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dc.contributor.authorWei, Jun-Jie
dc.contributor.authorWu, Xue-Feng
dc.contributor.authorMelia, Fulvio
dc.date.accessioned2017-03-03T00:09:29Z
dc.date.available2017-03-03T00:09:29Z
dc.date.issued2016-12-01
dc.identifier.citationThe H ii galaxy Hubble diagram strongly favours Rh = ct over ΛCDM 2016, 463 (2):1144 Monthly Notices of the Royal Astronomical Societyen
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.doi10.1093/mnras/stw2057
dc.identifier.urihttp://hdl.handle.net/10150/622740
dc.description.abstractWe continue to build support for the proposal to use H II galaxies (HIIGx) and giant extragalactic H II regions (GEHR) as standard candles to construct the Hubble diagram at redshifts beyond the current reach of Type Ia supernovae. Using a sample of 25 high-redshift HIIGx, 107 local HIIGx, and 24 GEHR, we confirm that the correlation between the emission -line luminosity and ionized -gas velocity dispersion is a viable luminosity indicator, and use it to test and compare the standard model Lambda CDM and the R-h = ct universe by optimizing the parameters in each cosmology using a maximization of the likelihood function. For the flat Lambda CDM model, the best fit is obtained with Omega(m) = 0.40(-0.09)(+0.09). However, statistical tools, such as the Akaike (AIC), Kullback (KIC) and Bayes (BIC) Information Criteria favour R-h = Ct over the standard model with a likelihood of approximate to 94.8-98.8 per cent versus only per cent. For wCDM (the version of ACDM with a dark -energy equation of state wde = Pde/Pde rather than was t WA = 1), a statistically acceptable fit is realized with Omega(m) = 0.221(-0.14)(+0.16) and wde = 0.511'0'21-5" which, however, are not fully consistent with their concordance values. In this case, wCDM has two more free parameters than R-h = Ct, and is penalized more heavily by these criteria. We find that R-h = Ct is strongly favoured over wCDM with a likelihood of approximate to 92.9-99.6 per cent versus only 0.4-7.1 per cent. The current HIIGx sample is already large enough for the BIC to rule out ACDM/wCDM in favour of R-h = Ct at a confidence level approaching 3 sigma.
dc.description.sponsorshipNational Basic Research Program ('973' Program) of China [2014CB845800, 2013CB834900]; National Natural Science Foundation of China [11322328, 11373068, 11603076]; Youth Innovation Promotion Association [2011231]; Strategic Priority Research Program 'The Emergence of Cosmological Structures' of the Chinese Academy of Sciences [XDB09000000]; Natural Science Foundation of Jiangsu Province [BK20161096]; Guangxi Key Laboratory for Relativistic Astrophysics; Amherst College; Chinese Academy of Sciences Visiting Professorships for Senior International Scientists [2012T1J0011]; Chinese State Administration of Foreign Experts Affairs [GDJ20120491013]en
dc.language.isoenen
dc.publisherOXFORD UNIV PRESSen
dc.relation.urlhttps://academic.oup.com/2016-08-17 00:00:00/article-lookup/doi/10.1093/mnras/stw2057en
dc.rights© 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Societyen
dc.subjectH II regionsen
dc.subjectgalaxies: generalen
dc.subjectcosmological parametersen
dc.subjectcosmology: observationsen
dc.subjectcosmology: theory - distance scaleen
dc.titleThe H II galaxy Hubble diagram strongly favours R-h = ct over Lambda CDMen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Dept Physen
dc.contributor.departmentUniv Arizona, Dept Astronen
dc.identifier.journalMonthly Notices of the Royal Astronomical Societyen
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-05-28T11:15:07Z
html.description.abstractWe continue to build support for the proposal to use H II galaxies (HIIGx) and giant extragalactic H II regions (GEHR) as standard candles to construct the Hubble diagram at redshifts beyond the current reach of Type Ia supernovae. Using a sample of 25 high-redshift HIIGx, 107 local HIIGx, and 24 GEHR, we confirm that the correlation between the emission -line luminosity and ionized -gas velocity dispersion is a viable luminosity indicator, and use it to test and compare the standard model Lambda CDM and the R-h = ct universe by optimizing the parameters in each cosmology using a maximization of the likelihood function. For the flat Lambda CDM model, the best fit is obtained with Omega(m) = 0.40(-0.09)(+0.09). However, statistical tools, such as the Akaike (AIC), Kullback (KIC) and Bayes (BIC) Information Criteria favour R-h = Ct over the standard model with a likelihood of approximate to 94.8-98.8 per cent versus only per cent. For wCDM (the version of ACDM with a dark -energy equation of state wde = Pde/Pde rather than was t WA = 1), a statistically acceptable fit is realized with Omega(m) = 0.221(-0.14)(+0.16) and wde = 0.511'0'21-5" which, however, are not fully consistent with their concordance values. In this case, wCDM has two more free parameters than R-h = Ct, and is penalized more heavily by these criteria. We find that R-h = Ct is strongly favoured over wCDM with a likelihood of approximate to 92.9-99.6 per cent versus only 0.4-7.1 per cent. The current HIIGx sample is already large enough for the BIC to rule out ACDM/wCDM in favour of R-h = Ct at a confidence level approaching 3 sigma.


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