Deep inside the core of Abell 1795: the Chandra view

By S. Ettori, A. C. Fabian, S. Allen, R. Johnstone. 2001

165 citations recorded by the source corpus.

We present X-ray spatial and spectral analysis of the Chandra data from the central of the cluster of galaxies Abell 1795. The plasma temperature rises outwards by a factor of 3, whereas the iron abundance decreases by a factor of 4. The spatial distribution of oxygen, neon, sulphur, silicon and iron shows that supernovae Type Ia dominate the metal enrichment process of the cluster plasma within the inner 150 kpc. Resolving both the gas density and temperature in nine radial bins, we recover the gravitational mass density profile and show that it flattens within 100 kpc as ρDM∝r-0.6 with a power-law index flatter than −1 at >3σ level. The observed motion of the central galaxy and the presence of excesses and deficits along the north–south direction in the brightness distribution indicate that the central cluster region is not relaxed. In the absence of any non-gravitational heating source, the data from the inner ∼200 kpc indicate the presence of a cooling flow with an integrated mass deposition rate of about 100 M⊙ yr−1. Over the same cluster region, the observed rate of 74 M⊙ yr−1 is consistent with the recent XMM-Newton Reflection Grating Spectrometer limit of 150 M⊙ yr−1.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/04ddd59beae9dcc815d0037dfee7873b32510f99

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Citations in the corpus

Chandra Observations of A2029: The Dark Matter Profile Down to below 0.01rvir in an Unusually Relaxed Cluster (2002, methodology): “: ð1Þ While r should strictly be iteratively calculated from the fitted density profile, it is easy to show that equation (1) is an excellent approximation to the correct r over the entire profile (e.g., Ettori et al. 2002a; see also our x 3.4).”
High-Resolution X-Ray Spectroscopic Constraints on Cooling-Flow Models for Clusters of Galaxies (2002, background): “The spatial distribution of H is remarkably similar to the coolest X-rays (Ettori et al. 2002), and the total luminosity is marginally sufficient to account for the missing soft X-ray luminosity (Fabian et al. 2001), but again the dynamical problem of partial cooling is not easily solved by this mec”
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.”
X-ray Spectroscopy of Cooling Clusters (2005, background): “…obtained at high spectral resolution have been augmented with further studies at low resolution that attempt to study the spatial distribution in greater detail (David et al. 2001; Böhringer et al. 2001; Molendi & Pizzolato 2001; Schmidt et al. 2001; Ettori et al. 2002; Johnstone et al. 2001).”
Feedback and metal enrichment in cosmological smoothed particle hydrodynamics simulations ¿ I. A model for chemical enrichment (2005, background): “…(e.g. Garnett & Shields 1987; Skillman, Kennicutt & Hodge 1989; Brodie & Huchra 1991; Zaritsky, Kennicutt & Huchra 1994; Mushotzky et al. 1996; Ettori et al. 2002; Tremonti et al. 2004; Lamareille et al. 2004) as well as at intermediate and high redshifts (e.g. Prochaska & Wolfe 2002;…”
CAUSE AND EFFECT OF FEEDBACK: MULTIPHASE GAS IN CLUSTER CORES HEATED BY AGN JETS (2011, background): “All the features of the pure CF model, discussed above, are in contrast with observations of galaxy clusters (Peterson et al. 2001, 2003; Ettori et al. 2002; Tamura et al. 2003; Peterson & Fabian 2006).”
Models of Galaxy Clusters with Thermal Conduction (2002, methodology): “For A1795, although both Chandra and XMM-Newton data sets are available (Ettori et al. 2002; Tamura et al. 2001), we do not use the XMM-Newton temperature profile because it is undeprojected.”
X‐ray properties of galaxy clusters and groups from a cosmological hydrodynamical simulation (2003, methodology): “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”
LoCuSS: comparison of observed X-ray and lensing galaxy cluster scaling relations with simulations (2008, unknown): “97 by Ettori et al. (2002), and S ∝ r0.”
Chemical enrichment of the intracluster and intergalactic medium in a hierarchical galaxy formation model (2003, background): “E-mail: gdelucia@mpa-garching.mpg.de The last decade has witnessed the accumulation of a large amount of data on the chemical composition of the intracluster gas (Mushotzky et al. 1996; De Grandi & Molendi 2001; Ettori et al. 2002).”
Thermal conduction and reduced cooling flows in galaxy clusters (2003, background): “…[7] McNamara et al. 2000; [8] Matsushita et al. 2002; [9] Molendi 2002; [10] Böhringer et al. 2001; [11] Young et al. 2002; [12] Allen et al. 2002; [13] Ettori et al. 2001; [14] Ettori et al. 2002; [15] Tamura et al. 2001; [16] Schmidt et al. 2001; [17] Johnstone et al. 1998; [18] Allen at al.”
The Dark Matter Distribution in the Central Regions of Galaxy Clusters: Implications for Cold Dark Matter (2003, background): “In general, X-ray analyses have led to wide ranging results, with β ranging from ≃0.6 (Ettori et al. 2002) through ≃1.2 (Lewis, Buote & Stocke 2003) to ≃1.9 (Arabadjis, Bautz & Garmire 2002).”
Chandra observations of Abell 2199 (2002, methodology): “Another approach, used on the cluster Abell 1795, is described by Ettori et al. (2002).”