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

Zhang, Haowen; Yang, Qian; Wu, Xue-Bing

doi:10.3847/1538-4357/aaa3e5

Cited by 6 publications

(7 citation statements)

References 39 publications

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“…Also, the emission lines are often too narrow in comparison to the width of the broad-band filter, and the contrast between the continuum and the line is difficult to measure. Zhang et al (2018) show that the line flux to continuum flux ratio should be 6 % or larger for the broad-band RM to be effective. To overcome these problems, Jiang et al (2016) used a combination of broad-band and medium-band with the band widths of 180-264 Å which are several times narrower than typical broad-band filter widths.…”

Section: Introductionmentioning

confidence: 89%

“…To overcome the shortcomings of the spectroscopic RM, purely photometric RM has successfully been performed adopting broad-bands only or a combination of broad-, medium-, and narrow-bands (Haas et al 2011;Pozo Nuñez et al 2012Edri et al 2012;Hernitschek et al 2015;Jiang et al 2016;Zu et al 2016;Zhang et al 2018). Such a technique opens up a possibility of performing the RM of more than thousands of AGNs at once, even using a moderately sized telescopes.…”

Section: Introductionmentioning

confidence: 99%

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Medium-band Photometry Reverberation Mapping of Nearby Active Galactic Nuclei

Kim

Choi

et al. 2019

ApJ

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Reverberation mapping (RM) is one of the most efficient ways to investigate the broad-line region around the central supermassive black holes of active galactic nuclei (AGNs). A common way of performing the RM is to perform a long term spectroscopic monitoring of AGNs, but the spectroscopic monitoring campaign of a large number of AGNs requires an extensive amount of observing time of medium to large size telescopes. As an alternative way, we present the results of photometric RM with medium-band photometry. As the widths of medium-band filters match well with the widths of AGN broad emission lines, the medium-band observation with small telescopes can be a cost-effective way to perform RM. We monitored five nearby AGNs with available spectroscopic RM results showing days to weeks scale variability. Observations were performed for ∼3 months with an average of 3 days cadence using three medium-band filters on a 0.43 m telescope. The time lags between the continuum and the Hα emission line light curves are calculated using the JAVELIN software and the discrete correlation function. We find time lags of 1.5-15.9 days for these AGNs, which are consistent with the time lags derived from previous spectroscopic RM measurements. This result demonstrates that even a 0.5 m class telescope can perform RM with medium-bands. Furthermore, we show that RM for tens of thousands AGNs is possible with a dedicated 1 m class telescope.

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Section: Introductionmentioning

confidence: 89%

Section: Introductionmentioning

confidence: 99%

Medium-band Photometry Reverberation Mapping of Nearby Active Galactic Nuclei

Kim

Choi

et al. 2019

ApJ

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“…A stochastic process model has been widely used to describe the optical variability of AGN accretion disks (e.g., Kelly et al 2009;MacLeod et al 2010;Zu et al 2013;Rakshit & Stalin 2017;Li & Wang 2018;Zhang et al 2018;Lu et al 2019;Burke et al 2021). Generally, the damped random-walk (DRW) model can provide a successful fit to the long-term variability of AGN accretion disks.…”

Section: Introductionmentioning

confidence: 99%

Characterizing the γ-Ray Variability of Active Galactic Nuclei with the Stochastic Process Method

Zhang¹,

Yan

Zhang³

2022

ApJ

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Gamma-ray astronomy in the time domain has been by now progressed further as the variabilities of active galactic nuclei (AGNs) on different timescales have been reported a lot. We study the γ-ray variabilities of 23 jetted AGNs by applying a stochastic process method to the ∼12.7 yr long-term light curve (LC) obtained by the Fermi-Large Area Telescope (Fermi-LAT). In this method, the stochastically driven damped simple harmonic oscillator (SHO) and the damped random-walk (DRW) models are used to model the long-term LCs. Our results show that the long-term variabilities of 23 AGNs can be characterized well by both SHO and DRW models. However, the SHO model is restricted in the overdamped mode, and the parameters are poorly constrained. The SHO power spectral densities (PSDs) are the same as those of the typical DRW PSD. In the plot of the rest-frame timescale that corresponds to the broken frequency in the PSD versus black hole mass, the intrinsic, characteristic γ-ray timescales of 23 AGNs occupy almost the same space with the optical variability timescales obtained from the accretion disk emission. This suggests a connection between the jet and the accretion disk. As with the optical variability of the AGN accretion disk, the γ-ray timescale is also consistent with the thermal timescale caused by the thermal instability in the standard accretion disk of AGNs.

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“…It has been shown that AGNs variability in the optical band can be well described by the DRW (e.g., Kelly et al 2009;Kozłowski et al 2010;MacLeod et al 2010MacLeod et al , 2011Zu et al 2013;Rakshit & Stalin 2017). The model has been widely used in modeling AGN light curves in reverberation mapping (RM) studies (see Zu et al 2011;Pancoast et al 2011;Grier et al 2012;Li et al 2013;Zhang et al 2018). The limitations of the DRW model in describing AGN variability characteristics will be discussed in Section 4.…”

Section: Sample and Propertiesmentioning

confidence: 99%

Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. X. Optical Variability Characteristics

Huang¹,

Zhang²,

Wang³

et al. 2019

ApJ

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We compiled a sample of 73 active galactic nuclei (AGNs) with reverberation mapping (RM) observations from RM campaigns including our ongoing campaign of monitoring super-Eddington accreting massive black holes (SEAMBHs). This sample covers a large range of black hole (BH) mass (M • = 10 6−9 M ⊙ ), dimensionless accretion rates (Ṁ = 10 −2.7 − 10 2.7 ) and 5100Å luminosity (L 5100 = 10 42−46 erg s −1 ), allowing us to systematically study the AGN variability and their relations with BH mass, accretion rates, and optical luminosity. We employed the damped random walk (DRW) model to delineate the optical variability of continuum at 5100Å and obtained damped variability timescale (τ d ) and amplitude (σ d ) using a Markov Chain Monte Carlo (MCMC) method. We also estimated the traditional variability amplitudes (F var ), which provide a model-independent measure and therefore are used to test the DRW results. We found that AGN variability characteristics are generally correlated with (M • ,Ṁ , L 5100 ). These correlations are smooth from sub-Eddington to super-Eddington accretion AGNs, probably implying that the AGN variability may be caused by the same physical mechanism.

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

Cited by 6 publications

References 39 publications

Medium-band Photometry Reverberation Mapping of Nearby Active Galactic Nuclei

Medium-band Photometry Reverberation Mapping of Nearby Active Galactic Nuclei

Characterizing the γ-Ray Variability of Active Galactic Nuclei with the Stochastic Process Method

Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. X. Optical Variability Characteristics

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