J/ApJ/904/170ivo://CDS.VizieR/J/ApJ/904/170doi:10.26093/cds/vizier.19040170CDSZhao D.Du M.Ho L.C.Debattista V.P.Shi J.2022-06-13T09:59:45Z2022-05-30T07:20:21ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frgalaxiesastronomical-modelsAlmost 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*~10^10.6^M{odot} 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*<10^10.6^M{odot}, 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*>10^10.6^M{odot} 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*>=10^10.6^M{odot} we find that the bar fraction is a nearly constant 60%.2020ApJ...904..170Zhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/904/170CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/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 webpagehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/904/170https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/904/170http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/904/170https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/904/170https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/904/170http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/904/170GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/ApJ/904/170/table1Properties of barred galaxiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintID[12/623331] Illustrus TNG Galaxy ID (1)meta.id;meta.mainintMass[10/11.4] Stellar mass of host galaxy, log (2)log(solMass)src.class.starGalaxyfloatkin[0.5/0.75] Fraction of kinetic energy in ordered rotation (2)phys.energy;arith.ratiofloatemax[0.25/0.89] Maximum ellipticitysrc.ellipticityfloatRmax[1.4/6.72] Bar size measured at maximum ellipticitykpcphys.angSizefloatRmax85[1.46/8.83] Bar size at 85% emax (3)kpcphys.angSizefloate_Rmax85[0/13.74] Upper error, Rmax85 (4)kpcstat.errorfloatE_Rmax85[0/1.29] Lower error, Rmax85 (4)kpcstat.error;stat.maxfloat