J/A+A/683/A205ivo://CDS.VizieR/J/A+A/683/A205doi:10.26093/cds/vizier.36830205CDSEpinat B.Contini T.Mercier W.Ciesla L.Lemaux B.C.Johnson S.D.,Richard J.Brinchmann J.Boogaard L.A.Carton D.Michel-Dansac L.,Bacon R.Krajnovic D.Finley H.Schroetter I.Ventou E.,Abril-Melgarejo V.Boselli A.Bouche N.F.Kollatschny W.Kovac K.,Paalvast M.Soucail G.Urrutia T.Weilbacher P.M.2024-11-07T20:01:42Z2024-03-20T09:55:16ZCDS support team

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

cds-question@unistra.frgalaxy-clustersgalaxiescatalogsredshiftedGalaxies migrate along cosmic web filaments from small groups to clusters, which makes the evolution of their properties look stronger as environments get denser. We introduce the MUSE gAlaxy Groups in COSMOS (MAGIC) survey built to study the impact of environment on galaxy evolution down to low stellar masses over the last eight Gyr. The MAGIC survey consists of 17 Multi-Unit Spectrocopic Exporer (MUSE) fields targeting 14 massive, known structures at intermediate redshift (0.3<z<0.8) in the COSMOS area, with a total on-source exposure of 67h. We securely measure redshifts for 1419 sources and identify 76 galaxy pairs and 67 groups of at least three members using a friends-of- friends algorithm. The environment of galaxies is quantified from group properties, as well as from global and local density estimators, inferred from galaxy number density and dynamics within groups. The MAGIC survey has increased the number of objects with a secure spectroscopic redshift over its footprint by a factor of ~5 compared to the previous extensive spectroscopic campaigns on the COSMOS field. Most of the new redshifts have apparent magnitudes in the z++ band z++_app>21.5. The spectroscopic redshift completeness is high: in the redshift range of [OII] emitters (0.25<z<1.5), where most of the groups are found, it globally reaches a maximum of 80% down to z++_app_=25.9, and it locally decreases from ~100% to ~50% in magnitude bins from z++_app_=23-24 to z++_app_=25.5. We find that the fraction of quiescent galaxies increases with local density and with the time spent in groups. A morphological dichotomy is also found between bulge-dominated quiescent and disk-dominated star-forming galaxies. As environment gets denser, the peak of the stellar mass distribution shifts towards M*>10^10^M_{sun}_, the fraction of galaxies with M*<10^9^M_{sun}_ decreasing significantly, even for star-forming galaxies. We also highlight peculiar features such as close groups, extended nebulae, and a gravitational arc. Our results suggest that galaxies are pre- processed in groups of increasing mass before entering rich groups and clusters. We publicly release two catalogs containing the properties of galaxies and groups, respectively.2024A&A...683A.205Ehttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/683/A205CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/ApJ/753/121 : zCOSMOS 20k sample group catalog to z<~1.2 (Knobel+, 2012)J/ApJS/224/24 : The COSMOS2015 catalog (Laigle+, 2016)J/MNRAS/483/3545 : X-ray centres of COSMOS galaxy groups (Gozaliasl+, 2019)J/A+A/677/A143 : Angular momentum in MAGIC. I. Environment (Mercier+, 2023)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/683/A205https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/683/A205http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/683/A205https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/683/A205https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/683/A205http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/683/A205GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/683/A205/group (MAGIC group catalog (table A1))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/683/A205/group?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/683/A205/group?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/683/A205/group?GETtext/xml+votable180.050000true150.05232.60740.005555555555555556Cone search capability for table J/A+A/683/A205/galaxy (*MAGIC galaxy catalog (table A2))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/683/A205/galaxy?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/683/A205/galaxy?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/683/A205/galaxy?GETtext/xml+votable180.050000true149.785131112.160071940.0055555555555555566/27256 27258https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/683/A205?format=asciidefaultJ/A+A/683/A205/groupMAGIC group catalog (table A1)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMGR[1/143] MAGIC group IDmeta.id;meta.mainintRAJ2000Right ascension (J2000) of the unweighted barycenter of the groupdegpos.eq.ra;meta.mainDEJ2000Declination (J2000) of the unweighted barycenter of the groupdegpos.eq.dec;meta.mainRichNumber of members within the groupmeta.numberintzMean redshift of the groupsrc.redshiftdoublesigma? Velocity dispersion of galaxies in the group, using the Gapper method (1)km/sphys.veloc.dispersionfloatnullablelogMvir? Group virial mass (1)log(solMass)phys.massfloatnullableR200? Group R200 radius (1)kpcphys.size.radius;pos.lgfloatnullableCGR? Group ID in the zCOSMOS 20k group catalog when matched (2)meta.idintnullableCW? Group ID in the COSMOS Wall group catalog when matched (3)meta.idintnullableXray? Group ID in the X-ray group catalog when matched (4)meta.idintnullableXraysep? Angular separation between MAGIC and X-ray centers (5)arcsecpos.angDistancefloatnullablelogXM200? Mass at radius R200 inferred from X-rays (5)log(solMass)phys.massfloatnullableXR200? R200 radius inferred from X-rays (5)kpcphys.size.radiusfloatnullableJ/A+A/683/A205/galaxy*MAGIC galaxy catalog (table A2)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintlogM*? Logarithm of stellar mass within a 3 arcsec aperture estimated from SED fitting with CIGALElog(solMass)phys.massdoublenullablee_logM*? Uncertainty on the logarithm of stellar mass within 3 arcsec apertureslog(solMass)stat.errordoublenullablelogSFR? Logarithm of SFR within a 3 arcsec aperture estimated from SED fitting with CIGALElog(solMass.yr**-1)phys.SFRdoublenullablee_logSFR? Uncertainty on the logarithm of SFR within 3 arcsec apertureslog(solMass.yr**-1)stat.error;phys.SFRdoublenullableE(B-V)? Color excess estimated from SED fitting with CIGALEmagphot.color.excessdoublenullableNUV-RP? NUV-r+ rest-frame color estimated from SED fitting with CIGALEmagphot.color;em.UV.200-300nm;em.opt.RdoublenullableRP-J? r+-J rest-frame color estimated from SED fitting with CIGALEmagphot.color;em.opt.RdoublenullableMGR? MAGIC group ID to which the galaxy belongs, as defined in the group catalogmeta.idintnullablelogVMCDGalaxy density at the location of the galaxy inferred from the VMC methodlog(Mpc**-2)src.densitydoublelogVMCODGalaxy over-density at the location of the galaxy inferred from the VMC methodsrc.densitydoublelogVORD? Galaxy density at the location of the galaxy inferred from Voronoi tessellationslog(Mpc**-2)src.densitydoublenullableDR? Distance to group centerkpcpos.distancedoublenullableDV? Velocity in the frame of the group with respect to the group redshiftkm/sphys.velocfloatnullableC2015? Object ID in the COSMOS2015 catalog (1)meta.idintnullableFieldName of the MAGIC fieldobs.fieldcharETA? Phase space parameterstat.fit.paramdoublenullableIDMAGIC object ID, of the form X_CGrY, where X is the identifier within the fields corresponding to COSMOS group CGrYmeta.id;meta.maincharRAJ2000Right ascension (J2000) (2)degpos.eq.ra;meta.mainDEJ2000Declination (J2000) (2)degpos.eq.dec;meta.mainzSystemic redshift of the source (2)src.redshiftdoubleConfid[0/3] Redshift confidence level from 1 (low) to 3 (high)meta.code.qualint