Impacts of different SNLS3 light-curve fitters on cosmological consequences of interacting dark energy models

Hu, Yazhou; Li, Miao; Li, Nan; Wang, Shuang

doi:10.1051/0004-6361/201526946

Cited by 20 publications

(13 citation statements)

References 90 publications

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“…It should be mentioned that, previous studies on the SNLS3 datasetWang & Wang (2013a) and JLA datasetLi et al (2016) found strong evidence for the redshift-dependence of color-luminosity parameter β, and this conclusion has significant effects on parameter estimation of various cosmological models;;;;Wang, Wen & Li (2016). In addition, different light-curve fitters of SNIa can also affect the results of cosmologyfitsBengochea (2011); Mohlabeng & Ralston (2013);Hu et al (2016). But in this work, for simplicity, we just adopt the most mainstream recipe of processing SNLS3 data, and do not consider the factors of time-varying β and different light-curve fitters.…”

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confidence: 90%

A closer look at the cosmological implications of the ΛHDE model

Wang

Wen

Zhou

et al. 2017

Mon. Not. R. Astron. Soc.

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In a previous paper Hu et al. (2015), we proposed a heterotic dark energy model, called ΛHDE, in which dark energy is composed of two components: cosmological constant (CC) and holographic dark energy (HDE). The aim of this work is to give a more comprehensive and systematic investigation on the cosmological implications of the ΛHDE model. Firstly, we make use of the current observations to constrain the ΛHDE model, and compare its cosmology-fit results with the results of the ΛCDM and the HDE model. Then, by combining a qualitative theoretical analysis with a quantitative numerical study, we discuss the impact of considering curvature on the cosmic evolutions of fractional HDE density Ω hde and fractional CC density Ω Λ , as well as on the ultimate cosmic fate. Finally, we explore the effects of adopting different types of observational data. We find that: (1) the current observational data cannot distinguish the ΛHDE model from the ΛCDM and the HDE model; this indicates that DE may contain multiple components. (2) the asymptotic solution of Ω hde and the corresponding cosmic fate in a flat universe can be extended to the case of a non-flat universe; moreover, compared with the case of a flat universe, considering curvature will make HDE closer to a phantom dark energy. (3) compared with JLA dataset, SNLS3 data more favor a phantom type HDE; in contrast, using other types of observational data have no significant impact on the cosmic evolutions of the ΛHDE model.1 The original HDE model have the circular logic problem. In other words, the existence of the future event horizon needs the accelerating expansion, while the dark energy component that cause accelerating expansion is given by the future event horizon. Due to this problem, the original HDE model cannot be derived by the action principle. But in a paper of our group Li & Miao (2012), we have constructed a action, which can derive the energy density form of HDE from the first principle. This means that, although it seems that the original HDE model has the circular logic problem, this problem is not a real problem in the framework of HDE. c 0000 RAS arXiv:1605.04356v2 [astro-ph.CO]

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confidence: 90%

A closer look at the cosmological implications of the ΛHDE model

Wang

Wen

Zhou

et al. 2017

Mon. Not. R. Astron. Soc.

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“…The possible redshift-dependence of the intrinsic scatter σint[80], as well as different choice of SN light-curve fitters[81,82], may also cause the systematic uncertainties of SNIa.…”

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Holographic dark energy

2017

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We review the paradigm of holographic dark energy (HDE), which arises from a theoretical attempt of applying the holographic principle (HP) to the dark energy (DE) problem. Making use of the HP and the dimensional analysis, we derive the general formula of the energy density of HDE. Then, we describe the properties of HDE model, in which the future event horizon is chosen as the characteristic length scale. We also introduce the theoretical explorations and the observational constraints for this model. Next, in the framework of HDE, we discuss various topics, such as spatial curvature, neutrino, instability of perturbation, time-varying gravitational constant, inflation, black hole and big rip singularity. In addition, from both the theoretical and the observational aspects, we introduce the interacting holographic dark energy scenario, where the interaction between dark matter and HDE is taken into account. Furthermore, we discuss the HDE scenario in various modified gravity (MG) theories, such as Brans-Dicke theory, braneworld theory, scalar-tensor theory, Horava-Lifshitz theory, and so on. Besides, we introduce the attempts of reconstructing various scalar-field DE and MG models from HDE. Moreover, we introduce other DE models inspired by the HP, in which different characteristic length scales are chosen. Finally, we make comparisons among various HP-inspired DE models, by using cosmological observations and diagnostic tools.

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“…It should be mentioned that, the intrinsic scatter σ int also has the hint of redshift-dependence[35] that will significantly affect the results of cosmology-fits. In addition, different light-curve fitters of SN can also affect the results of parameter estimation[36,37]. But in this work, we do not consider these factors for simplicity.…”

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confidence: 99%

Cosmological implications of different baryon acoustic oscillation data

Wang¹,

Hu²,

Li³

2017

Sci. China Phys. Mech. Astron.

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In this work, we explore the cosmological implications of different baryon acoustic oscillation (BAO) data, including the BAO data extracted by using the spherically averaged one-dimensional galaxy clustering (GC) statistics (hereafter BAO1) and the BAO data obtained by using the anisotropic two-dimensional GC statistics (hereafter BAO2). To make a comparison, we also take into account the case without BAO data (hereafter NO BAO). Firstly, making use of these BAO data, as well as the SNLS3 type Ia supernovae sample and the Planck distance priors data, we give the cosmological constraints of the ΛCDM, the wCDM, and the Chevallier-Polarski-Linder (CPL) model. Then, we discuss the impacts of different BAO data on cosmological consquences, including its effects on parameter space, equation of state (EoS), figure of merit (FoM), decelerationacceleration transition redshift, Hubble parameter H(z), deceleration parameter q(z), statefinder hierarchy S 4 (z) and cosmic age t(z). We find that: (1) NO BAO data always give a smallest fractional matter density Ωm0, a largest fractional curvature density Ω k0 and a largest Hubble constant h; in contrast, BAO1 data always give a largest Ωm0, a smallest Ω k0 and a smallest h. (2) For the wCDM and the CPL model, NO BAO data always give a largest EoS w; in contrast, BAO2 data always give a smallest w. (3) Compared with the case of BAO1, BAO2 data always give a slightly larger FoM, and thus can give a cosmological constraint with a slightly better accuracy. (4) The impacts of different BAO data on the cosmic evolution and the comic age are very small, and can not be distinguished by using various dark energy diagnosis and the cosmic age data.PACS numbers: 98.80.Es, 95.36.+x

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Impacts of different SNLS3 light-curve fitters on cosmological consequences of interacting dark energy models

Cited by 20 publications

References 90 publications

A closer look at the cosmological implications of the ΛHDE model

A closer look at the cosmological implications of the ΛHDE model

Holographic dark energy

Cosmological implications of different baryon acoustic oscillation data

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