Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/30417
DC Field | Value | Language |
---|---|---|
dc.contributor.author | GIOCOLI, CARLO | en_US |
dc.contributor.author | MOSCARDINI, LAURO | en_US |
dc.contributor.author | BALDI, MARCO | en_US |
dc.contributor.author | MENEGHETTI, MASSIMO | en_US |
dc.contributor.author | Metcalf, Robert B. | en_US |
dc.date.accessioned | 2021-02-16T16:49:24Z | - |
dc.date.available | 2021-02-16T16:49:24Z | - |
dc.date.issued | 2018 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/30417 | - |
dc.description.abstract | In this paper, we study the statistical properties of weak-lensing peaks in light cones generated from cosmological simulations. In order to assess the prospects of such observable as a cosmological probe, we consider simulations that include interacting Dark Energy (hereafter DE) models with coupling term between DE and Dark Matter. Cosmological models that produce a larger population of massive clusters have more numerous high signal-to-noise peaks; among models with comparable numbers of clusters those with more concentrated haloes produce more peaks. The most extreme model under investigation shows a difference in peak counts of about 20 per cent with respect to the reference Λ cold dark matter model. We find that peak statistics can be used to distinguish a coupling DE model from a reference one with the same power spectrum normalization. The differences in the expansion history and the growth rate of structure formation are reflected in their halo counts, non-linear scale features and, through them, in the properties of the lensing peaks. For a source redshift distribution consistent with the expectations of future space-based wide field surveys, we find that typically 70 per cent of the cluster population contributes to weak-lensing peaks with signal-to-noise ratios larger than 2, and that the fraction of clusters in peaks approaches 100 per cent for haloes with redshift z ⩽ 0.5. Our analysis demonstrates that peak statistics are an important tool for disentangling DE models by accurately tracing the structure formation processes as a function of the cosmic time. | en_US |
dc.language.iso | eng | en_US |
dc.title | Weak-lensing peaks in simulated light cones: investigating the coupling between dark matter and dark energy | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/sty1312 | en_US |
dc.identifier.scopus | 2-s2.0-85050800210 | en_US |
dc.identifier.isi | 000441288300084 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/478/4/5436/4999637 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 478 | en_US |
dc.relation.issue | 4 | en_US |
dc.relation.firstpage | 5436 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | 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 | 2018MNRAS.478.5436G | 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 | OAS Bologna | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.orcid | 0000-0002-9590-7961 | - |
crisitem.author.orcid | 0000-0003-1225-7084 | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
1801.01886.pdf | preprint | 4.13 MB | Adobe PDF | View/Open |
sty1312.pdf | Pdf editoriale | 6.9 MB | Adobe PDF | View/Open |
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