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Some of the first results are reported from RISE -a new fast camera mounted on the Liverpool Telescope primarily designed to obtain high time-resolution light curves of transiting extrasolar planets for the purpose of transit timing. A full and partial transit of WASP-3 are presented, and a Markov-Chain Monte Carlo analysis is used to update the parameters from the discovery paper. This results in a planetary radius of 1.29−0.12 R J and therefore a density of 0.82 +0.14 −0.09 ρ J , consistent with previous results. The inclination is 85.06 +0.16−0.15 deg, in agreement (but with a significant improvement in the precision) with the previously determined value. Central transit times are found to be consistent with the ephemeris given in the discovery paper; however, a new ephemeris calculated using the longer baseline results in T c (0) = 2 454 605.55915 ± 0.00023 HJD and P = 1.846835 ± 0.000002 days.

The outflowing proper motions of 15 knots in the dominant northwestern lobe of the high‐excitation poly‐polar planetary nebula NGC 6302 have been determined by comparing their positions relative to those of faint stars in an image taken at the San Pedro Martir Observatory in 2007 to those in a South African Astronomical Observatory archival plate obtained by Evans in 1956. The Hubble‐type expansion of this lobe is now directly confirmed in a model‐independent way from these measurements. Furthermore, an unambigous distance to NGC 6302 of 1.17 ± 0.14 kpc is now determined. Also, all the velocity vectors of the 15 knots (and two others) point back to the central source. An eruptive event from within the central torus ≈2200 yr previously must have created the high‐speed lobes of NGC 6302.