The K-Band Hubble Diagram For The Brightest Cluster Galaxies: A Test Of Galaxy Formation Models

1999 ◽  
pp. 407-407
Author(s):  
A. Aragón-Salamanca ◽  
C. M. Baugh ◽  
G. Kauffmann
Keyword(s):  
Galaxy Formation ◽  
Hubble Diagram ◽  
Cluster Galaxies ◽  
Brightest Cluster Galaxies ◽  
K Band

scholarly journals The K-Band Hubble Diagram for the Brightest Cluster Galaxies: A Test of Galaxy Formation Models

1999 ◽  
Vol 186 ◽  
pp. 407-407
Author(s):  
A. Aragón-Salamanca ◽  
C.M. Baugh ◽  
G. Kauffmann
Keyword(s):  
Galaxy Formation ◽  
Stellar Mass ◽  
Hubble Diagram ◽  
Redshift Range ◽  
Cluster Galaxies ◽  
Brightest Cluster Galaxies ◽  
Galaxy Formation And Evolution ◽  
Absolute Magnitudes ◽  
Luminosity Evolution ◽  
K Band

We analyze the K-band Hubble diagram for a sample of brightest cluster galaxies (BCGs) in the redshift range 0 < z < 1. We confirm that the scatter in the absolute magnitudes of the galaxies is small (0.3 magnitudes). The BCGs exhibit very little luminosity evolution in this redshift range: if q0 = 0.0 we detect no luminosity evolution; for q0 = 0.5 we measure a small negative evolution (i.e., BCGs were about 0.5 magnitudes fainter at z = 1 than today). If the mass in stars of these galaxies had remained constant over this period of time, substantial positive luminosity evolution would be expected: BCGs should have been brighter in the past since their stars were younger. A likely explanation for the observed zero or negative evolution is that the stellar mass of the BCGs has been assembled over time through merging and accretion, as expected in hierarchical models of galaxy formation. The colour evolution of the BCGs is consistent with that of an old stellar population (zform > 2) that is evolving passively. We can thus use evolutionary population synthesis models to estimate the rate of growth in stellar mass for these systems. We find that the stellar mass in a typical BCG has grown by a factor ≃ 2 since z ≃ 1 if q0 = 0.0 or by factor ≃ 4 if q0 = 0.5. These results are in remarkably good agreement with the predictions of semi-analytic models of galaxy formation and evolution set in the context of a hierarchical scenario for structure formation.

scholarly journals The K-Band Hubble Diagram for X-Ray Selected Brightest Cluster Galaxies

1998 ◽  
Vol 179 ◽  
pp. 339-341
Author(s):  
R.G. Mann ◽  
C.A. Collins
Keyword(s):  
Star Formation ◽  
List Type ◽  
Type Number ◽  
Hubble Diagram ◽  
Technical Problems ◽  
X Ray ◽  
Cluster Galaxies ◽  
Brightest Cluster Galaxies ◽  
The Absolute ◽  
Small Dispersion

The Hubble (magnitude-redshift) diagram for brightest cluster galaxies (BCGs) is a classic cosmological tool, widely studied because of the remarkably small dispersion (∼ 0.3 mag) in the absolute optical magnitudes of low redshift BCGs (Postman and Lauer 1995). Extending the BCG Hubble diagram to higher redshifts would greatly enhance its role as a cosmological probe, but this has been frustrated by several technical problems: – the conventional means of cluster selection in the optical become increasingly compromised by projection effects at z > 0.1– at higher redshifts the interpretation of optical magnitudes becomes increasingly complicated by the effects of possible star formation.

The light side of proto-cluster galaxies at z ∼ 4

2020 ◽  
Vol 15 (S359) ◽  
pp. 126-130
Author(s):  
Kei Ito
Keyword(s):  
Galaxy Formation ◽  
High Redshift ◽  
Cluster Galaxies ◽  
Active Structure ◽  
Brightest Cluster Galaxies ◽  
Sky Survey ◽  
Strategic Program ◽  
Light Side ◽  
Star Formation Histories ◽  
Early Galaxy

AbstractOverdense regions at high redshift, which are often called “protoclusters”, are thought to be a place where the early active structure formations are in progress. Thanks to the wide and deep-sky survey of Hyper Suprime-Cam Subaru Strategic Program, we have selected 179 protocluster candidates at z ˜ 4, enabling us to statistically discuss high-z overdense regions. I report results of the HSC-SSP protocluster project, focusing on a couple of results on the bright-end of protocluster galaxies. We identify the UV-brightest galaxies, which are likely progenitors of Brightest Cluster Galaxies. We find that these are dustier and larger than field galaxies. This suggests that galaxies in protoclusters have experienced different star formation histories at z ˜ 4. Also, the UV luminosity function of galaxies in protoclusters (PC UVLF) has a significant excess on the bright-end from field UVLF. The PC UVLF suggests that protoclusters contribute ˜ 5 – 16% of the total cosmic SFRD at z ˜ 4. The result implies that early galaxy formation occurs in protoclusters.

scholarly journals Brightest Cluster Galaxies & Cooling Flows

2012 ◽  
Vol 8 (S292) ◽  
pp. 169-174
Author(s):  
Philippe Salomé
Keyword(s):  
Galaxy Formation ◽  
Cluster Galaxies ◽  
Cooling Flows ◽  
Cooling Flow ◽  
Additional Heating ◽  
Brightest Cluster Galaxies ◽  
Central Regions ◽  
The Subject ◽  
Atomic Gas ◽  
Ultimate Fate

AbstractIn the absence of any form of feedback heating, the gas in the central regions of massive relaxed cluster should cool and initiate a cooling flow. The presence/efficiency of an additional heating and the ultimate fate of the cooling gas is the subject of an extensive debate. In the last decade, molecular and atomic gas have been found in many Brightest Cluster Galaxies. I will review these observational results and discuss their implication for galaxy formation/evolution, in the perspective of ALMA.

scholarly journals The role of Active Galactic Nuclei feedback in the formation of the brightest cluster galaxies

2012 ◽  
Vol 8 (S295) ◽  
pp. 362-365
Author(s):  
Davide Martizzi ◽  
Romain Teyssier ◽  
Ben Moore
Keyword(s):  
Active Galactic Nuclei ◽  
Galaxy Formation ◽  
Mass Fraction ◽  
Galactic Nuclei ◽  
Elliptical Galaxies ◽  
Stellar Mass ◽  
Cluster Galaxies ◽  
Brightest Cluster Galaxies ◽  
Hydrodynamical Simulations

AbstractThe formation of the brightest cluster galaxies (BCG) is a challenge for galaxy formation theory. We performed high resolution cosmological hydrodynamical simulations with the AMR code RAMSES to study the properties of the BCG which forms at the center of a Virgo–like cluster. We compare the results of 2 galaxy formation scenarios, one in which only supernovae feedback is included, and one in which also AGN feedback is considered. Properties of the simulated BCG which are comparable with those of observed massive elliptical galaxies and BCGs cannot be obtained if AGN feedback is not considered. The stellar-to-halo mass ratio in simulations without AGN feedback appears too large when compared to observations, while it is compatible the observationally determined values when AGN feedback is included. The kinematical and structural properties of the BCG are extremely different in the two models. When we do not include AGN feedback, the BCG is quickly rotating, with high Sérsic index, a clear mass excess in the center and a very large stellar mass fraction. When AGN feedback is considered, the BCG is slowly rotating, with a significantly cored surface density profile and low stellar mass fraction.

scholarly journals The formation of brightest cluster galaxies: the case of ABELL 407

2015 ◽  
Vol 48 (1) ◽  
Author(s):  
Louise O.V. Edwards
Keyword(s):  
Galaxy Formation ◽  
Cluster Galaxy ◽  
Cluster Galaxies ◽  
Brightest Cluster Galaxies ◽  
Galaxy Formation And Evolution ◽  
The Galaxy ◽  
Formation And Evolution ◽  
Intracluster Light

This article begins with a general introduction to galaxy formation and evolution and ends with a discussion of the long-term spectroscopic study: The Role of Close Companions in the Formation of Brightest Cluster Galaxies and Intracluster Light. To illustrate the power, goals and aims of this larger project, preliminary data for one of the galaxy clusters in our sample is presented, Abell 407, which appears to be caught in the act of forming its Brightest Cluster Galaxy (BCG).

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