XMM-Newton observations of the cluster of galaxies Sérsic 159-03

By J. Kaastra, C. Ferrigno, T. Tamura, F. Paerels, J. R. Peterson, J. Mittaz. 2000

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The cluster of galaxies Sersic 159-03 was observed with the XMM-Newton X-ray observatory as part of the Guaranteed Time program. X-ray spectra taken with the EPIC and RGS instruments show no evidence for the strong cooling flow derived from previous X-ray observations. There is a significant lack of cool gas below 1.5 keV as compared to standard isobaric cooling flow models. While the oxygen is distributed more or less uniformly over the cluster, iron shows a strong concentration in the center of the cluster, slightly offset from the brightness center but within the central cD galaxy. This points to enhanced type Ia supernova activity in the center of the cluster. There is also an elongated iron-rich structure ex- tending to the east of the cluster, showing the inhomogeneity of the iron distribution. Finally, the temperature drops rapidly beyond 4' from the cluster center.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

High-Resolution X-Ray Spectroscopic Constraints on Cooling-Flow Models for Clusters of Galaxies (2002, background): “Surprisingly, the observed spectra reveal a remarkable systematic deficit of emission at the lowest temperatures, as compared to the multiphase model (Peterson et al. 2001; Tamura et al. 2001a, 2001b; Kaastra et al. 2001; Xu et al. 2002; Sakelliou et al. 2002).”
Chandra observations of Abell 2199 (2002, background): “…Reflection Grating Spectrometer (RGS) data of other clusters also show little evidence for long-lived, steady-state cooling flows, in which gas cools from the cluster virial temperature to below 106 K by emitting observed X-radiation (Peterson et al. 2001; Tamura et al. 2001; Kaastra et al. 2001).”
The cool-core bias in X-ray galaxy cluster samples - I. Method and application to HIFLUGCS (2010, background): “However, this picture was not confirmed by the latest generation of X-ray telescopes (XMM-Newton, Chandra), which found no spectroscopic evidence for the presence of the cooling gas in the central regions of clusters predicted by the cooling-flow model (Peterson et al. 2001; Kaastra et al. 2001).”
The Dust Opacity of Star‐forming Galaxies (2001, background): “…(Edge 2001) are countered by XMM data that do not support the presence of large amounts of cool gas in the center of some of the clusters and, therefore, do not require a large amount of dust to explain the soft X-ray spectral shape (Tamura et al. 2001; Kaastra et al. 2001; Peterson et al. 2001).”
Universal gas density and temperature profile (2001, background): “…of the cluster (well inside the gas core) as shown by recent Chandra(McNamara et al. 2000; Allen et al. 2001a, 2001b) and XMM–Newton(Arnaud et al. 2001a, 2001b; Kaastra et al. 2001) temperature profiles, but for the outer parts seems to be in good agreement with both simulations and observations.”
Hot Gas In and Around Elliptical Galaxies (2003, background): “Likewise, in cluster scale flows there is no evidence for gas cooling below ∼ 1 − 2 keV (Peterson et al. 2001; Tamura et al. 2001; Kaastra et al. 2001; Molendi & Pizzolato 2001; Böhringer et al. 2002; Matsushita et al. 2002).”
What is a cool-core cluster? a detailed analysis of the cores of the X-ray flux-limited HIFLUGCS cluster sample (2009, methodology): “S1101/Sérsic 159-03 Kaastra et al. (2001) provided a detailed analysis of theXMM-Newton RGSandEPIC data.”
On the prevalence of radio‐loud active galactic nuclei in brightest cluster galaxies: implications for AGN heating of cooling flows (2006, background): “…shown that the temperature of cluster cores does not fall below ∼30 per cent of that at large radii, and that the amount of cooling gas is only about 10 per cent of that predicted for a classical cooling flow (e.g. David et al. 2001; Kaastra et al. 2001; Peterson et al. 2001; Tamura et al. 2001).”
A primer on hierarchical galaxy formation: the semi-analytical approach (2006, background): “…taken by the Chandra and XMM-Newton satellites indicate a lack of cold gas (i.e. below 1-2 KeV) in the intra-cluster medium, suggesting that some form of heating mechanism may be preventing the gas from attaining these temperatures (Fabian et al. 2001; Kaastra et al. 2001; Peterson et al. 2001).”
Hydrodynamical simulations of cluster formation with central AGN heating (2005, background): “However, up to the present time, optical and X-ray observations have failed to detect the required amount of this cool gas, suggesting that it is simply not there (e.g. McNamara et al. 2000; Tamura et al. 2001; Balogh et al. 2001; Kaastra et al. 2001; Fabian et al. 2001; C© 2005 The Authors.”
X‐ray properties of galaxy clusters and groups from a cosmological hydrodynamical simulation (2003, background): “…the observational picture emerging from Chandra and XMM–Newton observations: the ICM in cluster central regions has temperatures between 1/2 and 1/4 of the virial temperature, with no signature for the presence of colder gas (e.g., Kaastra et al. 2001; Peterson et al. 2001; Böhringer et al. 2002).”
X-ray Spectroscopy of the Cluster of Galaxies Abell 1795 with XMM-Newton (2000, result): “This result for A 1795 is similar to what has been found in A 1835 (Peterson et al. 2001) and Sérsic 159-03 (Kaastra et al. 2001).”
Spatially resolved X-ray spectroscopy of cooling clusters of galaxies (2003, unknown): “However, the amount of cool gas at lower temperatures was much smaller than predicted by the isobaric cooling flow model (Sérsic 159−3, Kaastra et al. 2001; A 1835, Peterson et al. 2001; A 1795, Tamura et al. 2001a).”
The Sunyaev-Zel'dovich angular power spectrum as a probe of cosmological parameters (2002, background): “…the virial radius, roughly corresponding tor2500, which is just in the range ofChandrasatellite for medium redshift clusters (McNamara et al. 2000; Allen, Ettori, & Fabian 2001; Allen et al. 2001) and well withinXMM/Newtonor BeppoSax(Arnaud et al. 2001a; Arnaud et al. 2001b; Kaastra et al. 2001).”
Thermal conduction and reduced cooling flows in galaxy clusters (2003, background): “High resolution observations of cooling flow clusters with XMM- Newton and Chandra show no evidence for the large amounts of multiphase gas expected in the inner regions of these objects (Peterson et al. 2001; Tamura et al. 2001; Kaastra et al. 2001; Peterson 2002).”
Galaxies in a simulated ΛCDM Universe – I. Cold mode and hot cores (2008, background): “While such feedback may be needed to explain the absence of cold gas in cooling flow clusters (Kaastra et al. 2001; Peterson et al. 2003), semi-analytic models may overestimate its global importance by assuming incorrect halo gas profiles (and thus excessive cooling).”
X-ray Spectroscopy of Cooling Clusters (2005, background): “Nor is it apparent in the detailed XMM/RGS spectra of cool cluster cores (Peterson et al. 2001; Tamura et al. 2001a; Kaastra et al. 2001; Sakelliou et al. 2002; Peterson et al. 2003).”