THE SHAPLEY SUPERCLUSTER .1. SPECTROSCOPIC OBSERVATIONS IN THE CENTRAL REGION

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dc.contributor.authorQUINTANA, H
dc.contributor.authorRAMIREZ, A
dc.contributor.authorMELNICK, J
dc.contributor.authorRAYCHAUDHURY, S
dc.contributor.authorSLEZAK, E
dc.date.accessioned2025-01-21T01:34:36Z
dc.date.available2025-01-21T01:34:36Z
dc.date.issued1995
dc.description.abstractWe present a new analysis of the kinematics of the Shapley supercluster based on radial velocities for 1087: galaxies in the clusters A3558 (Shapley 8), A3528 (Klemola 21), A3532 (Klemola 22), A3530, A3556 (SCI 1321-314), A3559 (CE 1327-292), A3560, A3562, SC 1329-314 and in the intercluster region of the core of the supercluster, of which 367 are new measurements. We also present accurate positions from APM and MAMA scans of the ESO/SERC Southern Sky Survey photographic plates. We obtain new velocity dispersions and estimate the masses of the member clusters, evaluating dynamical models of the supercluster. The supercluster is found to be significantly flattened. We find that for Omega(0)=0.3, H-0=75 km s(-1) Mpc(-1), the gravitational pull of the supercluster may account for up to 25% of the peculiar velocity of the Local Group required to explain the dipole anisotropy of the Cosmic Microwave Background radiation, in which case the mass of the supercluster would be dominated by intercluster dark matter. This fractional contribution would be considerably higher for combinations of significantly lower values of Omega(0) and higher values of H-0. 1995 American Astronomical Society.
dc.fuente.origenWOS
dc.identifier.issn0004-6256
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/97579
dc.identifier.wosidWOS:A1995RL50000001
dc.issue.numero2
dc.language.isoen
dc.pagina.final476
dc.pagina.inicio463
dc.revistaAstronomical journal
dc.rightsacceso restringido
dc.titleTHE SHAPLEY SUPERCLUSTER .1. SPECTROSCOPIC OBSERVATIONS IN THE CENTRAL REGION
dc.typeartículo
dc.volumen110
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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