J/MNRAS/467/3140ivo://CDS.VizieR/J/MNRAS/467/3140doi:10.26093/cds/vizier.74673140CDSSwinbank A.M.Harrison C.M.Trayford J.Schaller M.Smail I.,Schaye J.Theuns T.Smit R.Alexander D.M.Bacon R.Bower R.G.,Contini T.Crain R.A.De Breuck C.Decarli R.Epinat B.Fumagalli M.,Furlong M.Galametz A.Johnson H.L.Lagos C.Richard J.Vernet J.,Sharples R.M.Sobral D.Stott J.P.2024-08-17T20:18:17Z2019-12-16T10:13:56ZCDS support team

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

cds-question@unistra.frgalaxiescatalogsredshiftedgalaxy-kinematicsWe present a MUSE (Multi-Unit Spectroscopic Explorer) and KMOS (K-band Multi-Object Spectrograph) dynamical study 405 star-forming galaxies at redshift z=0.28-1.65 (median redshift <z>=0.84). Our sample is representative of the star-forming 'main sequence', with star formation rates of SFR=0.1-30M_{sun}_/yr and stellar masses M*=10^8^-10^11^M_{sun}_. For 49+/-4 per cent of our sample, the dynamics suggest rotational support, 24+/-3 per cent are unresolved systems and 5+/-2 per cent appear to be early-stage major mergers with components on 8-30kpc scales. The remaining 22+/-5 per cent appear to be dynamically complex, irregular (or face-on systems). For galaxies whose dynamics suggest rotational support, we derive inclination-corrected rotational velocities and show that these systems lie on a similar scaling between stellar mass and specific angular momentum as local spirals with j*=J/M*{prop.to}M*^2/3^ but with a redshift evolution that scales as j*{prop.to}M*^2/3^(1+z)^-1^. We also identify a correlation between specific angular momentum and disc stability such that galaxies with the highest specific angular momentum (log(j*/M*^2/3^)>2.5) are the most stable, with Toomre Q=1.10+/-0.18, compared to Q=0.53+/-0.22 for galaxies with log(j*/M*^2/3^)<2.5. At a fixed mass, the Hubble Space Telescope morphologies of galaxies with the highest specific angular momentum resemble spiral galaxies, whilst those with low specific angular momentum are morphologically complex and dominated by several bright star-forming regions. This suggests that angular momentum plays a major role in defining the stability of gas discs: at z~1, massive galaxies that have discs with low specific angular momentum are globally unstable, clumpy and turbulent systems. In contrast, galaxies with high specific angular momentum have evolved into stable discs with spiral structure where star formation is a local (rather than global) process.2017MNRAS.467.3140Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/467/3140CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/467/3140https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/467/3140http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/467/3140https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/467/3140https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/467/3140http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/467/3140GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/467/3140/table2 (Galaxy properties)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/467/3140/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/467/3140/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/467/3140/table2?GETtext/xml+votable180.050000true149.919179172.351152780.0055555555555555566/17678 17769 18717 19033 19433 27256 27258 27578 31529 44713 45526 46795 46831 47424 47463 481547.952274030004205e-20 3.852589004194616e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/467/3140?format=asciidefaultJ/MNRAS/467/3140/table2Galaxy propertieszRedshiftsrc.redshiftfloatDEJ2000Declination (J2000)pos.eq.dec;meta.mainrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDNamemeta.id;meta.maincharRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainVmag? V magnitude (AB)magphot.mag;em.opt.VfloatnullableKmag? K magnitude (AB)magphot.mag;em.IR.Kfloatnullablef(neb)Nebular emission line flux ([OII] in the case of MUSE and H{alpha} for KMOS)1e-20W.m**-2phot.flux;spect.linefloatrh*Deconvolved continuum emission half-light radiusarcsecphys.angSize;srcfloate_rh*rms uncertainty on rh*arcsecstat.errorfloatrhnebNnebular emission half-light radiusarcsecphys.angSize;srcfloate_rhnebrms uncertainty on rhnebarcsecstat.errorfloatHmag? Absolute H magnitudemagphys.magAbs;em.IR.HfloatnullablelogM*? Stellar masslog(solMass)phys.massfloatnullablesigmagal? Galaxy-integrated velocity dispersion as measured from the one-dimensional spectrumkm/sphys.veloc.dispersionintnullablee_sigmagal? rms uncertainty on sigmagalkm/sstat.errorintnullablesigmaint? Average intrinsic velocity dispersion within the galaxy (after correcting for beam smearing effects)km/sphys.veloc.dispersion;stat.meanintnullablee_sigmaint? rms uncertainty on sigmaintkm/sstat.errorintnullableV(3Rd)? Observed velocity at 3Rdkm/sphys.velocintnullablee_V(3Rd)? rms uncertainty on V(3Rd)km/sstat.errorintnullableinc? Disk inclinationdegsrc.orbital.inclinationintnullablee_inc? rms uncertainty on incdegstat.errorintnullableAv? Reddeningmagphys.absorptionfloatnullablej*? Angular momentumkm.s**-1.kpcphys.angMomentumintnullablee_j*? rms uncertainty on j*km.s**-1.kpcstat.errorintnullableSFR? Star-formation rate (1)solMass/yrphys.SFRintnullableClass[CDIM] Class (2)meta.codechar