Quantitative Morphology of the Intermediate-Redshift Galaxy Cluster Abell 2443 from Ground-based Imaging: Evidence for a Galaxy Concentration Index Correlation with Cluster Density

2001 ◽  
Vol 122 (1) ◽  
pp. 38-54 ◽  
Author(s):  
I. Trujillo ◽  
J. A. L. Aguerri ◽  
C. M. Gutiérrez ◽  
J. Cepa
Keyword(s):  
Concentration Index ◽  
Galaxy Cluster ◽  
Quantitative Morphology ◽  
Redshift Galaxy ◽  
Cluster Density ◽  
Intermediate Redshift

scholarly journals The intermediate-redshift galaxy cluster CL 0048-2942

2004 ◽  
Vol 429 (1) ◽  
pp. 101-114 ◽  
Author(s):  
M. Serote Roos ◽  
C. Lobo ◽  
F. Durret ◽  
A. Iovino ◽  
I. Márquez
Keyword(s):  
Galaxy Cluster ◽  
Redshift Galaxy ◽  
Intermediate Redshift

scholarly journals The Northern Sky Optical Cluster Survey. IV. An Intermediate-Redshift Galaxy Cluster Catalog and the Comparison of Two Detection Algorithms

2004 ◽  
Vol 128 (3) ◽  
pp. 1017-1045 ◽  
Author(s):  
P. A. A. Lopes ◽  
R. R. de Carvalho ◽  
R. R. Gal ◽  
S. G. Djorgovski ◽  
S. C. Odewahn ◽  
...  
Keyword(s):  
Galaxy Cluster ◽  
Cluster Survey ◽  
Detection Algorithms ◽  
Redshift Galaxy ◽  
Intermediate Redshift

scholarly journals The distant (z = 0.471) radiogalaxy 3C 435 A with the integral field spectrograph TIGER

1995 ◽  
Vol 149 ◽  
pp. 250-253
Author(s):  
B. Rocca-Volmerange ◽  
G. Adam ◽  
P. Ferruit ◽  
R. Bacon
Keyword(s):  
Energy Distribution ◽  
Galaxy Evolution ◽  
Large Degree ◽  
Emission Lines ◽  
Image Point ◽  
Redshift Galaxy ◽  
Stellar Energy ◽  
Integral Field Spectrograph ◽  
Intermediate Redshift ◽  
Integral Field

The distant radiogalaxies recently discovered at the most remote distances (z≥3.5) are among the best cosmological targets. However so various features caracterize these galaxies (red stellar energy distribution, huge emission lines, high density of galaxy companions, alignment of ultraviolet and radio axes, large degree of polarisation) that their structures are not simple to understand. Stellar populations will only become the best indicators of evolution of galaxies if these structures are clearly understood from a two-dimension spectroscopy on each image point. The integral field spectrograph TIGER is a unique instrument at the CFHT to give details on the nature and velocities of the various components of distant radiogalaxies.We present the observations with TIGER of an intermediate-redshift galaxy 3C435A (z=0.471) (Rocca-Volmerange et al, 1994). The two nebular lines [OII], [OIII] and the largely extended stellar continua are observable, allowing to date galaxy with the help of our evolution model. The present and past star formation activities and the origin of alignment will be thus analysed in terms of galaxy evolution.

scholarly journals An analysis of galaxy cluster mis-centring using cosmological hydrodynamic simulations

2020 ◽  
Vol 493 (1) ◽  
pp. 1120-1129
Author(s):  
Z Yan ◽  
N Raza ◽  
L Van Waerbeke ◽  
A J Mead ◽  
I G McCarthy ◽  
...  
Keyword(s):  
Galaxy Cluster ◽  
Mass Range ◽  
Three Dimensions ◽  
Cumulative Distribution ◽  
Density Profiles ◽  
Hydrodynamic Simulations ◽  
The Galaxy ◽  
Cluster Density ◽  
Cluster Properties ◽  
Using Data

ABSTRACT The location of a galaxy cluster’s centroid is typically derived from observations of the galactic and/or gas component of the cluster, but these typically deviate from the true centre. This can produce bias when observations are combined to study average cluster properties. Using data from the BAryons and HAloes of MAssive Systems (BAHAMAS) cosmological hydrodynamic simulations, we study this bias in both two and three dimensions for 2000 clusters over the 1013–1015 M⊙ mass range. We quantify and model the offset distributions between observationally motivated centres and the ‘true’ centre of the cluster, which is taken to be the most gravitationally bound particle measured in the simulation. We fit the cumulative distribution function of offsets with an exponential distribution and a Gamma distribution fit well with most of the centroid definitions. The galaxy-based centres can be seen to be divided into a mis-centred group and a well-centred group, with the well-centred group making up about $60{{\ \rm per\ cent}}$ of all the clusters. Gas-based centres are overall less scattered than galaxy-based centres. We also find a cluster-mass dependence of the offset distribution of gas-based centres, with generally larger offsets for smaller mass clusters. We then measure cluster density profiles centred at each choice of the centres and fit them with empirical models. Stacked, mis-centred density profiles fit to the Navarro–Frenk–White dark matter profile and Komatsu–Seljak gas profile show that recovered shape and size parameters can significantly deviate from the true values. For the galaxy-based centres, this can lead to cluster masses being underestimated by up to $10{{\ \rm per\ cent}}$.

scholarly journals DUST-OBSCURED STAR FORMATION IN INTERMEDIATE REDSHIFT GALAXY CLUSTERS

2010 ◽  
Vol 720 (1) ◽  
pp. 87-98 ◽  
Author(s):  
Rose A. Finn ◽  
Vandana Desai ◽  
Gregory Rudnick ◽  
Bianca Poggianti ◽  
Eric F. Bell ◽  
...  
Keyword(s):  
Star Formation ◽  
Galaxy Clusters ◽  
Redshift Galaxy ◽  
Intermediate Redshift

scholarly journals ACHANDRASTUDY OF TEMPERATURE SUBSTRUCTURES IN INTERMEDIATE-REDSHIFT GALAXY CLUSTERS

2009 ◽  
Vol 700 (2) ◽  
pp. 1161-1172 ◽  
Author(s):  
Liyi Gu ◽  
Haiguang Xu ◽  
Junhua Gu ◽  
Yu Wang ◽  
Zhongli Zhang ◽  
...  
Keyword(s):  
Galaxy Clusters ◽  
Redshift Galaxy ◽  
Intermediate Redshift

scholarly journals SPATIAL AND KINEMATIC DISTRIBUTIONS OF TRANSITION POPULATIONS IN INTERMEDIATE REDSHIFT GALAXY CLUSTERS

2014 ◽  
Vol 786 (1) ◽  
pp. 30 ◽  
Author(s):  
Steven M. Crawford ◽  
Gregory D. Wirth ◽  
Matthew A. Bershady
Keyword(s):  
Galaxy Clusters ◽  
Redshift Galaxy ◽  
Intermediate Redshift

scholarly journals More connected, more active: galaxy clusters and groups at z ∼ 1 and the connection between their quiescent galaxy fractions and large-scale environments

2019 ◽  
Vol 490 (1) ◽  
pp. 135-155 ◽  
Author(s):  
Seong-Kook Lee ◽  
Myungshin Im ◽  
Minhee Hyun ◽  
Bomi Park ◽  
Jae-Woo Kim ◽  
...  
Keyword(s):  
Star Formation ◽  
Galaxy Clusters ◽  
Large Scale ◽  
High Redshift ◽  
Galaxy Cluster ◽  
Spectroscopic Observation ◽  
Star Forming ◽  
Large Scale Structures ◽  
Photometric Redshift ◽  
Redshift Galaxy

ABSTRACT High-redshift galaxy clusters, unlike local counterparts, show diverse star formation activities. However, it is still unclear what keeps some of the high-redshift clusters active in star formation. To address this issue, we performed a multiobject spectroscopic observation of 226 high-redshift (0.8 < z < 1.3) galaxies in galaxy cluster candidates and the areas surrounding them. Our spectroscopic observation reveals six to eight clusters/groups at z ∼ 0.9 and z ∼ 1.3. The redshift measurements demonstrate the reliability of our photometric redshift measurements, which in turn gives credibility for using photometric redshift members for the analysis of large-scale structures (LSSs). Our investigation of the large-scale environment (∼10 Mpc) surrounding each galaxy cluster reveals LSSs – structures up to ∼10 Mpc scale – around many of, but not all, the confirmed overdensities and the cluster candidates. We investigate the correlation between quiescent galaxy fraction of galaxy overdensities and their surrounding LSSs, with a larger sample of ∼20 overdensities including photometrically selected overdensities at 0.6 < z < 0.9. Interestingly, galaxy overdensities embedded within these extended LSSs show a lower fraction of quiescent galaxies ($\sim 20{{\ \rm per\ cent}}$) than isolated ones at similar redshifts (with a quiescent galaxy fraction of $\sim 50 {{\ \rm per\ cent}}$). Furthermore, we find a possible indication that clusters/groups with a high quiescent galaxy fraction are more centrally concentrated. Based on these results, we suggest that LSSs are the main reservoirs of gas and star-forming galaxies to keep galaxy clusters fresh and extended in size at z ∼ 1.

Sign in / Sign up

Export Citation Format

Share Document