Speaker
Description
The characterization of AGN feedback is still an open issue. Theories and simulations indicate that AGN-galaxy co-evolution and feedback processes could be established through the generation of gas outflows. These are seen to arise from the innermost regions as powerful winds at sub-pc scales, visible in the X-ray band. We present the results from a systematic analysis of all the available Chandra and XMM-Newton data (as of October 2018) for Q2237+030, the Einstein Cross, a radio-quiet quasar at $\mathrm{z_Q=1.695}$, quadruply-imaged by a spiral galaxy at $\mathrm{z_L=0.0395}$.
We detect, for the first time, a fast X-ray wind in this object outflowing at $\mathrm{v_{out}\simeq0.1c}$, which seems to be powerful enough to significantly affect the host galaxy evolution ($\mathrm{\dot{E}_{kin}\simeq9\%\ L_{bol}}$). Given the absorption features detected throughout the data, we report also on the possible presence of a faster component of the wind ($\mathrm{v_{out}\sim0.5c}$). Evidence for outflows is found in nine spectra out of the sixteen analyzed, which allows us to give a rough estimate of the wind duty cycle as $\mathrm{\sim50\%}$.
| Affiliation | DIFA Bologna, OAS Bologna |
|---|---|
| Topic | Active Galactic Nuclei: accretion physics and evolution across cosmic time |
