AGN–starburst evolutionary connection: a physical interpretation based on radiative feedback

Ishibashi, W.; Fabian, A. C.

doi:10.1093/mnras/stw2063

Cited by 35 publications

(31 citation statements)

References 49 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The derived R l values are 3 × 10 −3 pc and 3 × 10 −4 pc, respectively, which are all much smaller than the torus sublimation radius, thereby conflicting with our initial assumption that the outflows are launched in the torus. In addition, the fully absorbed scenario is also inconsistent with observations (Leighly et al 2009); and more sophisticated calculations of radiation pressure implementing on dusty gas from the torus also indicated that the typical maximum outflow velocity is a few thousand km s −1 and hardly reaches v > 10000 km s −1 , even if an enhanced dust to gas ratio is adopted for luminous dusty quasars (e.g., Ishibashi & Fabian 2016;Ishibashi et al 2017). Therefore, we argue that the outflows in WPVS 007 may most probable to be launched in the region closer to the black hole, and the torus origin maybe less likely.…”

Section: Bal Velocity and Outflow Launch Radiusmentioning

confidence: 98%

On the origin of the dramatic spectral variability of WPVS 007

Wang

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We report the discovery of large-amplitude mid-infrared variabilities (MIR; ∼ 0.3 mag) in the Wide-field Infrared Survey Explorer W1 and W2 bands of the low-luminosity narrow-line Seyfert 1 galaxy WPVS 007, which exhibits prominent and varying broadabsorption lines (BALs) with blueshifted velocity up to ∼ 14000 km s −1 . The observed significant MIR variability, the UV to optical color variabilities in the Swift bands that deviate from the predictions of pure dust attenuation models, and the fact that Swift light curves can be well fitted by the stochastic AGN variability model suggest that its observed flux variabilities in UV-optical-MIR bands should be intrinsic, rather than owing to variable dust extinction. Furthermore, the variations of BAL features (i.e., trough strength and maximum velocity) and continuum luminosity are concordant. Therefore, we propose that the BAL variability observed in WPVS 007 is likely induced by the intrinsic ionizing continuum variation, alternative to the rotating-torus model proposed in a previous work. The BAL gas in WPVS 007 might be in the lowionization state as traced by its weak N v BAL feature; as the ionizing continuum strengthens, the C iv and Si iv column densities also increase, resulting in stronger BALs and the emergence of high-velocity components of the outflow. The outflow launch radius might be as small as ∼ 8 × 10 −4 pc under the assumption of being radiatively driven, but a large-scale origin (e.g., torus) cannot be fully excluded because of the unknown effects from additional factors, e.g., the magnetic field.

show abstract

Section: Bal Velocity and Outflow Launch Radiusmentioning

confidence: 98%

On the origin of the dramatic spectral variability of WPVS 007

Wang

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…Banerji et al 2015). In a broader context, we have proposed how such radiative feedback, which directly acts on the obscuring dusty gas, may provide a natural physical interpretation for the observed co-evolutionary sequence (Ishibashi & Fabian 2016). Therefore AGN radiative feedback naturally fits in the global picture of 'black hole-host galaxy coevolution' scenarios.…”

Section: The Importance Of Radiation Trappingmentioning

confidence: 99%

The energetics of AGN radiation pressure-driven outflows

Ishibashi

Fabian

Maiolino

2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The increasing observational evidence of galactic outflows is considered as a sign of active galactic nucleus (AGN) feedback in action. However, the physical mechanism responsible for driving the observed outflows remains unclear, and whether it is due to momentum, energy, or radiation is still a matter of debate. The observed outflow energetics, in particular the large measured values of the momentum ratio (ṗ/(L/c) ∼ 10) and energy ratio (Ė k /L ∼ 0.05), seems to favour the energy-driving mechanism; and most observational works have focused their comparison with wind energy-driven models. Here we show that AGN radiation pressure on dust can adequately reproduce the observed outflow energetics (mass outflow rate, momentum flux, and kinetic power), as well as the scalings with luminosity, provided that the effects of radiation trapping are properly taken into account. In particular, we predict a sub-linear scaling for the mass outflow rate (Ṁ ∝ L 1/2 ) and a super-linear scaling for the kinetic power (Ė k ∝ L 3/2 ), in agreement with the observational scaling relations reported in the most recent compilation of AGN outflow data. We conclude that AGN radiative feedback can account for the global outflow energetics, at least equally well as the wind energy-driving mechanism, and therefore both physical models should be considered in the interpretation of future AGN outflow observations.

show abstract

“…To demonstrate that the numerical setup is performing as expected we require an analytic solution to compare with. As an AGN feedback channel, radiation pressure on dust has been well studied via analytical models (Murray et al 2005;Ishibashi & Fabian 2015;Thompson et al 2015;Ishibashi & Fabian 2016;Ishibashi et al 2018). We follow the analytic model presented in Ishibashi & Fabian (2015) and Thompson et al (2015), also see Costa et al (2018a).…”

Section: Analytic Solutionmentioning

confidence: 99%

Radiative AGN feedback on a moving mesh: the impact of the galactic disc and dust physics on outflow properties

Barnes

Kannan

Vogelsberger

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Feedback from accreting supermassive black holes, active galactic nuclei (AGN), is now a cornerstone of galaxy formation models. In this work, we present radiation-hydrodynamic simulations of radiative AGN feedback using the novel AREPO-RT code. A central black hole emits radiation at a constant luminosity and drives an outflow via radiation pressure on dust grains. Utilising an isolated NFW halo we validate our setup in the single and multi-scattering regimes, with the simulated shock front propagation in excellent agreement with the expected analytic result. For a spherically symmetric NFW halo, an examination of the simulated outflow properties generated by radiative feedback demonstrates that they are lower than typically observed at a fixed AGN luminosity, regardless of the collimation of the radiation. We then explore the impact of a central disc galaxy and the assumed dust model on the outflow properties. The contraction of the halo during the galaxy's formation and modelling the production of dust grains results in a factor 100 increase in the halo's optical depth. Radiation is then able to couple momentum more efficiently to the gas, driving a stronger shock and producing a mass-loaded ∼ 10 3 M yr −1 outflow with a velocity of ∼ 2000 km s −1 , in agreement with observations. However, the inclusion of dust destruction mechanisms, like thermal sputtering, leads to the rapid destruction of dust grains within the outflow, reducing its properties below typically observed values. We conclude that radiative AGN feedback can drive outflows, but a thorough numerical and physical treatment is required to assess its true impact.

show abstract

AGN–starburst evolutionary connection: a physical interpretation based on radiative feedback

Cited by 35 publications

References 49 publications

On the origin of the dramatic spectral variability of WPVS 007

On the origin of the dramatic spectral variability of WPVS 007

The energetics of AGN radiation pressure-driven outflows

Radiative AGN feedback on a moving mesh: the impact of the galactic disc and dust physics on outflow properties

Contact Info

Product

Resources

About