X-Rays From a Radio-Loud Compact Broad Absorption Line Quasar 1045+352 and the Nature of Outflows in Radio-Loud Broad Absorption Line Quasars

Kunert-Bajraszewska, M.; Siemiginowska, Aneta; Janiuk, Agnieszka

doi:10.1088/0004-637x/705/2/1356

Cited by 13 publications

(19 citation statements)

References 58 publications

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“…In a sample of 15 BAL quasars, Montenegro-Montes et al (2008) find that all of them are compact at FIRST resolutions, and the majority remain compact at around 80 mas resolution. Even very long baseline interferometry (VLBI) observations, which has down to milli-arcsecond resolution, often show BAL quasars as compact objects (Doi et al 2009, Jiang & Wang 2008, Kunert-Bajraszewska et al 2009). The fact that it is required to observe many of these objects on size scales on the order of a few hundred parsecs or less before seeing any resolved structure (Kunert-Bajraszewska et al 2010, Liu et al 2008 suggests that they are intrinsically quite small.…”

Section: Introductionmentioning

confidence: 99%

A Very Large Array Survey of Radio-Selected SDSS Broad Absorption Line Quasars

DiPompeo

Brotherton

Breuck

et al. 2011

ApJ

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We have built a sample of 74 radio-selected broad absorption line quasars from the Sloan Digital Sky Survey Data Release 5 (SDSS DR5) and Faint Images of the Radio Sky at Twenty Centimeters (FIRST), along with a well matched sample of 74 unabsorbed "normal" quasars. The sources have been observed with the NRAO Very Large Array/Expanded Very Large Array at 8.4 GHz (3.5 cm) and 4.9 GHz (6 cm). All sources have additional archival 1.4 GHz (21 cm) data. Here we present the measured radio fluxes, spectral indices, and our initial findings. The percentage of BAL quasars with extended structure (on the order of 10%) in our sample is similar to previous studies at similar resolutions, suggesting that BAL quasars are indeed generally compact, at least at arsecond resolutions. The majority of sources do not appear to be significantly variable at 1.4 GHz, but we find two previously unidentified BAL quasars that may fit into the "polar" BAL category. We also identify a significant favoring of steeper radio spectral index for BAL compared to non-BAL quasars. This difference is apparent for several different measures of the spectral index, and persists even when restricting the samples to only include compact objects. Because radio spectral index is a statistical indicator of viewing angle for large samples, these results suggest that BAL quasars do have a range of orientations but are more often observed farther from the jet axis compared to normal quasars.

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Section: Introductionmentioning

confidence: 99%

A Very Large Array Survey of Radio-Selected SDSS Broad Absorption Line Quasars

DiPompeo

Brotherton

Breuck

et al. 2011

ApJ

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“…However, only a very small fraction of compact BAL quasars have been observed with VLBI so far [9,14,15,11,4,13,3,8]. About half of the observed sources have unresolved structures which prevents us from directly estimating their orientation from morphology, but the steepness of their radio spectrum can give us an idea about their orientation.…”

Section: Introductionmentioning

confidence: 99%

30 GHz monitoring of broad absorption line (BAL) quasars

Ceglowski¹,

Kunert-Bajraszewska²,

Pazderska³

et al. 2016

Proceedings of 11th European VLBI Network Symposium &Amp; Users Meeting — PoS(11th EVN Symposium)

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Broad absorption line (BAL) quasars have been studied for over thirty years. Yet it is still unclear why and when we observe broad absorption lines in quasars. Is this phenomenon caused by geometry or is it connected with the evolution process? Variability of the BAL quasars, if present, can give us information about their orientation, namely it can indicate whether they are oriented more pole-on. Using the Torun 32-metre dish equipped with the One Centimetre Receiver Array (OCRA) we have started a monitoring campaign of a sample of compact radio-loud BAL quasars. This 30 GHz variability monitoring program supplements the high-resolution interferometric observations of these objects we have carried out with the EVN and VLBA.

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“…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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X-Rays From a Radio-Loud Compact Broad Absorption Line Quasar 1045+352 and the Nature of Outflows in Radio-Loud Broad Absorption Line Quasars

Cited by 13 publications

References 58 publications

A Very Large Array Survey of Radio-Selected SDSS Broad Absorption Line Quasars

A Very Large Array Survey of Radio-Selected SDSS Broad Absorption Line Quasars

30 GHz monitoring of broad absorption line (BAL) quasars

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

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