Latest observational constraints on Cardassian models

Wang, TaiShan; Wu, Puxun

doi:10.1016/j.physletb.2009.06.002

Cited by 7 publications

(11 citation statements)

References 53 publications

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“…For instance, the Cosmic All-Sky Survey (CLASS) lensing sample have been used by Alcaniz, Dev & Jain (2005) to obtain the constraints q = 0.05 and n = −2.32 which are in tension with our SL fits. Wang & Wu (2009) estimated, using SNIa, BAO, CMB, Hubble parameter measurements and the gas mass fraction in galaxy clusters, q = 0.824 +0.750 −0.622 , and n = −0.091 +0.331 −1.908 which are in agreement with our confidence contours (see Figure 4). In addition, our limits are similar at 1σ to q = 0.480 +2.020 −0.080 , n = −0.600 +0.980 −0.450 computed by Feng & Li (2010) using the combination of SNIa (Constitution sample), BAO, and 5-yrs WMAP data.…”

Section: Idesupporting

confidence: 89%

A Magnified Glance Into the Dark Sector: Probing Cosmological Models With Strong Lensing in A1689

Magaña

Motta

Cárdenas

et al. 2015

ApJ

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In this paper we constrain four alternative models to the late cosmic acceleration in the Universe: Chevallier-Polarski-Linder (CPL), interacting dark energy (IDE), Ricci holographic dark energy (HDE), and modified polytropic Cardassian (MPC). Strong lensing (SL) images of background galaxies produced by the galaxy cluster Abell 1689 are used to test these models. To perform this analysis we modify the LENSTOOL lens modeling code. The value added by this probe is compared with other complementary probes: Type Ia supernovae (SNIa), baryon acoustic oscillations (BAO), and cosmic microwave background (CMB). We found that the CPL constraints obtained of the SL data are consistent with those estimated using the other probes. The IDE constraints are consistent with the complementary bounds only if large errors in the SL measurements are considered. The Ricci HDE and MPC constraints are weak but they are similar to the BAO, SNIa and CMB estimations. We also compute the figure-of-merit as a tool to quantify the goodness of fit of the data. Our results suggest that the SL method provides statistically significant constraints on the CPL parameters but weak for those of the other models. Finally, we show that the use of the SL measurements in galaxy clusters is a promising and powerful technique to constrain cosmological models. The advantage of this method is that cosmological parameters are estimated by modelling the SL features for each underlying cosmology. These estimations could be further improved by SL constraints coming from other galaxy clusters.

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Section: Idesupporting

confidence: 89%

A Magnified Glance Into the Dark Sector: Probing Cosmological Models With Strong Lensing in A1689

Magaña

Motta

Cárdenas

et al. 2015

ApJ

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“…The combined analysis gives Ω m = 0.248 +0.047 −0.013 , q = 1.098 +1.015 −0.465 and n = 0.014 +0.364 −0.946 , which is consistent with what given in Davis et al (2007) (see Fig. 4) and in Wang & Wu (2009) (Ω m = 0.271 +0.014 −0.015 , q = 0.824 +0.750 −0.622 , n = −0.091 +0.331 −1.908 ).…”

Section: Flat Modified Polytropic Cardassiansupporting

confidence: 87%

Testing Nonstandard Cosmological Models With Snls3 Supernova Data and Other Cosmological Probes

2011

ApJ

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We investigate the implications for some nonstandard cosmological models using data from the first three years of the Supernova Legacy Survey (SNLS3), assuming a spatially flat universe. A comparison between the constraints from the SNLS3 and those from other SN Ia samples, such as the ESSENCE, Union2, SDSS-II and Constitution samples, is given and the effects of different light-curve fitters are considered. We find that SN Ia with SALT2 or SALT or SIFTO can give consistent results and the tensions between different data sets and different lightcurve fitters are obvious for fewer-free-parameters models. At the same time, we also study the constraints from the SNLS3 along with data from the cosmic microwave background and the baryonic acoustic oscillations (CMB/BAO), and the latest Hubble parameter versus redshift (H(z)). Using model selection criteria such as χ 2 /dof, GoF, AIC and BIC, we find that, among all the cosmological models considered here (ΛCDM, constant w, varying w, DGP, modified polytropic Cardassian, and the generalized Chaplygin gas), the flat DGP is favored by the SNLS3 alone. However, when additional CMB/BAO or H(z) constraints are included, this is no longer the case, and the flat ΛCDM becomes preferred.

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“…On the other hand, Gaztañaga, Cabré & Hui (2009) determined other two Hubble parameter data at z = 0.24 and 0.43 from observations of BAO peaks. Cao et al (2011) used these newly observational H ( z ) data to constrain the interacting dark matter (IDM) scenario, and some other works for cosmological constraint can be found in Wang & Wu (2009), Gong et al (2010), Liang, Wu & Zhang (2010), Liang & Zhu (2011), Xu & Wang (2010) and Ma & Zhang (2011). For a recent review of the observational H ( z ) data, see e.g.…”

Section: Introductionmentioning

confidence: 99%

Testing the phenomenological interacting dark energy with observational H(z) data

Cao

Liang

Zhu

2011

Monthly Notices of the Royal Astronomical Society

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In order to test the possible interaction between dark energy and dark matter, we investigate observational constraints on a phenomenological scenario, in which the ratio between the dark energy and matter densities is proportional to the power‐law case of the scalefactor, r≡ (ρX/ρm) ∝aξ. By using the Markov chain Monte Carlo method, we constrain the phenomenological interacting dark energy model with the newly revised H(z) data, as well as the cosmic microwave background (CMB) observation from the 7‐year Wilkinson Microwave Anisotropy Probe (WMAP7) results, the baryonic acoustic oscillation (BAO) observation from the spectroscopic Sloan Digital Sky Survey (SDSS) Data Release 7 (DR7) galaxy sample and the Type Ia supernovae (SNe Ia) from the Union2 set. The best‐fitting values of the model parameters are Ωm0= 0.27+0.02−0.02 (1σ)+0.04−0.03 (2σ), ξ= 3.15+0.48−0.50(1σ)+0.72−0.71(2σ) and wX=−1.05+0.15−0.14(1σ)+0.21−0.21(2σ), which are more stringent than previous results. These results show that the standard Λ cold dark matter (ΛCDM) model without any interaction remains a good fit to the recent observational data; however, the interaction that the energy transferring from dark matter to dark energy is slightly favoured over the interaction from dark energy to dark matter. It is also shown that the H(z) data can give more stringent constraints on the phenomenological interacting scenario when combined with CMB and BAO observations, and the confidence regions of H(z)+BAO+CMB, SNe+BAO+CMB and H(z)+SNe+BAO+CMB combinations are consistent with each other.

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Latest observational constraints on Cardassian models

Abstract: PACS numbers: 98.80. Es, 95.35.+d, 98.80.Jk

Cited by 7 publications

References 53 publications

A Magnified Glance Into the Dark Sector: Probing Cosmological Models With Strong Lensing in A1689

A Magnified Glance Into the Dark Sector: Probing Cosmological Models With Strong Lensing in A1689

Testing Nonstandard Cosmological Models With Snls3 Supernova Data and Other Cosmological Probes

Testing the phenomenological interacting dark energy with observational H(z) data

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