J/A+A/708/A125ivo://CDS.VizieR/J/A+A/708/A125CDSMoretti A.Paladino R.Bacchini C.Marasco A.Giunchi E.,Poggianti B.M.Hunt L.K.Deb T.Vulcani B.Gullieuszik M.Lassen A.,Wolter A.Gitti M.Radovich M.Fritz J.Tomicic N.2026-05-04T07:43:19Z2026-03-31T10:28:48ZCDS support team

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

cds-question@unistra.frgalaxy-clustersradio-sourcesstar-forming-regionsmillimeter-astronomysubmillimeter-astronomySeveral studies have reported a nearly linear correlation between the molecular gas and star formation rate surface density, the so-called Kennicutt-Schmidt (KS) law. We aim to retrieve the KS relation for a sample of four star-forming galaxies located in nearby clusters, disturbed by the effects of the ram pressure stripping, as testing this law in galaxies subject to different environmental conditions can provide key information on the physics of star formation. To perform our analysis, we used ALMA band 6 and band 3 data coupled with MUSE data at spatial resolution of ~1 kpc. Moreover, we analyzed data of star-forming complexes detected through their H{alpha} ionized gas emission. We also derived the star formation efficiencies of the star-forming regions nested in these big complexes using the star formation rates derived from spatially resolved HST images and various recipes for the corresponding cold gas phase. We find that ram-pressure-stripped galaxies show normal-to-low star formation efficiencies, depending on the position within the galaxy and on the local gas density: the inner dense regions in the disk show higher efficiencies with respect to the outer regions, including the gaseous tails. The global relation between the star formation rate density and the molecular gas surface density is superlinear, likely suggesting the shortening of the depletion times at high gas mass densities caused by the ram pressure. Within the star-forming complexes, the star formation efficiency is very similar to the one observed at 1kpc scale in undisturbed star-forming disks. Interestingly, this result holds also for the star-forming complexes located in the stripped gas tails. The analysis of HST resolved clumps suggests that the molecular gas is not uniformly distributed within the star-forming complexes, but its density distribution follows a steeper profile.2026A&A...708A.125Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/708/A125CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/708/A125https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/708/A125http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/708/A125https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/708/A125https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/708/A125http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/708/A125GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/708/A125/table5 (Star forming clump properties)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/708/A125/table5?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/708/A125/table5?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/708/A125/table5?GETtext/xml+votable180.050000true10.38908-9.276760.0055555555555555566/17237 19130 20083 27224https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/708/A125?format=asciiMillimeterRadiodefaultJ/A+A/708/A125/table5Star forming clump propertiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBlobIdObject Identifiermeta.id;meta.maincharRAJ2000Right Ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.mainAreaBlob area measured by MUSEkpc**2phys.angSizefloatV21Velocitykm/sphys.velocdoublesigma21Velocity dispersionkm/sphys.veloc.dispersionfloatFlux21GCO(2-1) gaussian fluxJyphot.flux.density;em.radiofloatFlux21CO(2-1) total fluxJyphot.flux.density;em.radiofloate_Flux21Error on fluxJystat.errorfloatS/N21Signal-to-Noise ratiostat.snrfloatVisFlag[03] Visual classification flag (1)meta.codecharFlux21finFinal flux valueJyphot.flux.density;em.radiofloatMH2finFinal H_2_ masses1e+09solMassphys.massfloat