Evidence for Rapid Redshift Evolution of Strong Cluster Cooling Flows

Samuele, Rocco; McNamara, B. R.; Vikhlinin, A.; Mullis, C. R.

doi:10.1088/0004-637x/731/1/31

Cited by 29 publications

(42 citation statements)

References 34 publications

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“…Moving at higher redshift, for instance, lower metal abundance associated with the inner regions suggest that less pronounced cool cores are resolved in our sample (see e.g. Santos et al 2010;Samuele et al 2011). …”

Section: Results On the Spatially Resolved Abundance Evolutionmentioning

confidence: 85%

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

Ettori

Baldi

Balestra

et al. 2015

A&A

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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.

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Section: Results On the Spatially Resolved Abundance Evolutionmentioning

confidence: 85%

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

Ettori

Baldi

Balestra

et al. 2015

A&A

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“…Morphologically complex, extended nebulae of warm (10 4 K), ionized gas are nearly ubiquitous in cool core clusters like the Phoenix cluster (Hu et al 1985;Johnstone et al 1987;Heckman et al 1989;Crawford et al 1999;Edwards et al 2007;Hatch et al 2007;McDonald et al 2010McDonald et al , 2011a)-so much so that Hα luminosity has often been used as an alternative classification of rapid ICM cooling (Donahue et al 1992;Samuele et al 2011;McDonald 2011). The most spectacular such nebulae is found in the nearby Perseus cluster (Conselice et al 2001;Fabian et al 2003;Hatch et al 2006), with multiple filaments extending radially from the central galaxy to the cooling radius (∼60 kpc).…”

Section: Introductionmentioning

confidence: 99%

The State of the Warm and Cold Gas in the Extreme Starburst at the Core of the Phoenix Galaxy Cluster (Spt-Clj2344-4243)

McDonald

Swinbank

Edge

et al. 2014

ApJ

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We present new optical integral field spectroscopy (Gemini South) and submillimeter spectroscopy (Submillimeter Array) of the central galaxy in the Phoenix cluster (SPT-CLJ2344-4243). This cluster was previously reported to have a massive starburst (∼800 M yr −1 ) in the central, brightest cluster galaxy, most likely fueled by the rapidly cooling intracluster medium. These new data reveal a complex emission-line nebula, extending for >30 kpc from the central galaxy, detected at [O ii]λλ3726, 3729, [O iii]λλ4959, 5007, Hβ, Hγ , Hδ, [Ne iii]λ3869, and He ii λ4686. The total Hα luminosity, assuming Hα/Hβ = 2.85, is L Hα = 7.6 ± 0.4 ×10 43 erg s −1 , making this the most luminous emission-line nebula detected in the center of a cool core cluster. Overall, the relative fluxes of the low-ionization lines (e.g., [O ii], Hβ) to the UV continuum are consistent with photoionization by young stars. In both the center of the galaxy and in a newly discovered highly ionized plume to the north of the galaxy, the ionization ratios are consistent with both shocks and active galactic nucleus (AGN) photoionization. We speculate that this extended plume may be a galactic wind, driven and partially photoionized by both the starburst and central AGN. Throughout the cluster we measure elevated high-ionization line ratios (e.g., He ii/Hβ, [O iii]/Hβ), coupled with an overall high-velocity width (FWHM 500 km s −1 ), suggesting that shocks are likely important throughout the interstellar medium of the central galaxy. These shocks are most likely driven by a combination of stellar winds from massive young stars, core-collapse supernovae, and the central AGN. In addition to the warm, ionized gas, we detect a substantial amount of cold, molecular gas via the CO(3-2) transition, coincident in position with the galaxy center. We infer a molecular gas mass of M H 2 = 2.2 ± 0.6 × 10 10 M , which implies that the starburst will consume its fuel in ∼30 Myr if it is not replenished. The L IR /M H 2 that we measure for this cluster is consistent with the starburst limit of 500 L /M , above which radiation pressure is able to disperse the cold reservoir. The combination of the high level of turbulence in the warm phase and the high L IR /M H 2 ratio suggests that this violent starburst may be in the process of quenching itself. We propose that phases of rapid star formation may be common in the cores of galaxy clusters, but so short-lived that their signatures are quickly erased and appear only in a subsample of the most strongly cooling clusters.

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“…This suppression of star formation (SF) is mainly caused by interactions among the densely packed galaxies (e.g., Moore et al 1996;Gnedin 2003), and to a lesser extent by interactions between the hot, X-ray emitting intracluster medium (ICM) and the galaxies. The brightest cluster galaxy (BCG) that usually sits at the bottom of the E-mail:jsantos@arcetri.astro.it potential well and is coincident with the peak of the cluster X-ray emission, is typically a very massive, bright, early type galaxy, that only rarely is associated with significant star formation activity (e.g., Samuele et al 2011;Rawle et al 2012;Fogarty et al 2015).…”

Section: Introductionmentioning

confidence: 99%

“…This is partly because different diagnostics are used (e.g., optical emission lines, UV continuum, farinfrared) that may be affected by dust emission and AGN contamination, but also because samples are often not representative. In particular, Samuele et al (2011) investigated the star formation activity in a sample of 77 BCGs drawn from a flux limited, X-ray selected cluster sample and reported a lack of star formation in that sample, based only on optical emission lines. In contrast, Rawle et al (2012) detected star formation in 15 out of 68 BCGs using a more robust diagnostic based on the FIR emission.…”

Section: Introductionmentioning

confidence: 99%

Starbursting brightest cluster galaxy: a Herschel view of the massive cluster MACS J1931.8−2634

Santos

Balestra

Tozzi

et al. 2015

Monthly Notices of the Royal Astronomical Society: Letters

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We investigate the dust-obscured star formation properties of the massive, X-ray selected galaxy cluster MACS J1931.8-2634 at z=0.352. Using far-infrared (FIR) imaging in the range 100-500µm obtained with the Herschel telescope, we extract 31 sources (2σ) within r ∼1 Mpc from the brightest cluster galaxy (BCG). Among these sources we identify six cluster members for which we perform an analysis of their spectral energy distributions (SEDs). We measure total infrared luminosity (L IR ), star formation rate (SFR) and dust temperature. The BCG, with L IR =1.4×1012 L is an Ultra Luminous Infrared Galaxy and hosts a type II AGN. We decompose its FIR SED into AGN and starburst components and find equal contributions from AGN and starburst. We also recompute the SFR of the BCG finding SFR=150±15 M yr −1 . We search for an isobaric cooling flow in the cool core using Chandra X-ray data, and find no evidence for gas colder than 1.8 keV in the inner 30 kpc, for an upper limit to the istantaneous mass-deposition rate of 58 M yr −1 at 95% c.l. This value is 3× lower than the SFR in the BCG, suggesting that the on-going SF episode lasts longer than the ICM cooling events.

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Evidence for Rapid Redshift Evolution of Strong Cluster Cooling Flows

Cited by 29 publications

References 34 publications

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

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

The State of the Warm and Cold Gas in the Extreme Starburst at the Core of the Phoenix Galaxy Cluster (Spt-Clj2344-4243)

Starbursting brightest cluster galaxy: a Herschel view of the massive cluster MACS J1931.8−2634

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