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OMEGA – OSIRIS mapping of emission-line galaxies in A901/2 : III. Galaxy properties across projected phase space in A901/2
dc.contributor.author | Weinzirl, Timothy | pt_BR |
dc.contributor.author | Aragón-Salamanca, Alfonso | pt_BR |
dc.contributor.author | Gray, Meghan E. | pt_BR |
dc.contributor.author | Bamford, Steven Peter | pt_BR |
dc.contributor.author | Rodríguez del Pino, Bruno | pt_BR |
dc.contributor.author | Chies-Santos, Ana Leonor | pt_BR |
dc.contributor.author | Böhm, Asmus | pt_BR |
dc.contributor.author | Wolf, Christian | pt_BR |
dc.contributor.author | Cool, Richard J. | pt_BR |
dc.date.accessioned | 2017-11-25T02:26:59Z | pt_BR |
dc.date.issued | 2017 | pt_BR |
dc.identifier.issn | 0035-8711 | pt_BR |
dc.identifier.uri | http://hdl.handle.net/10183/170580 | pt_BR |
dc.description.abstract | We conduct a comprehensive projected phase-space analysis of the A901/2 multicluster system at z ∼ 0.165. Aggregating redshifts from spectroscopy, tunable-filter imaging and prism techniques, we assemble a sample of 856 cluster galaxies reaching 108.5M in stellar mass. We look for variations in cluster galaxy properties between virialized and non-virialized regions of projected phase space (PPS). Our main conclusions point to relatively gentle environmental effects, expressedmainly on galaxy gas reservoirs. (1) Stacking the four subclusters in A901/2, we find galaxies in the virialized region are more massive, redder and have marginally higher S´ersic indices, but their half-light radii and Hubble types are not significantly different. (2) After accounting for trends in stellar mass, there is a remaining change in rest-frame colour across PPS. Primarily, the colour difference is due to the absence in the virialized region of galaxies with rest frame B − V < 0.7 and moderate-to-high (M > 109.85 M ) stellar mass. (3) There is an infalling population of lower mass (M ≤ 109.85 M ), relatively blue (B − V < 0.7) elliptical or spheroidal galaxies that are strikingly absent in the virialized region. (4) The number of bona fide star-forming and active galactic nucleus galaxies in the PPS regions is strongly dictated by stellar mass. However, there remains a reduced fraction of star-forming galaxies in the centres of the clusters at fixed stellar mass, consistent with the star formation–density relation in galaxy clusters. (5) There is no change in specific Hα-derived star formation rates of star-forming galaxies at fixed mass across the cluster environment. This suggests that pre-processing of galaxies during infall plays a prominent role in quenching star formation. | en |
dc.format.mimetype | application/pdf | |
dc.language.iso | eng | pt_BR |
dc.relation.ispartof | Monthly notices of the Royal Astronomical Society. Oxford. Vol. 471, no. 1 (Oct. 2017), p. 182-200 | pt_BR |
dc.rights | Open Access | en |
dc.subject | Instrumentation: interferometers | en |
dc.subject | Metalicidade | pt_BR |
dc.subject | Mapeamentos astronômicos | pt_BR |
dc.subject | Galaxies: clusters: individual: A901/2 | en |
dc.subject | Galaxies: distances and redshifts | en |
dc.subject | Nucleo galatico | pt_BR |
dc.subject | Deslocamento para o vermelho | pt_BR |
dc.subject | Galaxies: star formation | en |
dc.title | OMEGA – OSIRIS mapping of emission-line galaxies in A901/2 : III. Galaxy properties across projected phase space in A901/2 | pt_BR |
dc.type | Artigo de periódico | pt_BR |
dc.identifier.nrb | 001051459 | pt_BR |
dc.type.origin | Estrangeiro | pt_BR |
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