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

Kakkad, D.; Mainieri, V.; Vietri, G.; Lamperti, Isabella; Carniani, Stefano; Cresci, G.; Harrison, C. M.; Marconi, A.; Bischetti, M.; Cicone, C.; Circosta, C.; Man, Allison; Mannucci, F.; Netzer, H.; Padovani, P.; Perna, M.; Puglisi, A.; Scholtz, J.; Tozzi, G.; Vignali, C.; Zappacosta, L.

doi:10.1093/mnras/stad439

Cited by 8 publications

(3 citation statements)

References 129 publications

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“…To do so we used the PSF-subtraction method proposed in Carniani et al (2013) and applied in several studies (e.g., Carniani et al 2015;Kakkad et al 2020Kakkad et al , 2023. This method consists of comparing the observed spectra across the MEGARA FOV with the spectrum extracted at the AGN position.…”

Section: A Spatially Resolved Analysismentioning

confidence: 99%

Multiphase characterization of AGN winds in five local type-2 quasars

Speranza,

Ramos Almeida,

Acosta-Pulido

et al. 2024

A&A

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We present MEGARA integral field unit (IFU) observations of five local type-2 quasars (QSO2s, z $ 0.1$) from the Quasar Feedback (QSOFEED) sample. These active galactic nuclei (AGN) have bolometric luminosities of $ erg s$^ $ and stellar masses of sim 1011 M$_ sun $. The LR-V grating of MEGARA allows us to explore the kinematics of the ionized gas through the O III lambda 5007 AA emission line. The nuclear spectra of the five QSO2s, extracted in a circular aperture of $ (sim 2.2 kpc) in diameter, matching the resolution of these seeing-limited observations, show signatures of high velocity winds in the form of broad (full width at half maximum, 1300leq FWHMleq 2240 and blueshifted components. We found that four out of the five QSO2s present outflows that we can resolve with our seeing-limited data, and they have radii ranging from 3.1 to 12.6 kpc. In the case of the two QSO2s with extended radio emission, we found that it is well aligned with the outflows, suggesting that low-power jets might be compressing and accelerating the ionized gas in these radio-quiet QSO2s. In the four QSO2s with spatially resolved outflows, we measured ionized mass outflow rates of 3.3-6.5 M$_ $ when we used S II -based densities, and of 0.7-1.6 M$_ $ when trans-auroral line-based densities were considered instead. We compared them with the corresponding molecular mass outflow rates (8 - 16 M$_ $), derived from CO(2-1) ALMA observations at 0.2 resolution. The cold molecular outflows carry more mass than their ionized counterparts. However, both phases show lower outflow mass rates than those expected from observational scaling relations where uniform assumptions on the outflow properties were adopted. This might be indicating that the AGN luminosity is not the only driver of massive outflows and/or that these relations need to be rescaled using accurate outflow properties (i.e., electron density and radius). We did not find a significant impact of the outflows on the global star formation rates when considering the energy budget of the molecular and ionized outflows together. However, spatially resolved measurements of recent star formation in these targets are needed in order to evaluate this fairly, considering the dynamical timescales of the outflows, of 3-20 Myr for the ionized gas and 1-10 Myr for the molecular gas.

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Section: A Spatially Resolved Analysismentioning

confidence: 99%

Multiphase characterization of AGN winds in five local type-2 quasars

Speranza,

Ramos Almeida,

Acosta-Pulido

et al. 2024

A&A

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“…It seems now clear that outflows (OFs) are ubiquitous in active galactic nuclei (AGN; Woo et al 2016;Fiore et al 2017;Cresci & Maiolino 2018;Torres-Papaqui et al 2020). However, what role these OFs play in the evolution of the AGN host galaxies is still an open question, as multifrequency observations are difficult to interpret when following one unifying model (Harrison et al 2018;Smirnova-Pinchukova et al 2022;Harrison et al 2023;Speranza et al 2024) and evidence of feedback is either negative (Chen et al 2019;Shimizu et al 2019;Shin et al 2019;Torres-Papaqui et al 2020;Ruschel-Dutra et al 2021;Molina et al 2022;Tripodi et al 2022;Kakkad et al 2023) or ambiguous (Fluetsch et al 2019;Scholtz et al 2020;Wylezalek et al 2020;Luo et al 2021;Tamhane et al 2022;Kharb & Silpa 2023;Kim et al 2023;Salomé et al 2023;Veilleux et al 2023).…”

Section: Introductionmentioning

confidence: 99%

The Role of Active Galactic Nucleus Winds in Galaxy Formation: Connecting AGN Outflows at Low Redshifts to the Formation/Evolution of Their Host Galaxies

Torres-Papaqui,

Coziol,

Robleto-Orús

et al. 2024

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Using Sloan Digital Sky Survey (SDSS) spectra, we applied an automatic method to search for outflows (OFs) in three large samples of narrow-line active galactic nuclei (AGN) at low redshifts (z < 0.4), separated into three spectral activity classes: radio-loud galaxies (RGs), 15,793; radio-quiet Seyfert 2 AGN (Sy2), 18,585; and LINERs, 25,656. In general, the probability of detecting an OF decreases along the sequence Sy1→Sy2→LINER/RG and independently of the AGN class, the wind velocity, traced by W80, increases with the AGN luminosity. Moreover W80 is systematically higher in RGs or any of the other AGN classes when detected in radio. These results support the idea that there are two main modes of production of OF, the radiative mode dominant in radio-quiet AGN and the jet mode dominant in RGs, although both modes could also happen simultaneously at different levels. From the spectra and SDSS photometry, the characteristics of the AGN host galaxies and their supermassive black holes (SMBHs) were also retrieved using the stellar population synthesis code STARLIGHT. This revealed that, independently of the AGN spectral class, (1) galaxy hosts with OFs have systematically later morphological types and higher star formation rates (SFRs) than their counterparts without OF, (2) the AGN occupy different positions in the specific diagnostic diagram (specific black hole accretion rate (sBHAR) versus specific SFR), which suggests they follow different evolutionary paths congruent with the morphology of their galaxy hosts, and (3) they show no evidence of AGN quenching or triggering of star formation. These results are consistent with a scenario explaining the different AGN classes as consequences of different formation processes of galaxies: early-type galaxies (LINERs and RGs) formed bigger bulges and more massive SMBHs, exhausting their reservoir of gas more rapidly than late-type galaxies (Sy2 and Sy1), and thereby quenching their star formation and starving their SMBHs.

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“…Other studies focused on resolving detailed geometries of the outflows in individual nearby AGNs with high spatial resolution and large field-of-view (FoV) IFU instruments such as Multi Unit Spectroscopic Explorer on the Very Large Telescope (Mingozzi et al 2019;Shin et al 2021;Juneau et al 2022). Recently, high-resolution near-infrared (NIR) IFU data using adaptive optics or James Webb Space Telescope revealed extreme ionized outflows in luminous quasars at cosmic noon (Kakkad et al 2020(Kakkad et al , 2023Vayner et al 2021Vayner et al , 2023Wylezalek et al 2022;Cresci et al 2023;Veilleux et al 2023).…”

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confidence: 99%

Unraveling the Complex Structure of AGN-driven Outflows. VI. Strong Ionized Outflows in Type 1 AGNs and the Outflow Size–Luminosity Relation

Kim,

Woo,

Luo

et al. 2023

ApJ

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We present spatially resolved gas kinematics, ionization, and energetics of 11 type 1 and 5 type 2 active galactic nuclei (AGNs) with strong ionized gas outflows at z <0.3 using Gemini Multi-Object Spectrograph Integral Field Unit data. We find a strongly blueshifted region in [O iii] velocity maps, representing an approaching cone in biconical outflows, and blueshifted and redshifted regions in Hα velocity maps, which show gravitationally rotating kinematics. AGN photoionization is dominant in the central region of most targets, and some of them also show ring-like structures of LINER or composite that surround the AGN-dominated center. Following our previous studies, we kinematically determine outflow sizes by the ratio between [O iii] and stellar velocity dispersion. Outflow sizes of type 1 AGNs follow the same kinematic outflow size–[O iii] luminosity relation obtained from the type 2 Integral Field Unit sample in Kang & Woo and Luo (updated slope 0.29 ± 0.04), while they are limited to the central kiloparsec scales, indicating the lack of global impact of outflows on the interstellar medium. Small mass outflow rates and large star formation rates of the combined sample support that there is no evidence of rapid star formation quenching by outflows, which is consistent with the delayed AGN feedback.

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

Cited by 8 publications

References 129 publications

Multiphase characterization of AGN winds in five local type-2 quasars

Multiphase characterization of AGN winds in five local type-2 quasars

The Role of Active Galactic Nucleus Winds in Galaxy Formation: Connecting AGN Outflows at Low Redshifts to the Formation/Evolution of Their Host Galaxies

Unraveling the Complex Structure of AGN-driven Outflows. VI. Strong Ionized Outflows in Type 1 AGNs and the Outflow Size–Luminosity Relation

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