Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/23321
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Coupon, J. | - |
dc.contributor.author | Arnouts, S. | - |
dc.contributor.author | van Waerbeke, L. | - |
dc.contributor.author | Moutard, T. | - |
dc.contributor.author | Ilbert, O. | - |
dc.contributor.author | van Uitert, E. | - |
dc.contributor.author | Erben, T. | - |
dc.contributor.author | GARILLI, BIANCA MARIA ROSA | - |
dc.contributor.author | Guzzo, L. | - |
dc.contributor.author | Heymans, C. | - |
dc.contributor.author | Hildebrandt, H. | - |
dc.contributor.author | Hoekstra, H. | - |
dc.contributor.author | Kilbinger, M. | - |
dc.contributor.author | Kitching, T. | - |
dc.contributor.author | Mellier, Y. | - |
dc.contributor.author | Miller, L. | - |
dc.contributor.author | SCODEGGIO, MARCO | - |
dc.contributor.author | Bonnett, C. | - |
dc.contributor.author | Davidzon, I. | - |
dc.contributor.author | DE LUCIA, GABRIELLA | - |
dc.contributor.author | Fritz, A. | - |
dc.contributor.author | Fu, L. | - |
dc.contributor.author | Hudelot, P. | - |
dc.contributor.author | Hudson, M. J. | - |
dc.contributor.author | Kuijken, K. | - |
dc.contributor.author | Leauthaud, A. | - |
dc.contributor.author | Le Fèvre, O. | - |
dc.contributor.author | McCracken, H. J. | - |
dc.contributor.author | Moscardini, L. | - |
dc.contributor.author | Rowe, B. T. P. | - |
dc.contributor.author | Schrabback, T. | - |
dc.contributor.author | Semboloni, E. | - |
dc.contributor.author | Velander, M. | - |
dc.contributor.author | Branchini, Enzo Franco | - |
dc.date.accessioned | 2020-03-17T14:04:35Z | - |
dc.date.available | 2020-03-17T14:04:35Z | - |
dc.date.issued | 2015 | - |
dc.identifier.issn | 0035-8711 | - |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/23321 | - |
dc.description | This work is primarily based on observations obtained with WIRCam, a joint project of CFHT, Taiwan, Korea, Canada, France, at the Canada–France–Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France and the University of Hawaii. The WIRCAM images have been collected during several semesters and from different programs. We thank G. Morrison, J. Willis and K. Thanjavur for leading some of these programmes as PIs, and a special thanks to the canadian agency who always highly ranked these proposals. We thank the Terapix team for the reduction of all the WIRCAM images and the preparation of the catalogues matching the T0007 CFHTLS data release. The CFHTLenS project is based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU, at the CFHT. This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. We thank the CFHT staff for successfully conducting the CFHTLS observations and in particular J.-C. Cuillandre and E. Magnier for the continuous improvement of the instrument calibration and the Elixir detrended data that we used. We also thank terapix for the quality assessment and validation of individual exposures during the CFHTLS data acquisition period, and E. Bertin for developing some of the software used in this study. CFHTLenS data processing was made possible thanks to significant computing support from the NSERC Research Tools and Instruments grant program, and to HPC specialist O. Toader. Part of the numerical computations were done on the Sciama High Performance Compute (HPC) cluster which is supported by the ICG, SEPNet and the University of Portsmouth. We thank M. Cousin and S. de la Torre for useful discussions related to this work. We thank S. Birrer and D. Wake for providing us with their measurements. JC acknowledges the support from the laboratoire de Marseille during his stay in 2014 September. The early stages of the CFHTLenS project was made possible thanks to the support of the European Commission's Marie Curie Research Training Network DUEL (MRTN-CT-2006-036133) which directly supported six members of the CFHTLenS team (LF, HH, PS, BR, CB, MV) between 2007 and 2011 in addition to providing travel support and expenses for team meetings. BR +CH and HHo+ acknowledge support from the European Research Council under EC FP7 grant numbers 240672 (BR), 240185 (CH) and 279396 (HHo). HHi is supported by the DFG Emmy Noether grant Hi 1495/2-1. AF acknowledges support by INAF through VIPERS grants PRIN 2008 and PRIN 2010. MJH acknowledges support from the  Natural Sciences and Engineering Research Council of Canada (NSERC). Author Contributions: All authors contributed to the development and writing of this paper. The authorship list reflects the lead authors of this paper (JC, SA, LVW, TM, OI, EVU) followed by two alphabetical groups. The first alphabetical group includes key contributors to the science analysis and interpretation in this paper, the founding core team and those whose long-term significant effort produced the final CFHTLenS data product, and the VIPERS collaboration leaders. The second group covers authors in alphabetical order who made a significant contribution to either the projects, this paper, or both. The CFHTLenS collaboration was co-led by CH and LVW. | - |
dc.description.abstract | We present new constraints on the relationship between galaxies and their host dark matter haloes, measured from the location of the peak of the stellar-to-halo mass ratio (SHMR), up to the most massive galaxy clusters at redshift z ̃ 0.8 and over a volume of nearly 0.1 Gpc<SUP>3</SUP>. We use a unique combination of deep observations in the CFHTLenS/VIPERS field from the near-UV to the near-IR, supplemented by ̃60 000 secure spectroscopic redshifts, analysing galaxy clustering, galaxy-galaxy lensing and the stellar mass function. We interpret our measurements within the halo occupation distribution (HOD) framework, separating the contributions from central and satellite galaxies. We find that the SHMR for the central galaxies peaks at M_{h, peak} = 1.9^{+0.2}_{-0.1}× 10^{12} M_{☉} with an amplitude of 0.025, which decreases to ̃0.001 for massive haloes ({{{M}_h}}> 10^{14} M_{☉}). Compared to central galaxies only, the total SHMR (including satellites) is boosted by a factor of 10 in the high-mass regime (cluster-size haloes), a result consistent with cluster analyses from the literature based on fully independent methods. After properly accounting for differences in modelling, we have compared our results with a large number of results from the literature up to z = 1: we find good general agreement, independently of the method used, within the typical stellar-mass systematic errors at low to intermediate mass (M_{star}<10^{11} M_{☉}) and the statistical errors above. We have also compared our SHMR results to semi-analytic simulations and found that the SHMR is tilted compared to our measurements in such a way that they over- (under-) predict star formation efficiency in central (satellite) galaxies. | - |
dc.language.iso | eng | - |
dc.title | The galaxy-halo connection from a joint lensing, clustering and abundance analysis in the CFHTLenS/VIPERS field | - |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stv276 | en_US |
dc.identifier.scopus | 2-s2.0-84930651778 | en_US |
dc.identifier.isi | 000355337500017 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/449/2/1352/1067069 | - |
dc.relation.medium | STAMPA | - |
dc.relation.volume | 449 | - |
dc.relation.issue | 2 | - |
dc.relation.firstpage | 1352 | - |
dc.relation.lastpage | 1379 | - |
dc.type.referee | REF_1 | - |
dc.description.international | sì | - |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | - |
dc.relation.journal | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | - |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2015MNRAS.449.1352C | - |
dc.description.apc | no | - |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegherò il file al passo 5-Carica) | - |
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 | IASF Milano | - |
crisitem.author.dept | IASF Milano | - |
crisitem.author.dept | O.A. Trieste | - |
crisitem.author.orcid | 0000-0001-7455-8750 | - |
crisitem.author.orcid | 0000-0002-2282-5850 | - |
crisitem.author.orcid | 0000-0002-6220-9104 | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
È visualizzato nelle collezioni: | 1.01 Articoli in rivista |
File in questo documento:
File | Descrizione | Dimensioni | Formato | |
---|---|---|---|---|
stv276.pdf | pdf editoriale | 4.71 MB | Adobe PDF | Visualizza/apri |
Page view(s)
71
controllato il 2-mag-2024
Download(s)
19
controllato il 2-mag-2024
Google ScholarTM
Check
Altmetric
Altmetric
Tutti i documenti in DSpace sono pubblicati ad Accesso Aperto, salvo diversa indicazione per alcuni documenti specifici.