HS 1700+6416: the first high-redshift unlensed narrow absorption line-QSO showing variable high-velocity outflows

Lanzuisi, G.; Giustini, M.; Cappi, M.; Dadina, M.; Malaguti, G.; Vignali, C.; Chartas, G.

doi:10.1051/0004-6361/201219481

Cited by 42 publications

(69 citation statements)

References 59 publications

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“…-The residuals above the expected energies of Fe Kα suggest the presence of an outflowing disk wind, as predicted by super-Eddington accretion models (e.g., Zubovas & King 2012), and observed in a handful of high-redshift QSOs accreting close to Eddington (Chartas et al 2003;Lanzuisi et al 2012;Vignali et al 2015). The presence of ionized material surrounding the SMBH is indeed one of the characteristics of highly accreting BHs (see, e.g., Ballantyne et al 2011).…”

Section: +198mentioning

confidence: 58%

NuSTARreveals the extreme properties of the super-Eddington accreting supermassive black hole in PG 1247+267

Lanzuisi

Perna

Comastri

et al. 2016

A&A

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PG1247+267 is one of the most luminous known quasars at z ∼ 2 and is a strongly super-Eddington accreting supermassive black hole (SMBH) candidate. We obtained NuSTAR data of this intriguing source in December 2014 with the aim of studying its high-energy emission, leveraging the broad band covered by the new NuSTAR and the archival XMM-Newton data. Several measurements are in agreement with the super-Eddington scenario for PG1247+267: the soft power law (Γ = 2.3 ± 0.1); the weak ionized Fe emission line; and a hint of the presence of outflowing ionized gas surrounding the SMBH. The presence of an extreme reflection component is instead at odds with the high accretion rate proposed for this quasar. This can be explained with three different scenarios; all of them are in good agreement with the existing data, but imply very different conclusions: i) a variable primary power law observed in a low state, superimposed on a reflection component echoing a past, higher flux state; ii) a power law continuum obscured by an ionized, Compton thick, partial covering absorber; and iii) a relativistic disk reflector in a lamp-post geometry, with low coronal height and high BH spin. The first model is able to explain the high reflection component in terms of variability. The second does not require any reflection to reproduce the hard emission, while a rather low high-energy cutoff of ∼100 keV is detected for the first time in such a high redshift source. The third model require a face-on geometry, which may affect the SMBH mass and Eddington ratio measurements. Deeper X-ray broad-band data are required in order to distinguish between these possibilities.

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Section: +198mentioning

confidence: 58%

NuSTARreveals the extreme properties of the super-Eddington accreting supermassive black hole in PG 1247+267

Lanzuisi

Perna

Comastri

et al. 2016

A&A

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“…This average value is close to the velocity derived for the outflow observed in PID352. Compared with other AGN showing UFOs, the peculiarity of PID352 is that it represents one of the few cases where an X-ray outflowing wind has been clearly detected at z > 1 (see also Chartas et al 2002Chartas et al , 2007Chartas et al , 2009Chartas et al , 2014Lanzuisi et al 2012). Furthermore, to our knowledge, PID352 is not a lensed quasar, while most of the z > 1 outflow detections are related to lensed systems.…”

Section: Radio Datamentioning

confidence: 74%

“…At the end of this obscured phase, massive quasar-driven outflows blow away most of the cold gas reservoir, creating a population of "red-and-dead" gas-poor elliptical galaxies (e.g., Cattaneo et al 2009). Support for this picture -at least for the most luminous AGN -comes from observations of kpc-scale outflows of molecular gas (e.g., Feruglio et al 2010;Sturm et al 2011;Veilleux et al 2013;Cicone et al 2014), as well as of neutral and ionized gas (e.g., Nesvadba et al 2008;Alexander et aloutflows (UFOs, with velocities typically up to 0.1-0.4c) have been clearly detected in X-rays in a sizable sample of AGN at low redshift (e.g., Reeves et al 2003;Pounds et al 2003;Tombesi et al 2010Tombesi et al , 2012aTombesi et al , 2014Tombesi et al , 2015Giustini et al 2011;Patrick et al 2012;Gofford et al 2013Gofford et al , 2015King et al 2014;Nardini et al 2015;Ballo et al 2015; see also Cappi 2006 for an early review; and Fabian 2012 for a more recent one) and also in a limited number of high-redshift quasars (e.g., Chartas et al 2002Chartas et al , 2007Chartas et al , 2009Chartas et al , 2014Saez et al 2009;Lanzuisi et al 2012). Although original claims of blueshifted absorption features were strongly debated (see Vaughan & Uttley 2008), recent high photon statistics in X-ray spectra of both radio-quiet (e.g., Tombesi et al 2010Tombesi et al , 2011Tombesi et al , 2012aGofford et al 2013) and radio-loud AGN (e.g., Gofford et al 2013;Tombesi et al 2014) have undoubtedly shown that these outflows are not ra...…”

Section: Introductionmentioning

confidence: 99%

The XMM deep survey in the CDF-S

Vignali

Iwasawa

Comastri

et al. 2015

A&A

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In active galactic nuclei (AGN)-galaxy co-evolution models, AGN winds and outflows are often invoked to explain why super-massive black holes and galaxies stop growing efficiently at a certain phase of their lives. They are commonly referred to as the leading actors of feedback processes. Evidence of ultra-fast (v > ∼ 0.05c) outflows in the innermost regions of AGN has been collected in the past decade by sensitive X-ray observations for sizable samples of AGN, mostly at low redshift. Here we present ultra-deep XMM-Newton and Chandra spectral data of an obscured (N H ≈ 2 × 10 23 cm −2 ), intrinsically luminous (L 2−10 keV ≈ 4 × 10 44 erg s −1 ) quasar (named PID352) at z ≈ 1.6 (derived from the X-ray spectral analysis) in the Chandra Deep Field-South. The source is characterized by an iron emission and absorption line complex at observed energies of E ≈ 2−3 keV. While the emission line is interpreted as being due to neutral iron (consistent with the presence of cold absorption), the absorption feature is due to highly ionized iron transitions (FeXXV, FeXXVI) with an outflowing velocity of 0.14 +0.02 −0.06 c, as derived from photoionization models. The mass outflow rate -∼2 M yr −1 -is similar to the source accretion rate, and the derived mechanical energy rate is ∼9.5 × 10 44 erg s −1 , corresponding to 9% of the source bolometric luminosity. PID352 represents one of the few cases where indications of X-ray outflowing gas have been observed at high redshift thus far. This wind is powerful enough to provide feedback on the host galaxy.

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“…The observed wavelengths of the C iv doublet (λλ 1548.20Å, 1550.77Å) imply that the UV absorber is outflowing with a speed of v CIV ∼ 19,400 km s −1 . The only other quasar detected to date with similar blueshifted X-ray absorption features and a narrow absorption line (NAL) outflow is the unlensed z=2.74 NAL quasar HS 1700+6414 (Lanzuisi et al 2012) which, however, has a ∼10 times lower 2-10 keV flux of 3-9×10 −14 erg s −1 cm −2 . Blueshifted X-ray broad absorption lines have been detected in several high-z quasars (i.e., APM 08279+5255, Chartas et al 2002;PG 1115+080, Chartas et al 2003andHS 1700+6416, Lanzuisi et al 2012).…”

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confidence: 99%

THE WIDE-ANGLE OUTFLOW OF THE LENSED z = 1.51 AGN HS 0810+2554

Chartas

Cappi

Hamann

et al. 2016

ApJ

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We present results from X-ray observations of the gravitationally lensed z = 1.51 AGN HS 0810+2554 performed with the Chandra X-ray Observatory and XMM-Newton. Blueshifted absorption lines are detected in both observations at rest-frame energies ranging between ∼1-12 keV at > ∼ 99% confidence. The inferred velocities of the outflowing components range between ∼0.1c and ∼0.4c.A strong emission line at ∼6.8 keV accompanied by a significant absorption line at ∼7.8 keV is also detected in the Chandra observation. The presence of these lines is a characteristic feature of a P-Cygni profile supporting the presence of an expanding outflowing highly ionized iron absorber in this quasar. Modeling of the P-Cygni profile constrains the covering factor of the wind to be > ∼ 0.6, assuming disk shielding. A disk-reflection component is detected in the XMM-Newton observation accompanied by blueshifted absorption lines. The XMM-Newton observation constrains the inclination angle to be < 45• at 90% confidence, assuming the hard excess is due to blurred reflection from the accretion disk.The detection of an ultrafast and wide-angle wind in an AGN with intrinsic narrow absorption lines (NALs) would suggest that quasar winds may couple efficiently with the intergalactic medium and provide significant feedback if ubiquitous in all NAL and BAL quasars.We estimate the mass-outflow rate of the absorbers to lie in the range of 1.5 and 3.4 M ⊙ yrfor the two observations. We find the fraction of kinetic to electromagnetic luminosity released by HS 0810+2554 is large (ǫ k = 9 +8 −6 ) suggesting that magnetic driving is likely a significant contributor to the acceleration of this outflow.

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HS 1700+6416: the first high-redshift unlensed narrow absorption line-QSO showing variable high-velocity outflows

Cited by 42 publications

References 59 publications

NuSTARreveals the extreme properties of the super-Eddington accreting supermassive black hole in PG 1247+267

NuSTARreveals the extreme properties of the super-Eddington accreting supermassive black hole in PG 1247+267

The XMM deep survey in the CDF-S

THE WIDE-ANGLE OUTFLOW OF THE LENSED z = 1.51 AGN HS 0810+2554

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