Super

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

doi:10.1051/0004-6361/202038551

Cited by 101 publications

(137 citation statements)

References 149 publications

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“…The total on-source exposure time ranges from 1 hr up to 6 hr. We refer to Kakkad et al (2020) for a detailed description of the SINFONI data reduction, but below we report the main steps. We used the ESO pipeline (3.1.1) which returns science, PSF, and distortion-corrected and wavelength-calibrated telluric cubes.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…Fiore et al 2017), would require a much larger number of sources in order to place significant constraints on a possible existing correlation at lower luminosities. While we are using CIV to trace the AGN winds in the BLR, the main aim of our survey is to trace the AGN-driven outflows in the NLR using the [OIII] line (Kakkad et al 2020). It is therefore interesting to compare the properties of the winds traced at such different physical scales.…”

Section: Connection Between CIV Velocity Shift and Agn Propertiesmentioning

confidence: 99%

“…Furthermore, we also compare the kinematic properties of the CIV and [OIII] emission lines. We used the non-parametric definition v 10 , that is, the velocity of the [OIII] at 10% of the cumulative line flux, to trace the [OIII] outflow velocity (see Kakkad et al 2020).…”

Section: Connection Between CIV Velocity Shift and Agn Propertiesmentioning

confidence: 99%

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Super

Vietri

Mainieri

Kakkad

et al. 2020

A&A

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Aims. The SINFONI survey for Unveiling the Physics and Effect of Radiative feedback (SUPER) was designed to conduct a blind search for AGN-driven outflows on X-ray-selected AGNs at redshift z ∼ 2 with high (∼2 kpc) spatial resolution, and to correlate them with the properties of their host galaxy and central black hole. The main aims of this paper are: (a) to derive reliable estimates for the masses of the black holes and accretion rates for the Type-1 AGNs in this survey; and (b) to characterise the properties of the AGN-driven winds in the broad line region (BLR). Methods. We analysed rest-frame optical and UV spectra of 21 Type-1 AGNs. We used Hα, Hβ, and MgII line profiles to estimate the masses of the black holes. We used the blueshift of the CIV line profile to trace the presence of winds in the BLR. Results. We find that the Hα and Hβ line widths are strongly correlated, as is the line continuum luminosity at 5100 Å with Hα line luminosity, resulting in a well-defined correlation between black hole masses estimated from Hα and Hβ. Using these lines, we estimate that the black hole masses for our objects are in the range Log (MBH/M⊙) = 8.4–10.8 and are accreting at λEdd = 0.04–1.3. Furthermore, we confirm the well-known finding that the CIV line width does not correlate with the Balmer lines and the peak of the line profile is blueshifted with respect to the [OIII]-based systemic redshift. These findings support the idea that the CIV line is tracing outflowing gas in the BLR for which we estimated velocities up to ∼4700 km s−1. We confirm the strong dependence of the BLR wind velocity on the UV-to-X-ray continuum slope, the bolometric luminosity, and Eddington ratio. We infer BLR mass outflow rates in the range 0.005–3 M⊙ yr−1, revealing a correlation with the bolometric luminosity consistent with that observed for ionised winds in the narrow line region (NLR), and X-ray winds detected in local AGNs, and kinetic power ∼10−7 − 10−4 × LBol. The coupling efficiencies predicted by AGN-feedback models are much higher than the values reported for the BLR winds in the SUPER sample; although it should be noted that only a fraction of the energy injected by the AGN into the surrounding medium is expected to become kinetic power in the outflow. Finally, we find an anti-correlation between the equivalent width of the [OIII] line and the CIV velocity shift, and a positive correlation between this latter parameter and [OIII] outflow velocity. These findings, for the first time in an unbiased sample of AGNs at z ∼ 2, support a scenario where BLR winds are connected to galaxy-scale detected outflows, and are therefore capable of affecting the gas in the NLR located at kiloparsec scale distances.

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Section: Observations and Data Reductionmentioning

confidence: 99%

Section: Connection Between CIV Velocity Shift and Agn Propertiesmentioning

confidence: 99%

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Super

Vietri

Mainieri

Kakkad

et al. 2020

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“…Although the observational constraints provided by current facilities are limited, they indeed suggest that galaxy-scale winds are highly prevalent at the peak of SF (z ∼ 1−3; e.g. Genzel et al 2014;Brusa et al 2015;Carniani et al 2016;Föerster-Schreiber et al 2018;Villar Martín et al 2020;Kakkad et al 2020), and may be extremely powerful at very early epochs (e.g. Maiolino et al 2012;Bischetti et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Physics of ULIRGs with MUSE and ALMA: The PUMA project

Perna

Arribas

Pereira-Santaella

et al. 2021

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Context. Ultraluminous infrared galaxies (ULIRGs) are characterised by extreme starburst (SB) and active galactic nucleus (AGN) activity, and are therefore ideal laboratories for studying the outflow phenomena and their feedback effects. We have recently started a project called Physics of ULIRGs with MUSE and ALMA (PUMA), which is a survey of 25 nearby (z < 0.165) ULIRGs observed with the integral field spectrograph MUSE and the interferometer ALMA. This sample includes systems with both AGN and SB nuclear activity in the pre-and post-coalescence phases of major mergers. Aims. The main goals of the project are (i) to study the prevalence of (ionised, neutral, and molecular) outflows as a function of the galaxy properties, (ii) to constrain the driving mechanisms of the outflows (e.g. distinguish between SB and AGN winds), and (iii) to identify and characterise feedback effects on the host galaxy. In this first paper, we present details on the sample selection, MUSE observations, and data reduction, and derive first high-level data products. Methods. MUSE data cubes were analysed to study the dynamical status of each of the 21 ULIRGs observed so far, taking the stellar kinematics and the morphological properties inferred from MUSE narrow-band images into account. We also located the ULIRG nuclei, taking advantage of near-infrared (HST) and millimeter (ALMA) data, and studied their optical spectra to infer (i) the ionisation state through standard optical line ratio diagnostics, and (ii) outflows in both atomic ionised ([O III], Hα) and neutral (Na ID) gas. Results. We show that the morphological and stellar kinematic classifications are consistent: post-coalescence systems are more likely associated with ordered motions, while interacting (binary) systems are dominated by non-ordered and streaming motions. We also find broad and asymmetric [O III] and Na ID profiles in almost all nuclear spectra, with line widths in the range [300 − 2000] km/s, possibly associated with AGN-and SB-driven winds. This result reinforces previous findings that indicated that outflows are ubiquitous during the pre-and post-coalescence phases of major mergers.

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“…We now move to trace the kinematics of the ionized gas on kpc scales using the [OIII]λ5007 line sampled with AO-assisted SINFONI observations in the H band (Kakkad et al 2020). As it is detailed in the Kakkad et al contribution to these proceedings, we first verified that the [OIII] emission was actually extended taking into account beam smearing effects (Husemann et al 2016;Villar-Martin et al 2016).…”

Section: Nlr Windsmentioning

confidence: 76%