A Revised Broad-Line Region Radius and Black Hole Mass for the Narrow-Line Seyfert 1 NGC 4051

Denney, K. D.; Watson, Linda C.; Peterson, Bradley M.; Pogge, Richard W.; Atlee, D. W.; Bentz, Misty C.; Bird, Jonathan C.; Brokofsky, D. J.; Comins, M. L.; Dietrich, M.; Doroshenko, V. T.; Eastman, Jason D.; Efimov, Yu. S.; Gaskell, C. Martin; Hedrick, C. H.; Klimanov, S. A.; Klimek, E. S.; Kruse, A.; Lamb, J. B.; Leighly, Karen M.; Minezaki, Takeo; Назаров, С. В.; Petersen, Eric; Peterson, Paul E.; Poindexter, S.; Schlesinger, Y.; Sakata, K.; Сергеев, С. Г.; Tobin, John J.; Unterborn, Cayman T.; Vestergaard, M.; Watkins, Aaron E.; Yoshii, Yuzuru

doi:10.1088/0004-637x/702/2/1353

Cited by 105 publications

(76 citation statements)

References 77 publications

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“…The 10 and 40 light days are explained as the radii of the VBLR and IMLR in Zhu, Zhang & Tang (2008). Recently, new observations of NGC 4051 gives a lag of the whole Hβ with respect to the continuum of about 1.75 days [11] which is near the days lag between the VBGC and the continuum in the observations we analyzed here. In our analysis based on our two-component model, the lags obtained from the whole Hβ are always between the lags obtained from the VBGC and IMGC.…”

Section: Simulationsupporting

confidence: 56%

“…This may provide an explanation to different lags of the whole Hβ obtained at different observation periods. For RM experiments focused on relatively low luminosity AGNs like NGC 4051 [11] , a large percentage of these AGNs are NLS1s whose broad Hβ are dominated by the IMGC [4] . The lag obtained from the whole Hβ may be near the radius of the IMLR and thus significantly different from that of the VBLR.…”

Section: Simulationmentioning

confidence: 99%

See 1 more Smart Citation

Diagnostics for the structure of AGNs’ broad line regions with reverberation mapping data: confirmation of the two-component broad line region model

Zhu

Zhang

2010

Sci. China Phys. Mech. Astron.

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Section: Simulationsupporting

confidence: 56%

Section: Simulationmentioning

confidence: 99%

Diagnostics for the structure of AGNs’ broad line regions with reverberation mapping data: confirmation of the two-component broad line region model

Zhu

Zhang

2010

Sci. China Phys. Mech. Astron.

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“…To examine whether SDSS J1707+6443 is consistent with the result of Matsuoka et al (2011), we estimated M BH and L bol /L Edd based on the velocity widths of C iv in the SDSS spectrum and Hβ in our MOIRCS spectrum. Note that it is debatable whether C iv-based or Hβ-based estimations are more accurate (see, e.g., Netzer et al 2004;Peterson et al 2004;Denney et al 2009). Therefore we used both emission lines to minimize possible systematic errors in the estimation of those parameters.…”

Section: Black Hole Mass and The Eddington Ratiomentioning

confidence: 99%

Near-infrared spectroscopy of a nitrogen-loud quasar SDSS J1707+6443

Araki

Nagao

Matsuoka

et al. 2012

A&A

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We present near-infrared spectroscopy of the z 3.2 quasar SDSS J1707+6443, obtained with MOIRCS on the Subaru Telescope. This quasar is classified as a "nitrogen-loud" quasar because of the fairly strong N iii] and N iv] semi-forbidden emission lines from the broad-line region (BLR) observed in its rest-frame UV spectrum. However, our rest-frame optical spectrum from MOIRCS shows strong [O iii] emission from the narrow-line region (NLR), suggesting that, at variance with the BLR, NLR gas is not metal-rich. To reconcile these contradictory results, there may be two alternative possibilities: (1) the strong nitrogen lines from the BLR are simply caused by a very high relative abundance of nitrogen and not by a very high BLR metallicity, or (2) the BLR metallicity is not representative of the metallicity of the host galaxy, which is better traced by the NLR. In either case, the strong broad nitrogen lines in the UV spectrum are ot indication of a chemically enriched host galaxy. We estimated the black hole mass and Eddington ratio of this quasar from the velocity width of both C iv and Hβ, which results in log(M BH /M ) = 9.50 and log(L bol /L Edd ) = −0.34. The relatively high Eddington ratio is consistent with our earlier result that strong nitrogen emission from BLRs is associated with high Eddington ratios. Finally, we detected significant [Ne iii] emission from the NLR, implying a quite high gas density of n e ∼ 10 6 cm −3 and suggesting a strong coupling between quasar activity and dense interstellar clouds in the host galaxy.

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“…For R > 3 pc, this lag is at least a century, and far longer lags are possible, as we shall see. This may be the reason why AGN showing other signs of super-Eddington phenomena (e.g., narrow-line Seyfert 1 galaxies) are nevertheless seen to have sub-Eddington luminosities (e.g., NGC 4051: Denney et al 2009). …”

Section: Accretion and Outflow In Active Galaxiesmentioning

confidence: 99%

Accretion and Outflow in Active Galaxies

King

2009

Proc. IAU

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Abstract. I review accretion and outflow in active galactic nuclei. Accreti4on appears to occur in a series of very small-scale, chaotic events, whose gas flows have no correlation with the largescale structure of the galaxy or with each other. The accreting gas has extremely low specific angular momentum and probably represents only a small fraction of the gas involved in a galaxy merger, which may be the underlying driver.Eddington accretion episodes in AGN must be common in order for the supermassive black holes to grow. I show that they produce winds with velocities v ∼ 0.1c and ionization parameters implying the presence of resonance lines of helium-like and hydrogen-like iron. The wind creates a strong cooling shock as it interacts with the interstellar medium of the host galaxy, and this cooling region may be observable in an inverse Compton continuum and lower-excitation emission lines associated with lower velocities. The shell of matter swept up by the shocked wind stalls unless the black hole mass has reached the value M σ implied by the M -σ relation. Once this mass is reached, further black hole growth is prevented. If the shocked gas did not cool as asserted above, the resulting ("energy-driven") outflow would imply a far smaller SMBH mass than actually observed. Minor accretion events with small gas fractions can produce galaxy-wide outflows, including fossil outflows in galaxies where there is little current AGN activity.

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A Revised Broad-Line Region Radius and Black Hole Mass for the Narrow-Line Seyfert 1 NGC 4051

Abstract: We present the first results from a high sampling rate, multi-month reverberation mapping campaign undertaken primarily at MDM Observatory with

Cited by 105 publications

References 77 publications

Diagnostics for the structure of AGNs’ broad line regions with reverberation mapping data: confirmation of the two-component broad line region model

Diagnostics for the structure of AGNs’ broad line regions with reverberation mapping data: confirmation of the two-component broad line region model

Near-infrared spectroscopy of a nitrogen-loud quasar SDSS J1707+6443

Accretion and Outflow in Active Galaxies

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