Multiphase Powerful Outflows Detected in High-z Quasars

Chartas, G.; Cappi, M.; Vignali, C.; Dadina, M.; James, Vincent; Lanzuisi, G.; Giustini, M.; Gaspari, M.; Strickland, S.; Bertola, E.

doi:10.3847/1538-4357/ac0ef2

Cited by 34 publications

(37 citation statements)

References 106 publications

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“…This scaling is significantly different from the one often assumed in models of AGN feedback used in cosmological simulations of galaxy formation, where the energy injection rate is assumed to be proportional to the mass accretion rate and hence to the bolometric luminosity (Schaye et al 2015;Weinberger et al 2017;Davé et al 2019). However, it is consistent with the results found in the hydrodynamical simulations of Nomura & Ohsuga (2017) and with current observational constraints (Gofford et al 2015;Chartas et al 2021).…”

Section: Dependence On Bh Mass and Mass Accretion Ratesupporting

confidence: 92%

Qwind3: UV line-driven accretion disc wind models for AGN feedback

Quera-Bofarull¹,

Done²,

Lacey³

et al. 2021

Preprint

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The ultraviolet (UV) bright accretion disc in active galactic nuclei (AGN) should give rise to line driving, producing a powerful wind which may play an important role in AGN feedback as well as in producing structures like the broad line region. However, coupled radiationhydrodynamics codes are complex and expensive, so we calculate the winds instead using a non-hydrodynamical approach (the Q framework). The original Q model assumed the initial conditions in the wind, and had only simple radiation transport. Here, we present an improved version which derives the wind initial conditions and has significantly improved ray-tracing to calculate the wind absorption self consistently given the extended nature of the UV emission. We also correct the radiation flux for relativistic effects, and assess the impact of this on the wind velocity. These changes mean the model is more physical, so its predictions are more robust. We find that, even when accounting for relativistic effects, winds can regularly achieve velocities (0.1 − 0.5) 𝑐, and carry mass loss rates which can be up to 30% of the accreted mass for black hole masses of 10 7−9 M , and mass accretion rates of 50% of the Eddington rate. Overall, the wind power scales as a power law with the black hole mass accretion rate, unlike the weaker scaling generally assumed in current cosmological simulations that include AGN feedback. The updated code, Q 3, is publicly available in GitHub †.

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Section: Dependence On Bh Mass and Mass Accretion Ratesupporting

confidence: 92%

Qwind3: UV line-driven accretion disc wind models for AGN feedback

Quera-Bofarull¹,

Done²,

Lacey³

et al. 2021

Preprint

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“…More recently, on 2016 January 13, SDSS J1353+1138 was observed with XMM-Newton . The analysis of the X-ray spectrum (Chartas et al 2021) revealed a significant absorption at ∼ 6.8 keV (consistent with Fe XXV), indicating the presence of a ∼ 0.31c UFO.…”

Section: Sdss J1353+1138mentioning

confidence: 64%

“…Our sample consists of two z ∼ 1.5 multiple lensed QSOs, HS 0810+2554 and SDSS J1353+1138, observed with the Spectrograph for INtegral Field Observations in the Near Infrared (SINFONI, Eisenhauer et al 2003) at the ESO Very Large Telescope (VLT) Unit Telescope 3 (UT3) within the framework of the program 0102.B-0377(A) (PI: G. Cresci). These objects were specifically selected as they are known to host UFOs (Chartas et al 2016;Chartas et al 2021) and to be at redshifts (z ∼ 1.5 and z ∼ 1.6 for HS 0810+2554 and SDSS J1353+1138, respectively), such that the optical rest-frame emission (tracing ionised outflows) falls in the range of wavelengths observed by SIN-FONI, namely, in the near-IR J-band (λ ∼ 1.1 − 1.4 µm). Consequently, this selection in redshifts corresponds to study objects at epochs close to the peak of AGN activity (z ∼ 2).…”

Section: Selection Of Targetsmentioning

confidence: 99%

“…Consequently, this selection in redshifts corresponds to study objects at epochs close to the peak of AGN activity (z ∼ 2). In total, there are fourteen high redshift (z > 1) QSOs with UFO detection, of which seven are found in the literature (among them, HS 0810+2554; see Dadina et al 2018 for an updated list), while the rest have not yet been published (including SDSS J1353+1138; Chartas et al 2021). These are among the brightest -in terms of 2-10 keV luminosity (L 2−10 keV > 10 45 erg s −1 , except for PID352 L 2−10 keV ∼ 10 44 erg s −1 ) -QSOs at high redshift; this is either because they are intrinsically luminous (of the total 14-QSO sample, only HS 1700+6416 and PID352; Lanzuisi et al 2012;Vignali et al 2015) or because they are subject to gravitational lens magnification (including APM 08279+5255, PG1115+080, H1413+117, HS 0810+2554 and MG J0414+0534 1 ; Hasinger et al 2002;Chartas et al 2003Chartas et al , 2007Chartas et al , 2009Chartas et al , 2016Dadina et al 2018).…”

Section: Selection Of Targetsmentioning

confidence: 99%

“…Moving to high redshifts (z > 1), the UFO detection is hampered by the resolution or sensitivity limits of the current observational facilities. In fact, the number of AGN hosting UFOs at z > 1 that have been discovered thus far drastically decreases to 14 objects (see Dadina et al 2018 on the list of published objects, and Chartas et al 2021 for the latest updates); of these, twelve are gravitationally lensed systems (Hasinger et al 2002;Chartas et al 2003Chartas et al , 2007Chartas et al , 2009Chartas et al , 2016Dadina et al 2018;Chartas et al 2021). Strong gravitational lensing is indeed a well-known, powerful tool to investigate the physical properties of distant quasars (QSOs).…”

Section: Introductionmentioning

confidence: 99%

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Connecting X-ray nuclear winds with galaxy-scale ionised outflows in two $z\sim1.5$ lensed quasars

Tozzi,

Cresci,

Marasco

et al. 2021

Preprint

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Aims. Outflows driven by active galactic nuclei (AGN) are expected to have a significant impact on host galaxy evolution, but the matter of how they are accelerated and propagated on galaxy-wide scales is still under debate. This work addresses these questions by studying the link between X-ray, nuclear ultra-fast outflows (UFOs), and extended ionised outflows, for the first time, in two quasars close to the peak of AGN activity (z ∼ 2), where AGN feedback is expected to be more effective. Methods. Our selected targets, HS 0810+2554 and SDSS J1353+1138, are two multiple-lensed quasars at z ∼ 1.5 with UFO detection that have been observed with the near-IR integral field spectrometer SINFONI at the VLT. We performed a kinematical analysis of the [O III]λ5007 optical emission line to trace the presence of ionised outflows. Results. We detected spatially resolved ionised outflows in both galaxies, extended more than 8 kpc and moving up to v > 2000 km/s. We derived mass outflow rates of ∼12 M yr −1 and ∼2 M yr −1 for HS 0810+2554 and SDSS J1353+1138. Conclusions. Compared with the co-hosted UFO energetics, the ionised outflow energetics in HS 0810+2554 is broadly consistent with a momentum-driven regime of wind propagation, whereas in SDSS J1353+1138, it differs by about two orders of magnitude from theoretical predictions, requiring either a massive molecular outflow or a high variability of the AGN activity to account for such a discrepancy. By additionally considering our results together with those from the small sample of well-studied objects (all local but one) having both UFO and extended (ionised, atomic, or molecular) outflow detections, we found that in 10 out of 12 galaxies, the large-scale outflow energetics is consistent with the theoretical predictions of either a momentum-or an energy-driven scenario of wind propagation. This suggests that such models explain the acceleration mechanism of AGN-driven winds on large scales relatively well.

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