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Accretion disk winds launched close to supermassive black holes (SMBHs) are aviable mechanism to provide feedback between the SMBH and the host galaxy. Weaim to characterize the X-ray properties of the inner accretion disk wind ofthe nearby active galactic nucleus (AGN) PG 1126-041, and to study itsconnection with the ultraviolet (UV)-absorbing wind. We perform spectroscopicanalysis of eight XMM-Newton observations of PG 1126-041 taken between 2004 and2015, using both phenomenological models and the most advanced accretion diskwind models available. For half of the dataset, we can compare the X-rayanalysis results with the results of quasi-simultaneous, high-resolutionspectroscopic UV observations taken with the Cosmic Origins Spectrograph (COS)on board the Hubble Space Telescope. The X-ray spectra of PG 1126-041 arecomplex and absorbed by ionized material which is highly variable on multipletime scales, sometimes as short as 11 days. Accretion disk wind models canaccount for most of the X-ray spectral complexity of PG 1126-041, with theaddition of massive clumps, represented by a partially covering absorber.Variations in column density ($N_H \sim 5-20 \times 10^{22}$ cm$^{-2}$) of thepartially covering absorber drive the observed X-ray spectral variability of PG1126-041. The absorption from the X-ray partially covering gas and from theblueshifted C IV troughs appear to vary in a coordinated way. The line of sighttoward PG 1126-041 offers a privileged view through a highly dynamic nuclearwind originating on inner accretion disk scales, making the source a verypromising candidate for future detailed studies of the physics of accretiondisk winds around SMBHs.

Coordinated X-ray and UV absorption within the accretion disk wind of the active galactic nucleus PG 1126-041