<i>XMM-Newton</i>reveals a Seyfert-like X-ray spectrum in the<i>z</i>= 3.6 QSO B1422+231

Dadina, M.; Vignali, C.; Cappi, M.; Lanzuisi, G.; Ponti, G.; Marco, Barbara De; Chartas, G.; Giustini, M.

doi:10.1051/0004-6361/201628467

Cited by 11 publications

(13 citation statements)

References 107 publications

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“…Performing the fit with the Pexrav model (Magdziarz & Zdziarski 1995) plus the Fe Kα emission line, we get consistent best-fit results for the continuum parameters. In addition, in B1422 the line is detected at 90% c.l., with parameters E line = 6.50 +0.18 −0.14 keV and EW = 80 +60 −40 eV rest frame (consistent with the results obtained in Dadina et al 2016 from a deeper XMM-Newton observation), while in 2MASSJ16 it is marginally detected, with EW < 125 eV.…”

Section: Phenomenological Modelsupporting

confidence: 88%

“…keV for B1422 and 2MASSJ16, respectively, implying coronal temperatures of ∼ 33 keV and ∼ 53 keV, assuming E cut /kT e ∼ 2 for optically thin coronae (Petrucci et al 2001). For B1422, our best-fit E cut is consistent, within 1σ, with the results from Dadina et al (2016), but the uncertainties derived here are 50% smaller. These E cut values place the two QSOs in the narrow region allowed by the runaway pair-production models: in Fig.…”

Section: Phenomenological Modelsupporting

confidence: 83%

“…The characterization of the X-ray emission from AGN is therefore the best tool available to investigate the physical properties of the innermost regions around accreting SMBHs and to measure coronal properties such as temperature, optical depth and geometry. Recent X-ray reverberation studies (De Marco et al 2013, Reis & Miller 2013, Cackett et al 2014, Kara et al 2016 suggest that the size R c of the hot corona producing the X-rays is in the range ∼ 3 − 20 R g , where R g = GM/c 2 is the gravitational radius for a black hole of mass M. Such a range has also been independently confirmed via microlensing studies (e.g. Pooley et al 2007, MacLeod et al 2015, Chartas et al 2016.…”

Section: Introductionmentioning

confidence: 84%

“…We note that B1422 is classified as moderately radio loud (R = 90, Dadina et al 2016) with a steep radio continuum (α r = 0.9, Orienti et al 2007), indicating that the source is highly inclined in the plane of the sky. In this case, the radio emission should be dominated by the lobes, and not by the jet, and the X-ray spectrum is not strongly contaminated by the jet component (see discussion in Dadina et al 2016). Notes.…”

Section: Target Selection and Observationsmentioning

confidence: 90%

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NuSTAR Measurement of Coronal Temperature in Two Luminous, High-redshift Quasars

Lanzuisi¹,

Gilli²,

Cappi³

et al. 2019

ApJL

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X-ray emission from AGN is believed to be produced via Comptonization of optical/UV seed photons emitted by the accretion disk, up-scattered by hot electrons in a corona surrounding the black hole. A critical compactness vs. temperature threshold is predicted above which any increase in the source luminosity, for a fixed size, would then generate positron-electron pairs rather than continue heating the coronal plasma. Current observations seem to confirm that all AGN populate the region below this critical line. These models, however, have never been probed by observations in the high-luminosity regime, where the critical line is expected to reach low temperatures. To fill this observational gap, we selected two luminous (log(L Bol )> 47.5 erg/s) quasars, 2MASSJ1614346+470420 (z=1.86) and B1422+231 (z=3.62), and obtained XMM-Newton and NuSTAR deep observations for them. We performed detailed spectral analysis of their quasi-simultaneous soft and hard Xray data, in order to constrain the parameters of their coronae. Using a phenomenological cut-off power-law model, with the inclusion of a reflection component, we derived rest-frame values of the high energy cut-off of E cut = 106 +102 −37 keV and E cut = 66 +17 −12 keV, respectively. Comptonization models consistently give as best-fit parameters electron temperatures of ∼ 45 keV and ∼ 28 keV, respectively, and optically thick coronae (τ > 1). These low coronal temperatures fall in the limited region allowed at these luminosities to avoid runaway pair production.

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Section: Phenomenological Modelsupporting

confidence: 88%

Section: Phenomenological Modelsupporting

confidence: 83%

Section: Introductionmentioning

confidence: 84%

Section: Target Selection and Observationsmentioning

confidence: 90%

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NuSTAR Measurement of Coronal Temperature in Two Luminous, High-redshift Quasars

Lanzuisi¹,

Gilli²,

Cappi³

et al. 2019

ApJL

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“…The detection of the FeKα emission line may indicate the presence of a reflection component. This feature is commonly observed in nearby Seyfert galaxies (e.g., Perola et al 2002), and recently it has been detected also in some high-z QSO (Dadina et al 2016, Lanzuisi et al 2016). To test this hypothesis and to further probe the robustness of the detection of the absorption feature against a more complex underlying continuum, we tried the Pexmon reflection model (Nandra et al 2007) fixing the incli- nation angle (Θ=30 • ) and the high-energy cut-off (E cut−o f f =100 keV).…”

Section: Data Reduction and Analysismentioning

confidence: 56%

Yet another UFO in the X-ray spectrum of a high-z lensed QSO

Dadina

Vignali

Cappi

et al. 2018

A&A

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Aims. Ultra-fast outflows (UFO) appear to be common in local active galactic nuclei (AGN) and may be powerful enough (Ė kin ≥1% of L bol ) to effectively quench the star formation in their host galaxies. To test feedback models based on AGN outflows, it is mandatory to investigate UFOs near the peak of AGN activity, that is, at high-z where only a few studies are available to date. Methods. UFOs produce Fe resonant absorption lines measured above ≈7 keV. The most critical problem in detecting such features in distant objects is the difficulty in obtaining X-ray data with sufficient signal-to-noise. We therefore selected a distant QSO that gravitational lensing made bright enough for these purposes, the z=2.64 QSO MG J0414+0534, and observed it with XMM-Newton for ≈78 ks.Results. The X-ray spectrum of MG J0414+0534 is complex and shows signatures of cold absorption (N H ≈4×10 22 cm −2 ) and of the presence of an iron emission line (E≈6.4 keV, EW=95±53 eV) consistent with it originating in the cold absorber. Our main result, however, is the robust detection (more than 5σ) of an absorption line at E int ≈9.2 keV (E obs ≈2.5 keV observer frame). If interpreted as due to FeXXVI, it implies gas outflowing at v out ≈0.3c. To our knowledge, this is the first detection of an UFO in a radio-loud quasar at z≥1.5. We estimated that the UFO mechanical output isĖ kin ≈2.5L bol withṗ out /ṗ rad ≈17 indicating that it is capable of installing significant feedback between the super-massive black hole (SMBH) and the bulge of the host galaxy. We argue that this also suggests a magnetic driving origin of the UFO.

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The properties of the X-ray corona in the distant (z= 3.91) quasar APM 08279+5255

Bertola

Vignali

Lanzuisi³

et al. 2022

A&A

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We present new joint XMM-Newton and NuSTAR observations of APM 08279+5255, a gravitationally-lensed, broad-absorption line quasar (z = 3.91). After showing a fairly stable flux (f2 − 10 ≃ 4 − 5.5 × 10−13 erg s−1) from 2000 to 2008, APM 08279+5255 was found in a fainter state in the latest X-ray exposures (f2 − 10 ≃ 2.7 × 10−13 erg s−1), which can likely be ascribed to a lower X-ray activity. Moreover, the 2019 data present a prominent Fe Kα emission line and do not show any significant absorption line. This fainter state, coupled to the first hard X-ray sampling of APM 08279+5255, allowed us to measure X-ray reflection and the high-energy cutoff in this source for the first time. From the analysis of previous XMM-Newton and Chandra observations, X-ray reflection is demonstrated to be a long-lasting feature of this source, but less prominent prior to 2008, possibly due to a stronger primary emission. The estimated high-energy cutoff (Ecut = 99−35+91 keV) sets a new redshift record for the farthest ever measured and places APM 08279+5255 in the allowed region of the compactness-temperature diagram of X-ray coronae, in agreement with previous results on high-z quasars.

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XMM-Newtonreveals a Seyfert-like X-ray spectrum in thez= 3.6 QSO B1422+231

Cited by 11 publications

References 107 publications

NuSTAR Measurement of Coronal Temperature in Two Luminous, High-redshift Quasars

NuSTAR Measurement of Coronal Temperature in Two Luminous, High-redshift Quasars

Yet another UFO in the X-ray spectrum of a high-z lensed QSO

The properties of the X-ray corona in the distant (z= 3.91) quasar APM 08279+5255

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