J/A+A/654/A105ivo://CDS.VizieR/J/A+A/654/A105doi:10.26093/cds/vizier.36540105CDSMarleau F.R.Habas R.Poulain M.Duc. P.A.Mueller O.Lim S.,Durrell P.R.Sanchez-Janssen R.Paudel S.Ahad S.L.Chougule A.,Bilek M.Fensch J.2025-12-03T20:00:51Z2021-10-20T07:41:11ZCDS support team

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

cds-question@unistra.frgalaxiescatalogsvisible-astronomyphotometryapparent-magnitudeRecent advances in deep dedicated imaging surveys over the past decade have uncovered a surprisingly large number of extremely faint low surface brightness galaxies with large physical sizes called ultra diffuse galaxies (UDGs) in clusters and, more recently, in lower density environments. As part of the Mass Assembly of early-Type GaLAxies with their fine Structures (MATLAS) survey, a deep imaging large program at the Canada-France-Hawaii Telescope (CFHT), our team has identified 2210 dwarf galaxies, 59 (~3%) of which qualify as UDGs. Averaging over the survey area, we find ~0.4 UDG per square degree. They are found in a range of low to moderate density environments, although 61% of the sample fall within the virial radii of groups. Based on a detailed analysis of their photometric and structural properties, we find that the MATLAS UDGs do not show significant differences from the traditional dwarfs, except from the predefined size and surface brightness cut. Their median color is as red as the one measured in galaxy clusters, albeit with a narrower color range. The majority of the UDGs are visually classified as dwarf ellipticals with log stellar masses of 6.5-8.7. The fraction of nucleated UDGs (~34%) is roughly the same as the nucleated fraction of the traditional dwarfs. Only five (~8%) UDGs show signs of tidal disruption and only two are tidal dwarf galaxy candidates. A study of globular cluster (GC) candidates selected in the CFHT images finds no evidence of a higher GC specific frequency S_N for UDGs than for classical dwarfs, contrary to what is found in most clusters. The UDG halo-to-stellar mass ratio distribution, as estimated from the GC counts, peaks at roughly the same value as for the traditional dwarfs, but spans the smaller range of ~10-2000. We interpret these results to mean that the large majority of the field-to-group UDGs do not have a different formation scenario than traditional dwarfs.2021A&A...654A.105Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/654/A105CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/MNRAS/446/120 : ATLAS3D project. XXIX (Duc+, 2015)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/654/A105https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/654/A105http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/654/A105https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/654/A105https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/654/A105http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/654/A105GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/654/A105/table1 (Photometric properties of the MATLAS UDGs)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/654/A105/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/654/A105/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/654/A105/table1?GETtext/xml+votable180.050000true20.6268.76140.0055555555555555566/664-665 4807 4840 5152 5196 5429 6010 7214 7385 8193 8195-8196 10523 10637 10639 11026 11246 11442 11791 11802 11813 11824 17761 18321 20015 25892 25907 25979 26055 26066 26149 26172-26173 27079 27199 27671 27714 27722 27844 28221 28491-28492 31455 36822https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/654/A105?format=asciiOpticaldefaultJ/A+A/654/A105/table1Photometric properties of the MATLAS UDGsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameUDG ID, MATLAS-NNNNmeta.id;meta.maincharRAJ2000Right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.mainMorphMorphologysrc.morphcharDist1Assumed host ETG distancepos.distancefloatDist2? Dwarf distancepos.distancefloatnullablegmagApparent magnitude in the g-bandmagphot.mag;em.opt.Bfloate_gmagApparent magnitude in the g-band erromagstat.error;phot.magfloatg-r? g-r color corrected for Galactic extinctionmagphot.color;em.opt.B;em.opt.Rfloatnullablee_g-r? g-r color corrected for Galactic extinction errormagstat.error;phot.color;em.opt.Bfloatnullableg-i? g-i color corrected for Galactic extinctionmagphot.color;em.opt.B;em.opt.Ifloatnullablee_g-i? g-i color corrected for Galactic extinction errormagstat.errorfloatnullablegMAGAbsolute magnitude in the g-band (1)magphys.magAbsfloate_gMAGAbsolute magnitude in the g-band (1)magstat.errorfloatSimbadSimbad column added by the CDSmeta.ref.urlcharJ/A+A/654/A105/table2Additional properties of the MATLAS UDGs (updated version from erratum, 03-Dec-2025)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameUDG ID, MATLAS-NNNNmeta.id;meta.maincharmu0Central surface brightness in the g-bandmag.arcsec**-2phot.mag.sbfloate_mu0Central surface brightness in the g-band errormag.arcsec**-2stat.errorfloatmueavgAverage surface brightness within one effective radius in the g-bandmag.arcsec**-2phot.mag.sbfloate_mueavgAverage surface brightness within one effective radius in the g-bandmag.arcsec**-2stat.errorfloatReEffective radius in arcsec in the g-bandarcsecphys.angSizefloate_ReEffective radius in arcsec in the g-bandarcsecstat.errorfloatRekpcEffective radius in kpc in the g-band (1)kpcphys.size.radiusfloate_RekpcEffective radius in kpc in the g-band error (1)kpcstat.errorfloatlog(M*)? Stellar mass computed based on the stellar mass-to-light ratios (2)log(solMass)phys.massfloatnullablee_log(M*)? Stellar mass computed based on the stellar mass-to-light ratios error (2)log(solMass)stat.errorfloatnullableMhalo/M*? Halo-to-stellar mass ratio (3)phys.mass;arith.ratiofloatnullablee_Mhalo/M*? Error on halo-to-stellar mass ratio, lower valuestat.errorfloatnullableE_Mhalo/M*? Error on halo-to-stellar mass ratio, upper valuestat.error;stat.maxfloatnullable