Ionized-gas Kinematics Along the Large-scale Radio Jets in Type-2 AGNs

Le, Huynh Anh N.; Woo, Jong-Hak; Son, Donghoon; Karouzos, Marios; Chung, Aeree; Tremou, Evangelia; Hwang, Narae; Park, Byeong Gon

doi:10.3847/1538-4357/aa9656

“…This is supported by the 'FIRST Classifier' (Alhassan et al 2018), which automatically identifies FIRST sources as compact or not, and determines that all of our sources are compact except for J1430+1339. This cautions against only relying on low-resolution radio data to identify low power/compact radio structures not associated with star formation in such systems (e.g., see Kimball et al 2011;Le et al 2017).…”

Section: Properties Of the Observed Radio Emissionmentioning

confidence: 99%

Prevalence of radio jets associated with galactic outflows and feedback from quasars

Jarvis

¹

,

Harrison

²

,

Thomson

³

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present 1-7 GHz high-resolution radio imaging (VLA and e-MERLIN) and spatially-resolved ionized gas kinematics for ten z < 0.2 type 2 'obscured' quasars (log[L AGN /erg s −1 ] 45) with moderate radio luminosities (log[L 1.4 GHz /W Hz −1 ]=23.3-24.4). These targets were selected to have known ionized outflows based on broad [O iii] emission-line components (FWHM≈800-1800 km s −1 ). Although 'radio-quiet' and not 'radio AGN' by many traditional criteria, we show that for nine of the targets, star formation likely accounts for 10 per cent of the radio emission. We find that ∼80-90 per cent of these nine targets exhibit extended radio structures on 1-25 kpc scales. The quasars' radio morphologies, spectral indices and position on the radio size-luminosity relationship reveals that these sources are consistent with being low power compact radio galaxies. Therefore, we favour radio jets as dominating the radio emission in the majority of these quasars. The radio jets we observe are associated with morphologically and kinematically distinct features in the ionized gas, such as increased turbulence and outflowing bubbles, revealing jetgas interaction on galactic scales. Importantly, such conclusions could not have been drawn from current low-resolution radio surveys such as FIRST. Our observations support a scenario where compact radio jets, with modest radio luminosities, are a crucial feedback mechanism for massive galaxies during a quasar phase.

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“…σ [OIII,out] is often considered as a tracer of outflow signatures in AGNs (e.g., Greene & Ho 2005a;Bae & Woo 2014;Woo et al 2016;Le et al 2017). In our analysis, we determined the outflow strengths of our sample such as σ [OIII,out] and V max .…”

Section: Maximum Outflow Velocitymentioning

confidence: 99%

“…This angular size is well defined within the SDSS aperture size. Following their method, we estimated the NLR size for our local SDSS and high redshift samples by using the size-luminosity relation (e.g., Bae et al 2017;Le et al 2017). Based on the bolometric luminosity of our sample, we estimated the [O III] luminosity of our local SDSS and high redshift samples to be in the range of L OIII ∼ 10 41.5 -10 43 erg s −1 (L bol = 700 × L OIII , LaMassa et al 2009).…”

Section: Aperture and Rotational Broadening Effectsmentioning

confidence: 99%

“…Thus, the [O III] emission line plays an important role in the study of cosmic evolution between M BH and their host galaxies. However, some studies have also found that the [O III] emission line often shows an asymmetric profile (e.g., the blue wing component), which could be interpreted as signatures of the nongravitational potential such as outflows (e.g., Heckman et al 1984;Bae & Woo 2014;Woo et al 2016;Le et al 2017). Because of this, some studies have suggested using only the core component of the [O III] emission line (s [ ] O ,core III ) as a surrogate for σ * (e.g., Greene & Ho 2005a; Komossa & Xu 2007;Bennert et al 2018).…”

mentioning

confidence: 99%

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[O iii] 5007 Å Emission Line Width as a Surrogate for σ _∗ in Type 1 AGNs?

Le

¹

,

Xue

²

,

Lin

³

et al. 2023

ApJ

Self Cite

1

0

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We present a study of the relation between the [O iii] 5007 Å emission line width (σ [OIII]) and stellar velocity dispersion (σ *), utilizing a sample of 740 type 1 active galactic nuclei (AGNs) with high-quality spectra at redshift z < 1.0. We find the broad correlation between the core component of the [O iii] emission line width ( σ [ O III , core ] ) and σ * with a scatter of 0.11 dex for the low redshift (z < 0.1) sample; for redshift (0.3 < z < 1.0) AGNs, the scatter is larger, being 0.16 dex. We also find that the Eddington ratio (L bol/L Edd) may play an important role in the discrepancies between σ [ O III , core ] and σ *. As the L bol/L Edd increases, σ [ O III , core ] tends to be larger than σ *. By classifying our local sample with different minor-to-major axis ratios, we find that σ * is larger than σ [ O III , core ] for those edge-on spiral galaxies. In addition, we also find that the effects of outflow strength properties such as maximum outflow velocity ( V max ) and the broader component of the [O iii] emission line width and line shift (σ [OIII,out] and V [OIII,out]) may play a major role in the discrepancies between σ [ O III , core ] and σ *. The discrepancies between σ [ O III , core ] and σ * are larger when V max , V [OIII,out], and σ [OIII,out] increase. Our results show that the outflow strengths may have significant effects on the differences between narrow-line region gas and stellar kinematics in AGNs. We suggest that caution should be taken when using σ [ O III , core ] as a surrogate for σ *. In addition, the substitute of σ [ O III , core ] for σ * could be used only for low luminosity AGNs.

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“…Some studies have revealed that the fraction of galaxies hosting AGNs is higher in GV galaxies, compared to red sequence (RS) and blue cloud (BC) galaxies (e.g., Silverman et al 2008;Schawinski et al 2010;Wang et al 2017). However, most of the evidence about the AGN activities interacting with the star formation within these galaxies is indirect (e.g., Silk & Rees 1998;Ishibashi & Fabian 2012;Zubovas et al 2013;Cresci et al 2015;Le et al 2017aLe et al , 2017bShin et al 2019). If AGN feedback indeed drives the quenching within these galaxies, then the timescales that the central black holes remain active should be comparable to the color transition timescales of GV galaxies.…”

Section: Introductionmentioning

confidence: 99%

AGN Lifetimes in UV-selected Galaxies: A Clue to Supermassive Black Hole-galaxy Coevolution

Lin¹,

Xue²,

Fang³

et al. 2022

Res. Astron. Astrophys.

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The coevolution between supermassive black holes (SMBHs) and their host galaxies has been proposed for more than a decade, albeit with little direct evidence about black hole accretion activities regulating galaxy star formation at z > 1. In this paper, we study the lifetimes of X-ray active galactic nuclei (AGNs) in UV-selected red sequence (RS), blue cloud (BC) and green valley (GV) galaxies, finding that AGN accretion activities are most prominent in GV galaxies at z ∼ 1.5–2, compared with RS and BC galaxies. We also compare AGN accretion timescales with typical color transition timescales of UV-selected galaxies. We find that the lifetime of GV galaxies at z ∼ 1.5–2 is very close to the typical timescale when the AGNs residing in them stay in the high-accretion-rate mode at these redshifts; for BC galaxies, the consistency between the color transition timescale and the black hole strong accretion lifetime is more likely to happen at lower redshifts (z < 1). Our results support the scenario where AGN accretion activities govern UV color transitions of host galaxies, making galaxies and their central SMBHs coevolve with each other.

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Ionized-gas Kinematics Along the Large-scale Radio Jets in Type-2 AGNs

Cited by 8 publications

References 49 publications

Prevalence of radio jets associated with galactic outflows and feedback from quasars

Prevalence of radio jets associated with galactic outflows and feedback from quasars

[O iii] 5007 Å Emission Line Width as a Surrogate for σ _∗ in Type 1 AGNs?

AGN Lifetimes in UV-selected Galaxies: A Clue to Supermassive Black Hole-galaxy Coevolution

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Ionized-gas Kinematics Along the Large-scale Radio Jets in Type-2 AGNs

Cited by 8 publications

References 49 publications

Prevalence of radio jets associated with galactic outflows and feedback from quasars

Prevalence of radio jets associated with galactic outflows and feedback from quasars

[O iii] 5007 Å Emission Line Width as a Surrogate for σ ∗ in Type 1 AGNs?

AGN Lifetimes in UV-selected Galaxies: A Clue to Supermassive Black Hole-galaxy Coevolution

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Product

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[O iii] 5007 Å Emission Line Width as a Surrogate for σ _∗ in Type 1 AGNs?