Fig. 7: Posterior distributions for H0 for individual events without GW170817. | Nature Communications

Fig. 7: Posterior distributions for H0 for individual events without GW170817.

From: Measuring the Hubble constant with a sample of kilonovae

Fig. 7: Posterior distributions for H0 for individual events without GW170817.The alternative text for this image may have been generated using AI.

We show them for GRB 060614, GRB 150101B, GRB 160821B, GRB 050709, and their combined posteriors are also shown. Fig. a is the Kasen24 model with 0.1 mag errors, b is the Bulla25 model with 0.1 mag errors, c is is the Kasen model with 0.25 mag errors, and d is is the Bulla model with 0.25 mag errors. The 1- and 2-σ regions determined by the superluminal motion measurement from the radio counterpart (blue)16, Planck CMB (TT,TE,EE+lowP+lensing) (green)34 and SHoES Cepheid-SN distance ladder surveys (orange)5 are also depicted as vertical bands.

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