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NASA Goddard Space Flight CenterAnna Trindade FalcãoMultiwavelength astrophysicist · Black-hole winds · AGN feedback
HST/WFC3 F814W continuum image of Mrk 477 from the left panel of published Figure 1. The image shows the galaxy's central stellar-light distribution used as input to the paper's GALFIT decomposition and enclosed-mass modeling. It is not an [O III] image, spectroscopic velocity map, Chandra image, X-ray-wind measurement, or feedback measurement.
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Research article · 2021

Hubble Space Telescope [O III] emission-line kinematics in two nearby QSO2s: a case for X-ray feedback

MNRAS 505(2), 3054–3069 (2021)

Paper-derived processed HST/WFC3 observational image · Published Figure 1 left panel

Published Figure 1, left panel. HST/WFC3 F814W continuum image of Mrk 477 used as the observational input to the three-component GALFIT stellar-light decomposition. The resulting model contributes to the enclosed stellar-mass profile used in the dynamical calculations. This panel contains no [O III] kinematics, X-ray measurement, or direct evidence of physical coupling or feedback.

Figure 1, left panel, from Trindade Falcão et al. 2021, “Hubble Space Telescope [O III] emission-line kinematics in two nearby QSO2s: a case for X-ray feedback,” MNRAS 505, issue 2, 3054–3069, DOI: 10.1093/mnras/stab1549. © 2021 The Author(s), published by Oxford University Press on behalf of the Royal Astronomical Society. HST: NASA/ESA; image analysis: Trindade Falcão et al. Converted from PNG to WebP for non-commercial research presentation under the RAS figure-reuse policy. No CC BY or broader public license is implied.

Research summary

Measured [O III] kinematics and model-dependent X-ray-wind interpretation

This paper models the dynamics of the narrow-line regions in Mrk 477 and Mrk 34 using previously measured HST [O III] morphology, spatially resolved line-centroid velocities and line widths, HST/WFC3 F814W stellar-mass profiles, and a 100 ks Chandra/ACIS observation of Mrk 34. The measured [O III] kinematics are compared with Cloudy-based radiative-acceleration, gas-expansion, and entrainment calculations. X-ray-wind velocities, mass-outflow rates, kinetic luminosities, and feedback efficiency are not directly measured: they require assumptions about ionization, dust, confinement, geometry, X-ray/[O III] mass correspondence, and the X-ray phase producing the observed optical disturbance. The proposed X-ray-driven disturbance, entrainment, efficient feedback, and Mrk 477-to-Mrk 34 evolutionary sequence remain interpretations or possibilities.