2004
DOI: 10.1051/0004-6361:20030621
|View full text |Cite
|
Sign up to set email alerts
|

K$_{\mbox{\fontsize{12pt}{14pt}\selectfont{\textit{s}}}}$-band luminosity function of thez= 1.237 cluster of galaxies RDCS J1252.9-2927

Abstract: Abstract. ESA's Infrared Space Observatory (ISO) was used to perform a deep survey with ISOCAM through three massive gravitationally lensing clusters of galaxies. The total area surveyed depends on source flux, with nearly seventy square arcminutes covered for the brighter flux levels in maps centred on the three clusters Abell 370, Abell 2218 and Abell 2390. We present maps and photometry at 6.7 µm (hereafter 7 µm) and 14.3 µm (hereafter 15 µm), showing a total of 145 mid-infrared sources and the associated s… Show more

Help me understand this report
View preprint versions

Search citation statements

Order By: Relevance

Paper Sections

Select...
2
1
1
1

Citation Types

9
44
0

Year Published

2005
2005
2019
2019

Publication Types

Select...
7

Relationship

3
4

Authors

Journals

citations
Cited by 44 publications
(53 citation statements)
references
References 103 publications
(156 reference statements)
9
44
0
Order By: Relevance
“…The flat faint-end slope, and the measured M * close to passive evolution predictions of the local cluster galaxy LF, point toward the LF bright end being similar to that of local clusters, beside evolution of the stellar populations. This extends to z ∼ 1.4 previous findings on the early assembly of the massive galaxy populations in the cluster core regions (De Propris et al 1999;Nakata et al 2001;Kodama & Bower 2003;Toft et al 2003;Ellis & Jones 2004;Toft et al 2004;Andreon 2006;Strazzullo et al 2006;De Propris et al 2007;Muzzin et al 2008;Mancone et al 2010). …”
Section: Figsupporting
confidence: 84%
“…The flat faint-end slope, and the measured M * close to passive evolution predictions of the local cluster galaxy LF, point toward the LF bright end being similar to that of local clusters, beside evolution of the stellar populations. This extends to z ∼ 1.4 previous findings on the early assembly of the massive galaxy populations in the cluster core regions (De Propris et al 1999;Nakata et al 2001;Kodama & Bower 2003;Toft et al 2003;Ellis & Jones 2004;Toft et al 2004;Andreon 2006;Strazzullo et al 2006;De Propris et al 2007;Muzzin et al 2008;Mancone et al 2010). …”
Section: Figsupporting
confidence: 84%
“…They are from the Sloan Digital Sky Survey (SDSS, York et al 2000;Strauss et al 2002) and have M V < M * V + 1 at 0.005 < z < 0.065. Our spectroscopy reaches a z-band magnitude of ∼23, which roughly corresponds to m * z + 1 at z = 1.2 for red galaxies with z − Ks ∼ 2 (Toft et al 2004;Strazzullo et al 2006). The magnitude cut applied to the SDSS data is relative to M * V at z = 0.…”
Section: Star Formation Activity As a Function Of Environmentmentioning
confidence: 72%
“…Toft and colleagues also found a substantial deficit of fainter ETGs, which could be seen as a manifestation of the down-sizing effect in a high redshift cluster, a hint of which was also noticed in other clusters at z ∼ 0. However, a more complete study of 3 rich clusters at 1.1 < ∼ z < ∼ 1.3, including the z = 1.237 cluster studied by Toft et al (2004), did not produce evidence of a down-sizing effect, down to at least 4 magnitudes below K * (Strazzullo et al 2006). This study confirmed the brightening of M * z and M * K by ∼ 1.3 mag, consistent with passive evolution of a population that formed at z > ∼ 2, and showed that the massive galaxies were already fully assembled at z ∼ 1.2, at least in the central regions of the 3 clusters.…”
Section: Cluster Ellipticalsmentioning
confidence: 87%
“…Kodama & Bower (2003) and Toft, Soucail, & Hjorth (2003) came to the same conclusions by studying the K-band LF of (respectively two and one) clusters at z ∼ 1. Breaking the z = 1 barrier, Toft et al (2004) constructed a very deep K-band LF of a rich RDCS cluster at z = 1.237, and concluded that the most massive ellipticals that dominate the top end of the LF were already in place in this cluster. They compared the cluster K-band LF (corresponding to the rest-frame z-band LF) to the z-band LF of local clusters (Popesso et al 2005) and derived a brightening by ∼ 1.4 mag in the rest-frame z-band characteristic magnitude, indeed as expected from pure passive evolution.…”
Section: Cluster Ellipticalsmentioning
confidence: 99%