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dc.contributor.authorZhao, Gong-Bo
dc.contributor.authorRaveri, Marco
dc.contributor.authorPogosian, Levon
dc.contributor.authorWang, Yuting
dc.contributor.authorCrittenden, Robert G.
dc.contributor.authorHandley, Will J.
dc.contributor.authorPercival, Will J.
dc.contributor.authorBeutler, Florian
dc.contributor.authorBrinkmann, Jonathan
dc.contributor.authorChuang, Chia-Hsun
dc.contributor.authorCuesta, Antonio J.
dc.contributor.authorEisenstein, Daniel J.
dc.contributor.authorKitaura, Francisco-Shu
dc.contributor.authorKoyama, Kazuya
dc.contributor.authorL'Huillier, Benjamin
dc.contributor.authorNichol, Robert C.
dc.contributor.authorPieri, Matthew M.
dc.contributor.authorRodriguez-Torres, Sergio
dc.contributor.authorRoss, Ashley J.
dc.contributor.authorRossi, Graziano
dc.contributor.authorSánchez, Ariel G.
dc.contributor.authorShafieloo, Arman
dc.contributor.authorTinker, Jeremy L.
dc.contributor.authorTojeiro, Rita
dc.contributor.authorVazquez, Jose A.
dc.contributor.authorZhang, Hanyu
dc.date.accessioned2018-03-01T00:33:14Z
dc.date.available2018-03-01T00:33:14Z
dc.date.issued2017-08-28
dc.identifier.citationZhao , G-B , Raveri , M , Pogosian , L , Wang , Y , Crittenden , R G , Handley , W J , Percival , W J , Beutler , F , Brinkmann , J , Chuang , C-H , Cuesta , A J , Eisenstein , D J , Kitaura , F-S , Koyama , K , L'Huillier , B , Nichol , R C , Pieri , M M , Rodriguez-Torres , S , Ross , A J , Rossi , G , Sánchez , A G , Shafieloo , A , Tinker , J L , Tojeiro , R , Vazquez , J A & Zhang , H 2017 , ' Dynamical dark energy in light of the latest observations ' Nature Astronomy , vol. 1 , pp. 627-632 . https://doi.org/10.1038/s41550-017-0216-zen
dc.identifier.issn2397-3366
dc.identifier.otherPURE: 251492284
dc.identifier.otherPURE UUID: fc6d3541-ddf8-4850-984c-45eceb705499
dc.identifier.otherBibCode: 2017NatAs...1..627Z
dc.identifier.otherScopus: 85033212942
dc.identifier.urihttp://hdl.handle.net/10023/12825
dc.description.abstractA flat Friedmann-Robertson-Walker universe dominated by a cosmological constant (Λ) and cold dark matter (CDM) has been the working model preferred by cosmologists since the discovery of cosmic acceleration1,2. However, tensions of various degrees ofsignificance are known to be present among existing datasets within the ΛCDM framework3-11. In particular, the Lyman-α forest measurement of the baryon acoustic oscillations (BAO) by the Baryon Oscillation Spectroscopic Survey3 prefers a smaller value of the matter density fraction ΩM than that preferred by cosmic microwave background (CMB). Also, the recently measured value of the Hubble constant, H0 = 73.24 ±1.74 km s-1 Mpc-1 (ref. 12), is 3.4σ higher than the 66.93 ± 0.62 km s-1Mpc-1 inferred from the Planck CMB data7. In this work, we investigate whether these tensions can be interpreted as evidence for a non-constant dynamical dark energy. Using the Kullback-Leibler divergence13 to quantify the tension between datasets, we find that the tensions are relieved by an evolving dark energy, with the dynamical dark energy model preferred at a 3.5σ significance level based on the improvement in the fit alone. While, at present, the Bayesian evidence for the dynamical dark energy is insufficient to favour it over ΛCDM, we show that, if the current best-fit dark energy happened to be the true model, it would be decisively detected by the upcoming Dark Energy Spectroscopic Instrument survey14.
dc.language.isoeng
dc.relation.ispartofNature Astronomyen
dc.rights© 2017, Macmillan Publishers Ltd, part of Springer Nature. This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1038/s41550-017-0216-zen
dc.subject3rd-DASen
dc.titleDynamical dark energy in light of the latest observationsen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1038/s41550-017-0216-z
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/1701.08165
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2017NatAs...1..627Z


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