{"status":"ok","message-type":"work","message-version":"1.0.0","message":{"indexed":{"date-parts":[[2026,10,10]],"date-time":"2026-10-10T04:57:14Z","timestamp":1791608234822,"version":"4.3.4"},"reference-count":120,"publisher":"MDPI AG","issue":"9","license":[{"start":{"date-parts":[[2025,8,24]],"date-time":"2025-08-24T00:00:00Z","timestamp":1755993600000},"content-version":"vor","delay-in-days":0,"URL":"https:\/\/creativecommons.org\/licenses\/by\/4.0\/"}],"content-domain":{"domain":[],"crossmark-restriction":false},"short-container-title":["Entropy"],"abstract":"<jats:p>We analyze two different scenarios for the late universe dynamics, resulting in Hubble parameters deviating from the \u039bCDM, mainly for the presence of an additional free parameter, which is the dark energy parameter. The first model consists of a pure evolutionary dark energy paradigm as a result of its creation by the gravitational field of the expanding universe. The second model also considers an interaction of the evolutionary dark energy with the matter component, postulated via the conservation of the sum of their ideal energy\u2013momentum tensors. These two models are then compared via the diagnostic tool of the effective running Hubble constant, with the binned data of the so-called \u201cMaster sample\u201d for the Type Ia Supernovae. The comparison procedures, based on a standard MCMC analysis, lead to a clear preference of data for the dark energy\u2013matter interaction model, which is associated with a phantom matter equation of state parameter (very close to \u22121) when, being left free by data (it has a flat posterior), it is fixed in order to reproduce the decreasing power-law behavior of the effective running Hubble constant, already discussed in the literature.<\/jats:p>","DOI":"10.3390\/e27090895","type":"journal-article","created":{"date-parts":[[2025,8,25]],"date-time":"2025-08-25T00:10:36Z","timestamp":1756080636000},"page":"895","update-policy":"https:\/\/doi.org\/10.3390\/mdpi_crossmark_policy","source":"Crossref","is-referenced-by-count":15,"title":["Two Dynamical Scenarios for Binned Master Sample Interpretation"],"prefix":"10.3390","volume":"27","author":[{"ORCID":"https:\/\/orcid.org\/0000-0002-2550-5553","authenticated-orcid":false,"given":"Giovanni","family":"Montani","sequence":"first","affiliation":[{"name":"Nuclear Department, ENEA, C.R. Frascati, Via E. Fermi 45, 00044 Frascati, Italy"},{"name":"Physics Department, \u201cSapienza\u201d University of Rome, P.le A. Moro 5, 00185 Roma, Italy"}],"role":[{"vocabulary":"crossref","role":"author"}]},{"ORCID":"https:\/\/orcid.org\/0009-0005-0594-4128","authenticated-orcid":false,"given":"Elisa","family":"Fazzari","sequence":"additional","affiliation":[{"name":"Physics Department, \u201cSapienza\u201d University of Rome, P.le A. Moro 5, 00185 Roma, Italy"},{"name":"Istituto Nazionale di Fisica Nucleare (INFN), Sezione di Roma, P.le A. Moro 5, 00185 Roma, Italy"},{"name":"Physics Department, Tor Vergata University of Rome, Via della Ricerca Scientifica 1, 00133 Roma, Italy"}],"role":[{"vocabulary":"crossref","role":"author"}]},{"ORCID":"https:\/\/orcid.org\/0000-0003-3811-2545","authenticated-orcid":false,"given":"Nakia","family":"Carlevaro","sequence":"additional","affiliation":[{"name":"Nuclear Department, ENEA, C.R. Frascati, Via E. Fermi 45, 00044 Frascati, Italy"}],"role":[{"vocabulary":"crossref","role":"author"}]},{"ORCID":"https:\/\/orcid.org\/0000-0003-4442-8546","authenticated-orcid":false,"given":"Maria Giovanna","family":"Dainotti","sequence":"additional","affiliation":[{"name":"Division of Science, National Astronomical Observatory of Japan, 2-21-1, Mitaka 181-8588, Tokyo, Japan"},{"name":"Astronomy Department, The Graduate University for Advanced Studies (SOKENDAI), Shonankokusaimura, Hayama, Miura 240-0115, Kanagawa, Japan"},{"name":"Space Science Institutes, 4765 Walnut St Ste B, Boulder, CO 80301, USA"}],"role":[{"vocabulary":"crossref","role":"author"}]}],"member":"1968","published-online":{"date-parts":[[2025,8,24]]},"reference":[{"key":"ref_1","doi-asserted-by":"crossref","first-page":"955","DOI":"10.1038\/35010035","article-title":"A flat Universe from high-resolution maps of the cosmic microwave background radiation","volume":"404","author":"Ade","year":"2000","journal-title":"Nature"},{"key":"ref_2","doi-asserted-by":"crossref","first-page":"20","DOI":"10.1088\/0067-0049\/208\/2\/20","article-title":"Nine-year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Final Maps and Results","volume":"208","author":"Bennett","year":"2013","journal-title":"Astrophys. 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