Show simple item record

dc.contributor.authorGeng, Chao-Qiang
dc.contributor.authorLee, Chung-Chi
dc.contributor.authorYin, Lu
dc.date.accessioned2021-01-28T16:13:49Z
dc.date.available2021-01-28T16:13:49Z
dc.date.issued2020-01
dc.date.submitted2019-06-12
dc.identifier.issn1434-6044
dc.identifier.others10052-020-7653-z
dc.identifier.other7653
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/316822
dc.descriptionFunder: 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>$$\alpha &gt;0$$</jats:tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mi>α</mml:mi><mml:mo>&gt;</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>$$\alpha &lt;2.83\times 10^{-4}$$</jats:tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mi>α</mml:mi><mml:mo>&lt;</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.languageen
dc.publisherSpringer Science and Business Media LLC
dc.rightsAttribution 4.0 International (CC BY 4.0)
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/
dc.subjectRegular Article - Theoretical Physics
dc.titleConstraints on a special running vacuum model
dc.typeArticle
dc.date.updated2021-01-28T16:13:49Z
prism.issueIdentifier1
prism.publicationNameThe European Physical Journal C
prism.volume80
dc.identifier.doi10.17863/CAM.63937
dcterms.dateAccepted2020-01-14
rioxxterms.versionofrecord10.1140/epjc/s10052-020-7653-z
rioxxterms.versionVoR
rioxxterms.licenseref.urihttp://creativecommons.org/licenses/by/4.0/
dc.identifier.eissn1434-6052
pubs.funder-project-idMinistry of Science and Technology, Taiwan (MoST-104-2112-M-007-003-MY3 and MoST-107-2119-M-00)
cam.issuedOnline2020-01-29


Files in this item

Thumbnail
Thumbnail

This item appears in the following Collection(s)

Show simple item record

Attribution 4.0 International (CC BY 4.0)
Except where otherwise noted, this item's licence is described as Attribution 4.0 International (CC BY 4.0)