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Forecasting the in situ properties of coronal mass ejections (CMEs) fromremote images is expected to strongly enhance predictions of space weather, andis of general interest for studying the interaction of CMEs with planetaryenvironments. We study the feasibility of using a single heliospheric imager(HI) instrument, imaging the solar wind density from the Sun to 1 AU, forconnecting remote images to in situ observations of CMEs. We compare thepredictions of speed and arrival time for 22 CMEs (in 2008-2012) to thecorresponding interplanetary coronal mass ejection (ICME) parameters at in situobservatories (STEREO PLASTIC/IMPACT, Wind SWE/MFI). The list consists offront- and backsided, slow and fast CMEs (up to $2700 \: km \: s^{-1}$). Wetrack the CMEs to $34.9 \pm 7.1$ degrees elongation from the Sun with J-mapsconstructed using the SATPLOT tool, resulting in prediction lead times of$-26.4 \pm 15.3$ hours. The geometrical models we use assume different CMEfront shapes (Fixed-$\Phi$, Harmonic Mean, Self-Similar Expansion), andconstant CME speed and direction. We find no significant superiority in thepredictive capability of any of the three methods. The absolute differencebetween predicted and observed ICME arrival times is $8.1 \pm 6.3$ hours ($rms$value of 10.9h). Speeds are consistent to within $284 \pm 288 \: km \: s^{-1}$.Empirical corrections to the predictions enhance their performance for thearrival times to $6.1 \pm 5.0$ hours ($rms$ value of 7.9h), and for the speedsto $53 \pm 50 \: km \: s^{-1}$. These results are important for Solar Orbiterand a space weather mission positioned away from the Sun-Earth line.

Connecting speeds, directions and arrival times of 22 coronal mass ejections from the Sun to 1 AU