J/A+A/631/A87ivo://CDS.VizieR/J/A+A/631/A87doi:10.26093/cds/vizier.36310087CDSVentou E.Contini T.Bouche N.Epinat E.Brinchmann J.Inami H.,Richard J.Schroetter I.Soucail G.Steinmetz M.Weilbacher P.2025-01-09T20:00:35Z2019-10-25T08:45:46ZCDS support team

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

cds-question@unistra.frgalaxiesspectroscopyredshiftedsurveysUsing the ILLUSTRIS cosmological simulation project, we investigate the relation between the separation of galaxies in a pair, both in velocity and projected spatial separation space, and the probability that these interacting galaxies will merge in the future. From this analysis, we propose a new set of criteria to select close pairs of galaxies along with a new corrective term to be applied to the computation of the galaxy merger fraction. We then probe the evolution of the major and minor merger fraction using the latest MUSE deep observations over the Hubble Ultra Deep Field, Hubble Deep Field South, COSMOS-Gr30 and Abell 2744 regions. From a parent sample of 2483 galaxies with spectroscopic redshifts, we identify 366 close pairs spread over a large range of redshifts (0.2<z<6) and stellar masses (10^7^-10^11^M_{sun}_). Using the stellar mass ratio between the secondary and primary galaxy as a proxy to split the sample into major, minor and very minor mergers, we found a total of 183 major, 142 minor and 47 very minor close pairs corresponding to a mass ratio range of 1:1-1:6, 1:6-1:100 and lower than 1:100, respectively. Due to completeness issues, we do not consider the very minor pairs in the analysis. Overall, the major merger fraction increases up to z~2-3 reaching 25% for pairs with the most massive galaxy with a stellar mass M*>10^9.5^M_{sun}_. Beyond this redshift, the fraction decreases down to ~5% at z~6. The major merger fraction for lower mass primary galaxies M*<10^9.5^M_{sun}_, seems to follow a more constant evolutionary trend with redshift. Thanks to the addition of new MUSE fields and new selection criteria, the increased statistics of the pair samples allow to narrow significantly the error bars compared to our previous analysis (Ventou et al., 2017A&A...608A...9V). The evolution of the minor merger fraction is roughly constant with cosmic time, with a fraction of 20% at z<3 and a slow decrease between 3<z<6 to 8-13%.2019A&A...631A..87Vhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/631/A87CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/575/A75 : MUSE 3D view of HDF-S (Bacon+, 2015)J/A+A/608/A2 : MUSE Hubble Ultra Deep Field Survey. II. (Inami+, 2017)J/MNRAS/473/663 : MUSE and HFFs Photometry of A2744 (Mahler+, 2018)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/631/A87https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/631/A87http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/631/A87https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/631/A87https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/631/A87http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/631/A87GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/631/A87/major (Major close pairs of galaxies (table B3))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/631/A87/major?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/631/A87/major?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/631/A87/major?GETtext/xml+votable180.050000true53.16196298-27.773905140.005555555555555556Cone search capability for table J/A+A/631/A87/minor (Minor close pairs of galaxies (table B4))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/631/A87/minor?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/631/A87/minor?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/631/A87/minor?GETtext/xml+votable180.050000true53.16992265-27.771024510.0055555555555555566/848 16486 27256 35935 45526https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/631/A87?format=asciidefaultJ/A+A/631/A87/majorMajor close pairs of galaxies (table B3)FieldSky observed with MUSE (1)obs.fieldcharRA2degSecond galaxy right ascension (J2000)degpos.eq.raDE2degSecond galaxy declination (J2000)degpos.eq.decrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintID1MUSE Identification number of the first galaxy in the pairmeta.id.part;meta.mainintRA1First galaxy right ascension (J2000)degpos.eq.ra;meta.mainDE1First galaxy declination (J2000)degpos.eq.dec;meta.mainz1MUSE spectroscopic redshift of the first galaxy in the pairsrc.redshiftfloatlogM1Stellar mass (in log) of the first galaxy in the pairlog(solMass)phys.massfloatID2MUSE Identification number of the second galaxy in the pairmeta.id.part;meta.maincharz2MUSE spectroscopic redshift of the second galaxy in the pairsrc.redshiftfloatlogM2Stellar mass (in log) of the second galaxy in the pairlog(solMass)phys.massfloatrpProjected separation between the two galaxies in the pairkpcpos.angDistancefloatDvVelocity difference between the two galaxies in the pairkm/sphys.veloc;arith.diffintSimbadNameSimbad column added by the CDSmeta.idcharnullableJ/A+A/631/A87/minorMinor close pairs of galaxies (table B4)FieldSky observed with MUSE (1)obs.fieldcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintID1MUSE Identification number of the first galaxy in the pairmeta.id.part;meta.mainintRA1First galaxy right ascension (J2000)degpos.eq.ra;meta.mainDE1First galaxy declination (J2000)degpos.eq.dec;meta.mainz1MUSE spectroscopic redshift of the first galaxy in the pairsrc.redshiftfloatlogM1Stellar mass (in log) of the first galaxy in the pairlog(solMass)phys.massfloatID2MUSE Identification number of the second galaxy in the pairmeta.id.part;meta.maincharRA2degSecond galaxy right ascension (J2000)degpos.eq.raDE2degSecond galaxy declination (J2000)degpos.eq.decz2MUSE spectroscopic redshift of the second galaxy in the pairsrc.redshiftfloatlogM2Stellar mass (in log) of the second galaxy in the pairlog(solMass)phys.massfloatrpProjected separation between the two galaxies in the pairkpcpos.angDistancefloatDvVelocity difference between the two galaxies in the pairkm/sphys.veloc;arith.diffintSimbadNameSimbad column added by the CDSmeta.idcharnullable