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Presently a ${>}3\sigma$ tension exists between values of the Hubble constant$H_0$ derived from analysis of fluctuations in the Cosmic Microwave Backgroundby Planck, and local measurements of the expansion using calibrators of type Iasupernovae (SNe Ia). We perform a blinded reanalysis of Riess et al. 2011 tomeasure $H_0$ from low-redshift SNe Ia, calibrated by Cepheid variables andgeometric distances including to NGC 4258. This paper is a demonstration oftechniques to be applied to the Riess et at. 2016 data. Our end-to-end analysisstarts from available CfA3 and LOSS photometry, providing an independentvalidation of Riess et al. 2011. We obscure the value of $H_0$ throughout ouranalysis and the first stage of the referee process, because calibration of SNeIa requires a series of often subtle choices, and the potential for results tobe affected by human bias is significant. Our analysis departs from that ofRiess et al. 2011 by incorporating the covariance matrix method adopted in SNLSand JLA to quantify SN Ia systematics, and by including a simultaneous fit ofall SN Ia and Cepheid data. We find $H_0 = 72.5 \pm 3.1$ (stat) $\pm 0.77$(sys) km s$^{-1}$ Mpc$^{-1}$ with a three-galaxy (NGC 4258+LMC+MW) anchor. Therelative uncertainties are 4.3% statistical, 1.1% systematic, and 4.4% total,larger than in Riess et al. 2011 (3.3% total) and the Efstathiou 2014reanalysis (3.4% total). Our error budget for $H_0$ is dominated by statisticalerrors due to the small size of the supernova sample, whilst the systematiccontribution is dominated by variation in the Cepheid fits, and for the SNe Ia,uncertainties in the host galaxy mass dependence and Malmquist bias.

A blinded determination of $H_0$ from low-redshift Type Ia supernovae, calibrated by Cepheid variables