Size and disk-like shape of the broad-line region of ESO 399-IG20

Núñez, F. Pozo; Westhues, C.; Ramolla, M.; Bruckmann, C.; Haas, Martín; Chini, R.; Steenbrugge, K. C.; Lemke, R.; Murphy, M.

doi:10.1051/0004-6361/201321047

Cited by 23 publications

(16 citation statements)

References 42 publications

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“…There were observations on 27 days, from which 24 had exposures in B, 19 in R, and 7 in the V filter. Data reduction and processing of the OCA data was performed in the same manner as reported in Pozo Nuñez et al (2013).…”

Section: A7 Ocamentioning

confidence: 99%

Anatomy of the AGN in NGC 5548

Mehdipour

Kaastra

Kriss

et al. 2015

A&A

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An extensive multi-satellite campaign on NGC 5548 has revealed this archetypal Seyfert-1 galaxy to be in an exceptional state of persistent heavy absorption. Our observations taken in 2013-2014 with XMM-Newton, Swift, NuSTAR, INTEGRAL, Chandra, HST and two ground-based observatories have together enabled us to establish that this unexpected phenomenon is caused by an outflowing stream of weakly ionised gas (called the obscurer), extending from the vicinity of the accretion disk to the broad-line region. In this work we present the details of our campaign and the data obtained by all the observatories. We determine the spectral energy distribution of NGC 5548 from near-infrared to hard X-rays by establishing the contribution of various emission and absorption processes taking place along our line of sight towards the central engine. We thus uncover the intrinsic emission and produce a broadband continuum model for both obscured (average summer 2013 data) and unobscured (<2011) epochs of NGC 5548. Our results suggest that the intrinsic NIR/optical/UV continuum is a single Comptonised component with its higher energy tail creating the "soft X-ray excess". This component is compatible with emission from a warm, optically-thick corona as part of the inner accretion disk. We then investigate the effects of the continuum on the ionisation balance and thermal stability of photoionised gas for unobscured and obscured epochs.

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Section: A7 Ocamentioning

confidence: 99%

Anatomy of the AGN in NGC 5548

Mehdipour

Kaastra

Kriss

et al. 2015

A&A

Self Cite

171

235

View full text Add to dashboard Cite

show abstract

“…Disc-shaped BLRs are popular in the literature (e.g. Decarli et al 2008;Gaskell & Goosmann 2013;Begelman & Silk 2016) and are commonly invoked to explain reverberation mapping results (Pozo Nuñez et al 2013;Pancoast et al 2014a,b;Goad & Korista 2014). Furthermore, R11 suggested that the broad emission lines form in a disc and trace the disc emission in terms of their anisotropy.…”

Section: Line Anisotropymentioning

confidence: 99%

Quasar emission lines as probes of orientation: implications for disc wind geometries and unification

Matthews

Knigge

Long

2017

Mon. Not. R. Astron. Soc.

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The incidence of broad absorption lines (BALs) in quasar samples is often interpreted in the context of a geometric unification model consisting of an accretion disc and an associated outflow. We use the the Sloan Digital Sky Survey (SDSS) quasar sample to test this model by examining the equivalent widths (EWs) of C iv 1550Å, Mg ii 2800Å, [O iii] 5007Å and C iii] 1909Å. We find that the emission line EW distributions in BAL and non-BAL quasars are remarkably similar -a property that is inconsistent with scenarios in which a BAL outflow rises equatorially from a geometrically thin, optically thick accretion disc. We construct simple models to predict the distributions from various geometries; these models confirm the above finding and disfavour equatorial geometries. We show that obscuration, line anisotropy and general relativistic effects on the disc continuum are unlikely to hide an EW inclination dependence. We carefully examine the radio and polarisation properties of BAL quasars. Both suggest that they are most likely viewed (on average) from intermediate inclinations, between type 1 and type 2 AGN. We also find that the low-ionization BAL quasars in our sample are not confined to one region of 'Eigenvector I' parameter space. Overall, our work leads to one of the following conclusions, or some combination thereof: (i) the continuum does not emit like a geometrically thin, optically thick disc; (ii) BAL quasars are viewed from similar angles to non-BAL quasars, i.e. low inclinations; (iii) geometric unification does not explain the fraction of BALs in quasar samples.

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“…All these CCF methods share a key assumption that the light curve containing contribution from the broad-line emission must be dominated by it, otherwise the peak at the position of a non-zero lag would be overwhelmed by the auto-correlation peak of the continuum at zero lags. Thus generally CCF-like methods only apply to spectroscopic reverberation mapping, sometimes also to broadband+narrowband photometric RM (e.g., Haas et al 2011;Pozo Nuñez et al 2013;Jiang et al 2016), in which, however, the contribution from the continuum to the narrow band light curve must be subtracted carefully. There are also some works applying CCF-like methods directly to broadband photometric data (e.g., Chelouche et al 2012), but due to the fact that the typical relative contribution of a broad emission line to the whole broadband is of the order of a few percent, this method cannot be expected to perform well on most of the quasars whose variability information comes only from their broadband photometric data.…”

Section: Introductionmentioning

confidence: 99%

Broadband Photometric Reverberation Mapping Analysis on SDSS-RM and Stripe 82 Quasars

Zhang

Yang

2018

ApJ

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We modified the broadband photometric reverberation mapping (PRM) code, JAVELIN, and tested the availability to get broad line region (BLR) time delays that are consistent with the spectroscopic reverberation mapping (SRM) project SDSS-RM. The broadband light curves of SDSS-RM quasars produced by convolution with the system transmission curves were used in the test. We found that under similar sampling conditions (evenly and frequently sampled), the key factor determining whether the broadband PRM code can yield lags consistent with the SRM project is the flux ratio of the broad emission line to the reference continuum, which is in line with the previous findings. We further found a critical line-to-continuum flux ratio, about 6%, above which the mean of the ratios between the lags from PRM and SRM becomes closer to unity, and the scatter is pronouncedly reduced. We also tested our code on a subset of SDSS Stripe 82 quasars, and found that our program tends to give biased lag estimations due to the observation gaps when the R-L relation prior in Markov Chain Monte Carlo (MCMC) is discarded. The performance of the damped random walk (DRW) model and the power-law (PL) structure function model on broadband PRM were compared. We found that given both SDSS-RM-like or Stripe 82-like light curves, the DRW model performs better in carrying out broadband PRM than the PL model.

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Size and disk-like shape of the broad-line region of ESO 399-IG20

Cited by 23 publications

References 42 publications

Anatomy of the AGN in NGC 5548

Anatomy of the AGN in NGC 5548

Quasar emission lines as probes of orientation: implications for disc wind geometries and unification

Broadband Photometric Reverberation Mapping Analysis on SDSS-RM and Stripe 82 Quasars

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