The Evolution of the Galactic Morphological Types in Clusters

By G. Fasano, B. Poggianti, W. Couch, D. Bettoni, P. Kjærgaard, M. Molés. 2000

224 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Ecology, Instrumentation

View Paper: https://www.semanticscholar.org/paper/9957c5002c1d9b94de09bddc2bee642e740a98aa

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Citations in the corpus

Stellar Population Diagnostics of Elliptical Galaxy Formation (2006, background): “(1997) and Fasano et al. (2000) showed that in clusters up to z ∼ 0.5 the fraction of true ellipticals is fairly constant, while the fraction of (star-forming) spirals rapidly increases at the expense of the S0’s.”
Environmental Effects on Late‐Type Galaxies in Nearby Clusters (2006, background): “In distant clusters, the spiral fraction is larger than in nearby clusters, the elliptical fraction is the same or larger, and the lenticular fraction is a factor of ∼2–3 smaller (Dressler et al. 1997; Fasano et al. 2000).”
Environment and self-regulation in galaxy formation (2009, background): “…Antonuccio-Delogu & Rifatto 2006; Holden et al. 2007; Park et al. 2007; van der Wel et al. 2007; Bamford et al. 2009) and intermediate redshift Universe (Dressler et al. 1997; Fasano et al. 2000; Treu et al. 2003; Smith et al. 2005; van der Wel et al. 2007; Pannella et al. 2009; Tasca et al. 2009).”
The Morphology-Density Relation in z ~ 1 Clusters (2005, background): “However, many previous observations, including the relatively weak dependence of fS0 on projected density, strongly suggest that ram pressure stripping alone cannot explain the morphological mix in clusters (e.g., D80; D97; Kodama & Smail 2001; Okamoto & Nagashima 2003).”
WINGS: a WIde-field Nearby Galaxy-cluster Survey. I. Optical imaging (2005, methodology): “Similarly, using excellentseeing, ground based imaging with the NOT telescope (La Palma), Fasano et al. (2000) completed the picture in the range 0.1 ≤ z ≤ 0.25, showing that the S0 population smoothly grows from z ∼ 0.5 to z ∼ 0, at the expense of the population of spiral galaxies.”
The Tully-Fisher relations of early-type spiral and S0 galaxies (2010, background): “…by high-redshift observations: while Dressler et al. (1997) show that the S0 fraction has risen at the expense of spirals since z≈ 0.5 (5 Gyr ago), Fasano et al. (2000) find that the present relative fraction of S0s and spirals was largely already in place in clusters at z≈ 0.2 (2.5 Gyr ago) and…”
Structure and Kinematics of Early-Type Galaxies from Integral Field Spectroscopy (2016, background): “The trend is much reduced in the field (Dressler et al. 1997; Fasano et al. 2000; Postman et al. 2005; Smith et al. 2005).”
Evolution since z = 1 of the Morphology-Density Relation for Galaxies (2004, background): “…et al. found that the fraction of lenticular galaxies in clusters declined by a factor of 2–3 betweenz=0 and z=0.5 and this evolution was accompanied by a corresponding increase in the fraction of star–forming spirals (see also Andreon 1998; Couch et al. 1998; Fasano et al. 2000; Treu et al. 2003).”
A Comparison of the Galaxy Populations in the Coma and Distant Clusters: The Evolution of k+a Galaxies and the Role of the Intracluster Medium (2003, background): “…1984; Ellingson et al. 2001; Kodama & Bower 2001; Stanford, Eisenhardt, & Dickinson 1998; Kodama et al. 1998), morphologies (Dressler et al. 1997; Fasano et al. 2000; van Dokkum et al. 2000; Lubin, Oke, & Postman 2002), scaling relations (Kelson et al. 1997, 2000; Ziegler & Bender 1997), and…”
BUDHIES II: a phase-space view of H i gas stripping and star formation quenching in cluster galaxies (2015, background): “Moreover, observations of distant galaxies have shown a steady rise in the fraction of S0s in clusters, along with a comparable decline in the spiral fraction since z ∼ 0.5, while the fraction of elliptical galaxies remains constant (Fasano et al. 2000; Desai et al. 2007).”
The Build-up of the Colour-Magnitude Relation (2005, background): “For example, the morphology–density relation is found to evolve (Dressler et al. 1997; Fasano et al. 2000; Treu et al. 2003; Smith et al. 2005, but see also Andreon 1998).”
Pre-Processing of Galaxies before Entering a Cluster (2003, background): “At the same time, various studies have reported a morphological evolution in cluster galaxies; they have shown that the fractions of S0 galaxies in clusters decrease toward a higher redshift (Dressler et al. 1997; Couch et al. 1994, 1998; Fasano et al. 2000).”
The Evolution of the Star Formation Activity in Galaxies and Its Dependence on Environment (2005, background): “This suggestion was supported by the findings of Fasano et al. (2000) that clusters atz ∼ 0.1− 0.2 have a low (high) S0/E number ratio if they display (lack) a strong concentration of elliptical galaxies towards the cluster center.”
The Environmental Dependence of Galaxy Properties in the Local Universe: Dependences on Luminosity, Local Density, and System Richness (2004, background): “…Lin, & Tucker 1998; Balogh et al. 1999; Poggianti et al. 1999; Couch et al. 2001; Lewis et al. 2002; Gómez et al. 2003; Blanton et al. 2003a) with possible evolution (Butcher & Oemler 1984; Couch & Sharples 1987; Dressler et al. 1997; Andreon 1998; Fasano et al. 2000; Goto et al. 2003a, 2004).”
The spatial and kinematic distributions of cluster galaxies in a ΩCDM universe: comparison with observations (2000, background): “This has recently been confirmed by a separate study by Fasano et al (2000).”
The ATLAS3D project - VII. A new look at the morphology of nearby galaxies: the kinematic morphology-density relation (2011, methodology): “This is interpreted as due to the fact that the morphologicalsegregation proceeds faster, and thus affects earlier, the denser cluster environments (Dressler et al. 1997; Fasano et al. 2000; Postman et l. 2005; Smith et al. 2005).”
THE GALAXY CONTENT OF SDSS CLUSTERS AND GROUPS (2007, background): “…also show a trend with redshift (Allington-Smith et al. 1993; Oemler et al. 1997; Balogh et al. 1997; Couch et al. 1998; van Dokkum et al. 2000; Fasano et al. 2000; Lubin et al. 2002; Goto et al. 2003; Treu et al. 2003; Wilman et al. 2005; Poggianti et al. 2006; Desai et al. 2007; van der Wel…”