The paper ‘Towards a direct detection of warm gas in galactic haloes at cosmological distances’ was published in Mon. Not. R. Astron. Soc. 306, L15–L18 (1999). The wrong version of Fig. 1, from an early draft version of the paper, was inadvertently published. The correct version of Fig. 1 is reproduced here. Everything else in the paper (including the caption of Fig. 1) remains unaltered.
The function 
representing the signal-to-noise ratio predicted for a fiducial observing run with the following parameters: telescope diameter D = 8 m, spherical target of physical size l = 40h−1 kpc (which is characteristic for metal-line absorbing haloes of L* galaxies); average column density (similar to the lower limit for optical thickness at the Lyman limit) log NH i = 17.4 cm−2, velocity dispersion σ = 20 km s−1 and two cases for the kinetic temperature, T = 3×104 and 104 K. The solid curve represents F(z) for an Ω = 1 and the dotted curve represents F(z) for an Ω = 0.1 universe (everywhere h = 0.75). The dash-dotted lines represent (feasible) cases of fixed emission measures (for T = 3×104 K) in an Ω = 1 universe, given for comparison.
The function representing the signal-to-noise ratio predicted for a fiducial observing run with the following parameters: telescope diameter D = 8 m, spherical target of physical size l = 40h−1 kpc (which is characteristic for metal-line absorbing haloes of L* galaxies); average column density (similar to the lower limit for optical thickness at the Lyman limit) log NH i = 17.4 cm−2, velocity dispersion σ = 20 km s−1 and two cases for the kinetic temperature, T = 3×104 and 104 K. The solid curve represents F(z) for an Ω = 1 and the dotted curve represents F(z) for an Ω = 0.1 universe (everywhere h = 0.75). The dash-dotted lines represent (feasible) cases of fixed emission measures (for T = 3×104 K) in an Ω = 1 universe, given for comparison.
