Reverberation Mapping Results for Five Seyfert 1 Galaxies

Grier, C. J.; Peterson, B. M.; Pogge, Richard W.; Denney, K. D.; Bentz, Misty C.; Martini, Paul; Сергеев, С. Г.; Kaspi, S.; Minezaki, Takeo; Zu, Ying; Kochanek, C. S.; Siverd, Robert J.; Shappee, B. J.; Stanek, K. Z.; Salvo, C. Araya; Beatty, Thomas G.; Bird, Jonathan C.; Bord, D. J.; Borman, G. A.; Chen, Xiao; Chen, C.; Cohen, S.; Dietrich, M.; Doroshenko, V. T.; Drake, Travis W.; Efimov, Yu. S.; Free, N.; Ginsburg, Idan; Henderson, Calen B.; King, A. L.; Koshida, Shintaro; Mogren, K.; Molina, Mallory; Mosquera, A. M.; Назаров, С. В.; Okhmat, D. N.; Pejcha, Ondřej; Rafter, Stephen E.; Shields, J. C.; Skowron, J.; Szczygiel, D.; Valluri, Monica; Saders, Jennifer L. van

doi:10.1088/0004-637x/755/1/60

Cited by 200 publications

(236 citation statements)

References 63 publications

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“…Through the modeling of the AGN light curves as a damped random walk (DRW; Zu et al 2011, 2013 andreference therein), this method appears to be consistent with previous crosscorrelation techniques (e.g. Grier et al 2012, for spectroscopic reverberation data). Using the SPEAR code 2 on our light curves, we obtain a time delay of τ spear = 18.4 +1.2 −1.0 .…”

Section: B-band R-bandsupporting

confidence: 66%

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

Núñez

Westhues

Ramolla

et al. 2013

A&A

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We present photometric reverberation mapping of the narrow-line Seyfert 1 galaxy ESO 399-IG20 performed with the robotic 15 cm telescope VYSOS-6 at the Cerro Armazones Observatory. Through the combination of broad-and narrow-band filters we determine the size of the broad-line emitting region (BLR) by measuring the time delay between the variability of the continuum and the Hα emission line. We use the flux variation gradient method to separate the host galaxy contribution from that of the active galactic nucleus (AGN), and to calculate the 5100 Å luminosity L AGN of the AGN. Both measurements permit us to derive the position of ESO 399-IG20 in the BLR size -AGN luminosity R BLR ∝ L 0.5 AGN diagram. We infer the basic geometry of the BLR through modeling of the light curves. The pronounced sharp variability patterns in both the continuum and the emission line light curves allow us to reject a spherical BLR geometry. The light curves are best fitted by a disk-like BLR seen nearly face-on with an inclination angle of 6 • ± 3 • and with an extension from 16 to 20 light days.

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Section: B-band R-bandsupporting

confidence: 66%

“…Because the narrow-band collects both the emission line flux and the underlying continuum, the challenge is to extract the pure emission line light curve. In the dedicated case study of 3C 120, Pozo Nuñez et al (2012) demonstrated that PRM reaches an accuracy similar to spectroscopic RM (Grier et al 2012).…”

Section: Introductionmentioning

confidence: 95%

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

Núñez

Westhues

Ramolla

et al. 2013

A&A

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“…Because the iron line has the main advantage of being in a 'clean' part of the spectrum, where it is not affected by the reprocessed black body emission or by continuum luminosity and broad line region radius, which can be used to estimate black hole mass when combined with optical line width (e.g. Kaspi et al 2000;Grier et al 2012), or the correlation between black hole mass and host galaxy bulge stellar velocity dispersion (e.g. Gebhardt et al 2000).…”

Section: The Iron K Lagmentioning

confidence: 99%

“…Such work has culminated in the measurement of black hole masses for a wide range of AGN (e.g. Grier et al 2012 and see Peterson & Bentz 2006 for a review) and is now leading to the measurement of the detailed structure of the BLR, identifying its inclination to the observer as well as whether the gas is simply orbiting, outflowing, inflowing or some combination of all three (Bentz et al 2010;Pancoast et al 2011Pancoast et al , 2013Grier et al 2013).…”

Section: Introductionmentioning

confidence: 99%

X-ray reverberation around accreting black holes

Uttley

Cackett

Fabian³

et al. 2014

Astron Astrophys Rev

437

601

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Luminous accreting stellar mass and supermassive black holes produce power-law continuum X-ray emission from a compact central corona. Reverberation time lags occur due to light travel time-delays between changes in the direct coronal emission and corresponding variations in its reflection from the accretion flow. Reverberation is detectable using light curves made in different X-ray energy bands, since the direct and reflected components have different spectral shapes. Larger, lower frequency, lags are also seen and are identified with propagation of fluctuations through the accretion flow and associated corona. We review the evidence for X-ray reverberation in active galactic nuclei and black hole X-ray binaries, showing how it can be best measured and how it may be modelled. The timescales and energy-dependence of the high frequency reverberation lags show that much of the signal is originating from very close to the black hole in some objects, within a few gravitational radii of the event horizon. We consider how these signals can be studied in the future to carry out X-ray reverberation mapping of the regions closest to black holes.

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“…Notable early attempts include Wanders et al (1995), Done & Krolik (1996), and Ulrich & Horne (1996), but recovered maps of velocity-resolved results, reminiscent of those shown in Figure 5, were ambiguous at best. In the last few years, however, reverberation programs have enjoyed much more success given the careful experimental setup and the resultant high quality of the data (Bentz et al 2009b(Bentz et al , 2010aDenney et al 2010;Grier et al 2012;De Rosa et al 2015).…”

Section: Blr Geometry and Kinematicsmentioning

confidence: 99%

AGN Reverberation Mapping

Bentz

2016

Astronomy at High Angular Resolution

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Reverberation mapping is now a well-established technique for investigating spatially-unresolved structures in the nuclei of distant galaxies with activelyaccreting supermassive black holes. Structural parameters for the broad emissionline region, with angular sizes of microarcseconds, can be constrained through the substitution of time resolution for spatial resolution. Many reverberation experiments over the last 30 years have led to a practical understanding of the requirements necessary for a successful program. With reverberation measurements now in hand for 60 active galaxies, and more on the horizon, we are able to directly constrain black hole masses, derive scaling relationships that allow large numbers of black hole mass estimates throughout the observable Universe, and begin investigating the detailed geometry and kinematics of the broad line region. Reverberation mapping is therefore one of the few techniques available that will allow a deeper understanding of the physical mechanisms involved in AGN feeding and feedback at very small scales, as well as constraints on the growth and evolution of black holes across cosmic time. In this contribution, I will briefly review the background, implementation, and major results derived from this high angular resolution technique.

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Reverberation Mapping Results for Five Seyfert 1 Galaxies

Cited by 200 publications

References 63 publications

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

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

X-ray reverberation around accreting black holes

AGN Reverberation Mapping

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