Reverberation Mapping of the Seyfert 1 Galaxy NGC 7469

Peterson, B. M.; Grier, C. J.; Horne, K.; Pogge, Richard W.; Bentz, Misty C.; Rosa, Gisella De; Denney, K. D.; Martini, Paul; Сергеев, С. Г.; Kaspi, S.; Minezaki, Takeo; Zu, Ying; Kochanek, C. S.; Siverd, Robert J.; Shappee, B. J.; Salvo, C. Araya; Beatty, Thomas G.; Bird, Jonathan C.; Bord, D. J.; Борман, Г. А.; Chen, Xiao; Chen, C. T.; 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.; Motohara, Kentaro; Назаров, С. В.; Okhmat, D. N.; Pejcha, Ondřej; Rafter, Stephen E.; Shields, J. C.; Skowron, D. M.; Valluri, Monica; Saders, Jennifer L. van; Yoshii, Yuzuru

doi:10.1088/0004-637x/795/2/149

Cited by 81 publications

(60 citation statements)

References 49 publications

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“…These results are consistent with all of these sources possessing an unbeamed non-thermal continuum that is the primary ionizing source for the gas that produces the observed Lyα emission line. While both the continuum and Lyα line are seen to vary, the substantial distance (1-10 pc) we have inferred for the Lyα emitting region does not allow the tight connection between continuum and line variability that is seen for Seyfert galaxies ("reverberation mapping"; Peterson et al 2014). However, one apparently successful narrow-line-region distance determination has been obtained for NGC 5548 using the [O III] 5007Å forbidden line (Peterson et al 2013).…”

Section: Conclusion and Summarymentioning

confidence: 68%

Far-Uv Emission Properties of Fr1 Radio Galaxies

Danforth¹,

Stocke²,

Begelman³

et al. 2016

ApJ

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The power mechanism and accretion geometry for low-power FR 1 radio galaxies is poorly understood in comparison to Seyfert galaxies and QSOs. In this paper we use the diagnostic power of the Lyα recombination line observed using the Cosmic Origins Spectrograph (COS) aboard the Hubble Space Telescope (HST) to investigate the accretion flows in three well-known, nearby FR 1s: M 87, NGC 4696, and Hydra A. The Lyα emission line's luminosity, velocity structure and the limited knowledge of its spatial extent provided by COS are used to assess conditions within a few parsecs of the super-massive black hole (SMBH) in these radio-mode AGN. We observe strong Lyα emission in all three objects with similar total luminosity to that seen in BL Lacertae objects. M 87 shows a complicated emission line profile in Lyα which varies spatially across the COS aperture and possibly temporally over several epochs of observation. In both NGC 4696 and M 87, the Lyα luminosities ∼ 10 40 ergs s −1 are closely consistent with the observed strength of the ionizing continuum in Case B recombination theory and with the assumption of near unity covering factor. It is possible that the Lyα emitting clouds are ionized largely by beamed radiation associated with the jets. Long-slit UV spectroscopy can be used to test this hypothesis. Hydra A and the several BL Lac objects studied in this and previous papers have Lyα luminosities larger than M 87 but their extrapolated, non-thermal continua are so luminous that they over-predict the observed strength of Lyα, a clear indicator of relativistic beaming in our direction. Given their substantial space density (∼ 4 × 10 −3 Mpc −3 ) the unbeamed Lyman continuum radiation of FR 1s may make a substantial minority contribution (∼ 10%) to the local UV background if all FR 1s are similar to M 87 in ionizing flux level.

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Section: Conclusion and Summarymentioning

confidence: 68%

Far-Uv Emission Properties of Fr1 Radio Galaxies

Danforth¹,

Stocke²,

Begelman³

et al. 2016

ApJ

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“…11 NGC 7469 was mapped twice by Collier et al (1998) and Peterson et al (2014). While their Hβ lags are consistent, the FWHM of Hβ is very different.…”

Section: Black Hole Masses and Accretion Ratesmentioning

confidence: 90%

Supermassive Black Holes With High Accretion Rates in Active Galactic Nuclei. V. A New Size–luminosity Scaling Relation for the Broad-Line Region

Zhang

et al. 2016

ApJ

146

141

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This paper reports results of the third-year campaign of monitoring super-Eddington accreting massive black holes (SEAMBHs) in active galactic nuclei (AGNs) between 2014 and 2015. Ten new targets were selected from the quasar sample of the Sloan Digital Sky Survey (SDSS), which have generally been more luminous than the SEAMBH candidates in the last two years. Hβ lags (t b H ) in five of the 10 quasars have been successfully measured in this monitoring season. We find that the lags are generally shorter, by large factors, than those of objects with same optical luminosity, in light of the well-known R Hβ -L 5100 relation. The five quasars have dimensionless accretion rates of Ṁ = 10-10 3 . Combining these with measurements of the previous SEAMBHs, we find that the reduction of Hβ lags depends tightly on accretion rates,, where t -R L is the Hβ lag from the normal R Hβ -L 5100 relation. Fitting 63 mapped AGNs, we present a new scaling relation for the broad-line region: . Implications of this new relation are briefly discussed.

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“…The other method to estimate the lag is the JAVELIN software developed by Zu et al (2011), which is widely employed not only in recent reverberation studies of the optical broad emission lines and the thermal dust emission of AGNs (e.g., Grier et al 2012;Koshida et al 2014;Peterson et al 2014), but also in analysis of the lag between flux variations of their X-ray emission and the UV-optical continuum emission (McHardy et al 2014;Shappee et al 2014;Lira et al 2015). It explicitly builds a model of a response light curve that is expressed as a convolution of a source light curve and a top-hat transfer function with a certain lag, and it fits the model to the …”

Section: Javelin Analysismentioning

confidence: 99%

X-Ray and Optical Correlation of Type I Seyfert NGC 3516 Studied With Suzaku and Japanese Ground-Based Telescopes

Noda

Minezaki

Watanabe

et al. 2016

ApJ

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From 2013 April to 2014 April, we performed X-ray and optical simultaneous monitoring of the type 1.5 Seyfert galaxy NGC3516. We employed Suzaku and five Japanese ground-based telescopes-the Pirka, Kiso Schmidt, Nayuta, MITSuME, and the Kanata telescopes. The Suzaku observations were conducted seven times with various intervals ranging from days or weeks to months, with an exposure of ∼50 ks each. The optical B-band observations not only covered those of Suzaku almost simultaneously, but also followed the source as frequently as possible. As a result, NGC3516 was found in its faint phase with a 2-10 keV flux of 0.21-2.70×10 −11 erg s. The 2-45 keV X-ray spectra were composed of a dominant variable hard power-law (PL) continuum with a photon index of ∼1.7 and a nonrelativistic reflection component with a prominent Fe-Kα emission line. Producing the B-band light curve by differential image photometry, we found that the B-band flux changed by ∼2.7×10 −11 erg s, which is comparable to the X-ray variation, and we detected a significant flux correlation between the hard PL component in X-rays and the B-band radiation, for the first time in NGC3516. By examining their correlation, we found that the X-ray flux preceded that in the B band by -+ 2.0 0.6 0.7 days (1σ error). Although this result supports the X-ray reprocessing model, the derived lag is too large to be explained by the standard view, which assumes a "lamppost"-type X-ray illuminator located near a standard accretion disk. Our results are better explained by assuming a hot accretion flow and a truncated disk.

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Reverberation Mapping of the Seyfert 1 Galaxy NGC 7469

Cited by 81 publications

References 49 publications

Far-Uv Emission Properties of Fr1 Radio Galaxies

Far-Uv Emission Properties of Fr1 Radio Galaxies

Supermassive Black Holes With High Accretion Rates in Active Galactic Nuclei. V. A New Size–luminosity Scaling Relation for the Broad-Line Region

X-Ray and Optical Correlation of Type I Seyfert NGC 3516 Studied With Suzaku and Japanese Ground-Based Telescopes

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