<i>XMM-Newton</i>Detection of the Rare Fanaroff-Riley Type II Broad Absorption Line Quasar FIRST J101614.3+520916

Schaefer, J. J.; Brotherton, Michael S.; Shang, Zhaohui; Gregg, Michael D.; Becker, R. H.; Laurent-Muehleisen, S. A.; Lacy, Mark; White, R. L.

doi:10.1086/506509

Cited by 3 publications

(8 citation statements)

References 36 publications

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“…They interpreted this X-ray weakness as a result of large intrinsic absorption columns. The above suggestions have been confirmed by the X-ray observations of another two radio-loud BAL quasars (Miller et al 2006;Schaefer et al 2006) and it seemed we could draw a separate correlation between an X-ray and radio luminosity for radio-loud BAL quasars. However, recent detections of X-ray bright radio-loud BAL quasars (Wang et al 2008;Giustini et al 2008) complicated the picture.…”

Section: X-ray Emission Of the Coronasupporting

confidence: 57%

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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

Kunert-Bajraszewska

Siemiginowska

Janiuk

2009

ApJ

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We present new results on X-ray properties of radio loud broad absorption line (BAL) quasars and focus on broadband spectral properties of a high ionization BAL (HiBAL) compact steep spectrum (CSS) radio-loud quasar 1045+352. This HiBAL quasar has a very complex radio morphology indicating either strong interactions between a radio jet and the surrounding interstellar medium or a possible re-start of the jet activity. We detected 1045+352 quasar in a short 5 ksec Chandra ACIS-S observation. We applied theoretical models to explain spectral energy distribution of 1045+352 and argue that non-thermal, inverse-Compton (IC) emission from the innermost parts of the radio jet can account for a large fraction of the observed X-ray emission. In our analysis we also consider a scenario in which the observed X-ray emission from radio-loud BAL quasars can be a sum of IC jet X-ray emission and optically thin corona X-ray emission. We compiled a sample of radio-loud BAL quasars that were observed in X-rays to date and report no correlation between their X-ray and radio luminosity. However, the radio-loud BAL quasars show a large range of X-ray luminosities and absorption columns. This is consistent with the results obtained earlier for radio-quiet BAL quasars and may indicate an orientation effect in BAL quasars or more complex dependence between X-ray emission, radio emission, and an orientation based on the radio morphology.

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Section: X-ray Emission Of the Coronasupporting

confidence: 57%

“…In addition radio-loud quasars are more X-ray loud than the radio-quiet quasars (Young et al 2009). However, X-ray observations of radio-loud BALs are sparse and only a handful of them have been observed in X-rays so far (Brotherton et al 2005;Miller et al 2006;Schaefer et al 2006;Wang et al 2008, and this paper).…”

Section: Introductionmentioning

confidence: 78%

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

Siemiginowska

Janiuk

2009

ApJ

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“…The unabsorbed X-ray emission might be associated with a radio jet, a partial-covering absorber, or scattered emission which is not absorbed. Similarly, Miller et al (2006) found variable and complex soft X-ray absorption (probably a partial-covering absorber) in the radio-loud BAL quasar PG 1004ϩ130 (also see Schaefer et al [2006] for X-ray data of radio-loud BAL quasar FIRST J101614.3ϩ520916).…”

Section: Introductionmentioning

confidence: 79%

XMM-Newton Observations of Broad Absorption Line Quasars with Polar Outflows

Wang

Jiang

Zhou

et al. 2008

ApJ

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We have selected a sample of broad absorption line (BAL) quasars which show significant radio variations, indicating the presence of polar BAL outflows. We obtained snapshot XMM observations of four polar BAL QSOs, to check whether strong X-ray absorption, one of the most prominent characteristics of most BAL QSOs, also exists in polar outflows. Two of the sources are detected in the X-ray. Spectral fittings show that they are X-ray normal with no intrinsic X-ray absorption, suggesting the X-ray shielding gas might be absent in polar BAL outflows. Comparing to non-BAL QSOs, one of two X-ray-nondetected sources remains consistent with X-ray normal, while the other one, which is an iron low-ionization BAL (FeLoBAL), shows an X-ray weakness factor of 119, suggesting strong intrinsic X-ray absorption. Alternative explanations for the nondetection of strong X-ray absorption in the two X-ray-detected sources are that (1) the absorption is more complex than a simple neutral absorber, such as partial covering absorption or ionized absorption; (2) there might be significant jet contribution to the detected X-ray emission. Current data are insufficient to test these possibilities, and further observations are required to understand the X-ray nature of polar BAL outflows.

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“…Other X-ray telescopes cannot match the angular resolution of Chandra, important for 3 BAL RLQs identified in the following references were checked for archival Chandra coverage: Brotherton et al 1998;Wills et al 1999;Gregg et al 2000;Becker et al 2000;Becker et al 2001;Menou et al 2001;Brotherton et al 2002;Lacy et al 2002;Ma et al 2002;Willott et al 2002;Jiang & Wang 2003;Benn et al 2005;Brotherton et al 2005;Gallagher et al 2005;Urrutia et al 2005;Gallagher et al 2006;Gregg et al 2006;Miller et al 2006;Schaefer et al 2006;Zhou et al 2006;Just et al 2007;Kunert-Bajraszewska et al 2007;Liu et al 2008;Montenegro-Montes et al 2008. minimizing background contamination with faint sources, and many also have lower sensitivies and/or cover a significantly different energy range. We searched the XMM-Newton archives for observations pointed to within 15 ′ of any of the BAL RLQs described above, and find coverage of only three objects that would meet our selection criteria: J081102.91+500724.5 (Wang et al 2008), J101614.25+520915.4 (Schaefer et al 2006), andJ151630.30−005625.5 (PI Boehringer).…”

Section: Selection Of Archival Bal Rlqsmentioning

confidence: 99%

“…Wang et al (2008) present XMM-Newton observations of four BAL RLQs believed to be viewed at low inclinations (three of which have low-ionization BALs and only one of which has R * > 100), finding the two detected BAL RLQs to lack intrinsic X-ray absorption and to possess normal X-ray luminosities. X-ray studies of individual BAL RLQs include the work of Schaefer et al (2006), who find J101614.25+520915.4 to be X-ray weak with significant soft X-ray emission, and Miller et al (2006), who detect variable X-ray absorption in the BAL RLQ PG 1004+130 (but with an observed column density less than that of most BAL RQQs) and suggest the power-law form and X-ray weakness of the unabsorbed X-ray spectrum may indicate a jet-dominated X-ray nuclear continuum. Statistical efforts to understand the X-ray properties of BAL RLQs require a larger sample covering a wide range of BAL and radio properties.…”

Section: Introductionmentioning

confidence: 99%

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

Brandt

Gibson

Garmire

et al. 2009

ApJ

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This work presents the results of a Chandra study of 21 broad absorption line (BAL) radio-loud quasars (RLQs). We conducted a Chandra snapshot survey of 12 bright BAL RLQs selected from SDSS/FIRST data and possessing a wide range of radio and C IV absorption properties. Optical spectra were obtained nearly contemporaneously with the Hobby-Eberly Telescope; no strong flux or BAL variability was seen between epochs. In addition to the snapshot targets, we include in our sample 9 additional BAL RLQs possessing archival Chandra coverage. We compare the properties of (predominantly high-ionization) BAL RLQs to those of non-BAL RLQs as well as to BAL radio-quiet quasars (RQQs) and non-BAL RQQs for context.All 12 snapshot and 8/9 archival BAL RLQs are detected, with observed X-ray luminosities less than those of non-BAL RLQs having comparable optical/UV luminosities by typical factors of 4.1-8.5. (BAL RLQs are also X-ray weak by typical factors of 2.0-4.5 relative to non-BAL RLQs having both comparable optical/UV and radio luminosities.) However, BAL RLQs are not as X-ray weak relative to non-BAL RLQs as are BAL RQQs relative to non-BAL RQQs. While some BAL RLQs have harder X-ray spectra than typical non-BAL RLQs, some have hardness ratios consistent with those of non-BAL RLQs, and there does not appear to be a correlation between X-ray weakness and spectral hardness, in contrast to the situation for BAL RQQs. RLQs are expected to have X-ray continuum contributions from both disk-corona and small-scale jet emission. While the entire X-ray continuum in BAL RLQs cannot be obscured to the same degree as in BAL RQQs, we calculate that the jet is likely partially -2covered in many BAL RLQs. We comment briefly on implications for geometries and source ages in BAL RLQs.

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XMM-NewtonDetection of the Rare Fanaroff-Riley Type II Broad Absorption Line Quasar FIRST J101614.3+520916

Cited by 3 publications

References 36 publications

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

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

XMM-Newton Observations of Broad Absorption Line Quasars with Polar Outflows

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

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