Simultaneous H<i>α</i> and dust reverberation mapping of 3C 120: Testing the bowl-shaped torus geometry

Ramolla, M.; Haas, Martín; Westhues, C.; Núñez, F. Pozo; Figaredo, Catalina Sobrino; Blex, Julia; Zetzl, M.; Kollatschny, W.; Hodapp, Klaus W.; Chini, R.; Murphy, M.

doi:10.1051/0004-6361/201732081

Cited by 27 publications

(26 citation statements)

References 84 publications

(140 reference statements)

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“…Furthermore, the vertical BRL structure is consistent with the bowlshaped geometry proposed by Goad et al (2012), e.g. tested by Ramolla et al (2018) for 3C 120. The 2D velocity maps of the Balmer line profiles reveal a faster response of the line wings (0−10 d) in comparison to a slower response of the line centers (10 − 30 d).…”

Section: Discussionsupporting

confidence: 86%

Spectral changes and BLR kinematics of eruptive changing-look AGN

Ochmann¹,

Kollatschny²,

Zetzl³

2020

caosp

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We present results of recent optical spectroscopic variability campaigns for HE 1136-2304 and NGC 1566 which exhibited X-ray outbursts in July 2014 and June 2018, respectively. We show that the broad line region (BLR) structure in the changing-look AGN HE 1136-2304 is similar to that of non-changing-look AGN and that the BLR kinematics is dominated by Keplerian accretion disk (AD) rotation. Furthermore, we present an optical spectrum of NGC 1566 taken only a few weeks after its X-ray outburst, clearly showing drastic spectral changes.

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Section: Discussionsupporting

confidence: 86%

Spectral changes and BLR kinematics of eruptive changing-look AGN

Ochmann¹,

Kollatschny²,

Zetzl³

2020

caosp

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“…Clavel et al 1991;Hu et al 2008;Zhu et al 2009;Kawaguchi & Mori 2010;Gandhi et al 2015), which could itself be dynamic and outflowing (Chan & Krolik 2016;Williamson et al 2019;Leftley et al 2019). This class of models can also have some beneficial reverberation characteristics if they have 'bowl-shaped' geometries (Goad et al 2012;Ramolla et al 2018). Many of the general principles we have discussed would apply to such models and further detailed simulations are worthwhile.…”

Section: Limitations and Caveatsmentioning

confidence: 99%

Stratified disc wind models for the AGN broad-line region: ultraviolet, optical, and X-ray properties

Matthews

Knigge

Higginbottom

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The origin, geometry and kinematics of the broad line region (BLR) gas in quasars and active galactic nuclei (AGN) are uncertain. We demonstrate that clumpy biconical disc winds illuminated by an AGN continuum can produce BLR-like spectra. We first use a simple toy model to illustrate that disc winds make quite good BLR candidates, because they are selfshielded flows and can cover a large portion of the ionizing flux-density (φ H -n H ) plane. We then conduct Monte Carlo radiative transfer and photoionization calculations, which fully account for self-shielding and multiple scattering in a non-spherical geometry. The emergent model spectra show broad emission lines with equivalent widths and line ratios comparable to those observed in AGN, provided that the wind has a volume filling factor of f V 0.1. Similar emission line spectra are produced for a variety of wind geometries (polar or equatorial) and for launch radii that differ by an order of magnitude. The line emission arises almost exclusively from plasma travelling below the escape velocity, implying that 'failed winds' are important BLR candidates. The behaviour of a line-emitting wind (and possibly any 'smooth flow' BLR model) is similar to that of the locally optimally-emitting cloud (LOC) model originally proposed by Baldwin et al (1995), except that the gradients in ionization state and temperature are large-scale and continuous, rather than within or between distinct clouds. Our models also produce UV absorption lines and X-ray absorption features, and the stratified ionization structure can partially explain the different classes of broad absorption line quasars.

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“…The BLR reverberation mapping observations for local Seyfert galaxies and some high redshift quasars have been carried out by several groups (e.g., Peterson et al 1998Peterson et al , 2004Kaspi et al 2000;Bentz et al 2009b;Denney et al 2010;Grier et al 2012;Du et al 2014;Fausnaugh et al 2017); a compilation of ∼ 40 AGNs with secure Hβ BLR lag detection can be found in Bentz & Katz (2015) (see also Bentz et al 2009aBentz et al , 2013. Dust reverberation mapping observations have also been measured for several AGNs (Clavel et al 1989;Glass 1992;Sitko et al 1993;Glass 2004;Suganuma et al 2006;Koshida et al 2014;Pozo Nuñez et al 2014Schnülle et al 2015;Lira et al 2015;Vazquez et al 2015;Mandal et al 2018;Ramolla et al 2018;Landt et al 2019). The first systematic investigation of dust reverberation mapping was carried out by the Multicolour Active Galactic Nuclei Monitoring (MAGNUM) project (Yoshii 2002;Yoshii et al 2003;Minezaki et al 2004;Tomita et al 2006;Suganuma et al 2006;Koshida et al 2009;Sakata et al 2010;Koshida et al 2014;Yoshii et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Rapid luminosity decline and subsequent reformation of the innermost dust distribution in the changing-look AGN Mrk 590

Kokubo

Minezaki

2019

Monthly Notices of the Royal Astronomical Society

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We examine the long-term optical/near-infrared (NIR) flux variability of a "changing-look"active galactic nucleus (AGN) Mrk 590 between 1998 and 2007. Multiband multi-epoch optical/NIR photometry data from the SDSS Stripe 82 database and the Multicolor Active Galactic Nuclei Monitoring (MAGNUM) project reveal that Mrk 590 experienced a sudden luminosity decrease during the period from 2000 to 2001. Detection of dust reverberation lag signals between V -and K-band light curves obtained by the MAGNUM project during the faint state in 2003 − 2007 suggests that the dust torus innermost radius R dust of Mrk 590 had become very small [R dust ≃ 32 light-days (lt-days)] by the year 2004 according to the aforementioned significant decrease in AGN luminosity. The R dust in the faint state is comparable to the Hβ broad line region (BLR) radius of R Hβ,BLR ≃ 26 lt-days measured by previous reverberation mapping observations during the bright state of Mrk 590 in 1990 − 1996.These observations indicate that the innermost radius of the dust torus in Mrk 590 decreased rapidly after the AGN ultraviolet-optical luminosity drop, and that the replenishment time scale of the innermost dust distribution is less than 4 years, which is much shorter than the free fall time scale of BLR gas or dust clouds. We suggest that rapid replenishment of the innermost dust distribution can be accomplished either by new dust formation in radiatively-cooled BLR gas clouds or by new dust formation in the disk atmosphere and subsequent vertical wind from the dusty disk as a result of radiation pressure.

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Simultaneous Hα and dust reverberation mapping of 3C 120: Testing the bowl-shaped torus geometry

Cited by 27 publications

References 84 publications

Spectral changes and BLR kinematics of eruptive changing-look AGN

Spectral changes and BLR kinematics of eruptive changing-look AGN

Stratified disc wind models for the AGN broad-line region: ultraviolet, optical, and X-ray properties

Rapid luminosity decline and subsequent reformation of the innermost dust distribution in the changing-look AGN Mrk 590

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