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Determining H0 using a model-independent method
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DOI：10.1007/s11467-016-0599-9.png)
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By using type Ia supernovae (SNIa) to provide the luminosity distance (LD) directly, which depends on the value of the Hubble constant H-0 = 100h 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 given redshift. Combining the Sloan Digital Sky Survey II (SDSS-II) SNIa from the MLCS2k2 light curve fit and galaxy cluster data, we find that at the 1 sigma confidence level (CL), h = 0.5867 +/- 0.0303 for the sample of the elliptical beta model for galaxy clusters, and h = 0.6199 +/- 0.0293 for that of the spherical beta model. The former is smaller than the values from other observations, whereas the latter is consistent with the Planck result at the 2 sigma CL and agrees very well with the value reconstructed directly from the H (z) data. With the SDSS-II SNIa and BAO measurements, a tighter constraint, h = 0.6683 +/- 0.0221, is obtained. For comparison, we also consider the Union 2.1 SNIa from the SALT2 light curve fitting. The results from the Union 2.1 SNIa are slightly larger than those from the SDSS-II SNIa, and the Union 2.1 SNIa + BAOs give the tightest value. We find that the values from SNIa + BAOs are quite consistent with those from the Planck and the BAOs, as well as the local measurement from Cepheids and very-low-redshift SNIa.
Keyword:
Hubble constant
luminosity distance
angular diameter distance
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