J/MNRAS/529/499ivo://CDS.VizieR/J/MNRAS/529/499doi:10.26093/cds/vizier.75290499CDSLazar I.Kaviraj S.Watkins A.E.Martin G.Bichang'a B.Jackson R.A.2024-11-06T20:35:21Z2024-04-18T07:41:28ZCDS support team

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

cds-question@unistra.frgalaxiesvisible-astronomygalaxy-classification-systemsccd-photometrycatalogsWe use a complete, unbiased sample of 257 dwarf (10^8^M_{sun}_<Mstar<10^9.5^M_{sun}_) galaxies at z<0.08, in the COSMOS field, to study the morphological mix of the dwarf population in low-density environments. Visual inspection of extremely deep optical images and their unsharp-masked counterparts reveals three principal dwarf morphological classes. 43 per cent and 45 per cent of dwarfs exhibit the traditional 'early-type' (elliptical/S0) and 'late-type' (spiral) morphologies, respectively. However, 10 per cent populate a 'featureless' class, that lacks both the central light concentration seen in early-types and any spiral structure - this class is missing in the massive-galaxy regime. 14 per cent, 27 per cent, and 19 per cent of early-type, late-type, and featureless dwarfs respectively show evidence for interactions, which drive around 20 per cent of the overall star formation activity in the dwarf population. Compared to their massive counterparts, dwarf early-types show a much lower incidence of interactions, are significantly less concentrated and share similar rest-frame colours as dwarf late-types. This suggests that the formation histories of dwarf and massive early-types are different, with dwarf early-types being shaped less by interactions and more by secular processes. The lack of large groups or clusters in COSMOS at z<0.08, and the fact that our dwarf morphological classes show similar local density, suggests that featureless dwarfs in low-density environments are created via internal baryonic feedback, rather than by environmental processes. Finally, while interacting dwarfs can be identified using the asymmetry parameter, it is challenging to cleanly separate early and late-type dwarfs using traditional morphological parameters, such as 'CAS', M20, and the Gini coefficient (unlike in the massive-galaxy regime).2024MNRAS.529..499Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/529/499CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/ApJS/258/11 : The COSMOS2020 catalog (Weaver+, 2022)https://hsc-release.mtk.nao.ac.jp/doc : HDC DR3 Home Pagehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/529/499https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/529/499http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/529/499https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/529/499https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/529/499http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/529/499GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/529/499/dw_class (Dwarf visual classifications, photo-z values and physical properties)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/529/499/dw_class?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/529/499/dw_class?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/529/499/dw_class?GETtext/xml+votable180.050000true150.84104363.0357795060.0055555555555555565/6814 6/27245 27247 27250 27344https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/529/499?format=asciiOpticaldefaultJ/MNRAS/529/499/dw_classDwarf visual classifications, photo-z values and physical propertiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDCatalog ID (ID)meta.id;meta.mainintHSCDR3HSC DR3 ID (ID_HSC_DR3)meta.idCOSMOS2020COSMOS2020 ID (ID_cosmos2020)meta.idintRAJ2000Right ascension (J2000) (RA)degpos.eq.ra;meta.mainDEJ2000Declination (J2000) (DEC)degpos.eq.dec;meta.mainMorphGalaxy morphology (Morphology) (1)src.morphcharInt-Flag[0/23] Interaction flag (Interaction_flag) (2)meta.codeintBar-Flag[0/1] Bar flag (0 = No bar present ; 1 = Bar present) (Bar_flag)meta.code.errorintlpzPDFPhotometric redshift (lp_zPDF) (3)src.redshift.photfloatb_lpzPDF? Photometric redshift lower 68 per cent confidence level (lp_zPDF_l68) (3)src.redshift.phot;phys.atmol.levelfloatnullableB_lpzPDF? Photometric redshift upper 68 per cent confidence level (lp_zPDF_u68) (3)src.redshift.phot;phys.atmol.levelfloatnullableloglpMassmedlog Stellar mass (lp_mass_med) (3)log(solMass)phys.massdoubleb_loglpMassmedlog Stellar mass lower 68 per cent confidence level (lp_mass_med_min68) (3)log(solMass)phys.mass;phys.atmol.leveldoubleB_loglpMassmedlog Stellar mass upper 68 per cent confidence level (lp_mass_med_max68) (3)log(solMass)phys.mass;phys.atmol.leveldoubleloglpSFRmed? log Star formation rate (lp_SFR_med) (3)log(solMass.yr**-1)meta.iddoublenullableb_loglpSFRmed? log Star formation rate lower 68 per cent confidence level (lp_SFR_med_min68) (3)log(solMass.yr**-1)meta.iddoublenullableB_loglpSFRmedlog Star formation rate upper 68 per cent confidence level (lp_SFR_med_max68) (3)log(solMass.yr**-1)meta.iddoublelpGMAGG band absolute rest-frame AB magnitude (HSC) (lp_MG) (3)magphys.magAbsdoublelpIMAGI band absolute rest-frame AB magnitude (HSC) (lp_MI) (3)magphys.magAbsdoublelptype[0/1] Star flag (0 : No star ; 1 : Star) (lp_type) (3)meta.code.errorintHSCimagAutoI band apparent magnitude (HSC) (HSC_i_MAG_AUTO) (4)magphot.mag;em.opt.IdoubleGextFlag[0/1]? G band extendedness flag (0 = Not extended ; 1 = Extended) (g_extendedness_value) (4)meta.codeintnullableRextFlag[0/1]? R band extendedness flag (0 = Not extended ; 1 = Extended) (r_extendedness_value) (4)meta.codeintnullableIextFlag[0/1]? I band extendedness flag (0 = Not extended ; 1 = Extended) (i_extendedness_value) (4)meta.codeintnullableZextFlag[0/1]? Z band extendedness flag (0 = Not extended ; 1 = Extended) (z_extendedness_value) (4)meta.codeintnullableJ/MNRAS/529/499/dw_paramDwarf morphological parametersrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDCatalog ID (ID)meta.id;meta.mainintCOSMOS2020COSMOS2020 ID (ID_cosmos2020)meta.idintBand[GRIYZ] Photometric band (Band)instr.bandpasscharCConcentration (C)meta.notedoubleA1.5RpetroAsymmetry calculated for an aperture up to 1.5 times the Petrosian radius (A_1.5Rpetro)spect.line.asymmetry;meta.modelleddoubleS1.5RpetroClumpiness calculated for an aperture up to 1.5 times the Petrosian radius (S_1.5Rpetro)src.morph.paramdoubleGiniGini coefficient (GINI)stat.fit.paramdoubleM20M20 value (M20)stat.fit.paramdoubleSersicNSersic index (SERSIC_N)stat.fit.paramdoubleA1RpetroAsymmetry calculated for an aperture up to the Petrosian radius (A_1Rpetro)spect.line.asymmetry;meta.modelleddoubleS1RpetroClumpiness calculated for an aperture up to the Petrosian radius (S_1Rpetro)src.morph.paramdouble