Simulating the effect of active galactic nuclei feedback on the metal enrichment of galaxy clusters

Fabjan, D.; Borgani, S.; Tornatore, L.; Saro, A.; Murante, Giuseppe; Dolag, K.

doi:10.1111/j.1365-2966.2009.15794.x

Cited by 253 publications

(361 citation statements)

References 122 publications

(312 reference statements)

Supporting

Mentioning

312

Contrasting

Order By: Relevance

“…Roediger et al (2007) studied the effect of bubble-induced motions on metallicity profiles through 3D hydro simulations. The new simulation by Fabjan et al (2010) showed a less steep central Fe peak including feedback from AGN in cD galaxies. The observed small scatter in the Fe abundance slope within 0.1r 180 in the cD clusters suggests a common process of metal supply and ejection in the cD galaxies.…”

Section: Fe Profiles Within the Cool Core Regionsmentioning

confidence: 81%

Radial profiles of Fe abundance in the intracluster medium of nearby clusters observed withXMM-Newton

Matsushita

2011

A&A

View full text Add to dashboard Cite

Aims. The abundances of Fe in the intracluster medium of nearby (z < 0.08) clusters were measured up to 0.3 ∼ 0.5r 180 . Methods. We analyzed 28 clusters of galaxies observed with XMM-Newton. We derived Fe abundances from the flux ratios of Fe lines to the continuum within an energy range of 3.5−6 keV to minimize and evaluate systematic uncertainties. Results. The radial profiles of the Fe abundances of relaxed clusters with a cD galaxy at their X-ray peak have similar slopes. These clusters show similar enhancements in the Fe abundance within 0.1r 180 , and at 0.1−0.3r 180 , they have flatter Fe abundance profiles at 0.4 ∼ 0.5 solar, with a small scatter. Most other clusters, including merging clusters, also have similar Fe abundance profiles beyond 0.1r 180 . These clusters may have universal metal enrichment histories, and a significant amount of Fe was synthesized at a very early stage in cluster formation. Mergers of clusters can destroy the central Fe peak.

show abstract

Section: Fe Profiles Within the Cool Core Regionsmentioning

confidence: 81%

Radial profiles of Fe abundance in the intracluster medium of nearby clusters observed withXMM-Newton

Matsushita

2011

A&A

View full text Add to dashboard Cite

show abstract

“…These measures represent the "footprint" of cosmic star formation history and are crucial to tracing the effect of SN feedback on the ICM at different cosmic epochs (e.g. Ettori 2005;Calura et al 2007;Cora et al 2008;Fabjan et al 2010). …”

Section: Introductionmentioning

confidence: 99%

The evolution of the spatially resolved metal abundance in galaxy clusters up toz= 1.4

Ettori

Baldi

Balestra

et al. 2015

A&A

View full text Add to dashboard Cite

Context. We present the combined analysis of the metal content of 83 objects in the redshift range 0.09−1.39, and spatially resolved in the three bins (0−0.15, 0.15−0.4, >0.4) R 500 , as obtained with similar analysis using XMM-Newton data in our previous two papers. Aims. By combining these two large data sets, we investigate the relations between abundance, temperature, radial position and redshift holding in the intracluster medium. Methods. We fit functional forms to the combination of the different physical quantities of interest, i.e., intracluster medium (ICM) metal abundance, radius, and redshift. We use the pseudo-entropy ratio to separate the cool core (CC) cluster population, where the central gas density tends to be relatively higher, cooler and more metal rich, from the non-cool core systems. Results. The average, redshift-independent, metal abundance measured in the three radial bins decreases moving outwards, with a mean metallicity in the core that is even three (two) times higher than the value of 0.16 times the solar abundance in Anders & Grevesse (1989, Geochim. Cosmochim. Acta, 53, 197) estimated at r > 0.4 R 500 in CC (NCC) objects. We find that the values of the emission-weighted metallicity are well fitted by the relation Z(z) = Z 0 (1 + z) −γ at the given radius. A significant scatter, intrinsic to the observed distribution and of the order of 0.05−0.15, is observed below 0.4 R 500 . The nominal best-fit value of γ is significantly different from zero (>3σ) in the inner cluster regions (γ = 1.6 ± 0.2) and in CC clusters only. These results are also confirmed with a bootstrap analysis, which provides a still significant negative evolution in the core of CC systems (P > 99.9 per cent, when counting the number of random repetitions, which yields γ > 0). No redshift evolution is observed when regions above the core (r > 0.15 R 500 ) are considered. A reasonable good fit of both the radial and redshift dependence is provided from the functional form Z(r, z) = Z 0 (1 + (r/0.15 R 500 ) 2 ) −β (1 + z) −γ , with (Z 0 , β, γ) = (0.83 ± 0.13, 0.55 ± 0.07, 1.7 ± 0.6) in CC clusters and (0.39 ± 0.04, 0.37 ± 0.15, 0.5 ± 0.5) for NCC systems. Conclusions. Our results represent the most extensive study of the spatially resolved metal distribution in the cluster plasma as function of redshift. Our study defines the limits that numerical and analytic models describing the metal enrichment in the ICM have to meet.

show abstract

“…The main argument in favour of this mode is that the AGN activity is directly tied to the state of the diffuse gas because the Bondi accretion rate depends on the gas density and temperature in the vicinity of the black hole (Allen et al 2006). For this reason, this is the fueling mode most commonly invoked in cosmological simulations of galaxies, galaxy groups and clusters of galaxies (e.g., Di Matteo, Springel & Hernquist 2005;Fabjan et al 2010;Dubois et al 2011;Bellovary et al 2013;Le Brun et al 2014). However, a detailed analysis of AGN activity in galaxy clusters (Rafferty et al 2006;McNamara, Rohanizadegan & Nulsen 2011) indicates that the hot-mode accretion is much too small (by orders of magnitude) to account for the observed outbursts (but see Fujita, Kawakatu & Shlosman 2014).…”

Section: Introductionmentioning

confidence: 99%

The regulation of star formation in cool-core clusters: imprints on the stellar populations of brightest cluster galaxies

Loubser

Babul

Hoekstra

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

A fraction of brightest cluster galaxies (BCGs) shows bright emission in the UV and the blue part of the optical spectrum, which has been interpreted as evidence of recent star formation. Most of these results are based on the analysis of broadband photometric data. Here, we study the optical spectra of a sample of 19 BCGs hosted by X-ray luminous galaxy clusters at 0.15 < z < 0.3, a subset from the Canadian Cluster Comparison Project (CCCP) sample. We identify plausible star formation histories of the galaxies by fitting Simple Stellar Populations (SSPs) as well as composite populations, consisting of a young stellar component superimposed on an intermediate/old stellar component, to accurately constrain their star formation histories. We detect prominent young (∼ 200 Myr) stellar populations in 4 of the 19 galaxies. Of the four, the BCG in Abell 1835 shows remarkable A-type stellar features indicating a relatively large population of young stars, which is extremely unusual even amongst star forming BCGs. We constrain the mass contribution of these young components to the total stellar mass to be typically between 1% to 3%, but rising to 7% in Abell 1835. We find that the four of the BCGs with strong evidence for recent star formation (and only these four galaxies) are found within a projected distance of 5 kpc of their host cluster's X-ray peak, and the diffuse, X-ray gas surrounding the BCGs exhibit a ratio of the radiative cooling-to-free-fall time (t c /t ff ) of ≤ 10. These are also some of the clusters with the lowest central entropy. Our results are consistent with the predictions of the precipitation-driven star formation and AGN feedback model, in which the radiatively cooling diffuse gas is subject to local thermal instabilities once the instability parameter t c /t ff falls below ∼ 10, leading to the condensation and precipitation of cold gas. The number of galaxies in our sample where the host cluster satisfies all the criteria for recent and ongoing star formation is small, but their stellar populations suggest a timescale for star formation to restart of the order of ∼ 200 Myrs.

show abstract

Simulating the effect of active galactic nuclei feedback on the metal enrichment of galaxy clusters

Cited by 253 publications

References 122 publications

Radial profiles of Fe abundance in the intracluster medium of nearby clusters observed withXMM-Newton

Radial profiles of Fe abundance in the intracluster medium of nearby clusters observed withXMM-Newton

The evolution of the spatially resolved metal abundance in galaxy clusters up toz= 1.4

The regulation of star formation in cool-core clusters: imprints on the stellar populations of brightest cluster galaxies

Contact Info

Product

Resources

About