TY - JOUR

T1 - Hubble Space Telescope observations of [O III] emission in nearby QSO2s

T2 - physical properties of the ionized outflows

AU - Falcao, Anna Trindade

AU - Kraemer, S. B.

AU - Fischer, T. C.

AU - Crenshaw, D. M.

AU - Revalski, M.

AU - Schmitt, H. R.

AU - Vestergaard, M.

AU - Elvis, M.

AU - Gaskell, C. M.

AU - Hamann, F.

AU - Ho, L. C.

AU - Hutchings, J.

AU - Mushotzky, R.

AU - Netzer, H.

AU - Storchi-Bergmann, T.

AU - Turner, T. J.

AU - Ward, M. J.

PY - 2021/1/1

Y1 - 2021/1/1

N2 - We use Hubble Space Telescope/Space Telescope Imaging Spectrograph long-slit G430M and G750M spectra to analyse the extended [O III] lambda 5007 emission in a sample of 12 nearby (z <0.12) luminous (L-bol > 1.6 x 10(45) erg s(-1)) QSO2s. The purpose of the study is to determine the properties of the mass outflows of ionized gas and their role in active galactic nucleus feedback. We measure fluxes and velocities as functions of radial distances. Using CLOUDY models and ionizing luminosities derived from [OIII] lambda 5007, we are able to estimate the densities for the emission-line gas. From these results, we derive masses of [O III]-emitting gas, mass outflow rates, kinetic energies, kinetic luminosities, momenta, and momentum flow rates as a function of radial distance for each of the targets. For the sample, masses are several times 10(3)-10(7) M-circle dot and peak outflow rates are from 9.3 x 10(-3) to 10.3 M-circle dot yr(-1). The peak kinetic luminosities are (3.4 x 10(-8))-(4.9 x 10(-4)) of the bolometric luminosity, which does not approach the (5.0 x 10(-3))-(5.0 x 10(-2)) range required by some models for efficient feedback. For Mrk 34, which has the largest kinetic luminosity of our sample, in order to produce efficient feedback there would have to be 10 times more [O III]-emitting gas than that we detected at its position of maximum kinetic luminosity. Three targets show extended [O III] emission, but compact outflow regions. This may be due to different mass profiles or different evolutionary histories.

AB - We use Hubble Space Telescope/Space Telescope Imaging Spectrograph long-slit G430M and G750M spectra to analyse the extended [O III] lambda 5007 emission in a sample of 12 nearby (z <0.12) luminous (L-bol > 1.6 x 10(45) erg s(-1)) QSO2s. The purpose of the study is to determine the properties of the mass outflows of ionized gas and their role in active galactic nucleus feedback. We measure fluxes and velocities as functions of radial distances. Using CLOUDY models and ionizing luminosities derived from [OIII] lambda 5007, we are able to estimate the densities for the emission-line gas. From these results, we derive masses of [O III]-emitting gas, mass outflow rates, kinetic energies, kinetic luminosities, momenta, and momentum flow rates as a function of radial distance for each of the targets. For the sample, masses are several times 10(3)-10(7) M-circle dot and peak outflow rates are from 9.3 x 10(-3) to 10.3 M-circle dot yr(-1). The peak kinetic luminosities are (3.4 x 10(-8))-(4.9 x 10(-4)) of the bolometric luminosity, which does not approach the (5.0 x 10(-3))-(5.0 x 10(-2)) range required by some models for efficient feedback. For Mrk 34, which has the largest kinetic luminosity of our sample, in order to produce efficient feedback there would have to be 10 times more [O III]-emitting gas than that we detected at its position of maximum kinetic luminosity. Three targets show extended [O III] emission, but compact outflow regions. This may be due to different mass profiles or different evolutionary histories.

KW - galaxies: active

KW - galaxies: kinematics and dynamics

KW - galaxies: quasars

KW - NARROW-LINE REGION

KW - ACTIVE GALACTIC NUCLEI

KW - BLACK-HOLES

KW - SEYFERT-1 GALAXIES

KW - STAR-FORMATION

KW - AGN OUTFLOWS

KW - GAS

KW - FEEDBACK

KW - QUASARS

KW - ULTRAVIOLET

U2 - 10.1093/mnras/staa3239

DO - 10.1093/mnras/staa3239

M3 - Journal article

VL - 500

SP - 1491

EP - 1504

JO - Royal Astronomical Society. Monthly Notices

JF - Royal Astronomical Society. Monthly Notices

SN - 0035-8711

IS - 1

ER -