Probing cosmic opacity with the type Ia supernovae and Hubble parameter

Abstract

In this paper, we probe the cosmic opacity with the newest Pantheon type Ia supernovae (SNIa) and the observational Hubble parameter $$\left( H(z)\right) $$ H ( z ) data based on the $$\Lambda $$ Λ CDM and wCDM models with or without spatial curvature. In the analysis, we marginalize the likelihood function of SNIa data over the pertinent nuisance parameter $${\mathcal {M}}$$ M , a combination of the absolute magnitude of SNIa $$M_{\mathrm{B}}$$ M B and the Hubble constant $$H_0$$ H 0 , with a flat prior. Two parameterizations of the optical depth $$\tau (z)$$ τ ( z ) associated to the cosmic absorption, namely $$\tau (z)=2\varepsilon z$$ τ ( z ) = 2 ε z and $$\tau (z)= (1+z)^{2\varepsilon }-1$$ τ ( z ) = ( 1 + z ) 2 ε - 1 , are adopted. We find that the results are not sensitive to the fiducial cosmological models, the spatial curvature and parameterizations of $$\tau (z)$$ τ ( z ) . Moreover, the results from the Pantheon data alone are consistent with a transparent universe ($$\varepsilon =0$$ ε = 0 ). And once the H(z) data is combined, $$\varepsilon =0$$ ε = 0 falls within the 68% confidence level (CL) of the best fit when a flat $$H_0$$ H 0 prior or the distance priors are used, while it falls within the 95% CL when a Gaussian distribution prior of $$H_0=74.03\pm 1.42$$ H 0 = 74.03 ± 1.42 km $$\mathrm {s}^{-1}\, \mathrm {Mpc}^{-1}$$ s - 1 Mpc - 1 is used.

Exploring the potentiality of future standard candles and standard sirens to detect cosmic opacity *

“…(P1) and (P2). Assuming that dimming of SNe Ia is mainly caused by intergalactic opa- −0.0002±0.0014 ± 0.0028 ± 0.0041 −0.0002±0.0020 ± 0.0040 ± 0.0058 ET × 1048 Panthoen (B) [76] 0.004 ± 0.026 □ ET × 2000 simulated SNe Ia (B) [76] 0.0000 ± 0.0044 □ ET × 740 JLA (B) [77] 0.002 ± 0.035 −0.006 ± 0.053 ET × 1048 Panthoen (B) [77] 0.009 ± 0.016 0.015 ± 0.025 SL SNe Ia (LSST) × SNe Ia (B) [39] ∆ϵ = 0.027 ∆ϵ = 0.082 581 SNe Ia + 19 H(z) ΛCDM (A) [40] 0.02 ± 0.055 □ H(z) × Union (A) [8] −0.01± 0.08 0.09 □ H(z)× Union (A) [9] −0.04± 0.08 0.07 □ H(z) × Union2.1 (B) [36] −0.01 ± 0.10 −0.01 ± 0.12 Clusters × Union2.1 (B) [38] 0.009± 0.059 0.055 0.014± 0.071 0.069 H(z)× JLA (B) [37] 0.07± 0.107 0.121 □ ages of old objects × Union2.1 (B) [34] 0.016± 0.078 0.075…”

“…Thus far, some studies have been devoted to detecting cosmic opacity by adopting specific cosmological models and SNe Ia observations in a model-dependent way [3,8,9,32]. To probe cosmic opacity in a model-independent way, tests are generally performed using current SNe Ia observations, BAO measurements, Hubble data, galaxy cluster samples, old passive galaxies, the gas mass fraction of galaxy clusters, and strong gravitational lensing [33][34][35][36][37][38][39][40][41]. However, more recently, Vary uk and Kroupa pointed out that the applicability of the CDDR is strongly limited due to the non-unique interpretation of the LD data in terms of cosmic opacity and the rather low accuracy and deficient extent of the currently available ADD data [42].…”