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|Title:||Morphological fractions of galaxies in WINGS clusters: revisiting the morphology-density paradigm||Authors:||Fasano, G.
POGGIANTI, Bianca Maria
Couch, W. J.
|Issue Date:||2015||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||449||Issue:||4||First Page:||3927||Abstract:||We present the morphology-density and morphology-radius relations (T-Σ and T-R, respectively) obtained from the WIde-field Nearby Galaxy-cluster Survey (WINGS) data base of galaxies in nearby clusters. Aiming to achieve the best statistics, we exploit the whole sample of galaxies brighter than M<SUB>V</SUB> = -19.5 (5504 objects), stacking up the 76 clusters of the WINGS survey altogether. Using this global cluster sample, we find that the T-Σ relation holds only in the inner cluster regions (R < 1/3 R<SUB>200</SUB>), while the T-R relation keeps almost unchanged over the whole range of local density. A couple of tests and two sets of numerical simulations support the robustness of these results against the effects of the limited cluster area coverage of the WINGS imaging. The above mentioned results hold for all cluster masses (X-ray luminosity and velocity dispersion) and all galaxy stellar masses (M<SUB>*</SUB>). The strength of the T-Σ relation (where present) increases with increasing M<SUB>*</SUB>, while this effect is not found for the T-R relation. Noticeably, the absence/presence of subclustering determines the presence/absence of the T-Σ relation outside the inner cluster regions, leading us to the general conclusion that the link between morphology and local density is preserved just in dynamically evolved regions. We hypothesize that some mechanism of morphological broadening/redistribution operates in the intermediate/outer regions of substructured (`non-relaxed') clusters, producing a strong weakening of the T-Σ relation.||Acknowledgments:||We acknowledge partial financial support by contract PRIN/MIUR 2009: ‘Dynamics and Stellar Populations of Superdense Galaxies’ (Code: 2009L2J4MN) and by INAF/PRIN 2011: ‘Galaxy Evolution with the VLT Survey Telescope (VST)’. BV was supported by the World Premier International Research Center Initiative (WPI), MEXT, Japan, and by the Kakenhi Grant-in-Aid for Young Scientists (B)(26870140) from the Japan Society for the Promotion of Science (JSPS).||URI:||http://hdl.handle.net/20.500.12386/23092||URL:||https://academic.oup.com/mnras/article/449/4/3927/1175350||ISSN:||0035-8711||DOI:||10.1093/mnras/stv500||Bibcode ADS:||2015MNRAS.449.3927F||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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