arXiv subjects

Gong-Bo Zhao

Publications and source records attributed to Gong-Bo Zhao.

189 records · Page 11Linked to original sources

arXiv2006

Probing for dynamics of dark energy and curvature of universe with latest cosmological observations

We use the newly released 182 Type Ia supernova data combined with the third-year Wilkinson Microwave Anisotropic Probe data (WMAP3) and large scale structure (LSS) information including SDSS and 2dFGRS to constrain the dark energy equation of state (EoS) as well as the curvature of universe $Ω_K$. Using the full dataset of Cosmic Microwave Background (CMB) and LSS rather than the shift parameter and linear growth factor, we make a Markov Chain Monte Carlo (MCMC) global fit, while paying particular attention to the dark energy perturbation. Parameterizing the EoS as $w_{DE}(a) = w_{0} + w_{1}(1-a)$, we find the best fit of ($w_0,w_1$) is ($-1.053,0.944$) and for $w_{DE}(a) = w_{0} + w_{1}\sin({3/2}π\ln(a))$, the best fit for ($w_0,w_1$) is ($-1.614,-1.046$). We find that a flat universe is a good approximation, namely, $|Ω_K|>0.06$ has been excluded by 2$σ$ yet the inclusion of $Ω_K$ can affect the measurement of DE parameters owing to their correlation and the present systematic effects of SNIa measurements.

astro-ph↗

arXiv2006

Weighing neutrinos in the presence of a running primordial spectral index

The three-year WMAP(WMAP3), combined with other cosmological observations from galaxy clustering and Type Ia Supernova (SNIa), prefers a non-vanishing running of the primordial spectral index independent of the low CMB multipoles. Motivated by this feature we study cosmological constraint on the neutrino mass, which severely depends on what prior we adopt for the spectral shape of primordial fluctuations, taking possible running into account. As a result we find a more stringent constraint on the sum of the three neutrino masses, m_ν< 0.76eV (2 σ), compared with m_ν< 0.90eV (2 σ) for the case where power-law prior is adopted to the primordial spectral shape.

astro-ph↗

arXiv2006

Detecting the ambient neutralino dark matter particles at accelerator

In this work, we present a new strategy to investigate the possibility of direct detection of the ambient neutralino matter at accelerator. We calculate the cross sections for both elastic and inelastic scattering processes of the dark matter particles with the beam particles at $e^+e^-$ and hadron colliders.

hep-ph↗

arXiv2006

Features in Dark Energy Equation of State and Modulations in the Hubble Diagram

We probe the time dependence of the dark energy equation of state (EOS) in light of three-year WMAP (WMAP3) and the combination with other tentative cosmological observations from galaxy clustering (SDSS) and Type Ia Supernova (SNIa). We mainly focus on cases where the EOS is oscillating or with local bumps. By performing a global analysis with the Markov Chain Monte Carlo (MCMC) method, we find the current observations, in particular the WMAP3 + SDSS data combination, allow large oscillations of the EOS which can leave oscillating features on the (residual) Hubble diagram, and such oscillations are potentially detectable by future observations like SNAP, or even by the CURRENTLY ONGOING SNIa observations. Local bumps of dark energy EOS can also leave imprints on CMB, LSS and SNIa. In cases where the bumps take place at low redshifts and the effective EOS are close to -1, CMB and LSS observations cannot give constraints on such possibilities. However, geometrical observations like (future) SNIa can possibly detect such features. On the other hand when the local bumps take place at higher redshifts beyond the detectability of SNIa, future precise observations like Gamma-ray bursts, CMB and LSS may possibly detect such features. In particular, we find that bump-like dark energy EOS on high redshifts might be responsible for the features of WMAP on ranges l \sim 30-50, which is interesting and deserves addressing further.

astro-ph↗

arXiv2006

Probing Inflation and Dark Energy with Current Cosmological Observations

It is commonly believed that our Universe has experienced two different stages of accelerated expansion. The early stage is known as inflation and the current acceleration is driven by dark energy. Observing inflation and dark energy dynamics are among the most important aspects of the current cosmological research. In this paper we make a first detailed probe of possible degeneracies between dynamical inflation and dark energy in light of current cosmological observations. We find the inclusion of inflation and dark energy parameters together make the parameter spaces broader, but interestingly deviation from scale-invariant primordial spectrum is sightly more favored by current cosmological observations when one marginalizes over dynamical dark energy models.

astro-ph↗

arXiv2006

Probing Dynamics of Dark Energy with Supernova, Galaxy Clustering and the Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations

Using the Markov chain Monte Carlo (MCMC) method we perform a global analysis constraining the dynamics of dark energy in light of the supernova (Riess "Gold" samples), galaxy clustering (SDSS 3D power spectra and SDSS lyman-αforest information) and the latest three-year Wilkinson Microwave Anisotropy Probe (WMAP) observations. We have allowed the dark energy equation of state to get across -1 and pay particular attention to the effects when incorrectly neglecting dark energy perturbations. We find the parameter space of dynamical dark energy is now well constrained and neglecting dark energy perturbations will make the parameter space significantly smaller. Dynamical dark energy model where the equation of state crosses -1 is mildly favored and the standard \LambdaCDM model is still a good fit to the current data.

astro-ph↗

arXiv2005

Observing Dark Energy Dynamics with Supernova, Microwave Background and Galaxy Clustering

Observing dark energy dynamics is the most important aspect of the dark energy research. In this paper we perform an analysis of the constraints on the property of dark energy from the current astronomical observations. We pay particular attention to the effects of dark energy perturbations. Using the data from SNIa (157 "gold" sample), WMAP and SDSS we find that the best fitting dark energy model is given by the dynamical model with the equation of state across -1. Nevertheless the standard \LambdaCDM models are still a very good fit to the current data and evidence for dynamics is currently not very strong. We also consider the constraints from SNLS.

astro-ph↗

arXiv2005

Perturbations of the Quintom Models of Dark Energy and the Effects on Observations

We study in this paper the perturbations of the quintom dark energy model and the effects of quintom perturbations on the current observations. Quintom describes a scenario of dark energy where the equation of state gets across the cosmological constant boundary $w = -1$ during evolution. We present a new method to show that the conventional dark energy models based on single k-essence field and perfect fluid cannot act as quintom due to the singularities and classical instabilities of perturbations around $w = -1$. One needs to add extra degrees of freedom for successful quintom model buildings. There are no singularities or classical instabilities in perturbations of realistic quintom models and they are potentially distinguishable from the cosmological constant. Basing on the realistic quintom models in this paper we provide one way to include the perturbations for dark energy models with parametrized equation of state across -1. Compare with those assuming no dark energy perturbations, we find that the parameter space which allows the equation of state to get across -1 will be enlarged in general when including the perturbations.

astro-ph↗

arXiv2001

Applicability of the Friedberg-Lee-Zhao method

Friedberg, Lee and Zhao proposed a method for effectively evaluating the eigenenergies and eigen wavefunctions of quantum systems. In this work, we study several special cases to investigate applicability of the method. Concretely, we calculate the ground-state eigenenergy of the Hellmann potential as well as the Cornell potential, and also evaluate the energies of the systems where linear term is added to the Coulomb and harmonic oscillator potentials as a perturbation. The results obtained in this method have a surprising agreement with the traditional method or the numerical results. Since the results in this method have obvious analyticity compared to that in other methods, and because of the simplicity for calculations this method can be applied to solving the Schrödinger equation and provides us better understanding of the physical essence of the concerned systems. But meanwhile applications of the FLZ method are restricted at present, especially for certain potential forms, but due to its obvious advantages, it should be further developed.

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