fits, with an average $Z \simeq 0.3$. This value is likely dominated by the effects of a group of strong (unresolved) iron lines around 1keV. The deduction of low coronal metallicity is a common feature of spectral fits to X-ray data from low-mass stars with high levels of magnetic activity (e.g. Briggs & Pye 2003; Güdel 2004). Telleschi et al. (2005) studied solar analogues at a range of ages, finding that coronal iron abundances decrease from solar values for an average coronal temperature of 4MK to half-solar at temperatures of 10MK. The NGC 2547 stars have average (emission measure weighted) coronal temperatures $>10$MK, so a coronal metallicity of $Z \simeq 0.3$ is not surprising.

  ------ ------- ------------------ --------------------- ------------------ ----------------------------- --------------------
   Star  $B-V$   $kT$               $\log$ EM             $Z$                $\chi^2$ ($\chi^{2}_{\nu}$)   $P(\geq \chi^{2})$
                 (keV)              (cm$^{-3}$)                                                            
    3    0.791   1.05 (0.98 1.11)   53.39 (53.33 53.45)   0.16 (0.14 0.21)   130.7 (1.49)                  0.01
    4    0.536   0.68 (0.65 0.74)   53.55 (53.49 53.62)   0.13 (0.10 0.18)   57.5 (0.80)                   0.89
    5    1.485   1.38 (1.26 1.66)   53.43 (53.34 53.48)   0.12 (0.07 0.21)   105.7 (1.22)                  0.08
    6    0.994   0.80 (0.74 0.87)   53.52 (53.46 53.58)   0.05 (0.03 0.07)   71.7 (0.96)                   0.59
    7    -0.06   0.69 (0.65 0.73)   53.16 (53.05 53.27)   0.23 (0.16 0.35)   