Advanced Camera for Surveys Photometry of the Cluster RDCS 1252.9–2927: The Color-Magnitude Relation at z = 1.24

By J. Blakeslee, M. Franx, M. Postman, Piero Rosati, B. Holden, G. Illingworth, H. C. Ford, N. Cross, C. Gronwall, Narciso Benitez and 13 more. 2003

188 citations recorded by the source corpus.

We investigate the color-magnitude (CM) relation of galaxies in the distant X-ray-selected cluster RDCS 1252.9-2927 at z = 1.24 using images obtained with the Advanced Camera for Surveys on the Hubble Space Telescope in the F775W and F850LP bandpasses. We select galaxies based on morphological classifications extending about 3.5 mag down the galaxy luminosity function, augmented by spectroscopic membership information. At the core of the cluster is an extensive early-type galaxy population surrounding a central pair of galaxies that show signs of dynamical interaction. The early-type population defines a tight sequence in the CM diagram, with an intrinsic scatter in observed (i775-z850) of 0.029 ± 0.007 mag based on 52 galaxies or 0.024 ± 0.008 mag for ~30 elliptical galaxies. Simulations using the latest stellar population models indicate an age scatter for the elliptical galaxies of about 34%, with a mean age τL ≳ 2.6 Gyr (corresponding to zL ≳ 2.7), and the last star formation occurring at zend ≳ 1.5. Transforming to rest-frame (U-B), we conclude that the slope and scatter in the CM relation for morphologically selected early-type galaxies show little or no evidence of evolution out to z ≈ 1.2. Thus, elliptical galaxies were already well established in X-ray-luminous clusters when the universe was a third of its present age.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/ed566514cc16bdce0795fb451400013926da6c44

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

Mass-to-Light Ratios of Field Early-Type Galaxies at z ~ 1 from Ultradeep Spectroscopy: Evidence for Mass-dependent Evolution (2005, methodology): “(Blakeslee et al. 2003) provide ACS imaging on the CL1252 ﬁeld in the i and z bands.”
Ages and metallicities of early-type galaxies in the SDSS: new insight into the physical origin of the colour-magnitude and the Mg2-sigmaV relations (2006, background): “Studies of evolution with cosmic time indicate that the slope of the colour-magnitude relation has changed little since z ∼ 1 (Kodama & Arimoto 1997; Kodama et al. 1998; Stanford et al. 1998; Blakeslee et al. 2003).”
The first appearance of the red sequence of galaxies in proto-clusters at 2 <~ z <~ 3 (2007, background): “…Bower, Lucey, & Ellis 1992), and is well recognised even in distant clusters at least out to z ∼ 1 (e.g., Ellis et al. 1997; ⋆ E-mail: kodama@optik.mtk.nao.ac.jp Kodama et al. 1998; Stanford, Eisenhardt, & Dickinson 1998; van Dokkum et al. 1998; 2001; Blakeslee et al. 2003; Stanford et al. 2006).”
Evolution and Environment of Early-Type Galaxies (2005, methodology): “Previous work indicates that the slope of the color magnitude relation does not evolve out to redshifts of order unity, and this has been used to argue that residuals from the color magnitude relation are indicators of age (e.g. Kodama et al. 1998; Blakeslee et al. 2003).”
THE ATACAMA COSMOLOGY TELESCOPE: ACT-CL J0102−4915 “EL GORDO,” A MASSIVE MERGING CLUSTER AT REDSHIFT 0.87 (2011, background): “…Galaxy In Figure 12, we plot the observed i-band magnitude of the BCGs of ACT clusters in the southern sample, plus the BCG’s for three X-ray–selected, massive, high redshift clusters: RDCS 1252.9−2927 (Blakeslee et al. 2003; Rosati et al. 2004; Demarco et al. 2007) at z = 1.237, XMMU J2235.”
ANCIENT LIGHT FROM YOUNG COSMIC CITIES: PHYSICAL AND OBSERVATIONAL SIGNATURES OF GALAXY PROTO-CLUSTERS (2013, background): “CEP 20921-400, São Cristóvão, Rio de Janeiro-RJ, Brazil quence, and ICM in place, suggesting formation redshifts for most of their stellar contents much beyond 2 (Blakeslee et al. 2003; Mei et al. 2006; Andreon 2008; Papovich et al. 2010; Rettura et al. 2010, 2011; Fassbender et al. 2011b).”
THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. V. IMPROVING THE DARK-ENERGY CONSTRAINTS ABOVE z > 1 AND BUILDING AN EARLY-TYPE-HOSTED SUPERNOVA SAMPLE (2011, background): “In addition to the data that were taken during the search, five clusters, CL1604+4304 (Postman et al. 2005), RDCS0910+54 (Mei et al. 2006), RDCS0848+44 (Postman et al. 2005), RDCS1252− 9 (Blakeslee et al. 2003) and XMMU2235.”
Protoclusters associated with z > 2 radio galaxies - I. Characteristics of high redshift protoclusters (2006, methodology): “For example, the analysis of galaxies inz ∼ 1 clusters showed that the stars in massive, early-type galaxies formed atz > 2 (e.g., Ellis et al., 1997; Stanford et al., 1998; Blakeslee et al., 2003; van Dokkum & Stanford, 2003; Holden et al., 2005).”
A mature cluster with X-ray emission at z = 2.07 (2010, background): “Indeed,z & 1 X-ray and colourselected structures are spatially compact and dominated by massive early-type galaxies, as their local counterparts (Blakeslee et al. 2003, Mullis et al. 2005, Stanford et al. 2006, Papovich et al. 2010, Tanaka et al. 2010, Henry et al. 2010, Kurk et al. 2009).”
The Evolving Luminosity Function of Red Galaxies (2006, background): “A red galaxy locus is also observed within the z 1 cluster and field galaxy populations (van Dokkum et al. 2000; Blakeslee et al. 2003; Bell et al. 2004; Willmer et al. 2006).”
The Morphology-Density Relation in z ~ 1 Clusters (2005, methodology): “For reference, the characteristic magnitude, m , for cluster galaxies is i775 ¼ 22:3 at z ¼ 0:83 (Goto et al. 2005) and z850 ¼ 22:7 at z ¼ 1:24 (Blakeslee et al. 2003b).”
Clusters of Galaxies in the First Half of the Universe from the IRAC Shallow Survey (2008, background): “It should be noted that the very low scatters reported for z > 1 clusters in, e.g., Blakeslee et al. (2003) and Mei et al. (2006) are calculated for galaxies known to have early-type morphologies, using much deeper photometry than the survey/discovery data used here.”
A GMBCG GALAXY CLUSTER CATALOG OF 55,424 RICH CLUSTERS FROM SDSS DR7 (2010, background): “…colors) and a slightly tilted color magnitude relation, the study of which has a long history, e.g. (Visvanathan & Sandage 1977; Bower et al. 1992; Gladders et al. 1998; López-Cruz et al. 2004; Blakeslee et al. 2003, 2006; De Lucia et al. 2007; Stott et al. 2009; Mei et al. 2009; Hao et al. 2009).”
Hubble Space Telescope and Spitzer Imaging of Red and Blue Galaxies at z ~ 2.5: A Correlation between Size and Star Formation Activity from Compact Quiescent Galaxies to Extended Star-forming Galaxies (2007, background): “…galaxies with little ongoing star formation and dust, although the fraction of blue late-type galaxies in clusters increases with redshift (e.g., Blakeslee et al. 2003; Toft et al. 2004; Bell et al. 2004; McIntosh et al. 2005; Lidman et al. 2004;Mullis et al. 2005; Cooper et al. 2007; Cassata…”
The Effect of Environment on the Ultraviolet Color-Magnitude Relation of Early-Type Galaxies (2006, background): “Later studies have found that there is no significant evolution in the optical CMR out to z ¼ 1 and further (Ellis et al. 1997; Gladders et al. 1998; Stanford et al. 1998; van Dokkum et al. 2000; Blakeslee et al. 2003; Ferreras et al. 2005).”
The Evolution of the Star Formation Activity in Galaxies and Its Dependence on Environment (2005, background): “…redshift (z > 2) over a short timescale, that have been observed in clusters up to and beyondz = 1 (Bower et al. 1992, Ellis et al. 1997, Barger et al. 1998, Kodama et al. 1998, van Dokkum et al. 2000,2001, Blakeslee et al. 2003, De Lucia et al. 2004, Barrientos et al., 2004, Holden et al. 2005).”
EVOLUTION OF THE COLOR–MAGNITUDE RELATION IN GALAXY CLUSTERS AT z ∼ 1 FROM THE ACS INTERMEDIATE REDSHIFT CLUSTER SURVEY (2008, methodology): “…otherwise impossible from the ground at high redshift: 1) the morphological classification of galaxies as Hubble types out to z ≈ 1 (e.g. Postman et al. 2005) and 2) galaxy color measurements to an accuracy of a few percent of a magnitude (Sirianni et al. 2005; Blakeslee et al. 2003a).”
Properties of Lyα emitters around the radio galaxy MRC 0316 257 (2005, methodology): “Although clusters of galaxies have been studied extensively out to z ∼ 1.3 (e.g. Rosati et al., 1999; Della Ceca et al., 2000; Stanford et al., 2002; Blakeslee et al., 2003b; Maughan et al., 2003; Toft et al., 2004), the epoch of cluster formation is stll an open question due to the difficulty in…”