J/MNRAS/521/1775 Galaxy Zoo barred galaxies properties with MaNGA (Geron+, 2023)
Galaxy Zoo kinematics of strongly and weakly barred galaxies.
Geron T., Smethurst R.J., Lintott C., Kruk S., Masters K.L., Simmons B.,
Mantha K.B., Walmsley M., Garma-Oehmichen L., Drory N., Lane R.R.
<Mon. Not. R. Astron. Soc. 521, 1775-1793 (2023)>
=2023MNRAS.521.1775G 2023MNRAS.521.1775G (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies ; Galaxies, nearby ; Spectroscopy ; Optical ;
Morphology ; Positional data ; Galaxies, radius ; Redshifts ;
Rotational velocities
Keywords: galaxies: bar - galaxies: evolution - galaxies: general -
galaxies: kinematics and dynamics - galaxies: structure
Abstract:
We study the bar pattern speeds and corotation radii of 225 barred
galaxies, using integral field unit data from MaNGA and the
Tremaine-Weinberg method. Our sample, which is divided between
strongly and weakly barred galaxies identified via Galaxy Zoo, is the
largest that this method has been applied to. We find lower pattern
speeds for strongly barred galaxies than for weakly barred galaxies.
As simulations show that the pattern speed decreases as the bar
exchanges angular momentum with its host, these results suggest that
strong bars are more evolved than weak bars. Interestingly, the
corotation radius is not different between weakly and strongly barred
galaxies, despite being proportional to bar length. We also find that
the corotation radius is significantly different between quenching and
star-forming galaxies. Additionally, we find that strongly barred
galaxies have significantly lower values for R, the ratio between the
corotation radius and the bar radius, than weakly barred galaxies,
despite a big overlap in both distributions. This ratio classifies
bars into ultrafast bars (R< 1.0; 11 per cent of our sample), fast
bars (1.0 <R< 1.4; 27 per cent), and slow bars (R> 1.4; 62 per cent).
Simulations show that R is correlated with the bar formation
mechanism, so our results suggest that strong bars are more likely to
be formed by different mechanisms than weak bars. Finally, we find a
lower fraction of ultrafast bars than most other studies, which
decreases the recently claimed tension with Lambda cold dark matter.
However, the median value of R is still lower than what is predicted
by simulations.
Description:
Bars are a relatively common structure in galaxies, with about
30-60 per cent of nearby galaxies hosting a bar, depending on the
redshift and wavelength range of the study. Bars can drive angular
momentum outwards and funnel gas to the centre of the galaxy. The
community has yet to reach a consensus on how to best define weak and
strong bars and on which detection method is superior. It was
addressed more recently by the Galaxy Zoo (GZ) team, who combined the
efforts of citizen scientists and machine learning to provide
morphological classifications of galaxies. These morphological
classifications included a distinction between weak and strong bars
based on visual morphology. It is becoming clear that the bar pattern
speed and the parameters as corotation radius derived are important to
study barred galaxies. The only reliable direct and model-independent
method to determine them is the Tremaine-Weinberg (TW) method
(Tremaine & Weinberg 1984ApJ...282L...5T 1984ApJ...282L...5T). It has been used
extensively in the past to study bar pattern speeds. The TW method
uses surface brightness and line-of-sight (LOS) velocity data to
estimate the pattern speed (i.e see introduction section).
In this paper, we use the TW method on integral-field spectroscopy
data from MaNGA survey (Bundy et al. 2015ApJ...798....7B 2015ApJ...798....7B) to estimate
bar pattern speeds, corotation radii and the dimensionless ratio for a
sample of 225 galaxies. This is the largest sample to date measured
with the TW method and includes both weakly and strongly barred
galaxies, identified using Galaxy Zoo. The theory of these parameter
computations are presented in section 2. We need resolved stellar
velocity and stellar flux data in order to implement the TW method,
which we obtain from the MaNGA survey which is part of the Sloan
Digital Sky Survey IV (SDSS-IV) collaboration (Blanton et al.
2017AJ....154...28B 2017AJ....154...28B). We used data from the seventeenth data release
of SDSS APOGEE (Abdurro'uf et al. 2022ApJS..259...35A 2022ApJS..259...35A, Cat. III/286).
MaNGA used the Baryon Oscillation Spectroscopic Survey (BOSS)
Spectrograph, which has a resolution of R∼2000 and a wavelength
coverage of 3600-10000 Å on the 2.5m Sloan Telescope at Apache
Point Observatory. For more information on the observing strategy,
survey design, data reduction process, sample selection and the data
analysis pipeline, please refer to section 3.1. Next, we have used the
GZ DESI project (Walmsley et al. 2023MNRAS.526.4768W 2023MNRAS.526.4768W, Cat.
J/MNRAS/526/4768, images are available at www.legacysurvey.org or
https://ui.adsabs.harvard.edu/link_gateway/2019AJ....157..168D
/DATASOURCE) to obtain morphological classifications and find weak and
strong bars.
We then provide in table1.dat for the 225 galaxies, inclination, bar
length, and position angles for TW method as explicited in section
3.3. Also, rotation curve are determined in order to compute Vrot and
corotation radius. The selection sample methodology with machine
classifications from GZ DESI and then thresholds as exposed in section
3.5. Finally, as presented in table3.dat and section 4, the TW output
results for the 225 targets.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 272 225 Astrometric, bar types, inclinations,
position angles, bar lengths of our barred
galaxies sample as described in section 3
table3.dat 429 225 The bar pattern speed, corotation radius and
dimensionless corotation radius-to-bar ratio of
our barred galaxies sample
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See also:
J/MNRAS/526/4768 : Galaxy Zoo DESI (Walmsley+, 2023)
J/MNRAS/509/3966 : Galaxy Zoo DR1&2, DR5 and DeepL version (Walmsley+, 2022)
J/MNRAS/473/4731 : Barred galaxies structural decomposition (Kruk+, 2018)
J/MNRAS/410/166 : Morphological types from Galaxy Zoo 1 (Lintott+, 2011)
J/A+A/596/A84 : S4G disk galaxies stellar mass distribution
(Diaz-Garcia+, 2016)
J/A+A/587/A160 : 3.6um S4G Galactic bars characterization (Diaz-Garcia+,2016)
J/A+A/416/515 : Starbursts in barred spiral galaxies. VI. (Davoust+, 2004)
J/ApJ/704/1657 : Hα rotation curves for 10 spiral galaxies
(Fathi+, 2009)
J/ApJ/659/1176 : Study of bars in 180 spiral galaxies (Marinova+, 2007)
J/ApJS/186/427 : Detailed morphology of SDSS galaxies (Nair+, 2010)
J/ApJS/182/559 : Corotation radii for 153 galaxies of OSUBSGS (Buta+, 2009)
J/ApJS/143/73 : Morphology of spiral galaxies (Eskridge+, 2002)
J/AJ/154/86 : MaNGA catalog, DR15 (Wake+, 2017)
J/AJ/114/2402 : Rotation curves of early-type galaxies (Courteau+, 1997)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- MANGA The MaNGA plate-ifu number of this target
(PLATEIFU)
13- 26 F14.10 deg RAdeg The right ascension of this target identical
to the OBJRA column in the MaNGA DRPALL
(J2000) (RA)
28- 43 F16.13 deg DEdeg The declination of this target identical to
the OBJDEC column in the MaNGA DRPALL (J2000)
(DEC)
45- 62 F18.15 deg i The inclination of the galaxy (inc)
64- 81 F18.16 deg e_i The error on the inclination (inc_err)
83-102 F20.16 deg PA The kinematic position angle of the galaxy
measured east of north between 0 and 180 (PA)
104-122 F19.17 deg e_PA The error on the galaxy PA (PA_err)
124-144 F21.17 deg PAbar The position angle of the bar measured east
of north between 0 and 180 (PA_bar)
146-166 F21.16 deg e_PAbar The error on the PA of the bar (PAbarerr)
168-186 F19.16 arcsec Rbar The bar radius as defined in section 3.3
(R_bar)
188-207 F20.18 arcsec e_Rbar The error on the bar radius (Rbarerr)
209-227 F19.16 kpc Rbardp The deprojected bar radius as defined in
section 3.3 (Rbardeproj_kpc)
229-249 F21.19 kpc e_Rbardp The error on the deprojected bar radius
(Rbardeprojkpcerr)
251-261 F11.9 --- z The redshift of the target taken from the NSA
catalog (redshift)
263-272 A10 --- BarType The bar type according to GZ DESI either
'Weak bar' or 'Strong bar' (bar_type)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- MANGA The MaNGA plate-ifu number of this
target (PLATEIFU)
13- 31 F19.16 km/s/arcsec Om*sin(i) Projected bar pattern speed of the
target Ωb*sin(i) with i the
inclination of the galaxy as defined
in section 2.1 (Omega_sini)
33- 51 F19.16 km/s/arcsec e_Om*sin(i) The lower limit of the pattern speed
Om*sin (i) (Omegasinill)
53- 71 F19.16 km/s/arcsec E_Om*sin(i) The upper limit of the pattern speed
Om*sin (i) (Omegasiniul)
73- 91 F19.16 km/s/arcsec Om The bar pattern speed of the target
as defined in section 2.1 (Omega)
93-111 F19.16 km/s/arcsec e_Om The lower limit of the pattern speed
Om (Omega_ll)
113-130 F18.15 km/s/arcsec E_Om The upper limit of the pattern speed
Om (Omega_ul)
132-150 F19.16 km/s/kpc Omph*sin(i) Projected physical bar pattern speed
of the target Ωphys,b*sin(i)
with i the inclination of the galaxy
as in sect. 2.1 (Omegaphyssini)
152-170 F19.16 km/s/kpc e_Omph*sin(i) The lower limit of the pattern speed
Omph*sin (i) (Omegaphyssini_ll)
172-190 F19.16 km/s/kpc E_Omph*sin(i) The upper limit of the pattern speed
Omph*sin (i) (Omegaphyssini_ul)
192-209 F18.15 km/s/kpc Omph The physical bar pattern speed of
the target Ωphys,b as
defined in section 2.1 (Omega_phys)
211-229 F19.16 km/s/kpc e_Omph The lower limit of the pattern speed
Omph (Omegaphysll)
231-248 F18.15 km/s/kpc E_Omph The upper limit of the pattern speed
Omph (Omegaphysul)
250-268 F19.16 arcsec Rcr ? The corotation radius of the
target (Rcr) (1)
270-288 F19.16 arcsec e_Rcr ? The lower limit of the corotation
radius Rcr (Rcr_ll)
290-308 F19.16 arcsec E_Rcr ? The upper limit of the corotation
radius Rcr (Rcr_ul)
310-328 F19.16 kpc Rcrph ? The physical corotation radius
(Rcr_phys) (1)
330-348 F19.16 kpc e_Rcrph ? The lower limit of the corotation
radius Rcrph (Rcrphysll)
350-368 F19.16 kpc E_Rcrph ? The upper limit of the corotation
radius Rcrph (Rcrphysul)
370-389 F20.17 --- R ? The dimensionless corotation
radius-to-bar radius ratio R=Rcr/Rbar
of the target as in sect. 2.3 (R)
391-409 F19.17 --- e_R ? The lower limit of R (R_ll)
411-429 F19.16 --- E_R ? The upper limit of R (R_ul)
--------------------------------------------------------------------------------
Note (1): Defined as Vc/Ωb with Vc is the circular velocity in the
flat part of the rotation curve (i.e. section 2.3). The radius Rcr
at which the angular speed of the stars in the disc is equal to
the pattern speed of the bar. For Rcrph we use Omph instead of Om.
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History:
From electronic version of the journal
License: CC-BY-4.0
(End) Luc Trabelsi [CDS] 29-May-2026