J/ApJ/772/135ivo://CDS.VizieR/J/ApJ/772/135doi:10.26093/cds/vizier.17720135CDSZaritsky D.Salo H.Laurikainen E.Elmegreen D.Athanassoula E.,Bosma A.Comeron S.Erroz-Ferrer S.Elmegreen B.Gadotti D.A.,Gil de Paz A.Hinz J.L.Ho L.C.Holwerda B.W.Kim T.Knapen J.H.,Laine J.Laine S.Madore B.F.Meidt S.Menendez-Delmestre K.,Mizusawa T.Munoz-Mateos J.C.Regan M.W.Seibert M.Sheth K.2018-01-08T06:37:50Z2015-03-09T13:13:31ZCDS support team

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

cds-question@unistra.frgalaxiesgalaxy-classification-systemsinfrared-photometryWe study the m=1 distortions (lopsidedness) in the stellar components of 167 nearby galaxies that span a wide range of morphologies and luminosities. We confirm the previous findings of (1) a high incidence of lopsidedness in the stellar distributions, (2) increasing lopsidedness as a function of radius out to at least 3.5 exponential scale lengths, and (3) greater lopsidedness, over these radii, for galaxies of later type and lower surface brightness. Additionally, the magnitude of the lopsidedness (1) correlates with the character of the spiral arms (stronger arm patterns occur in galaxies with less lopsidedness), (2) is not correlated with the presence or absence of a bar, or the strength of the bar when one is present, (3) is inversely correlated to the stellar mass fraction, f_*_, within one radial scale length, and (4) correlates directly with f_*_ measured within the radial range over which we measure lopsidedness. We interpret these findings to mean that lopsidedness is a generic feature of galaxies and does not, generally, depend on a rare event, such as a direct accretion of a satellite galaxy onto the disk of the parent galaxy. While lopsidedness may be caused by several phenomena, moderate lopsidedness (<A_1_>_i_+<A_1_>_o_)/2<0.3) is likely to reflect halo asymmetries to which the disk responds or a gravitationally self-generated mode. We hypothesize that the magnitude of the stellar response depends both on how centrally concentrated the stars are with respect to the dark matter and whether there are enough stars in the region of the lopsidedness that self-gravity is dynamically important.2013ApJ...772..135Zhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/772/135CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toVII/237 : HYPERLEDA. I. Catalog of galaxies (Paturel+, 2003)J/A+A/569/A91 : Optical imaging for S4G (Knapen+, 2014)J/A+A/562/A121 : ARRAKIS: resonance rings in S4G (Comeron+ 2014)J/AJ/147/134 : Tully-Fisher relation for S^4^G galaxies (Zaritsky+, 2014)J/ApJ/771/59 : S4G face-on gal. surface brightness (Munoz-Mateos+, 2013)J/ApJS/197/22 : The Carnegie-Irvine Galaxy Survey (GGS). II. (Li+, 2011)J/MNRAS/416/2415 : Morphological parameters of WHISP gal. (Holwerda+, 2011)J/ApJS/190/147 : Mid-IR galaxy morphology from S^4^G (Buta+, 2010)J/PASP/122/1397 : Spitzer Survey of Stellar Structure in Gal. (Sheth+, 2010)J/A+A/438/507 : Degree of lopsidedness for galaxies (Bournaud+, 2005)http://irsa.ipac.caltech.edu/data/SPITZER/S4G/ : S^4^G data home pagehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/772/135https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/772/135http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/772/135https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/772/135https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/772/135http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/772/135GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJ/772/135/table1 (The Sample of the S4G sample observed)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJ/772/135/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJ/772/135/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJ/772/135/table1?GETtext/xml+votable180.050000true306.2592167-81.57529440.0055555555555555566/697 4446 4891 4953 5142 5198 5200 5463 5492 5590 5818 5976 5980 6034 6047 6087 6093 6116 6649 7225 7653 7658 8085 8089 8195 8287 8320 8458 8473 8492 8640 8729 9041 10328 10607 10637 10892 10901 11024 11025 11246 11306 11325 11394 11434 11772 11965 12095 12122 16467 16544 16845 16886 17606 17741 17754 17927 18011 18209 18226 18507 18676 19614 19667 19708 20008 20023 21155 24735 24912 24926 25127 25356 25490 25509 25512 25652 25653 25705 25862 25889 25890 25927 25946 26065 26234 26303 26324 26338 26344 26726 27150 27604 27730 27763 27773 27774 27861 27949 28044 28054 28142 28208 28213 28221 28264 28304 28416 28495 28521 28538 28631 33193 33242 33271 33835 33920 34334 34401 34471 34493 34545 34603 34687 35193 35966 35967 36022 36229 36236 36287 36480 36635 36677 36732 36793 36796 36822 40791 43881 43954 43977 43978 44027 44718 44817 45050 45112 45296 46013 46399 46438 46491 46509 46525 46549 46736 46819 47458 48132 48464 49010https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJ/772/135?format=asciiOpticalInfrareddefaultJ/ApJ/772/135/table1The Sample of the S4G sample observedrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameGalaxy Namemeta.id;meta.maincharTType[-5/10]? Galaxy morphology from HyperLedasrc.morphfloatnullableDist[1/84]? Distance from NEDMpcpos.distance;pos.heliocentricfloatnullable3.6Mag[-23/-11]? Total absolute Spitzer 3.6 micron band AB magnitudemagphys.magAbs;em.IR.3-4umfloatnullableRS[7.2/164.1] Surface brightness profile exponential scale length (R_S_)pixphys.angSize;srcfloatchi2{chi}^2^ (per d.o.f.) for exponential fitstat.fit.chi2floatArm[-1/2]? Arm classification (1)src.class.structintnullableBar[0/2]? Bar classification (2)meta.code.classintnullable<A1>iAverage of A_1_/A_0_ for inner radial range (3)src.morph.paramfloate_<A1>iUncertainty in <A1>istat.errorfloat<A2>iAverage of A_2_/A_0_ for inner radial rangesrc.morph.paramfloate_<A2>iUncertainty in <A2>istat.errorfloat<A1>oAverage of A_1_/A_0_ for outer radial range (3)src.morph.paramfloate_<A1>oUncertainty in <A1>ostat.errorfloat<A2>oAverage of A_2_/A_0_ for outer radial rangesrc.morph.paramfloate_<A2>oUncertainty in <A2>ostat.errorfloatth1.i[-464/744] Average phase of m=1 component over inner radial range <{theta}_1_>_i_degsrc.morph.paraminte_th1.iUncertainty in th1.idegstat.errorintth1.o[-550/761] Average phase of m=1 component over outer radial range <{theta}_1_>_o_degsrc.morph.paraminte_th1.oUncertainty in th1.odegstat.errorintLCatCross-match within 10" with lopsidedness catalogs (Bournaud et al. 2005, J/A+A/438/507 and Holwerda et al. 2011, J/MNRAS/416/2415)meta.ref.urlintnullableSCatCross-match within 10" with S4G catalogs (Sheth et al. 2010, J/PASP/122/1397; Buta et al. 2010, J/ApJS/190/147 and Munoz-Mateos et al. 2013, J/ApJ/771/59)meta.ref.urlintnullableSimbadSimbad column added by the CDSmeta.ref.urlcharNEDSimbad column added by the CDSmeta.ref.urlcharLEDASimbad 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.main