http://arxiv.org/abs/1501.01818
In this letter, by using the type Ia supernovae (SNIa) to provide the luminosity distance (LD) directly, which is dependent on the value of the Hubble constant $H_0= 100 h\; {\rm km\; s^{-1}\; Mpc^{-1}}$, and the angular diameter distance from galaxy clusters or baryon acoustic oscillations (BAOs) to give the derived LD according to the distance duality relation, we propose a model-independent method to determine $h$ from the fact that different observations should give the same LD at a redshift. Combining the Union 2.1 SNIa and galaxy cluster data, we obtain that at the $1\sigma$ confidence level (CL) $h=0.589\pm0.030$ for the sample of the elliptical $\beta$ model for galaxy clusters, and $h=0.635\pm0.029$ for that of the spherical $\beta$ model. The former is smaller than the values from other observations, while the latter is consistent with the Planck result at the $1\sigma$ CL and agrees very well with the value reconstructed directly from the $H(z)$ data. With the Union 2.1 SNIa and BAO measurements, a tighter constraint: $h=0.681\pm0.014$, a $2\%$ determination, is obtained, which is very well consistent with the results from the Planck, the BAOs, as well as the local measurement from Cepheids and very low redshift SNIa.
P. Wu, Z. Li and H. Yu
Fri, 9 Jan 15
48/49
Comments: 11 pages, 3 figures
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