Constraints on a special running vacuum model
dc.contributor.author | Geng, Chao-Qiang | |
dc.contributor.author | Lee, Chung-Chi | |
dc.contributor.author | Yin, Lu | |
dc.date.accessioned | 2021-01-28T16:13:49Z | |
dc.date.available | 2021-01-28T16:13:49Z | |
dc.date.issued | 2020-01 | |
dc.date.submitted | 2019-06-12 | |
dc.identifier.issn | 1434-6044 | |
dc.identifier.other | s10052-020-7653-z | |
dc.identifier.other | 7653 | |
dc.identifier.uri | https://www.repository.cam.ac.uk/handle/1810/316822 | |
dc.description | Funder: Physics Division, National Center for Theoretical Sciences; doi: http://dx.doi.org/10.13039/100009638 | |
dc.description.abstract | <jats:title>Abstract</jats:title><jats:p>We study a special running vacuum model (RVM) with <jats:inline-formula><jats:alternatives><jats:tex-math>$$\Lambda = 3 \alpha H^2+3\beta H_0^4 H^{-2}+\Lambda _0$$</jats:tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mi>Λ</mml:mi><mml:mo>=</mml:mo><mml:mn>3</mml:mn><mml:mi>α</mml:mi><mml:msup><mml:mi>H</mml:mi><mml:mn>2</mml:mn></mml:msup><mml:mo>+</mml:mo><mml:mn>3</mml:mn><mml:mi>β</mml:mi><mml:msubsup><mml:mi>H</mml:mi><mml:mn>0</mml:mn><mml:mn>4</mml:mn></mml:msubsup><mml:msup><mml:mi>H</mml:mi><mml:mrow><mml:mo>-</mml:mo><mml:mn>2</mml:mn></mml:mrow></mml:msup><mml:mo>+</mml:mo><mml:msub><mml:mi>Λ</mml:mi><mml:mn>0</mml:mn></mml:msub></mml:mrow></mml:math></jats:alternatives></jats:inline-formula>, where <jats:inline-formula><jats:alternatives><jats:tex-math>$$\alpha $$</jats:tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mi>α</mml:mi></mml:math></jats:alternatives></jats:inline-formula>, <jats:inline-formula><jats:alternatives><jats:tex-math>$$\beta $$</jats:tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mi>β</mml:mi></mml:math></jats:alternatives></jats:inline-formula> and <jats:inline-formula><jats:alternatives><jats:tex-math>$$\Lambda _0$$</jats:tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:msub><mml:mi>Λ</mml:mi><mml:mn>0</mml:mn></mml:msub></mml:math></jats:alternatives></jats:inline-formula> are the model parameters and <jats:italic>H</jats:italic> is the Hubble one. This RVM has non-analytic background solutions for the energy densities of matter and radiation, which can only be evaluated numerically. From the analysis of the CMB power spectrum and baryon acoustic oscillation along with the prior of <jats:inline-formula><jats:alternatives><jats:tex-math>$$\alpha >0$$</jats:tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mi>α</mml:mi><mml:mo>></mml:mo><mml:mn>0</mml:mn></mml:mrow></mml:math></jats:alternatives></jats:inline-formula> to avoid having a negative dark energy density, we find that <jats:inline-formula><jats:alternatives><jats:tex-math>$$\alpha <2.83\times 10^{-4}$$</jats:tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mi>α</mml:mi><mml:mo><</mml:mo><mml:mn>2.83</mml:mn><mml:mo>×</mml:mo><mml:msup><mml:mn>10</mml:mn><mml:mrow><mml:mo>-</mml:mo><mml:mn>4</mml:mn></mml:mrow></mml:msup></mml:mrow></mml:math></jats:alternatives></jats:inline-formula> and <jats:inline-formula><jats:alternatives><jats:tex-math>$$\beta =(-0.2^{+3.9}_{-4.5})\times 10^{-4}$$</jats:tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mi>β</mml:mi><mml:mo>=</mml:mo><mml:mrow><mml:mo>(</mml:mo><mml:mo>-</mml:mo><mml:mn>0</mml:mn><mml:mo>.</mml:mo><mml:msubsup><mml:mn>2</mml:mn><mml:mrow><mml:mo>-</mml:mo><mml:mn>4.5</mml:mn></mml:mrow><mml:mrow><mml:mo>+</mml:mo><mml:mn>3.9</mml:mn></mml:mrow></mml:msubsup><mml:mo>)</mml:mo></mml:mrow><mml:mo>×</mml:mo><mml:msup><mml:mn>10</mml:mn><mml:mrow><mml:mo>-</mml:mo><mml:mn>4</mml:mn></mml:mrow></mml:msup></mml:mrow></mml:math></jats:alternatives></jats:inline-formula> (95<jats:inline-formula><jats:alternatives><jats:tex-math>$$\%$$</jats:tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mo>%</mml:mo></mml:math></jats:alternatives></jats:inline-formula> C.L.). We show that the RVM fits the cosmological data comparably to the <jats:inline-formula><jats:alternatives><jats:tex-math>$$\Lambda \hbox {CDM}$$</jats:tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mi>Λ</mml:mi><mml:mtext>CDM</mml:mtext></mml:mrow></mml:math></jats:alternatives></jats:inline-formula>. In addition, we relate the fluctuation amplitude <jats:inline-formula><jats:alternatives><jats:tex-math>$$\sigma _8$$</jats:tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:msub><mml:mi>σ</mml:mi><mml:mn>8</mml:mn></mml:msub></mml:math></jats:alternatives></jats:inline-formula> to the neutrino mass sum <jats:inline-formula><jats:alternatives><jats:tex-math>$$\Sigma m_\nu $$</jats:tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mi>Σ</mml:mi><mml:msub><mml:mi>m</mml:mi><mml:mi>ν</mml:mi></mml:msub></mml:mrow></mml:math></jats:alternatives></jats:inline-formula>.</jats:p> | |
dc.language | en | |
dc.publisher | Springer Science and Business Media LLC | |
dc.rights | Attribution 4.0 International (CC BY 4.0) | |
dc.rights.uri | https://creativecommons.org/licenses/by/4.0/ | |
dc.subject | Regular Article - Theoretical Physics | |
dc.title | Constraints on a special running vacuum model | |
dc.type | Article | |
dc.date.updated | 2021-01-28T16:13:49Z | |
prism.issueIdentifier | 1 | |
prism.publicationName | The European Physical Journal C | |
prism.volume | 80 | |
dc.identifier.doi | 10.17863/CAM.63937 | |
dcterms.dateAccepted | 2020-01-14 | |
rioxxterms.versionofrecord | 10.1140/epjc/s10052-020-7653-z | |
rioxxterms.version | VoR | |
rioxxterms.licenseref.uri | http://creativecommons.org/licenses/by/4.0/ | |
dc.identifier.eissn | 1434-6052 | |
pubs.funder-project-id | Ministry of Science and Technology, Taiwan (MoST-104-2112-M-007-003-MY3 and MoST-107-2119-M-00) | |
cam.issuedOnline | 2020-01-29 |
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