J/MNRAS/509/4457 Catalogue of outflows in E+A galaxies (Baron+, 2022)
Multiphase outflows in post-starburst E+A galaxies.
I. General sample properties and the prevalence of obscured starbursts.
Baron D., Netzer H., Lutz D., Prochaska J.X., Davies R.I.
<Mon. Not. R. Astron. Soc. 509, 4457-4479>
=2022MNRAS.509.4457B 2022MNRAS.509.4457B (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies ; Active gal. nuclei ; Stars, A-type ; Optical ;
Infrared sources ; Photometry ; Spectroscopy ;
Velocity dispersion ; Colors ; Line Profiles ; Mass loss
Keywords: galaxies: active; galaxies - evolution - galaxies: general -
galaxies: interactions - galaxies: star formation
Abstract:
E+A galaxies are believed to be a short phase connecting major merger
ultraluminous infrared galaxies (ULIRGs) with red and dead elliptical
galaxies. Their optical spectrum suggests a massive starburst that was
quenched abruptly, and their bulge-dominated morphologies with tidal
tails suggest that they are merger remnants. Active galactic nucleus
(AGN)-driven winds are believed to be one of the processes responsible
for the sudden quenching of star formation and for the expulsion
and/or destruction of the remaining molecular gas. Little is known
about AGN-driven winds in this short-lived phase. In this paper, we
present the first and unique sample of post-starburst galaxy
candidates with AGNs that show indications of ionized outflows in
their optical emission lines. Using Infrared Astronomical
Satellite-far infrared (IRAS-FIR) observations, we study the star
formation in these systems and find that many systems selected to have
post-starburst signatures in their optical spectrum are in fact
obscured starbursts. Using SDSS spectroscopy, we study the stationary
and outflowing ionized gas. We also detect neutral gas outflows in 40
per cent of the sources with mass outflow rates 10-100 times more
massive than in the ionized phase. The mean mass outflow rate and
kinetic power of the ionized outflows in our sample
(dM/dt ∼ 1M☉/yr, dE/dt ∼ 1041 erg/s) are larger than those
derived for active galaxies of similar AGN luminosity and stellar
mass. For the neutral outflow (dM/dt ∼ 10M☉/yr, dE/dt ∼ 1042 erg/s),
their mean is smaller than that observed in (U)LIRGs with and without
AGN.
Description:
Although some studies presented indirect evidence for AGN feedback
taking place in E+A galaxies (e.g. Kaviraj et al. 2007MNRAS.382..960K 2007MNRAS.382..960K;
French et al. 2018ApJ...862....2F 2018ApJ...862....2F, Cat. J/ApJ/862/2), little is known
about this process, in particular about AGN-driven winds, in this
short-lived phase. Tremonti et al. (2007ApJ...663L..77T 2007ApJ...663L..77T) found
high-velocity ionized outflows, traced by Mg II absorption, in z ∼ 0.6
post-starburst galaxies. Using an unsupervised Machine Learning
algorithm that searches for rare phenomena in a dataset, Baron &
Poznanski (2017MNRAS.465.4530B 2017MNRAS.465.4530B, Cat. J/MNRAS/465/4530) found a
post-starburst E+A galaxy with massive AGN-driven winds traced by
ionized emission lines. In a follow-up study in Baron et al.
(2017MNRAS.470.1687B 2017MNRAS.470.1687B), we used newly obtained ESI/Keck 1D spectroscopy
to model the star formation history (SFH) and the ionized outflows in
this system. In Baron et al. (2018MNRAS.480.3993B 2018MNRAS.480.3993B,
2020MNRAS.494.5396B 2020MNRAS.494.5396B), we used the integral field units (IFUs)
KCWI/Keck and MUSE/VLT to study the spatial distribution of the stars,
gas, and outflows, in two post-starburst galaxies hosting AGNs and
winds. This might suggest that AGN feedback, in the form of
galactic-scale outflows, is significant in the E+A galaxy phase.
The goal of this paper is to construct the first well-defined sample
of post starburst E+A galaxies with both AGNs and ionized outflows.
The main difference between our sample and those presented in past
studies is that the outflows in our sample are traced by strong
optical emission lines, allowing us to constrain the mass and
energetics of the winds (see e.g. Baron & Netzer 2019MNRAS.486.4290B 2019MNRAS.486.4290B,
Cat. J/MNRAS/486/4290). Using this sample, we aim to check whether AGN
feedback, in the form of galactic outflows, can have a significant
effect on their hosts evolution, (i.e see section Introduction).
First, we select post-starburst galaxies by an optical spectrum with
strong Balmer absorption lines, this evolutionary stage must be very
short, due to the short lifetime of A-type stars, making such systems
rare and comprising only ∼3 per cent of the general galaxy population.
Due to the AGN duty cycle, post-starburst galaxies hosting AGNs are
expected to be even rarer, and post-starburst galaxies hosting AGNs
and outflows are expected to be extremely rare. We describe our method
to select such sources from the Sloan Digital Sky Survey (SDSS; York
et al. 2000AJ....120.1579Y 2000AJ....120.1579Y) using their integrated (1D) optical
spectra of more than 2 million galaxies, (i.e refer to the section
Sample selection). Using model-fitting unsupervised ML approaches, we
found a total of 520 post starburst E+A galaxies with narrow emission
lines that are consistent with pure AGN photoionization. Out of these,
215 show evidence for an ionized outflow in one emission line, and 144
in multiple lines. Deriving outflow properties, such as mass outflow
rate and kinetic power, requires the detection of the outflow in
multiple emission lines (see e.g. Baron & Netzer 2019MNRAS.486.4290B 2019MNRAS.486.4290B,
Cat. J/MNRAS/486/4290). We therefore restrict the analysis to the 144
sources for which we detected multiple broad emission lines.
Next, from IRAS FIR 12, 15, 60, and 100 µm data and SDSS optical
spectra, we extract metadata properties on our 144 E+A galaxies and
AGN such as component luminosities (i.e sections 3.1 FIR data from
IRAS, 3.2.1 Stellar properties, 3.2.2 Ionized and neutral gas
properties and 3.2.3 AGN properties). We present optical and FIR
properties in two metadata tables mdat1fg.dat and mdat2fg.dat.
Finally, using these metadata and optical emission line spectra (i.e
see section 3.2.2 and 3.2.4 Outflow energetics), we estimated the
ionized and neutral outflow properties are based on various earlier
methods. Our results are presented in two groups, firstly ionized gas
results are divided in 4 tables according to parameters variations
r = (0.3,1,3) kpc and ne = 103 cm-3 as ionrmin.dat, ionravg.dat,
ionrmax.dat and ioncstn.dat. Secondly, neutral gas results are divided
in 3 tables according to parameter variations r = (0.3,1,3) kpc as
ntralmin.dat, ntralavg.dat and ntralmax.dat.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
mdat1fg.dat 108 144 Metadata properties part 1 of our 144 galaxies
sample
mdat2fg.dat 448 144 *Metadata properties part 2 of our 144 galaxies
sample
ionrmin.dat 143 144 Ionized outflow properties assuming an outflow
extent of 0.3 kpc
ionravg.dat 143 144 Ionized outflow properties assuming an outflow
extent of 1.0 kpc
ionrmax.dat 143 144 Ionized outflow properties assuming an outflow
extent of 3.0 kpc
ioncstn.dat 143 144 *Ionized outflow properties assuming an outflow
extent of 1.0 kpc under the assumption of
ne = 103 cm-3
ntralmin.dat 140 144 Neutral outflow properties assuming an outflow
extent of 0.3 kpc
ntralavg.dat 140 144 Neutral outflow properties assuming an outflow
extent of 1.0 kpc
ntralmax.dat 140 144 Neutral outflow properties assuming an outflow
extent of 3.0 kpc
--------------------------------------------------------------------------------
Note on mdat2fg.dat: We obtained the emission line spectra by subtracting
the best-fitting stellar models from the observed spectra. We modelled each
emission line as a sum of two Gaussians, one which represents the narrow
component and one that represents the broader, outflowing, component, (i.e
please refer to section 3.2.2 Ionized and neutral gas properties).
Note on ioncstn.dat: As explained in the 3.2.4 Outflow energetics, in
section 4.3, we use the three sets to perform a qualitative comparison of the
outflow properties in post-starburst E+A galaxies with those observed in other
systems (type II AGN and ULIRGs). Finally, these properties were derived using
estimates of the electron density, which in turn depends on LAGN through the
ionization parameter method. Therefore, we expect these properties to be
correlated with LAGN. In Section 4.3.3, we examine the main driver of the
observed outflows, by looking for correlations between the outflow properties
and LAGN and LSF. To avoid this dependency, we estimated (M,dM/dt,dE/dt)
under the assumption of constant ne = 103 cm-3. Assuming r = 1 kpc, this
combination of electron density and outflow extent is roughly consistent with
the observed line ratios in our sources.
--------------------------------------------------------------------------------
See also:
J/ApJ/862/2 : Post-starburst galaxy ages from SDSS (French+, 2018)
J/MNRAS/465/4530 : outlier detection algorithm for SDSS galaxies (Baron+, 2017)
J/MNRAS/486/4290 : AGN-driven winds through IR emission. II. (Baron+, 2019)
J/AJ/128/1002 : SDSS candidate type II quasars. II (Zakamska+, 2004)
https://www.sdss4.org/dr16/algorithms/qso_catalog : SDSS QSO DR16 home page
http://www.sdss3.org/ : SDSS-III home page
https://irsa.ipac.caltech.edu/Missions/iras.html : IRAS archive page
https://irsa.ipac.caltech.edu/applications/Scanpi/ : IRAS Scanpi tool
Byte-by-byte Description of file: mdat1fg.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Id ? Identifier number (id)
5- 5 I1 --- f_Id [0/1]?=- Flag indicates whether a source is
detected in FIR or not (is_detected) (1)
7- 24 F18.15 [10-7W] log(LSF) ?=- Logarthim of the star formation
luminosity derived from 60 micron by IRAS,
in units of erg/sec (logLSFFIR) (2)
26- 28 F3.1 [10-7W] e_log(LSF) Logarithm of the uncertainty of L(SF)
(logLSFFIR_err) (2)
30- 47 F18.15 [10-7W] log(LAGN) Logarithm of the AGN bolometric luminosity
in units of erg/sec (log_LAGN) (3)
49- 51 F3.1 [10-7W] e_log(LAGN) Logarithm of the uncertainty of L(AGN)
(logLAGNerr) (3)
53- 70 F18.15 [Msun] logM*16 ?=- The 16th percentile of the optical
stellar mass distribution
(logMopt_p16) (4)
72- 89 F18.15 [Msun] logM*50 ?=- The median 50th percentile of the
optical stellar mass distribution
(logMopt_p50) (4)
91-108 F18.15 [Msun] logM*84 ?=- The 84th percentile of the optical
stellar mass distribution
(logMopt_p84) (4)
--------------------------------------------------------------------------------
Note (1): Flag taking the values 1 and 0 respectively. If 0, the logLSFFIR
represents an upper limit on L(SF). To analyse the data, we used
scanpi3 (Helou & Walker 1988iras....7.....H 1988iras....7.....H), which is a tool for
stacking the calibrated survey scans. It allows one to extract the
flux of extended faint sources and to estimate upper limits for
undetected sources. Our use of scanpi to obtain FIR fluxes for nearby
AGNs follows the IRAS. The scanpi output includes the best-fitting
flux density (fv), the root mean square (RMS) deviation of the
residuals after the subtraction of the best-fitting template
(σ), and the offset of the peak of the best-fitting template
from the specified galaxy coordinates (Δ). The goodness of the
fit is represented by the correlation coefficient between the
best-fitting template and the data (ρ). Inspired by the approach
presented in Zakamska et al. (2004AJ....128.1002Z 2004AJ....128.1002Z,
Cat. J/AJ/128/1002), we consider a source detected in 60 µm if the
following requirements are met, ρ > 0.8, Δ < 0.4', and
fv/σ > 3. For the undetected sources, we defined their 60 µm
flux upper limit to be f + 3σ and its uncertainty to be σ,
where f is the reported flux. Out of the 144 galaxies in our sample,
60 are detected by more than 3σ at 60 µm, 79 are upper
limits, and 5 have no IRAS scans around their coordinates. We then
used the measured fluxes and upper limits to estimate the star
formation luminosity (LSF) and the SFR, (i.e refer to 3.1 FIR data
from IRAS section).
Note (2): For this we used the Chary & Elbaz (2001ApJ...556..562C 2001ApJ...556..562C, CE01)
templates to establish the relation between νLν luminosities
in our sample, the LSF/νLν ratio of the CE01 templates is
centred around 1.716, with a scatter of 0.0885 dex. We therefore
defined LSF = 1.716νLν(60µm) and adopted a conservative
uncertainty of 0.2 dex, (i.e see section 3.1 FIR data from IRAS).
Note (3): Derived from optical emission lines. We estimated the AGN bolometric
luminosity, LAGN, using the dust-corrected narrow line
luminosities of Hβ, [O I], and [O III]. Netzer
(2009MNRAS.399.1907N 2009MNRAS.399.1907N) presented two methods to estimate LAGN.
The first method is based on the narrow Hβ and [O III]
luminosities (equation 1 in Netzer 2009MNRAS.399.1907N 2009MNRAS.399.1907N),
and the second is based on the narrow [O I] and [O III] luminosities
(equation 3 in Netzer 2009MNRAS.399.1907N 2009MNRAS.399.1907N). We estimated LAGN using
the two methods and found consistent results for all the objects in
our sample. We adopted a conservative uncertainty of 0.3 dex for
LAGN (see Netzer 2009MNRAS.399.1907N 2009MNRAS.399.1907N for additional details),
(i.e see section 3.2.3 AGN properties).
Note (4): Extracted from SDSS casjobs logarithm of the stellar mass.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: mdat2fg.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Id ? Identifier number (id)
5- 8 I4 --- Plate Spectroscopic SDSS plate of the
object (plate)
10- 14 I5 --- MJD Spectroscopic SDSS MJD of the
object (mjd)
16- 19 I4 --- Fiber Spectroscopic SDSS fiberID of the
object (fiber)
21- 40 F20.18 --- z Redshift (redshift)
42- 59 F18.15 [10-7W] logLW4 The logarithm of the luminosity
in W4 band in WISE in units of erg/sec
(log_LW4)
61- 83 F23.19 [10-7W] e_logLW4 Logarithm of the uncertainty of
L(W4) (logLW4err)
85-104 F20.18 mag E(B-V) E(B-V) color excess towards
the stars (ebv_stars) (1)
106-123 F18.14 km/s sigma* The stellar velocity dispersion
(sigma_stars) (1)
125-144 F20.18 Gyr WageY The luminosity-weighted age of stars
younger than 1 Gyr (age_young) (1)
146-165 F20.16 Gyr WageO The luminosity-weighted age of stars
older than 1 Gyr (age_old) (1)
167-187 F21.18 mag E(B-V)N The E(B-V) color excess towards
the narrow kinematic component of the
ionized gas (ebvlinesnarrow) (2)
189-210 E22.17 10-7W LHaN The luminosity of the narrow Halpha
component in units of erg/sec
(LHalphanarrow)
212-233 E22.17 10-7W LOIIIN The luminosity of the narrow [OIII]
component in units of erg/sec
(LOIIInarrow)
235-252 F18.14 km/s sigmalN The velocity dispersion in the narrow
component of the ionized lines
(sigmalinesnarrow)
254-274 F21.18 [-] log([NII]/Ha)N The log([NII]/Halpha) ratio for the
narrow kinematic component
(NIIHalpharatio_narrow)
276-297 F22.19 [-] log([OIII]/Hb)N The log([OIII]/Hbeta) ratio for the
narrow kinematic component
(OIIIHbetaratio_narrow)
299-318 F20.17 mag E(B-V)B The E(B-V) towards the broad kinematic
component of the ionized gas
(ebvlinesbroad) (2)
320-341 E22.17 10-7W LHaB The luminosity of the broad Halpha
component in units of erg/sec
(LHalphabroad)
343-364 E22.17 10-7W LOIIIB The luminosity of the broad [OIII]
component in units of erg/sec
(LOIIIbroad)
366-383 F18.14 km/s sigmalB The velocity dispersion in the broad
component of the ionized lines
(sigmalinesbroad)
385-402 F18.13 km/s VmaxlB The maximal outflow broad lines
velocity (vmaxlines_broad) (3)
404-426 F23.20 [-] log([NII]/Ha)B The log([NII]/Halpha) ratio for the
broad kinematic component
(NIIHalpharatio_broad)
428-448 F21.18 [-] log([OIII]/Hb)B The log([OIII]/Hbeta) ratio for the
broad kinematic component
(OIIIHbetaratio_broad)
--------------------------------------------------------------------------------
Note (1): Derived by fitting a stellar population synthesis model to the optical
spectrum (i.e see 3.2.1 Stellar properties section).
Note (2): Derived from emission line decomposition of the optical emission
lines, please refer to 3.2.2 Ionized and neutral gas properties
section, specifically the equation (1). We estimated the colour excess
for the narrow and broad components separately. We then estimated the
dust-corrected line luminosities using the measured E(B-V).
Note (3): We defined the maximum blueshifted outflow velocity as
vionmax = Δvion -2σion, where Δvion is the
velocity shift of the broad lines with respect to systemic and
σion is the velocity dispersion, (i.e 3.2.2 Ionized and
neutral gas properties).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: ionrmin.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Id ? Identifier number (id)
5- 7 F3.1 kpc r0.3 Assumed outflow extent in kpc (r=0.3)
9- 27 F19.14 km/s Voutr0.3 Outflow velocity in km/sec (voutr=0.3) (G4)
29- 47 F19.16 [-] logUr0.3 Logarithm of the ionization parameter
(logUr=0.3)
49- 72 F24.16 cm-3 ner0.3 Electron density (ner=0.3)
74- 97 F24.13 Msun Mr0.3 Outflowing gas mass according to the Halpha
emission line (Mhalphar=0.3) (G3)
99-120 F22.18 Msun/yr dM/dtr0.3 Mass outflow rate according to the Halpha
emission line (Mdothalphar=0.3) (G3)
122-143 E22.17 10-7W dE/dtr0.3 Kinetic power in the wind according to the
Halpha emission line (Edothalphar=0.3) (G3)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: ionravg.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Id ? Identifier number (id)
5- 7 F3.1 kpc r1.0 Assumed outflow extent in kpc (r=1.0)
9- 27 F19.14 km/s Voutr1.0 Outflow velocity in km/sec (voutr=1.0) (G4)
29- 47 F19.16 [-] logUr1.0 Logarithm of the ionization parameter
(logUr=1.0)
49- 72 F24.16 cm-3 ner1.0 Electron density (ner=1.0)
74- 97 F24.13 Msun Mr1.0 Outflowing gas mass according to the Halpha
emission line (Mhalphar=1.0) (G3)
99-120 F22.18 Msun/yr dM/dtr1.0 Mass outflow rate according to the Halpha
emission line (Mdothalphar=1.0) (G3)
122-143 E22.17 10-7W dE/dtr1.0 Kinetic power in the wind according to the
Halpha emission line (Edothalphar=1.0) (G3)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: ionrmax.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Id ? Identifier number (id)
5- 7 F3.1 kpc r3.0 Assumed outflow extent in kpc (r=3.0)
9- 27 F19.14 km/s Voutr3.0 Outflow velocity in km/sec (voutr=3.0) (G4)
29- 47 F19.16 [-] logUr3.0 Logarithm of the ionization parameter
(logUr=3.0)
49- 72 F24.16 cm-3 ner3.0 Electron density (ner=3.0)
74- 97 F24.13 Msun Mr3.0 Outflowing gas mass according to the Halpha
emission line (Mhalphar=3.0) (G3)
99-120 F22.18 Msun/yr dM/dtr3.0 Mass outflow rate according to the Halpha
emission line (Mdothalphar=3.0) (G3)
122-143 E22.17 10-7W dE/dtr3.0 Kinetic power in the wind according to the
Halpha emission line (Edothalphar=3.0) (G3)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: ioncstn.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Id ? Identifier number (id)
5- 7 F3.1 kpc r1.0-n1000 Assumed outflow extent in kpc (r=1.0)
9- 27 F19.14 km/s Voutr1.0-n1000 Outflow velocity in km/sec
(vout_r=1.0,n=1000) (G4)
29- 47 F19.16 [-] logUr1.0-n1000 Logarithm of the ionization parameter
(logUr=1.0,n=1000)
49- 72 F24.16 cm-3 ne1000 Electron density (ne=1000)
74- 97 F24.13 Msun Mr1.0-n1000 Outflowing gas mass according to the
Halpha emission line
(Mhalphar=1.0,n=1000) (G3)
99-120 F22.18 Msun/yr dM/dtr1.0-n1000 Mass outflow rate according to the
Halpha emission line
(Mdothalphar=1.0,n=1000) (G3)
122-143 E22.17 10-7W dE/dtr1.0-n1000 Kinetic power in the wind according
to the Halpha emission line
(Edothalphar=1.0,n=1000) (G3)
--------------------------------------------------------------------------------
Byte-by-byte Description of file:ntralmin.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Id ? Identifier number (id)
5 I1 --- f_Id [0/1] Flag indicates whether an outflow was
detected through NaID absorption
(is_detected) (G1)
7- 9 F3.1 kpc r0.3 ?=- Assumed outflow extent in kpc (r=0.3)
11- 29 F19.14 km/s Vmaxr0.3 ?=- Maximum outflow velocity (Vmaxr=0.3)
(G1)
31- 52 E22.17 cm-2 NHIr0.3 ?=- Hydrogen column density extracted from
the NaID fitting (NHIr=0.3) (G2)
54- 72 F19.17 --- Cfr0.3 ?=- Local covering fraction related to wind
clumpiness extracted from the spectrum NaID
fitting (Cfr=0.3)
74- 95 F22.11 Msun Mr0.3 ?=- Outflowing gas mass according to the
Halpha emission line (Mhalphar=0.3) (G3)
97-117 F21.17 Msun/yr dM/dtr0.3 ?=- Mass outflow rate according to the
Halpha emission line (Mdothalphar=0.3)
(G3)
119-140 E22.17 10-7W dE/dtr0.3 ?=- Kinetic power in the wind according
to the Halpha emission line
(Edothalphar=0.3) (G3)
--------------------------------------------------------------------------------
Byte-by-byte Description of file:ntralavg.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Id ? Identifier number (id)
5 I1 --- f_Id [0/1] Flag indicates whether an outflow was
detected through NaID absorption
(is_detected) (G1)
7- 9 F3.1 kpc r1.0 ?=- Assumed outflow extent in kpc (r=1.0)
11- 29 F19.14 km/s Vmaxr1.0 ?=- Maximum outflow velocity (Vmaxr=1.0)
(G1)
31- 52 E22.17 cm-2 NHIr1.0 ?=- Hydrogen column density extracted from
the NaID fitting (NHIr=1.0) (G2)
54- 72 F19.17 --- Cfr1.0 ?=- Local covering fraction related to wind
clumpiness extracted from the spectrum NaID
fitting (Cfr=1.0)
74- 95 F22.11 Msun Mr1.0 ?=- Outflowing gas mass according to the
Halpha emission line (Mhalphar=1.0) (G3)
97-117 F21.17 Msun/yr dM/dtr1.0 ?=- Mass outflow rate according to the
Halpha emission line (Mdothalphar=1.0)
(G3)
119-140 E22.17 10-7W dE/dtr1.0 ?=- Kinetic power in the wind according
to the Halpha emission line
(Edothalphar=1.0) (G3)
--------------------------------------------------------------------------------
Byte-by-byte Description of file:ntralmax.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Id ? Identifier number (id)
5 I1 --- f_Id [0/1] Flag indicates whether an outflow was
detected through NaID absorption
(is_detected) (G1)
7- 9 F3.1 kpc r3.0 ?=- Assumed outflow extent in kpc (r=3.0)
11- 29 F19.14 km/s Vmaxr3.0 ?=- Maximum outflow velocity (Vmaxr=3.0)
(G1)
31- 52 E22.17 cm-2 NHIr3.0 ?=- Hydrogen column density extracted from
the NaID fitting (NHIr=3.0) (G2)
54- 72 F19.17 --- Cfr3.0 ?=- Local covering fraction related to wind
clumpiness extracted from the spectrum NaID
fitting (Cfr=3.0)
74- 95 F22.11 Msun Mr3.0 ?=- Outflowing gas mass according to the
Halpha emission line (Mhalphar=3.0) (G3)
97-117 F21.17 Msun/yr dM/dtr3.0 ?=- Mass outflow rate according to the
Halpha emission line (Mdothalphar=3.0)
(G3)
119-140 E22.17 10-7W dE/dtr3.0 ?=- Kinetic power in the wind according
to the Halpha emission line
(Edothalphar=3.0) (G3)
--------------------------------------------------------------------------------
Global notes:
Note (G1): As explained in the section 3.2.2 Ionized and neutral gas properties,
from study of NaID absorption in our sources (see also Appendix B
for spectra profil fitting method) we detect 69 NaID absorption
of 144 systems tagging neutral gas presence. More, we use the
best-fitting stellar velocity dispersion σ* to divide the
sample into objects with stationary NaI gas versus systems with an
outflow. Systems with a neutral outflow are defined as systems with
vNaImax > 2σ* + 70 km/s, where we took a safety margin of
70 km/s which is also similar to the spectral resolution of SDSS.
Out of 69 systems with NaID absorption, 58 host neutral outflows,
and 11 do not. We verified that all the systems showing NaID emission
were classified as systems hosting an outflow according to their
vNaImax.
Note (G2): We estimated the hydrogen column density via (Shih & Rupke
2010ApJ...724.1430S 2010ApJ...724.1430S, i.e equation 2 section 3.2.2 Ionized and neutral
gas properties).
Note (G3): As explained in the section 3.2.4 Outflow energetics, we use
Rupke et al. (2005ApJS..160..115R 2005ApJS..160..115R) and assumed the time-averaged
thin-shell model for the neutral gas, we used the expressions 3, 4
and 5 of this section to compute mass and energetic neutral outflows.
While for the ionized gas we apply ionization parameter method
and prescriptions in Baron & Netzer (2019MNRAS.486.4290B 2019MNRAS.486.4290B,
Cat. J/MNRAS/486/4290). We estimated for ionized and neutral gas
(M,dM/dt,dE/dt) for outflow extent r = (0.3,1,3) kpc.
Note (G4): We defined the maximum blueshifted outflow velocity as
vionmax = Δvion -2σion, where Δvion is the
velocity shift of the broad lines with respect to systemic and
σion is the velocity dispersion, (i.e 3.2.2 Ionized and
neutral gas properties).
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Luc Trabelsi [CDS] 26-Sep-2024