A global view of the inner accretion and ejection flow around super massive black holes

Giustini, M.; Proga, Daniel

doi:10.1051/0004-6361/201833810

Cited by 161 publications

(149 citation statements)

References 212 publications

(242 reference statements)

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“…For the reasons discussed above, caution should be taken when interpreting the quantitative behaviour of f BAL but the behaviour is consistent with an increased probability a quasar with a given C iv EW is seen as a BAL as the C iv-emission outflow signature increases. This empirical observation may be further consistent with the theoretical wind model of Giustini & Proga (2019), where the probability of a quasar hosting a radiation line driven wind increases with increasing accretion rate and BH mass.…”

Section: IV Emission Line Profilesupporting

confidence: 87%

BAL and non-BAL quasars: continuum, emission, and absorption properties establish a common parent sample

Rankine

Hewett

Banerji

et al. 2020

Monthly Notices of the Royal Astronomical Society

123

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Using a sample of 144 000 quasars from the Sloan Digital Sky Survey data release 14 we investigate the outflow properties, evident both in absorption and emission, of high-ionization Broad Absorption Line (BAL) and non-BAL quasars with redshifts 1.6 z ≤ 3.5 and luminosities 45.3 < log 10 (L bol ) < 48.2 erg s −1 . Key to the investigation is a continuum and emission-line reconstruction scheme, based on meanfield independent component analysis, that allows the kinematic properties of the C ivλ1550 emission line to be compared directly for both non-BAL and BAL quasars. C iv-emission blueshift and equivalent-width (EW) measurements are thus available for both populations. Comparisons of the emission-line and BAL-trough properties reveal strong systematic correlations between the emission and absorption properties. The dependence of quantitative outflow indicators on physical properties such as quasar luminosity and luminosity relative to Eddington-luminosity are also shown to be essentially identical for the BAL and non-BAL populations. There is an absence of BALs in quasars with the hardest spectral energy distributions (SEDs), revealed by the presence of strong He iiλ1640 emission, large C ivλ1550-emission EW and no measurable blueshift. In the remainder of the C iv-emission blueshift versus EW space, BAL and non-BAL quasars are present at all locations; for every BAL-quasar it is possible to identify non-BAL quasars with the same emission-line outflow properties and SED-hardness. The co-location of BAL and non-BAL quasars as a function of emission-line outflow and physical properties is the key result of our investigation, demonstrating that (high-ionization) BALs and non-BALs represent different views of the same underlying quasar population.

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Section: IV Emission Line Profilesupporting

confidence: 87%

BAL and non-BAL quasars: continuum, emission, and absorption properties establish a common parent sample

Rankine

Hewett

Banerji

et al. 2020

Monthly Notices of the Royal Astronomical Society

123

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“…As the terminal velocity of the wind is inversely proportional to its launching distance from the central SMBH, a lower X-ray emission favours, in general, the launch of faster radiation-driven accretion disc winds, compared to a higher X-ray emission (see e.g. Giustini & Proga 2019, for a recent review).…”

Section: Relationmentioning

confidence: 99%

The WISSH quasars project

Zappacosta

Piconcelli

Giustini

et al. 2020

A&A

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Hyper-luminous quasars (Lbol ≳ 1047 erg s−1) are ideal laboratories to study the interaction and impact of the extreme radiative field and the most powerful winds in the active galactic nuclei (AGN) nuclear regions. They typically exhibit low coronal X-ray luminosity (LX) compared to the ultraviolet (UV) and mid-infrared (MIR) radiative outputs (LUV and LUV); a non-negligible fraction of them report even ∼1 dex weaker LX compared to the prediction of the well established LX–LUV and LX–LUV relations followed by the bulk of the AGN population. In our WISE/SDSS-selected Hyper-luminous (WISSH) z = 2 − 4 broad-line quasar sample, we report on the discovery of a dependence between the intrinsic 2–10 keV luminosity (L2 − 10) and the blueshifted velocity of the CIV emission line (vCIV) that is indicative of accretion disc winds. In particular, sources with the fastest winds (vCIV ≳ 3000 km s−1) possess ∼0.5–1 dex lower L2 − 10 than sources with negligible vCIV. No similar dependence is found on LUV, LUV, Lbol, the photon index, or the absorption column density. We interpret these findings in the context of accretion disc wind models. Both magnetohydrodynamic and line-driven models can qualitatively explain the reported relations as a consequence of X-ray shielding from the inner wind regions. In case of line-driven winds, the launch of fast winds is favoured by a reduced X-ray emission, and we speculate that these winds may play a role in directly limiting the coronal hard X-ray production.

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“…This is similar to the case of wind from hot accretion flows, except that the stop radius should be systematically smaller due to the smaller enthalpy of cold wind. Those with a small stop radius, i.e., the so-called "failed wind", are invoked to explain the origin of broad line region of AGNs by Giustini & Proga (2019).…”

Section: Winds From Hot Accretion Flow With Both Black Hole and Galaxmentioning

confidence: 99%

Large-scale Dynamics of Winds Originating from Black Hole Accretion Flows. I. Hydrodynamics

Cui

Yuan

2020

ApJ

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Winds from black hole accretion flows are ubiquitous. Previous works mainly focus on the launching of wind in the accretion flow scale. It still remains unclear how far the winds can propagate outward and what is their large-scale dynamics. As the first paper of this series, we study the large-scale dynamics of thermal wind beyond accretion scales via analytical and numerical methods. Boundary conditions, which are crucial to our problem, are analyzed and presented based on the small-scale simulations combined with observations of winds. Both black hole and galaxy potential are taken into account. For winds originated from hot accretion flows, we find that the wind can reach to large scales. The radial profiles of velocity, density, and temperature can be approximated by v r ≈ v r0 , ρ ≈ ρ 0 (r/r 0 ) −2 , and T ≈ T 0 (r/r 0 ) −2(γ−1) , where v r0 , ρ 0 , T 0 are the velocity, density, and temperature of winds at the boundary r 0 (≡ 10 3 r g ), γ is the polytropic index. During the outward propagation, the enthalpy and the rotational energy compensate the increase of gravitational potential. For thin disks, we find that because the Bernoulli parameter is smaller, winds cannot propagate as far as the hot winds, but stop at a certain radius where the Bernoulli parameter is equal to the potential energy. Before the winds stop, the profiles of dynamical quantities can also be approximated by the above relations. In this case the rotational energy alone compensates the increase of the potential energy.

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A global view of the inner accretion and ejection flow around super massive black holes

Cited by 161 publications

References 212 publications

BAL and non-BAL quasars: continuum, emission, and absorption properties establish a common parent sample

BAL and non-BAL quasars: continuum, emission, and absorption properties establish a common parent sample

The WISSH quasars project

Large-scale Dynamics of Winds Originating from Black Hole Accretion Flows. I. Hydrodynamics

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