J/MNRAS/486/4290 AGN-driven winds through IR emission. II. (Baron+, 2019)
Discovering AGN-driven winds through their infrared emission.
II. Mass outflow rate and energetics.
Baron D., Netzer H.
<Mon. Not. R. Astron. Soc. 486, 4290-4303 (2019)>
=2019MNRAS.486.4290B 2019MNRAS.486.4290B (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; Infrared sources ; Spectroscopy
Keywords: galaxies: general - galaxies: evolution - galaxies: active -
galaxies: supermassive black holes - (galaxies:) quasars: general -
galaxies: star formation
Abstract:
The global influence of AGN-driven outflows remains uncertain, due to
a lack of large samples with accurately-determined outflow properties.
In the second paper of this series, we determine the mass and
energetics of ionized outflows is 234 type II AGN, the largest such
sample to date, by combining the infrared emission of the dust in the
wind (Paper I, Baron & Netzer, 2019MNRAS.482.3915B 2019MNRAS.482.3915B) with the emission
line properties. We provide new general expressions for the properties
of the outflowing gas, which depend on the ionization state of the
gas. We also present a novel method to estimate the electron density
in the outflow, based on optical line ratios and on the known location
of the wind. The inferred electron densities, ne∼104.5cm-3^, are
two orders of magnitude larger than typically assumed in most other
cases of ionized outflows. We argue that the discrepancy is due to the
fact that the commonly-used [SII]-based method underestimates the true
density by a large factor. As a result, the inferred mass outflow
rates and kinetic coupling efficiencies are
dM/dtout∼10-2(dM☉/yr) and epsilon=dE/dtkin/Lbol∼10-5
respectively, 1-2 orders of magnitude lower than previous estimates.
Our analysis suggests the existence of a significant amount of neutral
atomic gas at the back of the outflowing ionized gas clouds, with mass
that is a factor of a few larger than the observed ionized gas mass.
This has significant implications for the estimated mass and
energetics of such flows.
Description:
This data gives various ionized gas properties of the 234 systems
examined in this work. In particular, it gives the properties derived
from emission-line decomposition of the objects in the sample. The
data also contains information on the mass and energetics of the
outflows. The data is based on optical spectra obtained from the SDSS,
and on the publicly-available catalogs: MPA/JHU and ALPAKA.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table.dat 489 234 Properties of the 234 type II AGN sample
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Byte-by-byte Description of file: table.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- Plate SDSS identifier (plate) (SDSS_plate)
6- 10 I5 --- MJD SDSS identifier (MJD) (SDSS_mjd)
12- 14 I3 --- Fiber SDSS identifier (fiber) (SDSS_fiber)
16- 24 F9.7 --- z Redshift (redshift)
26- 36 F11.6 0.1nm OIIIWLn Central wavelength of narrow [OIII]
line (oiiiwlnarrow)
38- 48 F11.6 0.1nm OIIIWLb Central wavelength of broad [OIII]
line (oiiiwlbroad)
50- 62 F13.9 km/s sigmab Velocity dispersion of broad lines
(sigma_broad)
64- 77 F14.11 [-] logOIII/Hbn log([OIII]/Hbeta) of narrow lines
(logoiiihbeta_narrow)
79- 94 F16.13 [-] logNII/Han log([NII]/Halpha) of narrow lines
(logniihalpha_narrow)
96-109 F14.11 [-] logOIII/Hbb log([OIII]/Hbeta) of broad lines
(logoiiihbeta_broad)
111-126 F16.13 [-] logNII/Hab log([NII]/Halpha) of broad lines
(logniihalpha_broad)
128-140 F13.8 cm-3 SIIeden ? [SII]-based electron density of the
broad lines (siielectrondensity)
142-152 F11.8 [10-7W] logLbolOI ? [OI]-based AGN bolometric
luminosity (loglboloi)
154-164 F11.8 [10-7W] logLbolHb Hbeta-based AGN bolometric
luminosity (loglbolhbeta)
166-176 F11.8 [10-7W] logLOIIIb Dust-corrected broad [OIII]
luminosity (logloiii_broad)
178-188 F11.8 [10-7W] logLhab Dust-corrected broad Halpha
luminosity (loglhalpha_broad)
190-198 F9.6 [Msun] logM* Stellar mass from the MPA/JHU
catalog (logstellarmass)
200-211 F12.9 [Msun/yr] logSFR Star formation rate from the MPA/JHU
catalog (log_SFR)
213-228 F16.14 mag E(B-V)n E(B-V) color excess towards narrow
emission lines (ebv_narrow)
230-246 F17.15 mag E(B-V)b E(B-V) color excess towards broad
emission lines (ebv_broad)
248-263 F16.13 kpc rdust Mass-weighted location of the dust in
the outflow (see Paper I, Baron &
Netzer (2019MNRAS.482.3915B 2019MNRAS.482.3915B)
(rdustkpc)
265-287 F23.15 [cm-3] logUeden logU-based electron density of the
broad lines (logUelectrondensity)
289-302 F14.11 [-] logU logU ionization parameter of the
broad lines (logU)
304-327 F24.14 Msun dM/dtoutHa Outflowing ionized gas mass, based on
broad Halpha (Mouthalpha)
329-350 F22.19 Msun/yr dM/dtHa Ionized gas mass outflow rate, based
on broad Halpha (Mdothalpha)
352-373 E22.17 10-7W EkinHa Kinetic power in the wind, based on
broad Halpha (Ekinhalpha)
375-396 E22.17 --- EpsilonHa Coupling efficiency, based on broad
Halpha (Epsilon_halpha)
398-421 F24.14 Msun dM/dtOIII Outflowing ionized gas mass, based on
broad [OIII] (Moutoiii)
423-443 F21.19 Msun/yr dM/dt_OIII Ionized gas mass outflow rate, based
on broad [OIII] (Mdotoiii)
445-466 E22.17 10-7W EkinOIII Kinetic power in the wind, based on
broad [OIII] (Ekinoiii)
468-489 E22.17 --- EpsilonOIII Coupling efficiency, based on broad
[OIII] (Epsilon_oiii)
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Acknowledgements:
Dalya Baron, dalyabaron(at)gmail.com
References:
Baron & Netzer, Paper I 2019MNRAS.482.3915B 2019MNRAS.482.3915B
(End) Dalya Baron [TAU, Israel, Patricia Vannier [CDS] 12-Apr-2019