Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/31862
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Muccino, M. | en_US |
dc.contributor.author | Izzo, L. | en_US |
dc.contributor.author | Luongo, O. | en_US |
dc.contributor.author | Boshkayev, K. | en_US |
dc.contributor.author | AMATI, LORENZO | en_US |
dc.contributor.author | DELLA VALLE, Massimo | en_US |
dc.contributor.author | Pisani, G. B. | en_US |
dc.contributor.author | Zaninoni, E. | en_US |
dc.date.accessioned | 2022-03-24T11:45:09Z | - |
dc.date.available | 2022-03-24T11:45:09Z | - |
dc.date.issued | 2021 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/31862 | - |
dc.description.abstract | Observations of gamma-ray bursts up to z ∼ 9 are best suited to study the possible evolution of the universe equation of state at intermediate redshifts. We apply the Combo relation to a sample of 174 gamma-ray bursts to investigate possible evidence of evolving dark energy parameter w(z). We first build a gamma-ray burst Hubble's diagram and then we estimate the set (Ω<SUB>m</SUB>, Ω<SUB>Λ</SUB>) in the framework of flat and non-flat ΛCDM paradigm. We then get bounds over the wCDM model, where w is thought to evolve with redshift, adopting two priors over the Hubble constant in tension at 4.4σ, i.e., H<SUB>0</SUB> = (67.4 ± 0.5) km s<SUP>-1</SUP> Mpc<SUP>-1</SUP> and H<SUB>0</SUB> = (74.03 ± 1.42) km s<SUP>-1</SUP> Mpc<SUP>-1</SUP>. We show our new sample provides tighter constraints on Ω<SUB>m</SUB> since at z ≤ 1.2 we see that w(z) agrees within 1σ with the standard value w = -1. The situation is the opposite at larger z, where gamma-ray bursts better fix w(z) that seems to deviate from w = -1 at 2σ and 4σ level, depending on the redshift bins. In particular, we investigate the w(z) evolution through a piecewise formulation over seven redshift intervals. From our fitting procedure we show that at z ≥ 1.2 the case w < -1 cannot be fully excluded, indicating that dark energy's influence is not negligible at larger z. We confirm the Combo relation as a powerful tool to investigate cosmological evolution of dark energy. Future space missions will significantly enrich the gamma-ray burst database even at smaller redshifts, improving de facto the results discussed in this paper. | en_US |
dc.language.iso | eng | en_US |
dc.title | Tracing Dark Energy History with Gamma-Ray Bursts | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/1538-4357/abd254 | en_US |
dc.identifier.scopus | 2-s2.0-85102711012 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/1538-4357/abd254 | en_US |
dc.identifier.url | https://api.elsevier.com/content/abstract/scopus_id/85102711012 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 908 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 181 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | 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 | - |
dc.identifier.adsbibcode | 2021ApJ...908..181M | 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 | O.A. Capodimonte | - |
crisitem.author.orcid | 0000-0001-5355-7388 | - |
crisitem.author.orcid | 0000-0003-3142-5020 | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
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File | Descrizione | Dimensioni | Formato | |
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2012.03392.pdf | preprint | 1.74 MB | Adobe PDF | Visualizza/apri |
Muccino_2021_ApJ_908_181.pdf | [Administrators only] | 1.07 MB | Adobe PDF |
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