J/A+A/587/A160ivo://CDS.VizieR/J/A+A/587/A160doi:10.26093/cds/vizier.35870160CDSDiaz-Garcia S.Salo H.Laurikainen E.Herrera-Endoqui M.2018-01-08T06:38:18Z2016-03-09T08:05:49ZCDS support team

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

cds-question@unistra.frStellar bars play an essential role in the secular evolution of disk galaxies because they are responsible for the redistribution of matter and angular momentum. Dynamical models predict that bars become stronger and longer in time, while their rotation speed slows down. We use the Spitzer Survey of Stellar Structure in Galaxies (S^4^G) 3.6um imaging to study the properties (length and strength) and fraction of bars at z=0 over a wide range of galaxy masses (M*~=10^8^-10^11^M_{sun}_) and Hubble types (-3<=T<=10). We calculated gravitational forces from the 3.6um images for galaxies with a disk inclination lower than 65{deg}. We used the maximum of the tangential-to-radial force ratio in the bar region (Qb) as a measure of the bar-induced perturbation strength for a sample of ~600 barred galaxies. We also used the maximum of the normalized m=2 Fourier density amplitude (A_2_^max^) and the bar isophotal ellipticity ({epsilon}) to characterize the bar. Bar sizes were estimated i) visually, ii) from ellipse fitting, iii) from the radii of the strongest torque, and iv) from the radii of the largest m=2 Fourier amplitude in the bar region. By combining our force calculations with the HI kinematics from the literature, we estimated the ratio of the halo-to-stellar mass (Mh/M*) within the optical disk and by further using the universal rotation curve models, we obtained a first-order model of the rotation curve decomposition of 1128 disk galaxies. We probe possible sources of uncertainty in our Qb measurements: the assumed scale height and its radial variation, the influence of the spiral arms torques, the effect of non-stellar emission in the bar region, and the dilution of the bar forces by the dark matter halo (our models imply that only ~10% of the disks in our sample are maximal). We find that for early- and intermediate-type disks (-3<=T<5), the relatively modest influence of the dark matter halo leads to a systematic reduction of the mean Qb by about 10-15%, which is of the same order as the uncertainty associated with estimating the vertical scale height. The halo correction on Qb becomes important for later types, implying a reduction of ~20-25% for T=7-10. Whether the halo correction is included or not, the mean Qb shows an increasing trend with T. However, the mean A_2_^max^ decreases for lower mass late-type systems. These opposing trends are most likely related to the reduced force dilution by bulges when moving towards later type galaxies. Nevertheless, when treated separately, both the early- and late-type disk galaxies show a strong positive correlation between Qb and A_2_^max^. For spirals the mean {epsilon}~0.5 is nearly independent of T, but it drops among S0s (~0.2). The Qb and {epsilon} show a relatively tight dependence, with only a slight difference between early and late disks. For spirals, all our bar strength indicators correlate with the bar length (scaled to isophotal size). Late-type bars are longer than previously found in the literature. The bar fraction shows a double-humped distribution in the Hubble sequence (~75% for Sab galaxies), with a local minimum at T=4 (~40%), and it drops for M*<~10^9.5-10^M_{sun}_. If we use bar identification methods based on Fourier decomposition or ellipse fitting instead of the morphological classification, the bar fraction decreases by ~30-50% for late-type systems with T>=5 and correlates with Mh/M*. Our Mh/M* ratios agree well with studies based on weak lensing analysis, abundance matching, and halo occupation distribution methods, under the assumption that the halo inside the optical disk contributes roughly a constant fraction of the total halo mass (~4%). We find possible evidence for the growth of bars within a Hubble time, as (1) bars in early-type galaxies show larger density amplitudes and disk-relative sizes than their intermediate-type counterparts, and (2) long bars are typically strong. We also observe two clearly distinct types of bars, between early- and intermediate-type galaxies (T<5) on one side, and the late-type systems on the other, based on the differences in the bar properties. Most likely this distinction is connected to the higher halo-to-stellar ratio that we observe in later types, which affects the disk stability properties.2016A&A...587A.160Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/587/A160CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/PASP/122/1397 : S4G catalog Version 2 (Sheth+, 2010)J/ApJ/772/135 : 3.6um surface brightness from S4G (Zaritsky+, 2013)J/MNRAS/444/3015 : Morphologies of S4G galaxies (Laine+, 2014)J/A+A/569/A91 : Optical imaging for S4G (Knapen+, 2014)J/ApJS/219/4 : S4G pipeline 4: multi-component decompositions (Salo+, 2015)J/A+A/582/A86 : Catalogue of features in the S4G (Herrera-Endoqui+, 2015)J/ApJS/217/32 : S4G galaxy morphologies in the CVRHS system (Buta+, 2015)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/587/A160https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/587/A160http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/587/A160https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/587/A160https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/587/A160http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/587/A160GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/587/A160/tablea1 (Fundamental properties of S4G galaxies: distance, mass distribution, velocities and stellar disk)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/587/A160/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/587/A160/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/587/A160/tablea1?GETtext/xml+votable180.050000true359.115-81.56638890.0055555555555555565/6928 6941 6984-6985 6/35 38 602 611 664 690 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16737 16749 16807 16841 16845 16871 16881 16886 16898 16925 17007 17064 17076 17165 17245 17281 17286 17378 17424 17473-17474 17480 17502 17509 17592 17594 17598 17605-17606 17612 17688 17693 17717 17741 17745 17747 17753-17754 17759 17761 17773 17776 17780 17855 17905 17912 17925 17927 17990 18002 18011 18158 18200 18209 18214 18223 18226 18232 18315 18327 18379 18384-18385 18398 18415 18425 18429 18507 18542 18568 18639 18649-18650 18676-18677 18680 18760 18793 18800 18809 18813 18860 19272 19442 19449 19490-19491 19570 19576 19579 19611 19614 19667 19675 19678 19696-19697 19707-19708 19710 20000 20008 20014 20023 20044 20046 20226 20270 20353 21155 21195 22579 22594 22637 22690 22751 22780 24631 24675 24681 24732 24735 24748 24761 24769 24772 24777 24779 24794 24819-24820 24843 24849 24878 24896 24902 24912 24916 24926 24947 24949 24953 24957 24993 25044 25046-25047 25053-25054 25077-25079 25087 25094 25104 25125 25127 25135 25143-25144 25205 25303 25344 25346 25350 25353 25356 25438-25439 25460 25490 25498 25509 25512 25527 25581 25587 25591 25599 25613 25635 25640 25645 25647 25652-25653 25696 25705 25715 25725 25734 25738-25739 25741 25756 25762-25763 25768 25770 25775 25778-25779 25784-25785 25788 25790 25862 25874-25875 25883 25887-25890 25901 25904 25907 25927 25935 25945-25947 25958 25960 25966 25972 25979 25997 26055 26065 26068-26069 26072 26090 26113 26119 26125 26127-26128 26134 26148 26161 26175 26178 26214 26217 26234 26247 26264 26267-26268 26271 26279 26287 26294-26295 26303-26304 26307 26309 26312 26317-26318 26323-26324 26329-26331 26338 26343-26344 26346 26349 26351 26353 26362 26365 26377 26388 26423 26432 26451 26472 26507 26518 26528 26537 26540 26542 26555 26677 26724 26726 26803 26858 26862 26946 27024 27030 27044 27079 27090 27098 27150-27151 27186 27243 27255 27285 27347 27365 27367 27406 27426 27458 27482 27504 27512 27514-27515 27525 27555 27567-27568 27575 27591 27601 27603-27604 27606 27608 27623 27643 27650 27653-27654 27668-27669 27716 27718-27721 27723-27724 27728-27729 27731 27735-27736 27738 27741 27743 27748 27761 27763 27770 27772 27774 27789 27801 27811 27814 27828 27830 27841 27853 27857-27861 27863 27865 27871 27901 27905 27907-27908 27913-27914 27917-27919 27945 27947-27949 27955 28015 28019 28023 28035-28037 28039 28044-28046 28053-28054 28056 28058 28067 28076-28077 28123 28149 28162 28167 28172 28191 28200-28201 28208 28213 28218 28221 28234 28258 28264 28294 28299-28300 28304 28310 28325 28336 28363 28374 28381 28404 28416 28435 28444 28451 28463 28468 28486 28495-28496 28505 28508 28510 28516 28521 28529 28535 28538 28579 28593 28608 28610 28630-28631 28636-28637 28653 28666 31323 31345 31352 31360 31365 31369 31376 31451 31454 31469 31628 31632 32426 32439 32482 32487 32793 32909 32983 33142-33143 33164 33193 33228 33242 33271 33337 33434 33466 33522 33650 33654 33745 33835 33857 33864 33885 33920 33951 33954 33957-33958 33960 33982 34051 34189 34251 34272-34273 34295 34297 34302 34328 34334-34335 34343 34352 34362-34363 34377 34401-34402 34404 34449 34471 34476 34493-34495 34501 34511 34531 34533-34535 34538 34540 34542 34545 34554 34602-34603 34638 34641 34663 34674 34687 34695 34701 34724 34735 34910 34983 35193 35206 35214 35267 35287 35536 35581 35691 35746 35827 35863 35908 35922-35923 35925 35929 35960 35966-35967 35993 35995 36022 36049 36056 36062 36081 36107 36131 36134-36135 36147 36151 36163 36194-36195 36211 36229 36231 36234 36236 36240 36243 36245 36247 36250 36255 36258 36261 36266 36269 36276 36286-36288 36291 36300 36302 36325 36328 36332 36380 36415 36448 36450 36459 36480 36608-36609 36621 36633 36635 36648 36677 36684 36732 36734 36756 36785 36789-36790 36793 36796 36822 36831 36848 36857 38876 40436 40789 40791 43862 43865 43874 43878 43881 43883 43911 43920 43925 43948 43953-43956 43977-43978 44001 44003 44006 44010-44011 44025-44027 44461 44466 44579 44582 44584 44635-44636 44638 44660 44718 44741 44809 44817 44844 44866 44896 44900 44945 44947 44955 44998 45004 45037 45050 45054 45109 45112 45125 45178 45181 45296 45406 45469 45471 45512 45558 45562 45809 45886 45905 45990 46013 46062 46170 46175 46271 46304 46327 46398-46399 46429 46438 46443 46460 46463 46477 46479 46481 46491 46509 46519 46525 46545 46549 46562 46568-46569 46577 46597 46615 46628 46651 46676 46689 46696 46736 46738 46775 46797 46799 46808 46812 46819 47009 47030 47077 47084 47098 47381 47456 47458 47474 47556 48132 48193 48266 48283 48292 48406 48455-48456 48464 48484 48502 48605 48942 49010 49017 49118https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/587/A160?format=asciiInfrareddefaultJ/A+A/587/A160/tablea1Fundamental properties of S4G galaxies: distance, mass distribution, velocities and stellar diskrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintrfpDisplay the Radial force profiles of this galaxymeta.ref.urlcharrcdmDisplay the Rotation curve decomposition model of this galaxymeta.ref.urlcharGalaxyGalaxy identificationmeta.id;src.class.starGalaxy;meta.maincharprimaryM*? Total stellar masssolMassphys.massnullableDistDistance to the galaxyMpcpos.distancefloathzDisk scale-heightarcsecphys.angSize;srcfloate_hz1[] Uncertainty on the disk scale-height associated with a thicker disk in de Grijs/Speltincx relationarcsecstat.errorfloate_hz2[] Uncertainty on the disk scale-height associated with a thinner disk in de Grijs/Speltincx relationarcsecstat.errorfloatRopt? Estimated optical radiusarcsecphys.angSize;em.optdoublenullableVHI? Inclination-corrected HI maximum velocitykm/sspect.dopplerVelocdoublenullableV36max? Maximum of the stellar contribution to the rotation curvekm/sphys.veloc.rotatdoublenullablee_V36max1[] Uncertainty on the maximum of the stellar contribution to the rotation curve associated with a thicker disk in de Grijs/Speltincx relationkm/sstat.errorfloate_V36max2[] Uncertainty on the maximum of the stellar contribution to the rotation curve associated with a thinner disk in de Grijs/Speltincx relationkm/sstat.errorfloatV36maxRad? Radius of maximum velocity of the stellar component of the rotation curvearcsecphys.angSizedoublenullablee_V36maxRad1[]? Uncertainty on the radius of maximum velocity of the stellar component of the rotation curve associated with a thicker disk in de Grijs/Speltincx relationarcsecstat.errordoublenullablee_V36maxRad2[]? Uncertainty on the radius of maximum velocity of the stellar component of the rotation curve associated with a thinner disk in de Grijs/Speltincx relationarcsecstat.errordoublenullableV36Ropt? The stellar contribution to the rotation curve evaluated at the optical radiuskm/sphys.veloc.rotatdoublenullablee_V36Ropt1[]? Uncertainty on the stellar contribution to the rotation curve evaluated at the optical radius associated with a thicker disk in de Grijs/Speltincx relationkm/sstat.errordoublenullablee_V36Ropt2[]? Uncertainty on the stellar contribution to the rotation curve evaluated at the optical radius associated with a thinner disk in de Grijs/Speltincx relationkm/sstat.errordoublenullabledRV36? Inner slope of the stellar component of the rotation curvekm.s**-1.kpc**-1arith.grad;phys.velocdoublenullablee_dRV361[]? Uncertainty on the inner slope of the stellar component of the rotation curve associated with a thicker disk in de Grijs/Speltincx relationkm.s**-1.kpc**-1stat.errordoublenullablee_dRV362[]? Uncertainty on the inner slope of the stellar component of the rotation curve associated with a thinner disk in de Grijs/Speltincx relationkm.s**-1.kpc**-1stat.errordoublenullableahalo? Halo core radiuskpcphys.size.radiusdoublenullableVinfhalo? Halo velocity amplitude, corrected to match the HI maximum velocitykm/sphys.veloc.dispersiondoublenullableMh/M*? Stellar-to-halo mass ratio within the optical radiusphys.mass;arith.ratiodoublenullablebarindicates bar informations in tables A2 and/or A3meta.ref.urlcharSimbadSimbad column added by the CDSmeta.ref.urlchar_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainJ/A+A/587/A160/tablea2Bar maximum gravitational torques and radiirecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGalaxyGalaxy identificationmeta.id;meta.maincharQbBar maximum gravitational torquesrc.morph.paramfloate_Qb1[]? Uncertainty on the bar maximum gravitational torque associated with a thicker disk in de Grijs/Speltincx relationstat.errordoublenullablee_Qb2? Uncertainty on the bar maximum gravitational torque associated with a thinner disk in de Grijs/Speltincx relationstat.errorfloatnullableRQbBar maximum gravitational torque radiusarcsecphys.angSize;stat.maxfloate_RQb1[]? Uncertainty on the bar maximum gravitational torque radius associated with a thicker disk in de Grijs/Speltincx relationarcsecstat.errordoublenullablee_RQb2[]? Uncertainty on the bar maximum gravitational torque radius associated with a thinner disk in de Grijs/Speltincx relationarcsecstat.errorfloatnullableQbhcor? Bar maximum gravitational torque correcting for the dilution of the dark halosrc.morph.paramdoublenullableRQbhcor? Bar maximum gravitational torque radius correcting for the dilution of the dark haloarcsecphys.angSize;stat.maxdoublenullableQbbar? Bar-only maximum gravitational torquesrc.morph.paramdoublenullableRQbbar? Bar-only maximum gravitational torque radiusarcsecphys.angSize;stat.maxdoublenullableQbbarhcor? Bar-only maximum gravitational torque correcting also for the dilution of the dark halosrc.morph.paramdoublenullableRQbbarhcor? Bar-only maximum gravitational torque radius correcting also for the dilution of the dark haloarcsecphys.angSize;stat.maxdoublenullableQbS08? Bar maximum gravitational torque using the relation from Speltincx et al. (2008MNRAS.383..317S) for the disk thickness estimationsrc.morph.paramdoublenullablee_QbS081[]? Uncertainty on the bar maximum gravitational torque associated with a thicker disk in the relation from Speltincx et al. (2008MNRAS.383..317S)stat.errordoublenullablee_QbS082? Uncertainty on the bar maximum gravitational torque associated with a thinner disk in the relation from Speltincx et al. (2008MNRAS.383..317S)stat.errordoublenullableQTrbar? Radial force profile evaluated at the end of the barsrc.morph.paramdoublenullablee_QTrbar1[]? Uncertainty on the evaluation of the radial force profile at the end of the bar associated with a thicker disk in de Grijs/Speltincx relationstat.errordoublenullablee_QTrbar2? Uncertainty on the evaluation of the radial force profile at the end of the bar associated with a thinner disk in de Grijs/Speltincx relationstat.errordoublenullableQThcorrbar? Halo-corrected radial force profile evaluated at the end of the barsrc.morph.paramdoublenullableJ/A+A/587/A160/tablea3Bar intrinsic ellipticity and parameters from the Fourier dissection of barsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGalaxyGalaxy identificationmeta.id;meta.maincharEll? Bar intrinsic ellipticitysrc.ellipticitydoublenullableA2? Bar maximum normalized m=2 Fourier amplitudesrc.var.amplitudefloatnullableRA2? Bar maximum normalized m=2 Fourier amplitude radiusarcsecphys.angSize;stat.maxnullableA4? Bar maximum normalized m=4 Fourier amplitudesrc.var.amplitudedoublenullableRA4? Bar maximum normalized m=4 Fourier amplitude radiusarcsecphys.angSize;stat.maxnullableA6? Bar maximum normalized m=6 Fourier amplitudesrc.var.amplitudedoublenullableRA6? Bar maximum normalized m=6 Fourier amplitude radiusarcsecphys.angSize;stat.maxnullableA8? Bar maximum normalized m=8 Fourier amplitudesrc.var.amplitudedoublenullableRA8? Bar maximum normalized m=8 Fourier amplitude radiusarcsecphys.angSize;stat.maxnullableA2rbar? Normalized m=2 Fourier amplitude evaluated at the end of the barsrc.var.amplitudedoublenullable