SUPER

II. Spatially resolved ionised gas kinematics and scaling relations in z  ∼  2 AGN host galaxies

¹ European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla, 19001 Santiago de Chile, Chile
e-mail: dkakkad@eso.org
² European Southern Observatory, Karl-Schwarzschild-Strasse 2, Garching bei München, Germany
³ Cluster of Excellence, Boltzmann-Str. 2, 85748 Garching bei München, Germany
⁴ INAF IASF-Milano, Via Alfonso Corti 12, 20133 Milano, Italy
⁵ Scuola Normale Superiore, Piazza dei Cavalieri 7, 56126 Pisa, Italy
⁶ School of Mathematics, Statistics and Physics, Newcastle University, Newcastle upon Tyne NE1 7RU, UK
⁷ Centro de Astrobiología (CAB, CSIC–INTA), Departamento de Astrofísica, Cra. de Ajalvir Km. 4, 28850 Torrejón de Ardoz, Madrid, Spain
⁸ INAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
⁹ Centre for Extragalactic Astronomy, Department of Physics, Durham University, South Road, Durham DH1 3LE, UK
¹⁰ Chalmers University of Technology, Department of Earth and Space Sciences, Onsala Space Observatory, 43992 Onsala, Sweden
¹¹ Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, UK
¹² Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
¹³ INAF – Osservatorio Astronomico di Roma, Via Frascati 33, Monte Porzio Catone, 00078 Roma, Italy
¹⁴ Universitá degli Studi di Roma “Tor Vergata”, Via Orazio Raimondo 18, 00173 Roma, Italy
¹⁵ INAF – Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, 34143 Trieste, Italy
¹⁶ Dipartimento di Fisica e Astronomia, Universitá di Firenze, Via G. Sansone 1, Sesto Fiorentino, 50019 Firenze, Italy
¹⁷ Dipartimento di Fisica e Astronomia dell’Universitá degli Studi di Bologna, via P. Gobetti 93/2, 40129 Bologna, Italy
¹⁸ INAF/OAS, Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, via P. Gobetti 93/3, 40129 Bologna, Italy
¹⁹ Institute of Theoretical Astrophysics, University of Oslo, PO Box 1029, Blindern, 0315 Oslo, Norway
²⁰ School of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978, Israel
²¹ Max-Planck-Institut für extraterrestrische Physik (MPE), Giessenbachstrasse 1, 85748 Garching bei München, Germany
²² National Astronomical Observatory of Japan, Mitaka, 181-8588 Tokyo, Japan
²³ Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo (Kavli IPMU, WPI), Kashiwa 277-8583, Japan
²⁴ Department of Astronomy, School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan

Received: 1 June 2020
Accepted: 28 July 2020

Abstract

Aims. The SINFONI survey for Unveiling the Physics and Effect of Radiative feedback (SUPER) aims to trace and characterise ionised gas outflows and their impact on star formation in a statistical sample of X-ray selected active galactic nuclei (AGN) at z ∼ 2. We present the first SINFONI results for a sample of 21 Type 1 AGN spanning a wide range in bolometric luminosity (log L_bol = 45.4–47.9 erg s⁻¹). The main aims of this paper are to determine the extension of the ionised gas, characterise the occurrence of AGN-driven outflows, and link the properties of such outflows with those of the AGN.

Methods. We used adaptive optics-assisted SINFONI observations to trace ionised gas in the extended narrow line region using the [O III] λ5007 line. We classified a target as hosting an outflow if its non-parametric velocity of the [O III] line, w₈₀, was larger than 600 km s⁻¹. We studied the presence of extended emission using dedicated point-spread function (PSF) observations, after modelling the PSF from the Balmer lines originating from the broad line region.

Results. We detect outflows in all the Type 1 AGN sample based on the w₈₀ value from the integrated spectrum, which is in the range ∼650–2700 km s⁻¹. There is a clear positive correlation between w₈₀ and the AGN bolometric luminosity (> 99% correlation probability), and the black hole mass (98% correlation probability). A 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 outflows show an extension up to ∼6 kpc. The relation between maximum velocity and the bolometric luminosity is consistent with model predictions for shocks from an AGN-driven outflow. The escape fraction of the outflowing gas increases with the AGN luminosity, although for most galaxies, this fraction is less than 10%.