An XMM-Newton observation of the luminous Seyfert galaxy PG1211+143 in 2001 revealed the first clear evidence for a highly ionised high speed wind ( in a non-BAL AGN ) , with a velocity of v \sim 0.09c based on the identification of blue-shifted absorption lines in both EPIC and RGS spectra .
A subsequent analysis of EPIC spectra , including additional absorption lines , led to an upward revision of the wind speed to \sim 0.14c , while broad band modelling indicated the need for a second , partial covering absorber to account for continuum curvature and spectral variability .
We show here , in a new analysis of the XMM-Newton RGS data , that this additional absorber is detected in the soft X-ray spectra , with the higher spectral resolution providing a much improved velocity constraint , with v \sim 0.07c .
Similar variability of the \sim 0.07c and \sim 0.14c outflow components suggest they are physically linked , and we speculate that occurs by the fast ( primary ) wind impacting on small clumps of higher density , slow moving matter close to the disc .
We show that strong , velocity broadened soft X-ray emission features , located at the redshift of PG1211+143 indicate the extended scale of the ionised outflow .