The central parsec of NGC 3783: a rotating broad emission line region, asymmetric hot dust structure, and compact coronal line region

Amorim, A.; Bauböck, M.; Brandner, W.; Bolzer, M.; Clénet, Y.; Davies, R. I.; Zeeuw, P. T. de; Dexter, Jason; Drescher, A.; Eckart, A.; Eisenhauer, F.; Schreiber, N. M. Förster; Gao, F.; Garcia, Paulo J. V.; Genzel, R.; Gillessen, S.; Gratadour, Damien; Hönig, S. F.; Kaltenbrunner, D.; Kishimoto, M.; Lacour, S.; Lutz, D.; Millour, F.; Netzer, H.; Ott, Thomas; Paumard, T.; Perraut, K.; Perrin, G.; Peterson, Bradley M.; Petrucci, Pierre-Olivier; Pfuhl, O.; Prieto, M. A.; Rouan, D.; Sánchez-Bermúdez, J.; Shangguan, J.; Shimizu, T.; Schartmann, M.; Stadler, J.; Sternberg, A.; Straub, O.; Straubmeier, C.; Sturm, E.; Tacconi, L. J.; Tristram, K. R. W.; Vermot, P.; Fellenberg, S. von; Waisberg, I.; Widmann, F.; Woillez, J.

doi:10.1051/0004-6361/202040061

Cited by 57 publications

(7 citation statements)

References 106 publications

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“…The determined BLR radius is 150 light days ∼ 0.126 pc, which is in agreement with the previous reverberation-mapping studies. Two more sources -NGC 3783 and IRAS 09149-6206 -observed with the same instrument [42,43] showed the same pattern using the broad Brγ line.…”

Section: Introductionmentioning

confidence: 59%

The Wind Dynamics of Super-Eddington Sources in FRADO

Naddaf

2022

Dynamics

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We perform non-hydrodynamical 2.5D simulations to study the dynamics of material above accretion disk based on the disk radiation pressure acting on dust. We assume a super-accreting underlying disk with the accretion rate of 10 times the Eddington rate with central black hole mass ranging from 107 up to 109M⊙. Such high accretion rates are characteristic for extreme sources. We show that for high accretors the radiatively dust-driving mechanism based on the FRADO model always leads to a massive outflow from the disk surface, and the failed wind develops only at larger radii. The outflow rate strongly depends on the black hole mass, and an optically thick energy-driven solution can exceed the accretion rate for masses larger than 108M⊙ but momentum-driven outflow does not exceed the accretion rate even for super-Eddington accretion, therefore not violating the adopted stationarity of the disk. However, even in this case the outflow from the disk implies a strong mechanical feedback.

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Section: Introductionmentioning

confidence: 59%

The Wind Dynamics of Super-Eddington Sources in FRADO

Naddaf

2022

Dynamics

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“…The similarities between the inclinations and opening angle constraints for Hβ and He II support the interpretation that both emission lines are probing different regions of the same thick disk of gas. While the median values of the opening angles might suggest that the Hβ emitting region is more "puffed up" than the He II emitting region, as might be expected for a bowl-shaped model of the BLR like that proposed by Goad et al (2012), the large uncertainties on the He II opening angle mean that the two values formally agree. As expected from the differences in their mean time delays reported by Bentz et al (2021), the He IIemitting region is significantly more compact and close to the central ionizing source than the Hβ-emitting region, demonstrating clear ionization stratification within the BLR (e.g., Peterson 1993…”

Section: Geometry and Kinematicsmentioning

confidence: 80%

A Detailed View of the Broad Line Region in NGC 3783 from Velocity-Resolved Reverberation Mapping

Bentz,

Williams,

Street

et al. 2021

Preprint

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We have modeled the full velocity-resolved reverberation response of the Hβ and He II optical broad emission lines in NGC 3783 to constrain the geometry and kinematics of the low-ionization and highionization broad line region. The geometry is found to be a thick disk that is nearly face on, inclined at ∼ 18 • to our line of sight, and exhibiting clear ionization stratification, with an extended Hβ-emitting region (r median = 10.07 +1.10 −1.12 light days) and a more compact and centrally-located He II-emitting region (r median = 1.33 +0.34 −0.42 light days). In the Hβ-emitting region, the kinematics are dominated by near-circular Keplerian orbits, but with ∼ 40% of the orbits inflowing. The more compact He IIemitting region, on the other hand, appears to be dominated by outflowing orbits. The black hole mass is constrained to be M BH = 2.82 +1.55 −0.63 × 10 7 M , which is consistent with the simple reverberation constraint on the mass based on a mean time delay, line width, and scale factor of f = 4.82. The difference in kinematics between the Hβ-and He II-emitting regions of the BLR is intriguing given the recent history of large changes in the ionizing luminosity of NGC 3783 and evidence for possible changes in the BLR structure as a result.

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“…Nevertheless, we bear in mind the difficulties in performing SA observations. Currently, there are only a few AGNs with SA observation results published (GRAVITY Collaboration et al 2018, 2020, 2021aBosco et al 2021). This situation might change with the upgraded GRAVITY+ and next-generation 30 m class telescopes.…”

Section: Practical Concerns With Spectroastrometric Rmmentioning

confidence: 99%

“…GRAVITY can achieve an angular astrometric resolution down to ∼10 μs (GRAVITY Collaboration et al 2018), sufficient to resolve the BLRs of bright AGNs. This achievement, together with the subsequent successful observations of two other AGNs (GRAVITY Collaboration et al 2020, 2021a, ushered in a new pathway toward BLR physics.…”

Section: Introductionmentioning

confidence: 97%

Spectroastrometric Reverberation Mapping of Broad-line Regions

Wang

2023

ApJ

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Spectroastrometry measures source astrometry as a function of wavelength/velocity. Reverberations of spectroastrometric signals naturally arise in broad-line regions (BLRs) of active galactic nuclei (AGNs) as a result of the continuum variations that drive responses of the broad emission lines with time delays. Such signals provide a new diagnostic for mapping BLR kinematics and geometry, complementary to the traditional intensity reverberation mapping (RM) technique. We present a generic mathematical formalism for spectroastrometric RM and show that under realistic parameters of a phenomenological BLR model, the spectroastrometric reverberation signals vary on a level of several to tens of microarcseconds, depending on the BLR size, continuum variability, and angular-size distance. We also derive the analytical expressions of spectroastrometric RM for an inclined ring-like BLR. We develop a Bayesian framework with a sophisticated Monte Carlo sampling technique to analyze spectroastrometric data and infer the BLR properties, including the central black hole mass and angular-size distance. We demonstrate the potential of spectroastrometric RM in spatially resolving BLR kinematics and geometry through a suite of simulation tests. The application to realistic observation data of 3C 273 obtains tentative, but enlightening results, reinforcing the practical feasibility of conducting spectroastrometric RM experiments on bright AGNs with the operating Very Large Telescope Interferometer as well as possibly with the planned next-generation 30 m class telescopes.

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The central parsec of NGC 3783: a rotating broad emission line region, asymmetric hot dust structure, and compact coronal line region

Cited by 57 publications

References 106 publications

The Wind Dynamics of Super-Eddington Sources in FRADO

The Wind Dynamics of Super-Eddington Sources in FRADO

A Detailed View of the Broad Line Region in NGC 3783 from Velocity-Resolved Reverberation Mapping

Spectroastrometric Reverberation Mapping of Broad-line Regions

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