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http://hdl.handle.net/20.500.12386/23359
Campo DC | Valore | Lingua |
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dc.contributor.author | Merten, J. | en_US |
dc.contributor.author | MENEGHETTI, MASSIMO | en_US |
dc.contributor.author | Postman, M. | en_US |
dc.contributor.author | Umetsu, K. | en_US |
dc.contributor.author | Zitrin, A. | en_US |
dc.contributor.author | Medezinski, E. | en_US |
dc.contributor.author | NONINO, Mario | en_US |
dc.contributor.author | Koekemoer, A. | en_US |
dc.contributor.author | Melchior, P. | en_US |
dc.contributor.author | Gruen, D. | en_US |
dc.contributor.author | Moustakas, L. A. | en_US |
dc.contributor.author | Bartelmann, M. | en_US |
dc.contributor.author | Host, O. | en_US |
dc.contributor.author | Donahue, M. | en_US |
dc.contributor.author | Coe, D. | en_US |
dc.contributor.author | Molino, A. | en_US |
dc.contributor.author | Jouvel, S. | en_US |
dc.contributor.author | Monna, A. | en_US |
dc.contributor.author | Seitz, S. | en_US |
dc.contributor.author | Czakon, N. | en_US |
dc.contributor.author | Lemze, D. | en_US |
dc.contributor.author | Sayers, J. | en_US |
dc.contributor.author | Balestra, I. | en_US |
dc.contributor.author | Rosati, P. | en_US |
dc.contributor.author | Benítez, N. | en_US |
dc.contributor.author | BIVIANO, ANDREA | en_US |
dc.contributor.author | Bouwens, R. | en_US |
dc.contributor.author | Bradley, L. | en_US |
dc.contributor.author | Broadhurst, T. | en_US |
dc.contributor.author | Carrasco, M. | en_US |
dc.contributor.author | Ford, H. | en_US |
dc.contributor.author | Grillo, C. | en_US |
dc.contributor.author | Infante, L. | en_US |
dc.contributor.author | Kelson, D. | en_US |
dc.contributor.author | Lahav, O. | en_US |
dc.contributor.author | Massey, R. | en_US |
dc.contributor.author | Moustakas, J. | en_US |
dc.contributor.author | RASIA, ELENA | en_US |
dc.contributor.author | Rhodes, J. | en_US |
dc.contributor.author | Vega, J. | en_US |
dc.contributor.author | Zheng, W. | en_US |
dc.date.accessioned | 2020-03-18T15:57:35Z | - |
dc.date.available | 2020-03-18T15:57:35Z | - |
dc.date.issued | 2015 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/23359 | - |
dc.description | The research was in part carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. J. M. has received funding from the People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme (FP7/2007–2013) under REA grant agreement number 627288. M. M. thanks ORAU and NASA for supporting his research at JPL and acknowledges support from the contract ASI/INAF I/023/12/0, INFN/PD51, and the PRIN MIUR 20102011 “The dark universe and the cosmic evolution of baryons: from current surveys to Euclid.” K. U. acknowledges support from the National Science Council of Taiwan (grant NSC100-2112-M-001-008-MY3) and from the Academia Sinica Career Development Award. Support for A. Z. is provided by NASA through Hubble Fellowship grant # HST -HF-51334.01 A awarded by STScI. D. G., S. S. and P. R. were supported by SFB Transregio 33 “The Dark universe” by the Deutsche Forschungsgemeinschaft (DFG) and the DFG cluster of excellence “Origin and Structure of the universe.” This work was supported in part by contract research “Internationale Spitzenforschung II/2-6” of the Baden Württemberg Stiftung. The Dark Cosmology Centre is funded by the DNRF. J. S. was supported by NSF/AST1313447, NASA/NNX11AB07G, and the Norris Foundation CCAT Postdoctoral Fellowship. E.R. acknowledges support from the National Science Foundation AST-1210973, SAO TM3-14008X (issued under NASA Contract No. NAS8-03060) Figure 15. Convergence maps for 20 X-ray selected CLASH clusters. The field size for the map of Abell 1423 is , for CL J1226 it is , and for Abell 611 it is . For all other clusters the field size is . The color coding, together with the colorbar shows the lensing convergence, scaled to a redshift of z = 20,000. Extended white patches in the convergence maps indicate field masks, usually at the position of bright foreground stars. The orientation of all maps is north is up. Figure 16. Convergence/surface-mass density profiles for 19 X-ray selected CLASH clusters. The black data points show the mean convergence in each bin. The square inset in the bottom left of each panel is the covariance matrix of the binned data and the error bars attached to each black data point show the square root of the diagonal elements of this matrix. Shown by the blue line is the best-fit NFW profile to the data. All radii refer to the peak in the dark matter density distribution of each halo as a center. Drawn in red are , , and and the virial radius of the halo. The convergence values are scaled to a source redshift of z = 20,000. | - |
dc.description.abstract | We present a new determination of the concentration-mass (c-M) relation for galaxy clusters based on our comprehensive lensing analysis of 19 X-ray selected galaxy clusters from the Cluster Lensing and Supernova Survey with Hubble (CLASH). Our sample spans a redshift range between 0.19 and 0.89. We combine weak-lensing constraints from the Hubble Space Telescope (HST) and from ground-based wide-field data with strong lensing constraints from HST. The results are reconstructions of the surface-mass density for all CLASH clusters on multi-scale grids. Our derivation of Navarro-Frenk-White parameters yields virial masses between 0.53× {{10}<SUP>15</SUP>} {{M}<SUB>☉ </SUB>}/h and 1.76× {{10}<SUP>15</SUP>} {{M}<SUB>☉ </SUB>}/h and the halo concentrations are distributed around {{c}<SUB>200c</SUB>}̃ 3.7 with a 1σ significant negative slope with cluster mass. We find an excellent 4% agreement in the median ratio of our measured concentrations for each cluster and the respective expectation from numerical simulations after accounting for the CLASH selection function based on X-ray morphology. The simulations are analyzed in two dimensions to account for possible biases in the lensing reconstructions due to projection effects. The theoretical c-M relation from our X-ray selected set of simulated clusters and the c-M relation derived directly from the CLASH data agree at the 90% confidence level. | en_US |
dc.language.iso | eng | en_US |
dc.title | CLASH: The Concentration-Mass Relation of Galaxy Clusters | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1088/0004-637X/806/1/4 | en_US |
dc.identifier.scopus | 2-s2.0-84934933322 | en_US |
dc.identifier.isi | 000356810300004 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.1088/0004-637X/806/1/4 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 806 | en_US |
dc.relation.issue | 1 | en_US |
dc.relation.firstpage | 4 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | USA | en_US |
dc.contributor.country | GBR | en_US |
dc.contributor.country | DEU | en_US |
dc.contributor.country | ESP | en_US |
dc.contributor.country | AUT | en_US |
dc.contributor.country | CHL | en_US |
dc.contributor.country | JPN | en_US |
dc.contributor.country | ISR | en_US |
dc.contributor.country | NLD | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | en_US |
dc.identifier.adsbibcode | 2015ApJ...806....4M | en_US |
dc.relation.ercsector | Scienze Fisiche Settori ERC (ERC) di riferimento::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegherò 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 | OAS Bologna | - |
crisitem.author.dept | O.A. Trieste | - |
crisitem.author.dept | O.A. Trieste | - |
crisitem.author.dept | O.A. Trieste | - |
crisitem.author.orcid | 0000-0003-1225-7084 | - |
crisitem.author.orcid | 0000-0001-6342-9662 | - |
crisitem.author.orcid | 0000-0002-0857-0732 | - |
crisitem.author.orcid | 0000-0003-4175-002X | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
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