J/ApJ/904/170 1179 galaxies in the IllustrisTNG simulation (Zhao+, 2020)
Barred Galaxies in the IllustrisTNG Simulation.
Zhao D., Du M., Ho L.C., Debattista V.P., Shi J.
<Astrophys. J., 904, 170 (2020)>
=2020ApJ...904..170Z 2020ApJ...904..170Z
ADC_Keywords: Galaxies; Models
Keywords: Barred spiral galaxies ; Astronomical simulations
Abstract:
Almost two-thirds of disk galaxies in the local universe host bars,
which serve as important drivers of secular evolutionary processes.
While cosmological simulations are powerful tools to study the
formation and evolution of galaxies, they have often struggled to
generate reasonable bar populations. We measure the fraction, size,
and strength of bars in 3866 disk galaxies from the TNG100 run of the
advanced cosmological simulation IllustrisTNG. Consistent with
observations, about 55% of disk galaxies with stellar mass
M*∼1010.6M☉ are barred, and the relation between bar size and
total stellar mass is similar to that found in near-infrared surveys.
However, the formation of bars is suppressed in galaxies with
M*<1010.6M☉, which may result from the difficulty TNG100 has in
resolving short bars with radius <1.4kpc. In contrast, up to 75% of
massive disk galaxies with M*>1010.6M☉ have bars, ∼10%-20%
higher than observed. TNG100 overproduces relatively short bars
(radius ∼1.4-3kpc) with respect to the mass-bar size relation observed
in near-infrared surveys. Tracing the progenitors of z=0 massive
galaxies we find that the bar fraction increases from 25% to 63%
between z=1 and 0. Instead if we select all disk galaxies during z=0-1
with a constant mass cut of M*≥1010.6M☉ we find that the bar
fraction is a nearly constant 60%.
Description:
IllustrisTNG is an advanced magnetohydrodynamical cosmological
simulation run with the moving-mesh code AREPO. IllustrisTNG uses an
updated version of the Illustris galaxy formation model. We use the
TNG100 run, the highest-resolution version that is publicly
accessible. It simulates a volume with side length ∼111Mpc. The
average mass of the baryonic resolution elements in TNG100 reaches
1.39x106M☉. The gravitational softening length of the stellar
particles is set to ∼0.74kpc.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 43 1179 Properties of barred galaxies
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See also:
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/PASP/122/1397 : Spitzer Survey Stellar Structure in Galaxies (Sheth+, 2010)
J/ApJS/197/22 : The Carnegie-Irvine Galaxy Survey (GGS). II. (Li+, 2011)
J/A+A/582/A86 : Catalogue of features in the S4G (Herrera-Endoqui+, 2015)
J/A+A/587/A160 : 3.6um S4G Galactic bars characterization (Diaz-Garcia+, 2016)
J/ApJ/845/87 : CGS V. Statistical study of bars and buckled bars (Li+, 2017)
http://www.tng-project.org/ : The Illustris TNG project webpage
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- ID [12/623331] Illustrus TNG Galaxy ID (1)
8- 12 F5.2 [Msun] Mass [10/11.4] Stellar mass of host galaxy, log (2)
14- 17 F4.2 --- kin [0.5/0.75] Fraction of kinetic energy in ordered
rotation (2)
19- 22 F4.2 --- emax [0.25/0.89] Maximum ellipticity
24- 27 F4.2 kpc Rmax [1.4/6.72] Bar size measured at maximum
ellipticity
29- 32 F4.2 kpc Rmax85 [1.46/8.83] Bar size at 85% emax (3)
34- 38 F5.2 kpc e_Rmax85 [0/13.74] Upper error, Rmax85 (4)
40- 43 F4.2 kpc E_Rmax85 [0/1.29] Lower error, Rmax85 (4)
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Note (1): galaxy ID is the subhalo ID in snapshot 99 obtained by SUBFIND
algorithm given by the IllustrisTNG group.
Note (2): Mass and fraction of kinetic energy measured within a sphere of 30kpc
radius centered on the galaxy.
Note (3): Bar size defined as the radius where the ellipticity declines to
85% of the maximum value.
Note (4): Uncertainty caused by inner boundary and pixel size.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 13-May-2022