Incidence and energetics of AGN outflows in X-ray selected samples

Incidence and energetics of AGN outflows in X-ray selected samples Blessing MUSIIMENTA University of Bologna and INAF Supervisor: Marcella Brusa Musiimenta et al. (2023), 679, A84 Musiimenta et al. (2024), 687, A111 Collaborators: eROSITA, BiD4BEST, HSC team 6 - 15 AUGUST 2024 AGN feedback: why do we care? ➢AGN play a crucial role in galaxy formation and evolution McConnell+2011 ❑Explains ○Galaxy/BH scaling relation ○Galaxy luminosity functions ○Star formation efficiencies ○Galaxy morphology and colours, etc (DiMatteo+2005, Hopkins+2006,Dubois+2016). ❑Effect of AGNs on galaxy evolution still not understood. Wellons+2022 Blessing MUSIIMENTA AGN feedback UNIBO & INAF Properties of QSO in feedback/outflows ❖Physical: ▪Moderate NH, obscured and ‘dusty’ ▪Accretion close to Eddington limit ❖Observed: ▪X-ray+IR luminous ▪Faint optical Red colours ➢Blow-out phase is short and sources are rare: need large area surveys to efficiently select them. ➢Innovative selection methods and dedicated observations are usually necessary. ●Short phase ●The multiphase and multi scale nature. Goal: Develop an approach to isolate red, obscured and highly accreting QSO at z~0.5-3, search for the presence of ionised outflows and assess the effect of AGN outflows to their host galaxies by comparison with simulations. AGN feedback: Outflows Blessing MUSIIMENTA AGN feedback UNIBO & INAF Harrison and Ramos Almeida 2024 ➢Blow-out phase is short and sources are rare: need large area surveys to efficiently select them. ➢Innovative selection methods and dedicated observations are usually necessary. Properties of QSO in feedback/outflows ❖Physical: ▪Moderate NH, obscured and ‘dusty’ ▪Accretion close to Eddington limit ❖Observed: ▪X-ray+IR luminous ▪Faint optical Red colours ➢Blow-out phase is short and sources are rare: need large area surveys to efficiently select them. ➢Innovative selection methods and dedicated observations are usually necessary. ●Short phase ●The multiphase and multi scale nature. Goal: Develop an approach to isolate red, obscured and highly accreting QSO at z~0.5-3, search for the presence of ionised outflows and assess the effect of AGN outflows to their host galaxies by comparison with simulations. AGN feedback: Outflows Blessing MUSIIMENTA AGN feedback UNIBO & INAF Harrison and Ramos Almeida 2024 ➢Blow-out phase is short and sources are rare: need large area surveys to efficiently select them. ➢Innovative selection methods and dedicated observations are usually necessary. Properties of QSO in feedback/outflows ❖Physical: ▪Moderate NH, obscured and ‘dusty’ ▪Accretion close to Eddington limit ❖Observed: ▪X-ray+IR luminous ▪Faint optical Red colours Characterised by their luminous, obscured, and dust-enshrouded environments, as predicted by theoretical models AGN feedback: Properties of AGN with outflows Blessing MUSIIMENTA AGN feedback UNIBO & INAF Goal: Develop an approach to isolate red, obscured and highly accreting QSO at z~0.5-3, search for the presence of ionised outflows and assess the effect of AGN outflows to their host galaxies by comparison with simulations. Properties of QSO in feedback/outflows ❖Physical: ▪Moderate NH, obscured and ‘dusty’ ▪Accretion close to Eddington limit ❖Observed: ▪X-ray+IR luminous ▪Faint optical Red colours Characterised by their luminous, obscured, and dust-enshrouded environments, as predicted by theoretical models AGN feedback: Properties of AGN with outflows Blessing MUSIIMENTA AGN feedback UNIBO & INAF Goal: Develop an approach to isolate red, obscured and highly accreting QSO at z~0.5-3, search for the presence of ionised outflows and assess the effect of AGN outflows to their host galaxies by comparison with simulations. The eROSITA Final Equatorial-Depth Survey (eFEDS) eFEDS Selection in eFEDS hard sample (Nandra+2024) eROSITA all sky survey (eRASS) Blessing MUSIIMENTA AGN feedback UNIBO & INAF A new discovery space opened by eROSITA: Ionised AGN outflows from X–ray selected samples Musiimenta et al. (2023), 679, A84 Color selection methods Perna+2015, Brusa+2022, Zakamska+2016, Vayner+2021, perrotta+2019 Kakkad+2016, Lansbury+2020 853 sources X-ray and optical spectral propertiies 528 sources ~1400 candidates isolated ID608 (Follow up study in later slides) Selection of AGN in the feedback phase (z>0.5) from eFEDS Musiimenta et al. (2023), 679, A84 Blessing MUSIIMENTA AGN feedback UNIBO & INAF AGN outflow scaling relations Weak/no correlation •X-ray active is best tracer of fastest phase of winds •Their velocity doesn’t depend only on Lbol Strong correlation Large scatter: mass outflow rate also depends on other factors (Ramos Almeida+2022) ➢Mass outflow rate of 0.2 –23 M☉yr-1 Kinetic power of 40 - 44 erg s-1 ➢Kinetic coupling efficiencies 1-10% (in 30% of the sample) ➢Indicating that the outflow is very relevant from the energetic point of view. Importance of “sample selections” Musiimenta et al. (2023), 679, A84 AGN feedback UNIBO & INAF Musiimenta et al. ( 2024), 687, A111 Ionised AGN outflows in the Goldfish galaxy - The illuminating and interacting red quasar eFEDSJ091157.4+014327 (ID608) at z ~0.6 Has ionised outflows MUSE datacube The Goldfish galaxy Blessing MUSIIMENTA AGN feedback UNIBO & INAF & eROAGN WG Musiimenta et al. ( 2024), 687, A111 Ionised AGN outflows in the Goldfish galaxy - The illuminating and interacting red quasar eFEDSJ091157.4+014327 (ID608) at z ~0.6 (Musiimenta et al. ( 2024), 687, A111) HSC grz image About ID608 Red colors and obscured, with outflows Has ionised outflows MUSE datacube The Goldfish galaxy Blessing MUSIIMENTA AGN feedback UNIBO & INAF & eROAGN WG Musiimenta et al. ( 2024), 687, A111 Ionised AGN outflows in the Goldfish galaxy - The illuminating and interacting red quasar eFEDSJ091157.4+014327 (ID608) at z ~0.6 (Musiimenta et al. ( 2024), 687, A111) HSC grz image About ID608 Red colors and obscured, with outflows Goal ➢Explore environment around this sources. Is the quasar located in a merging system? ➢Accurate measurement of outflow properties. Has ionised outflows MUSE datacube The Goldfish galaxy Blessing MUSIIMENTA AGN feedback UNIBO & INAF & eROAGN WG Musiimenta et al. ( 2024), 687, A111 Ionised AGN outflows in the Goldfish galaxy - The illuminating and interacting red quasar eFEDSJ091157.4+014327 (ID608) at z ~0.6 (Musiimenta et al. ( 2024), 687, A111) Goal ➢Explore environment around this sources. Is the quasar located in a merging system? ➢Accurate measurement of outflow properties. HSC grz image About ID608 Red colors and obscured, with outflows Gas distribution, structures and companion galaxies (C) 53 kpc × 50 kpc FOV maps Musiimenta et al. ( 2024), 687, A111 Blessing MUSIIMENTA AGN feedback UNIBO & INAF Gas distribution, structures and companion galaxies (C) 53 kpc × 50 kpc FOV maps Musiimenta et al. ( 2024), 687, A111 Blessing MUSIIMENTA AGN feedback UNIBO & INAF A complex interacting system possibly merging with three other galaxies that are within ~ 50 kpc. [O III] emission line fitting: Kinematic Musiimenta et al. ( 2024), 687, A111 Blessing MUSIIMENTA AGN feedback UNIBO & INAF ➢Kinetic coupling efficiency too low (0.01-0.2%); ○outflow not very relevant from the energetic point of view. ➢Outflows are more likely AGN-driven than star formation-driven (mass loading is 5). ➢Total mass outflow rate = 9.6 M☉yr-1 ➢Total kinetic power = 1.9x1042 erg/s [O III] emission line fitting: Kinematic Musiimenta et al. ( 2024), 687, A111 Blessing MUSIIMENTA AGN feedback UNIBO & INAF ➢Kinetic coupling efficiency too low (0.01-0.2%); ○outflow not very relevant from the energetic point of view. ➢Outflows are more likely AGN-driven than star formation-driven (mass loading is 5). ➢Total mass outflow rate = 9.6 M☉yr-1 ➢Total kinetic power = 1.9x1042 erg/s Take away message and summarys •eROSITA is as a powerful discovery machine for AGN in the feedback phase. •Weak/no correlation between outflow velocity and bolometric luminosity. ○Highlights the importance of sample selections •X-ray active,obscured is best tracer of fastest phase of winds •A complex interacting system, possibly merging with three companion galaxies within ~50 kpc away. • The outflows more likely AGN - driven than SF driven and less relevant from the energetic point of view. Musiimenta et al.(2024), 687, A111 Musiimenta et al. (2023), 679, A84 Blessing MUSIIMENTA AGN feedback UNIBO & INAF