Investigating the radio-loud phase of broad absorption line quasars

Bruni, G.; González‐Serrano, J. I.; Pedani, M.; Benn, Chris; Mack, K.‐H.; Holt, J.; Montenegro‐Montes, F. M.; Jiménez-Luján, F.

doi:10.1051/0004-6361/201424424

Cited by 9 publications

(9 citation statements)

References 41 publications

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“…The key result of this work is the lack of strong differences in the UV spectral properties of RL and RQ BAL quasars, as well as between their fundamental physical properties, confirming the findings from the rest-frame optical of Bruni et al (2014). Though Table 2 shows that there are some differences, many of them are interrelated.…”

Section: Discussionsupporting

confidence: 78%

“…Runnoe et al (2013) found that RL BAL quasars are very similar to RQ BAL quasars in their optical emission-line properties, and RL BAL quasars are more "BAL-like" than "RL-like" in their EV1 properties. Bruni et al (2014) find that the rest-frame optical properties of RL and RQ BAL quasars, and physical parameters derived from them, are identical. Here, we examine the rest-frame ultraviolet (UV) spectral properties of a well-matched sample of 73 RL and 473 RQ BAL quasars, and search for significant differences in their properties.…”

Section: Introductionmentioning

confidence: 74%

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Radio-loud and radio-quiet BAL quasars: a detailed ultraviolet comparison

Rochais

DiPompeo

Myers

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Studies of radio-loud (RL) broad absorption line (BAL) quasars indicate that popular orientation-based BAL models fail to account for all observations. Are these results extendable to radio-quiet (RQ) BAL quasars? Comparisons of RL and RQ BAL quasars show that many of their properties are quite similar. Here we extend these analyses to the rest-frame ultraviolet (UV) spectral properties, using a sample of 73 RL and 473 RQ BAL quasars selected from the Sloan Digital Sky Survey (SDSS). Each RQ quasar is individually matched to a RL quasar in both redshift (over the range 1.5 < z < 3.5) and continuum luminosity. We compare several continuum, emission line, and absorption line properties, as well as physical properties derived from these measurements. Most properties in the samples are statistically identical, though we find slight differences in the velocity structure of the BALs that cause apparent differences in C IV emission line properties. Differences in the velocities may indicate an interaction between the radio jets and the absorbing material. We also find that UV Fe II emission is marginally stronger in RL BAL quasars. All of these differences are subtle, so in general we conclude that RL and RQ BAL QSOs are not fundamentally different objects, except in their radio properties. They are therefore likely to be driven by similar physical phenomena, suggesting that results from samples of RL BAL quasars can be extended to their RQ counterparts.

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Section: Discussionsupporting

confidence: 78%

Section: Introductionmentioning

confidence: 74%

Radio-loud and radio-quiet BAL quasars: a detailed ultraviolet comparison

Rochais

DiPompeo

Myers

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…The radio loudness associated to their powerful radio jets is probably driven by the efficient extraction of rotational energy from both the disk (Blandford & Payne 1982) and the black hole (Blandford & Znajek 1977); however, the exact physical mechanism behind the launching and acceleration of the most powerful radio jets is still under investigation (see Czerny & You 2016, for a recent review). We note how there are no apparent differences in observed properties such as black hole mass, Eddington ratio, and BLR size between radio-loud and radio-quiet BAL QSOs (Bruni et al 2014), suggesting that the physical difference between them might reside in different black hole spin values. The scarcity of powerful radio-loud FR II BAL QSOs is probably due to the combination of a large black hole mass needed to have a RL AGN (Laor 2000), which is possibly related to the merger history of the host galaxies, where coherent mergers can increase the value of the BH spin (e.g., Fanidakis et al 2011), and a high or very high ṁ to have a radiation driven BAL wind, all in all giving a small region of the M BH − ṁ parameter space where the phenomenon of radio-loud BAL QSO can manifest.…”

Section: Discussionmentioning

confidence: 77%

A global view of the inner accretion and ejection flow around super massive black holes

Giustini

Proga

2019

A&A

153

117

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Context. Understanding the physics and geometry of accretion and ejection around super massive black holes (SMBHs) is important to understand the evolution of active galactic nuclei (AGN) and therefore of the large scale structures of the Universe. Aims. We aim at providing a simple, coherent, and global view of the sub-parsec accretion and ejection flow in AGN with varying Eddington ratio,ṁ, and black hole mass, M BH . Methods. We made use of theoretical insights, results of numerical simulations, as well as UV and X-ray observations to review the inner regions of AGN by including different accretion and ejection modes, with special emphasis on the role of radiation in driving powerful accretion disk winds from the inner regions around the central SMBH.Results. We propose fiveṁ regimes where the physics of the inner accretion and ejection flow around SMBHs is expected to change, and that correspond observationally to quiescent and inactive galaxies; low luminosity AGN (LLAGN); Seyferts and mini-broad absorption line quasars (mini-BAL QSOs); narrow line Seyfert 1 galaxies (NLS1s) and broad absorption line quasars (BAL QSOs); and super-Eddington sources. We include in this scenario radiation-driven disk winds, which are strong in the highṁ, large M BH regime, and possibly present but likely weak in the moderateṁ, small M BH regime. Conclusions. A great diversity of the accretion/ejection flows in AGN can be explained to a good degree by varying just two fundamental properties: the Eddington ratioṁ and the black hole mass M BH , and by the inclusion of accretion disk winds that can naturally be launched by the radiation emitted from luminous accretion disks.

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“…Any association with the X-ray weakness appears rather challenging in the standard paradigm. J1425+54: A claim for a C iv BAL with absorption index AI 269 km s −1 was made by Bruni et al (2014). The feature seems to be actually resolved in three narrow components, and its origin remains somewhat uncertain.…”

Section: Appendix A: Gallery Of X-ray Spectramentioning

confidence: 99%

The most luminous blue quasars at 3.0 < z < 3.3

Nardini

Lusso

Risaliti

et al. 2019

A&A

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We present the X-ray analysis of 30 luminous quasars at z 3.0-3.3 with pointed XMM-Newton observations (28-48 ks) originally obtained by our group to test the suitability of active galactic nuclei as standard candles for cosmological studies. The sample was selected in the optical from the Sloan Digital Sky Survey Data Release 7 to be representative of the most luminous, intrinsically blue quasar population, and by construction boasts a high degree of homogeneity in terms of optical and UV properties. In the X-rays, only four sources are too faint for a detailed spectral analysis, one of which is formally undetected. Neglecting one more object later found to be radio-loud, the other 25 quasars are, as a whole, the most X-ray luminous ever observed, with rest-frame 2-10 keV luminosities of 0.5-7 × 10 45 erg s −1 . The continuum photon index distribution, centred at Γ ∼ 1.85, is in excellent agreement with those in place at lower redshift, luminosity, and black-hole mass, confirming the universal nature of the X-ray emission mechanism in quasars. Even so, when compared against the well-known L X -L UV correlation, our quasars show an unexpectedly varied behaviour, splitting into two distinct subsets. About two-thirds of the sources are clustered around the relation with a minimal scatter of 0.1 dex, while the remaining one-third appear to be X-ray underluminous by factors of > 3-10. Such a large incidence (≈25%) of X-ray weakness has never been reported in radio-quiet, non-broad absorption line (BAL) quasar samples. Several factors could contribute to enhancing the X-ray weakness fraction among our z 3 blue quasars, including variability, mild X-ray obscuration, contamination from weakline quasars, and missed BALs. However, the X-ray weak objects also have, on average, flatter spectra, with no clear evidence of absorption. Indeed, column densities in excess of a few ×10 22 cm −2 can be ruled out for most of the sample. We suggest that, at least in some of our X-ray weak quasars, the corona might experience a radiatively inefficient phase due to the presence of a powerful accretion-disc wind, which substantially reduces the accretion rate through the inner disc and therefore also the availability of seed photons for Compton up-scattering. The origin of the deviations from the L X -L UV relation will be further investigated in a series of future studies.

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Investigating the radio-loud phase of broad absorption line quasars

Cited by 9 publications

References 41 publications

Radio-loud and radio-quiet BAL quasars: a detailed ultraviolet comparison

Radio-loud and radio-quiet BAL quasars: a detailed ultraviolet comparison

A global view of the inner accretion and ejection flow around super massive black holes

The most luminous blue quasars at 3.0 < z < 3.3

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