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HST observations of [O III] emission in nearby QSO2s: Physical properties of the outflows

Published online by Cambridge University Press:  29 March 2021

Anna Trindade Falcao Open the ORCID record for Anna Trindade Falcao [Opens in a new window] ,
S. B. Kraemer Open the ORCID record for S. B. Kraemer [Opens in a new window] ,
T. C. Fischer ,
D. M. Crenshaw Open the ORCID record for D. M. Crenshaw [Opens in a new window] ,
M. Revalski  and
H. R. Schmitt Open the ORCID record for H. R. Schmitt [Opens in a new window]
Anna Trindade Falcao
Affiliation:
Institute for Astrophysics and Computational Sciences, Department of Physics, The Catholic University of America, Washington, DC, USA
S. B. Kraemer
Affiliation:
Institute for Astrophysics and Computational Sciences, Department of Physics, The Catholic University of America, Washington, DC, USA
T. C. Fischer
Affiliation:
Space Telescope Science Institute, Baltimore, MD, USA
D. M. Crenshaw
Affiliation:
Department of Physics and Astronomy, Georgia State University, Atlanta, GA, USA
M. Revalski
Affiliation:
Space Telescope Science Institute, Baltimore, MD, USA
H. R. Schmitt
Affiliation:
Naval Research Laboratory, Washington, DC, USA
Rights & Permissions [Opens in a new window]

Abstract

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We used Space Telescope Imaging Spectrograph (STIS) long slit medium-resolution G430M and G750M spectra to analyze the extended [O III] λ5007 emission in a sample of twelve QSO2s from Reyes et al. (2008). The purpose of the study was to determine the properties of the mass outflows and their role in AGN feedback. We measured fluxes and velocities as functions of deprojected radial distances. Using photoionization models and ionizing luminosities derived from [O III], we were able to estimate the densities for the emission-line gas. From these results, we derived masses, mass outflow rates, kinetic energies and kinetic luminosity rates as a function of radial distance for each of the targets. Masses are several times 103 - 107 solar masses, which are comparable to values determined from a recent photoionization study of Mrk 34 (Revalski). Additionally, we are studying the possible role of X-ray winds in these QSO2s.

Keywords

galaxies: activegalaxies: QSO2galaxies: kinematics and dynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S359: Galaxy Evolution and Feedback across Different Environments , March 2019 , pp. 269 - 271
Copyright
© The Author(s), 2021. Published by Cambridge University Press on behalf of International Astronomical Union

References

Crenshaw, et al. 2015, ApJ, 799, 83 CrossRefGoogle Scholar
Di, Matteo, et al. 2005, Nature,433, 604CrossRefGoogle Scholar
Ferland, et al. 2017, RMxAA, 49, 1379 Google Scholar
Fischer, et al. 2017, ApJ, 834, 30 CrossRefGoogle Scholar
Fischer, T. C., Kraemer, S. B., Schmitt, H. R., et al. 2018, ApJ, 856, 102 CrossRefGoogle Scholar
Hopkins & Elvis 2010, MNRAS, 401, 7 CrossRefGoogle Scholar
Kraemer, et al. 2000, ApJ, 532, 256 CrossRefGoogle Scholar
Mullaney, et al. 2013, MNRAS, 433, 622 CrossRefGoogle Scholar
Revalski, M., Crenshaw, D. M., Kraemer, S. B., et al. 2018, ApJ, 856, 46 CrossRefGoogle Scholar
Reyes, et al. 2008, AJ, 136, 2373 CrossRefGoogle Scholar