Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/27414
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | I. Chiu | en_US |
dc.contributor.author | J. Mohr | en_US |
dc.contributor.author | M. Mcdonald | en_US |
dc.contributor.author | S. Bocquet | en_US |
dc.contributor.author | M. L. Ashby | en_US |
dc.contributor.author | M. Bayliss | en_US |
dc.contributor.author | B. A. Benson | en_US |
dc.contributor.author | L. E. Bleem | en_US |
dc.contributor.author | M. Brodwin | en_US |
dc.contributor.author | S. Desai | en_US |
dc.contributor.author | J. P. Dietrich | en_US |
dc.contributor.author | W. R. Forman | en_US |
dc.contributor.author | C. Gangkofner | en_US |
dc.contributor.author | A. H. Gonzalez | en_US |
dc.contributor.author | C. Hennig | en_US |
dc.contributor.author | J. Liu | en_US |
dc.contributor.author | C. L. Reichardt | en_US |
dc.contributor.author | A. Saro | en_US |
dc.contributor.author | B. Stalder | en_US |
dc.contributor.author | S. A. Stanford | en_US |
dc.contributor.author | J. Song | en_US |
dc.contributor.author | T. Schrabback | en_US |
dc.contributor.author | R. Suhada | en_US |
dc.contributor.author | STRAZZULLO, VERONICA | en_US |
dc.contributor.author | A. Zenteno | en_US |
dc.date.accessioned | 2020-09-16T11:20:22Z | - |
dc.date.available | 2020-09-16T11:20:22Z | - |
dc.date.issued | 2016 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/27414 | - |
dc.description.abstract | We study the stellar, brightest cluster galaxy (BCG) and intracluster medium (ICM) masses of 14 South Pole Telescope (SPT) selected galaxy clusters with median redshift z = 0.9 and mass M500 = 6 × 1014 M☉. We estimate stellar masses for each cluster and BCG using six photometric bands, the ICM mass using X-ray observations and the virial masses using the SPT Sunyaev-Zel'dovich effect signature. At z = 0.9, the BCG mass M_{star }^{BCG} constitutes 0.12 ± 0.01 per cent of the halo mass for a 6 × 1014 M☉ cluster, and this fraction falls as M_{500}^{-0.58± 0.07}. The cluster stellar mass function has a characteristic mass M0 = 1011.0 ± 0.1 M☉, and the number of galaxies per unit mass in clusters is larger than in the field by a factor of 1.65 ± 0.20. We combine our SPT sample with previously published samples at low redshift and correct to a common initial mass function and for systematic virial mass differences. We then explore mass and redshift trends in the stellar fraction f⋆, the ICM fraction fICM, the collapsed baryon fraction fc and the baryon fraction fb. At a pivot mass of 6 × 1014 M☉ and redshift z = 0.9, the characteristic values are f⋆ = 1.1 ± 0.1 per cent, fICM = 9.6 ± 0.5 per cent, fc = 10.7 ± 1.1 per cent and fb = 10.7 ± 0.6 per cent. These fractions all vary with cluster mass at high significance, with higher mass clusters having lower f⋆ and fc and higher fICM and fb. When accounting for a 15 per cent systematic virial mass uncertainty, there is no statistically significant redshift trend at fixed mass. Our results support the scenario where clusters grow through accretion from subclusters (higher f⋆, lower fICM) and the field (lower f⋆, higher fICM), balancing to keep f⋆ and fICM approximately constant since z ∼ 0.9. | en_US |
dc.language.iso | eng | en_US |
dc.title | Baryon Content of Massive Galaxy Clusters (0.57 < z < 1.33) | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stv2303 | en_US |
dc.identifier.scopus | 2-s2.0-84954422819 | en_US |
dc.identifier.isi | 000368005900043 | en_US |
dc.identifier.url | http://arxiv.org/abs/1412.7823v2 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/455/1/258/984806 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 455 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 258 | en_US |
dc.relation.lastpage | 275 | en_US |
dc.type.referee | REF_1 | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2016MNRAS.455..258C | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | O.A. Trieste | - |
crisitem.author.orcid | 0000-0001-7975-2894 | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
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