Chandra observations of Abell 2199

By R. Johnstone, S. Allen, A. C. Fabian, Jeremy S. Sanders. 2002

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We present results from an analysis of two Chandra observations of the rich, nearby galaxy cluster Abell 2199. We find evidence (having corrected for projection effects) for radial gradients in temperature and metallicity in the X-ray emitting gas: the temperature drops from kT ∼ 4.2 keV at R = 200 kpc to 1.6 keV within R = 5 kpc of the centre. The metallicity rises from ∼0.3 solar at R = 200 kpc to ∼0.7 solar at R = 30 kpc before dropping to 0.3 solar within the central 5 kpc. We find evidence for structure in the surface brightness distribution associated with the central radio source 3C 338. No evidence is found for the gas having a large spread in temperature at any particular location despite the cooling time being short (<10 9 yr) within the central ∼15 kpc. Heating and mass cooling rates are calculated for various assumptions about the state of the gas.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/cba1f8dcb74096ae4de79df0cc20274b22ed6fe8

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Citations in the corpus

Thermal instability and the feedback regulation of hot haloes in clusters, groups and galaxies (2011, background): “We fix the outer electron number density to be ne,out = 0.0015 cm −3 for all halo masses, a value observed for Abell 2199 at 200 kpc (see Johnstone et al. 2002; see also Sharma et al. 2009 for details of the setup).”
Chandra Observations of A2029: The Dark Matter Profile Down to below 0.01rvir in an Unusually Relaxed Cluster (2002, background): “…build a picture of large-scale radial temperature variations (e.g., Irwin & Bregman 2001; Ettori, de Grandi, & Molendi 2002a), as well as two-dimensional temperature maps of disturbed systems (e.g., Briel & Henry 1994; Markevitch et al. 1998, 1999; de Grandi & Molendi 1999; Johnstone et al. 2002).”
A dynamical model for the distribution of dark matter and gas in galaxy clusters (2003, unknown): “…spectroscopic data coming from the Beppo-SAX and Chandra satellites (see, e.g., Allen, Schmidt & Fabian 2001; De Grandi & Molendi 2002; Ettori, De Grandi & Molendi 2002a; Ettori et al. 2002b; Johnstone et al. 2002), the complexity of the thermal structure inside galaxy clusters has been revealed.”
Chandra Temperature Profiles for a Sample of Nearby Relaxed Galaxy Clusters (2004, background): “…to the central region, typically within 0.2–0.3 virial radii (David et al. 2001; Schmidt et al. 2001; Mazzotta et al. 2002; Sun et al. 2003a, 2003b; Johnstone et al. 2002; Lewis et al. 2003; Buote & Lewis 2004), although attemptsweremade to go to larger radii (Markevitch et al. 2005; Markevitch &…”
Feedback heating by cosmic rays in clusters of galaxies (2007, background): “In the upper panels of Figure 4, the observational temperature and electron density profiles (Johnstone et al. 2002) are also shown.”
Models of Galaxy Clusters with Thermal Conduction (2002, background): “The observations place an upper limit on the mass accretion rate in a few clusters of about 10%–20% of the nominal value needed to explain the observed X-ray flux (e.g., David et al. 2001; Schmidt, Allen, & Fabian 2001; Johnstone et al. 2002).”
A deep Chandra observation of the Perseus cluster: shocks and ripples (2003, background): “The ripples or sound waves may disperse energy throughout the cooling region, which is one important criterion for a successful heat source with which to balance radiative cooling (Fabian 2001; Johnstone et al. 2002).”
High-Resolution X-Ray Spectroscopic Constraints on Cooling-Flow Models for Clusters of Galaxies (2002, background): “…European Photon Imaging Cameras (EPIC) and Chandra ACIS observations, where spectral fits have yielded significantly smaller _M values than expected (David et al. 2001; Böhringer et al. 2001; Molendi & Pizzolato 2001; Schmidt, Allen, & Fabian 2001; Ettori et al. 2002; Johnstone et al. 2002).”
Investigating AGN heating in a sample of nearby clusters (2006, background): “W G 4.8 2.6 28 A85 N G 5.3 7.0 14 9.0 ± 0.4 47.6 ± 1.3 81.4 ± 10.7 1.71 ± 0.23 2.54 ± 0.71 S G 6.4 8.6 22 A262 E 2.4 1.8 3.2 0.5 ± 0.0 31.4 ± 0.8 28.9 ± 3.20 0.92 ± 0.10 0.93 ± 0.10 W 2.7 1.9 3.4 A478 NE G 4.0 6.9 9.8 78.2 ± 3.0 84.8 ± 2.7 18.8 ± 2.63 0.22 ± 0.03 0.13 ± 0.02 SW G 4.5 7.7 10.7 A1795 ”
Spatially resolved X-ray spectroscopy of cooling clusters of galaxies (2003, unknown): “Many recent studies (David et al. 2001, Molendi & Pizzolato 2001, Johnstone et al. 2002, Matsushita et al. 2002, Schmidt et al. 2002, Sanders & Fabian 2002, Buote 2002) have argued to varying degrees that the temperature distribution at each radius is isothermal or very close to isothermal at each…”
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).”
Hot Gas In and Around Elliptical Galaxies (2003, background): “One of the most remarkable peculiarities in the abundance profiles are the central minima observed for almost all elements in M87 (Gastaldello & Molendi 2002), in NGC 4636 (Loewenstein & Mushotzky), in AWM 7 (Johnstone et al. 2002) and elsewhere.”
Thermal conduction and reduced cooling flows in galaxy clusters (2003, methodology): “Voigt et al. (2002) calculated the conductivity required to replace heat loss as a function of radius using the observed temperature and density profiles of Abell 1835 (Schmidt et al. 2001) and Abell 2199 (Johnstone et al. 2002).”
X‐ray properties of galaxy clusters and groups from a cosmological hydrodynamical simulation (2003, background): “Furthermore, Beppo–SAX (De Grandi & Molendi 2002; Ettori et al. 2002a), Chandra (Ettori et al. 2002b; Allen, Schmidt & Fabian 2001; Johnstone et al. 2002) and XMM–Newton (Tamura et al. 2001) data show that temperature profiles smoothly decline towards the cluster center.”
Cold molecular gas in cooling flow clusters of galaxies (2003, background): “Chandra images from Fabian et al. (2002) or Johnstone et al. (2002) have pointed out holes coincident with radio lobes and cold fronts showing the interaction between the radio source and the intra-cluster medium (e.g. in Hydra A, the Perseus cluster, Abell 1795, Abell 2199, the Virgo cluster).”
Comparing the temperatures of galaxy clusters from hydrodynamical N-body simulations to Chandra and XMM-Newton observations (2004, background): “…2003), cavities (Fabian et al. 2000; McNamara et al. 2000; Blanton et al. 2001; Markevitch et al. 2001; McNamara et al. 2001; Heinz et al. 2002; Johnstone et al. 2002; Mazzotta et al. 2002; Sanders & Fabian 2002; Smith et al. 2002; Young, Wilson & Mundell 2002), blobs and filaments (Fabian et…”