SUPER — AGN Feedback at Cosmic Noon: a Multi-phase and Multi-scale Challenge

Mainieri, V.; Circosta, C.; Kakkad, D.; Perna, M.; Vietri, G.; Bongiorno, A.; Brusa, M.; Carniani, Stefano; Cicone, C.; Civano, F.; Comastri, A.; Cresci, G.; Feruglio, C.; Fiore, F.; Georgakakis, A.; Harrison, Chris; Lamastra, Alessandra; Lamperti, Isabella; Lanzuisi, G.; Mannucci, F.; Marconi, A.; Menci, Nicola; Merloni, A.; Netzer, H.; Padovani, P.; Piconcelli, E.; Puglisi, A.; Salvato, M.; Scholtz, J.; Schramm, Malte; Silverman, J.; Vignali, C.; Zamorani, G.; Zappacosta, L.

doi:10.18727/0722-6691/5222

Cited by 2 publications

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“…The sample in this study is part of the SINFONI surv e y for Unveiling the Physics and Effect of Radiative feedback (see Circosta et al 2018 ;Kakkad et al 2020 ;Mainieri et al 2021 ). SUPER is an ESO large programme with the SINFONI instrument on board the VLT (Eisenhauer et al 2003 ) designed to characterize the properties of outflows in the ionized gas phase and their impact on host galaxies in a sample of 39 X-ray selected AGN at z ∼ 2 in AGN host galaxies at z ∼ 2.…”

Section: S a M P L E O B S E Rvat I O N S A N D Data R E D U C T I O Nmentioning

confidence: 99%

SUPER VII. morphology and kinematics of H α emission in AGN host galaxies at cosmic noon using SINFONI

Kakkad

Mainieri

Vietri

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We present spatially resolved Hα properties of 21 type 1 AGN host galaxies at z∼2 derived from the SUPER survey. These targets were observed with the adaptive optics capabilities of the SINFONI spectrograph, a near-infrared integral field spectrograph, that provided a median spatial resolution of 0.3″ (∼2 kpc). We model the Hα emission line profile in each pixel to investigate whether it traces gas in the narrow line region or if it is associated with star formation. To do this, we first investigate the presence of resolved Hα emission by removing the contribution of the AGN PSF. We find extended Hα emission in sixteen out of the 21 type 1 AGN host galaxies (76%). Based on the BPT diagnostics, optical line flux ratios and the line widths (FWHM), we show that the Hα emission in five galaxies is ionised by the AGN (30%), in four galaxies by star formation (25%) and for the rest (45%), the ionisation source is unconstrained. Two galaxies show extended Hα FWHM >600 km/s, which is interpreted as a part of an AGN-driven outflow. Morphological and kinematic maps of Hα emission in targets with sufficient signal-to-noise ratio suggest the presence of rotationally supported disks in six galaxies and possible presence of companions in four galaxies. In two galaxies, we find an anti-correlation between the locations of extended Hα emission and [O iii]-based ionised outflows, indicating possible negative feedback at play. However, in the majority of galaxies, we do not find evidence of outflows impacting Hα based star formation.

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Section: S a M P L E O B S E Rvat I O N S A N D Data R E D U C T I O Nmentioning

confidence: 99%

SUPER VII. morphology and kinematics of H α emission in AGN host galaxies at cosmic noon using SINFONI

Kakkad

Mainieri

Vietri

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Quasar feedback survey: molecular gas affected by central outflows and by ∼10-kpc radio lobes reveal dual feedback effects in ‘radio quiet’ quasars

Girdhar,

Harrison,

Mainieri

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We present a study of molecular gas, traced via CO (3–2) from ALMA data, of four z<0.2, ‘radio quiet’, type 2 quasars (Lbol ∼ 1045.3 − 46.2 erg s−1; L1.4 GHz ∼ 1023.7 − 24.3 W Hz−1). Targets were selected to have extended radio lobes (≥ 10 kpc), and compact, moderate-power jets (1–10 kpc; Pjet ∼ 1043.2 − 43.7 erg s−1). All targets show evidence of central molecular outflows, or injected turbulence, within the gas disks (traced via high-velocity wing components in CO emission-line profiles). The inferred velocities (Vout=250 – 440 km s−1) and spatial scales (0.6 – 1.6 kpc), are consistent with those of other samples of luminous low-redshift AGN. In two targets, we observe extended molecular gas structures beyond the central disks, containing 9 – 53 % of the total molecular gas mass. These structures tend to be elongated, extending from the core, and wrap-around (or along) the radio lobes. Their properties are similar to the molecular gas filaments observed around radio lobes of, mostly ‘radio loud’, Brightest Cluster Galaxies. They have: projected distances of 5 – 13 kpc; bulk velocities of 100 –340 km s−1; velocity dispersion of 30 – 130 km s−1; inferred mass outflow rates of 4 – 20 M⊙ yr−1; and estimated kinetic powers of 1040.3 − 41.7 erg s−1. Our observations are consistent with simulations that suggest moderate-power jets can have a direct (but modest) impact on molecular gas on small scales, through direct jet-cloud interactions. Then, on larger scales, jet-cocoons can push gas aside. Both processes could contribute to the long-term regulation of star formation.

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SUPER — AGN Feedback at Cosmic Noon: a Multi-phase and Multi-scale Challenge

Cited by 2 publications

References 0 publications

SUPER VII. morphology and kinematics of H α emission in AGN host galaxies at cosmic noon using SINFONI

SUPER VII. morphology and kinematics of H α emission in AGN host galaxies at cosmic noon using SINFONI

Quasar feedback survey: molecular gas affected by central outflows and by ∼10-kpc radio lobes reveal dual feedback effects in ‘radio quiet’ quasars

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