X-ray Spectroscopy of the Cluster of Galaxies Abell 1795 with XMM-Newton

By T. Tamura, J. Kaastra, J. R. Peterson, F. Paerels, J. Mittaz, S. Trudolyubov, G. Stewart, A. C. Fabian, R. Mushotzky, D. Lumb and 1 more. 2000

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The initial results from XMM-Newton observations of the rich cluster of galaxies Abell 1795 are presented. The spatially-resolved X-ray spectra taken by the European Photon Imaging Cameras (EPIC) show a temperature drop at a radius of $\sim 200$ kpc from the cluster center, indicating that the ICM is cooling. Both the EPIC and the Reflection Grating Spectrometers (RGS) spectra extracted from the cluster center can be described by an isothermal model with a temperature of $\sim 4$ keV. The volume emission measure of any cool component ($<1$ keV) is less than a few % of the hot component at the cluster center. A strong OVIII Lyman-alpha line was detected with the RGS from the cluster core. The O abundance and its ratio to Fe at the cluster center is 0.2--0.5 and 0.5--1.5 times the solar value, respectively.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

What Shapes the Luminosity Function of Galaxies? (2003, background): “…means by which the supply of cold gas to the galaxy disk may be reduced is suggested by recent Chandra and XMM observations of galaxy clusters (Peterson et al. 2001; Tamura et al. 2001; Fabian et al. 2001; Johnstone et al. 2002; Böhringer et al. 2002; McNamara et al. 2001; Nulsen et al. 2002).”
Temperature Profiles of Nearby Clusters of Galaxies (2001, methodology): “…where temperature profiles derived from XMM-Newton data are published, i.e. Coma cluster (Arnaud et al. 2001a) and A1795 (Arnaud et al. 2001b, Tamura et al. 2001), we have overplotted the XMM-Newton profile on our BeppoSAX profile (after converting their 90% uncertainties to our 1σ…”
The hydrodynamics of dead radio galaxies (2002, unknown): “By performing detailed emission line spectroscopy of several cooling flow clusters (e.g., Abell 1835, Peterson et al. 2001; Abell 1795, Tamura et al. 2001) with the reflection grating spectrometer (RGS) on XMM-Newton, one can probe the detailed temperature distribution of the ICM.”
The detection of molecular gas in the central galaxies of cooling flow clusters (2001, background): “…XMM-Newton X-ray observations that appear to show a deficit of X-ray line emission from the coolest gas components in several strong cooling flows (Tamura et al. 2001, Peterson et al. 2001) and recent Chandra observations indicating that cooling flows do not extend to large radii and have…”
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).”
Nonhydrostatic Gas in the Core of the Relaxed Galaxy Cluster A1795 (2001, background): “It has had sufficient time to develop a cool core (e.g., Edge, Stewart, & Fabian 1992), although its precise nature is debated (Tamura et al. 2001).”
Feedback heating by cosmic rays in clusters of galaxies (2007, background): “…show that while the temperature is declining toward the center, there is a remarkable lack of emission lines from the gas at temperature below about ∼ 1/3 of the ambient cluster temperature (e.g., Peterson et al. (2001, 2003); Tamura et al. (2001); for a review see Peterson & Fabian (2006)).”
The Cluster-Scale AGN Outburst in Hydra A (2004, background): “Despite this, little of the gas cools below∼ 1 keV (e.g. Peterson et al. 2001; Tamura et al. 2001; Peterson et al. 2003; Kaastra et al. 2004).”
A deep Chandra observation of the Perseus cluster: shocks and ripples (2003, methodology): “As has been found for many clusters with Chandra and XMM–Newton data (Peterson et al. 2001, 2003; Tamura et al. 2001), there is little gas at lower temperatures.”
On the soft X-ray spectrum of cooling flows (2000, background): “6 D I S C U S S I O N We have shown that the XMM-Newton RGS soft X-ray spectra of cooling flows are difficult to interpret.”
Cold molecular gas in cooling flow clusters of galaxies (2003, background): “Recent X-ray observations by Chandra, see Fabian (2002), Voigt et al. (2002) and XMM-Newton (Peterson et al. 2001; Tamura et al. 2001) have confirmed the presence of radial gradients in temperature in the cores of several clusters of galaxies.”
The Coevolution of Galaxies and Supermassive Black Holes: Insights from Surveys of the Contemporary Universe (2014, background): “In reality, however, observations show that the gas temperatures in the cluster cores are at most a factor 3 below the value at large radii, and the amount of cooling gas is only about 10% of the cooling flow prediction (e.g. Peterson et al. 2001, 2003, David et al. 2001, Tamura et al. 2001).”
X‐ray properties of galaxy clusters and groups from a cosmological hydrodynamical simulation (2003, background): “Observational data from spatially resolved spectroscopy with the ASCA (e.g., Markevitch et al. 1998), Beppo–SAX (De Grandi & Molendi 2002) and XMM–Newton (e.g., Pratt & Arnaud 2002) satellites show that temperature profiles decline at cluster–centric distances larger than about one quarter of the vi”
AGN heating and ICM cooling in the HIFLUGCS sample of galaxy clusters (2008, background): “…of cool gas in their Article published by EDP Sciences 836 R. Mittal et al.: AGN heating in the HIFLUGCS sample of galaxy clusters cores (e.g. Tamura et al. 2001; Peterson et al. 2001; Kaastra et al. 2001; Peterson et al. 2003; Xu et al. 2002; Sakelliou et al. 2002; Sanders et al. 2008),…”
What is a cool-core cluster? a detailed analysis of the cores of the X-ray flux-limited HIFLUGCS cluster sample (2009, background): “More recently, grating spectra fromXMM (Peterson et al. 2001; Tamura et al. 2001b,a; Kaastra et al. 2001; Xu et al. 2002; Sakelliou et al. 2002; Peterson et al. 2003; Sanders et al. 2008) have revealed that the gas in central regions is not cooling at the rates predicted by the traditional cooling…”
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).”