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I will present our results from the MAGNUM survey, which exploits the unique capabilities of the optical/NIR integral field spectrograph MUSE at VLT to study in detail the properties of outflows in nearby Seyferts and their impact on the ISM and star formation in the host (feedback mechanism). MUSE allowed us to map the ionized gas down to ~10 pc in several emission lines revealing ubiquitous kpc-scale outflows, whose properties (e.g. velocity, density, mass rate etc…) were spatially dissected. By matching MUSE with radio data, we detected an intriguing (and possibly common) phenomenon, likely produced by the impact of low-power jets on their host galaxy disks. Finally, we found also evidence of outflow-induced star formation. I will also present preliminary results from a survey of mergers and dual AGN with MUSE Wide- + Narrow-Field, aimed at characterizing outflow acceleration along the whole merger sequence at all spatial scales and the role of mergers in triggering AGN activity.

The origin of the tight correlations observed between the masses of supermassive black holes (SMBHs) and host galaxy properties is still debated. Negative feedback from AGN can provide a viable explanation for these correlations. According to the theoretical models, the ejective feedback resulting from radiatively-efficient episodes of gas accretion onto SMBHs may be the main responsible for the rapid shut-off of star formation and black hole growth in the early stages of the evolution of present-day massive galaxies, which must have taken place at z>2. Here we present near-IR (SINFONI) and millimetre (ALMA) observations of z~2.5 luminous (Lbol>1e47 Lsun) quasars showing fast and extended ionised outflows. These AGN-driven outflows appear to be able to expel a large fraction of molecular and ionised gas and suppress star formation in the outflow region. However, the detection of Halpha emission along the edges of the outflow cone indicates on-going star formation rates of at least 50 Msun/yr, suggesting either that AGN feedback does not affect the whole galaxy or that many feedback episodes are required before star formation is completely quenched. On the other hand, the detection also lead to a positive feedback interpretation: the AGN-driven outflow compress the surrounding gas inducing star formation. Our results highlight the possible double role of galaxy-wide outflows in host galaxy evolution. This is also supported by recent observations in the local Universe indicate that massive galactic outflows may ignite star formation within the outflow itself. We also present new ALMA observations of a sample of quasars at z∼6 optimised to investigate the extended emission associated with outflows as traced by the [CII]158μm line. Although strong and powerful AGN-driven outflows are expected at these redshifts, our analysis suggests that such outflows may not be as effective as expected in removing gas out of their host galaxies.

AGN outflows are believed to play a major role in shaping the properties of host galaxies, by sweeping away the gas and quenching star formation (negative feedback). In this framework our MAGNUM survey aims at investigating in detail the interplay between AGN activity and star formation processes in nearby active galaxies which, due to their vicinity, are the ideal laboratories to carry out such a study. The sample comprises ten famous nearby Seyfert galaxies so far, such as Circinus, NGC 1365 and NGC 4945. Thanks to its unique combination of large field of view and spectral coverage, MUSE at VLT allowed us to map the ionised gas down to ~10 pc in several nebular emission lines revealing ubiquitous kpc-scale outflows, whose properties (e.g. velocity, mass outflow rate, kinetic rate etc...) as a function of distance from the active nucleus were measured. By matching MUSE with Chandra X-ray observations we studied the ionized gas and the outflow kinematics and energetics in its different phases and spatial scales in NGC 1365, and obtained unique insights on the properties of the outflows and of the ISM.Additionally, we recently found evidence of a new mode of star formation, occurring within a starburst outflow itself, as predicted by recent models.

I will review the most important results from near-IR spectroscopic observations of WISE/SDSS selected hyper-luminous (WISSH) quasars, designed to accurately probe the role of nuclear activity in SMBH-galaxy self-regulated growth via extended outflows. The total sample consists of 90 broad-line quasars at the brightest end of theAGNluminosity function (L_bol > 1014 L_sun) and at the peak of their number density (z ~ 2.5 - 3.5). We found that WISSH quasars are typically powered by highly accreting (0.3-3 Ledd), ten billion solar masses SMBHs, demonstrating that WISSH provides a simple and valuable tool to complete the census of the extreme SMBH population in the Universe. The huge luminosity drives very powerful winds both at BLR and NLR scales. We discovered [OIII] emission lines with a broad profile, tracing ionized outflows with kinetic power up to ~4% of L_bol in ~30% of the sample.Remarkably, the remaining 70% of quasars lacks [OIII] emission but shows strong winds traced by 3,000-8,000 km/s blueshifts of the CIV broad emission line, revealing strong radiatively driven winds that dominate the BLR kinematics. Finally, I will discuss nuclear and outflows properties of WISSH quasars in terms of inclination angle and fundamentalAGNparameters such as bolometric luminosity, SMBH mass, Eddington ratio and the shape of the UV-X-ray continuum.

The standard QSO-galaxy co-evolutionary scenario predicts a phase of deeply "buried" supermassive black hole growth coexisting with a starburst (SB) before feedback phenomena deplete the cold molecular gas reservoir of the galaxy and an optically luminous QSO is revealed ("SB-QSO evolutionary sequence"). We tested simple SB-QSO paradigm predictions by comparing the molecular (carbon monoxide, CO) gas properties of 56 obscured and 49 unobscured QSO host galaxies at high-redshift (z~1-6) with those of ~ 170 high-z star forming galaxies from the literature. We found that, on average, obscured AGN at z >1 are associated with higher star formation efficiencies (SFEs) and lower gas fractions with respect to normal star forming galaxies and SBs at given stellar mass and redshift. These results could suggest that their cold gas content has been already depleted by powerful AGN-driven outflows. Moreover, we did not find any clear separation between the properties of unobscured and obscured QSOs (e.g. they have similar SFEs), suggesting a scenario where feedback can rapidly impact the host galaxy evolution.

The standard QSO-galaxy co-evolutionary scenario predicts a phase of deeply "buried" supermassive black hole growth coexisting with a starburst (SB) before feedback phenomena deplete the cold molecular gas reservoir of the galaxy and an optically luminous QSO is revealed ("SB-QSO evolutionary sequence"). We tested simple SB-QSO paradigm predictions by comparing the molecular (carbon monoxide, CO) gas properties of 56 obscured and 49 unobscured QSO host galaxies at high-redshift (z~1-6) with those of ~ 170 high-z star forming galaxies from the literature. We found that, on average, obscured AGN at z >1 are associated with higher star formation efficiencies (SFEs) and lower gas fractions with respect to normal star forming galaxies and SBs at given stellar mass and redshift. These results could suggest that their cold gas content has been already depleted by powerful AGN-driven outflows. Moreover, we did not find any clear separation between the properties of unobscured and obscured QSOs (e.g. they have similar SFEs), suggesting a scenario where feedback can rapidly impact the host galaxy evolution.

A WISE/SDSS-selected hyper-luminous quasar (WISSH) survey study on the BLR and galaxy scale winds

Outflows and SF in QSO

A detailed study of outflows in nearby galaxies with extended narrow line region with MUSE.

(On behalf of the WISSH collaboration) The WISE/SDSS-selected hyper-luminous quasar (WISSH) survey is an extensive multi-band observing program to investigate the role of nuclear activity in SMBH-galaxy self-regulated growth via extended outflows. Our ongoing project is designed to accurately probe the relationship between nuclear and host galaxy ISM properties in a large sample of ~90 quasars at the brightest end of the AGN luminosity function (log LBol > 47.3) and at the peak of their number density (z~2.5-3.5)We will report on the discovery of highly accreting (0.3-3Ledd), ten billion solar masses SMBHs being able to produce very powerful (up to ~ 4% of L_bol) ionized outflows and accretion disk windsThe impact of AGN-driven feedback on their host galaxies will be also discussed.

In this talk I will present the first results from the MAGNUM survey (Measuring Active Galactic Nuclei Under MUSE Microscope), which is aimed at exploiting the unique combination of large field of view and spectral range provided by MUSE for detailed physical studies of the interaction of AGN outflows with their host galaxies and of the connection between AGN activity and star formationData have been obtained for about ten galaxies so far, including the famous NGC 1068, NGC 1365, Circinus and NGC 4945. MUSE has allowed us to map the AGN-driven outflows in several different emission lines revealing a clear kinematical and spatial structure related to the ionisation cone and which depends on line excitation. Further insight has been gained by comparing emission line maps from MUSE with high resolution X-ray images from Chandra. Finally, possible evidence for star formation triggered by AGN outflows has been found.

The WISE/SDSS selected hyper-luminous (WISSH) quasars survey is an extensive multiband observing program (from millimeter wavelengths to hard X rays) to investigate the role of nuclear activity in SMBH-galaxy self-regulated growth via extended outflows. Our ongoing project is designed to accurately constrain both AGN and host galaxy ISM properties in a large sample of ~ 90 broad-line quasars at the brightest end of the AGN luminosity function (L_bol > 1e14 L_sun) and at the peak of their number density (z ~ 2 - 4)I will review the most relevant results obtained to date with emphasis on the discovery of extremely powerful (up to ~ 4% of L_bol) ionized outflows, the relation between AGN properties (obscuration, luminosity and Eddington ratio) and large-scale winds, and the SED of these hyper-luminous quasars.

The epoch between redshift of 1-3 has become the prime focus of many galaxy evolutionary studies as the accretion rates of super massive black holes at the galactic center and the star formation rates of their hosts peaked around this period, pointing to their co-evolution throughout cosmic history. We will present two different approaches to study the impact of high redshift AGN (z~1.5) on the host galaxy: a) CO(2-1) observations from ALMA in a sample of "main sequence" AGNs to compare the star formation efficiency and gas fractions in active and inactive galaxies. b) SINFONI-IFU observations of a representative sample of high redshift quasars for which we observe intermediate to high velocity outflows using [OIII]5007 line diagnostics. These outflows are extended up-to kiloparsec scales and have an asymmetric geometry. With these approaches, one is able to test the effect of AGN feedback on the molecular as well as the ionized gas content.

In this talk I will present the first results from the MAGNUM survey (Measuring Active Galactic Nuclei Under MUSE Microscope), which takes advantage of the unprecedented combination of the large field of view and spectral coverage of MUSE so as to carry out a detail study of the interaction of AGN outflows with the host galaxies and of the relation between AGN activity and star formation. The data comprise ten nearby galaxies so far, such as NGC 1365, NGC 1068 and Circinus. The analysis of MUSE data in many different emission lines has allowed to disentangle the various motions of the gas in the central regions of the galaxies (rotation, outflows and inflows), furthermore resolving the structure of the AGN-ionised cone. Other information of the separate phases of the gas (having different temperature, density and ionisation state) has been obtained thanks to the comparison with high resolution X-ray Chandra images. Moreover, possible evidence for star formation triggered by AGN outflows has been observed.