J/A+A/693/A21ivo://CDS.VizieR/J/A+A/693/A21doi:10.26093/cds/vizier.36930021CDSShen H.Esimbek J.Henkel C.Li D.Zhou J.He Y.Tang X.Wu G.,Komesh T.Tursun K.Zhou D.Sailanbek S.Berdikhan D.2025-02-24T20:02:20Z2024-12-23T10:08:34ZCDS support team

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

cds-question@unistra.frmolecular-cloudsco-line-emissionradio-astronomygalaxy-classification-systemsgalaxy-kinematicsThe W3/4 Giant Molecular Cloud (GMC) is an ideal target to study the impact of HII regions onto the surrounding molecular gas and star formation. We utilized PMO CO (1-0) data from the Milky Way Imaging Scroll Painting (MWISP) survey to analyze the cloud structure and the feedback effect from the W4 HII region. Our observations show that cold gas, traced by CO, mainly resides in the W3 GMC, with C^18^O concentrated in dense regions, while gas around W4 is dispersed. The ^13^CO position-position-velocity (PPV) distributions reveal a C shaped structure in the W3 cloud with more redshifted gas at higher galactic longitudes. A high density layer (HDL) region on the eastern side of the W3 region exhibits a flattened structure facing W4. Subdividing the area into sixteen subregions, we find that regions 6-9 on the HDL layer exhibit the strongest radiation, while clouds at the W4 bubble boundary not facing W3 exhibit weak signals, possibly due to star formation triggering and subsequent molecular gas dispersal by the HII region. Analysis along four paths from the W4 HII region to the far side shows a consistent trend of sharply increasing intensity followed by a slow decrease, indicating the gas is effectively eroded and heated by the photon dominated region (PDR) near the boundary of the HII region. Clump identification based on ^13^CO emission reveals 288 structures categorized as bubble, HDL, and quiescent clumps. Analysis of mass- radius and Virial-mass relationships show a potential for high-mass star formation in 29.5% (85/288) of the clumps, with 39.2% (113/288) being gravitationally bound. HDL clumps exhibit distinct L/M and velocity dispersion, suggesting an earlier evolutionary stage and gravitational instability compared to quiescent and bubble clumps. Clump parameter differences provide evidence for triggered and dispersed effects of the W4 HII region on the HDL and bubble regions, respectively.2025A&A...693A..21Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/693/A21CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/693/A21https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/693/A21http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/693/A21https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/693/A21https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/693/A21http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/693/A21GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/693/A21/table1 (^13^CO clump properties derived from dendrogram leaves of W3/4)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/693/A21/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/693/A21/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/693/A21/table1?GETtext/xml+votable180.050000true39.41860.57790.0055555555555555565/826 912 6/3308-3310 3605 3607 3652https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/693/A21?format=asciiOpticalRadiodefaultJ/A+A/693/A21/table1^13^CO clump properties derived from dendrogram leaves of W3/4recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintID[0/328] Leaf numbermeta.id;meta.mainintGLONGalactic longitudedegpos.galactic.lonGLATGalactic latitudedegpos.galactic.latVmeanMean velocity of the structurekm/sphys.veloc;stat.meanfloatFWHMFWHM line widthkm/sspect.line.widthfloatRadiusLeaf radiuspcphys.angSize;srcfloatLumLuminositysolLumphys.luminosityfloat_RA.icrsRight ascension (ICRS) (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.raindexed_DE.icrsDeclination (ICRS) (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.decindexedN(H2)H_2_ column density1e+22cm**-2phys.columnDensityfloatM(LTE)LTE masssolMassphys.massfloatMvirVirial masssolMassphys.massdoublealphavirVirial parameterphys.mass;arith.ratiofloatn(H2)Volume density10000cm**-3phys.densityfloatSigmaSurface mass densitysolMass.pc**-2phot.flux.density.sbfloatL/MThe ratio of luminosity to LTE mass0.001solLum.solMass**-1phys.luminosityfloatTexCO excitation temperatureKphys.atmol.excitation;spect.linefloatVthermThermal velocity dispersionkm/sphys.veloc.dispersionfloatVnthermNon-thermal velocity dispersionkm/sphys.veloc.dispersionfloatVntherm/VthermThe ratio of Vnthermal/vthermalphys.veloc;arith.difffloat