Morphologies and stellar populations of galaxies in the core of Abell 2218

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dc.creatorSanchez, S. F.
dc.creatorCardiel, N.
dc.creatorVerheijen, M.
dc.creatorPedraz, S.
dc.creatorCovone, G.
dc.date2006-11-21
dc.date2006-11-22
dc.date.accessioned2026-07-07T10:20:56Z
dc.date.available2026-07-07T10:20:56Z
dc.descriptionSUMMARIZED ABSTRACT: We present a study of the stellar populations and morphologies of galaxies in the core of the galaxy cluster Abell 2218. Integral field spectroscopy was obtained using PMAS/PPAK@3.5m CAHA to obtain a complete flux limited sample of cluster members within its field-of-view (~74"X64"). In addition of 31 galaxies with known redshifts in the outer regions, we built up a final sample of 59 spectroscopically confirmed cluster members. Multiban photometry and detailed morphologies were obtained using deep images taken with the HST/ACS camera in the BVRI and z-bands. The CM diagram shows that the E-type galaxies cover the range of brighter and redder colors. A large fraction of spiral galaxies ($\sim$50%) is found. They cover a wide range in colors. This result, together with the distributions of ages, metallicities and masses, indicates that E-type galaxies are more massive and have older stellar populations, while L-type galaxies are less massive and have a wider range of stellar Our results agree with a proposed two-step scenario for the evolution of galaxies in clusters. In addition, an extremely blue merging galaxy system is found at the core, with the nominal redshift of the cluster.
dc.description29 pages, 17 figures, accepted for publishing in MNRAS. (HST/ACS composite image: http://www.caha.es/sanchez/abell2218/BRI_big.jpg)
dc.identifierhttps://arxiv.org/abs/astro-ph/0611660
dc.identifierhttp://arxiv.org/abs/astro-ph/0611660
dc.identifierMon.Not.Roy.Astron.Soc.376:125-150,2007
dc.identifierdoi:10.1111/j.1365-2966.2007.11335.x
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/175009
dc.subjectAstrophysics
dc.titleMorphologies and stellar populations of galaxies in the core of Abell 2218
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