Dust reverberation-mapping of the Seyfert 1 galaxy WPVS48

Núñez, F. Pozo; Haas, Martín; Chini, R.; Ramolla, M.; Westhues, C.; Steenbrugge, K. C.; Kaderhandt, L.; Drass, H.; Lemke, R.; Murphy, M.

doi:10.1051/0004-6361/201323178

Cited by 31 publications

(31 citation statements)

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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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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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“…It has also been suggested that a component of hot graphite dust residing within the ISM dust sublimation radius is required to account for a peak in the NIR SED of broad-line AGN (Mor & Netzer 2012; 10 42 10 43 10 44 10 2 10 1 10 0 r lag (pc) Rd,ISM,iso Rd,C,iso toriso 10 42 10 43 10 44 10 45 10 2 10 1 10 0 toraniso Suganuma et al 2006Clavel et al 1989Koshida et al 2014Pozo Nunez et al 2015& 2014Mandal et al 2018Lira et al 2011& 2015 L V (erg/s) Fig. 23.-The K-band radius-luminosity relationships for the observationally determined values of r K available in the literature (Clavel et al 1989;Suganuma et al 2006;Lira et al 2011;Koshida et al 2014;Pozo Nuñez et al 2014;Lira et al 2015;Pozo Nuñez et al 2015;Mandal et al 2018) and for r RW,K values derived from a subset of our globally optically thick torus models. The values of r RW corresponding to the median value of the RWD and the range between minimum and maximum RWD values at λ = 2.2 µm are represented by a solid line and a shaded band, respectively, for both the isotropically (blue; left panel) and anisotropically (red; right panel) illuminated torus.…”

Section: Rwd-lwr Relationship and Implications Formentioning

confidence: 99%

“…The dust reverberation radius has now been measured by NIR (K-band) reverberation mapping for about 20 AGN (e.g., Nelson 1996;Oknyanskij & Horne 2001;Minezaki et al 2004;Suganuma et al 2006;Lira et al 2011;Koshida et al 2014;Pozo Nuñez et al 2014;Lira et al 2015;Mandal et al 2018). Some of the authors of this paper are members of a collaboration that recently conducted a 2.5 year monitoring campaign, during which 12 broad-line AGN were observed using the Spitzer Space Telescope at 3.6 and 4.5 µm, supported by ground-based optical observations.…”

Section: Introductionmentioning

confidence: 99%

Modeling the Infrared Reverberation Response of the Circumnuclear Dusty Torus in AGNs: An Investigation of Torus Response Functions

Almeyda

Robinson

Richmond

et al. 2020

ApJ

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The size and structure of the dusty circumnuclear torus in active galactic nuclei (AGN) can be investigated by analyzing the temporal response of the torus's infrared (IR) dust emission to variations in the AGN ultraviolet/optical luminosity. This method, reverberation mapping, is applicable over a wide redshift range, but the IR response is sensitive to several poorly constrained variables relating to the dust distribution and its illumination, complicating the interpretation of measured reverberation lags. We have used an enhanced version of our torus reverberation mapping code (TORMAC) to conduct a comprehensive exploration of the torus response functions at selected wavelengths, for the standard interstellar medium grain composition. The shapes of the response functions vary widely over the parameter range covered by our models, with the largest variations occurring at shorter wavelengths (≤ 4.5 µm). The reverberation lag, quantified as the response-weighted delay (RWD), is most affected by the radial depth of the torus, the steepness of the radial cloud distribution, the degree of anisotropy of the AGN radiation field, and the volume filling factor. Nevertheless, we find that the RWD provides a reasonably robust estimate, to within a factor of ∼ 3, of the luminosity-weighted torus radius, confirming the basic assumption underlying reverberation mapping. However, overall, the models predict radii at 2.2 µm that are a typically factor of ∼ 2 larger than those derived from K-band reverberation mapping. This is likely an indication that the innermost region of the torus is populated by clouds dominated by large graphite grains.

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“…We collect K-band lags and absolute V-band magnitudes M obs V of 20 AGN from the literature (Lira et al 2011;Koshida et al 2014;Pozo Nuñez et al 2014. These are used as a comparison sample to our simulations.…”

Section: Appendix A: Comparison Of Simulated Lag-luminosity Relation mentioning

confidence: 99%

Cosmology with AGN dust time lags–simulating the new VEILS survey

Hönig

Watson

Kishimoto

et al. 2016

Mon. Not. R. Astron. Soc.

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The time lag between optical and near-infrared continuum emission in active galactic nuclei (AGN) shows a tight correlation with luminosity and has been proposed as a standardisable candle for cosmology. In this paper, we explore the use of these AGN hot-dust time lags for cosmological model fitting under the constraints of the new VISTA Extragalactic Infrared Legacy Survey VEILS. This new survey will target a 9 deg 2 field observed in J-and K s-band with a 14-day cadence and will run for three years. The same area will be covered simultaneously in the optical griz bands by the Dark Energy Survey, providing complementary time-domain optical data. We perform realistic simulations of the survey setup, showing that we expect to recover dust time lags for about 450 objects out of a total of 1350 optical type 1 AGN, spanning a redshift range of 0.1 < z < 1.2. We use the lags recovered from our simulations to calculate precise distance moduli, establish a Hubble diagram, and fit cosmological models. Assuming realistic scatter in the distribution of the dust around the AGN as well as in the normalisation of the lag-luminosity relation, we are able to constrain Ω Λ in ΛCDM with similar accuracy as current supernova samples. We discuss the benefits of combining AGN and supernovae for cosmology and connect the present work to future attempts to reach out to redshifts of z > 4.

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Dust reverberation-mapping of the Seyfert 1 galaxy WPVS48

Cited by 31 publications

References 32 publications

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

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

Modeling the Infrared Reverberation Response of the Circumnuclear Dusty Torus in AGNs: An Investigation of Torus Response Functions

Cosmology with AGN dust time lags–simulating the new VEILS survey

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