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We present a detailed analysis of the  Chandra  High Energy Transmission Grating Spectrometer (HETGS) and  XMM–Newton  high‐resolution spectra of the bright Seyfert 1 galaxy, Mrk 290.  The  Chandra  HETGS spectra reveal complex absorption features that can be best described by a combination of three ionized absorbers. The outflow velocities of these warm absorbers are about  450 km s −1  , consistent with the three absorption components found in a previous far‐UV study. The ionizing continuum of Mrk 290 fluctuated by a factor of 1.4 during  Chandra  observations on a time‐scale of 17 d. Using the response in opacity of the three absorbers to this fluctuation, we put a lower limit on the distance from the ionizing source of 0.9 pc for the medium ionized absorber and an upper limit on a distance of 2.5 pc for the lowest ionized absorber. The three ionization components lie on the stable branch of the thermal equilibrium curve, indicating roughly the same gas pressure. Therefore, the thermal wind from the torus is most likely the origin of warm absorbing gas in Mrk 290.  During the  XMM–Newton  observation, the ionizing luminosity was 50 per cent lower compared to that in the  Chandra  observation. The Reflection Grating Spectrometer spectrum is well fitted by a two‐phase warm absorber, with several additional absorption lines attributed to a Galactic high‐velocity cloud, complex C. Neither the ionization parameter  ξ  nor the column density   N  H   of the two absorbing components varied significantly, compared to the results from  Chandra  observations. The outflow velocities of both components were  1260 km s −1  . We suggest that an entirely new warm absorber from the torus passed through our line of sight.  Assuming the torus wind model, the estimated mass outflow rate is  ∼0.1 M ⊙   per year while the nuclear accretion rate is  ∼0.04 M ⊙   per year. The O  vii  and Ne  ix  forbidden lines are the most prominent soft X‐ray emission lines, with a mean redshift of  700 km s −1   relative to the systematic velocity. There seems to be no relation between emission lines and warm absorbers.

Chandra and XMM–Newton view of the warm absorbing gas in Mrk 290