Discovery of six Ly<i>α</i> emitters near a radio galaxy at
 <i>z</i> ~ 5.2

Venemans, Bram; Röttgering, H. J. A.; Overzier, Roderik; Miley, G. K.; Breuck, C. De; Kurk, J.; Breugel, W. J. M. van; Carilli, C. L.; Ford, H. C.; Heckman, Timothy M.; McCarthy, Patrick J.; Pentericci, L.

doi:10.1051/0004-6361:200400041

Cited by 106 publications

(158 citation statements)

References 27 publications

Supporting

Mentioning

145

Contrasting

Order By: Relevance

“…These are the locations of the formation of the first objects in the Universe (e.g. Venemans et al 2004;Mobasher et al 2005;Ouchi et al 2005). Observations have already found superclusters at high redshifts (Nakata et al 2005;Swinbank et al 2007;Gal et al 2008;Tanaka et al 2009).…”

Section: Introductionmentioning

confidence: 97%

SDSS DR7 superclusters

Einasto

Liivamägi

Tago

et al. 2011

A&A

122

View full text Add to dashboard Cite

Aims. We study the morphology of a set of superclusters drawn from the SDSS DR7. Methods. We calculate the luminosity density field to determine superclusters from a flux-limited sample of galaxies from SDSS DR7 and select superclusters with 300 and more galaxies for our study. We characterise the morphology of superclusters using the fourth Minkowski functional V 3 , the morphological signature (the curve in the shapefinder's K 1 -K 2 plane) and the shape parameter (the ratio of the shapefinders K 1 /K 2 ). We investigate the supercluster sample using multidimensional normal mixture modelling. We use Abell clusters to identify our superclusters with known superclusters and to study the large-scale distribution of superclusters. Results. The superclusters in our sample form three chains of superclusters; one of them is the Sloan Great Wall. Most superclusters have filament-like overall shapes. Superclusters can be divided into two sets; more elongated superclusters are more luminous, richer, have larger diameters and a more complex fine structure than less elongated superclusters. The fine structure of superclusters can be divided into four main morphological types: spiders, multispiders, filaments, and multibranching filaments. We present the 2D and 3D distribution of galaxies and rich groups, the fourth Minkowski functional, and the morphological signature for all superclusters. Conclusions. Widely different morphologies of superclusters show that their evolution has been dissimilar. A study of a larger sample of superclusters from observations and simulations is needed to understand the morphological variety of superclusters and the possible connection between the morphology of superclusters and their large-scale environment.

show abstract

Section: Introductionmentioning

confidence: 97%

SDSS DR7 superclusters

Einasto

Liivamägi

Tago

et al. 2011

A&A

122

View full text Add to dashboard Cite

show abstract

“…The progenitors of z ∼ 0 clusters are overdense regions at higher redshift, although not necessarily virialized or dominated by quiescent populations (Steidel et al 1998). Such protoclusters have been detected around massive high-redshift radio galaxies at z ≥ 2 (Le Fevre et al 1996;Venemans et al 2002Venemans et al , 2004Venemans et al , 2005Venemans et al , 2007Stern et al 2003;Hatch et al 2009;Matsuda et al 2009). However, protoclusters have also been identified 'blindly' as significant overdensities of Lyman-break galaxies (LBGs) and Ly α emitters (LAEs) in regions where no massive radio galaxy is detected (Steidel et al 1998;Steidel, Adelberger & Shapley 2000;Ouchi et al 2005;Matsuda et al 2010).…”

Section: Introductionmentioning

confidence: 99%

An enhanced merger fraction within the galaxy population of the SSA22 protocluster atz = 3.1

Hine

Geach

Alexander

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

The overdense environments of protoclusters of galaxies in the early Universe (z > 2) are expected to accelerate the evolution of galaxies, with an increased rate of stellar mass assembly and black hole accretion compared to co-eval galaxies in the average density 'field'. These galaxies are destined to form the passive population of massive galaxies that dominate the cores of rich clusters today. While signatures of the accelerated growth of galaxies in the SSA22 protocluster (z = 3.1) have been observed, the mechanism driving this remains unclear. Here we show an enhanced rate of galaxy-galaxy mergers could be responsible. We morphologically classify Lyman-break Galaxies (LBGs) in the SSA22 protocluster and compare these to those of galaxies in the field at z = 3.1 as either active mergers or non-merging using Hubble Space Telescope ACS/F814W imaging, probing the rest-frame ultraviolet stellar light. We measure a merger fraction of 48±10 per cent for LBGs in the protocluster compared to 30±6 per cent in the field. Although the excess is marginal, an enhanced rate of mergers in SSA22 hints that galaxy-galaxy mergers are one of the key channels driving accelerated star formation and AGN growth in protocluster environments.

show abstract

“…Venemans et al 2004;Overzier et al 2006;Hatch et al 2011;Kuiper et al 2011) and quasars (e.g. Venemans et al 2007;Kim et al 2009;Utsumi et al 2010;Husband et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Early quenching of massive protocluster galaxies aroundz= 2.2 radio galaxies

Husband

Bremer

Stott

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

Radio galaxies are among the most massive galaxies in the high redshift universe and are known to often lie in protocluster environments. We have studied the fields of seven z = 2.2 radio galaxies with HAWK-I narrow-band and broad-band imaging in order to map out their environment using Hα emitters (HAEs). The results are compared to the blank field HAE survey HiZELS. All of the radio galaxy fields are overdense in HAEs relative to a typical HiZELS field of the same area and four of the seven are richer than all except one of 65 essentially random HiZELS subfields of the same size. The star formation rates of the massive HAEs are lower than those necessary to have formed their stellar population in the preceding Gyr -indicating that these galaxies are likely to have formed the bulk of their stars at higher redshifts, and are starting to quench.

show abstract

Discovery of six Lyα emitters near a radio galaxy at z ~ 5.2

Cited by 106 publications

References 27 publications

SDSS DR7 superclusters

SDSS DR7 superclusters

An enhanced merger fraction within the galaxy population of the SSA22 protocluster atz = 3.1

Early quenching of massive protocluster galaxies aroundz= 2.2 radio galaxies

Contact Info

Product

Resources

About