  Outflows of photoionized gas are commonly detected in the X-ray spectra of
Seyfert 1 galaxies. However, the evidence for this phenomenon in broad line
radio galaxies, which are analogous to Seyfert 1 galaxies in the radio-loud
regime, has so far been scarce. Here, we present the analysis of the X-ray
absorption in the radio-loud quasar 4C +74.26. With the aim of characterizing
the kinetic and the ionization conditions of the absorbing material, we fitted
jointly the XMM-Newton Reflection Grating Spectrometer (RGS) and the Chandra
High Energy Transmission Grating Spectrometer (HETGS) spectra, which were taken
4 months apart. The intrinsic continuum flux did not vary significantly during
this time lapse. The spectrum shows the absorption signatures (e.g., Fe-UTA,
\ion{O}{vii}, and \ion{Ne}{vii}--\ion{Ne}{x}) of a photoionized gas outflow
($N_{\rm H} \sim 3.5 \times 10^{21} \rm cm^{-2}$, $\log \xi \sim 2.6$, $v_{\rm
out}\sim 3600 \, \rm km \, s^{-1}$) located at the redshift of source. We
estimate that the gas is located outside the broad line region but within the
boundaries of the putative torus. This ionized absorber is consistent with the
X-ray counterpart of a polar scattering outflow reported in the optical band
for this source. The kinetic luminosity carried by the outflow is insufficient
to produce a significant feedback is this quasar. Finally, we show that the
heavy soft X-ray absorption that was noticed in the past for this source arises
mostly in the Galactic ISM.
