J/A+A/647/A100ivo://CDS.VizieR/J/A+A/647/A100doi:10.26093/cds/vizier.36470100CDSSu A.H.Salo H.Janz J.Laurikainen E.Venhola A.Peletier R.F.,Iodice E.Hilker M.Cantiello M.Napolitano N.Spavone M.Raj M.A.,van de Ven G.Mieske S.Paolillo M.Capaccioli M.Valentijn E.A.,Watkins A.E.2023-06-09T13:07:35Z2021-03-16T07:06:42ZCDS support team

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

cds-question@unistra.frgalaxy-clustersphotometrygalaxy-classification-systemsGalaxies either live in a cluster, a group, or in a field environment. In the hierarchical framework, the group environment bridges the field to the cluster environment, as field galaxies form groups before aggregating into clusters. In principle, environmental mechanisms, such as galaxy-galaxy interactions, can be more efficient in groups than in clusters due to lower velocity dispersion, which lead to changes in the properties of galaxies. This change in properties for group galaxies before entering the cluster environment is known as preprocessing. Whilst cluster and field galaxies are well studied, the extent to which galaxies become preprocessed in the group environment is unclear. We investigate the structural properties of cluster and group galaxies by studying the Fornax main cluster and the infalling Fornax A group, exploring the effects of galaxy preprocessing in this showcase example. Additionally, we compare the structural complexity of Fornax galaxies to those in the Virgo cluster and in the field. Our sample consists of 582 galaxies from the Fornax main cluster and Fornax A group. We quantified the light distributions of each galaxy based on a combination of aperture photometry, Sersic+PSF (point spread function) and multi-component decompositions, and non-parametric measures of morphology. From these analyses, we derived the galaxy colours, structural parameters, non-parametric morphological indices (Concentration C; Asymmetry A, Clumpiness S; Gini G; second order moment of light M_20_), and structural complexity based on multi-component decompositions. These quantities were then compared between the Fornax main cluster and Fornax A group. The structural complexity of Fornax galaxies were also compared to those in Virgo and in the field. We find significant (Kolmogorov-Smirnov test p-value <alpha=0.05) differences in the distributions of quantities derived from Sersic profiles (g'-r', r'-i', Re, and {bar}{mu}_e,r'_), and non-parametric indices (A and S) between the Fornax main cluster and Fornax A group. Fornax A group galaxies are typically bluer, smaller, brighter, and more asymmetric and clumpy. Moreover, we find significant cluster-centric trends with r'-i', Re, and {bar}{mu}_e,r'_, as well as A, S, G, and M_20_ for galaxies in the Fornax main cluster. This implies that galaxies falling towards the centre of the Fornax main cluster become fainter, more extended, and generally smoother in their light distribution. Conversely, we do not find significant group-centric trends for Fornax A group galaxies. We find the structural complexity of galaxies (in terms of the number of components required to fit a galaxy) to increase as a function of the absolute r'-band magnitude (and stellar mass), with the largest change occurring between -14mag<~Mr'<~-19,mag (7.5<~log_10_(M*/M_{sun}_)~=9.7). This same trend was found in galaxy samples from the Virgo cluster and in the field, which suggests that the formation or maintenance of morphological structures (e.g. bulges, bar) are largely due to the stellar mass of the galaxies, rather than the environment they reside in.2021A&A...647A.100Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/647/A100CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/ApJS/219/4 : S4G pipeline 4: multi-component decompositions (Salo+, 2015)J/A+A/608/A142 : Fornax Deep Survey with VST. III. (Venhola+, 2017)J/A+A/620/A165 : Fornax Deep Survey with VST. IV. (Venhola+, 2018)J/A+A/623/A1 : Fornax Deep Survey with VST. V. (Iodice+, 2019)J/A+A/639/A136 : Fornax Deep Survey with VST. IX. (Cantiello+, 2020)https://www.oulu.fi/astronomy/FDS_DECOMP/main/index.html :https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/647/A100https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/647/A100http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/647/A100https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/647/A100https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/647/A100http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/647/A100GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/647/A100/tablei1 (Summary table of FDS properties)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/647/A100/tablei1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/647/A100/tablei1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/647/A100/tablei1?GETtext/xml+votable180.050000true54.6209-35.45040.0055555555555555564/2158 5/8623 8636 6/34487 34491 34507 34510-34511 34520 34522-34523 34552-34554 35860 35905 35908-35909https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/647/A100?format=asciiOpticaldefaultJ/A+A/647/A100/tablei1Summary table of FDS propertiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintFDSFDS identification number, FDSNN_NNNNameta.id;meta.maincharFCCFCC identification number, FCCNNN, if availablemeta.idcharONameOther known catalog name from HyperLedameta.idcharRAJ2000Right ascension (J2000)degpos.eq.ra;meta.mainBar/T? Bar-to-total ratiophys.luminosity;arith.ratiofloatnullableSimbadSimbad column added by the CDSmeta.ref.urlcharDEJ2000Declination (J2000)degpos.eq.dec;meta.mainlogMstarlog10 of stellar mass in solar mass unitslog(solMass)phys.massfloatMCmodelModel components from multi-component decompositions (1)stat.paramcharB/T? Bulge-to-total ratiophys.luminosity;arith.ratiofloatnullableReffEffective radius from the outermost multi-component disk componentarcsecphys.angSizefloatS4Goverlap[Yes No] If galaxy is also in S4G (Salo et al., 2015, Cat. J/ApJS/219/4)meta.codecharJ/A+A/647/A100/table2Table of parameters from Sersic+PSF decompositionsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintFDSFDS identification number, FDSNN_NNNNbmeta.id;meta.maincharrmagSSersic r-band total magnitudemagphot.mag;em.opt.Rfloatg-rSSersic g-r colourmagphot.color;em.opt.B;em.opt.Rfloatr-iSSersic r-i colourmagphot.color;em.opt.R;em.opt.IfloatreffSersic effective radiusarcsecphys.angSizefloatnSersic indexstat.fit.paramfloatb/aSersic axial ratio (=b/a)phys.angSize;arith.ratiofloatPA[] Sersic position angledegpos.posAngfloatrmagPPSF r-band total magnitudemagphot.mag;em.opt.Rfloatg-rPPSF g-r colour indexmagphot.color;em.opt.B;em.opt.Rfloatr-iPPSF r-i colour indexmagphot.color;em.opt.R;em.opt.IfloatJ/A+A/647/A100/table3Table of non-parametric indicesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintFDSFDS identification number, FDSNN_NNNNameta.id;meta.maincharCConcentrationmeta.notefloatAAsymmetryspect.line.asymmetryfloatSClumpinesssrc.morph.paramfloatGGini coefficientmeta.notefloatM20Brightest second order moment of lightstat.variance;phys.composition.massLightRatiofloatDg-rOuter minus inner g-r colour differencemagphot.color;arith.difffloat