scholarly journals The growth of the red-sequence in clusters since ≃1

2009 ◽  
Vol 5 (H15) ◽  
pp. 88-88
Author(s):  
Roberto P. Muñoz ◽  
L. F. Barrientos ◽  
B. P. Koester ◽  
D. G. Gilbank ◽  
M. D. Gladders ◽  
...  
Keyword(s):  
Star Formation ◽  
Galaxy Clusters ◽  
Evolutionary Model ◽  
Large Ensemble ◽  
Cluster Galaxies ◽  
Nir Imaging ◽  
Measured Change ◽  
First Time ◽  
The Universe ◽  
Red Sequence

AbstractWe use deep nIR imaging of 15 galaxy clusters at z ≃ 1 to study the build-up of the red-sequence in rich clusters since the Universe was half its present age. We measured, for the first time, the luminous-to-faint ratio of red-sequence galaxies at z=1 from a large ensemble of clusters, and found an increase of 100% in the ratio of luminous-to-faint red-sequence galaxies from z=0.45 to 1.0. The measured change in this ratio as function of redshift is well-reproduced by a simple evolutionary model developed in this work, that consists in an early truncation of the star formation for bright cluster galaxies and a delayed truncation for faint cluster galaxies.

GALAXY EVOLUTION THROUGH THE COSMIC TIME

2010 ◽  
Vol 19 (08n10) ◽  
pp. 1371-1377
Author(s):  
T. P. IDIART ◽  
J. A. F. PACHECO ◽  
J. SILK
Keyword(s):  
Star Formation ◽  
Galaxy Evolution ◽  
Cosmic Time ◽  
Evolutionary Model ◽  
Stellar Populations ◽  
Elliptical Galaxies ◽  
Star Formation Activity ◽  
Formation And Evolution ◽  
The Universe

Elliptical galaxies are the best systems to study the early star formation activity in the universe. This work aims to understand the formation and evolution of these objects through the study of the integrated properties of their stellar populations. Here an evolutionary model is developed and their predicted spectrophotometric properties are presented.

scholarly journals Spectroscopic Evidences for Star Formation in Cooling Flow Galaxies

1996 ◽  
Vol 171 ◽  
pp. 349-349
Author(s):  
N. Cardiel ◽  
J. Gorgas ◽  
A. Aragon-Salamanca
Keyword(s):  
Star Formation ◽  
Galaxy Clusters ◽  
X Ray ◽  
Cluster Galaxies ◽  
Cooling Flows ◽  
Cooling Flow ◽  
Brightest Cluster Galaxies

X-ray observations have led to the conclusion that many galaxy clusters are hosting cooling flows. The brightest cluster galaxies could have accreted masses of the order of 1011–1012M⊙, but is still uncertain what the final fate of the accreted gas may be.

scholarly journals THE EVOLUTION OF DUSTY STAR FORMATION IN GALAXY CLUSTERS TOz= 1:SPITZERINFRARED OBSERVATIONS OF THE FIRST RED-SEQUENCE CLUSTER SURVEY

2013 ◽  
Vol 146 (4) ◽  
pp. 84 ◽  
Author(s):  
T. M. A. Webb ◽  
D. O'Donnell ◽  
H. K. C. Yee ◽  
David Gilbank ◽  
Kristen Coppin ◽  
...  
Keyword(s):  
Star Formation ◽  
Galaxy Clusters ◽  
Sequence Cluster ◽  
Cluster Survey ◽  
Red Sequence

scholarly journals The High-Redshift Clusters Occupied by Bent Radio AGN (COBRA) Survey

2015 ◽  
Vol 11 (S319) ◽  
pp. 62-62
Author(s):  
Rachel Paterno-Mahler ◽  
Elizabeth L. Blanton ◽  
Joshua Wing ◽  
M.L.N. Ashby ◽  
Mark Brodwin ◽  
...  
Keyword(s):  
Radio Source ◽  
Galaxy Clusters ◽  
Large Range ◽  
High Redshift ◽  
Cosmic Time ◽  
Optical Data ◽  
Radio Sources ◽  
Cluster Galaxies ◽  
Redshift Galaxy ◽  
Red Sequence

AbstractThe number of confirmed, high-redshift galaxy clusters is very low compared to the number of well-studied clusters nearby. Bent, double-lobed radio sources are frequently found in galaxy clusters, and thus can be used as tracers for efficiently locating high-redshift clusters. Using our Spitzer Snapshot Survey, we have identified approximately 300 potential new clusters with redshifts 0.7 < z < 3. These objects make up the high-redshift portion of the Cluster Occupied by Bent Radio AGN (COBRA) survey. We have created color-magnitude diagrams using infrared and optical data. Using the colors of the radio source host and the red sequence we can estimate redshifts for our clusters, as well as examine the evolution of the cluster galaxies over a large range of cosmic time.

scholarly journals Alignment of Red-Sequence Cluster Dwarf Galaxies: From the Frontier Fields to the Local Universe

2015 ◽  
Vol 11 (S319) ◽  
pp. 5-5
Author(s):  
Wayne A. Barkhouse ◽  
Haylee Archer ◽  
Jaford Burgad ◽  
Gregory Foote ◽  
Cody Rude ◽  
...  
Keyword(s):  
Galaxy Clusters ◽  
Dwarf Galaxies ◽  
Local Universe ◽  
Alignment Effect ◽  
Cluster Galaxies ◽  
Sequence Cluster ◽  
Redshift Galaxy ◽  
Red Sequence

AbstractWe investigate the alignment effect of red-sequence dwarf galaxies using a sample of 121 low-redshift galaxy clusters and cluster galaxies selected from the HST Frontier Fields.

scholarly journals Galaxy And Mass Assembly (GAMA): Defining passive galaxy samples and searching for the UV upturn

2019 ◽  
Vol 492 (2) ◽  
pp. 2128-2139
Author(s):  
S Phillipps ◽  
S S Ali ◽  
M N Bremer ◽  
R De Propris ◽  
A E Sansom ◽  
...  
Keyword(s):  
Star Formation ◽  
Cluster Galaxies ◽  
Star Forming ◽  
Stellar Component ◽  
Wide Range ◽  
Other Information ◽  
Mass Assembly ◽  
Clean Sample ◽  
Uv Upturn ◽  
Red Sequence

ABSTRACT We use data from the GAMA and GALEX surveys to demonstrate that the UV upturn, an unexpected excess of ultraviolet flux from a hot stellar component, seen in the spectra of many early-type galaxies, arises from processes internal to individual galaxies with no measurable influence from the galaxies’ larger environment. We first define a clean sample of passive galaxies without a significant contribution to their UV flux from low-level star formation. We confirm that galaxies with the optical colours of red sequence galaxies often have signs of residual star formation, which, without other information, would prevent a convincing demonstration of the presence of UV upturns. However, by including (NUV−u) and WISE (W2–W3) colours, and FUV data where it exists, we can convincingly constrain samples to be composed of non-star-forming objects. Using such a sample, we examine GALEX photometry of low-redshift GAMA galaxies in a range of low-density environments, from groups to the general field, searching for UV upturns. We find a wide range of (NUV−r) colours, entirely consistent with the range seen – and attributed to the UV upturn – in low-redshift red sequence cluster galaxies. The range of colours is independent of group multiplicity or velocity dispersion, with isolated passive galaxies just as likely to have blue UV-to-optical colours, implying significant upturn components, as those in richer groups and in the previous data on clusters. This is supported by equivalent results for (FUV−r) colours which are clear indicators of upturn components.

scholarly journals Measuring the total infrared light from galaxy clusters at z = 0.5–1.6: connecting stellar populations to dusty star formation

2020 ◽  
Vol 501 (2) ◽  
pp. 1970-1998
Author(s):  
Stacey Alberts ◽  
Kyoung-Soo Lee ◽  
Alexandra Pope ◽  
Mark Brodwin ◽  
Yi-Kuan Chiang ◽  
...  
Keyword(s):  
Star Formation ◽  
Galaxy Clusters ◽  
Dust Emission ◽  
Infrared Light ◽  
Spectral Energy ◽  
Cluster Emission ◽  
Cluster Galaxies ◽  
Radial Profiles ◽  
Low Mass ◽  
Massive Galaxy

ABSTRACT Massive galaxy clusters undergo strong evolution from z ∼ 1.6 to z ∼ 0.5, with overdense environments at high-z characterized by abundant dust-obscured star formation and stellar mass growth which rapidly give way to widespread quenching. Data spanning the near- to far-infrared (IR) can directly trace this transformation; however, such studies have largely been limited to the massive galaxy end of cluster populations. In this work, we present ‘total light’ stacking techniques spanning $3.4\!-\!500\, \mu$m aimed at revealing the total cluster emission, including low-mass members and potential intracluster dust. We detail our procedures for WISE, Spitzer, and Herschel imaging, including corrections to recover the total stacked emission in the case of high fractions of detected galaxies. We apply our techniques to 232 well-studied log$\, M_{200}/\mathrm{M}_{\odot }\sim 13.8$ clusters in multiple redshift bins, recovering extended cluster emission at all wavelengths. We measure the averaged IR radial profiles and spectral energy distributions (SEDs), quantifying the total stellar and dust content. The near-IR profiles are well described by an NFW model with a high (c ∼ 7) concentration. Dust emission is similarly concentrated, albeit suppressed at $r\lesssim 0.3\,$Mpc. The measured SEDs lack warm dust, consistent with the colder SEDs of low-mass galaxies. We derive total stellar masses consistent with the theoretical Mhalo−M⋆ relation and specific star formation rates that evolve strongly with redshift, echoing that of log$\, M_{\star }/\mathrm{M}_{\odot }\gtrsim 10$ cluster galaxies. Separating out the massive population reveals the majority of cluster far-IR emission ($\sim 70\!-\!80{{\ \rm per\ cent}}$) is provided by the low-mass constituents, which differs from field galaxies. This effect may be a combination of mass-dependent quenching and excess dust in low-mass cluster galaxies.

scholarly journals RECENT GALAXY MERGERS AND RESIDUAL STAR FORMATION OF RED SEQUENCE GALAXIES IN GALAXY CLUSTERS

2016 ◽  
Vol 827 (1) ◽  
pp. 32 ◽  
Author(s):  
Yun-Kyeong Sheen ◽  
Sukyoung K. Yi ◽  
Chang H. Ree ◽  
Yara Jaffé ◽  
Ricardo Demarco ◽  
...  
Keyword(s):  
Star Formation ◽  
Galaxy Clusters ◽  
Galaxy Mergers ◽  
Red Sequence

scholarly journals TheThreeHundred project: backsplash galaxies in simulations of clusters

2020 ◽  
Vol 492 (4) ◽  
pp. 6074-6085 ◽  
Author(s):  
Roan Haggar ◽  
Meghan E Gray ◽  
Frazer R Pearce ◽  
Alexander Knebe ◽  
Weiguang Cui ◽  
...  
Keyword(s):  
Galaxy Clusters ◽  
Galaxy Cluster ◽  
Recent History ◽  
Cluster Galaxies ◽  
Cluster Centre ◽  
Dynamical State ◽  
History Of ◽  
First Time

ABSTRACT In the outer regions of a galaxy cluster, galaxies either may be falling into the cluster for the first time or have already passed through the cluster centre at some point in their past. To investigate these two distinct populations, we utilize TheThreeHundred project, a suite of 324 hydrodynamical resimulations of galaxy clusters. In particular, we study the ‘backsplash population’ of galaxies: those that have passed within R200 of the cluster centre at some time in their history, but are now outside of this radius. We find that, on average, over half of all galaxies between R200 and 2R200 from their host at $z$ = 0 are backsplash galaxies, but that this fraction is dependent on the dynamical state of a cluster, as dynamically relaxed clusters have a greater backsplash fraction. We also find that this population is mostly developed at recent times ($z$ ≲ 0.4), and is dependent on the recent history of a cluster. Finally, we show that the dynamical state of a given cluster, and thus the fraction of backsplash galaxies in its outskirts, can be predicted based on observational properties of the cluster.

scholarly journals JD2 - Diffuse Light in Galaxy Clusters

2009 ◽  
Vol 5 (H15) ◽  
pp. 97-110 ◽  
Author(s):  
Magda Arnaboldi ◽  
Ortwin Gerhard
Keyword(s):  
Star Formation ◽  
Galaxy Clusters ◽  
Diffuse Light ◽  
Velocity Measurements ◽  
Cluster Galaxy ◽  
Cluster Galaxies ◽  
Magnitude Diagram ◽  
Hydrodynamical Simulations ◽  
Intracluster Light ◽  
Intermediate Redshift

AbstractDiffuse intracluster light (ICL) has now been observed in nearby and in intermediate redshift clusters. Individual intracluster stars have been detected in the Virgo and Coma clusters and the first color-magnitude diagram and velocity measurements have been obtained. Recent studies show that the ICL contains of the order of 10% and perhaps up to 30% of the stellar mass in the cluster, but in the cores of some dense and rich clusters like Coma, the local ICL fraction can be high as 40%-50%. What can we learn from the ICL about the formation of galaxy clusters and the evolution of cluster galaxies? How and when did the ICL form? What is the connection to the central brightest cluster galaxy? Cosmological N-body and hydrodynamical simulations are beginning to make predictions for the kinematics and origin of the ICL. The ICL traces the evolution of baryonic substructures in dense environments and can thus be used to constrain some aspects of cosmological simulations that are most uncertain, such as the modeling of star formation and the mass distribution of the baryonic component in galaxies.

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