SUPER — AGN Feedback At Cosmic Noon: A Multi-phase And Multi . - ESO

1.0KASHz, Lx 10 43.9 erg s –11log(M [M yr –1])Cumulative fracton2SUPER, Lx 10 44.8 erg s –10.8SUPER Bionical outflowSUPER Thin-shellFiori et al. (2017)Davies et al. (2020)3Wylezalek et al. W80 (km s –1)Figure 3. The inverse cumulative W80 distribution forthe Type-1 AGN in the SUPER survey (red; Kakkad etal., 2020), the KASHz survey matched in redshift(black; Harrison et al., 2016), a mass-matched low- redshift star-forming sample (blue; Wylezalek et al.,2020). The dashed black-line at 600 km s –1 corresponds to the W80 value used to define that a targethosts an AGN-driven outflow (well justified from thefact that almost all star-forming galaxies have W80values below this cut). Based on the above W80 criteria, all the Type-1 targets in SUPER show the presence of outflows, and 52% of the redshift matchedtargets in the KASHz survey show outflows. The difference between the W80 distributions for SUPERand KASHz surveys is due to the different luminosityrange of the AGN sampled by these surveys.The final sample consists of 39 AGN(Circosta et al., 2018) for which we havesuperb multi-wavelength ancillary data thatallow us to properly characterise the centralSMBH and its host galaxy: stellar masses(4 x 109 – 2 1011 M ), star formationrates (25–680 M yr–1) and AGN bolometricluminosities (2 1044 – 8 1047 erg s –1).Of the 39 targets, 22 are classified asType-1 (56%) and the remaining 17as Type-2 (44%), based on the presenceor absence of broad emission lines suchas Mg II or C IV in the rest-frame ultraviolet spectra.The SINFONI adaptive optics (AO) observations were performed in Laser GuideStar Seeing Enhancer (LGS-SE) mode,which has demonstrated the capabilityto achieve a point spread function (PSF)full width half maximum (FWHM) of0.2–0.3 arcseconds. This allows us tospatially resolve any outflows with sizeslarger than 2 kpc. This is a key featureof the survey that allows us to resolve thekinematics of the ionised gas at a finerspatial scale than seeing-limited observations (see Figure 1), and consequentlydecreases significantly the uncertaintiesin the derived physical properties of thedetected outflows. We set our observational strategy to be able to properly tracethe PSF using directly the light distribution of the broad Hβ components forType-1 AGN and dedicated observationsof PSF reference stars that we performedclose to the science observations ofType-2 AGN. Curve-of-growth analysisand more sophisticated methodologieshave been used to take into account anybeam-smearing effect in the data cubesand thereby to retrieve the best estimatesof the outflowing gas properties (forexample, extension and velocity; Kakkadet al., 2020).AGN outflow demography and scalingrelationsOne of the main goals of SUPER is toperform a demographic study of the incidence of AGN-driven outflows at z 2.In Kakkad et al. (2020) we present theresults obtained for the Type-1 AGN inthe SUPER sample and find that all of444546log(Lbol [erg s –1])4748Figure 4. Ionised gas [O III] mass outflow rate vs. thebolometric luminosity of the AGN in the SUPERType-1 sample (from Kakkad et al., 2020). The redshaded area and the black hatched area show themass outflow rates for the SUPER targets assuminga bi-conical outflow model and a thin shell model,respectively. The green shaded area shows the outflow rates for ionised gas from literature data compiled in Fiore et al. (2017) and the blue shaded regionshows the outflow rates for a low redshift X-ray AGNsample from Davies et al. (2020). The shadedregions all correspond to mass outflow rates assuming an electron density of 500–10 000 cm 3.them feature a galaxy-wide outflow (Figure 3). The parameter adopted to identifyoutflows is the velocity width of the [O III]line containing 80% of the flux (i.e., W80).A value of W80 larger than 600 km s –1 isconsidered a clear signature of an AGNdriven outflow, based on the W80 distributions of large galaxy samples at z 2(see Kakkad et al., 2020). We thereforeshow that AGN-driven outflows are common in a blind-selected sample of AGN atz 2, which obviously further supportsthe hypothesis that AGN-feedback playsan important role in galaxy evolution. Adetailed comparison of the PSF and the[O III] radial profile shows that the [O III]emission is spatially resolved for 35%of the Type-1 sample and the outflowsshow an extension up to 6 kpc.Another main goal of SUPER was to linkthe properties of the observed outflowswith the properties of the central SMBH(for example, its bolometric luminosity).The Messenger 182 202147

Tracing AGN winds from pc to kpcscalesSeveral theoretical models have beenproposed to describe how the energyreleased by the central SMBH couples tothe surrounding medium and generatesthe outflows observed on galaxy scales.With SUPER we have the remarkableopportunity to constrain the different models, since we are able to trace the windsfrom scales smaller than 1 pc out to several kpc. In Vietri et al. (2020), we useancillary data to study the high-ionisationC IV 1549 Å line originating from thebroad line region (BLR) surrounding thecentral SMBH. We confirm the wellknown fact that the C IV line width doesnot correlate with the Balmer lines andthe peak of the line profile is blueshiftedwith respect to the [O III]-based systemicredshift. These findings support the ideathat the C IV line is tracing outflowing gasin the BLR, for which we estimated velocities up to 4700 km s –1. We inferredBLR mass outflow rates in the range0.005–3 M yr –1, showing a correlationwith the bolometric luminosity consistentwith that observed for ionised winds inthe narrow line region (NLR) and X-raywinds detected in local AGN. Finally, wefound an anti-correlation between theequivalent width of the [O III] line and the48The Messenger 182 202160SUPER2.25WISSH Vietri et al. (2018)502.001.75401.50301.25EW [O III] (Å)Theoretical models of AGN outflows predict that fast winds originating from theaccretion disc impact on the ISM, resulting in a forward shock that expandswithin the host galaxy. This would naturally predict positive correlations betweenoutflow properties (for example, velocityand mass outflow rate) and AGN properties (see, for example, King & Pounds,2015). In Kakkad et al. (2020), we explorea range of plausible assumptions aboutthe physical properties of the outflow (itsgeometry, velocity and radius) and of theoutflowing gas (its electron density) andreport the range of derived mass outflowrates for each target. The mass outflowrates for the Type-1 sample are in therange 0.01–1000 M yr –1. After factoring in the systematic uncertainties in theoutflow models, these outflow rates seemto correlate with the bolometric luminosity of the AGN (see Figure 4), as expectedon the basis of the above theoreticalarguments.Mainieri V. et al., SUPER — AGN Feedback at Cosmic Noonlog(EW [O III] [Å])Astronomical Science1.00200.75–1000010002000v C50IV (km s –1)30004000500010C IV velocity shift (see Figure 5), and apositive correlation with the [O III] outflowvelocity. These findings, for the first timein an unbiased sample of AGN at z 2,support a scenario in which BLR windsare connected to galaxy-scale detectedoutflows and are therefore actually capable of affecting the gas in the NLRlocated at kpc scales (Vietri et al., 2020).Figure 5. [O III] equivalent width as a function of thevelocity shift of the C IV emission line for the SUPERsample (diamonds), colour-coded according to the[O III] equivalent width. Additionally, the WISE/SDSSSelected Hyperluminous quasars (WISSH; Bischettiet al., 2017) sample with reliable [O III] measurements are also reported (empty triangles). A clearanti-correlation is present, which supports the ideathat the BLR winds traced by the C IV are connectedwith the winds on kpc scales detected in the NLRusing the [O III] line (Vietri et al., 2020).Ongoing work, data releases andoutlookimpact that the AGN may have on them(Circosta et al., 2021).– The dust properties of our targets, astraced by ALMA Band-7 continuumobservations at high resolution, compared with the spatial location of theoutflow and of the unobscured star formation as traced by the SINFONI Hαemission (Lamperti et al., in preparation).– The outflow properties of the fullSUPER sample, and the dependenceon the host galaxy properties, forexample stellar mass and star formation rate (Perna et al., in preparation).At the time of writing all the data for theLarge Programme have been acquired,and a first set of results has been alreadypublished. The SUPER first data releaseis accessible via the ESO Science ArchiveFacility (SAF)2 and consists of flux- calibrated data cubes for half of the sample. Next year we plan to have a secondand final data release for the wholeSUPER sample.The team is working on a series of additional studies, combining the SINFONIdata with follow-up data obtained inrecent years. These include:– A systematic study of the moleculargas reservoir, as traced by ALMACO(3-2) observations, in the SUPERAGN host galaxies, to assess theSUPER has already fulfilled its ambitionand represents a major advancement inthe systematic studies of AGN-drivenoutflows at a crucial cosmic epoch corresponding to the peak of volume-averagedstar formation and supermassive blackhole accretion in the Universe. It further

complemented by the investment of substantial resources in the modelling of themulti-phase outflows, in particular withdetailed simulations able to trace the coldmolecular gas.AcknowledgementsWe are extremely grateful to the numerous ESO staffin Paranal Observatory for their dedication in carryingout the SINFONI observations, and to Elena Valenti ofESO’s User Support Department for excellent supportduring the execution of the Large Programme.ReferencesAlexander, D. M. et al. 2010, MNRAS, 402, 2211Begelman, M. C. 2003, Science, 300, 1898Bischetti, M. et al. 2017, A&A, 598, A122Brusa, M. et al. 2016, A&A, 588, A58Carniani, S. et al. 2015, A&A, 580, A102Cicone, C. et al. 2018, Nature Astronomy, 2, 176Circosta, C. et al. 2018, A&A, 620, 82Circosta, C. et al. 2021, A&A, in press,arXiv:2012.07965Coil, A. L. et al. 2015, ApJ, 801, 35Cresci, G. et al. 2015, ApJ, 799, 82Davies, R. et al. 2020, MNRAS, 498, 4150Faucher-Giguère, C.-A. & Quataert, E. 2012,MNRAS, 425, 605Fiore, F. et al. 2017, A&A, 601, A143Harrison, C. M. et al. 2012, MNRAS, 426, 1073Harrison, C. M. et al. 2016, MNRAS, 456, 1195Kakkad, D. et al. 2016, A&A, 592, A148Kakkad, D. et al. 2020, A&A, 642, 147Kewley, L. J. et al. 2013, ApJ, 774, 100King, A. R. & Pounds, K. 2003, MNRAS, 345, 657King, A. R. & Pounds, K. 2015, ARA&A, 53, 115Menci, N. et al. 2008, ApJ, 686, 219Nesvadba, N. P. H. et al. 2006, ApJ, 650, 693Nesvadba, N. P. H. et al. 2007, A&A, 475, 145Perna, M. et al. 2015, A&A, 583, A72Silk, J. & Rees, M. J. 1998, A&A, 331, L1Steidel, C. C. et al. 2014, ApJ, 795, 165Vayner, A. et al. 2017, ApJ, 851, 126Vietri, G. et al. 2018, A&A, 617, A81Vietri, G. et al. 2020, A&A, 644, 175Wylezalek, D. et al. 2020, MNRAS, 492, 4680Zubovas, K. & King, A. 2012, ApJ, 745, L34Links12SUPER website: www.super-survey.org SUPER first data release access via the ESO acollection SUPER&publ date 2020-09-29ESO/P. Horálekrepresents the ideal sample for follow-upstudies with current and future facilities.The hot ionised gas kinematics need tobe complemented with a significantinvestment of ALMA time to trace thecold molecular phase of the outflows (forexample, Cicone et al., 2018). The launchof the JWST will enable the study of theH2 rotational emission lines in the mid- infrared which could be used as an alternative means to trace the molecular phaseof these outflows. Finally, the next generation of integral field units at the forthcoming extremely large telescopes (forexample, the High Angular ResolutionMonolithic Optical and Near-infraredIntegral field spectrograph [HARMONI] atESO’s Extremely Large Telescope) willhave the necessary sensitivity and spatialresolution to trace the dependency of themass outflow rate as a function of radiusinside the galaxy, which is very muchneeded to provide strong constraints onthe different theoretical models. Finally,these observational efforts should beAs the Sun sets, ESO’s Very Large Telescope (VLT)springs into action to begin its nightly mission. Consisting of four 8.2-metre Unit Telescopes (UTs) —named Antu, Kueyen, Melipal, and Yepun — andfour smaller 1.8-metre Auxiliary Telescopes (ATs), theVLT is one of the most advanced telescope facilitiesin the world. All eight telescopes can be seen in thisimage, the smaller and rounder ATs scatteredamongst the larger and more angular UTs.The Messenger 182 202149

affecting the bulk of the baryons in the Universe. While the presence of such outflows out to kpc scales is now undisputed, their impact on the star . SUPER — AGN Feedback at Cosmic Noon: a Multi-phase and Multi-scale Challenge 10.0 1.0 Spatial re solution (kpc) 0.0 0.51 .0 1.52 .0 2.53 .0 3.54 .0 Redshift SUPER Carniani et al. (2015)