in the cluster as an explanation; they found both very fast and slow rotators among the X-ray selected members. A further possibility is that the energy distribution of the X-ray emitting plasma is rather different for the solar-type stars of NGC 2547 than for those in older clusters or cooler stars – the HRI observations had no spectral resolution and so a uniform conversion factor was used to estimate X-ray fluxes from count rates.

In this paper we present the results of an [*XMM-Newton*]{} observation of NGC 2547 using the European Photon Imaging Camera (EPIC), which seeks to characterise the coronal emission of solar-type (and lower mass) stars at $\simeq 30$Myr. The sensitivity of these X-ray images is better than the [*ROSAT*]{} HRI data, enabling us to identify cluster members with lower activity and measure X-ray emission from cluster members with lower mass. There is also some spectral resolution available with the EPIC data that allows us to test whether the X-ray spectra of the solar-type members of NGC 2547 are significantly different to active stars in other open clusters. Finally, we are able to look for possible variability in the level of X-ray emission of these young stars on 