Calibration of the galaxy cluster M-500-Υ-x relation with XMM-Newton

By M. Arnaud, E. Pointecouteau, G. W. P. S. D. CEA-Saclay, F. Cesr, F. M. Garching, Heidelberg · Germany. 2007

165 citations recorded by the source corpus.

The quantity YX, the product of the X-ray temperature TX and gas mass Mg, has recently been proposed as a robust low-scatter mass indicator for galaxy clusters. Using precise measurements from XMM-Newton data of a sample of 10 relaxed nearby clusters, spanning a YX range of 10 13 -10 15 MkeV, we investigate the M500-YX relation. The M500-YX data exhibit a power law relation with slope α = 0.548 ± 0.027, close to the self-similar value (3/5) and independent of the mass range considered. However, the normalisation is ∼20% below the prediction from numerical simulations including cooling and galaxy feedback. We discuss two effects that could contribute to the normalisation offset: an underestimate of the true mass due to the hydrostatic equilibrium assumption used in X-ray mass estimates, and an underestimate of the hot gas mass fraction in the simulations. A comparison of the functional form and scatter of the relations between various observables and the mass suggest that YX may indeed be a better mass proxy than TX or Mg,500.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/0913afc7c3ea73843c7afce549d423dc3465785e

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

Jet-regulated cooling catastrophe (2010, background): “Their gas fraction is the best fit to data from Vikhlinin et al. (2006), Arnaud et al. (2007) and Sun et al. (2009). a modest fraction of the gas is expelled by the AGN outside of the cluster.”
X-ray spectroscopy of galaxy clusters: studying astrophysical processes in the largest celestial laboratories (2009, background): “9 Left The mass–temperature relation of a sample of regular clusters from (Arnaud et al. 2007).”
Toward a Halo Mass Function for Precision Cosmology: The Limits of Universality (2008, background): “…2006; Kravtsov et al. 2006) and were shown to exist observationally (e.g., Mohr et al. 1999; Lin et al. 2004; Vikhlinin et al. 2006; Maughan 2007; Arnaud et al. 2007; Sheldon et al. 2007; Zhang et al. 2008) in the case when both observables and masses are defined within a certainspherical radius…”
THE LARGE-SCALE BIAS OF DARK MATTER HALOS: NUMERICAL CALIBRATION AND MODEL TESTS (2010, background): “This expectation is borne out for observables such as gas mass, core-excised luminosity, integrated SZ flux or its X-ray analog,YX (e.g., Mohr et al. 1999; Vikhlinin et al. 2006; Zhang et al. 2008; Vikhlinin et al. 2009; Arnaud et al. 2007, 2009; Sun et al. 2009).”
MASSIVE HALOS IN MILLENNIUM GAS SIMULATIONS: MULTIVARIATE SCALING RELATIONS (2009, result): “Figure 8 compares the mass scaling of ICM mass fractions at redshift zero in the models to XMM measurements for local clusters (Arnaud et al. 2007; Sun et al. 2009).”
CHANDRA CLUSTER COSMOLOGY PROJECT. II. SAMPLES AND X-RAY DATA REDUCTION (2008, background): “The observed Mtot–YX relation does follow very closely the expected self-similar scaling of Equation (11) (Figure 11; see also Arnaud et al. 2007).”
LoCuSS: comparison of observed X-ray and lensing galaxy cluster scaling relations with simulations (2008, methodology): “The comparison between our sample and the samples in Vikhlinin et al. (2006a), Maughan et al. (2007) and Arnaud et al. (2007) might indicate that the slope of the M−YX relation varies as a function of the mass range of the sample.”
NINE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL PARAMETER RESULTS (2012, methodology): “The mass (hence r500) for the scaling relation 1 is estimated using the hydrostatic equilibrium, while that for the scaling relations 2 and 3 is estimated using the M500-YX relation of Arnaud et al. (2007).”
SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION (2010, unknown): “Arnaud et al. (2007) find that the X-ray observed integrated pressure enclosed within r500, YX ≡ Mgas,500TX , for a given M500 is about a factor of 0.75 times the prediction from the Cooling+SF simulation of Nagai et al. (2007).”
CHANDRA STUDIES OF THE X-RAY GAS PROPERTIES OF GALAXY GROUPS (2008, result): “Our best-fit is also consistent with the XMM-Newton result by Arnaud et al. (2007) (10 clusters at YX > 10 13M⊙ keV), on both the slope (0.548±0.027) and the normalization (within ∼ 3%).”
STELLAR AND TOTAL BARYON MASS FRACTIONS IN GROUPS AND CLUSTERS SINCE REDSHIFT 1 (2009, methodology): “Therefore, we have to resort to an estimate of the mean trend of the gas mass fraction as a function of M500 established from an independent sample of well observed groups and clusters at z ≤ 0.2, selected from the samples of Vikhlinin et al. 2006 (V06), Arnaud et al. 2007 (APP07) and Sun et al. 200”
Galaxy cluster X-ray luminosity scaling relations from a representative local sample (REXCESS) (2008, methodology): “Luminosities and their associated scaling relations are given in Appendix B. Spectroscopic temperatures were measured in the [0.15 − 0.75]R500 aperture2 (referred to hereafter asT3) from iteration about theM500 − YX relation of Arnaud et al. (2007).”
The universal galaxy cluster pressure profile from a representative sample of nearby systems (REXCESS) and the Y-SZ-M-500 relation (2009, methodology): “The local M500–YX relation for relaxed clusters has recently been calibrated (Nagai et al. 2007; Maughan 2007; Arnaud et al. 2007; Vikhlinin et al. 2009), with excellent agreement achieved between various observations (e.g., see Arnaud et al. 2007).”
Gas entropy in a representative sample of nearby X-ray galaxy clusters (REXCESS): relationship to gas mass fraction (2009, methodology): “We estimateR500 iteratively as described in Kravtsov et al. (2006), from theupdated calibration of theM500–YX relation obtained by combining the Arnaud et al. (2007) results from nearby relaxed clusters with REXCESS data from morphologically relaxed systems.”
Scaling Properties of a Complete X-ray Selected Galaxy Group Sample (2014, result): “In contrast to Mgas, LX, and T the agreement between the slope and normalization of different works (e.g., Arnaud et al. 2007; Maughan 2007; Vikhlinin et al. 2009; Sun et al. 2009) is very good and is very close to the self-similar scenario independently of the fitting method.”
The MCXC: a meta-catalogue of x-ray detected clusters of galaxies (2010, methodology): “…and scaling relationshave recently been derived (Mantz et al. 2009), the mass proxy relations are typically separately calibrated using deep observations of well-understood and if possible representative samples (e.g., Arnaud et al. 2007; Maughan 2007; Vikhlinin et al. 2009; Pratt et al. 2009).”