[PDF] Top 20 What are protoclusters? – Defining high redshift galaxy clusters and protoclusters

... At high redshift protoclusters are still expanding with the Universe before collapse occurs after z = ...of protoclusters decreases with time until z ∼ 1, after which they rapidly ...view, ... See full document

... instance, clusters detected in a flux-limited X-ray survey tend to be relaxed, with cool, dense cores driving the X-ray luminosity into higher mass ...Optically-selected clusters at high redshifts ... See full document

... discovered galaxy clusters, drawn from the XMM -Newton Distant Cluster Project (B¨ohringer et ...and clusters are identified by means of digital sky images and then ...promising high ... See full document

... from clusters to groups (Cavaliere, Menci & Tozzi 1999; Wu, Fabian & Nulsen 1998, 2000; Balogh, Babul & Patton 1999; Bower et ...of clusters (Ponman et ...supernova-driven galaxy winds at ... See full document

... host-galaxy redshift of ...host galaxy redshift of ...this galaxy are expected to be SNe ...highest redshift SN Ia with a spectroscopic redshift and the highest ... See full document

... In addition to the emission line galaxies, we see a higher mean EW([O ii ]) at larger radius. Figure 3.7 shows the coadded normalized spectra of all early types binned by radial zone; top to bottom, they trace the mean ... See full document

... with galaxy bulge mass and stellar velocity disper- sion (see reviews in ...and galaxy growth largely comes from theoretical models of galaxy ...the galaxy mass function ...in galaxy ... See full document

... identify clusters is to make use of their galaxy populations, mainly in optical and infrared (IR) ...identify clusters in the optical and IR data, but the idea is basically the same: the goal is to ... See full document

... semi-analytic galaxy evolution model based on the Millennium simulation and compared it to an observational sample of galax- ies in low-redshift ...low-redshift galaxy clusters, and ... See full document

... at high redshift and impose magnetic fields of variable strength and structure as summarised in Table 2 ...simulated clusters at low redshift well reproduce the statistics of observed ... See full document

... 200 galaxy cluster candidates at ...the Clusters Around Radio Loud AGN (CARLA) project (Wylezalek et ...The clusters were found in the fields of radio-loud active galactic nuclei (RLAGNs), includ- ... See full document

... In this chapter, I use the Sloan Digital Sky Survey to construct a sample of 625 brightest group and cluster galaxies (BCGs) together with control samples of non– BCGs matched in stellar mass, redshift, and color. ... See full document

... When choosing a blank- fi eld survey suitable for comparison, it is important to compare “ like-for-like ” ( i.e., Condon 2007 ) . For instance, broad-beam surveys can hide the multiplicity of DSFGs; multiplicity was fi ... See full document

... At high redshift ( z ∼ 3) we find that 90 per cent of progenitors are still active, confirming that star-forming galaxies are the dominant population in ...at high redshift (see ...the ... See full document

... Although DSFGs appear to be poor tracers of large structure below z . 2.5 (Miller et al. 2015), the situa- tion appears to be quite different by z ∼ 5 (Miller et al. 2016; Oteo et al. 2017b) – albeit care must be taken ... See full document

... and clusters in ...of protoclusters, so instead we use measurements of individ- ual protoclusters (Clements et ...observed protoclusters have more star formation than the simulated ... See full document

... semi-analytic galaxy formation models of Fanidakis et al. (2011) suggest that galaxy mergers are very important for determin- ing whether an AGN becomes ...the galaxy merger ...expect high ... See full document

... We can estimate the strength of the magnetic field in the cluster from rotation measurements, RM, towards the central ra- dio source in M87. Owen et al. (1990) find an average RM of about 1000 rad m − 2 with peaks around ... See full document

... We investigate the effect of the window function on the multipole power spectrum in two different ways. First, we con- sider the convolved power spectrum including the window effect, which is obtained by following the ... See full document

... Observationally, the predicted abundance of substructures in clusters is one of the major successes of the CDM model (Springel et al. 2001a), but on galactic scales, it appears that simulations predict more ... See full document