The Morphology-Density Relation in z ~ 1 Clusters

By M. Postman, M. Franx, N. Cross, B. Holden, H. C. Ford, G. Illingworth, Tomotsugu Goto, R. Demarco, Piero Rosati, J. Blakeslee and 32 more. 2005

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We measure the morphology-density relation (MDR) and morphology-radius relation (MRR) for galaxies in seven z ~ 1 clusters that have been observed with the Advanced Camera for Surveys (ACS) on board the Hubble Space Telescope. Simulations and independent comparisons of our visually derived morphologies indicate that ACS allows one to distinguish between E, S0, and spiral morphologies down to z850 = 24, corresponding to L/L* = 0.21 and 0.30 at z = 0.83 and 1.24, respectively. We adopt density and radius estimation methods that match those used at lower redshift in order to study the evolution of the MDR and MRR. We detect a change in the MDR between 0.8 < z < 1.2 and that observed at z ~ 0, consistent with recent work; specifically, the growth in the bulge-dominated galaxy fraction, fE+S0, with increasing density proceeds less rapidly at z ~ 1 than it does at z ~ 0. At z ~ 1 and Σ ≥ 500 galaxies Mpc-2, we find ⟨fE+S0⟩ = 0.72 ± 0.10. At z ~ 0, an E+S0 population fraction of this magnitude occurs at densities about 5 times smaller. The evolution in the MDR is confined to densities Σ ≳ 40 galaxies Mpc-2 and appears to be primarily due to a deficit of S0 galaxies and an excess of Sp+Irr galaxies relative to the local galaxy population. The fE-density relation exhibits no significant evolution between z = 1 and 0. We find mild evidence to suggest that the MDR is dependent on the bolometric X-ray luminosity of the intracluster medium. Implications for the evolution of the disk galaxy population in dense regions are discussed in the context of these observations.

Subfields: Astronomy and Astrophysics, Instrumentation

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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.”
EVOLUTION OF THE COLOR–MAGNITUDE RELATION IN GALAXY CLUSTERS AT z ∼ 1 FROM THE ACS INTERMEDIATE REDSHIFT CLUSTER SURVEY (2008, methodology): “All ACS filter magnitudes are given in the AB system (Oke & Gunn 1983; for ACS see Sirianni et al. 2005), while magnitudes in the Johnson system (Johnson & Morgan 1953; Buser & Kurucz 1978; Bessel 1990) are given as Vega magnitudes (see also Appendix II).”
The zCOSMOS redshift survey: the role of environment and stellar mass in shaping the rise of the morphology-density relation from z ~ 1 (2009, methodology): “Further studies at high-z are mainly based on groups or clusters (Nuijten et al. 2005; Postman et al. 2005; Poggianti et al. 2008) and the first relevant attempts to extend this analysis to field galaxies (Smith et al. 2005; Capak et al. 2007; Guzzo et al. 2007; Holden et al. 2007; van der Wel et…”
WINGS: a WIde-field Nearby Galaxy-cluster Survey. I. Optical imaging (2005, background): “This change of the morphological mix in clusters is expressed in the evolution of the morphology-density relation with z (Dressler et al. 1997; Postman et al. 2005).”
The XMM-Newton Wide-Field Survey in the COSMOS Field: Statistical Properties of Clusters of Galaxies (2006, background): “…is justified by the large ages of cluster ellipticals and the lack of evolution in their morphological fraction with redshift (Smith et al. 2005; Postman et al. 2005; Wechsler et al. 2005; see also direct estimates from the COSMOS field in Capak et al. 2007 and Guzzo et al. 2007), where the…”
The Evolution of the Star Formation Activity in Galaxies and Its Dependence on Environment (2005, background): “Distant clusters generally contain a higher proportion of spirals, and a correspondingly lower proportion of S0 galaxies, than low-z clusters (Dressler et al. 1997, Couch et al. 1998, Fasano et al. 2000, Treu et al. 2003, Smith et al. 2005, Postman et al. 2005).”
Revisiting the Hubble sequence in the SDSS DR7 spectroscopic sample: a publicly available Bayesian automated classification (2010, background): “This 12% scatter is com- patible and even less than the typical scatter found when several people perform visual classifications on the same sample (e.g.Postman et al. 2005; Fukugita et al. 2007).”
A mature cluster with X-ray emission at z = 2.07 (2010, background): “The strong dependence of galaxy activity on the surrounding environment, which gives rise to the wellknown correlations of morphological type (Postman et al. 2005, Hwang & Park 2009, van der Wel et al. 2010) and decreas- ing star formation (Hashimoto et al. 1998, Patel et al. 2009, Rettura et al.…”
A Wide-Field Survey of Two z ~ 0.5 Galaxy Clusters: Identifying the Physical Processes Responsible for the Observed Transformation of Spirals into S0s (2007, background): “…the fraction of early-type (elliptical and S0) galaxies and the fraction of passive non-star-forming galaxies both grow with time, and at a rate that seems to depend sensitively on the local density of galaxies (Dressler et al. 1997; Poggianti et al. 1999; Smith et al. 2005a; Postman et al. 2005).”
The STAGES view of red spirals and dusty red galaxies: Mass-dependent quenching of star formation in cluster infall (2008, background): “The local morphology–density relation (Dressler 1980) appears to persist out to z ∼ 0.7 in the field (Guzzo et al. 2007) and to z ∼ 1 in clusters (Postman et al. 2005), while the SF–density relation appears to invert its slope between high redshift where SF first commences at highest densities (see…”
Galaxy Zoo: the dependence of morphology and colour on environment (2008, methodology): “The evolution found by previous studies (Smith et al. 2005; Postman et al. 2005) is attributed to effects of their luminosity-based selection.”
On the evolution and environmental dependence of the star formation rate versus stellar mass relation since z ∼ 2 (2013, background): “The environmental trends are also seen in the distant Universe (e.g. Kodama et al. 2001; Postman et al. 2005; Quadri etal.”
The build-up of the colour-magnitude relation in galaxy clusters since z ~ 0.8 (2006, background): “More recent work has provided us with a much more detailed picture of these differences (a very incomplete list of recent papers includes Stanford et al. 2005; Postman et al. 2005; Jørgensen et al. 2005; White et al. 2005; Poggianti et al. 2006; Strazzullo et al. 2006).”
SPECTROSCOPIC CONFIRMATION OF TWO MASSIVE RED-SEQUENCE-SELECTED GALAXY CLUSTERS AT z ∼ 1.2 IN THE SpARCS-NORTH CLUSTER SURVEY (2008, background): “…the SFR (e.g., Elbaz et al. 2007; Cooper et al. 2008; Poggianti et al. 2008), color (e.g., Cooper et al. 2007) and morphology (e.g., Dressler et al. 1997; Postman et al. 2005; Smith et al. 2005, Capak et al. 2007) are still correlated with local density, albeit differently from the nearby universe.”
The realm of the galaxy protoclusters (2016, background): “Massive clusters at z ∼ 1 generally have strong red sequences (e.g., Postman et al., 2005; Blakeslee et al., 2006; van der Wel et al., 2007; Patel et al., 2009; Mei et al., 2009; Muzzin et al., 2012; Foltz et al., 2015).”
The DEEP2 galaxy redshift survey: evolution of the colour–density relation at 0.4 < z < 1.35 (2006, background): “For example, building upon the work of Dressler et al. (1997), Smith et al. (2005) and Postman et al. (2005) find that the fraction of early–type galaxies increases steadily with density in cluster environments out to z ∼ 1, with the strength of the correlation weaker at z ∼ 1 than in local samples.”
The ATLAS3D project - VII. A new look at the morphology of nearby galaxies: the kinematic morphology-density relation (2011, background): “This is qualitatively in agreement with numerical simulations (Tonnesen et al. 2007) and with detailed predictions computed for a sample of eight clusters, as part of the LoCuSS survey, indicating that ram-stripping becomes important insider <∼ r200/3 (Smith et al. 2010, see also Moran et al. 2007),”