A<i>CHANDRA</i>SURVEY OF THE X-RAY PROPERTIES OF BROAD ABSORPTION LINE RADIO-LOUD QUASARS

Brandt, W. N.; Gibson, R. R.; Garmire, G. P.; Shemmer, Ohad

doi:10.1088/0004-637x/702/2/911

Cited by 23 publications

(31 citation statements)

References 91 publications

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“…Furthermore, in the specific case of another FRII radio galaxy, 3C 111, the UFO mass outflow rate (∼0.1−1 M yr −1 , i.e., similar to that of PID352) is much greater than the outflow funnelled into the jet (Ṁ out,j = 0.0005−0.005 M yr −1 ; Tombesi et al 2012b), implying that the UFO is much more massive than the jet, although its kinetic power can be one order of magnitude lower. Placed in a broader context, these results are suggestive of considerable feedback onto the host galaxy by winds and jets (see also the discussion in Miller et al 2009 about the co-existence of outflows and jets in radio-loud quasars and their connection with X-ray binaries).…”

Section: Radio Datamentioning

confidence: 77%

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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Section: Radio Datamentioning

confidence: 77%

The XMM deep survey in the CDF-S

Vignali

Iwasawa

Comastri

et al. 2015

A&A

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“…We have recently completed a systematic Chandra study of the X-ray properties of 21 radio-loud BAL quasars (12 new and 9 archival observations; Miller et al 2009). Our new Chandra snapshot observations targeted the optically brightest radio-loud BAL quasars found in SDSS Data Release 3.…”

Section: An X-ray Survey Of Bright Representative Radio-loud Bal Quamentioning

confidence: 99%

X-raying the Winds of Luminous Active Galaxies

Brandt¹,

Chartas

Gallagher

et al. 2009

AIP Conference Proceedings

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We briefly describe some recent observational results, mainly at X-ray wavelengths, on the winds of luminous active galactic nuclei (AGNs). These winds likely play a significant role in galaxy feedback. Topics covered include (1) Relations between X-ray and UV absorption in Broad Absorption Line (BAL) and mini-BAL quasars; (2) X-ray absorption in radio-loud BAL quasars; and (3) Evidence for relativistic iron K BALs in the X-ray spectra of a few bright quasars. We also mention some key outstanding problems and prospects for future advances; e.g., with the International X-ray Observatory (IXO).Comment: 7 pages, 3 figures, to appear in proceedings of the conference "The Monster's Fiery Breath: Feedback in Galaxies, Groups, and Clusters", June 2009, Madison, Wisconsi

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“…Several other studies, however, find that after accounting for intrinsic absorption (Luo et al 2013) or magnification of X-ray emission viewed from large inclination angles (Morabito et al 2014), BAL quasars are X-ray weak compared to non-BAL objects. Moreover, the degree of X-ray weakness for radio-loud and radio-quiet BAL quasars is different, with the radio-loud ones being less X-ray weak than radio-quiet ones, compared to non-BAL quasars (Miller et al 2009). A simple scenario suggested by a few authors says that the X-ray continuum of radio-loud BAL quasars is a superposition of disk/corona and small-scale jet X-ray emission Kunert-Bajraszewska et al 2009;Miller et al 2009).…”

Section: Introductionmentioning

confidence: 99%

“…Moreover, the degree of X-ray weakness for radio-loud and radio-quiet BAL quasars is different, with the radio-loud ones being less X-ray weak than radio-quiet ones, compared to non-BAL quasars (Miller et al 2009). A simple scenario suggested by a few authors says that the X-ray continuum of radio-loud BAL quasars is a superposition of disk/corona and small-scale jet X-ray emission Kunert-Bajraszewska et al 2009;Miller et al 2009).…”

Section: Introductionmentioning

confidence: 99%

Broadband nuclear emission in two radio-loud broad absorption line quasars

Kunert-Bajraszewska¹,

Janiuk

2015

A&A

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Aims. We present modelling and interpretation of the continuum broadband emission of two broad absorption line (BAL) quasars. The X-ray weakness of BAL quasars in comparison to non-BAL objects is possibly caused by the absorption of X-ray emission by the shielding material near the equatorial plane. On the other hand, the radio-loud BAL quasars are more X-ray loud than the radio-quiet ones. This suggests that part of the X-ray emission may arise from the radio jet. To investigate this possibility, we modelled the nuclear spectra of two BAL quasars in the whole available energy range. Methods. We focus on the emission from the very centres of these two objects, not greater than several parsecs. The source of emission was approximated by a single, homogeneous component that produces synchrotron and inverse-Compton radiation. The simplicity of the model allowed us to estimate the basic physical parameters of the emitting regions, using a universal analytic approach. Such methods have already been proposed to estimate basic physical parameters in blazars. For the first time, in a simplified form we propose this solution for quasars. In addition, we modelled the radiation spectra of the accretion disk and its corona to compare them with the jets' spectra. Results. We find that in the case of radio and X-ray luminous high-redshift object 3C 270.1, the nuclear X-ray continuum is dominated by the non-thermal, inverse-Compton emission from the innermost parts of the radio jet. However, the radio core of the lobe-dominated PG 1004+130 is probably too weak to produce significant part of the observed X-ray emission. A large contribution from the X-ray emitting accretion disk and corona is produced in our model for a sufficiently high mass of the black hole. However, it then exceeds the observed flux. Because the large intrinsic absorption was postulated recently by the NuSTAR observations, we propose that the disk-corona component may still account for the X-rays produced in this source. This part of the spectrum must nevertheless be dominated by the X-ray jet. The results of our modelling show that the jet-linked X-ray emission is present in both strong and weak radio sources, but its fraction seems to scale with the radio jet power.

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ACHANDRASURVEY OF THE X-RAY PROPERTIES OF BROAD ABSORPTION LINE RADIO-LOUD QUASARS

Cited by 23 publications

References 91 publications

The XMM deep survey in the CDF-S

The XMM deep survey in the CDF-S

X-raying the Winds of Luminous Active Galaxies

Broadband nuclear emission in two radio-loud broad absorption line quasars

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