Aims . The primary motivation for this project is to search for metal-rich star forming regions , in which , stars of super-solar metallicity will be created , as hopefully , will be extra-solar planets orbiting them !
The two aims of this project are : 1 : to show that our sample stars are young , lithium rich , magnetically active and non-accreting kinematic members of their respective regions . 2 : To measure the metallicity for such members .

Methods . The feros échelle spectrograph together with eso ’ s 2.2m telescope , was used to obtain high resolution ( R=32000 ) spectra for each of our weak-lined T-Tauri target stars .
The wavelength range of the spectra is \simeq 4000 - 8000 Ã .

Results . We find ( pre-main sequence ) model-dependent isochronal ages of the Lupus , Chamaeleon and CrA targets to be 9.1 \pm 2.1 Myr , 4.5 \pm 1.6 Myr and 9.0 \pm 3.9 Myr respectively .
The majority of the stars have Li i 6707.8 Ã equivalent widths similar to , or above those of , their similar mass Pleiades counterparts , confirming their youthfulness .
Most stars are kinematic members , either single or binary , of their regions .
We find a mean radial velocity for objects in the Lupus cloud to be { \overline { RV } } = +2.6 \pm 1.8 km s ^ { -1 } , for the Chamaeleon i & ii clouds , { \overline { RV } } = +12.8 \pm 3.6 km s ^ { -1 } whereas for the CrA cloud , we find { \overline { RV } } = -1.1 \pm 0.5 km s ^ { -1 } .

All stars are coronally and chromospherically active , exhibiting X-ray and H \alpha emission levels marginally less , approximately equal or superior to that of their older IC 2602/2391 and/or Pleiades counterparts .
All bar three of the targets show little or no signature of accretion from a circumstellar environment , according to their positions in a J - K/H - K ^ { { } ^ { \prime } } diagram .

For the higher quality spectra , we have performed an iron-line metallicity analysis for five ( 5 ) stars in Chamaeleon , four ( 4 ) stars in Lupus and three ( 3 ) stars in the CrA star forming regions .
These results show that all three regions are slightly metal-poor , with marginally sub-solar metallicities , with < [ Fe/H ] > = -0.11 \pm 0.14 , -0.10 \pm 0.04 & -0.04 \pm 0.05 respectively .

Conclusions . A sample of stars in several nearby , young star-forming regions has been established , the majority of which is young , lithium rich , magnetically active and are non-accreting kinematic members of their respective clouds .
Within the errors , each region is essentially of solar metallicity .
The spectroscopic data , comprising the major complement of observational products for this project , were collected at the European Southern Observatory at La Silla , Chile , proposal ID 70.C-0507 ( A ) .