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

Hagino, Kouichi; Done, Chris; Odaka, Hirokazu; Watanabe, Shin; Takahashi, Tadayuki

doi:10.1093/mnras/stx559

Cited by 30 publications

(30 citation statements)

References 69 publications

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“…Such an intermediate magnification factor is also in agreement with the upper limit of µ 8.2 derived by Saturni et al (2016) from the RM. We also note that a lower limit on APM 08279+5255 black hole mass M BH 4 × 10 9 M has been derived by Hagino et al (2017) through SED modeling. Using our fiducial luminosity and FWHM measurements for Mg II in Eq.…”

Section: Single-epoch Black Hole Mass Estimatesmentioning

confidence: 80%

“…Serendipitously discovered in a Galactic survey for cold carbon stars (Irwin et al 1998), it is archetypal to several categories of the quasar class, showing together many of the observational phenomena that can be found in such objects. In fact, beyond having evidence of both broad and intrinsic narrow (Ellison et al 2004) absorption features associated with the C IV λ1549 emission line, it also shows an uncommon O VI λ1030 BAL embedded in the Lyα forest (Hines et al 1999) and an X-ray ultra-fast outflow (UFO) associated to highly-ionized iron (Hasinger et al 2002;Chartas et al 2002;Saez et al 2009;Hagino et al 2017). Furthermore, its high-ionization emission lines, from Lyα to C III] λ1910, are characterized by a significant The reduced spectrum is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/617/A118 blueshift of ∼2500 km s −1 with respect to molecular (Downes et al 1999) and Balmer lines (Oyabu et al 2009).…”

Section: Introductionmentioning

confidence: 99%

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Restframe UV-to-optical spectroscopy of APM 08279+5255

Saturni

Bischetti

Piconcelli

et al. 2018

A&A

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We present the analysis of the restframe optical-to-UV spectrum of APM 08279+5255, a well-known lensed broad absorption line (BAL) quasar at z = 3.911. The spectroscopic data were taken with the optical DOLoRes and near-IR NICS instruments at TNG, and include the previously unexplored range between C III] λ1910 and [O III] λλ4959,5007. We have investigated the possible presence of multiple BALs by computing “balnicity” and absorption indexes (i.e., BI, BI0, and AI) for the transitions Si IV λ1400, C IV λ1549, Al III λ1860, and Mg II λ2800. No clear evidence for the presence of absorption features is found in addition to the already known, prominent BAL associated to C IV, which supports a high-ionization BAL classification for APM 08279+5255. We also studied the properties of the [O III], Hβ, and Mg II emission lines. We find that [O III] is intrinsically weak (F[OIII]∕FHβ ≲ 0.04), as it is typically found in luminous quasars with a strongly blueshifted C IV emission line (~2500 km s−1 for APM 08279+5255). We computed the single-epoch black hole mass based on Mg II and Hβ broad emission lines, finding MBH = (2 ÷ 3) × 1010μ−1 M⊙, with the magnification factor μ that can vary between 4 and 100 according to CO and restframe UV-to-mid-IR imaging respectively. Using a Mg II equivalent width (EW)-to-Eddington ratio relation, the EWMgII ~ 27 Å measured for APM 08279+5255 translates into an Eddington ratio of ~0.4, which is more consistent with μ = 4. This magnification factor also provides a value of MBH that is consistent with recent reverberation-mapping measurements derived from C IV and Si IV.

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Section: Single-epoch Black Hole Mass Estimatesmentioning

confidence: 80%

Section: Introductionmentioning

confidence: 99%

Restframe UV-to-optical spectroscopy of APM 08279+5255

Saturni

Bischetti

Piconcelli

et al. 2018

A&A

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“…APM 08279 exhibits AGN-driven outflows acting at different scales and involving different gas phases (Chartas et al 2009, Saez & Chartas 2011, Saturni et al 2016, Hagino et al 2017.…”

Section: Discussionmentioning

confidence: 99%

“…For v UFO = 0.22c, and a black hole mass in the range M(BH) = 2 × 10 9 − 10 10 M (Hagino et al 2017 and references therein), we estimated a nuclear outflow rate of 7.7-38 M /yr. The main parameters of the UFO are reported in Table 4.…”

Section: Molecular Outflowmentioning

confidence: 99%

On the discovery of fast molecular gas in the UFO/BAL quasar APM 08279+5255 atz= 3.912

Feruglio

Ferrara

Bischetti

et al. 2017

A&A

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We have performed a high sensitivity observation of the UFO/BAL quasar APM 08279+5255 at z=3.912 with NOEMA at 3.2 mm, aimed at detecting fast moving molecular gas. We report the detection of blueshifted CO(4-3) with maximum velocity (v95%) of −1340 km s −1 , with respect to the systemic peak emission, and a luminosity of L = 9.9 × 10 9 µ −1 K km s −1 pc −2 (where µ is the lensing magnification factor). We discuss various scenarios for the nature of this emission, and conclude that this is the first detection of fast molecular gas at redshift > 3. We derive a mass flow rate of molecular gas in the rangeṀ = 3 − 7.4 × 10 3 M /yr, and momentum boostṖ OF /Ṗ AGN ∼ 2 − 6, therefore consistent with a momentum conserving flow. For the largestṖ OF the scaling is also consistent with a energy conserving flow with an efficiency of ∼10-20%. The present data can hardly discriminate between the two expansion modes. The mass loading factor of the molecular outflow η =Ṁ OF /S FR is >> 1. We also detect a molecular emission line at a frequency of 94.83 GHz, corresponding to a rest frame frequency of 465.8 GHz, which we tentatively identified with the cation molecule N 2 H + (5-4), which would be the first detection of this species at high redshift. We discuss the alternative possibility that this emission is due to a CO emission line from the, so far undetected, lens galaxy. Further observations of additional transitions of the same species with NOEMA can discriminate between the two scenarios.

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“…On the other hand, it has been suggested that radiative acceleration of UFOs via UV linedriving is possible if they were in a sufficiently low ionization state near their launch points (e.g., Hagino et al 2015Hagino et al , 2017Nomura et al 2016;Nomura & Ohsuga 2017). In this scenario, as the UFOs flow outwards, they become increasingly ionized, until only H-and He-like Fe lines can be detected.…”

Section: Introductionmentioning

confidence: 99%

Physical Conditions in Ultra-fast Outflows in AGN

Kraemer

Tombesi

Bottorff

2018

ApJ

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XMM-Newton and Suzaku spectra of AGN have revealed highly ionized gas, in the form of absorption lines from H-like and He-like Fe. Some of these absorbers, "Ultra Fast Outlows (UFOs)", have radial velocities of up to 0.25c. We have undertaken a detailed photo-ionization study of high-ionization Fe absorbers, both UFOs and non-UFOs, in a sample of AGN observed by XMM-Newton. We find that the heating and cooling processes in UFOs are Compton-dominated, unlike the non-UFOs. Both types are characterized by Force Multipliers on the order of unity, which suggests that they cannot be radiatively accelerated in sub-Eddington AGN, unless they were much less ionized at their point of origin. However, such highly ionized gas can be accelerated via a Magneto-Hydrodynamic (MHD) wind. We explore this possibility by applying a cold MHD flow model to the UFO in the well-studied Seyfert galaxy, NGC 4151. We find that the UFO can be accelerated along magnetic streamlines anchored in the accretion disk. In the process, we have been able to contrain the magnetic field strength and the magnetic pressure in the UFO and have determined that the system is not in magnetic/gravitational equipartition. Open questions include the variabilty of the UFOs and the apparent lack of non-UFOs in UFO sources.

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

Cited by 30 publications

References 69 publications

Restframe UV-to-optical spectroscopy of APM 08279+5255

Restframe UV-to-optical spectroscopy of APM 08279+5255

On the discovery of fast molecular gas in the UFO/BAL quasar APM 08279+5255 atz= 3.912

Physical Conditions in Ultra-fast Outflows in AGN

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