Connection Between Mid-Infrared Emission Properties and Narrow-Line Region Outflows in Type 1 Active Galactic Nuclei

Zhang, Kai; Wang, Tinggui; Yan, Lin; Dong, Xiao-Bo

doi:10.1088/0004-637x/768/1/22

Cited by 17 publications

(17 citation statements)

References 63 publications

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“…In a forthcoming paper, we perform similar studies using BAL quasars (S. Zhang et al 2013 in preparation) and find significant correlations of β NIR with the velocities and absorption strength of BALs, in good agreement with the results presented here. One important question arises as to how the outflows relate to the hot dust in quasars.…”

Section: Summary and Discussionsupporting

confidence: 86%

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Outflow and Hot Dust Emission in High-Redshift Quasars

Wang

Xing

Zhang

et al. 2013

ApJ

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Correlations of hot dust emission with outflow properties are investigated, based on a large z∼ 2 non-broad absorption lines quasar sample built from the Wide-field Infrared Survey and the Sloan Digital Sky Survey data releases. We use the near infrared slope and the infrared to UV luminosity ratio to indicate the hot dust emission relative to the emission from the accretion disk. In our luminous quasars, these hot dust emission indicators are almost independent of the fundamental parameters, such as luminosity, Eddington ratio and black hole mass, but moderately dependent on the blueshift and asymmetry index (BAI) and full width at half-maximum (FWHM) of C IV lines. Interestingly, the latter two correlations dramatically strengthen with increasing Eddington ratio. We suggest that, in high Eddington ratio quasars, C IV regions are dominated by outflows so the BAI and FWHM(C IV) can reliably reflect the general properties and velocity of outflows, respectively. While in low Eddington ratio quasars, C IV lines are primarily emitted by virialized gas so the BAI and FWHM(C IV) become less sensitive to outflows. Therefore, the correlations for the highest Eddington ratio quasars are more likely to represent the true dependence of hot dust emission on outflows and the correlations for the entire sample are significantly diluted by the low Eddington ratio quasars. Our results show that an outflow with a large BAI or velocity can double the hot dust emission on average. We suggest that outflows either contain hot dust in themselves or interact with the dusty interstellar medium or torus.

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Section: Summary and Discussionsupporting

confidence: 86%

“…Recently, several works found interesting correlations between the outflow in narrow line region (NLR) and the mid-infrared emission(Zhang et al 2013;Hönig et al 2013). The outflows discussed here have much higher velocities than those in NLR.…”

mentioning

confidence: 99%

Outflow and Hot Dust Emission in High-Redshift Quasars

Wang

Xing

Zhang

et al. 2013

ApJ

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“…The sources in this sample have small contamination from host galaxies in their optical light, and their properties and data reduction are described in Dong et al (2011). Detailed analysis of narrow-line properties, especially the [O III]line, can be found in Zhang et al (2011Zhang et al ( , 2013aZhang et al ( , 2013b. The bolometric luminosity range of these sources is 10 44 -10 47 erg s −1…”

Section: Calibration Of the Kex Diagram Using Type 1 Agnsmentioning

confidence: 99%

A New Diagnostic Diagram of Ionization Sources for High-redshift Emission Line Galaxies

Zhang

Hao

2018

ApJ

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We propose a new diagram, the kinematics-excitation (KEx) diagram, which uses the [O III] λ5007/Hβ line ratio and the [O III] λ5007emission line width (σ [O III] ) to diagnose the ionization source and physical properties of active galactic nuclei (AGNs) and star-forming galaxies (SFGs). The KEx diagram is a suitable tool to classify emission line galaxies at intermediate redshift because it uses only the [O III] λ5007 and Hβ emission lines. We use the main galaxy sample of SDSS DR7 and the Baldwin−Phillips−Terlevich (BPT) diagnostic to calibrate the diagram at low redshift. The diagram can be divided into three regions: the KEx-AGN region, which consists mainly of pure AGNs, the KEx-composite region, which is dominated by composite galaxies, and the KEx-SFG region, which contains mostly SFGs. LINERs strongly overlap with the composite and AGN regions. AGNs are separated from SFGs in this diagram mainly because they preferentially reside in luminous and massive galaxies and have higher [O III]/Hβ than SFGs. The separation between AGNs and SFGs is even cleaner thanks to the additional 0.15/0.12dex offset in σ [O III] at fixed luminosity/stellar mass. We apply the KEx diagram to 7866 galaxies at 0.3<z<1 in the DEEP2 Galaxy Redshift Survey, and compare it to an independent X-ray classification scheme using Chandra observations. X-ray AGNs are mostly located in the KEx-AGN region, while X-ray SFGs are mostly located in the KEx-SFG region. Almost all Type 1 AGNs lie in the KEx-AGN region. These tests support the reliability of this classification diagram for emission line galaxies at intermediate redshift.At z∼2, the demarcation line between SFGs and AGNs is shifted by ∼0.3dex toward higher values of σ [O III] due to evolution effects.

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“…However, Zhang et al (2013) found that the ratio of the [O III] wing and the bolometric luminosity is correlated with the mid-infrared covering factor. The wing is believed to rise from turbulent polar outflows in the inner narrow-line region (Peng et al 2014), and thus they propose that this indicates that a considerable fraction of the warm dust producing mid-infrared emission in AGN is likely embedded in polar outflows.…”

Section: Polar Dustmentioning

confidence: 95%

“…Such sources are plenty (see e.g. Zhang et al 2013;Lyu & Rieke 2018), and unfortunately we have no way of estimating the polar dust contribution without careful spectral energy distribution (SED) modelling or direct high-resolution mid-infrared observations of the emitting region, since such data is not available. Moreover, there are indications that high Eddington ratio sources, such as NLS1s, have a tendency to show more polar dust (Leftley et al 2019).…”

Section: Polar Dustmentioning

confidence: 99%

Unravelling the origin of extended radio emission in narrow-line Seyfert 1 galaxies with the JVLA

Järvelä,

Dahale,

Crepaldi

et al. 2021

Preprint

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Narrow-line Seyfert 1 (NLS1) galaxies are believed to be active galactic nuclei (AGN) in the early stages of their evolution. Some dozens of them have been found to host relativistic jets, whilst the majority of NLS1s has not even been detected in radio, emphasising the heterogeneity of the class in this band. In this paper, our aim is to determine the predominant source of radio emission in a sample of 44 NLS1s, selected based on their extended kpc-scale radio morphologies at 5.2 GHz. We accomplish this by analysing their spatially resolved radio spectral index maps, centred at 5.2 GHz, as the spectral index carries information about the production mechanisms of the emission. In addition, we utilise several diagnostics based on mid-infrared emission to estimate the star formation activity of their host galaxies. These data are complemented by archival data to draw a more complete picture of each source. We find an extraordinary diversity among our sample. Approximately equal fractions (∼10-12 sources) of our sources can be identified as AGN-dominated, composite, and host-dominated. Among the AGN-dominated sources are a few NLS1s with very extended jets, reaching distances of tens of kpc from the nucleus. One of these, J0814+5609, hosts the most extended jets found in an NLS1 so far. We also identify five NLS1s that could be classified as compact steep-spectrum sources. In addition, one source shows a possible kpc-scale relic reaching well outside the host galaxy and restarted nuclear activity, and one could belong to the NLS1 subclass hosting relativistic jets that seems to be absorbed at lower radio frequencies (< 10 GHz). We further conclude that due to the variety seen in NLS1s simple proxies, such as the star formation diagnostics also employed in this paper, and the radio loudness parameter, are not ideal tools for characterising NLS1s. We emphasise the necessity of examining NLS1s as individuals, instead of making assumptions based on their classification. When these issues are properly taken into account, NLS1s offer an exceptional environment to study the interplay of the host galaxy and several AGN-related phenomena, such as jets and outflows.

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Connection Between Mid-Infrared Emission Properties and Narrow-Line Region Outflows in Type 1 Active Galactic Nuclei

Cited by 17 publications

References 63 publications

Outflow and Hot Dust Emission in High-Redshift Quasars

Outflow and Hot Dust Emission in High-Redshift Quasars

A New Diagnostic Diagram of Ionization Sources for High-redshift Emission Line Galaxies

Unravelling the origin of extended radio emission in narrow-line Seyfert 1 galaxies with the JVLA

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