A multi-epoch spectroscopic study of the BAL quasar APM 08279+5255

Saturni, Francesco Gabriele; Trèvese, D.; Vagnetti, F.; Perna, M.; Dadina, M.

doi:10.1051/0004-6361/201527152

Cited by 27 publications

(49 citation statements)

References 82 publications

(196 reference statements)

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“…The red channel is shortpassed to reject a large fraction of Meinel rovibrational emissions which grow rapidly at wavelengths longer than ∼ 700 nm. Quasar spectra were taken from: QSO J0831+5245 [79], QSO B0350-073 (SDSS DR14, [52]), and QSO B0422+004 [80]. The skyglow spectrum is from Ref.…”

Section: Discussionmentioning

confidence: 99%

Cosmic Bell Test Using Random Measurement Settings from High-Redshift Quasars

et al. 2018

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In this Letter, we present a cosmic Bell experiment with polarization-entangled photons, in which measurement settings were determined based on real-time measurements of the wavelength of photons from high-redshift quasars, whose light was emitted billions of years ago; the experiment simultaneously ensures locality. Assuming fair sampling for all detected photons and that the wavelength of the quasar photons had not been selectively altered or previewed between emission and detection, we observe statistically significant violation of Bell's inequality by 9.3 standard deviations, corresponding to an estimated p value of ≲7.4 × 10 −21 . This experiment pushes back to at least ∼7.8 Gyr ago the most recent time by which any local-realist influences could have exploited the "freedom-of-choice" loophole to engineer the observed Bell violation, excluding any such mechanism from 96% of the space-time volume of the past light cone of our experiment, extending from the big bang to today.

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Section: Discussionmentioning

confidence: 99%

Cosmic Bell Test Using Random Measurement Settings from High-Redshift Quasars

et al. 2018

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“…This technique combines the virial theorem with the BLR radius -luminosity relation (see e.g. Kaspi et al 2005;Bentz et al 2013;Saturni et al 2016), allowing an estimate of the black hole mass from measurements of the BLR line width and AGN luminosity. Different empirical relations have been calibrated in recent years (e.g.…”

Section: Nuclear Propertiesmentioning

confidence: 99%

An X-ray/SDSS sample

Perna

Lanzuisi

Brusa

et al. 2017

A&A

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Aims. The connection between the growth of super-massive black holes (SMBHs) and the evolution of their host galaxies is nowadays well established, although the underlying mechanisms explaining their mutual relations are still debated. Multi-phase fast, massive outflows have been postulated to play a crucial role in this process. The aim of this work is to constrain the nature and the fraction of outflowing gas in active galactic nuclei (AGNs) as well as the nuclear conditions possibly at the origin of such phenomena. Methods. We present a large spectroscopic sample of X-ray detected SDSS AGNs at z < 0.8 with a high signal-to-noise ratio in the [O III]λ5007 line to unveil the faint wings of the emission profile associated with AGN-driven outflows. We used X-ray and optical flux ratio diagnostics to select the sample. We derived physical and kinematic characterization by re-analysing optical (and X-ray) spectra. Results. We derive the incidence of ionized (∼40%) and atomic (<1%) outflows covering a wide range of AGN bolometric luminosity from 10 42 to 10 46 erg/s. We also derive bolometric luminosities and X-ray bolometric corrections to test whether the presence of outflows is associated with an X-ray loudness, as suggested by our recent results obtained by studying high-z QSOs. Conclusions. We study the relations between the outflow velocity inferred from [O III] kinematic analysis and different AGN power tracers, such as black hole mass (M BH ), [O III], and X-ray luminosity. We show a well-defined positive trend between outflow velocity and L X , for the first time, over a range of 5 order of magnitudes. Overall, we find that in the QSO-luminosity regime and at M BH > 10 8 M the fraction of AGNs with outflows becomes >50%. Finally, we discuss our results about X-ray bolometric corrections and outflow incidence in cold and ionized phases in the context of an evolutionary sequence allowing two distinct stages for the feedback phase: first, an initial stage characterized by X-ray/optical obscured AGNs, in which the atomic gas is still present in the ISM and the outflow processes involve all the gas components and, second, a later stage associated with unobscured AGNs, in which the line of sight has been cleaned and the cold components have been heated or exhausted.

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“…Hence the black hole mass of APM 08279+5255 must be larger than 4 × 10 9 M⊙ even in the unlikely case that R is the same. While the upper limit of the magnification factor is estimated by the reverberation mapping (Saturni et al 2016), the lower limit is not. Here, we simply set a lower limit to be µ = 2 since no magnification µ = 1 seems to be unlikely for such a high luminosity object.…”

Section: Broadband Sed and Quasar Parametersmentioning

confidence: 99%

Revisiting the extremely fast disc wind in a gravitationally lensed quasar APM 08279+5255

Hagino

Done

Odaka

et al. 2017

Monthly Notices of the Royal Astronomical Society

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The gravitationally lensed quasar APM 08279+5255 has the fastest claimed wind from any AGN, with velocities of 0.6-0.7c, requiring magnetic acceleration as special relativisitic effects limit all radiatively driven winds to v<0.3-0.5c. However, this extreme velocity derives from interpreting both the narrow and broad absorption features in the X-ray spectrum as iron absorption lines. The classic ultrafast outflow source PDS 456 also shows similar absorption systems, but here the higher energy, broader feature is generally interpreted as an absorption edge. We reanalyse all the spectra from APM 08279+5255 using a full 3-dimensional Monte Carlo radiative transfer disc wind model for the ionised wind at 0.1-0.2c, together with complex absorption from lower ionisation material, and find that this is a better description of the data. Thus there is no strong requirement for outflow velocities beyond 0.2c, which can be powered by radiation driving. We show that UV line driving is especially likely given the spectral energy distribution of this source which is intrinsically UV bright and X-ray weak. While the peak of this emission is unobservable, it must be luminous enough to power the observed hot dust, favouring at least moderate black hole spin.

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A multi-epoch spectroscopic study of the BAL quasar APM 08279+5255

Cited by 27 publications

References 82 publications

Cosmic Bell Test Using Random Measurement Settings from High-Redshift Quasars

Cosmic Bell Test Using Random Measurement Settings from High-Redshift Quasars

An X-ray/SDSS sample

Revisiting the extremely fast disc wind in a gravitationally lensed quasar APM 08279+5255

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