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Register a new userConnecting Cluster Substructure in Galaxy Cluster Cores at z=0.2 With Cluster Assembly Histories
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We use semi-analytic models of structure formation to interpret gravitational lensing measurements of substructure in galaxy cluster cores (R<=250kpc/h) at z=0.2. The dynamic range of the lensing-based substructure fraction measurements is well matched to the theoretical predictions, both spanning f_sub~0.05-0.65. The structure formation model predicts that f_sub is correlated with cluster assembly history. We use simple fitting formulae to parameterize the predicted correlations: Delta_90 = tau_90 + alpha_90 * log(f_sub) and Delta_50 = tau_50 + alpha_50 * log(f_sub), where Delta_90 and Delta_50 are the predicted lookback times from z=0.2 to when each theoretical cluster had acquired 90% and 50% respectively of the mass it had at z=0.2. The best-fit parameter values are: alpha_90 = (-1.34+/-0.79)Gyr, tau_90 = (0.31+/-0.56)Gyr and alpha_50 = (-2.77+/-1.66)Gyr, tau_50 = (0.99+/-1.18)Gyr. Therefore (i) observed clusters with f_sub<~0.1 (e.g. A383, A1835) are interpreted, on average, to have formed at z>~0.8 and to have suffered <=10% mass growth since z~0.4, (ii) observed clusters with f_sub>~0.4 (e.g. A68, A773) are interpreted as, on average, forming since z~0.4 and suffering >10% mass growth in the ~500Myr preceding z=0.2, i.e. since z=0.25. In summary, observational measurements of f_sub can be combined with structure formation models to estimate the age and assembly history of observed clusters. The ability to ``age-date approximately clusters in this way has numerous applications to the large clusters samples that are becoming available.
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We present X-ray and spectroscopic confirmation of a cluster assembling from multiple, distinct galaxy groups at z=0.371. Initially detected in the Las Campanas Distant Cluster Survey, the structure contains at least four X-ray detected groups that lie within a maximum projected separation of 4 Mpc and within dv=550 km/s of one another. Using Chandra imaging and wide-field optical spectroscopy, we show that the individual groups lie on the local sigma-T relation, and derive a total mass of M>=5e14 solar masses for the entire structure. We demonstrate that the groups are gravitationally bound to one another and will merge into a single cluster with >=1/3 the mass of Coma. We also find that although the cluster is in the process of forming, the individual groups already have a higher fraction of passive members than the field. This result indicates that galaxy evolution on group scales is key to developing the early-type galaxies that dominate the cluster population by z~0.
The thesis work is focused on the analysis of the galaxy clusters ABCG 209, at z~0.2, which is characterized by a strong dynamical evolution. The data sample used is based mainly on new optical data (EMMI-NTT: B, V and R band images and MOS spectra), acquired in October 2001 at the European Southern Observatory in Chile. Archive optical data (CFHR12k: B and R images), and X-ray (Chandra) and radio (VLA) observations are also analysed. The main goal of the present analysis is the investigation of the connection between internal cluster dynamics and star formation history, aimed at understanding the complex mechanisms of cluster formation and evolution. The analysis of the internal dynamics of the cluster and the study of the galaxy luminosity function (LF) suggest an observational scenario in which ABCG 209 is undergoing a strong dynamical evolution with the merging of two or more subclumps along the SE-NW direction in a plane which is not parallel to the plane of sky. The effect of cluster environment on the global properties of the cluster galaxies is examined through the analysis of the LFs, colour-magnitude relations, and average colours.Moreover cluster dynamics and large-scale structure have a strong influence on galaxy evolution, so it is performed a detailed study of spectroscopic properties of 102 luminous member galaxies. All the results support an evolutionary scenario in which ABCG 209 is characterized by a sum of two components: an old galaxy population, formed very earlier (z >~ 3), and a younger population of infalling galaxies. Moreover this cluster may have experimented 1 or 2 Gyrs ago a merging with an infalling galaxy group, as indicated also by the previous dynamical analysis.
We quantify the star formation (SF) in the inner cores ($mathcal{R}$/$R_{200}$$leq$0.3) of 24 massive galaxy clusters at 0.2$lesssim$$z$$lesssim$0.9 observed by the $Herschel$ Lensing Survey and the Cluster Lensing and Supernova survey with $Hubble$. These programmes, covering the rest-frame ultraviolet to far-infrared regimes, allow us to accurately characterize stellar mass-limited ($mathcal{M}_{*}$$>$$10^{10}$ $M_{odot}$) samples of star-forming cluster members (not)-detected in the mid- and/or far-infrared. We release the catalogues with the photometry, photometric redshifts, and physical properties of these samples. We also quantify the SF displayed by comparable field samples from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. We find that in intermediate-$z$ cluster cores, the SF activity is suppressed with respect the field in terms of both the fraction ($mathcal{F}$) of star-forming galaxies (SFG) and the rate at which they form stars ($mathcal{SFR}$ and $smathcal{SFR} = mathcal{SFR}/mathcal{M}_{*}$). On average, the $mathcal{F}$ of SFGs is a factor $sim$$2$ smaller in cluster cores than in the field. Furthermore, SFGs present average $mathcal{SFR}$ and $smathcal{SFR}$ typically $sim$0.3 dex smaller in the clusters than in the field along the whole redshift range probed. Our results favour long time-scale quenching physical processes as the main driver of SF suppression in the inner cores of clusters since $z$$sim$0.9, with shorter time-scale processes being very likely responsible for a fraction of the missing SFG population.
Many processes within galaxy clusters, such as those believed to govern the onset of thermally unstable cooling and AGN feedback, are dependent upon local dynamical timescales. However, accurately mapping the mass distribution within individual clusters is challenging, particularly towards cluster centres where the total mass budget has substantial radially-dependent contributions from the stellar, gas, and dark matter components. In this paper we use a small sample of galaxy clusters with deep Chandra observations and good ancillary tracers of their gravitating mass at both large and small radii to develop a method for determining mass profiles that span a wide radial range and extend down into the central galaxy. We also consider potential observational pitfalls in understanding cooling in hot cluster atmospheres, and find tentative evidence for a relationship between the radial extent of cooling X-ray gas and nebular H-alpha emission in cool core clusters. Amongst this small sample we find no support for the existence of a central entropy floor, with the entropy profiles following a power-law profile down to our resolution limit.
A large fraction of the stellar mass in galaxy clusters is thought to be contained in the diffuse low surface brightness intracluster light (ICL). Being bound to the gravitational potential of the cluster rather than any individual galaxy, the ICL contains much information about the evolution of its host cluster and the interactions between the galaxies within. However due its low surface brightness it is notoriously difficult to study. We present the first detection and measurement of the flux contained in the ICL at z~1. We find that the fraction of the total cluster light contained in the ICL may have increased by factors of 2-4 since z~1, in contrast to recent findings for the lack of mass and scale size evolution found for brightest cluster galaxies. Our results suggest that late time buildup in cluster cores may occur more through stripping than merging and we discuss the implications of our results for hierarchical simulations.
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