J/MNRAS/511/4223 Neutral gas winds of MaNGA-DR15 galaxies (Avery+, 2022)
Cool outflows in MaNGA a systematic study and comparison to the warm phase.
Avery C.R., Wuyts S., Forster Schreiber N.M., Villforth C., Bertemes C.,
Hamer S.L., Sharma R., Toshikawa J., Zhang J.
<Mon. Not. R. Astron. Soc. 511, 4223-4237 (2022)>
=2022MNRAS.511.4223A 2022MNRAS.511.4223A (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Star Forming Region ; Interstellar medium ;
Spectroscopy ; Photometry ; Optical ; Line Profiles ; Redshifts ;
Galaxies, radius ; Active gal. nuclei ; Radial velocities ;
Space velocities ; Mass loss
Keywords: ISM: jets and outflows - galaxies: evolution - galaxies: ISM -
galaxies: kinematics and dynamics
Abstract:
This paper investigates the neutral gas phase of galactic winds via
the Na I Dλλ5890, 5895Å feature within z ∼ 0.04 MaNGA
galaxies and directly compares their incidence and strength to the
ionized winds detected within the same parent sample. We find evidence
for neutral outflows in 127 galaxies (∼5 per cent of the analysed
line-emitting sample). Na I D winds are preferentially seen in
galaxies with dustier central regions and both wind phases are more
often found in systems with elevated star formation rate (SFR) surface
densities, especially when there has been a recent upturn in the star
formation activity according to the SFR5Myr / SFR800Myr parameter.
We find the ionized outflow kinematics to be in line with what we
measure in the neutral phase. This demonstrates that, despite their
small contributions to the total outflow mass budget, there is value
to collecting empirical measurements of the ionized wind phase to
provide information on bulk motion in the outflow. Depending on dust
corrections applied to the ionized gas diagnostics, the neutral phase
has ∼1.2-1.8 dex higher mass outflow rates (dM/dtout), on average,
compared to the ionized phase. We quantify scaling relations between
dM/dtout and the strengths of the physical wind drivers (SFR,
LAGN). Using a radial-azimuthal stacking method, and by considering
inclination dependencies, we find results consistent with biconical
outflows orthogonal to the disc plane. Our work complements other
multiphase outflow studies in the literature that consider smaller
samples, more extreme objects, or proceed via stacking of larger
samples.
Description:
In this paper, we analyse the incidence of neutral gas outflows via
the Na I Dλλ5890, 5895 Å transition, starting
from the same sample of line-emitting MaNGA galaxies that represent
the underlying population considered in Avery et al.
(2021MNRAS.503.5134A 2021MNRAS.503.5134A). After outlining the methodology of outflow
identification and characterization, we discuss about the relative
incidence of detectable neutral gas winds compared to the subset of
322 objects showing evidence for ionized gas outflows and the
underlying analysed sample. For the 74 objects that have detectable
winds in both gas phases, we contrast the ionized and neutral wind
properties. For the full sample of 127 galaxies featuring detectable
neutral gas outflows, we quantify their strength as a function of key
drivers such as the galaxies SFR. We further consider constraints on
the outflow geometry by mapping the average spatial distribution of
outflow via a radial/azimuthal stacking procedure and by considering
trends with inclination, (i.e see section Introduction).
This work makes use of data cubes from the MaNGA integral-field
spectroscopic galaxy survey (Bundy et al. 2015ApJ...798....7B 2015ApJ...798....7B). We
refer the reader to section 2.1 in Avery et al. (2021MNRAS.503.5134A 2021MNRAS.503.5134A)
for details on the parent sample used for this work. To summarize, we
take the 4239 MaNGA Data Release 15 (DR15) objects that are
successfully analysed by the MaNGA data analysis pipeline and
cross-matched to the MPA-JHU data base (Kauffmann et al.
2003MNRAS.346.1055K 2003MNRAS.346.1055K; Brinchmann et al. 2004MNRAS.351.1151B 2004MNRAS.351.1151B; Salim et
al. 2007ApJS..173..267S 2007ApJS..173..267S), providing measurements of total stellar
masses and SFRs as well as their associated uncertainties. Next as
shown in section 2.2 and 2.3, we apply constraints to include sources
showing ionized or neutral gas with Na I D signature spectra and also
to keep evidence of neutral gas outflows (see section 2.4 outflow
criteria). Among the first sample, we find 127 galaxies in total that
show neutral gas outflows and 322 hosting an ionized outflow in
Avery's sample meanwhile a subset of only 74 MaNGA galaxies show
outflows in both the ionized and neutral gas phases.
Thus, we provided physical properties sample of our 375 MaNGA galaxies
detectable outflow winds in the tablea1.dat. It includes Avery's and
MPA-JHU data base properties and from our work : blueshifts, outflow
velocities, mass outflow rates of the neutral wind gas, (i.e see
section 2.6 Outflow properties).
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 83 375 Properties of MaNGA galaxies sample with
detectable ionized and neutral winds
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See also:
J/A+A/623/A171 : Mkn 848 MaNGA 3-D data cube (Perna+, 2019)
J/ApJ/883/175 : First release of the MaNGA Stellar Library (MaStar)
(Yan+, 2019)
J/ApJS/262/36 : SDSS-IV MaNGA: pyPipe3D data for 10000 galaxies
(Sanchez+, 2022)
J/AJ/154/86 : MaNGA catalog, DR15 (Wake+, 2017)
https://data.sdss.org/sas/dr15/manga/spectro/ : MaNGA data SDSS archive server
Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- MaNGAId Identifier for MaNGA galaxy
(MaNGAId)
12- 16 F5.3 --- z Spectrscopic redshifts (z)
18- 22 F5.2 [kpc] logRe Logarithm of the effective radii
quantified on the NASA-Sloan Atlas
r-band images are taken directly
from MaNGA DR15 (logRe)
24- 25 I2 deg i ? Inclination angle (i) (1)
27- 31 F5.2 [Msun] logM* Logarithm of galaxy stellar masses
are adopted from the MPA-JHU data
base (logMstar)
33- 37 F5.2 [Msun/yr] logSFR Logarithm of SFRs are adopted from
the MPA-JHU data base (logSFR)
39- 43 F5.2 [10-7W] logLAGN ? Logarithm of AGN luminosities
(logLAGN) (2)
45- 50 F6.1 km/s DvBion ? Systematic blueshift
ΔvB,ion velocity of the
ionized wind gas
(ΔvB,ion) (3)
52- 57 F6.1 km/s DvBNaID ? Systematic blueshift
ΔvB,NaID velocity of the
neutral wind gas derived in this
work (ΔvB,NaID)
59- 64 F6.1 km/s VoutIon ? Overall outflow velocity of the
ionized wind gas (vout,ion) (3)
66- 71 F6.1 km/s VoutNaID ? Overall outflow velocity of the
neutral wind gas derived in this
work (vout,NaID)
73- 77 F5.2 [Msun/yr] log(dM/dtIon) ? Logarithm of ionized gas mass
outflow rate (logMdotout,ion) (4)
79- 83 F5.2 [Msun/yr] log(dM/dtNaID) ? Logarithm of NaI D neutral gas
mass outflow rate
(logMdot_out,NaID) (5)
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Note (1): Inclinations are derived from the NSA-projected axial ratio
measurements using equation 8 in the section 3.4 Outflow geometry,
unless morphological classifications (e.g. mergers) suggest that
the axial ratio may represent a poor proxy of inclination.
Note (2): The logLAGN are quantified on the basis of the [O III] luminosity of
spaxels with line ratios outside the star-forming region of the
BPT-NII diagram as explained in Avery et al. 2021MNRAS.503.5134A 2021MNRAS.503.5134A
section 2.2.5.
Note (3): These are derived in Avery et al. 2021MNRAS.503.5134A 2021MNRAS.503.5134A.
Note (4): Based on equation 3 of the section 2.2.8 in Avery et al.
2021MNRAS.503.5134A 2021MNRAS.503.5134A.
Note (5): Based on equation 5 of the section 2.6 Outflow properties in our work.
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History:
From electronic version of the journal
(End) Luc Trabelsi [CDS] 29-Jan-2025