*L. Graziani[1], B. Ciardi[2], M. Glatzle[2], M. B. Eide[2], M. C. Orofino[1], S. Gallerani[1] [1] Scuola Normale Superiore di Pisa, Pisa, Italy [2] Max Planck Institute for Astrophysics, Garching bei Muenchen, Germany Massive black holes in evolving galaxies: from quasars to quiescence June 25-29, 2018 Institut d'Astrophysique de Paris (IAP), Paris - France X­rays ionization and heating by high­redshift quasars Here we discuss the impact of quasars (QSOs) on the ionization and heating of host and field galaxies and on the intergalactic medium (IGM), by showing the results of radiative transfer simulations accounting for X­rays and secondary electrons. By adopting a multi­scale approach (100 h­1 / 25 h­1 / 1 h­1 cMpc boxes) we study the importance of feedback in different environments and the impact on observables present at different scales. The role of QSO in the general context of a full reionization simulation [1­2] and their relative contribution in the evolution of the first Gyr of our Universe is addressed in the first box. The second box considers a single QSO HII region in a case matching a ULAS J1120+0641­like QSO. Implications for the HII region properties are also discussed [3]. Finally, new small scale simulations accounting for X­rays triggered photo­dissociation regions and metal ions are introduced in the last box [5­6­7]. Abstract Large scale reionization: impact of different sources Figure 1: 3D visualization of the HII, HeII and HeIII fractions in the QSO environment, as produced by both the central QSO and the surrounding galaxies with full UV and X-ray physics [1]. The images refer to a time tQ = 107 yr after the QSO has been turned on at z = 10. The simulation box is 50h-1 cMpc. Large scale reionization is dominated by the concerted impact of different sources. Galaxies drive the process during H-reionization, while QSOs create peculiar high-redshift environments and drive He-reionization [1,2]. Figure 2: Maps of temperature at z = 10 for galaxies only models with different assumptions of escape fractions ( GAL*), and galaxies+QSO models (GAL*+QSO) with UV and X-Rays [1]. Galaxies start to reionize the IGM at z = 15, while the QSO is turned on at z = 10 with a lifetime of 107 yr. The maps have a side length of 50h-1 cMpc and the width of the slice is 195h-1 ckpc. The galaxy and QSO H II (He III) I-front is shown as green and blue solid (dotted) contour, respectively. Figure 3: Maps in the plane of the first QSO at z = 12. Columns indicate different combinations of source types [2]. The upper rows show either HII or T, while the lower rows show the difference with respect to the first panel (stars only case). Simulation Box 100h-1 cMpc [3]. [1] Kakiichi, K.; Graziani, L.; Ciardi, B.; Meiksin, A.; et al., 2015, MNRAS, 468, 3 [2] Eide, M. B.; Graziani, L.; Ciardi, B.; Feng, Y.; et al., 2018, MNRAS, 476, 1 [3] Khandai, N.; Di Matteo, T.; Croft, R.; Wilkins, S.; et al., 2015, MNRAS, 450, 2 [4] Graziani L.; Ciardi B.; Glatzle, M., 2018, MNRAS, in press (DOI:10.1093/mnras/sty1367) [5] Barai, P.; Gallerani, S.; Pallottini, A.; Ferrara, A.; et al., 2018, MNRAS, 473, 3 [6] Graziani, L.; Maselli, A.; Ciardi, B., 2013, MNRAS, 431, 1 [7] Orofino, M. C.; Graziani, L.; Gallerani, S., et al., 2018, MNRAS, in prep. [8] Graziani, L.; Gallerani, S.;Orofino, M. C., et al., 2018, MNRAS, in prep. Reference Local scale: QSO host and field galaxies Figure 6: Slice cut of the simulation in [5] showing the gas number density (left panle), the velocity field ( middle) and the temperature field (right) in a plane intercepting both the QSO outflow and the galaxy host. The box is 1h-1 cMpc and it is shown in cell units (1 cell = 0.78 kpc physical). The simulation redshift is z=6. Figure 8: Star formation rate (SFR) evolution in redshift of a massive halo invested by the QSO outflow. Two feedback configurations are shown: spherical and conical. The evolution of star formation is strongly impacted by different modeling of QSO outflow [7