BAT AGN Spectroscopic Survey – XIX. Type 1 versus type 2 AGN dichotomy from the point of view of ionized outflows

Rojas, A. F.; Sani, E.; Gavignaud, I.; Ricci, Cláudio; Lamperti, Isabella; Koss, Michael; Trakhtenbrot, Benny; Schawinski, Kevin; Oh, Kyuseok; Bauer, F. E.; Bischetti, M.; Boissay-Malaquin, Rozenn; Bongiorno, A.; Harrison, Fiona A.; Kakkad, D.; Masetti, N.; Ricci, F.; Shimizu, T.; Stalevski, Marko; Stern, Daniel; Vietri, G.

doi:10.1093/mnras/stz3386

Cited by 44 publications

(46 citation statements)

References 91 publications

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“…DiPompeo et al 2018, as well as lower luminosity local AGN samples (e.g. Rojas et al 2020). Additionally, our result provides an interesting connection to extremely red QSOs (ERQs), where very high [O iii] velocities of FWHM > 2000 km s −1 have been observed (Zakamska et al 2016;Hamann et al 2017;Mehdipour & Costantini 2018;Perrotta et al 2019;Temple et al 2019;Villar Martín et al 2020).…”

Section: The Origin Of Qso Reddening: the Dusty Wind Scenariosupporting

confidence: 67%

The multiwavelength properties of red QSOs: Evidence for dusty winds as the origin of QSO reddening

Rivera

Alexander

Rosario

et al. 2021

A&A

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Fundamental differences in the radio properties of red quasars (QSOs), as compared to blue QSOs, have been recently discovered, positioning them as a potential key population in the evolution of galaxies and black holes across cosmic time. To elucidate the nature of these objects, we exploited a rich compilation of broad-band photometry and spectroscopic data to model their spectral energy distributions (SEDs) from the ultraviolet to the far-infrared and characterise their emission-line properties. Following a systematic comparison approach, we characterise the properties of the QSO accretion, obscuration, and host galaxies in a sample of ∼1800 QSOs at 0.2 < z < 2.5, classified into red and control QSOs and matched in redshift and luminosity. We find no strong differences in the average multiwavelength SEDs of red and control QSOs, other than the reddening of the accretion disk expected by the colour selection. Additionally, no clear link can be recognised between the reddening of QSOs and the interstellar medium as well as star formation properties of their host galaxies. Our modelling of the infrared emission using dusty torus models suggests that the dust distributions and covering factors in red QSOs are strikingly similar to those of the control sample, inferring that the reddening is not related to the torus and orientation effects. Interestingly, we detect a significant excess of infrared emission at rest-frame 2−5 μm, which shows a direct correlation with optical reddening. To explain its origin, we investigated the presence of outflow signatures in the QSO spectra, discovering a higher incidence of broad [O III] wings and high C IV velocity shifts (> 1000 km s−1) in red QSOs as compared to the control sample. We find that red QSOs that exhibit evidence for high-velocity wind components present a stronger signature of the infrared excess, suggesting a causal connection between QSO reddening and the presence of hot dust distributions in QSO winds. We propose that dusty winds at nuclear scales are potentially the physical ingredient responsible for the optical colours in red QSOs, as well as a key parameter for the regulation of accretion material in the nucleus.

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Section: The Origin Of Qso Reddening: the Dusty Wind Scenariosupporting

confidence: 67%

The multiwavelength properties of red QSOs: Evidence for dusty winds as the origin of QSO reddening

Rivera

Alexander

Rosario

et al. 2021

A&A

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“…One option is to assume a spherically or biconically symmetric flow with constant velocity and uniform density up to a given radius (e.g. Cano-Díaz et al 2012;Brusa et al 2015;Bischetti et al 2017;Fiore et al 2017;Rojas et al 2020). In this scenario, the outflow rate decreases over time, and what one calculates is the initial outflow rate that is traced by the material at the maximum radius considered.…”

Section: O U T F L Ow M a S S A N D R At Ementioning

confidence: 99%

Ionized outflows in local luminous AGN: what are the real densities and outflow rates?

Davies

Baron

Shimizu

et al. 2020

Monthly Notices of the Royal Astronomical Society

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118

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We report on the determination of electron densities, and their impact on the outflow masses and rates, measured in the central few hundred parsecs of 11 local luminous active galaxies. We show that the peak of the integrated line emission in the AGN is significantly offset from the systemic velocity as traced by the stellar absorption features, indicating that the profiles are dominated by outflow. In contrast, matched inactive galaxies are characterised by a systemic peak and weaker outflow wing. We present three independent estimates of the electron density in these AGN, discussing the merits of the different methods. The electron density derived from the [SII] doublet is significantly lower than than that found with a method developed in the last decade using auroral and transauroral lines, as well as a recently introduced method based on the ionization parameter. The reason is that, for gas photoionized by an AGN, much of the [SII] emission arises in an extended partially ionized zone where the implicit assumption that the electron density traces the hydrogen density is invalid. We propose ways to deal with this situation and we derive the associated outflow rates for ionized gas, which are in the range 0.001–0.5 M⊙ yr−1 for our AGN sample. We compare these outflow rates to the relation between $\dot{M}_{\rm out}$ and LAGN in the literature, and argue that it may need to be modified and rescaled towards lower mass outflow rates.

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“…There are three common AGN classifications that are each observed to be X-ray faint: Type 2 (obscured) AGN, broad absorption line (BAL) quasars, and weak emission-line quasars (WLQs, with Lyα+N V equivalent widths of 10 Å). Type 2 AGN are not intrinsically X-ray weak relative to Type 1 AGN, but their soft X-ray flux is obscured by thick column densities (n H 10 22 cm −2 , e.g., Rojas et al 2020) to-noise ratios below 5, and those sources with X-ray spectral photon indices of Γ < 1.6, where the latter is indicative of obscuration (e.g., Ricci et al 2017). Although the unlensed value of J0100+2802 is consistent with the expectations of Lusso & Risaliti (2016), for the µ = 450 scenario, J0100+2802 resides on the extreme tail of the ∆α OX distribution.…”

Section: Is J0100+2802 X-ray Faint?mentioning

confidence: 99%

X-Ray Evidence Against the Hypothesis that the Hyper-Luminous z=6.3 Quasar J0100+2802 is Lensed

Connor,

Stern,

Bañados

et al. 2021

Preprint

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The z = 6.327 quasar SDSS J010013.02+280225.8 (hereafter J0100+2802) is believed to be powered by a black hole more massive than 10 10 M , making it the most massive black hole known in the first billion years of the Universe. However, recent high-resolution ALMA imaging shows four structures at the location of this quasar, potentially implying that it is lensed with a magnification of µ ∼ 450 and thus its black hole is significantly less massive. Furthermore, for the underlying distribution of magnifications of z 6 quasars to produce such an extreme value, theoretical models predict that a larger number of quasars in this epoch should be lensed, implying further overestimates of early black hole masses. To provide an independent constraint on the possibility that J0100+2802 is lensed, we re-analyzed archival XMM-Newton observations of the quasar and compared the expected ratios of X-ray luminosity to rest-frame UV and IR luminosities. For both cases, J0100+2802's X-ray flux is consistent with the no-lensing scenario; while this could be explained by J0100+2802 being Xray faint, we find it does not have the X-ray or optical spectral features expected for an X-ray faint quasar. Finally, we compare the overall distribution of X-ray fluxes for known, typical z 6 quasars. We find a 3σ tension between the observed and predicted X-ray-to-UV flux ratios when adopting the magnification probability distribution required to produce a µ = 450 quasar.

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BAT AGN Spectroscopic Survey – XIX. Type 1 versus type 2 AGN dichotomy from the point of view of ionized outflows

Cited by 44 publications

References 91 publications

The multiwavelength properties of red QSOs: Evidence for dusty winds as the origin of QSO reddening

The multiwavelength properties of red QSOs: Evidence for dusty winds as the origin of QSO reddening

Ionized outflows in local luminous AGN: what are the real densities and outflow rates?

X-Ray Evidence Against the Hypothesis that the Hyper-Luminous z=6.3 Quasar J0100+2802 is Lensed

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