The first appearance of the red sequence of galaxies in proto-clusters at 2 lsimzlsim 3

Kodama, Tadayuki; Tanaka, Ichi; Kajisawa, Masaru; Kurk, J.; Venemans, Bram; Breuck, C. De; Vernet, J.; Lidman, C.

doi:10.1111/j.1365-2966.2007.11739.x

Cited by 179 publications

(245 citation statements)

References 59 publications

Supporting

Mentioning

222

Contrasting

Order By: Relevance

“…As pointed out by Doherty et al (2009), the J and K s band photometric zero-points used in Kodama et al (2007) were off by ∼0.3 mag. We re-measured the zero points from the standard stars observed in the same nights and adopted those revised zero points.…”

Section: Pks1138mentioning

confidence: 99%

The environmental dependence of galaxy properties atz = 2

Tanaka¹,

Breuck²,

Venemans³

et al. 2010

A&A

Self Cite

View full text Add to dashboard Cite

We report on the environmental dependence of galaxy properties at z = 2.15. We construct multi-band photometric data sets in the (proto-)cluster PKS1138-26 field and in the GOODS field. We then fit spectral energy distributions of the galaxies with model templates generated with the latest stellar population synthesis code and derive physical properties of galaxies from the fits. To quantify the environmental dependence of galaxy properties, a special care is taken of systematic errors -we use data sets that have almost the same wavelength samplings, use the same code to fit SEDs with the same set of templates, and compare relative differences between the two samples. We find that the PKS1138 galaxies have similar ages, shorter star formation time scales, lower star formation rates, and weaker dust extinction compared to the GOODS galaxies at z ∼ 2. This trend is similar to that observed locally, suggesting that the environmental dependence of galaxy properties is already partly in place as early as z = 2.15. We show that the PKS1138 galaxies assemble the bulk of their masses ∼1 Gyr earlier than field galaxies, i.e., the galaxy formation depends on environment. Galaxy mergers should frequently occur during the first collapse of clusters and they might play an important role in driving the observed environmental dependence of galaxy properties at z = 2.15.

show abstract

Section: Pks1138mentioning

confidence: 99%

The environmental dependence of galaxy properties atz = 2

Tanaka¹,

Breuck²,

Venemans³

et al. 2010

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…The mid-IR cameras on board the Spitzer and Akari satellites has extended the range and power of multicolour surveys, producing confirmed and candidate clusters up to z ∼ 1.7 (Stanford et al 2005;Eisenhardt et al 2008;Goto et al 2008). However, most of the previous techniques present some difficulties in the range 1.5 < z < 2.5, where we expect to observe the formation of the red sequence and the first hints of colour segregation (Cucciati et al 2006;Kodama et al 2007). Searching for extended X-ray sources becomes progressively more difficult at great distances, because the surface brightness of the X-ray emission fades as (1 + z) 4 .…”

Section: Introductionmentioning

confidence: 99%

A comprehensive study of large-scale structures in the GOODS-SOUTH field up to ${\mathsf z} \sim $ 2.5

Salimbeni

Castellano

Pentericci

et al. 2009

A&A

View full text Add to dashboard Cite

Aims. The aim of the present paper is to identify and study the properties and galactic content of groups and clusters in the GOODSSouth field up to z ∼ 2.5, and to analyse the physical properties of galaxies as a continuous function of environmental density up to high redshift. Methods. We used the deep (z 850 ∼ 26), multi-wavelength GOODS-MUSIC catalogue, which has a 15% of spectroscopic redshifts and accurate photometric redshifts for the remaining fraction. On these data, we applied a (2+1)D algorithm, previously developed by our group, that provides an adaptive estimate of the 3D density field. We supported our analysis with simulations to evaluate the purity and the completeness of the cluster catalogue produced by our algorithm. Results. We find several high-density peaks embedded in larger structures in the redshift range 0.4-2.5. From the analysis of their physical properties (mass profile, M 200 , σ v , L X , U − B vs. B diagram), we find that most of them are groups of galaxies, while two are poor clusters with masses a few times 10 14 M . For these two clusters we find from the Chandra 2Ms data an X-ray emission significantly lower than expected from their optical properties, suggesting that the two clusters are either not virialised or are gas poor. We find that the slope of the colour magnitude relation, for these groups and clusters, is constant at least up to z ∼ 1. We also analyse the dependence on environment of galaxy colours, luminosities, stellar masses, ages, and star formations. We find that galaxies in high-density regions are, on average, more luminous and massive than field galaxies up to z ∼ 2. The fraction of red galaxies increases with luminosity and with density up to z ∼ 1.2. At higher z this dependence on density disappears. The variation of galaxy properties as a function of redshift and density suggests that a significant change occurs at z ∼ 1.5-2.

show abstract

“…One therefore expects that, at higher redshift, the scatter in colour increases as the epoch when the stellar populations were formed is approached. Indeed, changes in the red sequence in galaxy structures have been observed between low redshift and redshifts z = 2.2-3.1 (De Lucia et al 2007;Kodama et al 2007;Zirm et al 2008), in the sense that the faint end of the red sequence becomes less populated, although a dependence on cluster richness may also play a role (Andreon 2008).…”

Section: Introductionmentioning

confidence: 99%

“…For the overdensities of galaxies known at high redshift, this is often problematic because their cluster members are selected on the basis of either their star formation activity (blue members, e.g., Kurk et al 2000;Pentericci et al 2000;Venemans et al 2002;Steidel et al 2005), or lack of it (red members, e.g., Best et al 2003;Kodama et al 2007;McCarthy et al 2007). The most well studied high-redshift systems confirmed to be clusters on the basis of their X-ray emission, are found between z = 1.0 and z = 1.4, redshifts for which spectroscopic data of both the red and blue populations can be practically acquired (e.g., at z = 1.26, Demarco et al 2007; Mei et al 2006).…”

Section: Introductionmentioning

confidence: 99%

GMASS ultradeep spectroscopy of galaxies at z ~ 2

Kurk

Cimatti

Zamorani

et al. 2009

A&A

Self Cite

108

142

View full text Add to dashboard Cite

Context. Clusters of galaxies represent important laboratories for studying galaxy evolution and formation. Well established and relaxed clusters are known below z < 1.4, as well as, clusters in formation found close to radio galaxies at z > 2, but the in-between redshift range, during which clusters are expected to undergo significant changes, is almost unexplored. Aims. By studying a galaxy overdensity in redshift and angular distribution at z = 1.6, uncovered in the Galaxy Mass Assembly ultra-deep Spectroscopic Survey (GMASS), we provide insight into the evolution of cluster galaxies at high redshift. Methods. We present a study of the significance of the galaxy overdensity at z = 1.6, Cl 0332-2742, its velocity dispersion, and X-ray emission. We identify the colour bimodality of the cluster members and compare the properties of members of Cl 0332-2742 with galaxies outside the overdensity. Results. From the redshifts of the 42 overdensity members, we measure a velocity dispersion of 500 km s −1 . We conservatively estimate the overdensity in redshift space for the spike at z = 1.6 in the GMASS field to be 8.3 ± 1.5. A map of the surface density of galaxies at z = 1.6 in the GMASS field shows that its structure is irregular with several filaments and local overdensities. The differences in the physical properties of Cl 0332-2742 member and field galaxies agree with the latest hierarchical galaxy formation models: for overdensity members, the star formation rate (SFR), and specific SFR, is approximately 50% lower than for the field galaxies; overdensity galaxies are twice the age, on average, of field galaxies; and there is a higher proportion of both massive (M > 10 10.7 M ), and early-type galaxies, inside Cl 0332-2742 than in the field. Among the 42 members, seven have spectra consistent with being passively evolving, massive galaxies. These are all located within an area where the surface density of z = 1.6 galaxies is highest. In a z − J colour-magnitude diagram, the photometric data of these early-type galaxies are in close agreement with a theoretical red sequence of a galaxy cluster at redshift z = 1.6, which formed most of its stars in a short burst of star formation at z ∼ 3. Conclusions. We conclude that the redshift spike at z = 1.6 in the GMASS field represents a sheet-like structure in the cosmic web, and that the area with the highest surface density within this structure, containing already seven passively evolving galaxies, will evolve into a cluster of galaxies at a later time.

show abstract

The first appearance of the red sequence of galaxies in proto-clusters at 2 lsimzlsim 3

Cited by 179 publications

References 59 publications

The environmental dependence of galaxy properties atz = 2

The environmental dependence of galaxy properties atz = 2

A comprehensive study of large-scale structures in the GOODS-SOUTH field up to ${\mathsf z} \sim $ 2.5

GMASS ultradeep spectroscopy of galaxies at z ~ 2

Contact Info

Product

Resources

About