The zCOSMOS redshift survey: the role of environment and stellar mass in shaping the rise of the morphology-density relation from z ~ 1

By L. Tasca, Jean-Paul Kneib, A. Iovino, O. Fèvre, K. Kovač, M. Bolzonella, S. Lilly, R. Abraham, P. Cassata, O. Cucciati and 50 more. 2009

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For more than two decades we have known that galaxy morphological segregation is present in the Local Universe. It is important to see how this relation evolves with cosmic time. To investigate how galaxy assembly took place with cosmic time, we explore the evolution of the morphology-density relation up to redshift z~1 using about 10000 galaxies drawn from the zCOSMOS Galaxy Redshift Survey. Taking advantage of accurate HST/ACS morphologies from the COSMOS survey, of the well-characterised zCOSMOS 3D environment, and of a large sample of galaxies with spectroscopic redshift, we want to study here the evolution of the morphology-density relation up to z~1 and its dependence on galaxy luminosity and stellar mass. The multi-wavelength coverage of the field also allows a first study of the galaxy morphological segregation dependence on colour. We further attempt to disentangle between processes that occurred early in the history of the Universe or late in the life of galaxies. The zCOSMOS field benefits of high-resolution imaging in the F814W filter from the Advanced Camera for Survey (ACS). We use standard morphology classifiers, optimised for being robust against band-shifting and surface brightness dimming, and a new, objective, and automated method to convert morphological parameters into early, spiral, and irregular types. We use about 10000 galaxies down to I_AB=22.5 with a spectroscopic sampling rate of 33% to characterise the environment of galaxies up to z~1 from the 100 kpc scales of galaxy groups up to the 100 Mpc scales of the cosmic web. ABRIDGED

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

View Paper: https://www.semanticscholar.org/paper/08de9fc76b144cb2c1786115b88366f6d72e7070

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Citations in the corpus

The ATLAS3D project - VII. A new look at the morphology of nearby galaxies: the kinematic morphology-density relation (2011, background): “…classified as ellipticals, suggesting that the most massive galaxies are already in place beyondz ∼ 1 (Stanford et al. 1998; Postman et al. 2005; Tasca et al. 2009), while most of the observed evolution consists of a transformation of spirals into S0s (Smith et al. 2005; Moran et al. 2007).”
Structure and Kinematics of Early-Type Galaxies from Integral Field Spectroscopy (2016, background): “…that these massive ellipticals were already passive from larger redshift and remain so during their evolution (Stanford et al. 1998; Postman et al. 2005; Tasca et al. 2009), while most of the observed evolution consists of a transformation of spirals into S0s (Smith et al. 2005; Moran et al. 2007).”
Tracking the impact of environment on the galaxy stellar mass function up to z ~ 1 in the 10 k zCOSMOS sample (2009, background): “…infer that all the galaxy properties depending on mass will also dependon environment by virtue of the GSMF environmental dependence, as shown in the case of the colour-density and morphologydensity relations (Cucciati et al. 2009; Tasca et al. 2009) and of the AGN fraction (Silverman et al. 2009).”
Environment and self-regulation in galaxy formation (2009, background): “This implies that the impact of environment increases with decreasing galaxy mass (Tasca et al. 2009).”
THE RISE AND FALL OF PASSIVE DISK GALAXIES: MORPHOLOGICAL EVOLUTION ALONG THE RED SEQUENCE REVEALED BY COSMOS (2009, unknown): “C O ] 2 1 Ju l 2 01 0 been studied (Bundy et al. 2006; Cucciati et al. 2006; Cooper et al. 2008; Capak et al. 2007a; van der Wel 2008; Pannella et al. 2009; Tasca et al. 2009; Bolzonella et al. 2009).”
Measures of Galaxy Environment I - What is "Environment"? (2011, background): “These techniques are better suited to analysing targeted halo and galaxy environment correlations and have proven valuable in the current era of large galaxy survey data sets, where galaxy catalogues can be simultaneously ‘sliced’ in multiple orthogonal directions to isolate the dependence of specif”
MASS AND ENVIRONMENT AS DRIVERS OF GALAXY EVOLUTION IN SDSS AND zCOSMOS AND THE ORIGIN OF THE SCHECHTER FUNCTION (2010, methodology): “The reader is referred to a number of detailed studies of the properties of galaxies in different environments that have been undertaken using this sample (Cucciati et al., 2009, Tasca et al., 2009, Iovino et al., 2009, Kovač et al., 2009, Vergani et al., 2010, Zucca et al., 2009).”
The Evolution of Galaxy Structure Over Cosmic Time (2014, methodology): “For field galaxies, Tasca et al. (2009) examine the morphology-density relationship for 100,000 galaxies in the COSMOS survey.”
THE CHANDRA COSMOS SURVEY. III. OPTICAL AND INFRARED IDENTIFICATION OF X-RAY POINT SOURCES (2012, methodology): “We correlated the C-COSMOS counterparts catalog with the Tasca et al. (2009) catalog which reports the morphological parametric quantities, computed using Morpheus 2005 (Abraham et al. 2007) on HST-ACS images, for several thousands COSMOS sources toi=22.5.”
Bulge mass is king: the dominant role of the bulge in determining the fraction of passive galaxies in the Sloan Digital Sky Survey (2014, background): “Additionally there is a tendency for galaxies at higher densities to be more bulge dominated and hence have higher Sérsic index and concentration parameters (Dressler 1984, Moran et al. 2007, Tasca et al. 2009).”
THE zCOSMOS 10k-BRIGHT SPECTROSCOPIC SAMPLE (2009, background): “…and redshift (Maier et al. 2009; Bolzonella et al. 2009; Pozetti et al. 2009; Cucciati et al. 2009; Iovino et al. 2009; Kovac et al. 2009b; Tasca et al. 2009; Vergani et al. 2009; Zucca et al. 2009), studies of the correlation function (Gilli et al. 2009; Meneux et al. 2009; de la Torre…”
zCOSMOS – 10k-bright spectroscopic sample - The bimodality in the galaxy stellar mass function: exploring its evolution with redshift (2009, methodology): “…in the morphological classification, we used two of the available estimates, i.e., the Zurich Estimator of Structural Types (ZEST; Scarlata et al. 2007a) and a non-parametric estimate derived by our collaborators in Marseille (MRS hereafter, Cassata et al. 2007, 2008, Tasca et al. 2009).”