Hubble Space Telescope FOS observations of KPD 0005 + 5106 - A subluminous WN-WC descendant with ongoing mass outflow?

Quantifying the AGN-driven outflows in ULIRGs (QUADROS) IV: HST/STIS spectroscopy of the sub-kpc warm outflow in F14394+5332

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz1755 ◽

2019 ◽

Vol 488 (2) ◽

pp. 1813-1821 ◽

Cited By ~ 1

Author(s):

C Tadhunter ◽

L Holden ◽

C Ramos Almeida ◽

D Batcheldor

Keyword(s):

Hubble Space Telescope ◽

Outer Part ◽

Ionization State ◽

Space Telescope ◽

High Ionization ◽

Mass Outflow ◽

Outflow Region ◽

First Time ◽

Imaging Spectrograph ◽

Luminous Infrared Galaxy

ABSTRACT Considerable uncertainties remain about the nature of warm, AGN-driven outflows and their impact on the evolution of galaxies. This is because the outflows are often unresolved in ground-based observations. As part of a project to study the AGN outflows in some of the most rapidly evolving galaxies in the local Universe, here we present Hubble Space Telescope (HST)/Space Telescope Imaging Spectrograph (STIS) observations of F14394+5332E that resolve the sub-kpc warm outflow for the first time in an ultra-luminous infrared galaxy. The observations reveal a compact, high-ionization outflow region (rmax ∼ 0.9 kpc) set in a more extensive (rmax ∼ 1.4 kpc) halo that is kinematically quiescent and has a lower ionization state. A large line width (600 < FWHM < 1500 km s−1) is measured throughout the outflow region, and the outflowing gas shows a steep velocity gradient with radius, with the magnitude of the blueshifted velocities increasing from ∼500 to 1800 km s−1 from the inner to the outer part of the outflow. We interpret the observations in terms of the local acceleration, and hydrodynamic destruction, of dense clouds as they are swept up in a hot, low-density wind driven by the AGN. We discuss the implications for measuring the mass outflow rates and kinetic powers for the AGN-driven outflows in such objects.

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Hubble Space Telescope Observations of [O III] Emission in Nearby QSO2s: Physical Properties of the Ionised Outflows

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa3239 ◽

2020 ◽

Author(s):

Anna Trindade Falcão ◽

S B Kraemer ◽

T C Fischer ◽

D M Crenshaw ◽

M Revalski ◽

...

Keyword(s):

Physical Properties ◽

Emission Line ◽

Hubble Space Telescope ◽

Radial Distance ◽

Flow Rates ◽

Space Telescope ◽

Bolometric Luminosity ◽

Mass Outflow ◽

Peak Outflow ◽

Imaging Spectrograph

Abstract We use Hubble Space Telescope (HST)/ Space Telescope Imaging Spectrograph (STIS) long-slit G430M and G750M spectra to analyse the extended [O III] λ5007 emission in a sample of twelve nearby (z >0.12) luminous (Lbol > 1.6 × 1045 erg s−1) QSO2s. The purpose of the study is to determine the properties of the mass outflows of ionised gas and their role in AGN feedback. We measure fluxes and velocities as functions of radial distances. Using Cloudy models and ionising luminosities derived from [O III] λ5007, 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 103M⊙ − 107M⊙ and peak outflow rates are 9.3 × 10−3M⊙ yr−1 to 10.3 M⊙ yr−1. The peak kinetic luminosities are 3.4 × 10−8 to 4.9 × 10−4 of the bolometric luminosity, which does not approach the 5.0 × 10−3 - 5.0 × 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 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.

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