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Chen, Y; Xu, LX; Chen, Y (reprint author), Chinese Acad Sci, Natl Astron Observ, Key Lab Computat Astrophys, Beijing 100012, Peoples R China.
Galaxy clustering, CMB and supernova data constraints on phi CDM model with massive neutrinos
Source PublicationPHYSICS LETTERS B
Language英语
AbstractWe investigate a scalar field dark energy model (i.e., phi CDM model) with massive neutrinos, where the scalar field possesses an inverse power-law potential, i.e., V(phi) alpha phi(-alpha) (alpha > 0). We find that the sum of neutrino masses Sigma m(nu) has significant impacts on the CMB temperature power spectrum and on the matter power spectrum. In addition, the parameter alpha also has slight impacts on the spectra. A joint sample, including CMB data from Planck 2013 and WMAP9, galaxy clustering data from WiggleZ and BOSS DR11, and JLA compilation of Type Ia supernova observations, is adopted to confine the parameters. Within the context of the phi CDM model under consideration, the joint sample determines the cosmological parameters to high precision: the angular size of the sound horizon at recombination, the Thomson scattering optical depth due to reionization, the physical densities of baryons and cold dark matter, and the scalar spectral index are estimated to be theta(*) = (1.0415(0.0011)(+0.0012)) x 10(-2), tau = 0.0914(0.0242)(+0.0266), Omega(b)h(2)= 0.0222 +/- 0.0005, Omega(c)h(2) = 0.1177 +/- 0.0036, and n(s) = 0.9644(-0.0119)(+0.0118), respectively, at 95% confidence level (CL). It turns out that alpha < 4.995 at 95% CL for the phi CDM model. And yet, the Lambda CDM scenario corresponding to alpha = 0 is not ruled out at 95% CL. Moreover, we get Sigma m(nu) < 0.262 eV at 95% CL for the phi CDM model, while the corresponding one for the Lambda CDM model is Sigma m(nu) < 0.293 eV. The allowed scale of Sigma m(nu) in the phi CDM model is a bit smaller than that in the Lambda CDM model. It is consistent with the qualitative analysis, which reveals that the increases of alpha and Sigma m(nu) both can result in the suppression of the matter power spectrum. As a consequence, when alpha is larger, in order to avoid suppressing the matter power spectrum too much, the value of Sigma m(nu) should be smaller. (C) 2015 The Authors. Published by Elsevier B.V.
2016
Volume752Pages:66-75
Subject AreaAstronomy & Astrophysics ; Physics
DOIhttp://dx.doi.org/10.1016/j.physletb.2015.11.022
Indexed BySCI
Funding OrganizationNational Natural Science Foundation of China [11133003, 11573031, 11275035] ; National Natural Science Foundation of China [11133003, 11573031, 11275035] ; National Natural Science Foundation of China [11133003, 11573031, 11275035] ; National Natural Science Foundation of China [11133003, 11573031, 11275035] ; Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences [XDB09000000] ; Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences [XDB09000000] ; Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences [XDB09000000] ; Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences [XDB09000000] ; China Postdoctoral Science Foundation [2015M571126] ; China Postdoctoral Science Foundation [2015M571126] ; China Postdoctoral Science Foundation [2015M571126] ; China Postdoctoral Science Foundation [2015M571126] ; Young Researcher Grant of National Astronomical Observatories, Chinese Academy of Sciences ; Young Researcher Grant of National Astronomical Observatories, Chinese Academy of Sciences ; Young Researcher Grant of National Astronomical Observatories, Chinese Academy of Sciences ; Young Researcher Grant of National Astronomical Observatories, Chinese Academy of Sciences ; Open Project Program of State Key Laboratory of Theoretical Physics, Institute of Theoretical Physics, Chinese Academy of Sciences [Y4KF101CJ1] ; Open Project Program of State Key Laboratory of Theoretical Physics, Institute of Theoretical Physics, Chinese Academy of Sciences [Y4KF101CJ1] ; Open Project Program of State Key Laboratory of Theoretical Physics, Institute of Theoretical Physics, Chinese Academy of Sciences [Y4KF101CJ1] ; Open Project Program of State Key Laboratory of Theoretical Physics, Institute of Theoretical Physics, Chinese Academy of Sciences [Y4KF101CJ1]
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Document Type期刊论文
Identifierhttp://ir.itp.ac.cn/handle/311006/21812
Collection理论物理所科研产出_SCI论文
Corresponding AuthorChen, Y (reprint author), Chinese Acad Sci, Natl Astron Observ, Key Lab Computat Astrophys, Beijing 100012, Peoples R China.
Recommended Citation
GB/T 7714
Chen, Y,Xu, LX,Chen, Y . Galaxy clustering, CMB and supernova data constraints on phi CDM model with massive neutrinos[J]. PHYSICS LETTERS B,2016,752:66-75.
APA Chen, Y,Xu, LX,&Chen, Y .(2016).Galaxy clustering, CMB and supernova data constraints on phi CDM model with massive neutrinos.PHYSICS LETTERS B,752,66-75.
MLA Chen, Y,et al."Galaxy clustering, CMB and supernova data constraints on phi CDM model with massive neutrinos".PHYSICS LETTERS B 752(2016):66-75.
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