2013).”
Galaxy cluster X-ray luminosity scaling relations from a representative local sample (REXCESS) (2008, background): “…of the X-ray mass-temperature relation have shown percent-level agreement in normalisation and that the slope is not greatly different from the self-similar expectation (Arnaud et al. 2005; Vikhlinin et al. 2006), although it may be slightly steeper (Arnaud et al. 2005; Sun et al. 2008).”
A Census of Baryons in Galaxy Clusters and Groups (2007, methodology): “A similar analysis can be performed for r200 using the sample of Arnaud et al. (2005), but with the limitation that only five clusters in this sample have published velocity dispersions.”
The Atacama Cosmology Telescope: A Catalog of >4000 Sunyaev–Zel’dovich Galaxy Clusters (2020, methodology): “We use the Arnaud et al. (2005) mass–temperature relation to convert M500c to temperature at a given cluster redshift, and then we apply the formulae of Itoh et al. (1998) to calculate frel at each frequency.”
A WEAK LENSING STUDY OF X-RAY GROUPS IN THE COSMOS SURVEY: FORM AND EVOLUTION OF THE MASS–LUMINOSITY RELATION (2009, background): “In contrast, the evolution of the LX −M relation is still under much debate with certain authors finding that the LX −M relation evolves in a self-similar fashion (Lumb et al. 2004; Arnaud et al. 2005; Kotov & Vikhlinin 2005; Maughan 2007) while others do not (Ettori et al. 2004).”
Radial temperature profiles for a large sample of galaxy clusters observed with XMM-Newton (2008, unknown): “We computeR180 from the mean temperature and the redshift (Arnaud et al. 2005): R180 = 1780 ( kTM 5 keV )1/2 h(z)−1 kpc, (3) whereh(z) = (Ωm(1 + z)3 + ΩΛ)1/2.”
LoCuSS: comparison of observed X-ray and lensing galaxy cluster scaling relations with simulations (2008, methodology): “We also performed the fitting with the slope fixed to the values 1.49 and 1.489 (consistent with our fit 1.65±0.26) as used in Arnaud et al. (2005) and Vikhlinin et al. (2006a).”
NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL PARAMETER RESULTS (2012, unknown): “…relating the X-ray luminosity, LX , to the size, r500: 22 1. r500 = 0.753 h−1 Mpc E(z) [LX/(10 44 h−2 erg s−1)]0.228 (Böhringer et al. 2007), derived from the LX -temperature relation of Ikebe et al. (2002) and the size-temperature relation of Arnaud et al. (2005), 2. r500 = 0.717 h−1 Mpc E1.”
The universal galaxy cluster pressure profile from a representative sample of nearby systems (REXCESS) and the Y-SZ-M-500 relation (2009, background): “R2500 is defined asR2500 = 0.44R500 from the scaling relations presented in Arnaud et al. (2005).”