Determining H 0 using a model-independent method

• Published in: Frontiers of physics Vol. 12; no. 1; p. 129801
• Main Authors: Wu, Pu-Xun, Li, Zheng-Xiang, Yu, Hong-Wei
• Format: Journal Article
• Language: English
• Published: Higher Education Press 01.02.2017
• Subjects: angular diameter distance; Hubble constant; luminosity distance
• ISSN: 2095-0462; 2095-0470
• DOI: 10.1007/s11467-016-0599-9

By using type Ia supernovae (SNIa) to provide the luminosity distance (LD) directly, which depends on the value of the Hubble constant H 0 = 100 h 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 σ confidence level (CL), h=0.5867±0.0303 for the sample of the elliptical β model for galaxy clusters, and h=0.6199±0.0293 for that of the sphericall β model. The former is smaller than the values from other observations, whereas the latter is consistent with the Planck result at the 2 σ 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.